INAF - Osservatorio Astronomico di Bologna

INAF
Osservatorio Astronomico di Bologna
Annual Report 2007
Osservatorio Astronomico di Bologna
Via Ranzani 1, I-40127 Bologna, ITALY
Tel.: +39-051-2095701 ; Fax: +39-051-2095700
http://www.bo.astro.it/
Cover: Iron and Oxygen distribution maps in faked X-ray observations of numerically simulated galaxy clusters (Rasia et al. 2007).
Introduction
The Osservatorio Astronomico di Bologna, one of the twelve Italian
Observatories, is a research structure of the National Institute for Astrophysics (INAF), operating under the supervision of the Ministry for
Education, University and Research (MIUR). The Ministry provides
most of the financial resources which make our activity possible.
This Report gives an overview of our scientific research, covering
a wide range of astrophysical topics, as well as operational and educational activities. OAB astronomers are mostly involved in:
• studies of stellar populations and galactic evolution and their
cosmological implications;
• studies of the structure, evolution and distribution of galaxies,
clusters and AGNs, and their contribution to the cosmological
backgrounds;
• numerical studies in the field of gas hydrodynamics and turbulence simulations;
• management and upgrading of the two telescopes in Loiano (152
and 60 cm) and development of astronomical instruments in the
framework of national and international programs.
• outreach and educational initiatives, through exhibitions, lectures and workshops.
Most of these studies are based on an intensive use of the most
advanced ground-based and space instruments available today at all
wavelengths. They are carried out in collaboration with many international and national institutes and, locally, with the Università
di Bologna, Dipartimento di Astronomia and with two other research
structures of INAF, Istituto di Radioastronomia and Istituto di Astrofisica Spaziale e Fisica Cosmica-Bologna. A large fraction of the staff
is involved in international long-term projects.
The Observatory’s community mourns the loss of our colleague
Federico Delpino, who passed away suddenly in September, and is
greatly missed, personally and professionally.
This report was edited by Roberto Bedogni, Michele Bellazzini,
Alberto Cappi, Antonio De Blasi, Hans de Ruiter, Emiliano Diolaiti,
Silvia Galleti, Monica Marra, Roberto Merighi, Francesco Poppi, Giovanna Stirpe, and Valentina Zitelli.
Flavio Fusi Pecci
(Director)
Osservatorio Astronomico di
Bologna: 2007
• Director: Flavio Fusi Pecci
• Deputy Director: Monica Tosi
Staff
• Scientific Staff: Bardelli, Sandro; Bedogni, Roberto; Bellazzini,
Michele; Bolzonella, Micol; Bragaglia, Angela; Buzzoni, Alberto;
Cacciari, Carla; Cappi, Alberto; Carretta, Eugenio; Ciliegi, Paolo;
Clementini, Gisella; Comastri, Andrea; Delpino, Federico (deceased, Sept. 16); D’ Ercole, Annibale; De Ruiter, Hans; Diolaiti,
Emiliano; Ettori, Stefano; Federici, Luciana; Finelli, Fabio; Fusi
Pecci, Flavio; Gilli, Roberto; Gruppioni, Carlotta; Londrillo,
Pasquale; Meneghetti, Massimo; Merighi, Roberto; Mignoli, Marco; Montegriffo, Paolo; Origlia, Livia; Pancino, Elena; Parmeggiani, Gianluigi; Pozzetti, Lucia; Sancisi, Renzo (retired, June
1); Stanghellini, Letizia; Stirpe, Giovanna Maria; Tosi, Monica;
Zamorani, Giovanni; Zitelli, Valentina; Zucca, Elena
• Computer Centre: Di Luca, Roberto; Gatti, Michele; Lolli, Marco;
Policastro, Rocco
• Laboratory: Bregoli, Giovanni; Ciattaglia, Costantino (retired,
Feb. 1); Innocenti, Giancarlo
• Logistic Support: Ravaglia, Maurizio; Tinti, Franco (retired,
Mar. 1)
• Loiano Staff: Bernabei, Stefano; Bruni, Ivan; De Blasi, Antonio;
Gualandi, Roberto; Muzi, Ivo; Salomoni, Paolo (retired, Aug. 1)
• Administration: Abicca, Renata; Caddeo, Sandra; Diodato, Olga;
Orlandi, Marco; Piccioni, Annalia; Polastri, Tiziana; Venturini,
Adele
• Library: Marra, Monica
• Reception: Caputo, Silvana; Iuso, Annalisa
PhD, fellows and contracts:
• PhD grants funded by INAF–OAB: Cocozza, Gabriele; Contreras
Ramos, Rodrigo; Coppa, Graziano; Lombardi, Gianluca; Lombini, Matteo; Lusso, Elisabetta; Macario, Giulia; Perina, Sibilla.
.
• PhD students with OAB supervisors: Correnti, Matteo; Dalessandro, Emanuele; De Boni, Cristiano; Donnarumma, Annamaria; Fabbri, Sara; Guido, Vincenzo; Marinoni, Silvia; Morandi,
Andrea; Moresco, Michele; Morgan, John; Mucciarelli, Alessio;
Paci, Francesco, Verma, Rashmi.
• Post-grad: Altavilla, Giuseppe; Beccari, Giacomo; Galleti, Silvia; Greco, Claudia; Melioli, Claudio; Montemaggi, Matteo;
Poppi, Francesco; Rossetti, Emanuel.
• Post-doc: Angeretti, Luca; Cignoni, Michele; Fiorentino, Giuliana; Fritz, Jacopo; Gastaldello, Fabio; Gitti, Myriam; Lamareille,
Fabrice; Lanzoni, Barbara; Romano, Donatella.
• Contracts: Ciattaglia, Sante Costantino.
• Collaborations: Braccesi, Alessandro; Sancisi, Renzo.
Contents
1 Stars and Stellar Populations
1.1 The Galaxy . . . . . . . . . . . . . . . . . . . . . . . .
1.1.1 Chemical evolution models . . . . . . . . . . .
1.1.2 Open clusters as tracers of the evolution of the
abundance gradients. . . . . . . . . . . . . . . .
1.1.3 A census of the Galaxy with GAIA . . . . . . .
1.2 Globular Clusters . . . . . . . . . . . . . . . . . . . . .
1.2.1 Observational tests of theoretical stellar models
1.2.2 Mass loss in RGB stars . . . . . . . . . . . . . .
1.2.3 ω Centauri . . . . . . . . . . . . . . . . . . . .
1.2.4 Abundances in Halo Globular Clusters . . . . .
1.2.5 Na-O anti-correlation and HB: a clue to GC formation . . . . . . . . . . . . . . . . . . . . . . .
1.2.6 The Blue Straggler Star Population in Globular
Clusters . . . . . . . . . . . . . . . . . . . . . .
1.2.7 Clusters and field stars in the Galactic bulge:
an infrared view . . . . . . . . . . . . . . . . . .
1.2.8 The Globular Cluster System of the Andromeda
galaxy . . . . . . . . . . . . . . . . . . . . . . .
1.3 Nearby Galaxies . . . . . . . . . . . . . . . . . . . . . .
1.3.1 The Magellanic Clouds: field and cluster populations . . . . . . . . . . . . . . . . . . . . . . .
1.3.2 Super Star Clusters in nearby star forming galaxies
1.3.3 The accreted component of the Galactic Halo:
The Sagittarius Dwarf Spheroidal . . . . . . . .
1.3.4 The accreted component of the Galactic disc:
Canis Major and the Monoceros Ring . . . . .
1.3.5 The remote globular cluster NGC2419 . . . . .
1.3.6 Star formation histories and evolution of resolved
galaxies . . . . . . . . . . . . . . . . . . . . . .
1.4 Synthetic model atmospheres of stars and high-resolution
stellar population synthesis . . . . . . . . . . . . . . . .
1.5 Pulsating variable stars . . . . . . . . . . . . . . . . .
1.5.1 The infrared JHK light curves of RR Lyr . . . .
1.5.2 Variable stars in the remote Galactic globular
cluster NGC 2419 . . . . . . . . . . . . . . . . .
1.5.3 Variable stars in nearby galaxies . . . . . . . .
1.5.4 IZw18: the “Rosetta stone” without a distance
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2 Extragalactic Astronomy and
Cosmology
2.1 Structure and evolution of galaxies . . . . . . . . . . .
2.1.1 Neutral hydrogen studies . . . . . . . . . . . . .
2.2 Active galactic nuclei and star-forming
galaxies . . . . . . . . . . . . . . . . . . . . . . . . . .
2.2.1 Optical studies . . . . . . . . . . . . . . . . . .
2.2.2 Near-IR studies . . . . . . . . . . . . . . . . . .
2.2.3 X-ray studies . . . . . . . . . . . . . . . . . . .
2.3 Surveys and observational cosmology . . . . . . . . . .
2.3.1 The VIMOS/VLT Deep Survey (VVDS) . . . .
2.3.2 The GMASS redshift survey . . . . . . . . . . .
2.3.3 The ELAIS/SWIRE survey . . . . . . . . . . .
2.3.4 The Herschel guaranteed time extragalactic survey: PACS Evolutionary Probe (PEP) . . . . .
2.3.5 The HELLAS2XMM survey . . . . . . . . . . .
2.3.6 The X-ray background in the Chandra and XMM
era . . . . . . . . . . . . . . . . . . . . . . . . .
2.3.7 The COSMOS project . . . . . . . . . . . . . .
2.3.8 Radio surveys . . . . . . . . . . . . . . . . . . .
2.3.9 The SPACE/DUNE/EUCLID project . . . . .
2.3.10 The reionisation of the Universe in quintessence
cosmological models . . . . . . . . . . . . . . .
2.4 Galaxy clusters and large-scale structure . . . . . . . .
2.4.1 Mass Reconstruction in Galaxy Clusters . . . .
2.4.2 Cluster detections using SZ and X-ray . . . . .
2.4.3 Gravitational Lensing . . . . . . . . . . . . . . .
2.4.4 The MUSIC project . . . . . . . . . . . . . . .
2.4.5 Galaxy clusters in the CFHTLS . . . . . . . . .
2.4.6 A search for Relics and Halos in the redshift
range z = 0.2–0.4 . . . . . . . . . . . . . . . . .
2.4.7 Interaction between thermal intra-cluster medium
and relativistic plasma in cooling flow clusters of
galaxies . . . . . . . . . . . . . . . . . . . . . .
2.4.8 Properties of cooling cores in X-ray galaxy clusters
2.4.9 Metal abundance of the Intracluster Medium . .
2.4.10 X-ray properties of high-redshift galaxy clusters
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3 Hydrodynamics
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4 Instruments and Technology
4.1 The GAIA project . . . . . . . . . . . .
4.2 GIANO: An ultra-stable IR spectrometer
4.2.1 GIANO Control Software . . . .
4.2.2 GIANO Data Reduction Software
4.3 Site testing . . . . . . . . . . . . . . . .
4.4 Large Binocular Camera . . . . . . . . .
4.5 LINC-NIRVANA . . . . . . . . . . . . .
4.6 ELT Design Study . . . . . . . . . . . .
4.7 Infrared Test Cameras for LBT . . . . .
4.8 MAORY . . . . . . . . . . . . . . . . . .
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5 Loiano Observing Site
5.1 Operations and use of the 152 cm telescope . . . . . .
5.2 Loiano computer station . . . . . . . . . . . . . . . .
5.3 Applications to the 152 cm telescope . . . . . . . . .
5.4 Loiano cooperation . . . . . . . . . . . . . . . . . . .
5.5 Scientific production involving
the 152 cm Telescope . . . . . . . . . . . . . . . . . .
5.5.1 International refereed pubblications . . . . . .
5.5.2 Published conference proceeding and circulars
5.5.3 Catalogs . . . . . . . . . . . . . . . . . . . . .
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6 Computer Centre and Computer
Network
6.1 General Description . . . . . . . . . . . .
6.2 Computer centre improvements . . . . .
6.3 Improvements in the geographic network
6.3.1 Computer networks . . . . . . . .
6.3.2 Web applications . . . . . . . . .
6.4 Routine activities . . . . . . . . . . . . .
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8 Outreach and Educational Activities
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8.1 Outreach Activities . . . . . . . . . . . . . . . . . . . . 146
8.1.1 Total lunar eclipse, 30 March . . . . . . . . . . 146
8.1.2 Saturn occultation, 22nd of May . . . . . . . . . 147
iii
8.2
8.3
8.1.3 La Scienza in Piazza . . . . . . . . . . . . . . .
8.1.4 Col Favore del Buio . . . . . . . . . . . . . . . .
8.1.5 Il giorno del Sole, 10 June . . . . . . . . . . . .
8.1.6 BoSky 2007 . . . . . . . . . . . . . . . . . . . .
8.1.7 Con il laser tra le stelle . . . . . . . . . . . . . .
8.1.8 Sputnik50: mezzo secolo di era spaziale . . . . .
8.1.9 Il Cielo sulla Valle . . . . . . . . . . . . . . . .
8.1.10 Powers of 10, a journey across the Universe . . .
Educational Activities . . . . . . . . . . . . . . . . . .
8.2.1 Large Binocular Telescope: un binocolo per scoprire i misteri dell’Universo . . . . . . . . . . .
8.2.2 Origine e Evoluzione del Sistema solare . . . . .
8.2.3 What is your weight on other planets? . . . . .
8.2.4 Parco delle Stelle . . . . . . . . . . . . . . . . .
8.2.5 Conferenze alla Specola . . . . . . . . . . . . . .
Educational and Public Outreach . . . . . . . . . . . .
8.3.1 Publications . . . . . . . . . . . . . . . . . . . .
8.3.2 E-articles and web pages . . . . . . . . . . . . .
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9 List of Publications
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10 Observing Campaigns
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11 Positions Held in Working Groups
and Science Policy Committees
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12 Organization of Workshops
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13 Seminars and Visiting Astronomers
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14 “Laurea” thesis
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15 PhD theses
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16 Post-Doctoral, Post-Laurea fellowships and Contracts238
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1
Stars and Stellar Populations
True colour image of the starburst irregular galaxy NGC 4449 as seen
by the Advanced Camera for Survey (ACS) on board of the Hubble
Space Telescope with visible filters (B, V, I and Hα ). 400000 stars
have been resolved in this image. Hot bluish star clusters are scattered
throughout the galaxy. NGC 4449 has been forming stars since several
billion years, but is currently experiencing a star formation event much
stronger than in the past. These studies are performed by INAF-OAB
scientists in collaborations with colleagues from the STScI (Baltimore,
USA). Image Credit: NASA, ESA and A. Aloisi (STScI, ESA).
People involved at OAB:
• Scientific staff: M. Bellazzini, A. Bragaglia, A. Buzzoni, C. Cacciari, E. Carretta, G. Clementini, L. Federici, F. Fusi Pecci, P.
Montegriffo, L. Origlia, E. Pancino, G. Parmeggiani, M. Tosi;
• Technical staff: M. Lolli;
• Fellows and contracts: G. Altavilla, L. Angeretti, G. Beccari, M.
Cignoni, R. Contreras, M. Correnti, G. Fiorentino, S. Galleti, C.
Greco, B. Lanzoni, S. Perina, D. Romano, E. Rossetti;
The study of stellar populations and stellar systems is a very active research field at the OAB since its foundation. The interests range from
the evolution of galaxies to Galactic and extragalactic star clusters,
from chemical evolution to variable stars, covering the whole range of
astronomical wavelengths.
The present description of the activity in the year 2007 has been
organized, as usual, in a few main Sections to provide a very general
overview: 1. The Galaxy, 2. Globular clusters, 3. Nearby Galaxies, 4.
Population Synthesis, 5. Pulsating Variable stars.
1.1
1.1.1
The Galaxy
Chemical evolution models
People involved at OAB: Romano, Tosi.
Models of Galactic chemical evolution can nowadays reproduce the
vast majority of the observed characteristics of our Galaxy. Yet, there
are a number of open questions which require further studies (see
e.g. the review by Tosi, 2007a). Among these are the evolution of
the primordial elements (D, 3 He, 4 He and 7 Li) produced during the
Big Bang, the evolution of the abundance gradients in the Galactic
disc, the anomalous chemical abundances observed in stellar clusters.
Particularly intriguing is the dispersion of local deuterium abundances,
now firmly established thanks to extensive FUSE investigations. Its
origin is lively debated, with some people favouring very localized
infall of external gas, others favouring depletion onto dust grains, and
others a combination of both effects to explain it.
3
In 2007, we completed the study of the D depletion onto dust grains
as the major cause of its observed dispersion, and of the corresponding
implications on what should be taken as the current D abundance
in the solar neighbourhood. We have reached the conclusion that
the representative local value is not the highest measured one, but
D/H = 1.9 × 10−5 , consistent with standard Big Bang and galaxy
evolution scenarios (Steigman, Romano & Tosi 2007).
We have studied the chemical evolution of ω Cen, assuming it to
be both a real globular cluster and the fossil nucleus of an accreted
galaxy (see Sect. 1.2.3).
To better understand the evolution of the Galaxy, we have started
a new project, in collaboration with Luca Ciotti (Astr. Dept., Univ.
of Bologna), to combine our detailed chemical evolution code with a
more appropriate treatment of star and gas dynamics. The difficulty
of this combined approach resides in the very different timescales of
the chemical and dynamical processes, and requires a careful tuning of
the numerical procedure. Once completed, the code will be applied to
the disk of the Milky Way, for which a wealth of observational data are
available to constrain the models. The impact of this new approach
on the predictions for the evolution of the metallicity gradient is likely
to be fundamental.
1.1.2
Open clusters as tracers of the evolution of the abundance gradients.
People involved at OAB: Bragaglia, Carretta, Cignoni, Origlia, Pancino, Tosi
Open clusters (OC’s) are excellent tools to understand the evolution
of the disc of our Galaxy from both the chemical and structural points
of view.
i) We are working on the “Bologna Open Cluster Chemical Evolution” project (BOCCE), intended to probe the chemical evolution of
the Galaxy by studying in more detail the metallicity and age distribution with galactocentric distance. We are homogeneously analysing a
large sample of open clusters at various Galactic locations and covering
a wide range in age and metallicity. Age, distance modulus, reddening
and approximate metallicity are derived from their Colour-Magnitude
Diagrams (CMDs) using the synthetic CMD technique developed by
Tosi at the OAB, and are further constrained by the observed lumi4
Figure 1: CMDs for the two intermediate age open clusters NGC2324
and NGC2477; stars indicated by larger symbols have been observed
with FLAMES@VLT.
nosity functions. Precise and homogeneous elemental abundances are
determined from high resolution spectroscopy.
Our recent completed works on photometry include the very old
clusters Be 32, King 11 (Tosi et al. 2007) and Be 20, Be 66 (Andreuzzi
et al., submitted), all observed with the TNG. Analysis of a few unstudied OCs observed with the Loiano telescope is in progress. During
a two-month period in Santiago (ESO-Chile), Bragaglia has finished
the photometric reduction of To 2 in collaboration with Marconi, and
synthetic CMDs are being built by Tosi. The CFHT data on NGC
6791, the oldest and most metal-rich OC of the MW, are being analyzed, mostly by Cignoni, by means of new evolutionary tracks built
on purpose for the high metallicity ([Fe/H] ≥ 0.4 dex) of the cluster
(in collaboration with S. Degl’Innocenti, P. Prada Moroni - Pisa - and
P. Ventura, M. Castellani - Roma). Finally, an interesting by-product
of the project has been the comparison of the stellar field population
seen in the back/foreground of OCs with models of Galactic populations (thin and thick disk, halo), to determine the scale-length and
scale-height of the thin and thick disks (Cignoni et al. 2008).
Abundances based on high resolution spectra were obtained on our
5
Figure 2: A small region of the FLAMES@VLT spectra obtained for
the stars of the open clusters NGC2324 and NGC2477. The arrows
indicate some of the lines used in the analysis.
metallicity scale for NGC 6791 and NGC 6253, the two most metalrich OCs, with [Fe/H] ' +0.45, based on SARG, FEROS and UVES
spectra (Carretta et al. 2007).
We have also analysed FLAMES@VLT spectroscopic data (in collaboration with Sestito and Randich, INAF-Arcetri Obs.) on NGC
2324, NGC 2477, NGC 2660, NGC 3960, Be 32, Be 20, Be 29, Mel 66,
and Cr 261 (Bragaglia et al. 2008, Sestito et al. 2008).
The web page http://www.bo.astro.it/~angela/bocce.html displays all the OCs in our sample already studied, with the relative
bibliography; the photometry tables can be downloaded from there.
This research is in collaboration with Gratton (INAF-Padova Obs.),
Marconi (ESO), Andreuzzi (INAF-Roma Obs., TNG), Di Fabrizio
(INAF-TNG), Randich, Sestito (INAF-Arcetri Obs.), Kalirai (UCO
Lick).
6
ii) Within the framework of a project aimed at the extension of the
calibration of the Ca-triplet as a metallicity indicator to higher metallicities and younger ages, we have also collected several high-resolution
spectra of open clusters using [email protected] m and UVES@VLT.
Three red clump stars have been observed in each of the following clusters, spanning a range of metallicities and ages, some of which have
never been studied before with high resolution spectroscopy: Cr 110,
M 67, NGC 2099, NGC 2420, NGC 7789, Trumpler 5, Berkeley 39,
M 11, NGC 2141, Berkeley 32, NGC 752 plus the Hyades and Praesepe. All spectra are of a suitable quality (R ∼ 30000 and S/N ∼ 100
per pixel) to also derive accurate abundances of iron peak elements,
α-elements, heavy s-process elements. The data reduction is now complete and the first paper of the series has been recently published
(Carrera et al. 2007). Moreover, the detailed abundance analysis of
the first five open clusters is near completion.
This research is in collaboration with C. Gallart and R. Carrera
(IAC Tenerife, Spain) and R. Zinn (Yale University, USA)
1.1.3
A census of the Galaxy with GAIA
People involved at OAB: Altavilla, Bellazzini, Bragaglia, Cacciari,
Clementini, Diolaiti, Federici, Fusi Pecci, Montegriffo, Pancino, Rossetti
The ESA space project GAIA, planned for launch in 2011, is one of
the ESA Cornerstone missions, and will provide astrometric, photometric and spectroscopic data of very high quality for about 1.3 × 19
stars brighter than V = 20. This will allow to reach an unprecedented
level of information and knowledge on several of the most fundamental astrophysical issues, such as mapping of the Milky Way, stellar
physics (classification and parameterization), Galactic kinematics and
dynamics, study of the resolved stellar populations in the Local Group,
distance scale, age of the Universe, dark matter (potential tracers),
reference frame (quasars, astrometry), planet detection, fundamental
physics, Solar physics, Solar system science.
The paramount importance of this space mission in the study of the
Galaxy and Local Group stellar populations induced many researchers
to get involved in the preparatory work for software, data analysis,
calibrations and related auxiliary ground based observations.
As one of the main tasks of the OAB GAIA-Team in the GAIA
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project is to assemble the Grid of Spectro-Photometric Standard Stars
that will be used to convert all photometry and spectrophotometry
coming from the satellite into an absolute flux scale (in physical units).
Some of the work we are doing will provide general-use products for
the whole astronomical community. In particular we are performing a
main observational campaign to obtain accurate absolute spectrophotometry for ∼ 200 suitably selected standard stars and an ancillary
campaign to check the flux constancy of our candidate standard stars.
Just to give an idea of the amount of work that we are doing, during
2007 we had a total of ∼ 25 observing night at various telescopes and
∼ 30 have been awarded for 2008.
More details on the mission and on the involvement of people at the
OAB in the fields of absolute photometric calibration and of variable
stars are given in the “Instruments and Technology” Section.
1.2
1.2.1
Globular Clusters
Observational tests of theoretical stellar models
People involved at OAB: Beccari, Bellazzini, Cacciari, Fusi Pecci,
Origlia, Pancino.
Stellar evolutionary models are often used to derive relevant properties of globular star clusters (GCs) and galaxies, such as their age and
metal content. The Luminosity Function of the stellar sequences in
the CMDs, from the Main Sequence Turn Off (MS-TO) up to the termination of the Asymptotic Giant Branch (AGB), has been recognized
as the most powerful tool for testing stellar evolutionary models (with
particular regard to the accuracy of the input physics, the reliability
of canonical assumptions, etc.).
A fully fruitful test requires that the observations be a) complete, b)
statistically significant, and c) accurate and adequate for each specific
evolutionary sequence. Point (a) means that virtually all of the stars
in a given area of the cluster are measured down to a given magnitude
level, and that reliable corrections for incompleteness can be applied
below that level. Point (b) means that observations should cover most
of the cluster extension. Point (c) requires infrared observations to
measure the cool Red Giant Branch (RGB) stars and UV observations
to properly study the blue sequences such as the Horizontal Branch
and the Blue Stragglers.
8
Figure 3: Color image of the globular cluster NGC 5466 obtained
from B,V,r observations performed with the blue and red channels of
the Large Binocular Camera (LBC) at the Large Binocular Telescope
(LBT). The image is the result of the stacking of 7 × 60 s exposures in
V and rSDSS plus 7 × 90s exposures in B. The mean seeing measured
on the single images is around 0.7 arcsec. These data are part of a
programme which uses the wide field capabilities of the LBC to the
best advantage, to study the radial distribution of the Blue Straggler
population in a sample of low density globular clusters.
1.2.2
Mass loss in RGB stars
People involved at OAB: Cacciari, Fusi Pecci, Origlia
The IR spectral range is also particularly suitable to study the mass
loss process in giant stars. Mass loss is a crucial parameter in any
stellar evolution modelling. The late evolutionary stages of low- and
intermediate-mass giant stars are strongly influenced by mass loss pro9
cesses. Yet, our lack of empirical estimates on mass loss in low-mass
RGB and AGB stars remains one of the most serious stumbling blocks
for a comprehensive understanding of stellar evolution. A pilot survey of GCs performed with ISOCAM in the 10 µm spectral region
(Origlia et al. 2002) has placed the whole problem into a new perspective that we can explore in deeper detail now, thanks to the powerful
capabilities of the NASA Spitzer Space Telescope. Follow-up Spitzer
observations have been recently obtained, aimed at studying mass loss
along the entire RGB in 17 globular clusters with different metallicities. The data analysis is almost complete. First results on 47 Tuc
have been published in Origlia et al. (2007). About 100 giant stars
show an excess of mid-IR light above that expected from their photospheric emission. This is plausibly due to dust formation in mass
flowing from these stars. This mass loss extends down to the level of
the horizontal branch and increases with luminosity. The mass loss
is episodic, occurring in only a fraction of stars at a given luminosity.
Using a simple model and our observations we derive mass-loss rates
for these stars. Finally, we obtain the first empirical mass-loss formula
calibrated with observations of Population II stars. The dependence
on luminosity of our mass-loss rate is considerably shallower than the
widely used Reimers law.
This work is in collaboration with F. Ferraro, S. Fabbri (Univ.
of Bologna), E. Valenti (ESO, Chile), R.T. Rood (Univ. of Virginia,
USA), R.M. Rich (UCLA, USA).
From a different perspective, the mass loss phenomenon can be
studied in the brightest globular cluster red giant stars, by comparing
the Hα line from high resolution spectra with accurate chromospheric
models. The best match between the observed and calculated profile reveals the presence of a velocity field and hence outflow (mass
loss). This type of analysis, which had previously been done in the
globular cluster NGC 2808, has been extended to a dozen bright red
giant stars in the stellar system Omega Cen, using high S/N high resolution (UVES) spectra taken by E. Pancino. Optical and infrared
photometry from the ground and from space (HST and Spitzer) are
also available, to help derive the physical characteristics of the stars
and of the possible circumstellar envelope. The target stars cover more
than 1 dex in metallicity range and therefore will provide information
on the dependence of the mass-loss on metallicity. This work is in
progress, and is done in collaboration with P. Mauas (Univ. of Buenos
Aires) and S. Fabbri (Univ. of Bologna).
10
1.2.3
ω Centauri
People involved at OAB: Bellazzini, Cacciari, Origlia, Pancino, Romano, Tosi.
ω Centauri is the largest (M = 2.9 × 106 M , Merrit et al. 1997),
brightest cluster in the Galactic Halo, and surely the most peculiar one
in terms of structure, kinematics and stellar contents. It is in fact the
only GC which shows undisputed variations in the chemical content of
its stars. From this point of view, ω Cen could be considered a bridge
system between genuine globulars, which are unable to retain the gas
ejected by their former massive stars, and dwarf galaxies, which are
the least massive self-enriching stellar systems known.
Recent photometric surveys have revealed the presence of several
anomalous sequences in the CMD indicating a complex star formation
and chemical enrichment history for ω Centauri (Pancino et al. 2001).
For instance, Bedin et al. (2004) discovered a bifurcation in the MS of
the cluster. Although the location of the observed blue Main Sequence
(bMS) would suggest a low metallicity, spectroscopic studies indicate
that it has a high metal abundance (Piotto et al. 2005). Hence, it
cannot be associated to the dominant metal poor population. At
present it does not seem possible to obtain a satisfying explanation of
such a feature without assuming large He-abundance variations.
Our group is conducting a long-term multi-approach programme
to investigate the nature and the evolution of this fascinating stellar
system (see Ferraro et al. 2003) and has actively participated in many
of the most exciting discoveries of the latest years (for example, on
the anomalously red and metal-rich RBG and faint SGB), publishing
a number of original results on the structural, photometric, chemical
and kinematic properties of ω Cen (Pancino et al. 2000, 2002, 2003;
Ferraro et al. 2002, 2004; Sollima et al. 2004, 2005a, 2005b; Origlia et
al. 2003; Bellazzini et al. 2004; Ferraro et al. 2006).
In particular, during 2007:
i) Using FLAMES-GIRAFFE observations we derived very accurate radial velocities (to ±0.5 km s−1 ) for 650 RGB stars of ω Cen.
As a first application of this large database we have studied the behaviour of the rotation curve as a function of metallicity, as there were
preliminary claims that the most metal rich stars do not participate in
11
Figure 4: Radial velocity as a function of distance along the major
axis (X) for different sub-populations in the RGB of ω Cen. Upper
panel (blue dots): Metal Poor stars; Middle panel (green dots): Metal
Intermediate stars; Lower panel (red dots): Metal Rich stars. The velocity distribution of the star on the positive (dotted line) and negative
(continuous line) sides of the X axis are compared in the corresponding left panels. The probability that the two wings of the distribution
are drawn from the same parent population – according to a KS test
– are also reported.
the overall rotation of the cluster (Norris et al. 1997). We have found
(Pancino et al. 2007) that in fact RGB stars of any metallicity appear
to share the same rotation pattern (see Fig. 4).
ii) We performed a wide field photometric survey using deep FORS1
12
observations in order to sample the bMS population over a large radial extent. The population was traced over a large field of view up to
26 arcmin from the cluster center. We found that bMS stars are significantly more concentrated toward the cluster centre than the other
“normal” MS stars. The bMS morphology and its position in the
CMD were used to constrain the helium overabundance required to
explain the observed MS morphology. This analysis shows that bMS
stars appear to be more concentrated than the other “normal” cluster
stars (Sollima et al. 2007a; see Fig. 5).
iii) By means of deep FORS1/VLT and ACS/Hubble Space Telescope observations of a wide area in ω Cen we measured the luminosity
function of main-sequence stars down to R = 22.6 and F814W = 24.5.
The luminosity functions obtained were converted into mass functions
and compared with analytical initial mass functions (IMFs) available
in the literature. The mass function obtained, reaching M ∼ 0.15M ,
can be well reproduced by a broken power law with indices x = −2.3
for M > 0.5M and x = −0.8 for M < 0.5M . Since the stellar
populations of ω Cen have been proved to be actually unaffected by
dynamical evolution processes, the mass function measured in this
stellar system should represent the best approximation of the IMF of
a star cluster. The comparison with the MF measured in other Galactic globular clusters suggests that there could be possible primordial
differences in the slope of the low-mass end of their MF (Sollima et
al. 2007b).
iv) Numerical models were computed for the chemical evolution of
ω Cen (see Sect. 1.1.1). In Romano et al. (2007), we have examined
both the hypotheses that ω Cen be a real globular cluster or the relic
nucleus of an accreted dwarf Speroidal galaxy, disrupted during the
capture by the Milky Way. We have found that only in the latter
scenario the models are able to reproduce the observed chemical properties of the system. What remains unclear is how ω Cen managed
to get the amazingly high helium abundance of Y = 0.38 suggested
in the literature to explain the observed secondary blue main-sequence.
In summary, the Bologna key project on ω Cen is fully active, with
a wealth of data being reduced and new observations being continuously performed. The work is in collaboration with scientists of several
international institutes, among which F. Ferraro (Astr. Dept., Univ. of
13
Figure 5: Tracing the double Main Sequence of ω Cen through the
whole cluster. From Sollima et al. (2007b).
Bologna), O. Straniero (INAF-Teramo Obs.), M. Catelan (Univ. Cat.
Chile), J. Borissova (ESO), D. Minniti (Univ. Cat. Chile), H. Smith
(MSU), and R. T. Rood (UVA).
1.2.4
Abundances in Halo Globular Clusters
People involved at OAB: Bragaglia, Carretta, Pancino.
Thanks to the new efficient optical and IR spectrographs with high
resolution and multi-object capabilities mounted on 4m and 10m-class
telescopes, high quality spectra can be obtained for tens to hundreds of
stars in each GC in very reasonable exposure times. Detailed and precise chemical abundances of many key elements (Fe, light, α, proton14
capture and neutron-capture elements) can now be measured for stars
in Galactic GCs from the RGB tip to the MS Turn-Off. This field has
triggered an increasing interest from many researchers at the OAB
and we illustrate below the status of the various projects.
1.2.5
Na-O anti-correlation and HB: a clue to GC formation
People involved at OAB: Bragaglia, Carretta, Pancino.
In recent years, many studies found several clear exceptions to the
classical view of Galactic Globular Clusters as purely mono-metallic
populations. The only elements showing very homogeneous abundances in GC stars are those produced by explosions of Supernovae,
in particular iron peak elements and, in some cases, α elements.
However, large star-to-star intrinsic variations for abundances of
the lightest elements (from Li and C to Mg and Al) are known to
exist in every GGC examined so far. Part of these chemical anomalies
(those related to Li, C, N, and their isotopes) share the same behaviour
of field stars of similar metallicity, but heavier nuclei (noticeably Na,
O, Mg, Al) present in GGC a peculiar pattern not seen in halo field
analogs and still not well explained.
The emerging picture is that globular clusters are not a true example of Simple Stellar Population, and that their early evolution was
probably not very simple. This is indicated by stars that populate
side-by-side the same evolutionary locus from the late RGB down to
the unevolved main sequence and show very different surface abundances of light elements (C, N, O, Na, Al).
The observed variations observed for Li, C and N are partly explained by the normal evolution of low mass giants, where changes in
surface abundances are due to the standard first dredge-up after the
Main Sequence phase, plus a second mixing mechanism that occurs
when the advancing H-burning shell crosses the chemical discontinuity left behind by the retreating convective envelope (the RGB-bump
point). Both mixing episodes bring to the surface products of an incomplete CNO-cycle, lowering the Li, C abundances and the isotopic
ratio of 12 C/13 C and increasing the N abundance (see Gratton, Sneden
and Carretta 2004 for a recent review). However, variations of heavier
elements cannot be explained with this scenario.
The star-to-star anti-correlation between the O and Na abundances
15
(see Gratton, Sneden, Carretta 2004) is the main sign of the (unexpected) presence of material processed through the complete CNO
cycle in GC stars, most likely from thermally pulsing intermediatemass AGB (IM-AGB) stars of an early stellar generation, undergoing
hot bottom burning and/or fast rotating massive stars losing material at the end of their main sequence phase. The age difference between the two populations (a few 108 yr) is too small to be directly
detectable as different Turn-Offs (TO’s), but may be unveiled by a
careful abundance analysis of the relics of now-extinct first generation
stars, whose nucleosynthetic yields are possibly incorporated in the
present observed GC stars.
We have observed about 19 Galactic GCs selected to span the
whole range of different physical parameters (metallicity, concentration, density, HB morphology, mass, etc.); in more than 70 hours
at VLT-UT2 with FLAMES we collected about 100 high resolution
spectra of RGB stars in each GC. Analysing this large and homogeneous dataset, we plan to answer fundamental questions such as: (i)
Were/Are GC stars really born in a single “instantaneous” burst? (ii)
How do abundance anomalies within each individual GC relate to the
formation and early evolution of the GC itself and of each individual
cluster member?
Our analysis is now complete, and we are mining the huge amount
of data we have at hand (see Fig. 6). The main first results are:
a) the extent of the Na-O anticorrelation (as quantified by the
interquartile range of the [O/Na] ratio, IQR[O/Na], see Carretta et
al. 2007) is strictly related to the very blue (and hotter) end of the
horizontal branch (HB), with a high level of statistical significance;
b) very extended anticorrelations are only observed in massive
globular clusters; however, a large observed mass alone does not guarantee the development of a strong anticorrelation. An example of this
rule is 47 Tuc, a massive cluster with a moderate Na-O anticorrelation;
c) if we take into account the orbital motions of clusters in the
Galaxy, we derive a very good correlation between the IQR[O/Na]
and a bivariate quantity including both clusters’ mass and orbital
parameters: extended anticorrelations require large mass and largesized, eccentric, long orbits, taking the GCs far away from the central
regions of the Galaxy, where the GCs are more affected by bulge/disk
shocks;
d) in all GCs we found a population of stars of primordial composition similar to field stars of similar metallicity [Fe/H];
16
Figure 6: Na-O anticorrelations found in 19 GCs observed with
FLAMES@VLT (red dots are measures and blue symbols are upper
limits). Notice that this anticorrelation was found in all GCs studied
so far, but with different extensions.
e) in all GCs the bulk of the stars (50–70%) belongs to an intermediate component, a second generation population with modified, but
not extreme, composition;
f) finally, an extremely oxygen-poor component of second generation stars is observed in a few clusters, preferentially massive ones
(but not in all clusters, as said above).
This work is in collaboration with Gratton, Lucatello, Desidera,
Momany (INAF-Padova Obs.), Piotto (Univ. of Padova), D’Antona
(INAF-Roma Obs.), Leone, Catanzaro (INAF-Catania Obs.), Cassisi
(INAF-Teramo Obs.), François (Obs. Paris), Recio-Blanco (Obs. Nice)
and many more. This project received funding by INAF-PRIN 2005
and by the PRIN-MUR 2007.
17
1.2.6
The Blue Straggler Star Population in Globular Clusters
People involved at OAB: Beccari, Bellazzini, Fusi Pecci, Lanzoni
It is now generally accepted that Blue Straggler Stars (BSS) are more
massive than the normal MS stars, and are the result of mass transfer
between binary companions (MT-BSS), possibly up to the coalescence
of the binary system, or merger of two single or binary stars driven by
stellar collisions (COL-BSS).
To finally unveil their nature and their formation mechanisms, we
are using several different and complementary approaches, including
high-resolution and multi-wavelength photometric observations, deep
high-resolution spectroscopy, and Monte-Carlo dynamical simulations.
We performed high-resolution and wide-field photometry in the
ultraviolet and optical bands to study the radial distribution of BSS
within their host globular clusters (GCs). While normal cluster populations (such as red giant and horizontal branch stars) do not show
any spatial segregation, the radial distribution of BSS was found to be
bimodal (i.e., highly peaked in the centre, decreasing at intermediate
radii, and rising again outward) in several GCs (such as M3, 47 Tucanae, NGC 6752, M5, M55). Suitable dynamical simulations were
used to show that such a bimodality can be explained only if a sizable
fraction (≥ 20–40%) of the cluster BSS population is made of MT-BSS,
responsible for the external rising branch of the distribution, with the
balance being COL-BSS, mainly contributing to the central peak. This
suggests that both formation channels are simultaneously at work in
GCs. Once a larger sample of GCs will have been studied with such
an approach, the detailed comparison between the BSS population
properties, and the cluster structural and dynamical characteristics
will allow us to shed light on the complex interplay between stellar
evolution and dynamical processes in dense stellar systems (Lanzoni
et al. 2007a,b,c; Mapelli et al. 2006). This line of research has received
a remarkable boost in the last year thanks to the availability of the
wide field camera LBC on the part-Italian 2 × 8 m LBT telescope.
This instrument is ideal to obtain the very efficient multi-wavelength
radial coverage of GCs required for the detailed analyses of the BSS
populations which we are performing. In particular we have completed
a thorough study of M53 (Beccari et al. 2008), and the final analysis
18
Figure 7: B,V,r Color-Magnitude Diagram of NGC5466 obtained with
the LCB@LBT. Note the very clean sequence of BSS at B − r < 0.5
and 18.5 < r < 20.0.
of an exceptionally good data-set on the cluster NGC5466 (see Fig. 7)
is currently ongoing.
This work is in collaboration with Ferraro, Dalessandro, Sollima
(Univ. Bologna), Rood, Schiavon (Univ. of Virginia, USA), Mapelli
(Zurich Univ., Switzerland), Sigurdsson (Pennsylvania State Univ.,
USA), Sanna (Univ. Roma Tor Vergata), Sills (McMaster Univ., Canada),
Manicini (Univ. Firenze).
19
1.2.7
Clusters and field stars in the Galactic bulge: an infrared view
People involved at OAB: Origlia.
Bulge GCs are a fundamental stellar population of our Galaxy and it is
most interesting to compare their detailed chemical abundances with
the Galactic halo populations (McWilliam & Rich 1994). For most of
the bulge population, foreground extinction is so large as to preclude
any photometric and spectroscopic optical study. In the last few years
we have undertaken a long-term project devoted to study the Galactic
bulge in the infrared, to minimize the effects of extinction.
Using the SOFI medium-resolution imager/spectrograph at the
ESO NTT telescope and the NIRSPEC high-resolution echelle spectrograph at Keck II, we are performing a systematic survey of M giant
stars in bulge globular clusters as well as in several fields at different
distances from the Galactic centre. From a detailed analysis of the
IR colour-magnitude diagrams we construct a catalogue of 24 Galactic globular clusters toward the bulge (Valenti, Ferraro, Origlia 2007).
The compilation includes measurements of the cluster reddening, distance, photometric metallicity, horizontal branch/red clump, and red
giant branch morphological (e.g., mean ridgelines) and evolutionary
(e.g., bump and tip) features.
From the analysis of the high resolution spectra, we measured several single roto-vibrational OH lines and CO bandheads to derive accurate oxygen and carbon abundances. Other metal abundances can
be derived from the atomic lines of Fe I, Mg I, Si I, Ti I, Ca I and
Al I. Abundance analysis is performed by using full spectral synthesis
techniques and equivalent width measurements of representative lines.
In the past years Results have been already published for 8 GCs
(Origlia, Rich & Castro 2002, Origlia & Rich 2004, Origlia et al. 2005,
Origlia, Valenti & Rich 2005), and for the Baade window (Rich &
Origlia 2005). This year we published the results for a field at 150
pc from the Galactic centre (Rich, Origlia, Valenti 2007) and for two
additional massive clusters (Origlia, Valenti & Rich 2008), namely
NGC6440 and NGC6441. We find an overall [α/Fe] enhancement up
to about solar metallicities, both in the cluster and field populations,
that is consistent with a scenario in which the bulge formed early,
with rapid enrichment. We also developed a model of the chemical
20
evolution of the Galactic bulge (Ballero et al. 2007) in the context of
an inside-out scenario for the formation of the Milky Way. The model
contains updated stellar yields from massive stars and its predictions
have been compared with new observations of chemical abundance
ratios and metallicity distributions in order to provide constraints on
the formation and evolution of the bulge.
We started a survey of Galactic bulge clusters by using adaptive
optics imaging in the near IR with NAOS/CONICA at the VLT. The
goal of this project is to obtain deep photometry in the J and H bands
well below the Turn-Off region for an accurate estimate of the absolute
and relative ages of the clusters. First results on NGC6440 have been
recently submitted for publication in ApJL (Origlia et al. 2008).
This work is in collaboration with F. Ferraro, (Univ. of Bologna),
E. Valenti (ESO, Chile), R.M. Rich (UCLA, USA), F. Matteucci and
S. Ballero (Univ. of Trieste).
1.2.8
The Globular Cluster System of the Andromeda galaxy
People involved at OAB: Bellazzini, Buzzoni, Cacciari, Federici, Fusi
Pecci, Parmeggiani, Perina, Galleti.
The M31 globular cluster system is the largest found in the Local
Group, sufficiently close to allow detailed observations and little affected by reddening, at least for a large outer sub-set. Since the intrinsic depth of the spheroid is small compared to the distance to M31, in
the study of the basic properties and comparisons one can remove the
degeneracies introduced by the uncertain knowledge of the individual
distances. In practice, M31 offers the unique opportunity of studying
in very good detail the GC system of a spiral galaxy that is similar to
the MW, without some of the limitations that affect the Galactic GC
system.
The study of the M31 GC system is a long-term project started at
the OAB in the early 1980s and recently revived by new observational
programmes (Galleti et al. 2004, 2005, 2006a,b, 2007; Federici et al.
2007; Fusi Pecci et al. 2005). The OAB M31 team, in collaboration
with scientists of other Italian and foreign institutions, is carrying out
the exhaustive systematic census of M31 GC candidates using both
photometry (from the UV to the IR bands) and spectroscopy. The
purpose of the project is to use the globular cluster system to improve
our knowledge of the mass, dynamics and chemical evolution of the
21
Figure 8: Stamp images (8 × 8 arcsec2 ) of eighteen candidate young
clusters observed within our HST-WFPC2 survey. The pictures are
the central region of the PC images in F450W.
parent galaxy.
The main ongoing programmes are summarized in the following:
i) Our continuously updated on-line catalogue (Revised Bologna
Catalogue of M31 globular clusters–RBC, Galleti et al. 2004) has become the most complete and widely used reference in the field. The
RBC web site (http://www.bo.astro.it/M31/) scores more than 600
contacts per year from all over the world.
22
ii) The clusters located at large projected distances from the centre of the galaxy are particularly interesting because they provide the
maximum “leverage” to constrain the galaxy mass profile at large
radii, where kinematical information is missing even from the H I
surveys. In this framework, we have started a programme to search
for new clusters at projected galactocentric distances larger than 40
kpc. Candidates are selected from the 2MASS Extended Source Catalog (XSC) and then followed up with low resolution spectroscopy
with Dolores@TNG and BFOSC@Loiano, as described in Galleti et
al. (2005, 2007). At present we have identified five new remote and
bright clusters (Galleti et al. 2005, 2007), one of which has been studied in great detail with HST (Galleti et al 2006a, Federici et al. 2007;
see also Sect. 1.5.5). Observing time was obtained at the TNG and at
the Loiano telescope to complete the survey.
iii) The presence in M31 of stellar systems similar to the MW
globulars in luminosity and shape, but with integrated colours significantly bluer than the bluest MW counterparts, is well known and
documented. As a follow-up of our recent study (Fusi Pecci et al. 2005)
on these young and bright clusters, a large HST survey in collaboration with scientists of foreign institutions (HST cycle 15, PI Cohen)
is in progress, to check the real nature of these objects that seem to
have no counterpart in the Milky Way. Twenty one candidates were
imaged with WFPC2. The data reduction is now complete and the
analysis of the CMDs is ongoing (see Fig. 8); a first paper has been
submitted, presenting the data reduction strategy to be applied to the
whole survey and the analysis.
iv) In a previous study of the CMDs obtained from WFPC2/HST
observations for 19 GCs in M31 we showed that the M31 globular clusters are similar to the MW globulars, with an indication of the presence
of an intermediate age cluster population and of the occurrence of the
second-parameter effect (Rich et al. 2005). To verify and enforce that
result, in 2007 we performed the same analysis on a further sample
of M31 GCs, using HST/ACS archive data. We derived the CMDs
of 24 objects classified as GC in the Revised Bologna Catalogue. Of
these, 2 turned out to be stars and 11 had very noisy data (due to
field contamination) and no reliable CMD could be derived. For the
remaining 11 GCs the CMDs were good enough to obtain estimates
of metallicity, reddening and distance for the individual objects. This
brings to 30 the total number of M31 GCs with usable CMD. A paper
is in preparation.
23
This work is in collaboration with M. Rich (Caltech) and C. Corsi
(INAF-OAR). The PhD research project of Sibilla Perina is aimed at
the study of star clusters in M31, particularly focussed on the class of
young and luminous clusters identified by Fusi Pecci et al. (2005).
1.3
1.3.1
Nearby Galaxies
The Magellanic Clouds: field and cluster populations
People involved at OAB: Angeretti, Carretta, Cignoni, Fusi Pecci,
Origlia, Tosi.
At OAB several studies are being performed on the Magellanic Clouds,
using both their clusters and field populations to trace galaxy and
stellar evolution.
The spectral evolution of a Simple Stellar Population (SSP) and its
most evident colour glitches are ideal clocks for dating primeval galaxies and deriving a suitable, empirical relation between look-back time
and redshift. The empirical calibration of the clock which determines
the spectral evolution of SSPs and its readability are the primary goals
of our project. The globular cluster system of the Magellanic Clouds
(MC) provides a unique opportunity to investigate the integrated spectrophotometric behavior of stellar populations as a function of both
age and chemical composition. We are tackling these major astrophysical objectives by means of a coordinated spectrophotometric survey
on a representative sample of MC clusters, aimed at determining with
great accuracy and in a homogeneous way their age, metallicity and
overall integrated spectral properties.
i) During a number of successful observing runs with SOFI@NTT,
our group secured high quality J, H, K photometry of 20 LMC clusters spanning the age range between 50 Myr and a few Gyr. We have
also obtained mid-IR photometry during Cycle 1 observations with
the NASA Spitzer Space Telescope. Populous and complete near-IR
CMDs covering the entire RGB extension have been obtained. The
mid-IR data are under analysis. The high quality and homogeneity of
such an IR database provided the most accurate empirical determination of the occurrence of the so-called AGB and RGB phase transitions. The results for the intermediate age clusters in the LMC have
been published in Ferraro et al. (2004), Mucciarelli et al. (2006) and
24
Figure 9: Color-Magnitude Diagram of the LMC intermediate-age
globular cluster NGC 1978 obtained with ACS@HST (Mucciarelli et
al. 2007, AJ, 133, 2053).
demonstrated that the full development of the RGB occurs at ages
around 700 Myr and is a relatively fast event (duration ∼ 300 Myr).
Recently, we published (Mucciarelli et al. 2008) the results for 4 intermediate age clusters in the SMC. We find that in the 5–7 Gyr
old clusters AGB stars account for 6% of the total light in the Ksband, Carbon stars are lacking and RGB stars account for 45% of
the total bolometric luminosity. These empirical findings are in good
agreement with the theoretical predictions. Finally, we derived photometric metallicities computed by using the properties of the RGB and
finding an iron content of [Fe/H] = −1.18, −1.08, −0.99 and −0.96
dex for NGC 339, 361, 416 and 419 respectively.
25
ii) Accurate ages for individual clusters based on deep ACS@HST
photometry and updated models of stellar evolution have been also obtained. Results for 2 intermediate-age clusters, namely NGC1978 and
NGC 1783, were published in Mucciarelli et al. (2007); Mucciarelli,
Origlia & Ferraro (2007). We find ages of 1.4 and 1.9 Gyr respectively, with an overall uncertainty of 0.1 Gyr. The correct reading
of the age from a SSP requires the accurate knowledge of the global
metallicity. This major piece of information, namely a self-consistent
metallicity scale and a detailed description of the abundance patterns
of MC clusters, is still lacking. In order to fill such a gap, we started
a project to provide a homogeneous metallicity scale based on high
resolution optical (using UVES+GIRAFFE at the ESO-VLT) and IR
spectroscopy (using CRIRES@ESO-VLT) for a representative sample
of MC clusters.
The detailed iron abundance analysis of 11 giant stars in NGC
1978, a massive, intermediate-age stellar cluster, characterized by a
high ellipticity and suspected to have a metallicity spread, was published in Ferraro et al. (2006). Recently, we published the chemical
abundances of light odd-Z, α, iron-peak, and neutron-capture elements
for 27 red giant stars in NGC 1651, 1783, 1978, and 2173. All the analyzed abundance patterns behave similarly in the four clusters and
also show negligible star-to-star scatter within each cluster. We find
[Fe/H] = −0.30 ± 0.03, −0.35 ± 0.02, −0.38 ± 0.02, and −0.51 ± 0.03
dex for NGC 1651, 1783, 1978, and 2173, respectively. The measurement of light odd-Z nuclei gives slightly subsolar [Na/Fe] and a
more significant [Al/Fe] depletion (∼ −0.50 dex). The [α/Fe] abundance ratios are nearly solar, while the iron-peak elements well trace
those of the iron. S-process elements behave in a peculiar way: light
s-elements give subsolar [Y/Fe] and [Zr/Fe] abundance ratios, while
heavy s-elements give enhanced [Ba/Fe], [La/Fe], and [Nd/Fe] with
respect to the solar values. Also, the [Eu/Fe] abundance ratio turns
out to be enhanced (∼ 0.4 dex).
This research is in collaboration with F. Ferraro, A. Mucciarelli
(Univ. of Bologna), V. Testa (INAF-Roma Obs.), C. Maraston (Univ.
of Portsmouth, UK)
iii) As major players in the international collaboration aimed at
studying the evolution of the SMC as a prototype of dwarf irregular
galaxies, in 2007 we completed the analysis of our ACS@HST data of 7
old clusters in the SMC (Glatt et al. 2008a and Glatt et al. 2008b) and
continued (Tosi et al. 2008) the photometry of 6 fields in key galactic
26
locations (three ACS fields in the SMC central region, two in the wing
toward the LMC, and one in the SMC halo).
Within the same collaboration, we also continued our analysis of
the HST/ACS fields around the young clusters SMC NGC 346 and
NGC 602. Evidence of triggered star formation seems to exist in both
fields (Carlson et al. 2007, Sabbi et al. 2007). In spite of their very
different locations (NGC 346 is close to the SMC centre, while NGC
602 is at its outskirts, in the SMC wing), both regions contain not
only objects (MS and pre-MS stars) as young as 3 Myr, but also a
conspicuous population about 4.5 Gyr old, corresponding to the bulk
population of the SMC field. We have derived the present-day mass
function of NGC 346 from its most massive stars (60 M ) down to 0.6
M and described the uncertainties and problems affecting the derivation of the Initial Mass Function (Sabbi et al. 2008). We have derived
the star formation history of the NGC 602 field, using the synthetic
CMD method with two independent approaches, and found that the
activity in the young cluster is extremely recent, but overimposed on a
rather continuous, although much lower, level of star formation typical
of the whole SMC (Cignoni et al. 2008).
This collaboration includes, among others, A. Nota, E. Sabbi,
M. Sirianni (STScI), J. Gallagher (Univ. of Wisconsin, USA) and E.
Grebel (ARI, Heidelberg). This research was partially supported by
PRIN-INAF05 CRA 1.06.08.16.
1.3.2
Super Star Clusters in nearby star forming galaxies
People involved at OAB: Origlia.
Integrated high-dispersion spectroscopy of massive star clusters is a
promising method for abundance analysis in extragalactic young stellar populations. Using the NIRSPEC spectrograph at Keck II, we
have obtained infrared spectra of a few young and luminous luminous
super-star clusters (SSCs) in nearby galaxies. First results on the
SSC in the spiral galaxy NGC 6946 were published in Larsen et al.
(2006). This year we published the results for the massive star cluster ‘B’ in the nearby dwarf irregular galaxy NGC 1569 (Larsen et al.
2008). From spectral synthesis and equivalent width measurements,
we obtain abundances and abundance patterns. We derived [Fe/H] =
−0.63 ± 0.08, a supersolar [α/Fe] abundance ratio of +0.31 ± 0.09,
and an O abundance of [O/H] = −0.29 ± 0.07. We also measured a
27
low 12 C/13 C ≈ 5 ± 1 isotopic ratio. Using archival imaging from the
Advanced Camera for Surveys onboard the Hubble Space Telescope
(HST), we construct a Color Magnitude Diagram for the cluster in
which we identify about 60 red supergiant (RSG) stars, consistent with
the strong RSG features seen in the H-band spectrum. The mean effective temperature of these RSGs, derived from their observed colours
and weighted by their estimated H-band luminosities, is 3790 K, in excellent agreement with our spectroscopic estimate of Teff = 3800 ± 200
K. From the CMD, we derive an age of 15–25 Myr, slightly older than
previous estimates based on integrated broad-band colours. We derive
a radial velocity of 78 ± 3 km s−1 and a velocity dispersion of 9.6 ± 0.3
km s−1 . In combination with an estimate of the half-light radius of
0.20 ± 0.05 arcsec from the HST data, this leads to a dynamical mass
of (4.4 ± 1.1) × 105 M . The dynamical mass agrees very well with
the mass predicted by simple stellar population models for a cluster of
this age and luminosity, assuming a normal stellar initial mass function. The cluster core radius appears smaller at longer wavelengths,
as previously found in other extragalactic young star clusters.
1.3.3
The accreted component of the Galactic Halo: The
Sagittarius Dwarf Spheroidal
People involved at OAB: Bellazzini, Correnti.
There is now a growing body of observational evidence in favour of
an inhomogeneous halo, where the traces of the slow building up by
hierarchical merging of sub-units should be still observable (Bell et
al. 2007). The Sagittarius dwarf Spheroidal Galaxy (Sgr dSph; Ibata
et al. 1994) is the most evident and striking example of a real time
accretion event occurring in the Galactic Halo. The main body of Sgr
dSph orbits well within the Galactic spheroid (RGC ' 16 kpc) and
shows clear signs of being disrupted by the Galactic tidal field. Thus,
the Sgr dSph is (and has been) one of the major contributors to the
stellar content of the whole Galactic Halo.
Our research on the Sagittarius galaxy and its Stream is continuously ongoing with a constant production of new published results (Monaco et al. 2002, 2003, 2004, 2005a,b, 2007; Bellazzini et al.
1999a,b, 2003a,b, 2006a,b; Correnti et al. 2007). A high-resolution
spectroscopy survey of stars in the various branches of the Sgr Stream
is also ongoing and is providing the first interesting results (Monaco
28
Figure 10: N-body simulation of the orbital decay by dynamical friction of a model of the globular cluster M54 within a model of its host
galaxy, Sgr dSph. Sgr is modelled with 105 particles (not shown in
the plot to display as clearly as possible the evolution of the cluster)
distributed as a NFW halo with M = 4.2 × 108 M . M54 is modelled with 104 particles, distributed as an equilibrium King model of
M = 1.5 × 106 M . See Bellazzini et al. 2008, for further details. Note
that the cluster is driven to the very center of the galaxy – from its
initial orbit – in t ' 1.5 Gyr.
29
et al. 2007).
A huge kinematical study of the nucleus of Sgr and of the giant
cluster M54 that resides in the nucleus itself is also in progress. This
includes the analysis of the radial velocity for 1152 stars observed
with VLT-FLAMES and Keck-DEIMOS, as well as a suite of N-body
simulations aimed at verifying the hypothesis that M54 could have
been driven to its present position by dynamical friction (Bellazzini et
al. 2008; see Fig. 10).
M. Correnti, within his PhD project, is using SDSS data to take
accurate measures of the northern branch of the Sgr tidal Stream.
Preliminary results of this study were presented in Correnti et al.
(2007, 2008).
This research is in collaboration with Ferraro (Univ. of Bologna),
L. Monaco (ESO), R. Ibata (Obs. Strasbourg), N. Martin (MPI), M.
Irwin (Cambridge), D. Mackey (Edinburgh), and S.Chapman (Caltech). Matteo Correnti’s PhD project is focussed on the study of
galactic relics, including Sgr. This research was partly supported by
INAF-PRIN05 grant n. CRA 1.06.08.02 (PI: M. Bellazzini).
1.3.4
The accreted component of the Galactic disc: Canis
Major and the Monoceros Ring
People involved at OAB: Bellazzini.
The study of the nature and of the physical characteristics of the large
remnant discovered by Martin et al. (2004, see also Bellazzini et al.
2004) and of the possibly associated Monoceros Ring is in progress
on several fronts. A large kinematic survey is providing the basic
constraints for the construction of a realistic model of the disruption
of CMa (Martin et al. 2005, 2006), while the structure of the remnant
has been traced with Red Clump stars in Bellazzini et al. (2006c). An
extension of this analysis to the whole CMa/Monoceros system using
Main Sequence stars as tracers is in progress and is expected to provide
clear indications on the actual nature of this huge substructure in the
outer Galactic Disc (Conn et al. 2007, 2008).
This research is in collaboration with: R. Ibata, N. Martin (Strasbourg Obs.), G. Lewis, B. Conn (Sidney Univ.), M.J. Irwin (Cambridge, UK). This research is partly supported by the INAF-PRIN05
grant n. CRA 1.06.08.02.
30
1.3.5
The remote globular cluster NGC2419
People involved at OAB: Bellazzini, Correnti.
NGC2419 stands out as one of the most interesting and less known
objects of the whole halo of the Milky Way. This metal-poor ([Fe/H] =
−2.1), very bright cluster (MV = −9.4) resides in the remotest fringes
of the halo (RGC = 91.5 kpc) where the relics of past merging events
are expected to be most easily preserved (Bullock & Johnston, 2004,
ASPCS, 327, 80). Indeed there are claims of the detection of tidal
debris in its surroundings (Newberg et al., 2003, ApJ, 596, L191).
Its half-light radius is significantly larger than that of ordinary GCs of
similar luminosity (by a factor of > 3), being more similar to the nuclei
of dwarf elliptical galaxies. Also its total luminosity is more than one
order of magnitude larger than GCs with similar velocity dispersion
(σ = 2.7 ± 0.8 km −1 ). As a first step of a project aimed at a thorough
study of this mysterious stellar system, we have derived a new Surface
Brightness profile based on HST and ground-based data that fully
confirms – with state of the art independent data – the anomalous
structural parameters of the cluster (Bellazzini 2007). Dalessandro et
al. (2008) have also shown that there is no sign of star segregation
by mass in this cluster, thus supporting the idea that – at odds with
classical globulars – NGC2419 is not relaxed by two-body encounters
but should be considered as a non-collisional system
1.3.6
Star formation histories and evolution of resolved galaxies
People involved at OAB: Angeretti, Cignoni, Romano, Tosi.
We are applying the method developed at the Bologna Observatory to
infer the star formation history (SFH) from the CMDs of their resolved
stellar populations to a number of galaxies of different morphological
type, mass and metallicity. In 2007 we worked at the derivation of the
SFHs of metal-poor late-type dwarf galaxies located both inside and
outside the Local Group.
Late-type dwarf galaxies are ideal systems to understand galaxy
evolution, because their proximity allows one to examine in detail important issues, such as the occurrence of galactic winds, the chemical
enrichment of the interstellar and intergalactic media, the photomet-
31
Figure 11: Deep Color Magnitude Diagram of NGC 2419 from drizzled
HST-ACS/WFC images (Dalessandro et al. 2008).
ric evolution of galaxies. Their low level of evolution, as implied by
the low metallicity and the high gas content, makes these systems the
most similar to primeval galaxies and, therefore, the most useful to
infer the primordial galaxy conditions. Furthermore, they have been
suggested to represent the building blocks of larger galaxies. Understanding how late-type dwarfs evolve and what were their conditions
at early epochs is therefore crucial also for cosmological purposes. It is
fundamental to derive the SFH in a number of representative systems
of the major morphological sub-classes: blue compact galaxies, dwarf
irregulars, giant irregulars (see e.g. the review by Tosi 2007b).
To this aim we have undertaken a long term project to study,
from deep and accurate HST photometric data, the stellar populations
of dwarfs of particular interest (“normal” ones, the most metal-poor
32
ones, the most active ones, those with evidence of galactic winds). In
2007 we concentrated on the most metal poor one (IZw18) and on the
most active one (NGC 4449) with proprietary ACS@HST data (PI of
both proposals A. Aloisi).
All the dwarf galaxies with appropriate photometry show a prominent population of red giant stars, and are therefore actively forming
stars since at least several Gyrs, but some authors still claimed that the
most metal poor dwarfs are genuinely young systems: among these,
IZw18, which is the most metal poor (1/30–1/50 of solar, depending
on the adopted solar metallicity) star forming galaxy ever discovered
and is therefore a key object in cosmological studies. In particular,
Izotov & Thuan (2004) claimed that IZw18 does not contain red giants
and, as a consequence, that this galaxy started forming stars only less
than 0.5 Gyr ago. However, by re-analysing their own ACS@HST data
with more refined methods, we have shown that an RGB is very likely
to exist in IZw18, indicating an age of at least 2 Gyr (Tosi et al. 2007).
Moreover, our own ACS@HST photometry, performed with appropriate time series photometry to find IZw18’s Cepheids has allowed us
both to accurately estimate the distance from the period-luminosity
relation and to derive the deepest possible CMD. We confirm the existence of the RGB, derive the galaxy distance from the RGB tip, the
carbon stars and the Cepheids (see Sect. 1.5.4) and find a value of 18.2
Mpc from all three independent methods (Aloisi et al. 2007a,b). This
high distance, larger than previously estimated, is the reason why red
giants were so difficult to identify until now. These results were the
subject of a joint press release (10 Oct. 2007) by NASA/ESA/INAF.
We also observed the whole body of NGC 4449 with ACS@HST,
and derived the CMDs of the various sub-regions from accurate data
analysis (Annibali et al. 2008). Again, the SFH of this system will be
derived with our synthetic CMD method.
To allow for a more rapid but reliable derivation of the SFHs of
many different galaxy regions, we modified our synthetic CMD procedure, updating it with the newest photometric conversion tables appropriate for the ACS filters, including stellar evolution models with
the metallicities suitable for the examined galaxies, and adding statistical tests for the model selection. A preliminary version of the
updated procedure was applied to two of the M31 fields observed
with HST around the target globular clusters described in Sect.1.2.8,
namely around G11 and G219 (Angeretti et al. 2008). The two regions
turn out to have somewhat different histories and different metallic33
ity distributions, with the field near G219 requiring solar metallicity
for the most recent population. The new version of the code is being applied to the two late-type dwarfs presented above (IZw18 and
NGC 4449) and to the other metal poor dwarf SBS-1415 for which we
presented the data analysis in 2005.
In 2007 we also analysed our new ACS@HST data of the outer
regions and halo of the starburst dwarf irregular NGC 1569, whose
SFH in the central region we already derived (Greggio et al. 1998 and
Angeretti et al. 2005) from optical (WFPC2@HST) and near-infrared
(Nicmos@HST) data. These data allowed us to clearly resolve RGB
stars down to two magnitudes below the RGB tip (Grocholski et al.
2008). This not only shows that, once again, this galaxy has been
forming stars for at least several Gyrs, but also leads to an important
improvement on its distance: from the RGB tip, we found indeed that
NGC 1569 is almost 1 mag farther than previously thought on the
basis of very uncertain indicators. The actual distance is 3.4 Mpc and
not 2.2. This deep photometry in non crowded, non active regions will
allow us to infer the first epoch and the level of past SF in this galaxy,
which has been so strongly active in the last 1 Gyr, and possibly show
what triggered the recent unusually high activity.
As mentioned in Sect. 1.3.1 we are also studying the SFH of the
SMC fields observed with ACS@HST. To that purpose we are using
our classical Bologna synthetic CMD method as well as that developed
by M. Cignoni and described in Cignoni et al. (2006). The comparison between the two independent approaches will also allow a better
estimate of the uncertainties.
These studies are in collaboration with, among others, A. Aloisi, F.
Annibali and A. Nota (STScI USA), E. Held and L. Greggio (INAFPadova Obs.), J. Gallagher (Wisconsin Univ., USA). This research
was partly supported by PRIN-INAF05 CRA 1.06.08.16.
1.4
Synthetic model atmospheres of stars and highresolution stellar population synthesis
People involved at OAB: Buzzoni
In collaboration with the Mexican group of the Instituto Nacional de
Astronomı́a, Óptica y Electrónica (Inaoe) of Puebla (M. Chavez, E.
Bertone and L. Rodriguez), we further carried on the long-term project
34
for high-resolution spectral synthesis of stellar model atmospheres and
stellar populations.
Figure 12: The expected effect on metal indices by increasing electronic pressure (Pe ) in stellar atmosphere. This effect can be induced
either by increasing surface gravity log g (that is by “packing” atoms
more efficiently) or by increasing metal abundance (thus increasing the
main e− donors to the plasma). Note the different trend of the index
strength depending whether gravity or metallicity are acting. In the
first case (left panel) we expect a weaker index for dwarf stars compared to giants due to the wiping effect of damping broadening in the
spectral features with increasing gravity. Conversely (right panel), the
index tends to be stronger if we increase the corresponding elemental
abundance.
In this framework, relying on the Uvblue ultraviolet library by
Rodriguez-Merino et al. (2005) (consisting of 1770 model atmospheres
at R = λ/∆λ = 50000, across the 850–4500 Å interval), we synthesized a theoretical set of seventeen narrow-band indices, according to
the definition by Fanelli et al. (1987, 1990, 1992). These indices probe
spectral features and continuum slope of stars in the mid-UV wavelength region, between 2200 and 3100 Å. In particular, our calculations
aimed at exploring the index behaviour in terms of the leading stellar
parameters, such as temperature and surface gravity, while we also examined with special care index sensitivity to any change in chemical
composition, a task only feasible under a theoretical approach.
In this respect, line indices such as Fe i 3000, BL 3096 and Mg i 2852,
35
and the continuum index 2828/2921 were found to be among the least
sensitive features to [M/H], quite a special characteristic to be taken
into account for the analysis of integrated spectra of stellar systems.
In fact, bearing in mind that the UV light of stellar aggregates is dominated by stars at the turn off, one would expect the effects of chemical
composition to be in general stronger than those due for instance to
surface gravity (namely the stellar mass) at fixed temperature (see, as
an explanatory sketch, Fig. 12).
Figure 13: Synthetic (Uvblue) vs. empirical indices for the Wu et
al. (1991) IUE high-gravity (log g > 3.5 dex) stars (solid dots). The
straight dotted line in each panel marks the location of the one-to-one
correlation (slope unity), while the solid line is the least-squares linear
fit to the data. Open dots are rejected data points for peculiar or
supergiant stars.
While most of the Fanelli indices display fully negligible variations
with instrumental resolution (less than a few percent), in some cases
(such as for instance BL 3096) we detected changes up to 20% in the
FWHM interval between 6–10 Å. At the standard-system resolution
(i.e. 6 Å FWHM), it is of special relevance to assess to which extent
the synthetic output matches the empirical measurements. For this
test we relied on the Wu et al. (1991) IUE spectral sample of stars
(some 100 objects along the full spectral-type sequence). Quite comfortingly, five line and continuum indices (namely FeI3000, 2110/2570,
2828/2921, S2850 and S2850L) display a remarkable good correlation
with observations and are correctly reproduced by the models over the
entire range of the parameter space pertinent to dwarf and giant stars
(see Fig. 13). In addition, two more indices (namely Mg Wide and
BL 3096) display only marginal discrepancies to within observational
errors, while the rest of the indices are either under- or overestimated.
36
For the five well reproduced indices we provided the polynomial
fitting functions, that correlate the observed strength with the intrinsic stellar atmospheric parameters. For the under- or overestimated
indices we proposed, instead, the corresponding relations of tranformation to self-consistently convert theoretical results to the Fanelli/IUE
standard system. This study represents the first attempt to synthesize
mid-UV indices from high-resolution theoretical spectra, and foresees
important applications for the study of the ultraviolet morphology of
old and intermediate-age (t ≥ 1 Gyr) stellar aggregates.
1.5
Pulsating variable stars
People involved at OAB: Bellazzini, Cacciari, Clementini, Contreras,
Federici, Fiorentino, Greco, Fusi Pecci, Tosi.
Pulsating variable stars are fundamental tools to set the astronomical
distance scale, and to sample different stellar populations in galaxies. In particular, the RR Lyrae stars are excellent tracers of the
oldest stellar population in galaxies. They bear witness to the epoch
of galaxy formation, and their pulsation properties (periods, periodamplitude relations, etc.) can provide fundamental insights on the
processes that lead to the assembling of galaxies. Also, they are the
primary Population II distance indicators in the LG, through the RR
Lyrae luminosity-metallicity relation, (MV (RR)−[Fe/H]) and the P -L
relation in the K band. On the other hand, Cepheids are among the
brightest stellar candles. Their P -L relation remains the most important of the primary distance indicators for nearby galaxies hosting a
young stellar population, up to distances of 30 Mpc.
The role of pulsating variable stars in establishing the astronomical distance scale has been a major field of study at the INAF-OAB
since 1984. A large number of new projects (see e.g. Clementini 2007a,
Clementini et al. 2007b) were started in more recent years, in collaboration with scientists of the INAF-Padova, Napoli and Merate Observatories, as well as with scientists of several International Institutes,
to map out the variable star content in galaxies of different morphological type and to exploit their potential as distance indicators and
stellar population tracers.
37
1.5.1
The infrared JHK light curves of RR Lyr
The first and basic step for the use of RR Lyrae stars as standard
candles is a careful and accurate determination of their absolute magnitude. RR Lyr is the nearest (i.e. brightest) and the best-studied
variable star of its type and therefore plays a crucial role in setting
the zero-point of the distance scale. We have obtained the first infrared (JHK) complete light curves for RR Lyr, derived a new estimate of reddening, distance and physical parameters for this star,
provided a more reliable and accurate absolute calibration of the period K-luminosity relation and discussed the implications of these new
results on the zero-point of the distance scale (Sollima et al. 2008).
This work was done in collaboration with A. Sollima (Univ. of Bologna) and A. Piersimoni (INAF-Teramo Obs.), as well as astronomers
from the Pulkovo Observatory and the Sobolev Astronomical Institute
(St. Petersburg).
1.5.2
Variable stars in the remote Galactic globular cluster
NGC 2419
People involved at OAB: Clementini, Federici, Greco
NGC 2419, one of the brightest and most distant clusters in the MW
halo, is a metal poor Oosterhoff type II system suspected to be the
relic of an extragalactic system accreted by the MW. Using deep B,
V , I time-series CCD photometry over about 10 years, we have identified 101 variable stars in NGC 2419, of which 60 are new discoveries,
doubling the known RR Lyrae stars and detecting for the first time
SX Phoenicis stars. The properties of the RR Lyrae stars confirm that
NGC 2419 is an Oosterhoff II cluster. The colour-Magnitude Diagram
reaches about 2.6 mag below the cluster turn-off. Its features disfavour
the interpretation of NGC 2419 as either having an extragalactic origin or being the relic of a dwarf galaxy tidally disrupted by the Milky
Way (Ripepi et al. 2007a,b, Greco et al. 2007a, Di Criscienzo et al.
2007, 2008a). A paper presenting the catalogue of light curves and the
distance to the cluster derived with different techniques based on the
various variable stars detected in NGC 2419 is in an advanced stage
of preparation (Di Crescienzo et al. 2008b).
This work is in collaboration with Marconi, Musella, Ripepi, Dall’Ora (INAF-Napoli Obs.), Di Crescienzo (INAF-Roma Obs.), Di Fab-
38
rizio (INAF-TNG). This research was partly supported by MIURPRIN04 grant n. CRA 1.06.02.03 and by PRIN-INAF06 grant n. CRA
1.06.09.15.
1.5.3
Variable stars in nearby galaxies
People involved at OAB: Clementini, Contreras, Fiorentino, Greco,
Tosi.
Increasing samples of pulsating variable stars populating the classical
instability strip, from the turnoff of the oldest populations to a few
magnitudes brighter than the HB, are being found in the LG galaxies, irrespective of the galaxy morphological type. The detection and
study of the pulsating variables in a number of LG galaxies (Fornax, Ursa Minor, Small Magellanic Cloud), as well as in several of
the new satellites of the Milky Way recently discovered in the Sloan
Digital Sky Survey catalogue, is being carried out in collaboration
with Held, Gullieuszik and Rizzi (INAF-Padova Obs.), Poretti (INAFBrera Obs.), Marconi, Musella, Ripepi, Dall’Ora (INAF-Napoli Obs.),
Di Fabrizio (INAF-TNG), Smith (MSU), Catelan (PUC, Chile), Pritzl
(Macalester Univ.), Nota (STScI), Gallagher (Univ. Wisconsin), Grebel
(ARI, Heidelberg), Kinemuchi (Univ. Wyoming), Beers (MSU).
The Fornax Project
The Fornax project (Clementini et al. 2007b) is an international collaboration set up to make a comprehensive and deep (V ≤ 26 mag)
study of the variable star population in the field and globular clusters of the Fornax dSph. To this end we have carried out a wide-area
(∼ 1 deg2 ) time series photometric survey of the galaxy field with the
wide field imager of the 2.2m ESO/MPI telescope at La Silla and the 8
CCD mosaic of the CTIO 4m Blanco telescope. High spatial resolution
photometry of the Fornax GCs was obtained instead with the 6.5m
Baade telescope and the SOAR 4.1m telescope, and complemented by
Hubble Space Telescope WFPC2 data. The galaxy instability strip
was mapped from the Dwarf Cepheids (DCs, V ∼ 24–25 mag) to the
Anomalous Cepheids (ACs, V ∼ 19 mag), with a total number of
about 2000 variable stars. The vast majority of the variable stars detected in the Fornax dSph are of RR Lyrae type (including an extraordinarily large number of double-mode pulsators), in agreement with
39
the galaxy’s predominantly old stellar population. However, several
ACs tracing the galaxy’s intermediate-age stars and 85 high-amplitude
short-period variables with properties similar to metal-poor galactic
SX Phoenicis stars were also detected (see Clementini et al. 2006,
Greco et al. 2008a, Poretti et al. 2007, 2008). The latter were used to
reconstruct the Period-Luminosity relation for short-period pulsating
stars (Poretti et al. 2008). According to the pulsation properties of
the RR Lyrae stars the Fornax GCs have been found to belong to
an Oosterhoff-intermediate class and to fill the Oosterhoff-gap defined
by the Galactic GCs (Greco et al. 2007a,b, 2008b). Our findings allow us to exclude that the MW halo can have assembled by stripping
of Fornax dSph-like protogalactic fragments, and demonstrate that
the Fornax dSph conforms instead to the other, already known, dSph
satellites of the MW, which are found to show noteworthy differences
from most Galactic halo stars, both in the chemistry of their old stars
and in the properties of their variable star populations.
This study is in collaboration with Held, Gullieuszik (INAF-Padova
Obs.), Poretti (INAF-Brera Obs.), Catelan (PUC), Smith (MSU),
Pritzl (Macalester Univ.). This research was partly supported by
MIUR-PRIN04 grant n. CRA 1.06.02.03 and by PRIN-INAF06 grant
n. CRA 1.06.09.15.
The Ursa Minor dSph galaxy
The star formation history of the Ursa Minor (UMi) dSph is being
investigated through the study of the galaxy’s variable star populations. We have obtained V , I time series photometry of selected fields
of Ursa Minor with the 1.5m telescope of the Bologna Observatory
at Loiano and near-infrared (K) photometry with NICS@TNG. The
selected fields contain 5 of the 7 Anomalous Cepheids (ACs) known in
UMi, and the peak of stellar density that Kleyna et al. (2003) identify
with an unbound stellar cluster sloshing back and forth within the
UMi halo. The proprietary visual data were combined with SUBARU
and INT archive data of the galaxy. Our CMD for the galaxy reaches
3.5 magnitudes below the galaxy turnoff, showing an extraordinarily
rich harvest of SX Phoenicis stars. The study of the light curves of
the galaxy’s variable stars is in progress.
This study is in collaboration with Marconi, Ripepi, Musella, Dall’Ora (INAF-Napoli Obs.).
40
The “Small Magellanic Cloud in Space and Time”
As part of an international collaboration aiming at the detailed study
of the stellar populations, structure and evolution of the Small Magellanic Cloud (SMC, see Sect. 1.3.1), new candidate variable stars were
identified in the SMC cluster NGC121 based on HST WFPC2 archive
and ACS proprietary (PI: J. Gallagher) images of the cluster. The
new candidates are located from the cluster’s Main Sequence up to
the Red Giant Branch. Twenty-seven of them are on the cluster’s
Horizontal Branch and are very likely RR Lyrae stars. We also detected 20 Dwarf Cepheid candidates in the central region of NGC121
(Fiorentino et al. 2008a). Our results confirm the “true” globular
cluster nature of NGC121, a cluster which is at the young end of the
Galactic globulars age range (Glatt et al. 2008).
Guaranteed time observations to study constant and variable star
populations of the SMC body, Bridge and Stream down to the turn-off
of the oldest stars, are planned for OmegaCAM@VST (the STEP@VST
survey, PI: V. Ripepi, CoIs: members of the OAB; Ripepi et al. 2006).
The SMC project was also extended to the near-infrared in the framework of the approved VMC@VISTA (The VISTA near-infrared Y JKs
survey of the Magellanic System, PI: M. Cioni, CoIs: members of the
OAB) ESO public survey whose first observations will start in 2009
(see Cioni et al. 2008).
This study is in collaboration with Ripepi, Marconi, Musella, Cappellaro (INAF-Napoli Obs.), Nota, Sirianni (STSCI), Gallagher (Univ.
Wisconsin), Cioni (Univ. Hertfordshire, UK), and Grebel (ARI, Heidelberg).
Stellar Archeology in the Milky Way halo: variable stars and
stellar populations in the newly discovered Milky Way satellites
Λ-cold-dark-matter hierarchical models of galaxy formation suggest
that the halo of the Milky Way (MW) was assembled, at least in part,
through the accretion of protogalactic fragments partially resembling
the present-day dwarf Spheroidal (dSph’s) companions of the MW
(e.g., Grebel, 2005). A number of Galactic halo fragments may thus
originate from dSph’s that were accreted by the MW. However, so
far we have failed to identify these possible “building blocks” of the
Galactic halo, since the nine known dSph satellites of the MW have
41
shown some noteworthy differences from most halo stars, both in the
chemistry and in the properties of their variable star populations. In
the last couple of years several new dSph companions of the MW were
discovered in the Sloan Digital Sky Survey photometric catalogue (see
e.g. Belokurov et al. 2006a,b; Zucker et al. 2006a,b). These new
galaxies could be the shreds from the violent building phase of the
MW.
Our team is undertaking a long-term project aimed at searching for
and fully characterizing the variable star content as well as the stellar
populations of several of the new LG members. Time-series multiband observations reaching each galaxy’s main sequence turnoff were
obtained between 2006 and 2007 for 8 of the new systems (namely:
Bootes I, Bootes II, Coma, Canes Venatici I – CVn I –, Canes Venatici
II – CVn II –, Ursa Major II, Leo IV, and Hercules) using a variety of
telescopes from the 1.5m to the 4.3m size. Analysis of Bootes I, CVn
I, CVn II, Coma, UMa II and Leo IV was completed and results have
already been partially published (Bootes I: Dall’Ora et al. 2006, 2007;
CVn I: Kuehn et al. 2008; CVn II: Greco et al. 2008c). Lyrae stars
were identified in all the galaxies we have analyzed so far. According
to the pulsation properties of their RR Lyrae stars Bootes I, CVn II,
Coma, UMa II and Leo IV turned out to belong to an Oosterhoff II
class (Dall’Ora et al. 2008), while CVn I is found to be of Oosterhoffintermediate type (Kuehn et al. 2008).
This study is in collaboration with Ripepi, Marconi, Musella, Dall’Ora (INAF-Napoli Obs.), Di Fabrizio (INAF-TNG), Smith (MSU),
Catelan (PUC, Chile), Pritzl (Macalester Univ.), Kinemuchi (Univ.
Wyoming), Beers (MSU).
1.5.4
IZw18: the “Rosetta stone” without a distance
People involved at OAB: Clementini, Contreras, Fiorentino, Tosi
IZw18 is the most metal poor galaxy ever observed in the local Universe and, due to the apparent lack of an old population, it has long
been regarded as a possible example of a galaxy undergoing its first
burst of star formation, and a local analogue of primordial galaxies
in the distant Universe. However, it may be possible that the old
population of IZw18 is at the limits of present-day instrumental capabilities, because the galaxy is much further away than previously
believed. Quoted distances in the literature have ranged from 10 to
42
20 Mpc.
Figure 14: V and I light curves of Classical Cepheids in IZw18, from
Fiorentino et al. (2008, in preparation). The stars’ periods are labelled.
We have discovered and obtained periods and light curves for Classical Cepheids (CCs) in IZw18, by means of Alard’s ISIS image sub43
traction tool, based on deep F606W, F814W time series imaging of
this Blue Compact galaxy obtained in 2005 with the ACS@HST (PI:
A. Aloisi, CoIs: members of the OAB, see also Sect. 1.5.4). Examples of the light curves for 3 Classical Cepheids and one long period
variable in IZw18 are shown in Fig 14. New theoretical pulsation models of CCs suited for the extremely low metallicity of this primordial
galaxy (Z = 0.0004, Y = 0.24) have also been computed to interpret
the properties of the variable stars discovered in IZw18 (Fiorentino et
al. 2007, Marconi et al. 2008, in preparation). Our theoretical and observational combined efforts have allowed to resolve the controversy on
the nature of IZw18, by direct determination of the galaxy’s distance
using its CCs (Aloisi et al. 2007a,b, Fiorentino et al. 2007, 2008b).
The catalogue of light curves is published in Fiorentino et al. (2008c,
in prepaparation).
The study is in collaboration with, among others, A. Aloisi, F.
Annibali (STScI, USA), Saha (NOAO), Marconi, Musella (INAF-OA
Napoli). This research is partly supported by the INAF-PRIN06 grant
nĊRA 1.06.09.15.
Figure 15: Examples of the B light curves for Cepheids and RR
Lyrae stars in M31 observed during the October 2007 SDT run with
LBC@LBT. Each data point corresponds to a 300 sec exposure, typical error bars of the individual data points are of the order of 0.004–
0.02 mag for the Classical Cepheids, 0.06–0.07 mag for the Anomalous
Cepheids, and of 0.09–0.17 mag for the RR Lyrae stars. The stars’
periods are labelled.
44
1.5.5
Variable stars in the Andromeda galaxy
People involved at OAB: Bellazzini, Cacciari, Clementini, Contreras,
Federici, Fusi Pecci, Tosi
As the nearest giant spiral galaxy, Andromeda (M31) provides a unique
opportunity to study the structure and evolution of a massive galaxy
and, by comparison with the Milky Way (MW), to address the question of variety in the evolutionary histories of massive spirals. Our
team is carrying out an observational programme aimed at monitoring the pulsation characteristics of the short and intermediate period
pulsating variable stars in the M31 halo, in its giant tidal stream and
in the M31 GCs. Nine hours of observing time with the Large Binocular Telescope (LBC@LBT) were awarded to the project during the
Science Demonstration Time of the blue camera (PI G. Clementini)
and a further 20 hours were awarded in 2008. Time-series observations
of the selected fields of Andromeda were obtained in October 2007 and
September 2008.
Fig.16 shows the color-magnitude diagram of one of our M31 stream
fields. On the other hand, 78 orbits with WFPC2 on board of the HST
were awarded in HST Cycle 15 (PI G. Clementini) to study the variable star population of six properly selected globular clusters of M31.
Observations were obtained from June to September 2007. Data reduction has been completed for all 6 clusters, analysis of the light
curves is in progress. In B514 we have discovered more than a hundred
RR Lyrae stars with light curves of excellent quality (see Contreras et
al. 2008).
The study is in collaboration with: Marconi, Ripepi (INAF-NApoli
Obs.), Smith (MSU), Catelan (PUC, Chile), Pritzl (Macalester Univ.),
Kinemuchi (Univ. Wyoming).
45
Figure 16: V, B − V color magnitude diagram of a stream region of
M31 observed during the October 2007 SDT run with LBC@LBT,
showing the comparison with isochrones from Girardi et al. (2000, and
following updates) for ages in the range from 63 to 700 million years
which well fit the young and intermediate-age stellar components, and
with the mean ridge lines of the Galactic globular clusters (GCs) M15,
M3, 47 Tuc and NGC6553 for the old stellar component. Examples of
the different types of variable stars detected in this portion of M31 are
shown by larger filled dots; they include RR Lyrae stars (at V ∼ 25
mag), Anomalous Cepheids (at V ∼ 24 mag), Classical Cepheids (V ≥
22 mag) and a couple of binary systems. Stars mark variables for which
we have a good sampling of the light curves (see Fig. 15). The longdashed lines show the boundaries of the theoretical instability strips
for RR Lyrae stars, and for Anomalous Cepheids with Z = 0.0004 and
1.3 < M < 2.2M (from Marconi et al. 2004).
46
2
Extragalactic Astronomy and
Cosmology
Adaptively smoothed XMM–Newton image of the galaxy cluster Abell
514. The size of the image is about 25 arcmin (∼ 2 Mpc). The
cluster emission shows an elongated shape with two bright subclumps,
indicative of an ongoing merger. From Weratschnig et al. 2008, A&A
in press.
People involved at OAB:
• Scientific staff: S. Bardelli, M. Bolzonella, A. Cappi, P. Ciliegi,
A. Comastri, H.R. de Ruiter, S. Ettori, R. Gilli, C. Gruppioni,
M. Meneghetti, R. Merighi, M. Mignoli, L. Origlia, L. Pozzetti,
R. Sancisi, G.M. Stirpe, G. Zamorani, V. Zitelli, E. Zucca;
• Fellows and contracts: A. Braccesi, J. Fritz, M. Gitti, F. Lamareille, M. Montemaggi, G. Parmeggiani, R. Sancisi.
Observational extragalactic astronomy has traditionally been one of
the main themes of research at the Bologna Observatory. It includes a
wide range of subjects, from the structure and evolution of “normal”
galaxies, to the physical properties of active galactic nuclei (AGN) and
galaxy clusters, to large-scale structures and observational cosmology.
The extragalactic research at the Bologna Observatory is characterized by a multi-wavelength (radio, infrared, optical, X-ray) study of
galaxies, AGN and clusters of galaxies. Much of this research is based
on an intensive use of the most advanced instruments available today:
the ESO optical/NIR telescopes (including VLT), the Hubble Space
Telescope, the X-ray satellites Chandra and XMM-Newton, the IR
satellite Herschel, the Westerbork, VLA and ATCA radio-telescopes.
2.1
2.1.1
Structure and evolution of galaxies
Neutral hydrogen studies
People involved at OAB: R.Sancisi.
Galaxy Interactions, accretion, minor mergers
R. Sancisi, F. Fraternali (Univ. of Bologna), T. Oosterloo (ASTRON,
Dwingeloo) and T. van der Hulst (Univ. of Groningen) have continued their study of cold gas accretion in galaxies and have written a
review published in Astron Astrophys Rev (2008) 15:189-223. They
have concluded that there is a mean “visible” accretion rate of cold
gas in galaxies of at least 0.2 M /yr.
49
High velocity gas and HI halos of spiral galaxies
R. Boomsma (Univ. of Groningen), T. Oosterloo (ASTRON, Dwingeloo), F. Fraternali (Univ. of Bologna), T. van der Hulst (Univ. of
Groningen) and R. Sancisi have completed the study of the vertical
structure and kinematics (high-velocity gas and HI holes) of the HI
in the spiral galaxy NGC 6946. The results have been presented in a
paper (A&A in press, 2008, arXiv/0807.3339B).
2.2
2.2.1
Active galactic nuclei and star-forming
galaxies
Optical studies
People involved at OAB: de Ruiter, Stirpe, Zitelli.
Optical monitoring of bright AGN
V. Zitelli and G. Stirpe, in collaboration with D. Trevese (Univ. of
Roma La Sapienza) and F. Vagnetti (Univ. of Roma Tor Vergata), are
continuing the analysis of photometric and spectroscopic monitoring
of high-z quasars using the Loiano and Asiago telescopes to study the
variability of both continuum and broad emission lines in AGN. The
aim of the project is the extension to MB > −26 of the correlation
found, in type 1 Seyferts and low-z QSOs, between source luminosity
and the primary estimate of the size of the Broad Line Region (BLR)
obtained from echo-mapping. The correlation is used to extend the
estimates of virial masses and accretion rates to non-monitored sources
(secondary estimates), on the basis of the estimated BLR sizes and of
the measured broad-line widths.
The first light curves of two AGN were published in Trevese et al.
2007, showing a variation in luminosity of the order of 0.1 mag occurring in the CIV and MgII lines, with a measurement accuracy of ∼5%.
Continuum variability
Despite the huge number of QSOs discovered by recent surveys, constraining the evolution of the luminosity function at the bright end,
adequate AGN samples are still lacking at the faint end. Most QSO
samples are selected by the color technique, which cannot be applied
50
at low intrinsic luminosities, due to contamination by the host galaxy.
In 2007 Zitelli and Stirpe, in collaboration with Trevese and Vagnetti,
started a spectroscopical study of a composite sample of AGN candidates selected in SA57 following different searching techniques, to
identify low luminosity AGN, and break down the sample into different classes of objects. AGN candidates were obtained through optical
variability and/or X-ray emission. Of special interest are the extended
variable objects, which are expected to be galaxies hosting LLAGN.
Among the 26 new classified objects a fair number (9) show typical
AGN spectra, 10 objects show Narrow Emission Line Galaxy spectra,
and in most of them (8/10) optical variability suggests the presence of
LLAGN. Results are published in Trevese et al. (2008, A&A, 477, 473).
Emission lines and variability of AGN
G. Stirpe, in collaboration with J. Sulentic (Univ. of Alabama), P.
Marziani, M. Calvani and P. Repetto (INAF–Padova Observatory),
has continued the study of the broad-emission line characteristics of a
sample of high-z QSOs. The analysis of the full sample of more than 50
QSOs (selected from the Hamburg-ESO survey) with z = 0.9÷3.0 was
completed: the principal aims were to obtain estimates of the blackhole mass, of the Eddington ratio and line-profile information. The
data are being used within the framework of the Boroson-Green Eigenvector 1 (E1), which correlates various measured properties of the optical emission lines of AGN, extending it to the high-luminosity domain.
The use of Hβ (shifted to the IR band) instead of the more easily observable MgII or CIV lines, makes the analysis homogeneous with that
performed on low-redshift AGN. The high-luminosity sources, while
not occupying a separate region in the E1 parameter space, are not
present in the region with the lowest line widths, and show a systematic decline in the equivalent width of the [O III] lines.
G. Stirpe has worked with a student (R. Bellini) on the reduction
and analysis of VLT monitoring data of three high-z QSOs, obtained
with ISAAC in the 2001–2005 period. Differential photometry in the
K-band, and spectroscopy of Hα (also in the K-band), were analysed in order to obtain the continuum and emission-line light curves.
While the length of the campaign was too short to obtain a meaningful line vs. continuum lag, the high quality of the data has allowed to
study line-profile variations which took place during the monitoring.
In particular, the rms spectrum of Hα in one of the QSOs displayed a
51
double-peak profile. This property had not yet been detected in a highluminosity AGN, but so far only in a handful of low-z Seyfert 1 nuclei.
It could be caused by the variations in the BLR taking place either in
a disk structure, or in a bipolar outflow. Further analysis is underway.
The project is in collaboration with A. Marconi (Dept. of Astronomy,
Univ. of Firenze), A. Capetti (INAF–Torino Observatory), A. Robinson and D. Axon (Rochester Institute of Technology).
The environment of AGN
V. Zitelli, in collaboration with P. Focardi (Univ. of Bologna) is continuing the study of compact groups of galaxies and, in particular, of
the role of active galaxies (AGN) in dense environment. Ample evidence has been reported of a complex environment around AGN up to
z ∼ 3. However, while it is well established that radio loud quasars,
radio galaxies and BLLacs reside in denser than average regions, the
role of the environment and of interactions on Seyfert galaxies is to
some extent still controversial, also because the samples used so far
are limited in number. To reduce the statistical uncertainty, Zitelli
and collaborators adopt a strategy based on the analysis of a statistically significant sample of nearby AGN and appropriate control
samples selected on the basis of criteria independent of morphology
and environmental properties. A sample of about 300 physical compact groups was extracted applying an automatic code to 3-D galaxy
catalogues. The presentation of the sample and the preliminary results are reported in Focardi et al. (2006, A&A, 456, 467). The first
nuclear spectral classification, performed using standard diagnostic
diagrams, of 48 UZC-BGPs, which represents more than half of the
whole sample, is presented in Focardi et al. (2008, A&A, 484, 655),
and shows that AGN are characterized by an advanced morphological type while the SB phenomenon occurs with the same frequency
in early and late spirals. Whether and how these unusual characteristics relate to the pair environment needs to be further investigated.
LLAGN and LLAGN candidates do not always show similar properties; the former are more luminous in B, richer in early-type (E-S0s)
galaxies, and half of them are hosted in galaxies showing visible signs
of interaction with fainter companions suggesting that minor interactions might be a driving mechanism for a fraction of LLAGN. The
differences between LLAGN and LLAGN candidates might confirm
the heterogeneous nature of this class of objects.
52
HST images of B2 radio galaxies
H.R. de Ruiter, in collaboration with A. Capetti (INAF–Torino Obs.),
P. Parma and R. Fanti (INAF–IRA, Bologna), and R. Morganti (ASTRON, Dwingeloo), has studied HST images (in two colours, V and
I) of about 60 radio galaxies selected from the B2 sample of low luminosity radio galaxies. Brightness profiles were derived for almost all
galaxies. An interesting conclusion has emerged from this work: radio
active galaxies are only of the “core”-type (i.e. galaxies in which the
inner brightness profile gradient is very shallow or even about zero),
while power-law profiles are exclusively found in radio-quiescent galaxies. A current model to explain the shallow cores is that they are the
result of depletion of the inner regions, due to the presence of a binary
black hole in the centre of the galaxy. At present H. de Ruiter is developing a more sophisticated computer program for fitting brightness
profiles with a number of different model profiles.
For some of the B2 radio galaxies spectroscopic observations with
the TNG have been carried out, in order to obtain central velocity
dispersions, and study the core fundamental plane. This programme
is a collaboration between H.R. de Ruiter, P. Parma (INAF–IRA) and
D. Bettoni and R. Falomo (INAF–Padova Obs.). A paper describing
the spectroscopic data is now being prepared for submission to A&A.
2.2.2
Near-IR studies
People involved at OAB: Comastri, Origlia.
Metal enrichment in starburst galaxies
The analysis of a deep (about 100 ksec) XMM observation of M82 was
completed in 2007 and published in Ranalli et al. (2008). The most important results can be summarized as follows: The broad-band (0.5–10
keV) emission is due to at least three spectral components: (i) continuum emission from point sources; (ii) thermal plasma emission from
hot gas; and (iii) charge-exchange emission from neutral metals (Mg
and Si). The plasma emission has a double-peaked differential emission measure, with the peaks at ∼ 0.5 and ∼ 7 keV. Spatially resolved
spectroscopy has shown that the chemical absolute abundances are
not uniformly distributed in the outflow, but are larger in the out53
skirts and smaller close to the galaxy centre. The abundance ratios
also show spatial variations. Despite the much improved quality of the
available X-ray data with respect to the previous observation (Origlia
et al. 2004), the X-ray-derived oxygen abundance is lower than that
measured in the atmospheres of red supergiant stars, leading to the hypothesis that a significant fraction of oxygen ions have already cooled
off and no longer emit at energies < ∼ 0.5 keV.
This work is carried out in collaboration with P. Ranalli (Astronomy Dept., Univ. of Bologna) and R. Maiolino (INAF–Osservatorio
Astronomico di Roma).
2.2.3
X-ray studies
Suzaku Observations of Compton Thick AGN
People involved at OAB: Comastri, Gilli
A fraction as high as 50% of nearby AGN are obscured by large
amounts of gas and dust with column densities (NH > 1024 cm−2 )
which are optically thick to Compton scattering. Compton Thick
AGN are required by AGN synthesis models to fit the XRB 30 keV
peak and to reconcile the estimate of the Super Massive Black Hole
(SMBH) mass density obtained by integrating the AGN luminosity
function with that of relic SMBH in nearby bulges. In the X-ray band,
the primary emission is visible only at energies above about 10 keV
and thus they are severely underrepresented even in the deepest XMM
and Chandra surveys. Ongoing Swift/BAT and INTEGRAL/IBIS surveys. are currently surveying the hard X-ray sky. Although limited
to relatively bright fluxes, the large area covered has allowed the detection of more than 100 hard X-ray selected AGN. The sample is
in principle unbiased against Compton Thick sources, however only a
handful of them were clearly classified as Compton Thick combining
the hard X-ray surveys data with archival (ASCA, BeppoSAX and
XMM) spectra. It is likely that several of them may be hiding among
the unidentified Swift and INTEGRAL sources or were not recognized
as such due to the limited counting statistics. In 2007 we have obtained Suzaku observations of two candidate CT AGN detected above
10 keV (a follow-up of a successful proposal approved in 2006 for two
other sources). Thanks to the good sensitivity in the 10–60 keV band
of the Suzaku pin detector, good quality, broad band (∼ 0.5–60 keV)
54
spectra were obtained. The data analysis is ongoing. The first results
indicate a variety of spectral shapes. One of them is clearly Compton
Thick, while the other is heavily obscured (NH ∼ a few 1023 cm−2 ).
The covering fraction of the X-ray absorber is also very different among
the sources. In one object the lack of X-ray emission below ∼ 4 keV
suggests that the nuclear source may be fully covered by obscuring
material. The iron line emission in at least two of the four objects is
extremely complex, requiring several components.
This research is in collaboration with C. Vignali (Astronomy Dept.,
Univ. of Bologna).
2.3
Surveys and observational cosmology
A large fraction of the Observatory staff is involved in surveys of extragalactic objects1 . Some of these surveys are ongoing long-term
projects, but quite a few have started only recently, or will start in
the near future. They will require observing time with the new generation of optical, infrared and X-ray telescopes such as VLT, Spitzer,
Herschel, Chandra, XMM-Newton.
2.3.1
The VIMOS/VLT Deep Survey (VVDS)
People involved at OAB: Bardelli, Bolzonella, Cappi, Ciliegi, Lamareille, Merighi, Pozzetti, Zamorani, Zucca.
The visual spectrograph VIMOS2 is mounted at VLT-Melipal and saw
its first light successfully on February 26, 2002. Results from the
VVDS have been published in the last few years in about 40 refereed
papers. A few of the main issues which are addressed with these data
are:
• precise estimates, on the basis of a single sample with well understood selection criteria, of the evolution of the luminosity and
1
As an aid to observational cosmologists, de Ruiter has made available a collection of cosmological formulae, which is updated periodically. For a number of models (the standard Friedmann model, flat models with non-zero cosmological constant, and some more exotic ones) distances, volumes and look-back times are given
as a function of redshift. The latest version (in PDF format) can be consulted at (or
downloaded from) the WEB-site: http://www.bo.astro.it/~deruiter/cosmo/
2
http://www.oamp.fr/virmos/
55
mass function of galaxies and of the star formation history up
to z ∼ 2;
• detailed tests of the predictions of various models of galaxy evolution (e.g. hierarchical versus monolithic models);
• studies of the properties and evolution of clustering up to high
redshift and of the relation between the spatial distribution of
luminous and dark matter (bias).
In 2007 the main contributions to the VVDS survey by the researchers at the Bologna Observatory were:
1. analysis of the evolution of the Galaxy Stellar Mass Function
(GSMF) up to z = 2.5;
2. an estimate of the Luminosity Functions (LFs) in the red bands;
3. an estimate of the history of mass assembly for galaxies of different stellar masses and types;
4. comparison of the VVDS data with hierarchical models from the
Millennium simulations;
5. analysis of the faint end of the Luminosity Function of Type-1
AGN.
1. We have derived the GSMF in the VVDS deep survey from
(1) the optical (I-selected 17.5 ≤ IAB ≤ 24) spectroscopic sample
up to z = 1.2 and from (2) the near-IR sample (K-selected KAB <
22.34 & KAB < 22.84) up to z = 2.5, with photometric redshifts
accurately calibrated on the VVDS spectroscopic sample. At low redshifts (z ' 0.2) we found a substantial population of low-mass galaxies
(< 109 M ) consisting of faint blue galaxies (MI − MK ' 0.3). Our
data are consistent with mild or negligible (< 30%) evolution of the
number density of massive galaxies (> 6 × 1010 M ) up to z ∼ 0.7. For
less massive systems the no-evolution scenario is instead excluded.
Specifically, a large fraction (≥ 50%) of massive galaxies have already
been assembled, and have converted most of their gas into stars at
z ∼ 1, thus ruling out ‘dry mergers’ as the major mechanism of their
assembly history below z ' 1. This fraction decreases to ∼ 33% at
56
Figure 17: Histograms showing the fraction of galaxies taken from
VVDS as a function of the amplitude of the 4000 Å Balmer break (an
estimator of stellar ages, Dn (4000)) in five different ranges of stellar
mass and in four redshift bins. The first row shows the distribution
for the local Universe taken from the SDSS. This figure shows a clear
dependency of the stellar age, as inferred by the Dn (4000) distribution,
on the stellar mass that holds at all epochs up to z ∼ 1.3.
57
z ∼ 2. The number density of low-mass systems has increased continually (by a factor up to 4.1 ± 0.9) from z = 2 to the present age. This
is consistent with a prolonged mass assembly also at z < 1.
2. In the same K-selected sample, covering a wide area of ∼ 620
arcmin2 , we are also studying the evolution of the Luminosity Functions (LFs) in the red bands I, J and K up to a redshift z ∼ 2.5. In
agreement with data available in the literature, but now with better
statistics, we found that the bright end of the K-band LF is already
in place at z ≥ 1.5. The K-band LFs for different photometric types,
defined as in Zucca et al. (2006), were also computed, and this study
will be complemented by computing, for the same galaxy types, the
evolution of the stellar mass functions.
3. Using a mass-limited sample of 4048 galaxies taken from the
VVDS we have discussed to what extent stellar mass drives galaxy
evolution, showing for the first time the interplay between stellar ages
and stellar masses over the past ∼ 8 Gyr (0.5 ≤ z ≤ 1.3, see Fig. 17
taken from Vergani et al. 2008).
Using the amplitude of the 4000Å Balmer break Dn (4000) as a
stellar age estimator, we observe that low-mass galaxies have younger
ages of the underlying stellar population, i.e. small Dn (4000), while
the galaxy distribution moves to higher Dn (4000), or older stellar ages,
at increasing stellar mass. This behaviour is observed also in the local
Universe but, as cosmic time goes by, we witness an increasing abundance of massive spectroscopically defined early-type systems at the
expense of the late-type systems. This spectral transformation is also
confirmed by the evolution of our type-dependent stellar mass function. This is a process which started at early epochs and continues
efficiently down to the local Universe. As shown in Fig. 17 by Vergani and VVDS collaborators, the underlying stellar ages of late-type
galaxies apparently do not show evolution, most likely as a result of a
continuous and efficient formation of new stars.
We find that the activity and efficiency of forming stars are mechanisms that depend on galaxy stellar mass, and the stellar mass assembly becomes progressively less efficient in massive systems as time
elapses. In the same paper it is also shown that the role of dry merging
events at z < 1.3 is marginal, since our estimated efficiency in stellar
mass assembly can account for most of the progressive accumulation
of observed passively evolving galaxies.
4. In 2007 we also started a study aiming at comparing the observed MFs and LFs in the VVDS with hierarchical model predictions
58
using the Millennium simulations limited to I < 24 (De Lucia et al.
2006). Preliminary results show an excess of the Millennium MFs at
intermediate/low masses (< 1010 M ) compared to the VVDS MFs.
Furthermore, Millennium MFs show no or only small evolution with
redshift compared to the local estimate, i.e. milder than in VVDS, up
to z = 1.6, and a faster evolution at higher redshifts.
Concerning the comparison between luminosity functions, while
the global LFs are in good agreement, the Millennium LFs are significantly different from the VVDS ones, for the various photometric
types. This is particularly true for early type galaxies, with the Millennium simulation having too many red galaxies of low luminosity.
The differences between VVDS and Millennium LFs decrease towards
the latest type galaxies, even if an excess of very bright blue galaxies
appears at low redshift in the Millennium with respect to the VVDS.
5. The VVDS sample of 130 faint, broad-line AGN, selected on
the basis of their spectra, and therefore free of any morphological
and colour selection biases, was used to derive the optical luminosity
function and its evolution up to z = 3.6. By combining our faint
VVDS sample with the large sample of bright AGN extracted from
the SDSS DR3, we have found that the best fit evolutionary model is
a luminosity dependent density evolution (LDDE) model, similar to
those derived from the major X-surveys. On the basis of this model
we have found, for the first time from the analysis of optically selected
samples, that the peak of the AGN space density shifts significantly
towards lower redshift going to lower luminosity objects. This result is
consistent with a scenario of “AGN cosmic downsizing”, in which the
density of more luminous AGN, possibly associated to more massive
black holes, peaks earlier in the history of the universe (i.e. at higher
redshift), than that of low luminosity ones, which reaches its maximum
later (i.e. at lower redshift).
2.3.2
The GMASS redshift survey
People involved at OAB: Bolzonella, Mignoli, Pozzetti, Zamorani.
The Bologna Observatory has participated in the “Galaxy Mass Assembly ultradeep Spectroscopic Survey (GMASS)” project, which is
carried out in collaboration with the observatories of Arcetri and
Padova, ESO and the Astronomy Department of the Bologna University. Despite the tremendous recent progress in observational cosmol59
ogy, the mechanisms leading to the birth and the evolution of galaxies
are still poorly known. In particular, understanding and tracing the
cosmic history of galaxy mass assembly is one of the main open issues
of galaxy formation and evolution. Recent results at z < 1 and z > 3
suggest that most of the galaxy mass was built at z ∼ 1–3.
The GMASS aim was to study galaxies at z > 1.4 by performing ultra-deep ESO VLT + FORS2 multi-object spectroscopy with
very long integration times (15–40 hours per mask) of infrared-selected
galaxies (m4.5 < 23) with high-quality photometric redshifts zphot >
1.4. The GMASS target field (about 50 square arcminutes) is located in the GOODS-CDFS. This field includes several galaxies with
already known spectroscopic redshifts, and a large collection of multiwavelength data from UV (GALEX), optical (HST), NIR (VLT), MIR
+FIR (Spitzer), radio and X-ray data.
The observations were completed in 2005 and provided spectra
of 208 objects. Redshift measurements were completed, providing a
redshift for most (182/208) of the observed objects. The most striking
feature of the GMASS z distribution is a very significant peak in the
redshift distribution at z ' 1.6 (33 objects from GMASS + 7 from
the literature).
In the last couple of years in Bologna we have carried out the determination of optimised photometric redshifts, stellar masses, star formation efficiency and age of the stellar population through the fitting
of the multi-band photometric SEDs, using different codes of stellar
population models (i.e. Bruzual & Charlot 2003, Maraston 2005 and
Charlot & Bruzual 2007). An analysis of the Galaxy Stellar Mass
Function (GSMF) up to z = 3 using the spectroscopic sample and the
whole photometric sample is currently in progress in Bologna, with
particular attention given to the GSMF in the structure at z = 1.61.
We have analysed in detail the subsample of 13 early-type galaxies at 1.4 < z < 2.5 in collaboration with Bologna University and
Padova. A stacked spectrum with an equivalent integration time of
∼ 500 h was obtained, covering the UV range from 2500 to 3500Å and
showing typical features of an old stellar population. Using various
libraries of synthetic stellar population models we found that the spectral and photometric SED properties indicate very weak or absent star
formation, moderately old stellar ages of ∼ 1 Gyr (for solar metallicity) and stellar masses in the range of 1010−11 M , thus implying that
the major star formation and assembly processes for these galaxies
occurred at z > 2. Low metallicity values (Z < 0.2Z ) are excluded
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both by the SED fitting and by the spectrum fitting. These galaxies
have morphologies that are predominantly compact and spheroidal.
However, their sizes (Re ≤ 1 kpc) are much smaller (by a factor 2–3)
than those of spheroids with similar mass in the present-day Universe.
We suggest that these “superdense” passive galaxies at 1 < z < 2 are
the remnants of the powerful starbursts occurring in submillimetreselected galaxies at z > 2 and evolve subsequently by gradually increasing their sizes with mechanisms like major dry-merging and/or
envelope accretion, more or less rapidly depending on their mass and
environment (Cimatti et al. 2008).
In parallel, we are studying also the structure at z = 1.61, deriving
some physical parameters like over-density, both in mass and in galaxies, total mass and dynamical status. We find a velocity dispersion
consistent with 500 km s−1 , and from the estimated galaxy overdensity (∼ 6–9) and the volume that the galaxies occupy, we estimate a
mass of 5 × 1013 M for the overdense structure. We have also studied
differences, in terms of mass, colour and age, between the galaxies
within the structure and field galaxies at the same redshift (Kurk et
al. 2008, submitted).
A systematic analysis on both the single spectra of the brightest
galaxies and the composite spectra of homogeneous classes of fainter
objects is currently underway at the Bologna Observatory. This study
is aimed at measuring the equivalent widths of the main nebular lines,
the UV spectral slopes and the interstellar gas dynamics.
2.3.3
The ELAIS/SWIRE survey
People involved at OAB : Ciliegi, Comastri, Gruppioni, Mignoli, Pozzetti, Zamorani.
ELAIS is a large European project, involving 19 different institutes,
initially aimed at studying the nature and evolution of the extragalactic sources detected by the Infrared Space Observatory (ISO) in selected areas of the sky. The ELAIS fields are also targets selected by
the Spitzer Legacy Programme SWIRE (PI: C. Lonsdale, Caltech)
C. Gruppioni, G. Zamorani, A Comastri and L. Pozzetti, in collaboration with F. Pozzi (UniBo), M. Polletta (INAF-IASF) and the
SWIRE consortium, have performed a detailed study of the SEDs of
the largest available highly (72%) complete spectroscopic sample of
mid-infrared (MIR) selected galaxies and AGN at intermediate red61
shift. The sample contains 203 extragalactic sources from the 15-µm
survey in the ELAIS-SWIRE field S1, all with measured spectroscopic
redshift. Most of these sources have full multi-wavelength coverage
from the far-UV (GALEX) to the far-infrared (Spitzer) and lie in the
redshift range 0.1 < z < 1.3. Due to its size, this sample allowed us
for the first time to characterise the spectral properties of the sources
responsible for the strong evolution observed in the MIR. Based on
SED-fitting techniques we have classified the MIR sources, identifying
AGN signatures in about 50% of them. This fraction is significantly
higher than that derived from optical spectroscopy (∼29%) and is due
in particular to the identification of AGN activity in objects spectroscopically classified as galaxies. This might be partly due to the fact
that the spectroscopic classification can be somewhat unreliable because of host galaxy dilution in the optical. It is likely that in most
of our objects, the AGN is either obscured or of low-luminosity, and
thus it does not dominate the energetic output at any wavelength, except in the MIR, showing up just in the range where the host galaxy
SED has a minimum. The fraction of AGN strongly depends on the
flux density, with that derived through the SED-fitting being about
20% at S15µm ∼ 0.5-1 mJy and gradually increasing up to 100% at
S15µm > 10 mJy, while that obtained from optical spectroscopy is
never > 30%, even at the highest flux densities. The results of this
work will be very useful for updating all models aimed at interpreting
the deep infrared survey data and, in particular, for constraining the
nature and the role of dust-obscured systems in the intermediate/highredshift Universe.
C. Gruppioni, A. Comastri, G. Zamorani, in collaboration with
C. Vignali and F. Pozzi (UniBo), F. Fiore and C. Feruglio (INAFOAR), A. Martinez-Sansigre (MPIA, Heidelberg), M. Jarvis (Hertfordshire, UK), A. Omont (IAP, France), have obtained optical spectra
with the TNG for 26 mid-IR selected sources detected by the Spitzer
SWIRE survey in the Lockman Hole and ELAIS N1-N2 fields. The targets were accurately selected to sample both the population of heavily
obscured AGN and dusty starbursts at high redshifts, close to the peak
of both quasar and star-formation activity. The adopted multi-color
selection technique, which combines medium-deep NIR/MIR (Spitzer)
and optical photometry, is particularly promising in selecting the most
heavily obscured AGN and vigorous star-forming galaxies at high redshifts (≈ 1.5–3.0), which would remain elusive by even the deepest
X-ray and infrared observations.
62
We were able to measure emission lines and reliable redshifts for 10 of
the proposed targets. The remainder showed no obvious lines in their
spectra, and remain unidentified. The 10 identified objects are those
with brighter optical counterpart among the target sample and turned
out to be all AGN with redshifts in the range 1 < z < 4, consistent
with predictions based on IR/optical colours.
2.3.4
The Herschel guaranteed time extragalactic survey:
PACS Evolutionary Probe (PEP)
People involved at OAB: Gruppioni
The PACS Evolutionary Probe (PEP) is a Herschel guaranteed time
key programme survey of the extragalactic sky, aimed at studying
the restframe far-infrared emission of galaxies up to redshifts ∼ 3,
as a function of environment. The survey will shed new light on the
constituents of the cosmic IR background and their nature, as well as
on the co-evolution of AGN and starbursts.
The PEP survey is driven by science goals addressing a number of
key open topics in galaxy evolution, which are outlined in the following
paragraphs.
What are the constituents of the Cosmic Infrared Background
(CIB)? One of the most direct results of deep PACS surveys will be
the resolution of the majority of the CIB into individual well detected
sources, at wavelengths near the CIB peak which contains most of the
energy and represents most of the cosmic star formation and metal
production, modulo the contribution of AGN. We expect to resolve
about 80%, 85% and 55% of the CIB due to galaxies at 75, 110, and
170 microns into individual 5-σ detected sources for the blank field
surveys. These fractions clearly depend on the faint number counts
at these wavelengths that only PACS can measure. Using the wealth
of multi-wavelength data already existing in the chosen well-studied
fields and techniques like SED fitting, as well as dedicated follow up
projects, we will be able to determine the physical nature of these objects, for example redshifts, luminosities, morphologies, masses, star
formation histories, and the role of AGN.
How does the star formation rate density and galaxy luminosity function evolve? The PEP survey will sample the critical farinfrared peak of star forming galaxy SEDs and will probe a large part
63
of the infrared luminosity function, down to luminosities of ∼ 1011 L
at redshift 1 and < 1012 L at redshift 2. This will enable a detailed
study of the evolution of the infrared luminosity function with redshift,
expanding on the results based on mid-infrared or submm surveys and
suppressing the associated uncertainties due to extrapolation of the IR
SEDs. The multi-wavelength coverage of the PEP fields will ensure a
robust estimate of photometric stellar masses, hence extending studies of the evolution of the specific star formation rate to the currently
missing obscured component of star formation.
What is the relation of far-infrared emission and environment
at intermediate redshift? What are the clustering properties
of infrared galaxies? The far-infrared emission is a calorimeter of
star formation for many types of galaxies, hence a large far-infrared
survey is a unique method to determine in which environments most
of the cosmic star formation occurred. In the local universe, luminous infrared galaxies mostly avoid the dense cluster environments in
which star formation has already declined. Optical studies and observed overdensities of submm sources around massive high redshift
objects (e.g. Ivison et al. 2000, Stevens 2003) already indicate that
this must change dramatically at high redshift, towards a strong clustering of infrared sources in dense regions. First results from Spitzer
surveys indicate that the reversal of the star formation-density relation indeed happens at z ≤ 1, at lower redshift than suggested by
current hierarchical models: a domain well sampled by PACS surveys
(Elbaz et al. 2007).
What is the role of AGN and how do they co-evolve with
galaxies? The close relation in the local universe between black hole
mass and bulge properties calls for studies of how AGN and galaxies co-evolve. According to recent models, feedback by AGN is also
central to terminating star formation in massive galaxies (Croton et
al. 2006). Both locally and at high redshift, many infrared galaxies
host both star formation and an active nucleus (e.g. Genzel et al.
1998, Alexander et al. 2003, 2005, Valiante et al. 2007). The PEP
survey will shed new light on this relation, as a function of redshift
and of galaxy properties, by studying for significant AGN samples the
rest frame far-infrared emission and its relation to the AGN properties. PEP will also probe the far-infrared emission of fully obscured
AGN not detected in X-ray surveys. In combination with SPIRE,
64
and Spitzer 24-µm data, PEP/PACS will determine the overall SEDs
of active galaxies, including AGN mid-IR emission. Hence PEP will
quantify the total energetics of the obscured phases in black-hole evolution, as well as of the associated star formation.
What is the infrared emission and total energetics of known
galaxy populations? What is the role of extinction? Optical/
near-infrared techniques efficiently identify large samples of galaxies
at redshifts of 1 and above. The significance of these populations often
depends on fairly uncertain extinction corrections in the estimation of
star formation rates. By directly probing the rest-frame far-infrared
emission of objects classes like z ∼ 1 [OII] emitters, EROs, J-K selected distant red galaxies, BX/BM, BzK, (lensed) LBGs we will be
able to measure their actual star formation rates. Comparison of these
measurements with extrapolations from shorter wavelengths will determine the regimes where these extrapolations hold or fail, and determine full UV plus IR contributions to cosmic star-formation.
This research is in collaboration with MPE-Garching, CEA-Saclay,
IAC and HSC. Other PEP members in Bologna are A. Cimatti and
F. Pozzi (UniBo) and in Italy P. Andreani (ESO), R. Maiolino and
A. Grazian (INAF-OAR), G. Rodighiero (UniPd), M. Nonino (OATS).
2.3.5
The HELLAS2XMM survey
People involved at OAB: Ciliegi, Civano, Comastri, Mignoli, Pozzetti,
Zamorani.
This research is in collaboration with C. Vignali (Astronomy Dept.,
Univ. of Bologna)
The HELLAS2XMM survey is a large national project, started in 2001,
carried out in collaboration with several Italian institutes (INAFArcetri and Rome Observatories, INAF-IASF Milano and Univ. of
Rome 3). The survey strategy is complementary to deep pencil beam
surveys and was conceived to sample a different portion of the luminosity–redshift plane, with the aim to obtain a robust estimate of the
luminosity function and evolution of X-ray selected AGN. The final
catalogue (Cocchia et al. 2007) includes ≈ 230 sources detected in the
65
2–10 keV band over ∼ 1.4 deg2 (i.e., 10 XMM-Newton fields), above
a limiting flux of ∼ 10−14 erg cm−2 s−1 . Spectroscopic identifications
are available for ≈ 70% of the sample. Dedicated follow–up multiwavelength observations, over different portions of the electromagnetic spectrum, were also obtained for carefully selected sub-samples
of sources.
The project is close to its natural end and has produced over the
last few years 12 refereed papers (one or two additional papers are
likely to be submitted in the near future) plus a large number of conference proceedings papers and invited talks.
The most important results from the HELLAS2XMM project in
2007 can be summarized as follows:
• A fraction of the order of 10–15% of hard X-ray selected sources
in the HELLAS2XMM survey (as well as in other surveys) are
characterized by high X-ray to optical flux ratios (X/O), faint
optical counterparts and red (R − K) optical to infrared colors.
Deep photometric and spectroscopic observations have shown
that the large majority of them are obscured AGN at z ∼ 1–
2. Thanks to an approved Guest Observer programme on the
Spitzer Observatory (PI A. Comastri) MIPS and IRAC photometry was available for a sample of 19 sources. Nine of them have
extended near-infrared (K band) morphologies well fitted by an
early type galaxy profile, while the remaining 10 are pointlike.
Pointlike sources have less extreme X/O and R − K colors than
those with extended morphology. All of them are spectroscopically identified as narrow line AGN at 0.7 < z < 2. The broad
band SED from optical to 24µm were fitted with the Fritz et
al. (2006) torus model adding, when required, the host galaxy
starlight emission. The free parameters of the model include the
torus size, the covering factor and the optical depth along the
line of sight, the radial and azimuthal dust spatial distribution.
The results (which are the subject of a paper in preparation)
indicate that, on average, the best fit is obtained for line of
sights close to the equatorial plane and for relatively low optical depths. The bolometric corrections (defined as the ratio
between the bolometric and the 2–10 keV luminosity) show a
large spread in the range 10 to 100. The Black Hole masses and
the Eddington ratio were estimated using the MBH -LK relation.
The results indicate that these obscured AGN are powered by
66
massive Black Holes in massive galaxies with relatively low (<
0.1) Eddington ratios.
• One of the most intriguing findings of the HELLAS2XMM survey is the detection of a few sources characterized by X-ray
luminosities typical of AGN (in the range 1042 –1043 erg s−1 ),
hosted by passive galaxies with an early type morphology without any obvious sign of nuclear activity in their optical spectra. These sources have been named XBONGs, X-ray Bright
Optically Normal Galaxies. In 2007 the paper reporting the results of a detailed multiwavelength and morphological analysis
of four XBONG was published (Civano et al. 2007). A weak
nuclear source is unambiguously detected in two of them. The
accretion rate (about 0.001 in Eddington units) estimated from
the MBH -Mbulge relation would be consistent with a Radiative
Inefficient Accretion Flow (RIAF) solution. Alternatively the
nuclear source is not powerful enough to efficiently ionize the
circumnuclear gas and produce emission lines. The thermal Xray spectrum of another source coupled with the lack of nuclear
emission indicates that the X-ray luminosity may be ascribed to
the galaxy itself and/or to diffuse emission from a poor group
of galaxies. The morphological analysis of the fourth XBONG
leads to inconclusive results due to the presence of two close optical nuclei in a common envolope. The X-ray luminosity may be
due to both of them and is unresolved by XMM. It is concluded
that only a fraction of sources classified as XBONG are powered
by accretion onto SMBH.
2.3.6
The X-ray background in the Chandra and XMM era
People involved at OAB: Gilli, Comastri.
This research is in collaboration with G. Hasinger (MPE-Garching).
A detailed and self-consistent modeling of the cosmic X-ray background (XRB) based on the most up-to-date X-ray luminosity functions (XLF) and evolution of AGN was published by Gilli, Comastri
& Hasinger (2007). A web based tool for computing the contribution
to the XRB spectrum and the logN-logS in different bands for AGN in
any redshift, luminosity or NH bin was developed, tested and released
to the community at the address:
67
Figure 18: Upper panel: The cosmic XRB spectrum as observed by
different instruments (datapoints) and the predicted contribution of
unabsorbed AGN (red line), moderately obscured AGN (blue line),
and sum of the two (magenta line). The most relevant XRB measurements are explained on the top left. Also shown are the XRB fractions
resolved in different deep X-ray fields (red diamonds, cyan crosses and
black crosses, gold datapoints). For a full description of the symbols
see Gilli, Comastri & Hasinger (2007). Lower panel: same as the
previous panel but including also the contribution of Compton-thick
AGN (black line).
68
http://www.bo.astro.it/~gilli/xrb.html;
http://www.bo.astro.it/~gilli/counts.html
(see also Fig. 18). The tool was very well received and used by several
colleagues in scientific papers and in observational proposals.
2.3.7
The COSMOS project
COSMOS is a pan-chromatic imaging and spectroscopic survey of a
1.4 × 1.4 deg2 field designed to study the co-evolution of galaxies and
their central black holes out to high redshifts, placing them in the
context of the large scale structure in which they reside and with high
resolution morphological information. This global multiwavelength
collaboration is built around an HST Treasury programme (PI: Scoville), entailing the largest ever allocation of HST telescope time (590
orbits for ACS I band imaging of the full field) integrated by numerous observational campaigns at all wavelengths (from radio to X-ray).
A large number of OAB scientists are deeply involved in the analysis
and interpretation of several datasets and in particular in the projects
listed below:
The XMM-COSMOS and Chandra-COSMOS surveys
People involved at OAB: Civano, Comastri, Gilli, Zamorani.
This research is in collaboration with C. Vignali (Astronomy Dept.,
Univ. of Bologna), M. Brusa (MPE-Garching) and the XMM-COSMOS
and C-COSMOS teams.
Because of their superb efficiency in localizing and identifying AGN
and distant clusters of galaxies, X-ray observations are a crucial element of the COSMOS survey. The 2 deg2 COSMOS field was observed
for a total of 1.4 Msec (25 pointings repeated twice) with XMMNewton. The combination of the XMM-Newton X-ray throughput,
the unprecedented solid angle coverage of optical and near infrared
imaging photometry, optical spectroscopy, mid- to far-infrared Spitzer
observations and deep radio data makes this field the best suited to
probe for the first time 3D clustering in the X-ray band and detect
sufficient numbers of high-redshift AGN to probe the growth phase of
black holes. The first results of the XMM–COSMOS survey have been
published on the Astrophysical Journal Special Issue (Vol. 172; 2007
69
September 1).
During 2007 the master catalogues of both X-ray sources and optical counterparts (including multiwavelength identification and redshift information when available) were completed. The papers describing the catalogues are either submitted or in an advanced state
of preparation. The final number of pointlike sources in the entire
XMM-COSMOS field is 1822. Thanks to the vigorous programmes of
optical spectroscopy carried out with VIMOS at VLT and IMACS at
the Magellan Telescopes, about 650 X-ray sources were spectroscopically identified. Further spectroscopic campaigns are undergoing at
VLT and Keck, to increase the number of spectroscopic redshifts. The
large number of X-ray sources and the associated multiwavelength information have been, and are being, exploited for a variety of scientific
projects including: the X-ray spectral analysis, the calculation of the
correlation function (both angular and spatial), the Spectral Energy
Distribution (SED) of X-ray sources and in particular of obscured
AGN over a wide range of redshifts and luminosities, the estimate of
the space density of high redshift (z > 3) QSO. The XMM data are
also being extensively used to constrain the role of SMBH activity in
galaxy evolution.
The central square degree of the COSMOS field was also observed
by Chandra for a total integration time of 1.8 Msec (the largest Chandra programme ever approved). The observing strategy was designed
to reach a sensitivity of about 2×10−16 erg cm−2 s−1 (more than a factor ∼ 3 deeper than XMM) with an excellent (< 2 arcsec HPD over the
entire field) spatial resolution. The observations were performed in the
period November 2006–May 2007. In 2007 a large fraction of resources
(especially in terms of manpower) was dedicated to the analysis of the
Chandra data. A major effort was the setup and the testing of a dedicated procedure for the detection of Chandra sources. A multistep
approach was developed, making use of the expertise acquired in the
analysis of XMM data and of dedicated software for the Chandra data.
Extensive and detailed simulations, reproducing the tiling of the real
observations, were realized and analyzed with the same techniques.
The almost final catalogue contains 1760 independent X-ray sources
down to a limiting 0.5–2 keV flux of about 2 × 10−16 erg cm−2 s−1 ,
closely matching expectations. About half of the Chandra sources are
associated to XMM ones. The total number of X-ray sources in the
XMM and Chandra surveys is of the order 3000, making COSMOS a
unique database for a wide variety of statistical studies.
70
The most important scientific projects that are carried out with
Chandra concern the evolution of galaxies and AGN within their full
environmental context, probing up to 20 Mpc scales at z ∼ 1. In
particular it will be possible to study the influence of the environment in triggering AGN activity, to probe galaxy interactions, and to
study the galaxy activity in groups and clusters. The excellent spatial
resolution is also well suited for statistical studies (with the stacking technique) of various classes of sources not individually detected
(starforming galaxies, Lyman Break galaxies etc.). The stacking technique was successfully applied to search for heavily obscured, possibly
Compton Thick AGN, selected on the basis of extreme mid-infrared
(MIPS 24 µm), near infrared (K band) and optical (R band) colors.
The zCOSMOS survey
People involved at OAB: Bardelli, Bolzonella, Cappi, Ciliegi, Coppa,
Lamareille, Mignoli, Pozzetti, Zamorani, Zucca.
The zCOSMOS project (600 hours with VIMOS over four semesters
approved in 2004 and started on April 2005; P.I. S. Lilly) is a major
treasury redshift survey in the COSMOS field. This project, in which
there is a significant involvement of researchers of the Bologna Observatory, consists of two parallel surveys: (1) the bright survey, aiming at
observing ∼ 20 000 magnitude-selected galaxies with IAB ≤ 22.5 and
0.1 ≤ z ≤ 1.2 over 1.7 deg2 ; (2) the deep survey, with approximately
10 000 galaxies selected through colour-selection criteria expected to
be at 1.4 < z < 3.0, within the central 1 deg2 . At the end of the 2006
observing season, we have observed approximately 10 000 bright spectra. All of them have been reduced, with a success rate in redshift
measurement of ∼ 92%, by the zCOSMOS collaboration, involving,
besides the Bologna group, other institutes in Zurich, Milano, Marseille, Toulouse and Garching. Based on the current rate of execution,
we project a completion of zCOSMOS-bright observations by 2008
July and of the zCOSMOS-deep observations a year later.
The main goal of the spectroscopic survey zCOSMOS is to characterize galactic environments throughout the COSMOS volume out
to redshifts z ∼ 3. Some of the main topics that will be addressed
to understand the evolution of galactic systems are: (1) the study of
large-scale structures by means of the measure of the density field,
the evolution of correlation functions, the selection of a catalogue of
71
groups, (2) the study of diagnostics derived from spectra to determine
star-formation rates of galaxies, active galactic nuclei (AGN) classification, reddening by dust, stellar population ages, and metallicities,
(3) the description of the galaxy population by means of various distribution functions, such as the Luminosity and Galaxy Stellar Mass
Functions, as a function of different galaxy types and environments,
(4) the extension of the previous studies complementing the spectroscopic sample with the excellent photometric redshifts available in this
field.
The analysis of the reduced spectroscopic data is currently in
progress. Bologna is mainly involved in the study of the evolution
of stellar mass and luminosity functions of the bright spectroscopic
catalogue divided in photometric and spectroscopic types, morphology and environment, as well as in the classification of galaxy types
from the spectral analysis.
Using the spectroscopic 10k sample, we have estimated the stellar
mass content of each galaxy. Stellar masses were derived through SED
fitting of the extensive and deep available multi-band photometry from
the U to the Mid-IR bands at redshift fixed to zspec . In Bologna we
have also performed a comparison among the different methods to
estimate stellar masses inside the zCOSMOS collaboration.
We have derived the galaxy stellar Mass Function (MF) from z ∼ 0
to z = 1.2, for the global population and for 2 broad classes, corresponding qualitatively to early and late type galaxies respectively,
defined by their photometric multiband spectral energy distribution
(SED), morphological and/or spectral classification, or by their SSFR,
and in different environments (Pozzetti et al., Bolzonella et al. in
preparation). Preliminary results show a galaxy bimodality in the
global MF in the range 0.1 < z < 0.5, explained by the different
populations of late/early type galaxies at different masses. We find
an increase with cosmic time of the fraction and number densities of
early-type galaxies with log M < 11 and a negligible evolution for
the most massive ETGs. Conversely, the number density of low mass
(log M < 10.3) late type galaxies increases with cosmic time (at least
at z < 0.5), while above this mass they remain almost constant in
number density from z ∼ 1. This behaviour can be interpreted as a
combination of a transformation with cosmic time from blue active spiral galaxies of intermediate mass into red passive early and spheroidal
galaxies, and a continuous replacement by blue active low-mass spirals
growing in stellar mass.
72
The environmental effect in the MF is visible both in its shape, with
the afore mentioned bimodality more evident in denser regions, and in
the population of galaxies inhabiting the extreme environments: the
transformation of intermediate mass late type galaxies, contributing
the most of the MFs in low density regions, into early type galaxies,
which dominate the MF in dense environments, seems to act more
rapidly in dense regions from z ∼ 1 to z ∼ 0.1.
A similar approach is adopted to compute Luminosity Functions
(LF) and to study their evolution as a function of the spectrophotometric and morphological types and of the environment. We find
that late type galaxies are the main responsible of the LF evolution
with redshift. In particular, at low redshifts (z = [0.1 − 0.3]) elliptical galaxies dominate the bright end of the LF, while spiral galaxies
dominate the faint end; irregular galaxies increase their contribution
at the lowest luminosities. At intermediate redshifts (z = [0.3 − 0.8])
spiral galaxies increase their luminosities and their contribution to the
bright end of the LF is similar to that of elliptical galaxies. At high
redshifts (z > 0.8) irregular galaxies strongly evolve and therefore
the three morphological types almost equally contribute to the total
LF. Concerning the environment, at low redshift galaxies in overdense
regions have a brighter and flatter LF than galaxies in underdense
regions. This difference decreases with increasing redshift.
The node of Bologna has also led the work on the definition and
first application of a galaxy classification cube which makes use of
Cosmos data (ACS morphology and Subaru photometry) and zCOSMOS spectra obtained in P75, the 1K bright spectroscopic sample,
using directly observable parameters such as emission-line equivalent
widths and continuum indices, observed photometric colours instead of
synthetic colours and a parametric-based morphological classification.
The principal axis of the galaxy classification cube is built following the spectral classification scheme adopted by Mignoli et al. (2005)
in the K20 survey. This classification, which uses only the equivalent width of the [OII]3727Å line and the 4000Å break index (D4000),
allows to define three main classes: 1) red quiescent galaxies, which
show a large D4000 value and a faint, or undetected, [OII] emission
line; 2) blue star-forming galaxies, with small D4000 values and intense emission lines; 3) a small group of objects, which show emission
lines but a red stellar continuum forms what we call the intermediate
class of galaxies. This galaxy spectroscopic bimodality is naturally
linked to the colour bimodality observed in the galaxy population (see
73
e.g. Balogh et al. 2004). Indeed, the observed B − z colour shows
the best behaviour in separating red quiescent from blue starforming
galaxies. The correspondence between colour and spectral classification is very good, with about 90% of the zCOSMOS bright galaxies
having concordant classifications. The third axis of the classification
cube is based on the HST/ACS morphological classification, as performed by the Zurich Estimator of Structural Types (ZEST ; Scarlata
et al. 2007). The third parameter (morphology) is less well correlated
with the first two: in fact a good correlation between the spectral classification and that based on morphological analysis (early-/late-type
galaxies) is achieved only after partially complementing the morphological classification with additional colour information.
This analysis of the whole classification cube indicates that the
galaxy bimodality already discovered in single parameters holds also
in 3D: about 85% of the galaxies show a fully concordant classification, being either quiescent, red, bulge-dominated galaxies (∼ 20%)
or star-forming, blue, disk-dominated galaxies (∼ 65%). These results imply that the galaxy bimodality is a consistent behaviour both
in morphology, colour and dominant stellar population, at least out
to z ∼ 1. The application of the Classification Cube to the first 1K
zCOSMOS sample is now concluded (Mignoli et al. 2008, in press),
and we are currently exploring more sophisticated techniques (Principal Component Analysis, Grouping methods) to analyze the ten times
larger 10K sample and to investigate the nature of the galaxies that
violate the optical “3D concordance”.
The VLA-COSMOS survey
People involved at OAB: Ciliegi, Bardelli, Zamorani.
This work is carried out in collaboration with M. Bondi (INAF-IRA
Bologna), E. Schinnerer, V. Smolcic, K. Janke (Max Plank Institute,
Heidelberg, Germany), and C. Carilli (NRAO, Socorro, USA).
To match the typical resolution of optical-NIR ground-based data (∼ 1
arcsec), a deep radio survey was performed with the VLA in the Aarray configuration (which provides a resolution of about 2 arcsec at
1.4 GHz). A total of 240 hours in Array A and 24 hours in array C
was observed from October 2004 to August 2005. All these data were
analyzed and a mosaic map of 2 deg2 was obtained with a resolution
74
of ∼ 2 arcsec and a sensitivity of 10µJy/beam. A total of 3644 radio
sources were extracted down to a radio flux of 45µJy (Schinnerer et
al. 2006).
These VLA observations represent a fundamental contribution to
the COSMOS project and will provide definitive answers to a number
of key questions, including:
1. the secure identification of dust-obscured galaxies and their contribution to the cosmic star formation history;
2. the evolution of the FIR/radio correlation for star forming galaxies;
3. the evolution of radio-loud AGN as a function of environment;
4. the evolution of low luminosity radio AGN to high-z.
During 2007, we concluded the analysis of the COSMOS-VLA data
to determine the effect of bandwidth smearing, the incompleteness
produced by the noise bias and resolution bias, and to derive the
radio source counts at 1.4 GHz.
The effect of bandwidth smearing on the radio sources in the catalogue was quantified comparing the peak and total flux densities in the
final mosaic and in each of the individual pointings where the source
was closest to the centre of the field. We find that the peak flux densities in the original VLA-COSMOS Large Project catalogue have to
be divided by a factor of about 0.8 or 0.9, depending on the distance
from the mosaic centre. The completeness of the radio catalogue was
tested using samples of simulated radio sources with different angular
size distributions. These simulated sources were added to the radio
image and recovered using the same techniques used to produce the
radio catalogue. The fraction of missed sources as a function of the
total flux density is a direct measure of the incompleteness. Finally,
we derived the radio source counts down to 60 µJy with unprecedented
good statistics. A comparison with the findings of other surveys shows
good agreement in the flux density range 0.06–1 mJy, confirming the
upturn at 0.5 mJy and a possible decline of the source counts below
∼ 0.1 mJy. All results have been published in Bondi, Ciliegi et al.
2008.
Moreover, during 2007, the properties of the COSMOS-VLA sources
were analyzed using a newly developed optical color-based method to
75
separate star-forming (SF) from active galactic nucleus (AGN) galaxies at intermediate redshifts (z < 1.3). We classify the objects into
(1) star candidates, (2) quasi-stellar objects, (3) AGN, (4) SF, and
(5) high-redshift (z > 1.3) galaxies. We find that SF galaxies are not
the dominant population at sub-mJy flux levels, as previously often
assumed, but that they represent an approximately constant fraction
of 30–40% in the flux density range from ∼ 50 µJy to 0.7 mJy. In
summary, based on the entire VLA-COSMOS radio population at 20
cm, we find that the radio population at these flux densities is a mixture of roughly 30–40% of SF and 50–60% of AGN galaxies, with a
minor contribution (∼ 10%) of QSOs. The results of this work have
been published in Smolcic et al. 2008a.
Finally, making use of the above classification, we have derived the
cosmic star formation history out to z = 1.3 using a sample of ∼ 350
radio selected star forming galaxies. We have precisely measured the
high-luminosity end of the star forming galaxy luminosity function
(SFR > 100 solar mass/ year; equivalent to ULIRGs) out to z =
1.3, finding a somewhat slower evolution than previously derived from
mid-infrared data. We find that more stars are forming in luminous
starbursts at high redshift. We use extrapolations based on the local
radio galaxy luminosity function; assuming pure luminosity evolution,
we derive L∗ ∝ (1 + z)2.1 or L∗ ∝ (1 + z)2.1 , depending on the choice
of the local radio galaxy luminosity function. Thus, our radio-derived
results independently confirm the ∼ 1 order of magnitude decline in
the CSFH since z ∼ 1. A detailed description of these results is
reported in Smolcic et al. 2008b.
2.3.8
Radio surveys
The VIRMOS RADIO survey
People involved at OAB: Bardelli, Ciliegi, Zamorani, Zucca.
The 1 deg2 VVDS area was observed with the VLA at 1.4 GHz with
a resolution of ∼ 6 arcsec and a sensitivity of about 17 µJy/beam.
A total of 1054 radio sources were extracted with a flux greater than
∼ 80 µJy. While the main properties of the radio sources in the VVDS
field have been already published (Bondi et al. 2003, Ciliegi et al. 2005)
during 2007 we analyzed their luminosity function.
Galaxy properties and luminosity functions are estimated in an
76
unbiased way up to z ∼ 1.0 for radio loud and radio quiet early type
galaxies and late type galaxies. Radio loud late type galaxies show
significantly redder colors with respect to radio quiet objects of the
same class and this is an effect related to the radio emission (probably
the presence of dust). Moreover, we have estimated optical luminosity
functions, stellar masses and star formation rate distributions for radio sources, and compared them with those derived for a well defined
control sample, finding that the probability for a galaxy of being a
radio emitter significantly increases when these parameters have high
values. Radio loud early type galaxies show luminosity evolution in
their bivariate radio-optical luminosity function, due to an evolution
in the radio-optical ratio. The lack of evolution of the mass function
of radio loud early type galaxies means that no new AGN are formed
at redshift z < 1. On the contrary, radio loud late type objects show
a strong evolution, both in luminosity and in density, of the radio
luminosity function for z > 0.7. This evolution is the mirror of the
strong optical evolution of this class and no significant change of the
radio-optical ratio with redshift is required. With the knowledge of
the radio-optical ratio and of the optical and radio luminosity functions for late type galaxies, we show that it is possible to estimate the
star formation history of the Universe up to redshift z ∼ 1.5, using
the optical galaxies as tracers of the global radio emission (see Figure
19). A detailed description of the this work is reported in Bardelli et
al. (2008, A&A submitted).
The ATESP Survey
The ATESP catalogue contains about 3000 radio sources down to a
20cm flux limit of ∼ 0.4 mJy. The radio data (including new data at
5 GHz) are being used for various purposes:
i) determining the radio properties of ESP galaxies (e.g. the radio
luminosity function of various types of galaxies);
ii) deep radio source counts and optical identification of ATESP
sources. A subsample with data at both 1.4 and 5 GHz was studied in detail using deep UBVRIJK imaging from the ESO Deep Survey (Mignano et al. 2008, A&A, 477, 459). This resulted in a high
identification rate (78%) and reliable determinations of (photometric)
redshifts for the majority of sources.
iii) detailed optical studies of smaller selected areas: at present a
sample of about 70 objects, complete to I = 19.0, has been observed at
77
Figure 19: Red points are our estimate of the star formation density
evolution as a function of redshift. Black squares are the same quantity
as estimated by Tresse et al. (2007) without dust correction. Other
points and lines are values from the literature
78
ESO, and spectroscopic data are available for all objects. Spectroscopy
of part of the fainter objects has recently been carried out with the
VLT and the analysis of the spectra is in progress;
iv) obtain more insight in the accretion processes responsible for
the production of radio sources (in particular the FR I type sources
associated with early type galaxies). New ATCA (Australia Telescope
Compact Array) data at high radio frequencies (5, 8.4 and 20 GHz),
carried out in July 2007 and 2008, allow us to study the spectral index
behaviour at low (< 10 GHz) and high (> 10 GHz) frequencies. We
find that spectra with an upturn at high frequencies are very rare or
even absent among the sources associated with early type galaxies,
and thus appear to be almost exclusively found in quasar-like AGN.
A paper describing the high frequency observations is being prepared
for submission to A&A. Further radio observations are planned.
This work is done in collaboration with I. Prandoni and P. Parma
(INAF-IRA), L. Gregorini (University of Bologna), and R. Ricci and
R.D. Ekers (ATNF - Australia).
Bright galaxies from WENSS
People involved at OAB: de Ruiter, Stirpe.
The Westerbork Northern Sky Survey has mapped the sky (above
declination +30o ) at 325 MHz (and is complementary to the NVSS
survey at 20 cm made by the VLA). The overall catalogue contains
about 200000 radio sources with flux density above 15 mJy. Work is
in progress at the Bologna Observatory to extract from the WENSS
catalogue all radio sources associated with “bright” (i.e. mr < 16.5)
galaxies. An almost final list of about 3500 WENSS bright galaxies
is now available; a last check of this list is being done. Several spinoff programmes are in progress: a number of possible “dying” radio
sources (characterized by a steep radio spectral index) were selected
for further study with the VLA at different frequencies. The new
information on the radio structure and spectral index confirms that
two of the three sources are indeed fossile sources, while the third is a
fossile source in which the radio activity has restarted. A new sample
of candidate dying sources was presented in Parma et al. (2007, A&A,
470, 875). This work is done in collaboration with P. Parma and K.-H.
Mack (INAF-IRA), R. Fanti (University of Bologna), and M. Murgia
and F. Govoni (INAF-Cagliari). .
79
2.3.9
The SPACE/DUNE/EUCLID project
People involved at OAB: Zamorani, Mignoli, Pozzetti, Gruppioni, Comastri, Meneghetti.
In 2007, an intense activity was dedicated to the preparation of a proposal submitted to ESA in response to the call for the first planning
cycle of the Cosmic Vision 2015–2025 programme. The project, called
SPACE (SPectroscopic All-sky Cosmic Explorer, PI A. Cimatti, Astronomy Dept., Univ. of Bologna), was successful and pre-selected by
ESA in October 2007.
SPACE proposed to perform the first (almost) all-sky spectroscopic
survey of the Universe, taking spectra between 0.6 and 1.8µm, with a
spectral resolution R = 400 of more than half a billion galaxies down to
magnitudes AB = 23 with SNR = 5 per resolution element. SPACE
achieves its remarkable sensitivity, sky and wavelength coverage by
performing multi-slit near-IR spectroscopy in outer space and in slit
mode, thanks to the use of the current generation of MEMS devices.
By accurately (dz < 0.001) locating hundreds of millions of galaxies, SPACE will observe Baryonic Acoustic Oscillation patterns in the
Universe between 5 and 10 billion years ago, improving the figure of
merit for the knowledge of dark energy by more than an order of magnitude. SPACE will also perform a deep survey (AB = 26), targeting
2 million galaxies in the range 2 < z < 10, and a survey of a 1 degree strip centred on the galactic plane in integral field mode. The
datasets from the SPACE core and GO programmes will represent a
long lasting legacy that will be data mined for many years to come.
In 2008 the SPACE project was merged with the DUNE project.
The primary goal of DUNE, a wide-field space imager, was also the
study of dark energy and dark matter, mainly measuring the weak
lensing effect of large scale structures. The resulting merged project
(EUCLID), which includes both the spectroscopic (SPACE) and the
imaging (DUNE) capabilities, is currently in the phase A study. Part
of the work required to assess the capabilities of DUNE is being done
at OAB by the image simulation group.
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2.3.10
The reionisation of the Universe in quintessence cosmological models
People involved at OAB: Meneghetti
Recent observations of the CMB, of the IGM and of the Lyman-α
transmitted flux in the spectra of high redshift quasars suggest that
the Universe has been completely reionized between redshifts 6 and
10. During the reionisation epoch, the neutral gas produced at recombination is ionized by the UV radiation emitted by the first luminous
sources. In fact, reionisation is still a poorly understood process because of the unknown nature of the ionizing sources and of the complex physical mechanisms producing the radiation emission. Moreover, reionisation is expected to proceed differently in cosmological
scenarios with dynamical dark-energy.
In Crociani et al. (2007), we investigate the effects that a dynamic
dark energy component dominant in the universe at late epochs has on
reionization. We follow the evolution of HII regions with the analytic
approach of Furlanetto and Oh (2005) in two different universes for
which we assume the Peebles and Ratra (2003) and Brax and Martin (2000) quintessence models and we compare our results to the
LCDM scenario. We show that, for a fixed ionization efficiency, at
the same cosmological epoch the topology of bubbles is dominated
by high-mass objects and the characteristic size of the ionized regions
is slightly smaller than in the LCDM model, especially at the latest
stages of reionization, due to the higher recombination efficiency. As
a consequence, the bubbles’ ‘epoch of overlap’ occurs earlier than in
LCDM. Finally, we show how the different evolution of the HII regions affects the transmission of the high-z QSO spectra, reducing the
Lyman flux absorption at small optical depths.
2.4
2.4.1
Galaxy clusters and large-scale structure
Mass Reconstruction in Galaxy Clusters
People involved at OAB: Meneghetti, Ettori, Donnarumma
A large effort was dedicated to the study of gravitational lensing by
galaxy clusters. Thanks to their huge mass and concentration, these
cosmic structures are the most powerful lenses observable in the Universe. The lensing phenomena produced by them cover a broad range
81
of events, from the production of multiple images and arcs in the central regions (strong lensing), to the weak distortions of the shapes
of distant galaxies in the cluster outskirts (weak lensing). In both
in the strong and weak regimes, lensing allows us to trace the total
projected mass distribution in galaxy clusters. Combining this with
other observations, such as the X-ray emission by the hot gas filling
the intergalactic space, we can deduce important information about
the equilibrium state of galaxy clusters, their formation history, and
their role as cosmological probes.
We have investigated the topic of cluster mass reconstruction both
theoretically and observationally. From the observational point of
view, we have completed the combined strong-lensing and X-ray analysis of one of the most controversial clusters in the literature, MS2137.
In Donnarumma et al. (2008, submitted to MNRAS), we analysed
state of the art Chandra observations to recover the profiles of the
ICM properties and the total mass distribution. The notable strong
lensing features of MS2137.3 allow us, taking advantage of the lensing inversion code Lenstool, to reconstruct its projected mass in the
central regions with a good accuracy. We finally compare the results obtained with both methods. Our mass estimates for MS2137.3
are in agreement within the errors, leading to a mean, extrapolated
value of M200 ' 4.1 ± 0.4 × 1014 M . Some other studies, including
the reconstruction of other interesting clusters are currently on-going.
In particular, we are using strong lensing techniques to obtain a mass
model for the cluster A611, using the commissioning data of the newly
established Large Binocular Telescope.
In collaboration with scientists from the University of Heidelberg,
we have worked on the development of a code for non-parametric mass
reconstructions of clusters combining strong and weak lensing data.
Combinations of both effects promise to constrain density profiles of
galaxy clusters well, and thus to allow testing of the CDM expectation
on dark-matter halo density profiles. We have further developed an
algorithm recently proposed for this purpose by Cacciato et al. (2006).
It recovers a lensing potential optimally reproducing observations of
both strong- and weak-lensing effects by combining high resolution
in cluster cores with the larger-scale information in weak lensing. We
have then applied it to weak- and strong-lensing data of the cluster MS
2137 and obtain a parameter-free solution which is in good qualitative
agreement with our parametric study. The results of this analysis are
82
being published in a paper by Merten et al. (2008, submitted to A&A).
From the theoretical point of view, we have used the recently developed Skylens software (described below) to produce mock optical
observations of clusters obtained from N-body and hydrodynamical
simulations as lenses. The results of such simulations have been used
to test several reconstruction techniques. We have estimated that
currently used techniques measure the projected mass profiles of clusters with an accuracy better than ∼ 10%. We have then compared
the de-projected mass profiles to those of the simulated clusters, assuming spherical symmetry of the matter distributions. We find that
de-projected masses can be significantly off the true masses, due to the
tri-axiality of the clusters. In particular, in the cases of the strongest
lensing clusters, which are objects preferentially seen through their
major axis, the differences between true and observed mass can be
of order 200–300% in the strong-lensing region. Such mismatches between cluster mass estimates are frequent when comparing stronglensing and X-ray observations. The results of this study are being
published in a paper by Meneghetti et al. (2008, in preparation).
2.4.2
Cluster detections using SZ and X-ray
People involved at OAB: Meneghetti
In Pace et al. (2008), we calibrated the number density, completeness, reliability, and the lower mass limit of galaxy-cluster detections
through their thermal SZ signal and compare them to X-ray cluster
detections. The method used is the following. We simulated maps of
the thermal SZ effect and the X-ray emission from light cones constructed in a large, hydrodynamical, cosmological simulation volume,
including realistic noise contributions. The maps were convolved with
linear, optimised, single- and multi-band filters to identify local peaks
and their signal-to-noise ratios. The resulting peak catalogues were
then compared to the halo population in the simulation volume to
identify true and spurious detections. We find that multi-band filtering improves the statistics of SZ cluster detections considerably
compared to single-band filtering. Observations with the characteristics of ACT detect clusters with masses M > 6 − 9 × 1013 M /h, quite
independent of redshift, reach 50% completeness at ∼ 1014 M /h and
100% completeness at ∼ 2 × 1014 M /h. Samples are contaminated
83
by a few spurious detections, but only by a small percentage. This
is broadly comparable to X-ray cluster detections with XMM-Newton
with 100 ks exposure time in the soft band, except that the mass limit
for X-ray detections increases much more steeply with redshift than
for SZ detections. A comparison of true and filtered signals in the SZ
and X-ray maps confirms that the filters introduce at most a negligible
bias.
2.4.3
Gravitational Lensing
People involved at OAB: Meneghetti
Cosmological applications of strong lensing
The frequency of strong-lensing events is very sensitive to the geometry of the universe and to many properties of the lenses like their
dynamical state, their concentration and their abundances. All of
these are cosmology-dependent. Thus, the number of strong-lensing
events is a powerful cosmological indicator.
With the aim of better understanding the impact of several cluster
properties on lensing, in Meneghetti et al. (2007) we investigate how
ellipticity, asymmetries and substructures separately affect the ability of galaxy clusters to produce strong-lensing events, and how they
influence the arc morphologies and fluxes.
In Fedeli et al. (2008), we use semi-analytic modelling of the galaxycluster population and its strong lensing efficiency to explore how the
expected abundance of large gravitational arcs on the sky depends on
σ8 . Our models take all effects into account that have been shown to
affect strong cluster lensing substantially, in particular cluster asymmetry, substructure, merging, and variations in the central density
concentrations. We show that the optical depth for long and thin arcs
increases by approximately one order of magnitude when σ8 increases
from 0.7 to 0.9, owing to a constructive combination of several effects.
Models with high σ8 are also several orders of magnitude more efficient
in producing arcs at intermediate and high redshifts. Finally, we use
realistic source number counts to quantitatively predict the total number of arcs brighter than several magnitude limits in the R and I bands.
Image simulations
84
In lensing studies, noise is produced by the PSF, by charge diffusion
effects in the CCD images and by the intrinsic shapes of the background galaxies, and all these effects strongly influence the distortion
measurements. To cover this gap between theoretical studies of gravitational lensing and observations, we developed the code Skylens for
realistic simulations of optical observations. The code includes 1) most
of the instrumental types of noise, 2) noise caused by the sky backgrounds and foregrounds, 3) realistic description of the background
galaxies as obtained by shapelet decompositions of galaxies retrieved
from public archives 4) lensing effects by matter distributions obtained
from N-body and hydrodynamical simulations.
In Melchior, Meneghetti & Bartelmann (2007), we discussed the
applicability and reliability of the shapelet technique for scientific image analysis. We quantified the effects of non-orthogonality of sampled
shapelet basis functions and misestimation of shapelet parameters.
We performed the shapelet decomposition on artificial galaxy images
with underlying shapelet models and galaxy images from the GOODS
survey. We further extended the work by decomposing the ∼ 10000
galaxies observed in the Hubble-Ultra-Deep-Field.
The characteristics of our code are described in detail in Meneghetti
et al. (2008).
2.4.4
The MUSIC project
People involved at OAB: Cappi.
A. Cappi is involved in the MUSIC project (MUlti-wavelength Sample of Interacting Clusters), in collaboration with S. Maurogordato
(PI), C. Benoist, A. Bijaoui, C. Ferrari, E. Slezak (Observatoire de la
Côte d’Azur), Hervé Bourdin (Università di Roma), M. Arnaud and
J-L. Sauvageot (CEA/CEN, Saclay). This project is based on optical
observations (ESO 3.6m and VLT, CFHT) and on X-ray observations
with XMM-Newton and Chandra, while complementary radio observations are carried out in collaboration with Luigina Feretti (INAF-IRA
Bologna). We now have a database on clusters in different evolutionary phases, suited for a systematic statistical study and a quantitative
comparison with theoretical predictions.
Among the past published results we can mention A521, a complex,
relatively rich cluster at z ∼ 0.25, in the middle of two filamentary
structures (Maurogordato et al. 2000; Ferrari et al. 2003), and A3921,
85
for which we have shown that it is in the central phase of the merging
process, and that its population of star forming and post-starburst
galaxies appears to confirm the downsizing scenario (Ferrari et al.
2005).
Particularly remarkable is another Abell cluster, A2163, at a redshift z ∼ 0.2, which we observed with VIMOS at the VLT, obtaining
∼ 512 high resolution spectra with excellent signal to noise ratio; 357
of them are associated to the cluster. Photometric observations in 5
passbands with the WFI@ESO 2.2m telescope, have also been reduced.
A2163 is the hottest X-ray Abell cluster, with many gravitational arcs
and with one of the largest radio halos ever detected. In this work
we have identified the main components and merger directions and
estimated its dynamical mass, which is in good agreement with the
X-ray estimate (Maurogordato, Cappi, Ferrari et al. 2007).
A comparison of the optical results with X-ray data has also been
done in collaboration with H. Bourdin (Univ. of Rome), M.Arnaud
and J.-L. Sauvageot (Saclay).
An important aspect of the merging process on which we are focussing is how it can affect star formation in galaxies. Combining
photometric and spectroscopic information we are carrying out a more
detailed analysis, and we are investigating the star formation history
of A2163 in collaboration with Jarle Brinchman (Leiden).
2.4.5
Galaxy clusters in the CFHTLS
People involved at OAB: Cappi.
A. Cappi is also involved in an ongoing study of clusters detected in
the Canada French Hawaii Telescope Legacy Survey (CFHTLS), in
collaboration with C. Benoist, C. Ferrari, S. Maurogordato, F. Martel, E. Slezak (Observatoire de Nice), L. Olsen (Dark Cosmology Centre, Copenhagen, Denmark), C. Adami and A. Mazure (Laboratoire
d’Astrophysique de Marseille, France). The CFHTLS is a project of
the French community based on a large photometric survey carried
out with the wide field camera Megaprime. In particular, the Wide
Synoptic Survey consists of a photometric catalogue in five passbands
(u∗ g 0 r0 i0 z 0 ) complete to the magnitudine r0 = 25.7 on 172 deg2 . As
a first step of this project, at the Observatoire de la Côte d’Azur a
database has been implemented: this database includes the cluster catalogue obtained through the matched filter technique (Olsen, Benoist,
86
Cappi et al. 2007, 2008). From the analysis of these clusters photometric redshifts for member galaxies, profiles and luminosity functions
have been obtained. In the end, this catalogue should provide a cluster sample with a completeness limit in mass, in order to study cluster
evolution and to constrain the cosmological parameters.
2.4.6
A search for Relics and Halos in the redshift range
z = 0.2–0.4
People involved at OAB: Bardelli, Zucca
This work is carried out in collaboration with T. Venturi, G. Brunetti
(INAF–IRA Bologna), D. Dallacasa, R. Cassano (Astronomy Dept.,
Univ. of Bologna), P.Mazzotta (Rome University), P. Rao (Pune, India).
Cluster scale diffuse radio sources, known as radio halos (if located at
the cluster centre) and relics (if at the cluster periphery) are ∼ Mpc
regions of emission, with no optical identification and steep radio spectrum. Their origin is attributed to synchrotron radiation from relativistic electrons mixed with the thermal plasma in the ICM, and
accelerated in large scale magnetic fields. Theoretical works have
shown that merger-driven turbulence and/or shocks may be able to
(re-)accelerate electrons in the ICM producing the radio emission from
halos and relics (e.g. Brunetti 2004, JKAS, 37, 493) and predicted the
evolution of halos with redshifts. Hence it is important to investigate in detail the cluster merger phenomenon, in order to connect the
physics of mergers to the presence of a halo and/or a relic. Such an
investigation must be carried out through i) the statistical analysis of
a large sample of clusters, in order to derive a global understanding of
the halo/relic - merger connection and to test the predictions of the
theoretical models and ii) the multifrequency analysis of individual
merging clusters with high sensitivity observations in the radio, X-ray
and optical bands in oreder to estimate the energy input coming from
the merging.
The 610 MHz GMRT Radio Halo Survey (Venturi et al. 2007,
A&A, 463, 937; Venturi et al. 2008 A&A 484, 327) was carried out to
search for new halos and relics in galaxy clusters with 0.2 < z < 0.4,
and to compare the fraction of massive clusters hosting a radio halo
in this redshift range with the predictions of the theoretical model
87
for the origin of these sources in the same z interval. A statistical
sample of 50 clusters was selected from the REFLEX and eBCS Xray catalogues, and GMRT 610 MHz observations were perfomed for
34 sources with no radio information available in the literature. We
found two new giant radio halos in A209 and RXCJ2003.5−2323, and
exceptional system of two relics and one halo in RXCJ1314−2515 and
a relic in A521 (Giacintucci et al. 2006, New Astronomy, 11, 437).
Moreover, we detected a diffuse peripheral source of unclear nature in A781, a core-halo source in Z7160, a candidate radio halo in
A1682 and suspect central emission in Z2661. Including information
from the literature, a total of 10 clusters in the sample host a radio
halo. A very important result of our work is that 25 out of the 34
clusters observed with the GMRT do not host extended central emission at the sensitivity level of our observations, and for 20 of them
firm upper limits to the radio power of a giant radio halo were derived. The GMRT Radio Halo Survey shows that radio halos are not
common, and our findings on the fraction of giant radio halos in massive clusters are consistent with the statistical expectations based on
the re-acceleration model. Our results favour primary to secondary
electron models (see also Cassano et al. 2008, A&A 480, 687).
Regarding A521 (see Fig. 20) we performed a detailed spectral
analysis based on the integrated radio spectrum between 235 MHz
and 4.9 GHz, and on the spectral index image in the frequency range
327–610 MHz (Giacintucci et al. 2008, A&A 486 347). The integrated
spectrum of the relic is consistent with a single power law; the spectral
index image shows a clear trend of steepening going from the outer
portion of the relic toward the cluster centre. Our results are consistent
with acceleration of relativistic electrons by a shock in the intracluster
medium. This scenario is supported by our detection of an X-ray
surface brightness edge coincident with the outer border of the radio
relic. This edge is probably a shock front.
2.4.7
Interaction between thermal intra-cluster medium and
relativistic plasma in cooling flow clusters of galaxies
People involved at OAB: Gitti.
During 2007 we continued the study of the connection between thermal
and non-thermal emission from the Intra-Cluster Medium (ICM) in a
sample of galaxy clusters that are likely to host diffuse radio emission
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Figure 20: Left panel: smoothed Chandra image of A521 in the 0.5–4
keV energy band. Right panel: same image as left panel with overlaid
GMRT 610 MHz contours of the A521 field. The resolution of the
radio image is 13.100 × 8.100 , PA 56◦ . Contour levels are spaced by a
factor 2 starting from 0.2 mJy b−1
usually classified as a radio mini-halo. Our main goal is to understand
the link between thermal ICM and relativistic plasma in cooling flow
clusters by means of X-ray and radio observations.
After studying the galaxy cluster which hosts the most energetic
AGN outburst currently known, MS0735+7421 (Gitti et al. 2007a,
ApJ, 660, 1118), and the most X-ray luminous cluster RX J1347.5−1145
(Gitti et al. 2007b, A&A, 470, L25 ; Gitti et al. 2007c, A&A, 472, 383),
we have now undertaken the analysis of the other galaxy cluster in our
sample, RBS 797. In particular, we have analyzed new radio data obtained at 1.4 GHz with the VLA in C array and produced a combined
map with resolution ∼ 8 arcsec by using also the existing data in
A and B array. The total flux density of the source is ∼ 23 mJy.
By subtracting the flux detected in A array, we confirm the presence
of extended radio emission on large-scale (radius ∼ 100 kpc), with
flux density ∼ 5 mJy. We are in the process of analyzing proprietary
Chandra data of RBS 797 in order to study the interaction of the radio
source with the thermal ICM in this cluster (Gitti et al., in preparation). At the same time, the analysis of X-ray observations of the
giant cavity clusters Hercules A (proprietary XMM-Newton data) and
Hydra A (archival Chandra data) is being carried out in collaboration
89
with the Harvard-Smithsonian Center for Astrophysics.
We have also studied the statistical properties of radio mini-halos
with respect to giant radio halos in order to investigate the origin of
these extended radio sources and discuss the basic physical differences
between them (Cassano, Gitti, & Brunetti 2008, A&A, 486, L31). In
particular, we performed a morphological comparison between giant
radio halos and radio mini-halos in galaxy clusters based on radio–
X-ray luminosity, P1.4 -LX , and radio luminosity-size, P1.4 -RH , correlations. We found evidence that, similarly to giant halos, P1.4 -LX and
P1.4 -RH trends may exist also for mini-halos: mini-halo clusters share
the same region of giant halo clusters in the (P1.4 , LX ) plane, whereas
they are clearly separated in the (P1.4 , RH ) plane. The synchrotron
emissivity of mini-halos is found to be more than 50 times larger than
that of giant halos, implying a very efficient process for their origins.
By assuming a scenario of sporadic turbulent particle re-acceleration
for both giant and mini halos, we argue that, regardless of the origin of the turbulence, a more efficient source of injection of particles
is required in mini-halos, and this may result from the central radio
galaxy or from proton-proton collisions in the dense cool core regions.
As a complementary part of this project, in collaboration with the
Innsbruck University we have investigated the relation between the
X-ray properties and Faraday Rotation measures of the cluster Abell
514, with the aim to study the connection of magnetic fields and the
ICM (Weratschnig, Gitti, Schindler, & Dolag 2008, A&A in press).
By analyzing proprietary XMM-Newton data, we studied the overall
cluster properties such as temperature and metallicity distribution
with high accuracy. This allowed us to investigate in detail the special
morphology and complex dynamics of this cluster. In particular, the
substructures seen in the X-ray image (see figure on page 47) as well
as in the temperature and abundance distribution indicate that the
cluster is in an ongoing merging phase. By comparing our X-ray data
with radio measurements taken from the literature, we found that
Abell 514 confirms the observed relation between the X-ray luminosity
and the sigma of the Rotation Measure.
2.4.8
Properties of cooling cores in X-ray galaxy clusters
People involved at OAB: Ettori.
To define a framework for the formation and evolution of the cool90
ing cores in X-ray galaxy clusters, in Ettori & Brighenti (2008) we
use time-dependent 1D hydrodynamical equations to study how the
physical properties of the inner regions change as a function of the
cosmic time under the action of radiative cooling and gravity only.
We follow the evolution of the cooling radius and of the profiles of
the gas density, temperature and surface brightness. We show that
the behaviour of the inner slopes of the gas temperature and density
profiles are the most sensitive and unambiguous tracers of an evolving
cooling core. Their values after 10 Gyrs of radiative losses, Tgas ∝ r0.4
and ngas ∝ r−1.2 , are in remarkable agreement with the observational
constraints available for nearby X-ray luminous cooling core clusters.
Because our simulations do not consider any AGN heating, they imply
that the feedback process does not greatly alter the gas density and
temperature profiles as generated by radiative cooling alone.
In Santos et al. (2008), we investigate the detection of Cool Cores
(CCs) in the distant galaxy cluster population, with the purpose of
measuring the CC fraction out to redshifts 0.7 ≤ z < 1.4. Using a
sample of nearby clusters spanning a wide range of morphologies, we
define criteria to characterize cool cores, which are applicable to the
high redshift sample. We measure the surface brightness concentration, cSB , as the ratio between the peak and the diffuse emission. To
verify that this is an unbiased parameter as a function of redshift,
we developed a model-independent “cloning” technique to simulate
the nearby clusters as they would appear at the same redshifts and
luminosities as those in the distant sample. A more physical parameterization of CC presence is obtained by computing the cooling time
at a radius of 20 kpc from the cluster centre. The distribution of cSB
and the stacked radial profiles of the low-z sample show 3 degrees of
SB cuspiness: non-CC, moderate and strong CC. The same analysis
applied to the high-z clusters reveals two regimes: non-CC and moderate CC. The cooling time distribution corroborates this result by
showing a strong negative correlation with cSB . Our analysis indicates a significant fraction of distant clusters harboring a moderate
CC out to z = 1.4, similar to those found in the local sample. The
absence of strong cooling which we report is likely to be linked with
a higher merger rate expected at redshift z > 0.7, and should also be
related with the shorter age of distant clusters, implying less time to
develop a cool core.
This work is carried out in collaboration with F. Brighenti (Univ.
of Bologna), S. Borgani (Univ. of Trieste), P. Rosati (ESO), J. Santos
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(ESO, INAF-Trieste Obs.), P. Tozzi (INAF-Trieste Obs.).
2.4.9
Metal abundance of the Intracluster Medium
People involved at OAB: Ettori.
The baryonic content of galaxy clusters is about 15% of the total mass
and is distributed among a hot X-ray emitting phase and a cold component mostly traced by stars. Such a cold component is only 10% of
the total baryons and is responsible for the metal enrichment through
star formation activity. The ICM is a high-temperature optically thin
plasma in hydrostatic equilibrium. Its emission is well modeled by a
thermal bremsstrahlung continuum plus characteristic emission lines
that depend directly upon the ion abundances, i.e., assuming a collisional ionization equilibrium, on the absolute element abundance and
the plasma temperature. Due to these simple properties, the X-ray
determination of metal abundances in the ICM is physically robust
and reliable. For reference, the cluster plasma with solar abundance
contains 74% of hydrogen in mass, 25% of helium and about 1.2% of
heavier elements.
To understand how and when the metals accumulate in the intracluster medium, Ettori (2005, 2007) uses models of the rates of type
Ia (including the recently suggested existence of two populations of
progenitors) and Core Collapse Supernovae to describe the enrichment
history of the cluster plasma. These rates provide a good match to (i)
the local abundance ratios, (ii) the negative evolution of the cluster
metallicity, and (iii) the overall production of Fe, that at z = 0 has
been released from SNe Ia by more than 60% (see Fig. 21).
In Rasia et al. (2008), we study the systematics affecting the
intra-cluster medium metallicity measurements through the analysis
of the faked X-ray observations of numerically simulated galaxy clusters (Fig. 21), finding that i) the Iron is recovered with high accuracy
for both hot (T > 3 keV) and cold (T < 2 keV) systems; at intermediate temperatures, however, we find a systematic overestimate which
depends on the number counts; ii) Oxygen is well recovered in cold
clusters, while in hot systems the X-ray measurement may overestimate the true value by a factor up to 2–3; iii) The measurement of
Magnesium is always difficult because of its weakness; despite this,
for cold systems (i.e. with T < 2 keV) we do not find any systematic
behavior, while for very hot systems (i.e. with T > 5 keV) the spec92
Figure 21: (Upper panel) Observed distribution of the metal abundance (diamonds; the error on the mean and the relative dispersion
are indicated) from Balestra et al. (2006) and theoretical predictions
from Ettori (2005, 2007). (Lower panel)) Iron and Oxygen distribution maps in four simulated clusters (Rasia et al. 2007).
93
troscopic measurement may strongly overestimate the true value up
to a factor of 4; iv) Silicon is well recovered for all the clusters in our
sample.
The distribution of the metal abundance as a function of (i) redshift
and (ii) gas temperature for a sample of 56 galaxy clusters at z >
0.3 and with Tgas between 3 and 15 keV observed with Chandra is
presented in Balestra, Tozzi, Ettori et al. (2007; see Fig. 21). We find
that the Iron abundance measured within (0.15–0.3)Rvir in clusters
below 5 keV is, on average, a factor of ∼ 2 larger than in hotter
clusters. Furthermore, the Iron abundance is significantly higher in the
redshift range 0.3–0.5 and is approximately constant around the value
0.25 at z > 0.5, providing robust indications on the time scale and
physical processes which drive the chemical enrichment of the ICM. In
Baldi, Ettori et al. (2007), we present the analysis of the temperature
and metallicity profiles of a sample of galaxy clusters in the redshift
range 0.1–0.3 selected from the Chandra archive. Single power-laws
can describe properly both the temperature and metallicity profiles at
radii larger than 0.1r180 in both Cooling-Core (CC) and Non-CoolingCore (NCC) clusters. A significant deviation is only present in the
inner 0.1r180 , where the effect of the central cooling is larger.
This work is carried out in collaboration with P. Tozzi (INAFTrieste Obs.), P. Mazzotta (Univ. of Rome, Tor Vergata), A. Baldi
(CfA), I. Balestra (MPE Garching), S. Borgani (Univ. of Trieste),
E. Rasia (Univ. of Michigan), P. Rosati (ESO).
2.4.10
X-ray properties of high-redshift galaxy clusters
People involved at OAB: Ettori.
The study of the physical properties of galaxy clusters up to redshift
1.3 aims at investigating how the hierarchical formation of these structures occurs and evolves.
We have already collected and analyzed the Chandra exposures of
about 70 objects with gas temperature larger than 3 keV and z > 0.3.
We are carrying on the analysis of their integrated X-ray properties to
update and extend the work on the gas mass fraction and the scaling
relations presented in Ettori et al. 2003, 2004a, 2004b. The study of
the distribution of the gas mass fraction is now submitted (Ettori et
al. 2008). By using only the cluster baryon fraction as a proxy for the
cosmological parameters, we obtain that Ωm is very well constrained
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at the value of 0.25 with a relative statistical uncertainty of 10% and
a further systematic error of about (−6, +14)%. On the other hand,
constraints on ΩΛ and w are weaker due to the presence of larger
statistical and systematic uncertainties (of the order of 40% on ΩΛ and
larger than 50% on w). We discuss how our constraints are affected
by several systematics, namely the assumed baryon fraction in stars,
the depletion parameter and the sample selection.
In Morandi, Ettori & Moscardini (2007a) and Morandi & Ettori
(2007b), we have investigated the scaling relations and gas entropy
profiles in a sample of highly X-ray luminous clusters with detected
Sunyaev-Zel’dovich signal in the redshift range 0.14–0.82 and with different states of relaxation. The X-ray and SZ scaling relations indicate
a tension between the quantities more related to the global energy of
the system (e.g. gas temperature, gravitating mass) and the indicators
of the structure of the ICM (e.g. gas density profile, central Compton
parameter y0 ). When the slope is fixed to the self-similar value, these
relations consistently show a negative evolution suggesting a scenario
in which the ICM at higher redshift has lower X-ray luminosity and
pressure in the central regions than predicted by self-similar models.
The entropy distribution of the intracluster gas reflects both accretion
history of the gas and processes of feedback which provide a further
energy besides the potential one. We recover the gas density, temperature and entropy profiles in a non-parametric way. We observe that
the entropy profiles are remarkably similar outside the core and can be
described by simple power-laws with a slope of 1.0–1.2. We measure
an entropy level at 0.1R200 of 100–500 keV cm2 and a central plateau
which spans a wide range of value (between a few and 200 keV cm2 )
depending on the state of relaxation of the source. To characterize the
energetic of the central regions, we compare the radial behaviour of
the temperature of the gas with the temperature of the dark matter
TDM by estimating the excess of energy ∆E = 3/2k(Tgas − TDM ). ∆E
ranges from 0 in typical cooling-core clusters to a few keV within 100
kpc in non-cooling core systems. Overall, we demonstrate that the
different observed behaviour of the entropy profiles represent different
stages of the relative relevance of heating and cooling in regulating
the feedback that shapes the ICM distribution in these final products
of the hierarchical model for structure formation.
The internal dynamics of a dark matter structure may have the remarkable property that the local temperature in the structure depends
on direction. This is parametrized by the velocity anisotropy which
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must be zero for relaxed collisional structures, but has been shown
to be non-zero in numerical simulations of dark matter structures. In
Host et al. (2008), we present a method to infer the radial profile of the
velocity anisotropy of the dark matter halo in a galaxy cluster from Xray observables of the intracluster gas. This non-parametric method
is based on a universal relation between the dark matter temperature
and the gas temperature which is confirmed through numerical simulations. We apply this method to observational data and we find
that the velocity anisotropy is significantly different from zero at intermediate radii. Thus we find a strong indication that dark matter is
effectively collisionless on the dynamical time-scale of clusters, which
implies an upper limit on the self-interaction cross-section per unit
mass.
This work is carried out in collaboration with A. Morandi (Univ.
of Bologna, DARK Univ. of Copenhagen), P. Tozzi (INAF-Trieste
Obs.), S. Borgani (Univ. of Trieste), L. Moscardini (Univ. of Bologna),
P. Rosati (ESO).
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3
Hydrodynamics
Distribution of the Galactic disk gas involved in a Galactic fountain.
Isodensity curves of the SN II ejecta are superposed, highlighting the
fountain pattern and the cloud formation. Because the density of the
ejecta is much lower than that of the ISM, it is represented on a different scale in order to make it visible in the figure. The four panels
represent snapshots taken at t=130 Myr (top-left), t=136.5 Myr (topright), t=143 Myr (bottom-left), t=149.5 Myr (bottom-right) of the
fountains with an external cloud falling toward the disk. The logarithmic density scale of the disk gas is in c.g.s, and the spatial scale is
in kpc.
People involved at OAB:
• Scientific staff: R. Bedogni, A. D’Ercole, P. Londrillo.
R. Bedogni continued the study of the evolution of the instabilities
for Type II SNe, compared for different density distributions of the
ejecta starting from the self-similar solutions at very early times. The
computations were extended to very late times, when Type I Sne are in
the regime of cooling also in the case of absence of clouds. A detailed
computation of drag effects is ongoing.
P. Londrillo applied a general 3D MHD code (ECHO) to study
resistive magnetic reconnection (in collaboration with S. Landi et al.).
The code has been extended and tested for general relativity in Kerr
metric (in collaboration with L. Del Zanna et al.)
P. Londrillo developed and tested a general N-body code for MOND
gravity. The code has been applied to study gravitational collapse in
a galaxy formation scenario (in collaboration with L. Ciotti and C.
Nipoti, Univ. of Bologna).
In collaboration with A. Marcolini, B. Gibson (Centre for Astrophysics, UK) and G. Battaglia (Univ. of Groningen, Netherlands)
, A.DErcole continued to study the properties of dwarf spheroidal
galaxies (dSphs), focussing in particular on their central regions. It
has been shown that in several Local Group dSphs, including Sculptor and Fornax, the chemical properties of the stars forming within
the galactic core can differ substantially from those situated at larger
radii. Inspecting our 3D hydrodynamical models (taking into account
the explosions and the pollution of SNe II and SNe Ia), we find that
the stars forming within two core radii (20% of the total) are relatively
iron-rich and α-depleted compared to the stars forming in the rest of
the galaxy. We also find that the actual three-dimensional stellar velocity dispersion shows a depression in the central region, where the
most metal-rich (i.e. [Fe/H]-rich) stars are partly segregated. This
naturally results in two different stellar populations, with an anticorrelation between [Fe/H] and velocity dispersion, in the same sense as
that observed in the Sculptor and Fornax dSphs.
DErcole, in collaboration with A. Pipino and F. Matteucci (Univ.
of Trieste), extended 1D hydrodynamical and chemical models of the
star formation in elliptical galaxies also to the bulge of spiral galaxies,
finding a homogeneous behaviour of the gradients of [Fe/H] and [α/Fe].
The latter, in particular, are rather flat and can be both positive or
99
negative. It is found that the observed variety of these gradients can
be explained by physical processes, generally not taken into account in
simple chemical models, such as metal-enhanced radial flows coupled
with different initial conditions for the galactic protocloud.
DErcole and C. Melioli, in collaboration with F. Brighenti (Univ. of
Bologna), extended the 3D hydromodels of Galactic Fountains taking
into account the effect of SN II within multiple O-B association. It
turns out that the metals produced by the SNe II do not move radially
far from the place where they have been produced, thus not influencing
the chemical gradient of the disk. We also find that 10% of the SN
II energy is injected in the hot gaseous Galactic halo, contrasting its
tendency to cool radiatively.
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4
Instruments and Technology
The cryostat of GIANO, the infrared spectrograph for the TNG.
People involved at OAB:
• Scientific staff: Bellazzini, Bragaglia, Cacciari, Ciliegi, Clementini, Diolaiti, Federici, Fusi Pecci, Montegriffo, Origlia, Pancino,
Tosi, Zitelli
• Technical staff: Bregoli, Ciattaglia, Innocenti, Lolli
• Contracts: Altavilla, Beccari, Contreras, Lanzoni, Lombardi,
Rossetti
4.1
The GAIA project
People involved at OAB: Altavilla, Bellazzini, Bragaglia, Cacciari,
Clementini, Federici, Fusi Pecci, Montegriffo, Pancino, Rossetti
The activity for GAIA of the European astronomical community is
presently focussed on the definition and preparation of all the technical aspects related to the data processing (the aspects related to
operations are taken care of by ESA). The Italian community, within
the Data Processing and Analysis Consortium (DPAC), responded to
the ESA Announcement of Opportunity (AO) in December 2006, with
contributions in the areas of astrometry, photometry and simulations,
as well as in various aspects of scientific exploitation. The Italian contribution to the GAIA project is very significant, placing Italy among
the top 3 major contributors along with France and the UK.
Several members of the OAB have expressed interest and are now
contributing actively to the project, both to the task of defining the
absolute calibration of the GAIA photometric system, and to the study
of variable sources with GAIA.
The absolute calibration of the GAIA photometric system is part of
the duties of Coordination Unit 5 (CU5), and is done by two Development Units, DU13 and DU14, under the management of the OAB (E.
Pancino and C. Cacciari, respectively). In particular, DU13 is responsible for providing the sample of Spectrophotometric Standard Stars
(SPSS) with accurate flux-calibrated SEDs (mostly obtained from a
dedicated ground-based observing campaign), and DU14 is responsible for deriving the relations and parameters to convert the internally
calibrated GAIA photometric data into absolute calibrated fluxes using these SPSS, as well as providing the algorithms and Java classes
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for the application of this calibration to all GAIA photometric data.
During 2007 the selection of the candidate SPSS and observing facilities for the ground-based observing campaign was completed, as well
as the pilot programmes to test various aspects of the observations.
Protocols for standard observing and data reduction procedures were
defined and set up in order to ensure homogeneity and uniformity in
the final data products. The main observing campaign was started at
various observing sites (Calar Alto, TNG and San Pedro Martir for
photometry and spectroscopy, Loiano and REM at ESO for variability monitoring). Within the DU14, strategies and procedures for the
preliminary definition and construction of the calibration algorithms
were set up with the help of the simulations then available. A Wiki
facility for the Bologna activity was set up and opened to the external
collaborators, and the internal data base and archive were defined and
set up in their preliminary structure, and were populated with the first
data.
Members of the OAB are actively contributing to the Coordination
Unit 7 (CU7), which is dedicated to the study of variable sources with
GAIA. In particular, G. Clementini manages the task Supplementary
Observations for CU7 which is responsible for providing supplementary ground-based and satellite time-series observations to prepare and
verify the variability results in the GAIA catalogue, and the workpackage Cepheids/RRLyrae, within the task Specific Object Studies, which
is responsible for developing specific tools and procedures for the classification and characterization of Cepheids and RR Lyrae stars that
will be observed by GAIA. During 2007 a network of ground-based
small and medium size telescopes to carry out supplementary observations for GAIA was set up and maintained. The network, which
includes telescopes from a few centimetres to the 1–1.5 m size, spread
over more than 10 different sites, should start collecting training observations for CU7 at the beginning of 2009. A review of existing
photometric and spectroscopic observations of variable sources is also
in progress. The OGLE and Hipparcos catalogues of variable stars
have already been put in the CU7 software system in Geneva, other
catalogues (e.g. SDSS, MACHO etc.) are under investigation. We
have completed a census of software already available and identified
new tools to be developed to validate and refine the classification of
Cepheids and RR Lyrae stars provided by the classification group,
and to derive specific parameters to be inserted in the GAIA catalogue. The corresponding Cepheids and RR Lyrae stars Software Re104
quirement Specification document was produced and posted on GAIA
Livelink at the end of 2007.
Most members of the GAIA team have attended the international
meetings relevant to these tasks, and the Java Workshop held in Bologna in March 2007.
This large and extensive preparatory work which is being carried
out by the OAB team for GAIA is documented in several technical notes available on the GAIA Livelink (GAIA-C5-TN-OABO-GA001, GAIA-C5-TN-OABO-PMN-001, GAIA-C7-TN-OABO-GC-001,
GAIA-C7-SP-OABO-GC-001) as well as in numerous internal reports
on Wiki-BO.
This activity is in collaboration with Italian scientists mainly in
Napoli, Padova, Roma, Teramo, Torino and Catania, and with international researchers mainly in Barcelona, Cambridge, Geneva, Leiden
and Groningen.
4.2
GIANO: An ultra-stable IR spectrometer for
the TNG
People involved at OAB: Montegriffo, Origlia, Rossetti, Lolli
The recent development of high sensitivity infrared (IR) spectrometers
has opened a new window in astrophysics. The investigation of the 1 to
2.5 µm band has yielded the discovery of a wealth of diagnostic tools,
both in terms of absorption features and emission lines, which are
crucial for a thorough understanding of several hot topics of modern
astrophysics, from faint solar system objects and extra-solar planets
to stellar clusters and galaxies, up to the highest redshift quasars.
The much reduced extinction at these wavelengths allows IR spectrometers to pierce the dust embedding several Galactic and extragalactic objects, which are heavily obscured in the optical. At high
redshift several emission and absorption spectral features, commonly
exploited when studying local galaxies, are shifted into the IR. These
and several other advantages of IR spectroscopy have led to a rapid
growth of the community of astronomers, from essentially any scientific field, making use of these facilities. GIANO is an optimized near
IR spectrograph which can yield, in one shot, complete 0.9–2.5 µm
spectra either at low (RS = 400) or high (up to R = 46000 with a 0.500
slit) resolutions maintaining, in both modes, a very high stability and
105
throughput throughout the whole spectral range.
This project is part of the Second Generation Instrumentation
Plan of the Telescopio Nazionale Galileo (TNG) located at Roque
de Los Muchachos Observatory (ORM), La Palma, Spain. The core
of GIANO is the spectrometer unit which uses, in double pass, the
same optical elements (3 aspheric mirrors) as collimator and camera.
These feed, through cross-disperser prisms, a commercial 23.2 ll/mm
R2 echelle grating acting as high resolution disperser. All these elements and the 20482 Hawaii-2 array are fixed to an optical bench which
will operate in vacuum at cryogenic and thermostated temperatures.
By simply inserting a flat mirror in front of the echelle the instrument
“changes its face” (hence the name GIANO) and becomes a low resolution spectrometer with an unprecedented combination of spectral
coverage, throughput and resolution. Measurements of circular and
linear polarization can be obtained using a combination of beam splitters and super-achromatic retarders which can be inserted/rotated in
the pre-slit optical system.
The GIANO team includes several Italian researchers and technicians from INAF (Bologna, Firenze, Catania and Padova Observatories, Fundacion Galileo Galilei) and has collaborations with the Istituto Nazionale di Ottica Applicata (Firenze) and a few engineering
companies. The project management is undertaken in a coordinate
way by L. Origlia (Bologna) – Principal Investigator – and E. Oliva
(Arcetri-FGG) – Project Manager.
OAB is providing the high-level software of the instrument, to
fulfill all astronomy-related tasks and to act as an interface between
the low-level software and the astronomer/operator. It also provides
the scientific software, by including the observing block preparation
tools and the off-line data reduction pipeline.
More details about the project can be found on the GIANO Web
page http://www.bo.astro.it/giano/.
4.2.1
GIANO Control Software
The GIANO control software runs on a dedicated PC-Linux workstation and besides performing software control of the whole system is
also responsible for the control of all sensors and of moving mechanisms, both inside and outside the GIANO cryostat. The management
of all these controls is handled by dedicated tasks called Instrument
Status (IS).
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Almost all Instrument Control Software (ICS) modules are written
in Tcl/Tk scripting language and the communications between the
GIANO ICS and all IS tasks are performed by means of IP or local
sockets.
The ICS is also interfaced with the GIANO DCS (Detector Control Software) which is structured in two different parts: one residing
inside the PC-Linux, and the other running on the embedded processor at the focal plane electronics and having direct access to the
hardware. These two distinct branches are interfaced by means of a
standard ethernet connection through which data and commands are
sent to Unix-like sockets. The software portion inside the embedded
processor manages the section of the appropriate waveform for the detector, controls the data flow and can handle special observing modes
such as multiple starts and stops.
At the end of 2007 Criotec Impianti S.r.l. (a company specialized
in cryogenic constructions) completed the manufacturing of the GIANO cryostat and of its optical bench. After the testing phase, the
overall cryogenic system was delivered to the Infrared Laboratory of
INAF Osservatorio Astrofisico di Arcetri where, at the beginning of
2008, the mounting of various spectrometer components started.
The decision to have the GIANO cryogenic system controlled by
an industrial PLC (Programmable Logic Controller), which communicates, through low level software, with the GIANO workstation, required additional software modules devoted to the interface with the
PLC, developed at OAB. In particular,
• IS1plc: a daemon to record all GIANO cryostat telemetry variables;
• IS1gui: a Graphical User Interface used both to monitor the
cryostat telemetry variables and to modify some cryostat control
parameters;
• IS1plot: a graphical tool to display the GIANO telemetry variables;
• IS1temp: a daemon to record all 32 temperature sensors positioned within the cryostat;
107
• IS2gld: a standalone utility used to test the GIANO cryogenic
motors during the instrumental assembling phase.
4.2.2
GIANO Data Reduction Software
The Giano Data Reduction Software (hereafter DrG) was designed to
run on different Unix/Linux platforms and relies on utilities available
under the Unix public domain software. The entire data flow will be
in the FITS and ASCII formats. The DrG back end will be entirely
written in C99; the front end will be developed in C99 using Gnu GTK
libraries and, at some stage, with the popular DS9 display program
via XPA access point. We also plan to release a command-line version
working in unattended automatic mode.
The DrG package will be provided with makefiles generated by
Gnu automake and a configure script generated by Gnu autoconf. A
small number of external libraries will be needed.
GIANO is an instrument with very few observing modes, each of
them producing quite a constant and repeatable distribution of light
on the array. This allows us to develop a highly optimized code: 2
main setups will be available for the high and low resolution, respectively. The DrG modules will be grouped in a few major tasks, namely
Calibration, Pre-reduction, Reduction, Analysis and Utilities.
During 2007 the main modules for the automatic spectrum extraction and calibration were completed, and they are now under final
testing.
4.3
Site testing
People involved at OAB: Zitelli, Lombardi
The site testing activity at OAB includes the analysis of instantaneous
and long term records of meteorological data of astronomical sites,
with the aim of selecting the best site for future optical telescopes.
This activity involves several Italian scientists (Bologna, Padova, Fundacion Galileo Galilei) and is the subject of a PhD thesis. For several
years the most important astronomical sites were monitored on a continuous basis by automatic weather stations. All these instantaneous
and long term records are important tools for meteorological and climatological studies, and also for the calibration of remote satellite
sensing of atmospheric and ground conditions. The analysis of the
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main synoptic meteo parameters at the Observatorio del Roque de
los Muchachos started in 2006 and was completed in 2007. Results
are published in PASP 119, 292 (2007); it was shown that the pressure changes precede the temperature changes typically by 2–3 hours,
suggesting the possibility to predict atmospheric temperatures a few
hours in advance. At the time of writing, further investigation is in
progress extending the analysis to other sites, in order to confirm this
result, which could be of great benefit for adaptive optics and mirror
maintenance. Dust measurements in situ, just outside the dome of
Telescopio Nazionale Galileo (TNG), were regularly collected with a
portable dust counter, operating on particles with sizes in the 0.3–5.0
µm range. The dust meter counter in use (Abacus 301, Particle Meas.
Syst. Inc.) quite often required manual operations, including regular download of the data to a computer and cleaning of the device.
Furthermore, it was sometimes difficult to separate the contribution
of the solid dust particles from that of condensed water vapour. For
these reasons, its replacement was planned with a more advanced dust
meter, such as the Lasair II particle counter (from A&L.CO Industries
srl) operating in the 0.3–25 µm range, fully automatic and controllable
from a PC. The analysis of the dust data collected at the level of the
main mirror of the TNG was completed and the results are published
in A&A 483, 651 (2008).
A detailed study of the Paranal Surface Layer was performed in
situ during 2007 and 2008 using several new generation instruments
such as: DIMM, MASS, LuSci, SLODAR and Generalized-SCIDAR.
The results are published as internal reports of the Site Selection Committee of the European Extremely Large Telescope.
4.4
Large Binocular Camera
People involved at OAB: Diolaiti, Beccari, Bellazzini, Cacciari, Clementini, Contreras, Federici, Fusi Pecci, Lanzoni, Tosi
The Large Binocular Camera (LBC) is a double wide field prime focus
imager for the Large Binocular Telescope (LBT), designed for multiwavelength observations in seeing-limited mode. The two channels,
named Blue (LBCB) and Red (LBCR), are optimized for different
wavelength ranges, from the near UV to 1 µm. The instrument is
characterized by challenging optical and mechanical tolerances, due
to the very fast focal ratio of the optics. Another somewhat unique
109
Figure 22: Alignment of LBCR. Note J. Hill (LBT Observatory technical director) reflected by the LBT primary mirror. Picture courtesy
of R. Bertram (LBT Observatory).
feature is represented by the size of the optics: the largest lens of the
two optical correctors has a diameter of 810 mm, one of the largest in
the world. A detailed description of the project can be found on the
web page http://lbc.oa-roma.inaf.it.
During 2007, OAB contributed to the optical alignment of the
red channel prime focus corrector at the telescope: this activity was
successfully completed during two technical runs in March and May
2007.
A team of astronomers at OAB collaborated in the science demonstration of LBC, with two observing programmes: a study of variable
stars and stellar populations in M31 and a study of Blue Straggler
Stars in M53.
110
4.5
LINC-NIRVANA
People involved at OAB: Bregoli, Ciattaglia, Ciliegi, Diolaiti, Innocenti
LINC-NIRVANA is a near infrared imaging interferometer for the
Large Binocular Telescope (LBT). It is built by a Consortium of German and Italian institutes. A detailed description of the project can
be found on the web page http://www.mpia-hd.mpg.de/LINC.
The basic working principle of the instrument is known as Fizeau
interferometry: the beams collected by the two LBT apertures are
corrected for the effects of the atmospheric turbulence by two multi
conjugate adaptive optics systems, then co-phased in real time and
combined inside a cryogenic camera, where they interfere in the focal
plane. LINC-NIRVANA is expected to have unprecedented imaging
performance in the near infrared, both in terms of angular resolution
and limiting magnitude, thanks to the interferometric mode and to
the large collecting area of the two LBT apertures combined together.
From the angular resolution viewpoint, LINC-NIRVANA will have the
same resolution of a 23 m telescope, corresponding to the maximum
baseline length of the interferometer.
The full resolution of LINC-NIRVANA will be recovered by multiple exposures of the same object, observed at different baseline orientations of the interferometer. The algorithms for the image combination
and reconstruction play a fundamental role. OAB is involved in the
definition of the science case and in the analysis of the observational
strategies, including the data reduction step. During 2007, a detailed
study was performed concerning this aspect, testing the capability of
AIRY-LN, a specific software developed at the DISI Department of the
University of Genova for the simulation and the reconstruction of the
LINC-NIRVANA images. Starting from HST images, we simulated the
expected emission from a galaxy at z ∼ 1 with magnitude Ks = 18.
K-band background emission of 13.5 mag arcsec−2 was assumed while
the pixel scale of the simulated images was set to 5 mas pixel−1 to
match the LINC-NIRVANA resolution. A total of six images at different hour angles were obtained. Using these simulated images, we
obtained the final reconstructed images using the software package
AIRY-LN. These images were analyzed with standard data reduction
software, showing that the reconstruction algorithm is fundamental to
obtain a good reproduction of the original flux and morphology and
111
Figure 23: Mid-High layer Wavefront Sensor of Linc-Nirvana, after
the integration and testing phase in the optical laboratory of OAB.
to exploit the capabilities of the instrument.
OAB is also involved in the design, procurement and integration of
the wavefront sensors for the multi-conjugate adaptive optics system
of LINC-NIRVANA. During 2007, the integration and testing of the
first Mid-High layer Wavefront Sensor was almost completed. The
unit, ready to be shipped to the Max-Planck Institut für Astronomie
– Heidelberg, is shown in Figure 23.
This work is in collaboration with G. Cosentino, I. Foppiani, B.
Marano, L. Schreiber at the Astronomy Dept., Univ. of Bologna, and
M. Lombini at INAF-Arcetri Obs. (at OAB at the time of writing).
112
4.6
ELT Design Study
People involved at OAB: Diolaiti
The ELT Design Study is a development project undertaken under
ESO’s leadership by several European institutes and companies. It
is funded in part by the European Commission under its Framework
Programme 6. The study covers technologies and concepts required
for the eventual design and construction of a European extremely large
optical and infrared telescope, with a diameter in the 30–60m range.
A more detailed description of the project may be found on the web
page http://www.eso.org/projects/elt-ds/.
The OAB personnel involved coordinated the work package ‘Novel
Adaptive Optics Concepts’, which addresses the theoretical and experimental study of wavefront sensing techniques related to the use of
artificial laser guide stars for adaptive optics systems. OAB, in collaboration with the Astronomy Dept. – Univ. of Bologna (I. Foppiani, L.
Schreiber), performed a detailed study of the impact of the perspective
elongation effect of laser guide stars on the performance of common
wavefront sensors. A first order design (laser power, detector properties) for a Shack-Hartmann wavefront sensor for an Extremely Large
Telescope was presented, along with an alternative optical solution to
the spot elongation problem.
The work package ‘Novel Adaptive Optics Concepts’ was completed in 2007.
4.7
Infrared Test Cameras for LBT
People involved at OAB: Bregoli, Ciattaglia, Diolaiti, Innocenti
The Infrared Test Cameras (IRTC) are two near infrared technical
imagers, conceived for the commissioning of the Gregorian foci of the
Large Binocular Telescope (LBT). The IRTC design is characterized
by three combinations of field of view-focal plane sampling, to allow
the use of the instrument in different working conditions, ranging from
the commissioning of the telescope in seeing-limited mode to the testing of the performance of the LBT adaptive optics system. The optics,
the mechanics and the control electronics are based on a custom design; a commercial infrared camera, using a InGaAs sensor, was chosen
as detector.
113
Figure 24: The first Infrared Test Camera for LBT at the end of the
integration phase in the optical laboratory of OAB, just before passing
the acceptance test.
The project, coordinated by OAB, was carried out in collaboration with the Astronomy Dept. – Univ. of Bologna (G. Cosentino, I.
Foppiani), the Max-Planck Institut für Astronomie – Heidelberg and
INAF-Arcetri Obs. (M. Lombini, with OAB at the time of writing).
The design and construction of these two technical imagers started
in February 2007 on a very fast track: the first IRTC was completed
and formally accepted in November 2007, the second a few months
later; both units were delivered and installed by OAB in early 2008.
114
4.8
MAORY
People involved at OAB: Bellazzini, Bregoli, Diolaiti, Ciliegi, Innocenti
MAORY (Multi-conjugate Adaptive Optics RelaY) is a post-focal
adaptive optics module for the future 42 m European Extremely Large
Telescope. An advanced conceptual design study for this instrument is
in progress, in the framework of an agreement between ESO and OAB,
which is leading a Consortium including other INAF astronomical Observatories (Arcetri and Padova) and the Office National d’Études et
de Recherches Aérospatiales (ONERA). The project is also funded by
the European Union, through the Framework Programme 7 (FP7).
MAORY is expected to provide a field of view of up to 2 arcminutes, corrected for the effects of the atmospheric turbulence, over the
near infrared wavelength range 0.8–2.4µm. The module is required
to produce a uniform correction over the field of view with high sky
coverage. The current design is based on the use of two post-focal
deformable mirrors, that complement the ground-layer correction provided by the adaptive telescope. From the wavefront sensing point of
view, MAORY includes a multiple reference source wavefront sensor,
based on the use of artificial and natural guide stars.
The candidate instruments fed by MAORY are a high angular resolution imaging camera, a wide spectral band single field spectrograph
and a multi-object spectrograph. The most prominent science cases
for the module in combination with the instruments are those requiring
a medium level of adaptive optics correction, with high sky coverage
and remarkable stability of the correction over the field of view, for
instance stellar population studies and deep observations of distant
galaxies.
The work performed at OAB is in close collaboration with the
Astronomy Dept. – Univ. of Bologna (G. Cosentino, I. Foppiani, B.
Marano, L. Schreiber).
The kick-off meeting of the study was held in November 2007. A
more detailed description of the project will be presented in the next
annual report.
115
5
Loiano Observing Site
An internal view of the dome of the G.D. Cassini telescope at the
Loiano observing site
People involved at OAB:
• Scientific staff: V. Zitelli
• Technical staff: S. Bernabei, G. Bregoli, I. Bruni, C. Ciattaglia
(retired 1, February 2007), A. De Blasi, R. Gualandi, G. Innocenti, I. Muzi, P. Salomoni (retired 1, August 2007).
• Fellows and contracts: S. Galleti
Loiano, observing site of the INAF–Bologna Observatory, is located at
785 m of height above sea level, at a distance of 37 km from Bologna.
The site, 23 hectares of wood, hosts 3 buildings: the 152 cm and 60
cm telescopes, and the guesthouse. The person in charge of the Loiano
observing site is Valentina Zitelli.
The 152 cm telescope, dedicated to G.D. Cassini, was built by
REOSC and has been operating since 1976. A general description of
the Cassini telescope is given in Table 1.
The main focal instruments presently available at the telescope
are:
1. BFOSC (Bologna Faint Object, Spectrograph and Camera), a
spectrograph/focal reducer based on transmitting optics ranging
from 330 to 1100 nm, equipped with an EEV 1340 × 1300 CCD
camera and the possibility to choose between two sets of filters:
a standard Johnson-Kron-Cousins system and a Gunn system.
An Hα filter has also been made available recently.
2. A two-channel Photoelectric Photometer (3 colors).
BFOSC, the multipurpose instrument for spectroscopy and imaging belonging to the xFOSC family of instruments, has been the most
scheduled instrument, with about 80% of the total allocated time,
well matching the seeing and the variable meteo conditions of the
Loiano site. The user manual of BFOSC is available at the web page:
http://www.bo.astro.it/~loiano/TechPage/bfosceng/BFOSC.htm
Two autoguiding systems are available: one for the telescope and
one for the rotation of the dome. The technical reports with the description of these systems are available at the web page:
http://www.bo.astro.it/bap/files/rep12-2004-02-text.pdf,
119
Table 1. Cassini telescope
Mount type
Optical configuration
Main mirror diameter
Focal ratio (main mirror)
Cassegrain focus
English
Ritchey-Chrétien
152 cm
F/3
equivalent focal length: 1200 cm
equivalent focal ratio: F/8
scale: 16.8 arcsec/mm
FOV: 70 arcmin
http://www.bo.astro.it/bap/files/rep12-2004-03-text.pdf (in
Italian).
The 60cm telescope was built in 1933 by Zeiss of Jena. It
was originally equipped with a photographic camera at the f/3 direct focus, and around 1960 it was modified to an f/20 Cassegrain
system. At present it is equipped with a 5-colour photometer. A
new Marconi CCD camera (series 4710, 13µm pixel size, 1055 × 1026
pxs) is mounted at the Cassegrain focus modified by a focal reducer
to f/5.6, and is now permanently used for training undergraduate
students. A user’s technical report can be found at the web page:
http://www.bo.astro.it/~loiano/ManualeCCD60cm/ManualeCCD60
cm.htm
This telescope is mainly used for educational activities and, during
the summer, also for outreach activities (see section Outreach and
Educational activities for more details).
5.1
Operations and use of the 152 cm telescope
People involved at OAB: Bernabei, Bregoli, Bruni, Ciattaglia, De
Blasi, Gualandi, Innocenti, Muzi, Salomoni (retired 1 July 2007), Zitelli
Fellows and contracts: Galleti
The 152 cm telescope is regularly used for scientific observations, and
is available for about 350 nights/year. The statistics of useful nights
for the last years are given in Table 2, where it is shown that about 30%
120
Figure 25: Histogram of the measured seeing at the 152cm telescope.
of the nights are lost to poor weather. Figure 25 shows the distribution
of the seeing. The median value is ∼ 2 arcsec, with several nights at
∼ 1.5 arcsec.
Table 2. Cassini Telescope – Nights used per year
nights/year
1999
2000
2001
2002
2003
2004
2005
2006
2007
used (t>50%)
used (t<50%)
used for test
not used (weather)
not used (technical)
not assigned
maintenance
98
22
33
179
4
29
131
29
10
179
5
11
0
118
33
10
179
3
18
4
133
37
6
167
0
14
8
147
41
3
148
0
17
9
126
38
6
160
0
33
2
110
42
4
161
2
35
11
129
47
7
108
6
58
10
115
53
8
116
26
46
1
Time is allocated every 6 months, starting in February and August.
Four technicians in turn guarantee the night-time technical assistance.
121
5.2
Loiano computer station
People involved at OAB: Bruni, Di Luca, Gualandi, Innocenti, Lolli
After the installation in 2002 of the 2Mbit connection between the
Loiano Observatory and Bologna, a fibre optic link was installed, connecting the 152cm Loiano telescope, the old 60cm telescope and the
guesthouse.
Images produced during observation runs can now be immediately
downloaded and made available to the observers. It is also possible
to pre-reduce the observed data with a PC in a local network. IRAF
packages are available and it is possible to implement other software
facilities.
5.3
Applications to the 152 cm telescope
The main observing programmes of 2007 at the 152 cm telescope can
be summarized as follows:
• optical counterparts of Gamma Ray Bursts;
• variable stars;
• detection of microlensing events;
• monitoring of variable sources (SNe, Novae, X-ray sources, etc.);
• photometry and spectroscopy of extragalactic objects;
• open clusters and globular clusters in our Galaxy and in nearby
galaxies;
• scientific observations coordinated with other projects (satellites,
WET, etc.). An example can be seen on the web page of the
WET Project (Whole Earth Telescope Project), where the list
of used telescopes is at the link:
http://www.physics.udel.edu/darc/wet/index.html;
• testing of prototypes and instrumentation for other telescopes
(i.e. the GASP polarimeter designed by M. Redfern, Galway
University);
122
• practical training and workshops for students (Italian and foreign);
• outreach activities during special events.
The pressure factor (nights requested/nights available) is ∼ 1.4. In
total, 318 nights were allocated for observations. Of these, 45 (14%)
were spent on didactic observations by several Universities. Service
observing is offered and is becoming increasingly popular, 32% of all
nights being requested in this mode. Service observations were conducted during 77 nights in 2007 (∼24% of the scheduled time; this is
made possible by the presence of a resident astronomer).
The approved observing programs are listed below and included
several long term programs.
1. Altavilla G., et al.: GAIA Calibration Working Group: Monitoring candidate Spectrophotometric Standard Stars against variability.
2. Bartolini C. (Univ. of Bologna), et al.: Fast Photometry of exoplanets and X-ray binaries.
3. Bonfanti C. (Ist. “R. Steiner” di Milano), et al.: Esercitazioni
per il “Progetto Michelangelo” su fotometria e spettroscopia di
oggetti celesti.
4. Bragaglia A., Tosi M., et al.: Colour-magnitude diagrams of
unstudied or badly studied Open Clusters. A pilot (part II).
5. Butler R. (Univ. of Galway, Ir), et al.: High speed Imaging &
Polarization studies with the Galway GASP-BerkeleyCam and
L3-CCD camera systems.
6. Clementini G., et al..: Stellar Archaeology in the Milky Way
halo: variable stars and stellar populations in the Coma dwarf
Spheroidal galaxy (dSph).
7. de Martino D. (INAF–OAC) et al.: X-ray counterparts of hard
X-ray Intermediate Polar candidates.
8. Dolci M. (INAF-OATeramo), et al.: A coordinated effort towards
a well-sampled photometric and spectroscopic database of supernovae.
123
9. Focardi P. (Univ. of Bologna), Zitelli V., et al.: The role of
environment-activity relationship on galaxies.
10. Galleti S., Bellazzini M., Buzzoni A., Cacciari C., Federici L., Fusi Pecci F.: A survey of remote and peculiar globular
cluster in M31.
11. Gavazzi, G. (Univ. of Milano Bicocca), et al.: A complete survey
of LINERS in the Virgo and Coma clusters.
12. Giovannelli, F. (INAF-IASF, Roma), et al.: Spectrophotometric
and photometric observations of X-ray binaries and interactions
with SNRs.
13. Greco G. (Univ. of Bologna), et al.: Target of Opportunity of
Afterglows of GRBs.
14. Maiorano E. (INAF-IASF, Bologna), et al.: Peering at the redshift of one GRB afterglow in Loiano.
15. Marano B. (Univ. of Bologna): Corso di strumentazione per
astrofisica, Modulo ottico.
16. Masetti N. (INAF-IASF, Bologna), et al.: Testing the extragalactic origin of INTEGRAL sources.
17. Meurs Evert J.A. (Dunsink Observatory), et al.: Spectroscopy
and Hα imaging of runaway stars.
18. Nesci R. (Univ. of Roma La Sapienza), et al.: Multiband photometry of very red BL Lacs.
19. Nesci R. (Univ. of Roma La Sapienza), et al.: Follow-up of
Blazar sample of Swift sources.
20. Neustroev V. (Univ. of Galway, Ir), et al.: Photometry of Cataclysmic Variables.
21. Norci L. (Dunsink Observatory), et al.: Spectrophotometry.
22. Norci L. (Dunsink Observatory), et al.: Hα imaging of circumstellar nebulae around FS CMa stars.
124
23. Poggiani, R. (Univ. of Pisa), et al.: Intranight variability of
blazars.
24. Poggiani, R. (Univ. of Pisa), et al.: Post-outburst spectroscopy
of novae.
25. Poggiani, R. (Univ. of Pisa), et al.: Photometry and spectroscopy
of normal galaxies, active galaxies and nebulae.
26. Polcaro, V.F. (INAF-IASF, Roma), et al.: Very High Mass Stars
Evolution.
27. Redfern M. (NUI Galway, Ir), et al.: Test observations.
28. Ripepi V. (INAF-OAC), et al.: Definizione della striscia di instabilità per le stelle nane brune giovani.
29. Ripepi V. (INAF-OAC), et al.: Studio della pulsazione nelle
stelle di pre-sequenza principale: i) stelle di massa intermedia,
ii) stelle nane brune.
30. Romoli M. (Univ. of Firenze), et al.: Esercitazioni per i corsi
Esperimentazioni IIIB (CdL Fisica, UniFI) e Laboratorio Astrofisica I (CdLS Fisica e Astrofisica, UniFI) su fotometria e
spettroscopia di oggetti celesti.
31. Rossi C. (Univ. of Roma La Sapienza), et al.: Absolute luminosities and distances of late M and AGB stars in the galactic
halo.
32. Shore S.N. (Univ. of Pisa), et al.: Monitoring of AG Dra and
Especially Active Symbiotic Stars
33. Silvotti R. (INAF-OAC), et al.: A giant planet orbiting the extreme horizontal branch star V 391 Pegasi.
34. Strafella F. (Univ. of Lecce), et al.: Probing MACHOs by observation of M31 pixel lensing.
The Bologna Observatory provides also the support necessary for their
degrees to students in Physics and Astronomy of National and European Universities. Both Loiano telescopes are used in a full immersion
125
stage, as described on the web page of the presentation of the courses
for Physics and Astronomy of the University of Galway in Ireland:
http://www.nuigalway.ie/faculties departments/physics/
courses/a201syll.html
• List of applications for undergradate students of both Italian
and European degrees in Astrophysics:
1. Bonfanti C. (Milano Steiner): 2 nights
2. Gavazzi G. (Milano Bicocca): 10 nights
3. Marano B. (Bologna Univ.): 8 nights
4. Norci L. (Dunsink Observatory): 6 nights
5. Poggiani R. (Pisa Univ.): 4 nights
6. Redfern M. (NUI-Galway-IE): 10 nights.
7. Vianello G. (Bologna Univ.): 7 nights Summer School
http://astro.nuigalway.ie/staff/butler ray.html
http://www.compsoc.nuigalway.ie/~sven/projects/
loiano/fieldtrip.htm
8. Romoli M. (Firenze Univ.): 5 nights
5.4
Loiano cooperation
Loiano hosts equipment of the Solid Earth Physics group used to study
the Earth’s crust deformation and mean sea level. This research group
is interested in monitoring and measuring with high accuracy the longterm vertical crustal motions. Starting with the analysis of the Adriatic coast and of the Po valley, during the last eight years the group
have developed a permanent GPS network consisting of five stations
(Medicina, Bologna, Porto Corsini, Trieste and Loiano). The fibre link
connection provides continous information from GPS to the physics
group. This makes it possible to correlate and model the observed
seasonal fluctuations with environmental parameters.
126
5.5
Scientific production involving
the 152 cm Telescope
5.5.1
International refereed pubblications
1. Bonnet-Bidaud, J. M.; de Martino, D.; Falanga, M.; Mouchet,
M.; Masetti, N.: IGR J00234+6141: a new INTEGRAL source
identified as an intermediate polar 2007, A&A, 473, 185
2. Bosch-Ramon, V.; Motch, C.; Rib, M.; Lopes de Oliveira, R.; et
al: Exploring the connection between the stellar wind and the
non-thermal emission in LS 5039, 2007, A&A, 473, 545
3. Calchi Novati, S.; Covone, G.; de Paolis, F.; Dominik, M.; et al:
Probing MACHOs by observation of M 31 pixel lensing with the
1.5 m Loiano telescope, 2007, A&A, 469, 115
4. Cortese, L.; Minchin, R. F.; Auld, R. R.; Davies, J. I.; et al:
The Arecibo Galaxy Environment Survey: II. A HI view of the
Abell cluster 1367 and its outskirts, 2008, MNRAS, 383, 1519
5. Costa, J.E.S., S.O. Kepler, D.E. Winget, et al.: The pulsation
modes of the pre-white dwarf PG 1159−035, 2008, A&A, 477,
627
6. Decarli, R.; Gavazzi, G.; Arosio, I.; Cortese, L.; Boselli, A.; et
al.: The census of nuclear activity of late-type galaxies in the
Virgo cluster, 2007, MNRAS, 381, 136
7. Focardi, P., V.Zitelli, S.Marinoni: Nucler activity in galaxy pairs:
a spectroscopic analysis of 48 UZC-BGPs 2008, A&A, 484, 655
8. de Marchi, F.; Poretti, E.; Montalto, M.; Piotto, G.; et al.:
Variable stars in the open cluster NGC 6791 and its surrounding
field, 2007, A&A, 471, 515
9. Galleti, S.; Bellazzini, M.; Federici, L.; Buzzoni, A.; Fusi Pecci,
F.: An updated survey of globular clusters in M 31. II. Newly
discovered bright and remote clusters, 2007, A&A, 471, 127
10. Giovannelli, F.; Bernabei, S.; Rossi, C.; Sabau-Graziati, L.: HeI
doubled emission lines from A0535+26 = HDE 245770. A possible interpretation, 2007, A&A, 475, 651
127
11. Giovannelli, F., Sabau-Graziati, L.: The Impact of Multifrequency Observations on Our Knowledge of the Physics of the
Universe, 2007, Chinese J. Astron. Astrophys. in press
12. Giovannelli, F.: Cataclysmic Variables: A Review. 2007, Chinese J. Astron. Astrophys. in press
13. Gonzalez-Riestra, R; R. F. Viotti, T. Iijima, C. Rossi, et al: AG
Draconis observed with XMM-Newton 2008, A&A, 481, 725
14. Landi R., Masetti N., Morelli L., Palazzi, E.; Bassani, L.; et
al.: The AGN nature of 11 out of 12 Swift/RXTE unidentified
sources through optical and X-Ray spectroscopy, 2007, ApJ, 669,
109
15. Miroshnichenko, A. S., N. Manset, A. V. Kusakin, E. L. Chentsov,
et al: 2007, Toward Understanding the B[e] Phenomenon: II.
New Galactic FS CMa Stars ApJ, 671, 828
16. Montalto, M.; Piotto, G.; Desidera, S.; de Marchi, F.; et al.: A
new search for planet transits in NGC 6791, 2007, A&A, 470,
1137
17. Ripepi, V.; Bernabei, S.; Marconi, M.; Ruoppo, A.; Palla, F.;
et al.: Discovery of δ Scuti pulsation in the Herbig Ae star VV
Serpentis, 2007, A&A, 462, 1023
18. Silvotti, R.; Schuh, S.; Janulis, R.; Solheim, J.E.; Bernabei, S.
et al.: A giant planet orbiting the ‘extreme horizontal branch’
star V391 Pegasi, 2007, Nature, 449, 189
19. Stassun, Keivan G.; van den Berg, M.; Feigelson, Eric: A Simultaneous Optical and X-Ray Variability Study of the Orion
Nebula Cluster. II. A Common Origin in Magnetic Activity,
2007, ApJ, 660, 704
20. Taubenberger, S.; Hachinger, S.; Pignata, G.; Mazzali, P. A.; et
al.: The underluminous Type Ia Supernova 2005bl and the class
of objects similar to SN 1991bg, 2008, MNRAS, 385, 75
21. Tosi, M, A. Bragaglia, M. Cignoni: The old open clusters Berkeley 32 and King 11, 2007, MNRAS, 378, 3057
128
22. Viotti, R.F., Galleti, S., Gualandi, R., Montagni, F., Polcaro,
V.F., et al.: 2007, A&A, 464, L53
23. Wolf, Marsha J.; Drory, Niv; Gebhardt, Karl; Hill, Gary J.:
Ages and Metallicities of Extragalactic Globular Clusters from
Spectral and Photometric Fits of Stellar Population Synthesis
Models 2007, ApJ, 655, 179
5.5.2
Published conference proceeding and circulars
24. Bufano, F.; Benetti, S.; Turatto, M.; Zampieri, L.; Gal-Yam, A.;
et al: Type II-Plateau Supernova 2005ay: an extensive study
from Ultraviolet to Near-Infrared, 2007, in: The Multicolored
Landscape of Compact Objects and their Explosive Origins. AIP
Conference Proceedings, 924, 271
25. Dall’Ora, M.; Clementini, G.; Kinemuchi, K.; Ripepi, V.; et al.:
RR Lyrae stars in the Bootes structure, 2007, IAUS, 241,331
26. Giovannelli, F.: Twenty Years of Astroparticle Physics. 2007, in
Frontier Objects in Astrophysics and Particle Physics, F. Giovannelli, G. Mannocchi (eds.), Italian Physical Society, Editrice
Compositori Bologna, Italy, 93, 3
27. Gonzalez-Riestra, R.; Viotti, R.F.; Rossi, C.; Iijima, T., et al.:
The high temperature of the AG Dra symbiotic system: the
impact of past and future UV observations, 2007, Space Astronomy: the UV window to the Universe. El Escorial (Spain), May
28th–June 1st, ApSS in press
28. Greco G., Terra F., Bartolini C., Guarnieri A., et al: GRB
070125: optical observations, 2007, GCN, 6047, 1
29. Greco, G., Terra F., Bartolini C., Guarnieri A., et al.: GRB
070311: optical observation, 2007, GCN, 6204, 1
30. Greco, G., Terra F., Bartolini C., Guarnieri A., et al.: GRB
070612B: optical observations, 2007, GCN, 6541, 1
31. Greco, G.; Terra, F.; Bartolini, C.; Guarnieri, A.; et al.: GRB
071112C: optical observation, 2007, GCN, 7089, 1
129
32. Lutz, R, S. Schuh, R. Silvotti et al.: Light curve analysis of
the hybrid sdB pulsators HS0702+6043 and HS2201+2610, 2007
proc. of the meeting on Hot subdwarf stars and related objects,
Bamberg July 2007, in press (astro-ph/07104871)
33. Marconi, M., Ripepi, V., Oliviero, M., Errico, L., et al.: 2007,
Indication of pulsation in young Brown Dwarfs Communications
in Asteroseismology, 150, 377
34. Masetti, N.; Morelli, L.; Cellone, S. A.; Bassani, L.; et al.: Spectroscopy of six optical candidates to unidentified INTEGRAL
sources 2007, The Astronomer’s Telegram, 1033, 1
35. Polcaro V.F., Norci L., Meurs E.J.A., Bernabei S.: The Very
Unusual HMXRB HD 34921, 2007, ASPC, 367, 471
36. Polcaro, V. F.; Viotti, R. F.; Rossi, C.; Norci, L; et al.: The
physics of Luminous Blue Variables and UV perspectives, 2007,
Space Astronomy: the UV window to the Universe. El Escorial
(Spain), May 28th–June 1st,(ApSS, in press)
37. Schuh, S., Silvotti, R.: Detection of a giant planet around a pulsating extreme horizontal branch star: the oldest known planet?,
2007, Astronomische Nachrichten, vol.328, Issue 7, p.658
38. Silvotti, R.; Schuh, S.; Janulis, R.; Bernabei, S.; et al.: The
O–C Diagram of the Subdwarf B Pulsating Star HS 2201+2610:
Detection of a Giant Planet?, 2007, ASPC, 372, 369
39. Silvotti, R: The (sdB+giant planet) system V 391 Peg: different
scenarios for its previous evolution, 2007 proc. of the meeting
on Hot subdwarf stars and related objects, Bamberg July 2007,
in press
40. Terra F., Greco G., Bartolini C., Guarnieri A., et al.: GRB
070125: optical observation, 2007, GCN, 6064 1
41. Terra F., Greco G., Bartolini C., Guarnieri A., et al: GRB
070518: optical observation, 2007, GCN, 6458, 1
42. Viotti, R.F., Friedjung, M., Gonzalez-Riestra, R., et al.: The
Non-Standard Multifrequency Behavior of AG DRA, 2007, Baltic
Astronomy, 16, 20
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5.5.3
Catalogs
43. de Marchi, F.; Poretti, E.; Montalto, M.; Piotto, G.; et al: V
light curves of NGC 6791 variable stars (De Marchi+, 2007),
2007, yCat, 34710515
44. Galleti, S.; Bellazzini, M.; Federici, L.; Buzzoni, A.; Fusi Pecci,
F.: New globular clusters in M 31 (Galleti+, 2007), 2007, yCat
34710127
45. Smriglio, F.; Dasgupta, A. K.; Boyle, R. P.: Vilnius photometry
on M92 (Smriglio+, 2006) 2007, yCat, 34580767
Note: An important contribution included in the previous list of
papers is from Silvotti et al., who using 418 hours of time series photometry in the last 7 years obtained the O-C diagrams of the two main
pulsation frequencies for the star V391 Pegasi, a pulsating extreme
horizontal branch star. The diagram shows both a long term component corresponding to the secular variation of the pulsation period,
and also a sinusoidal component due to the presence of a planetary
mass body. This is the first detection of a planet around a post red
giant star, proving that planets with orbital distance < 2 AU can
survive the expansion of the red giant. About 40% of the data used
in this paper were obtained using the Loiano telescope. The paper
appeared in Nature, in the issue published on 13 September 2007.
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6
Computer Centre and Computer
Network
The HPC Beowulf Cluster
People involved at OAB:
• Scientific staff: F. Delpino (until 16/9/2007), R. Merighi;
• Technical staff: R. Di Luca, M. Gatti, M. Lolli, R. Policastro.
6.1
General Description
The Bologna Astronomical Observatory, hereafter OAB, is hosted in
two buildings belonging to the University of Bologna, and shares these
spaces with The Department of Astronomy of the Bologna University.
The main network infrastructures belong to the University of Bologna
and are managed by CeS.I.A (Centro per lo Sviluppo e la Gestione
dei Servizi Informatici di Ateneo).
The computer network is formed by two class C subnets, with IP
addresses belonging to the Bologna University domain. Network lines
in each of the two buildings previously mentioned are cabled on two
Cabletron network-switches, owned respectively by OAB and CeS.I.A.
These switches are fibre-connected (gigabit) with an HP Procurve 2824
router-switch, interfaced with a Fortigate 400 firewall. The output line
from the firewall goes to the frontier-router. Both the firewall and the
frontier-router are owned and managed by CeS.I.A.
A third partitioned class C subnet connects the Loiano Observatory and the few offices still remaining in the former Observatory
location, in the old Observatory Tower.
In the last few years, due to the lack of space in the buildings in use,
the OAB rented some external offices, hosting post-doc students and
a laboratory. CeS.I.A. offered a laser bridge and micro-wave bridge to
connect these spaces to the internal network.
The computer centre hardware is formed by some Linux servers,
hosting the general services (dns, print server, IDL license manager,
web server) and intensive-computing facilities (two HP DS-20 and one
HP DS-25), by a HPC Beowulf Linux cluster for parallel computing,
and about 200 personal workstations. OAB owns about 65% of these
machines.
About 40 PCs are dedicated to academic activities (informatics
lab and pre-graduate students), and another 15 PCs belong to the
administrations of the two institutions.
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Workstations are mainly dual boot Linux/Windows PCs. In the
last three years, old HP Alpha workstations have been progressively
replaced by Apple PowerMacs (dual-processor IBM PowerPC or quadprocessor Intel Xeon). Also, several obsolete PC-Linux workstations
were replaced by Apple iMacs (Intel Core 2 Duo). At present, the
number of Apple Macs is about 40 units, between servers, laptops,
and iMacs.
Printing facilities, managed by a Linux print server, are represented
by 14 b/w laser printers, two color laser printers, and one large format
color printer.
The HPC Beowulf cluster, a joint venture between OAB and Department of Astronomy, is formed by 16 dual-processor Linux computers, connected in a local gigabit network.
6.2
Computer centre improvements
People involved at OAB: Delpino, Di Luca, Gatti, Lolli, Merighi, Policastro.
During 2007 some Power Mac, quad-processor, Intel Dual Core
based machines, with 2–4 GBy RAM and 250–500 GBy disk space were
bought. Basically these machines were dedicated to data reduction,
or used as main computing facilities by groups.
Also, some Apple iMacs, bi-processor 2 GHz Intel Core-Duo CPU,
250 GB SATA disk, and 1-2GB RAM were chosen to replace Unix
computers. The performances and the integration of these devices
have been quite good. These all-in-one devices were also very much
appreciated because of their low noise and temperature dissipation.
The BEOWULF Cluster, mainly financed by the Department of
Astronomy, with partial financial support by the Observatory of Bologna, started its activity in January 2007. The cluster consists of
16 bi-processor linux PCs linked together through a gigabyte switch.
One of these PCs will act as file server, uses a private network to hide
the Beowulf Cluster to the public network, and acts as an interface for
the public access running a NIS service. From the software point of
view, Intel Cluster Tool Kit and Intel Fortran Compiler were installed
on the system.
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6.3
6.3.1
Improvements in the geographic network
Computer networks
People involved at OAB: Delpino, Di Luca.
Delpino completed the Directory Service of the Observatory (DSO),
which drives the authentication and authorization policies for the
email service. A new application for the self provisioning and deprovisioning of accounts, now being tested, will directly interact with
the human resources database. The user interface with DSO was fully
revised and extended in its functionalities; it makes use of the new
DOTNET APIs, and allows a full integration with the mail service,
based on Microsoft Exchange software. The DSO UI will be soon be
extended with a B2B module for user identification and authorization
by means a web service, which will offer a simple and easy way to
perform user login for all intranet and internet applications.
Delpino developed a Web support for multimedia contents (audio,
video, slides) for the Observatory’s scientific outreach. It is designed
to implement an e-learning platform full distance modules on astronomical and astrophysical topics.
Delpino also took care of the security of the local network, operating a border firewall in collaboration with the Computer Emergency
Response Team of the local University, to which the Observatory network belongs.
As a member of the University of Bologna’s Network Scientific
Committee, Delpino was engaged in the Lepida Network project, the
wide area broadband network of the Regione Emilia Romagna, presently
in its final phase.
6.3.2
Web applications
People involved at OAB: Gatti, Lolli.
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During 2007 the GIANO web pages (http://www.bo.astro.it/giano/)
were continuously updated.
Lolli updated the Loiano time request form.
Gatti is maintaining and improving the Administration’s web site.
Useful information was made available, including staff database, different sets of forms for internal use and legislative references.
6.4
Routine activities
People involved at OAB: Di Luca, Gatti, Lolli, Policastro.
As well as all the activities described above, a large part of the
work of the computer centre staff was, as usual, dedicated to routine
activities such as hardware and software maintenance, failure management and user assistance.
Routine operations include:
• backup and user management on computers dedicated to datareduction
• supply of consumables (toners, paper for printers, magnetic supports for backup etc.)
• printer maintenance
• local network management
• administrative management of the computer centre (software
and hardware licenses, guarantees, purchases, maintenance contracts)
• updates and new installations of application software for astronomical reduction (MIDAS, IRAF etc.)
• management of the Observatory’s WWW server
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7
Library
A view of the library
People involved at OAB:
• Library staff: M. Marra.
As in the previous year, the main changes at the library in 2007 were
those related to the turnover in personnel concerning the Dept. of
Astronomy. Ms. Giulia Pincelli left the library in May, after winning a
public competition in her home-town and was temporarily substituted
by the contractor A. Soglia until July. A new stable C-level unit was
assigned to the library by the University of Bologna in September.
Nevertheless, the opening hours suffered no reduction, and on the
contrary the library was open to the public also in August (3 days a
week, most of the month).
A major intervention was made in the library office in July, with
the opening of a new, large sliding door connecting the office directly
with the main reading room. The involvement by the library director,
Prof. Palumbo, of all parties concerned – from all of the librarians to
all of the appropriate technicians – made of this intervention a success
whose results were appreciated by workers, patrons and users alike.
As for the library services, users, as always, have especially appreciated the book loan service, which is essential for a physical public
formed mainly by University students. At present, local book loans
have reached the number of 1850/year, increasing by as much as
+35% compared to 2006. INAF has contributed with almost 4000 euros (+ ∼ 8%) to the purchase of ∼ 50 new books, both scientific and
educational, as well as to a few subscriptions to technical journals the
majority of which, as always, are in any case bought by the University
of Bologna in their scientific cooperative subscription. The document
delivery service has proved to be one of the most used services of the
library, and has also much increased (+40% compared to 2006, but
still manageable in number). Documents were almost exclusively sent
to outer researchers or libraries, whereas local researchers seemed to
find locally almost everything they needed.
In October, an initiative from the new coordination of technical libraries of the Bologna University promoted a questionnaire for library
users, aimed at understanding possible specific information needs by
library users. The questionnaire was submitted to the students attending our library, and one of the results was the need for some instruction
in the use of the main databases and catalogues. Later, in 2008, the
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library direction approved a local initiative for the fulfillment of these
needs.
The project of a new special library for science education was instead set aside, after a short partial experimentation, due to technical
considerations.
At the end of the year, Marra prepared a detailed analysis on the
modes and use of the book loan service by local users (researchers and
students), in order to help improve the service and acquire new books.
The training of new part-time collaborators completed the local
main duties for the librarians.
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8
Outreach and Educational Activities
Sputnik50: mezzo secolo di era spaziale, Sputnik’s 50th Anniversary:
the dawn of space age.
People involved at OAB:
• Scientific staff: S. Bardelli, R. Bedogni, A. Buzzoni, M. Bellazzini, A. Cappi, F. Delpino, A. D’Ercole, E. Diolaiti, F. Fusi
Pecci, S. Galleti, G. Parmeggiani, F. Poppi, V. Zitelli, E. Zucca.
• Technical staff: S. Bernabei, I. Bruni, C. Ciattaglia, A. De Blasi,
R. Di Luca, O. Diodato, R. Gualandi, G. Innocenti, M. Orlandi,
R. Policastro, M. Ravaglia, F. Tinti.
The popularization of astronomy provides an important link between
the scientific astronomical community and society, giving visibility to
scientific success stories and supporting both formal and informal science education. While the principal task of an astronomer is to further
our knowledge of the Universe, disseminating this new information to
a wider audience than the scientific community is becoming increasingly important.
The Bologna Astronomical Observatory is very active in outreach
activities. Astronomy is an area that naturally captures the publics
imagination and OAB capitalizes on this interest with a host of efforts.
Our programs appeal to many different audiences, with a special emphasis on long term efforts within the local community, primary and
secondary level students and the general public. Our outreach activities range from observations, exhibits and public lectures, to working
directly with local high school students. There is a mixture of individual efforts, concerted programming by larger research initiatives, and
active collaborations and partnerships. Indeed, we have a long-term
and stable partnership between the OAB, the Astronomy Department
of the University of Bologna, the Institute of Radio Astronomy and
the amateur astronomers of Bologna (Associazione Astrofili Bolognesi)
and of San Giovanni in Persiceto in the province of Bologna (Astrofili
Persicetani). Particulary notable is the intense collaboration started
three years ago with the Marino Golinelli Foundation, which brings
Science to the people in places where the people are, the city squares.
The outreach activities during 2007 were:
• Total lunar eclipse, 30 March;
• Saturn occultation, 22 May;
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• La Scienza in Piazza;
• Col Favore del Buio;
• Il giorno del Sole, 10 June;
• BoSky 2007;
• Con il laser tra le stelle;
• Sputnik50: mezzo secolo di era spaziale;
• Il Cielo sulla Valle;
• Powers of 10, a journey across the Universe.
The educational activities in the same period were:
• Large Binocular Telescope: un binocolo per scoprire i misteri
dellUniverso;
• Origine e Evoluzione del Sistema solare;
• What is your weight on other planets?;
• Parco delle Stelle;
• Conferenze alla Specola.
8.1
8.1.1
Outreach Activities
Total lunar eclipse, 30 March
People involved at OAB: Bedogni, De Blasi, Di Luca, Fusi Pecci, Parmeggiani, Poppi.
On the occasion of the total lunar eclipse of 30 March, OAB organized a public observation in via Ranzani 1, in the courtyard of the
Observatory. Public lectures were held by Fabrizio Bónoli (University
of Bologna) and by Roberto Bedogni on the mythology and physics of
the Moon. More than 800 people attended the event.
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8.1.2
Saturn occultation, 22nd of May
People involved at OAB: Bardelli, Bruni, Bedogni, De Blasi, Di Luca,
Fusi Pecci. Gualandi, Parmeggiani, Poppi.
On 22 May more than 500 people observed the occultation of Saturn by the Moon at the main office of the OAB in Bologna, and as
many people did the same at the Loiano Astronomical Station. In Bologna the images of the occultation were also captured with a digital
camera and projected on a large monitor. Additional AAB telescopes
were available for the direct observation of the phenomenon. The
observation was led by Fusi Pecci.
8.1.3
La Scienza in Piazza
People involved at OAB: Bruni, Bedogni, Ciattaglia, De Blasi, Di
Luca, Fusi Pecci, Galleti, Gualandi, Innocenti, Parmeggiani, Poppi,
Ravaglia, Tinti, Zitelli.
During 2007 OAB has continued its collaboration with the “Marino
Golinelli” Foundation, which organizes La Scienza in Piazza (A Town
Square for Science). This is an activity which addresses schools, in
order to promote a responsible approach amongst the young generations, with a format whose goal is to carry Science throughout cities,
towns, villages and transforming them into open air Science Centres.
La Scienza in Piazza wishes to promote a general critical awareness of
scientific developments and a positive perception of science. The 2007
edition involved as many as seven towns located in Emilia-Romagna
and more than 51000 visitors actively participated in the activities
proposed.
It is worth noting that 2007 saw the first edition of the La Scienza
in Piazza held in Loiano. Astronomical exhibits (Origine e Evoluzione
del Sistema solare and What is your weight on other planets? ), observations of the night sky with the 152cm telescope, hands-on activities
(Build a scale model of the Solar system) and public lectures were the
main activities of the event.
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8.1.4
Col Favore del Buio
People involved at OAB: Bruni, De Blasi, Galleti, Gualandi, Parmeggiani, Poppi, Zitelli.
Eleven years ago the collaboration between the OAB and the Council for Culture of the Province of Bologna led to the creation of the
Col Favore del Buio event. This is a programme to visit the telescopes, radio telescopes, planetarium and astronomical museums of
the Province.
The event is organized by the OAB and proposes guided tours of
the Loiano Observatory, the Radio Astronomy Observatory of Medicina, the Museum of the Specola, the amateur observatories of San
Giovanni in Persiceto and Monte San Pietro, the Planetarium and the
Meteorite Collection of San Giovanni Persiceto and the Educational
Laboratory of the Planetarium Didactic Classroom of the Bologna
City Council. The visitors, during the year 2007, were over 32000.
The event gives people the opportunity to observe through the 60
cm telescope of the Loiano Observatory. These sessions are mainly
for visual viewing and an astronomer introduces celestial tourists to
stars, planets and other heavenly bodies. For the year 2007, 57 nights
were scheduled and over 2500 people observed and speculated about
the sky.
8.1.5
Il giorno del Sole, 10 June
People involved at OAB: Bardelli, Bruni, Bedogni, De Blasi, Di Luca,
Fusi Pecci, Gualandi, Parmeggiani, Poppi, Zitelli, Zucca.
2007 was the “International Heliophysical Year” (IHY), and 10
June was an open-doors day proposed by IHY-EUROPE all over Europe. The idea was to receive the public in the research institutes
to investigate topics related to the International Heliophysical Year.
OAB and the Council for Culture of the Province of Bologna organized a Sun day in the Villa Smeraldi Park, a beautiful park near
Bologna, with a Solar System exhibition, lectures, projections, solar
telescopes, an educational laboratory for primary-school students, a
musical show and a laser tour of the sky in the evening. Over 700
adults and children attended the event.
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8.1.6
BoSky 2007
People involved at OAB: Bardelli, Bedogni, Bruni, Cappi, Delpino,
De Blasi, Di Luca, Fusi Pecci, Gualandi, Parmeggiani, Poppi.
OAB organized, with the support of the Bologna City Council, in
the framework of the summer event Bé – Bologna estate, two events
to promote public awareness of astronomy.
Serata con il laser ai Giardini Margherita. In July a night sky
observation was organized at the Giardini Margherita park of Bologna. A laser beam was used to identify and describe major stars or
naked-eye objects in each constellation (i.e. “Betelgeuse is a red supergiant star”, or, “that fuzzy patch is the Andromeda galaxy”), to draw
the constellation patterns and to find the North Star and deep-space
objects. Interesting astronomical images were projected on a screen
to support the explanation. Those activities were led by Fusi Pecci.
More than 1000 people attended the event.
Incontri di astronomia. During the summer, six public lectures
were held in the courtyard of the Observatory, within walking distance
of the city centre. The multidisciplinary lectures aimed to focus in a
non-technical way on some of the foremost astronomical questions of
our day, and to investigate the connections between astronomy and
others disciplines such as mathematics, geophysics and poetry. The
lectures, delivered by talented speakers, were highly stimulating. Over
100 people attended every lecture.
8.1.7
Con il laser tra le stelle
People involved at OAB: Bardelli, Bruni, Bedogni, Di Luca, Fusi Pecci,
Galleti, Gualandi, Parmeggiani, Poppi.
Observations of the night sky with a laser were held in seven more
locations at San Lazzaro, Monte San Pietro, Bolzano, and San Giovanni in Persiceto. In each event nearly 200 people were taught how
to orientate themselves in the dark sky with the help of the laser. The
events were led by Bardelli, Bedogni, Fusi Pecci, Marano.
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8.1.8
Sputnik50: mezzo secolo di era spaziale
People involved at OAB: Bedogni, Di Luca, Orlandi, Fusi Pecci, Parmeggiani, Poppi, Zitelli.
History changed on October 4, 1957, when the Soviet Union successfully launched Sputnik I, the world’s first artificial satellite. On 2
and 3 October OAB organized a high-level public conference to celebrate the 50th anniversary of the Sputnik launch, and to commemorate
Professor Giampietro Puppi, a great scientist and animator of research
on space astrophysics and technology at the Bologna University. The
lectures were attended by 200 people, and in an evening event more
than 500 people attended a lecture by Margherita Hack.
OAB also edited a CD-ROM hypertext, Sputnik50, which dealt
with the history of space exploration and with the historical and social
changes that occurred during those years, from the Sputnik launch in
1957 to the human landing on the Moon in 1969. Over 5000 CD were
distributed in the secondary schools and libraries of the Province of
Bologna.
8.1.9
Il Cielo sulla Valle
People involved at OAB: Bardelli, Bedogni, Bellazzini, Cappi, Fusi
Pecci, Parmeggiani, Poppi,
These were five public evening lectures in the San Lazzaro Mediateca, the new Cultural Centre and Library in San Lazzaro, about
the Universe, Big Bang, Solar System, Time and Space in Astronomy,
Extrasolar Planets. Seventy people attended each lecture.
8.1.10
Powers of 10, a journey across the Universe
People involved at OAB: Parmeggiani, Poppi.
Powers of ten: a journey across the universe is a new exhibit built
with a grant from MIUR. Changing scale by just a few powers of ten
dramatically alters your perspective. Using a series of photographs,
the exhibit Potenze di 10: un viaggio attraverso l’universo takes its
viewers on a voyage from Bologna’s towers to the edge of the Universe.
150
The exhibit offers visitors the opportunity to learn about scale. Scale
is like geography. If you don’t know where New Zealand is when you
hear it mentioned in the news, you won’t have a place to hang it in your
mind. Numbers are the same. The exhibit, formed by 25 panels with
astronomical images, was displayed in many schools of the Province
of Bologna during 2007.
8.2
8.2.1
Educational Activities
Large Binocular Telescope: un binocolo per scoprire i
misteri dell’Universo
People involved at OAB: Diolaiti, Fusi Pecci, Parmeggiani, Poppi.
OAB took part in the National Astronomy Week promoted by
MIUR with a lecture on the new Large Binocular Telescope built in
Arizona, partly with Italian funding. The speakers were Fusi Pecci
and Diolaiti, and the lecture, held in the main hall of the Specola, was
attended by more than 100 students.
8.2.2
Origine e Evoluzione del Sistema solare
People involved at OAB: Bedogni, Delpino, Ciattaglia, De Blasi, Di
Luca, Diodato, Fusi Pecci, Innocenti, Parmeggiani, Policastro, Poppi,
Ravaglia, Tinti, Zitelli.
Thanks to a financial grant from MIUR, OAB created the Solar
System exhibit Origine e Evoluzione del Sistema solare. During 2007
the travelling exhibit was in Faenza and in Casalecchio (Bologna).
8.2.3
What is your weight on other planets?
People involved at OAB: Bedogni, Delpino, Ciattaglia, De Blasi, Di
Luca, Diodato, Fusi Pecci, Innocenti, Parmeggiani, Poppi, Ravaglia,
Tinti, Zitelli.
You can weigh yourself and compare your weight on the different
planets of our solar system with this new exhibit. A balance, which
can be moved from one place to another was built with a scale that
151
allows to compare your weight on the earth to that on the other planets. When people talk about weight, they are really talking about the
pull of gravity on an object, or the force required to lift an object. So
weight depends on gravity! The higher the gravity, the more something weighs! A planet’s gravity will depend on how big it is: the
greater the mass of the planet (e.g. Jupiter), the greater its gravity
and therefore, the more you will weigh. Going to somewhere like the
Moon, which is less massive than Earth and therefore has less gravity
will reduce your weight.
8.2.4
Parco delle Stelle
People involved at OAB: Bernabei, Bruni, De Blasi, Galleti, Gualandi,
Parmeggiani, Zitelli.
The Parco delle Stelle is an educational park developed by the
OAB for students and the general public, and was built with a grant
from the MIUR. The following exhibits are present in the park that
sorrounds the telescopes:
Solar system model. In order to understand the dimensions of our
planetary system and the distances to the various planets, the OAB, in
collaboration with the Astronomy Department, has built a scale model
of the Solar System. It starts from the 152cm telescope building and
goes along a path in the forest, reaching the dome that hosts the
60cm telescope. One meter along this path corresponds to 15 million
kilometres. To give a better idea of the dimensions of the planets
and of the Sun there is a second unit of measure, with one centimetre
corresponding to 7000 kilometres. The model is very useful to give
people a better understanding of the locations and sizes of objects in
the Solar system.
Solar telescope. A Coronado solar telescope allows people to see
the Sun in Hα light and understand its physical characteristics.
Sundial. A modern sundial has been built to show how the Sun
moves in the sky.
Cosmic Calendar. In The Dragons of Eden, Carl Sagan proposed
to put the history of the universe, all 13 billion years of it, into just
one year, with the Big Bang occurring in the first few seconds of New
Year’s Day, and all our known history occurring in the final seconds
before midnight on December 31. Using this time scale, each month
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would equal a little over a billion years. In the Cosmic Calendar
exhibit we have used the suggestion of Sagan and created a path with
a panel for each month of the year along the path that leads to the
60cm dome. This activity helps students to understand how human
activities fit into the grand scale of cosmic time.
The Parco delle Stelle is always open and, upon reservation, it is
possible to arrange guided tours for schools.
The 60cm telescope can be visited throughout the Col Favore del
Buio, and the 1.52m telescope (G.D. Cassini) is open to the general
public only the first Saturday of each month and to schools at any
time of the year, upon reservation.
8.2.5
Conferenze alla Specola
People involved at OAB: Bardelli, Bedogni, Buzzoni, Cappi, Di Luca,
Diodato, Orlandi, Fusi Pecci, Parmeggiani, Poppi, Zucca.
On the first Thursday of every month, at the Specola, the old
Observatory of Bologna in the town centre, a lecture is held on an
astronomical subject. The audience is mainly formed by high school
students. On average 80/90 people attend each lecture. The texts of
the lectures are available on the web page of the Observatory.
8.3
Educational and Public Outreach
Bardelli gave public lectures at the Castello di Serravalle.
Bedogni gave lectures for the astronomical summer school in Saltara
17–20 July; lectures for the Primo Levi course at the University of
Bologna; public lectures in the Modena Council, in San Giovanni in
Persiceto and in Riccione.
Zucca gave lectures for a high school in Ovada.
D’Ercole is the editor of the Spigolature astronomiche column, which
appears in Giornale di Astronomia.
Parmeggiani is the books page editor of Giornale di Astronomia.
De Blasi contributes regularly to the astronomy sections Occhi al cielo
of the monthly newsmagazine Explora. He published over 15 articles
and short communications during 2007.
Cappi, D’Ercole, Bedogni, De Blasi, Lolli, Orlandi, Parmeggiani, and
Poppi reviewed books for Giornale di Astronomia during 2007.
153
8.3.1
Publications
1. AA.VV, Sputnik50: mezzo secolo di era spaziale
CD-ROM Hypertext, September 2007
8.3.2
E-articles and web pages
1. AA.VV., Parco delle Stelle e Mostra
www.bo.astro.it/universo/mostra
2. A. De Blasi, Notiziario Astronomico
www.bo.astro.it/~loiano/NotiziarioAstronomico/
154
9
List of Publications
REFEREED PAPERS 2007
1. Aloisi A., Clementini G., Tosi M., Annibali F., Contreras
R., Fiorentino G., Mack J., Marconi M., Musella I., Saha A.,
Sirianni M., van der Marel R.P., 2007, I Zw 18 Revisited with
HST ACS and Cepheids: New Distance and Age, ApJ 667, L151
2. Altavilla G., Stehle M., Ruiz-Lapuente P., Mazzali P., Pignata
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N., Goobar A., Harutyunyan A., Pastorello A., Patat F., Rich
J., Salvo M., Schmidt B. P., Stanishev V., Taubenberger S.,
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of SN 2004dt, A&A 475, 585
3. Arnouts S., Walcher C.J., Le Fèvre O., Zamorani G., Ilbert
O., Pozzetti L., Bardelli S., Tresse L., Zucca E., Le Brun
V., Charlot S., Lamareille F., McCracken H.J., Bolzonella
M., [...], Cappi A., Ciliegi P., [...], Merighi R., et al., The
SWIRE-VVDS-CFHTLS surveys: stellar mass assembly over
the last 10 Gyears. Evidence for a major build up of the red
sequence between z=2 and z=1, A&A 476, 137
4. Baldi A., Ettori S., Mazzotta P., Tozzi P., Borgani S., 2007,
A Chandra Archival Study of the Temperature and Metal Abundance Profiles in Hot Galaxy Clusters at 0.1 &lt; z &lt; 0.3,
ApJ 666, 835
5. Balestra I., Tozzi P., Ettori S., Rosati P., Borgani S., Mainieri
V., Norman C., Viola M., 2007, Tracing the evolution in the iron
content of the intra-cluster medium, A&A 462, 429
6. Ballero S. K., Matteucci F., Origlia L., Rich R. M., 2007, Formation and evolution of the Galactic bulge: constraints from
stellar abundances, A&A 467, 123
155
7. Beccari G., Bellazzini M., Clementini G., Federici L.,
Fusi Pecci F., Galleti S., Montegriffo P., [...], Diolaiti E. et
al., 2007, A near-ultraviolet view of the Inner Region of M 31
with the Large Binocular telescope, A&A 476, 193
8. Bellazzini M., 2007, The surface brightness profile of the remote cluster NGC 2419, A&A 473, 171
9. Bernabei S., Marconi M., Ripepi V., Leccia S., Rodrı́guez E.,
Oswalt T. D., López-González M. J., Aceituno F. J., Ruoppo A.,
Palla F., Monteiro M. J. P. F. G., Molinari E., Chincarini G.,
Zerbi F. M., Covino S., Testa V., Tosti G., Vitali F., Antonelli
L. A., Conconi P., Malaspina G., Nicastro L., Palazzi E., 2007,
REM observations of the Herbig Ae stars V346 Ori and PDS2,
Communications in Asteroseismology 150 57
10. Berta S., Lonsdale C. J., Siana B., Farrah D., Smith H. E., Polletta M. C., Franceschini A., Fritz J., Perez-Fournon I., RowanRobinson M., Shupe D., Surace J., 2007, Keck spectroscopy of z
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11. Bondi M., Ciliegi P., Venturi T., Dallacasa D., Bardelli S.,
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O., Contini T., Garilli B., Iovino A., Temporin S., Vergani D.,
2007, The VVDS-VLA deep field. III. GMRT observations at
610 MHz and the radio spectral index properties of the sub-mJy
population, A&A 463, 519
12. Bongiorno A., Zamorani G., Gavignaud I., Marano B., Paltani
S., Mathez G., Picat J.P., Cirasuolo M., Lamareille F., Bottini
D., Garilli B., Le Brun V., Le Fèvre O., Maccagni D., Scaramella
R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami
C., Arnouts S., Bardelli S., Bolzonella M., Cappi A., [...],
Merighi R., Pellò R., Pollo A., Pozzetti L., Radovich M.,
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Merluzzi P., Temporin S., Vergani D., Walcher C.J., 2007, The
VVDS type-1 AGN sample: the faint end of the luminosity function, A&A 472, 443
156
13. Bonifacio P., Pasquini L., Molaro P., Carretta E., François P.,
Gratton R. G., James G., Sbordone L., Spite F., Zoccali M.,
2007, Variations in the lithium abundances of turn off stars in
the globular cluster 47 Tucanae, A&A 470, 153
14. Brusa M., Zamorani G., Comastri A., Hasinger G., Cappelluti N., Civano F., Finoguenov A., MAinieri V., Salvato M.,
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Mignoli M., et al., 2007, The XMM–Newton wide–field survey
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ApJS 172, 353
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the COSMOS Field. II. X-Ray Data and the logN-logS Relations,
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20. Carretta E., Bragaglia A., Gratton R. G., Catanzaro G.,
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157
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II. The Na-O anticorrelation in the globular cluster NGC 6752,
A&A 464, 927
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chemical composition of the peculiar bulge globular cluster NGC
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the Red Giant Branch and the Horizontal Branch Extension in
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24. Chavez M., Bertone E., Buzzoni A., Franchini M., Malagnini
M. L., Morossi C., Rodriguez-Merino L. H., 2007, Synthetic MidUV Spectroscopic Indices of Stars, ApJ 657, 1046
25. Ciotti L., Lanzoni B., Volonteri M., 2007, The Importance of
Dry and Wet Merging on the Formation and Evolution of Elliptical Galaxies, ApJ 658, 65
26. Civano F., Mignoli M., Comastri A., Vignali C., Fiore F.,
Pozzetti L., Brusa M., La Franca F., Matt G., Puccetti S., Cocchia F., 2007, The HELLAS2XMM survey. XI. Unveiling the
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Ibata R. A., Martin N. F., Bellazzini M., Sharp R., Tuntsov
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158
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Multiwavelength Study of Massive Galaxies at z 2. II. Widespread
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Elbaz D., Frayer D., Renzini A., Pope A., Alexander D. M.,
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Formation and Galaxy Growth, ApJ 670, 156
31. de la Torre S., [...], Bardelli S., Bolzonella M., Cappi A.,
Charlot S., Ciliegi P., [...], Merighi R., [...], Pozzetti L., [...],
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32. Del Zanna L., Zanotti O., Bucciantini N., Londrillo P., 2007,
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473, 11
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Böhringer H., Brusa M., Capak P., Cappelluti N., Comastri
A., [...], Zamorani G., 2007, The XMM-Newton Wide-Field
Survey in the COSMOS Field: Statistical Properties of Clusters
of Galaxies, ApJS 172, 182
39. Fiorentino G., Marconi M., Musella I., Caputo F., 2007, Classical Cepheid pulsation models. XI. Effects of convection and
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40. Franzetti P., [...], Zamorani G., [...], Bardelli S., Bolzonella
M., Cappi A., Ciliegi P., [...], Merighi R., [...], Pozzetti
L., Radovich M., Zucca E., Cucciati O., Walcher C.J., 2007,
The VIMOS-VLT deep survey. Color bimodality and the mix of
galaxy populations up to z 2, A&A 465, 711
41. Fritz J., Poggianti B. M., Bettoni D., Cava A., Couch W. J.,
D’Onofrio M., Dressler A., Fasano G., Kjærgaard P., Moles M.,
Varela J., 2007, A spectrophotometric model applied to cluster
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42. Frontera F., Orlandini M., Landi R., Comastri A., Fiore F.,
Setti G., Amati L., Costa E., Masetti N., Palazzi E., 2007, The
Cosmic X-Ray Background and the Population of the Most Heavily Obscured AGNs, ApJ 666, 86
43. Galleti S., Bellazzini M., Federici L., Buzzoni A., Fusi
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II. Newly discovered bright and remote clusters, A&A 471, 127
44. Giacintucci S., Venturi T., Murgia M., Dallacasa D., Athreya R.,
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clusters, A&A 476, 99
160
45. Gilli R., Comastri A., Hasinger G., 2007, The synthesis of
the cosmic X-ray background in the Chandra and XMM-Newton
era, A&A 463, 79
46. Gilli R., Daddi E., Chary R., Dickinson M., Elbaz D., Giavalisco M., Kitzbichler M., Stern D., Vanzella E., 2007, The
spatial clustering of mid-IR selected star forming galaxies at z
1 in the GOODS fields, A&A 475, 83
47. Giovannelli F., Bernabei S., Rossi C., Sabau-Graziati L., 2007,
HeI doubled emission lines from A0535+26 &equiv; HDE 245770.
A possible interpretation, A&A 475, 651
48. Gitti M., Ferrari C., Domainko W., Feretti L., Schindler S.,
2007, Discovery of diffuse radio emission at the center of the
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49. Gitti M., McNamara B. R., Nulsen P. E. J., Wise M. W.,
2007, Cosmological Effects of Powerful AGN Outbursts in Galaxy
Clusters: Insights from an XMM-Newton Observation of MS
0735+7421, ApJ 660, 1118
50. Gitti M., Piffaretti R., Schindler S., 2007, Mass distribution in
the most X-ray-luminous galaxy cluster RX J1347.5-1145 studied
with XMM-Newton, A&A 475, 441
51. Gitti M., Piffaretti R., Schindler S., 2007, Mass distribution in
the most X-ray-luminous galaxy cluster RX J1347.5-1145 studied
with XMM-Newton, A&A 472, 383
52. Gratton R. G., Lucatello S., Bragaglia A., Carretta E., Cassisi S., Momany Y., Pancino E., Valenti E., Caloi V., Claudi
R., D’Antona F., Desidera S., François P., James G., Moehler
S., Ortolani S., Pasquini L., Piotto G., Recio-Blanco A., 2007,
Na-O anticorrelation and horizontal branches. V. The Na-O anticorrelation in NGC 6441 from Giraffe spectra, A&A 464, 953
53. Greco C., Clementini G., Catelan M., Held E. V., Poretti
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161
54. Gruppuso A., Burigana C., Finelli F., 2007, The impact of
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55. Guzzo L., Cassata P., Finoguenov A., Massey R., Scoville N.Z.,
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A Large-Scale Structure at z=0.73 and the Relation of Galaxy
Morphologies to Local Environment, ApJS 172, 254
56. Hasinger G., Cappelluti N., Brunner H., Brusa M., Comastri
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I., Miyaji T., Molendi S., Paltani S., Sanders D. B., Scoville
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The XMM-Newton Wide-Field Survey in the COSMOS Field.
I. Survey Description, ApJS 172, 29
57. Kausch W., Gitti M., Erben T., Schindler S., 2007, ARCRAIDER.
I. Detailed optical and X-ray analysis of the cooling flow cluster
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58. Kinman T. D., Cacciari C., Bragaglia A., Buzzoni A., Spagna
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59. Krumpe M., Lamer G., Schwope A. D., Wagner S., Zamorani
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60. La Franca F., Puccetti S., Sacchi N., Feruglio C., Fiore F.,
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62. Lanzoni B., Dalessandro E., Ferraro F. R., Miocchi P., Valenti
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64. Lanzoni B., Sanna N., Ferraro F. R., Valenti E., Beccari G.,
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65. Lee T.-H., Stanghellini L., Ferrario L., Wickramasinghe D.,
2007, High-Resolution Spectra of Bright Central Stars of Bipolar
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133, 987
66. Lilly S.J., Le Fvre O., Renzini A., Zamorani G., [...], Mignoli
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67. Lombardi G., Zitelli V., Ortolani S., Pedani M., 2007, El
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68. Mainieri V., Hasinger G., Cappelluti N., Brusa M., Brunner H.,
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69. Mannucci F., Buttery H., Maiolino R., Marconi A., Pozzetti L.,
2007, Evidence for strong evolution of the cosmic star formation
density at high redshifts, A&A 461, 423
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70. Marconi M., Ripepi V., Oliviero M., Errico L., Magrı́ M., Vittone A., Palla F., Bernabei S., 2007, Indication of pulsation in
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377
71. Maturi M., Schirmer M., Meneghetti M., Bartelmann M.,
Moscardini L., 2007, Searching dark-matter halos in the GaBoDS
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72. McNamara D. H., Clementini G., Marconi M., 2007, A δ Scuti
Distance to the Large Magellanic Cloud, AJ 133, 2752
73. Melchior P., Meneghetti M., Bartelmann M., 2007, Reliable
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74. Meneghetti M., Argazzi R., Pace F., Moscardini L., Dolag K.,
Bartelmann M., Li G., Oguri M., 2007, Arc sensitivity to cluster
ellipticity, asymmetries, and substructures, A&A 461, 25
75. Meneghetti M., Bartelmann M., Jenkins A., Frenk C., 2007,
The effects of ellipticity and substructure on estimates of cluster
density profiles based on lensing and kinematics, MNRAS 381,
171
76. Miroshnichenko A. S., Manset N., Kusakin A. V., [...], Bernabei
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Toward Understanding the B[e] Phenomenon. II. New Galactic
FS CMa Stars, ApJ 671, 828
77. Miyaji T., Zamorani G., Cappelluti N., Gilli R., Griffiths
R. E., Comastri A., Hasinger G., Brusa M., Fiore F., Puccetti
S., Guzzo L., Finoguenov A., 2007, The XMM-Newton WideField Survey in the COSMOS Field. V. Angular Clustering of
the X-Ray Point Sources, ApJS 172, 396
78. Mobasher B., Capak P., Scoville N.Z., [...], Mignoli M., Scodeggio M., 2007, Photometric Redshifts of Galaxies in COSMOS,
ApJS 172, 117
79. Monaco L., Bellazzini M., Bonifacio P., Buzzoni A., Ferraro
F.R., Marconi G., Sbordone L., Zaggia S., 2007, High-resolution
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spectroscopy of RGB stars in the Sagittarius streams. I. Radial
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80. Morandi A., Ettori S., 2007, Entropy profiles in X-ray luminous
galaxy clusters at z &gt; 0.1, MNRAS 380, 1521
81. Morandi A., Ettori S., Moscardini L., 2007, X-ray and SunyaevZel’dovich scaling relations in galaxy clusters, MNRAS 379, 518
82. Mucciarelli A., Ferraro F. R., Origlia L., Fusi Pecci F., 2007,
The Globular Cluster NGC 1978 in the Large Magellanic Cloud,
AJ 133, 2053
83. Mucciarelli A., Origlia L., Ferraro F. R., 2007, The IntermediateAge Globular Cluster NGC 1783 in the Large Magellanic Cloud,
AJ 134, 1813
84. Nipoti C., Londrillo P., Ciotti L., 2007, Galaxy merging in
modified Newtonian dynamics, MNRAS 381, L104
85. Nipoti C., Londrillo P., Ciotti L., 2007, Dissipationless Collapses in Modified Newtonian Dynamics, ApJ 660, 256
86. Nipoti C., Londrillo P., Zhao H., Ciotti L., 2007, Vertical dynamics of disc galaxies in modified Newtonian dynamics, MNRAS 379, 597
87. Noordermeer E., van der Hulst J. M., Sancisi R., Swaters R. S.,
van Albada T. S., 2007, The mass distribution in early-type disc
galaxies: declining rotation curves and correlations with optical
properties, MNRAS 376, 1513
88. Olsen L.F., Benoist C., Cappi A., Maurogordato S., Mazure A.,
Slezak E., Adami C., Ferrari C., Martel F., 2007, Galaxy clusters
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Deep fields, A&A 461, 81
89. Oosterloo T., Fraternali F., Sancisi R., 2007, The Cold Gaseous
Halo of NGC 891, AJ 134, 1019
90. Origlia L., Rood R. T., Fabbri S., Ferraro F. R., Fusi Pecci
F., Rich R. M., 2007, The First Empirical Mass-Loss Law for
Population II Giants, ApJ 667, LL85
165
91. Pace F., Maturi M., Meneghetti M., Bartelmann M., Moscardini L., Dolag K., 2007, Testing the reliability of weak lensing
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92. Paltani S., [...], Bardelli S., Tresse L., Zamorani G., Zucca
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C., Arnouts S., Bardelli S., Bolzonella M., Bottini D., Cappi
A., Charlot S., Ciliegi P., Contini T., Foucaud S., Franzetti P.,
Gavignaud I., Guzzo L., Ilbert O., Iovino A., Lamareille F.,
McCracken H.J., Marano B., Marinoni C., Mazure A., Meneux
B., Merighi R., Paltani S., Pelló R., Pollo A., Pozzetti L.,
Radovich M., Vergani D., Zamorani G., Zucca E., Bondi M.,
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47. Lombardi G., Zitelli V., Ortolani S., Pedani M., Ghedina A.,
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VIENNA, AUSTRIA
SUBMITTED PAPERS 2008
1. Abbas U., de la Torre S., Le Fèvre O., Guzzo L., Marinoni
C., Pollo A., Zamorani G., Bottini D., Garilli B., Le Brun V.,
Maccagni D., Scaramella R., Scodeggio M., Tresse L., Vettolani
G., Zanichelli A., Adami C., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T.,
Foucaud S., Franzetti P., Gavignaud I., Ilbert O., Iovino A.,
Lamareille F., McCracken H.J., Marano B., Mazure A., Meneux
B., Merighi R., Paltani S., Pellò R., Pozzetti L., Radovich M.,
Vergani D., Zucca E., Bondi M., Bongiorno A., Brinchmann J.,
Cucciati O., de Ravel L., Gregorini L., Perez-Montero E., Mellier Y., Merluzzi P., Temporin S., Walcher C.J. , The VIMOS
VLT Deep Survey: Evolution of the Halo Occupation Distribution since z ∼ 1, 2008, A&A, submitted
2. Bardelli S., Zucca E., Bolzonella M., Ciliegi P., Gregorini
L., Zamorani G., Bondi M., Zanichelli A., Tresse L., Vergani
D., Gavignaud I., Bongiorno A., Bottini D., Garilli B., Le Brun
V., Le Fèvre O., Maccagni D., Scaramella R., Scodeggio M.,
Vettolani G., Adami C., Arnouts S., Cappi A., Charlot S.,
Contini T., Foucaud S., Franzetti P., Guzzo L., Ilbert O., Iovino
A., Lamareille F., McCracken H.J., Marano B., Marinoni C.,
Mazure A., Meneux B., Merighi R., Paltani S., Pellò R., Pollo
205
A., Pozzetti L., Radovich M., Abbas U., Brinchmann J., Cucciati O., de la Torre S., de Ravel L., Memeo P., Perez-Montero
E., Mellier Y., Merluzzi P., Temporin S., De Ruiter H.R., Parma
P. , The VVDS-VLA Deep Field: IV. Radio–Optical properties,
2008, A&A, submitted
3. Cappelluti N., Brusa M., Hasinger G., [...] Comastri A., [...],
Gilli R., [...], Zamorani G., 2008, The XMM-Newton Wide
Field Survey in the COSMOS field, ApJ, submitted
4. Cignoni M., Sabbi E., Nota A., Tosi M., Degl’Innocenti S.,
Prada Moroni P., Angeretti L., Carlson L., Gallagher J., Meixner
M., Sirianni M., Smith L.J., 2008, Star formation history in the
SMC: the case of NGC602, AJ, submitted
5. de Ravel L., Le Fèvre O., Tresse L., Bottini D., Garilli B.,
Le Brun V., Maccagni D., Scaramella R., Scodeggio M., Vettolani G., Zanichelli A., Adami C., Arnouts S., Bardelli S.,
Bolzonella M., Cappi A., Charlot S., Ciliegi P., Contini T.,
Foucaud S., Franzetti P., Gavignaud I., Guzzo L., Ilbert O.,
Iovino A., Lamareille F., McCracken H.J., Marano B., Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S., Pellò
R., Pollo A., Pozzetti L., Radovich M., Vergani D., Zamorani
G., Zucca E., Bondi M., Bongiorno A., Brinchmann J., Cucciati O., de la Torre S., Gregorini L., Memeo P., Perez-Montero
E., Mellier Y., , The VIMOS VLT Deep Survey: Evolution of the
major merger rate since z ∼ 1 from spectroscopicaly confirmed
galaxy pairs, 2008, A&A, submitted (astro-ph/arXiv:0807.2578)
6. Donnarumma A., Ettori S., Meneghetti M., 2008, X-ray and
strong lensing mass estimate of MS2137.3–2353, MNRAS, submitted
7. Ettori S., Morandi A., Tozzi P., Balestra I., Borgani S., Rosati
P., Lovisari L., Terenziani F., 2008, The cluster gas mass fraction
as a cosmological probe: a revised study, A&A, submitted
8. Fiore F., Puccetti S., Brusa M., Salvato M., Zamorani G.,
[...] Comastri A., [...] Gilli R., et al, 2008, Chasing Highly
Obscured QSOs in the COSMOS Field, ApJ, submitted
206
9. Gastaldello F., Buote D.A., Temi P., Brighenti F., Mathews
W.G., Ettori S., 2008, The X-ray cavities, filaments and cold
fronts in the core of the galaxy group NGC5044, ApJ, submitted
10. Gilli R., Zamorani G., [...] , Pozzetti, L., [...] , Comastri
A., [...] , Bardelli S., Bolzonella M., [...] Mignoli M., [...]
Vergani D., [...] , Zucca E., [...] , Cappi A., et al., 2007, The
spatial clustering of X-ray selected AGN in the XMM-COSMOS
field, A&A, submitted
11. Kurk J., Cimatti A., Zamorani G., Halliday C., Mignoli M.,
Pozzetti L., Daddi E, Rosati P., Dickinson M.; Bolzonella M.,
Cassata P., Renzini A., Franceschini A., Rodighiero G., Berta
S., GMASS Ultradeep Spectroscopy of Galaxies at z ∼ 2 ? IV.
Witnessing the assembly of a galaxy cluster at z = 1.6? , 2008,
A&A, submitted
12. Marziani P., Sulentic J.W., Stirpe G., Zamfir S., Calvani M.,
2008, VLT/ISAAC Spectra of the Hβ Region in IntermediateRedshift Quasars. III. Hβ Broad Line Profile Analysis and Inferences on BLR Structure, A&A, submitted
13. Merten, J., Cacciato, M., Meneghetti M., Mignone, C., Bartelmann, M., 2008, Combining weak and strong cluster lensing:
Applications to simulations and MS2137, A&A, submitted
14. Origlia L., 2008, Mass loss in Population II giant stars, MemSAIt, 79, 432
15. Mucciarelli A., Ferraro F.R., Origlia L., Carretta E., Fusi
Pecci F., 2008, The chemical composition of the intermediateage globular clusters in the Large Magellanic Cloud, MemSAIt,
79, 529
16. Fabbri S., Origlia L., Rood R. T., Ferraro F.R., Fusi Pecci F.,
Rich M.R., 2008, An IRAC@Spitzer survey of GGCs., MmSAI,
79, 720
17. Gavignaud I., Wisotzki L., Bongiorno A., Paltani S., Zamorani G., Møller P., Le Brun V., Husemann B., Lamareille F.,
Schramm M., Le Fèvre O., Bottini D., Garilli B., Maccagni D.,
207
Scaramella R., Scodeggio M., Tresse L., Vettolani G., Zanichelli
A., Adami C., Arnaboldi M., Arnouts S., Bardelli S., Bolzonella M., Cappi A., Charlot S., Ciliegi P., [...], Merighi
R., Pellò R., Pollo A., Pozzetti L., Radovich M., Zucca E.,
[...], Vergani D. , Eddington ratios of faint AGN at intermediate
redshift: Evidence for a population of half-starved black holes?,
2008, A&A, submitted
18. Lamareille F., Brinchmann J., Contini T., Walcher C.J., Charlot S., Perez-Montero E., Zamorani G., Pozzetti L., Bolzonella
M., Garilli B., Paltani S., Bongiorno A., Le Fèvre O., Bottini
D., Le Brun V., Maccagni D., Scaramella R., Scodeggio M.,
Tresse L., Vettolani G., Zanichelli A., Adami C., Arnouts S.,
Bardelli S., Cappi A., Ciliegi P., Foucaud S., Franzetti P.,
Gavignaud I., Guzzo L., Ilbert O., Iovino A., McCracken H.J.,
Marano B., Marinoni C., Mazure A., Meneux B., Merighi R.,
Pellò R., Pollo A., Radovich M., Vergani D., Zucca E., Romano
A., Grado A., Limatola L. , Physical properties of galaxies and
their evolution in the VIMOS VLT Deep Survey: I. The evolution of the mass–metallicity relation up to z ∼ 0.9, 2008, A&A,
submitted
19. Maier C., Lilly S.J., Zamorani G., Scodeggio M., Lamareille F.,
Contini T., Sargent M.T., Scarlata C., Oesch P., Carollo C.M.,
Le Fèvre O., Renzini A., Kneib J.P., Mainieri V., Bardelli S.,
Bolzonella M., Bongiorno A., Caputi K.I., Coppa G., Cucciati O., de la Torre S., de Ravel L., Franzetti P., Garilli B.,
Iovino A., Kampczyk P., Knobel C., Kovac K., Le Borgne J.F.,
Le Brun V., Mignoli M., Pellò R., Peng Y., Perez-Montero E.,
Ricciardelli E., Silverman J.D., Tanaka M., Tasca L., Tresse L.,
Vergani D., Zucca E., Abbas U., Bottini D., Cappi A., Cassata
P., Cimatti A., Fumana M., Guzzo L., Halliday C., Leauthaud
A., Maccagni D., Marinoni C., McCracken H.J., Memeo P.,
Meneux B., Porciani C., Pozzetti L., Scaramella R., Walcher
C.J. , The morphological dependence of the star formation activity on stellar mass surface density in zCOSMOS galaxies at
0.5 < z < 0.9 compare with SDSS galaxies at 0.04 < z < 0.08,
2008, ApJ, submitted
20. Perez-Montero E., Contini T., Lamareille F., Brinchmann J.,
208
Walcher C.J., Charlot S., Bolzonella M., Pozzetti L., Bottini
D., Garilli B., Le Brun V., Le Fèvre O., Maccagni D., Scaramella
R., Scodeggio M., Tresse L., Vettolani G., Zanichelli A., Adami
C., Arnouts S., Bardelli S., Cappi A., Ciliegi P., Foucaud S.,
Franzetti P., Gavignaud I., Guzzo L., Ilbert O., Iovino A., McCracken H.J., Marano B., Marinoni C., Mazure A., Meneux B.,
Merighi R., Paltani S., Pellò R., Pollo A., Radovich M., Vergani D., Zamorani G., Zucca E., Physical properties of galaxies
and their evolution in the VIMOS VLT Deep Survey: II. Extending the mass–metallicity relation to the range z ∼ 0.89 − 1.24,
2008, A&A, submitted
21. Rosa Gonzalex D., Terlevich E., Terlevich R., Jimenez Bailon
E., Ranalli P., Comastri A., Laird E., Nandra K., 2008, Evolution of the X-ray luminosity function in young HII Galaxies,
MNRAS, submitted
22. Scodeggio M., Vergani D., Cucciati O., Iovino A., Franzetti P.,
Garilli B., Lamareille F., Bolzonella M., Pozzetti L., Abbas
U., Marinoni C., Contini T., Bottini D., Le Brun V., Le Fèvre O.,
Maccagni D., Scaramella R., Tresse L., Vettolani G., Zanichelli
A., Adami C., Arnouts S., Bardelli S., Cappi A., Charlot S.,
Ciliegi P., Foucaud S., Gavignaud I., Guzzo L., Ilbert O., McCracken H.J., Marano B., Mazure A., Meneux B., Merighi R.,
Paltani S., Pellò R., Pollo A., Radovich M., Zamorani G., Zucca
E., Bondi M., Bongiorno A., Brinchmann J., de la Torre S.,
de Ravel L., Gregorini L., Memeo P., Perez-Montero E., Mellier
Y., Temporin S., Walcher C.J. , The VIMOS VLT Deep Survey:
Stellar mass segregation and large–scale galaxy environment in
the redshift range 0.2 < z < 1.4, 2008, A&A, submitted
23. Silverman J.D., Lamareille F., Maier C., Lilly S.J., Mainieri
V., Brusa M., Cappelluti N., Hasinger G., Zamorani G., Scodeggio M., Bolzonella M., Contini T., Carollo C.M., Kneib J.P.,
Le Fèvre O., Bardelli S., Bongiorno A., Brunner H., Caputi
K.I., Civano F., Comastri A., Coppa G., Cucciati O., de la Torre
S., de Ravel L., Elvis M., Finoguenov A., Fiore F., Franzetti P.,
Garilli B., Gilli R., Iovino A., Kampczyk P., Knobel C., Kovac
K., Le Borgne J.F., Le Brun V., Merloni A., Mignoli M., Pellò
R., Peng Y., Perez-Montero E., Ricciardelli E., Tanaka M., Tasca
209
L., Tresse L., Vergani D., Vignali C., Zucca E., Abbas U., Bottini D., Cappi A., Cassata P., Cimatti A., Fumana M., Guzzo
L., Leauthaud A., Maccagni D., Marinoni C., McCracken H.J.,
Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., Salvato M., Scaramella R., Walcher C.J. , Ongoing and co-evolving
star formation in zCOSMOS galaxies hosting Active Galactic
Nuclei, 2008, ApJ, submitted
24. Smolcic V., Zamorani G., Schinnerer E., Bardelli S., Bondi
M., Carilli C.L. , Ciliegi P., Merloni A., Paglione T., Salvato
M., Scodeggio M., Scoville N., Cosmic evolution of radio selected active galactic nuclei in the COSOS fie ld, 2008, ApJ, in
press submitted
25. Trump J., Impey C.D., Elvis M., [...], Comastri A., et al., 2008,
The COSMOS AGN Spectroscopic Survey, ApJ, submitted
26. Walcher C.J., Lamareille F., Vergani D., Arnouts S., Buat V.,
Charlot S., Tresse L., Le Fèvre O., Bolzonella M., Brinchmann
J., Pozzetti L., Zamorani G., Bottini D., Garilli B., Le Brun
V., Maccagni D., Milliard B., Scaramella R., Scodeggio M., Vettolani G., Zanichelli A., Adami C., Bardelli S., Cappi A.,
Ciliegi P., Contini T., Franzetti P., Foucaud S., Gavignaud I.,
Guzzo L., Ilbert O., Iovino A., McCracken H.J., Marano B.,
Marinoni C., Mazure A., Meneux B., Merighi R., Paltani S.,
Pellò R., Pollo A., Radovich M., Zucca E., Lonsdale C., Martin
D.C. , The VVDS-SWIRE-GALEX-CFHTLS surveys: Physical
properties of galaxies at z below 1.2 from photometric data, 2008,
A&A, submitted (astro-ph/arXiv:0807.4636)
210
10
Observing Campaigns
RADIOTELESCOPES
1. GMRT+235 MHz -327 MHz, Halos and Relics in galaxy cluster: spectral properties and connection with cluster mergers., PI:
T. Venturi, Co–I: S. Giacintucci, G. Brunetti, R. Athreya, S.
Bardelli, R. Cassano, D. Dallacasa, G. Setti, 40 hours, June July 2007, service mode
2. ATCAAssessing the AGN component of the faint radio population, PI: I. Prandoni, Co–I: H. De Ruiter, P. Parma et al., 20
GHz: 12 hours; 4.8 and 8.4 GHZ: 20 hours, 2007, service mode
ESO TELESCOPES
VLT
3. ESO VLT+CRIRES, Chemical enrichment of Bulge globular clusters: Liller 1 and Terzan 5, PI: L. Origlia, Co–I: E. Valenti,
F.R. Ferraro, R..M. Rich, S. Fabbri, 3 nights, July 2007, service
mode
4. ESO VLT+CRIRES+FLAMES, A global screening of the chemical abundances and abundance patterns in the Large Magellanic
Cloud globular clusters, PI: L. Origlia, Co–I: A. Mucciarelli,
F.R. Ferraro, E. Valenti, S. Fabbri, 5 nights, December 2007,
service mode
5. ESO VLT+FLAMES, The Na-O anticorrelaStion in M 54, the
closest, high mass extragalactic Globular Cluster, PI: E. Carretta, Co–I: M. Bellazzini, A. Bragaglia, et al., 36hr, AprSep 2008 (assigned in 2007), service mode
211
6. ESO VLT+FLAMES, The origin and evolution of metals in the
LMC: a novel and powerful constraint on its star formation history, PI: V. Hill, Co–I: D. Romano, M. Tosi et al, 25 hours,
March 2007, service mode
7. ESO VLT+SINFONI, Following the mass assembly of galaxies
at the key epoch 1.0 < z < 1.8 from a complete sample observed
with SINFONI., PI: T. Contini, Co–I: [...], F. Lamareille, [...], S.
Bardelli, E. Zucca, [...] , 147 hours, 2007, service mode
8. ESO VLT+VIMOS MOS, zCOSMOS: The evolutionary links between galaxies, their nuclei, their morphologies and their environments., PI: S. Lilly, Co–I: [...], S. Bardelli, M. Bolzonella,
A. Cappi, F. Lamareille, M. Mignoli, G, Zamorani, E.
Zucca and the zCOSMOS team, 73 hours , 2007, service mode
9. ESO VLT+VIMOS MOS, VIMOS VLT Deep Survey (VVDS):
a complete census of the high redshift population of galaxies from
a deep 22.5 ≤ IAB ≤ 24.75 survey., PI: O. LeFevre, Co–I: [...], S.
Bardelli, M. Bolzonella, A. Cappi, P. Ciliegi, F. Lamareille,
R. Merighi, L. Pozzetti, G, Zamorani, E. Zucca and the
VVDS team, 41 hours , 2007, service mode
10. ESO VLT+VISIR, Diffraction-limited mid-infrared imaging of
heavily obscured AGN detected in hard X-rays, PI: H. Horst,
Co–I: P. Gandhi, A. Comastri, R. Gilli, A. Smette, C. Vignali, 12 hr, 2007, service mode
3.6m
11. ESO 3.6m+EFOSC 2, Reconstructing the merging scenario and
star formation history in interacting galaxy clusters, PI: S. Maurogordato, Co–I: M . Arnaud, E. Belsole, C. Benoist, A. Bijaoui,
H. Bourdin, A. Cappi, C. Ferrari et al., 3 nights, August 2007,
212
service mode
NTT
12. ESO NTT+EMMI, Relics and Halos at intermediate redshifts:
testing the merging paradigm., PI: S. Bardelli, Co–I: S. Giacintucci, T. Venturi, E. Zucca, D. Dallacasa, R. Cassano, G.
Brunetti, G. Setti, 3 nights, April 2007, visitor mode
13. ESO NTT+SOFI, Probing the stellar populations of the inner
Bulge globular clusters, PI: E. Valenti, Co–I: F.R. Ferraro, L.
Origlia, S. Perina, 3 nights, July 2007, service mode
2.2m
14. ESO 2.2m+WFI, The low-surface brightness galaxy population
in small groups: the case of NGC3923, PI: A. Buzzoni, Co–I:
S. Cellone, E. Held, 3 nights, January 2007, visitor mode
15. ESO 2.2m+WFI, Stellar Archeaology in the Milky Way Halo:
variable stars and stellar populations in the Hercules dwarf Spheroidal
galaxy (dSph), PI: G. Clementini, Co–I: T. Beers, M. Dall’Ora,
M. Di Criscienzo, L. Di Fabrizio, C.Greco et al., 20.3 hours,
12-16 July 2007, service mode
16. ESO 2.2m+WFI, Reconstructing the merging scenario and star
formation history in interacting galaxy clusters, PI: S. Maurogordato, Co–I: M . Arnaud, E. Belsole, C. Benoist, A. Bijaoui,
H. Bourdin, A. Cappi, C. Ferrari et al., 3.8 hours, June 2007,
service mode
213
ITALIAN TELESCOPES AND OTHER TELESCOPES WITH ITALIAN PARTICIPATION
LBT
17. LBT 8.4m+LBC Pulsating variable stars in the halo and streams
of Andromeda: hints on the galaxy star formation history and
assembling PI: G. Clementini, Co-I: M. Bellazzini, C. Cacciari, L. Ciotti, E. Diolaiti, L. Federici, F. Fusi Pecci,
P. Londrillo, B. Marano, C. Nipoti, M. Tosi, M. Marconi,
I. Musella, V. Ripepi, E. Poretti, 8h SDT, October 11-18, 2007
18. LBT 2x8.4m+Blue+Red Pulsating variable stars in the giant
stream of Andromeda: hints on the galaxy star formation history and assembling PI: G. Clementini, Co-I: G. Beccari,
M. Bellazzini, C. Cacciari, L. Ciotti, R. Contreras, E. Diolaiti, L. Federici, F. Fusi Pecci, B. Marano, M. Tosi, M.
Marconi, I. Musella, V. Ripepi, E. Poretti, 9h
TNG
19. TNG+DOLORES, A survey of remote and peculiar globular clusters in M31, PI: S. Galleti, Co–I: M. Bellazzini, A. Buzzoni,
L. Federici, F. Fusi Pecci, S. Perina, 5 nights, September
2007, visitor mode
20. TNG+DOLORES, Ground Based Spectrophotometry for Gaia:
A Pilot Programme (TAC 13 AOT15/07A), PI: C. Cacciari,
Co–I: E. Pancino, A. Bragaglia, M. Bellazzini, L. Federici,
E. Rossetti, E. Diolaiti, P. Montegriffo, G. Altavilla et
al., 3 nights, May 2007, visitor mode
21. TNG+DOLORES, Spectrophotometric standard stars observations for GAIA’s absolute flux calibration (TAC 37 AOT16/07B),
214
PI: E. Pancino, Co–I: C. Cacciari, G. Altavilla, M. Bellazzini, A. Bragaglia, E. Diolaiti, L. Federici, P. Montegriffo,
E. Rossetti et al., 5 nights, January 2008 (approved in June
2007), visitor mode
22. TNG+DOLORES, Spectrophotometric standard stars observations for GAIA’s absolute flux calibration (TAC 3 AOT17/08A),
PI: E. Pancino, Co–I: C. Cacciari, G. Altavilla, M. Bellazzini, A. Bragaglia, E. Diolaiti, L. Federici, P. Montegriffo, E.
Rossetti et al., 7 nights, May 2008 (approved in 2007), visitor
mode
23. TNG+DOLORES, Unveiling obscured activity at high redshift,
PI: C. Vignali, Co–I: C. Gruppioni, F. Pozzi, G, Zamorani, R.
Gilli, A. Comastri, P. Ciliegi et al., 3 nights, August 2007,
visitor mode
24. TNG+DOLORES, Ground Based Spectrophotometry for Gaia:
A Pilot Programme. (TAC 13 AOT15/07A), PI: C. Cacciari,
Co–I: E. Pancino, A. Bragaglia, M. Bellazzini, L. Federici,
E. Rossetti, E. Diolaiti, P. Montegriffo, G. Altavilla et
al., 3 nights, May 2007, visitor mode
25. TNG+DOLORES, Investigating the nature of low luminosity
Active Galactic Nuclei (AOT15/07A TAC 44), PI: PI D. Trevese,
Co–I: V. Zitelli, 18h , service mode
26. TNG+DOLORES, Investigating the nature of low luminosity
Active Galactic Nuclei (AOT17/08A TAC 36), PI: PI D. Trevese,
Co–I: V. Zitelli, 32h Class A, service mode
27. TNG+LRS, A survey of remote and peculiar globular clusters
in M31, PI: S. Galleti, Co–I: M. Bellazzini, A. Buzzoni, L.
Federici, F. Fusi Pecci, S. Perina, 5 nights, September 2007,
215
visitor mode
28. TNG+SARG, The chemical composition of the Sagittarius Northern Stream, PI: L. Monaco, Co–I: M. Bellazzini, A. Buzzoni,
F. Ferraro, S. Zaggia, G. Marconi, P. Bonifacio, L. Sbordone, 29
hours (Class B), August 2007, service mode
29. TNG+SARG, Open Clusters as tracers of the Galactic Disk
(BOCCE project), PI: A. Bragaglia, Co–I: E. Carretta. M.
Tosi, R. Gratton, G. Andreuzzi, L. Di Fabrizio, 24hr, 31 Aug-01
Sep 2007, Oct 2007-Jan 2008, service mode
30. TNG+SARG, Open Clusters as tracers of the Galactic Disk
(BOCCE project), PI: A. Bragaglia, Co–I: E. Carretta. M.
Tosi, R. Gratton, G. Andreuzzi, L. Di Fabrizio, 23hr, Feb-Jul
2008 (assigned in 2007), service mode
Loiano
31. Cassini 1.5m+BFOSC, The role of environment-activity relationship on galaxies, PI: P. Focardi, Co–I: Zitelli V., 10, service
mode
32. Cassini 1.5m+BFOSC, A survey of remote and peculiar globular clusters in M31, PI: S. Galleti, Co–I: M. Bellazzini, A.
Buzzoni, C. Cacciari, L. Federici, F. Fusi Pecci, 9 nights,
September-November 2007, visitor mode
33. Cassini 1.5m+BFOSC, Assembling the Grid of Spectrophotometric Standard Stars for GAIA: testing observational strategies and
the effects of extinction., PI: G. Altavilla, Co–I: E. Pancino,
A. Bragaglia, C. Cacciari, L. Federici, M. Bellazzini, 3
nights, February 2007, visitor mode
216
34. Cassini 1.5m+BFOSC, GAIA Calibration Working Group: Monitoring candidate Spectrophotometric Standard Stars against variability, PI: G. Altavilla, Co–I: E. Pancino, M. Bellazzini,
A. Bragaglia, C. Cacciari, L. Federici, P. Montegriffo, E.
Rossetti, 8 nights, August, September, October 2007,January
2008, visitor mode
35. Cassini 1.5m+BFOSC, Colour-magnitude diagrams of unstudied
or badly studied Open Clusters. A pilot (part II), PI: A. Bragaglia, Co–I: M. Tosi, 4 nights, Jan-Jun 2007, service mode
36. Cassini 1.5m+BFOSC, Stellar Archeaology in the Milky Way
Halo: variable stars and stellar populations in the Coma dwarf
Spheroidal galaxy (dSph), PI: G. Clementini, Co-I: M. Dall’Ora,
V. Ripepi, M. Di Criscienzo, M. Marconi, C. Greco, K. Kinemuchi, T. Beers, H.A. Smith, M. Catelan, 10 nights, 12-16 March,
13-17 April, 2007, service mode
FOREIGN TELESCOPES
Keck
37. KECK+NIRSPEC, Near IR spectroscopy of Bulge giants, PI:
R.M. Rich, Co–I: L. Origlia, 12 hours, April 2007, visitor mode
38. KECK+OSIRIS, Near IR spectroscopy of M31 and M32 Bulge
giants, PI: R.M. Rich, Co–I: L. Origlia, K. Gebhardt, 1, September 2007, visitor mode
217
Subaru
39. Subaru+MOIRCS, High-Redshift Black Hole Growth in Dense
Environments with COSMOS, PI: A. Koekemoer, Co–I: A. Comastri, G, Zamoraniet al. , 3 nights, approved in December
2007, service mode
LAS CAMPANAS OBSERVATORY (LCO)
40. Baade 6.5m+IMACS Stellar Archeaology in the Milky Way Halo:
variable stars and stellar populations in Hercules and Leo IV
dwarf Spheroidal galaxies PI: M. Catelan, Co-I: K. Kinemuchi,
H.A. Smith, G. Clementini, B. Pritzl, M. Dall’Ora, T. Beers,
V. Ripepi, 2 half nights, 27-28 March, 2007
WILLIAM HERSCHEL TELESCOPE (WHT)
41. WHT 4.2m+PFIP imager Stellar Archeaology in the Milky Way
Halo: variable stars and stellar populations in the Canes Venatici I dSph PI: G. Clementini, Co-I: M. Dall’Ora, M. Di
Criscienzo, M. Marconi, V. Ripepi, L. Di Fabrizio, C. Greco,
K. Kinemuchi, C. Rodgers, T. Beers, C. Kuehn, H.A. Smith, M.
Catelan, B. Pritzl, 3 nights, 10-12 May, 2007
LOWELL 1.8m
42. Lowell 1.8m+PRISM WFI, Stellar Archeaology in the Milky Way
Halo: variable stars and stellar populations in the Ursa Major
II dwarf Spheroidal galaxy (dSph), PI: K. Kinemuchi, Co–I: C.
Rodgers, F. Rivera, L. Portscheller, B. Kelly, R. Barlow, G.
Clementini et al., 4 nights, 19-22 February, 2007,
218
ISAAC NEWTON TELESCOPE (INT)
43. INT 2.5m+WFC Stellar Archeaology in the Milky Way Halo, PI:
V. Ripepi, Co-I: T. Beers, G. Clementini, K. Kinemuchi, M.
Dall’Ora, 4 nights, April 20-23, 2007
WYOMING INFRARED OBSERVATORY
(WIRO)
44. WIRO 2.3m+WIRO-Prime Stellar Archeaology in the Milky Way
Halo, PI: K. Kinemuchi, Co-I: C. Rodgers, G. Clementini, et
al., 2 nights, January 16-17, 2007; 4 nights March 2007; 4 nights,
April 10-13, 2007; 4 nights, May 8-12, 2007
SOUTHERN ASTROPHYSICAL RESEARCH
TELESCOPE (SOAR)
45. SOAR 4.1m+Optical Imager Stellar Archeaology in the Milky
Way Halo, PI: H.A. Smith, Co-I: K. Kinemuchi, M. Catelan, G.
Clementini, et al. half night, March 14, 2007; 1 night, April
22, 2007
CAHA 2.2m
46. CAHA 2.2m+CAFOS, Ground based spectrophotometry for Gaia:
a Pilot Programme. (F07-2.2-033), PI: C. Jordi (Universitat de
Barcelona-IEEC), Co–I: C. Cacciari, A. Bragaglia et al., 6
nights, March-April 2007, visitor mode
47. CAHA 2.2m+CAFOS, Ground-based observations for Gaia’s calibrations: spectrophotometric standard stars (H07-2.2-024), PI:
C. Jordi, Co–I: F. Figueras, J.M. Carrasco, B. López Martı́,
M. Manteiga, A. Ulla, J.M. Appellaniz, C. Cacciari, E. Pancino, A. Bragaglia, G. Altavilla, S.C. Trager, C. Soubiran,
6+6nights, October 2007, visitor mode
219
48. CAHA 2.2m+CAFOS, Ground based spectrophotometry for Gaia:
a Pilot Programme. (F07-2.2-033), PI: C. Jordi, Co–I: C. Cacciari, A. Bragaglia, S.C. Trager, F. Figueras, J.M. Carrasco,
C. Fabricius, 6 nights, March-April 2007, visitor mode
additional service time (in 7 different nights in May, June, July
2007) to compensate bad weather
49. CAHA 2.2m+CAFOS, Ground-based observations for Gaia’s calibrations: spectrophotometric standard stars (H07-2.2-024), PI:
C. Jordi, Co–I: F. Figueras, J.M. Carrasco, B. López Martı́, [...],
C. Cacciari, E. Pancino, A. Bragaglia, G. Altavilla et al.,
6+6nights, October 2007, visitor mode
50. CAHA 2.2m+CAFOS, Ground based observations for Gaia’s calibrations: spectrophotometric standard stars. (F08-2.2-043), PI:
C. Jordi (Universitat de Barcelona-IEEC), Co–I: F. Figueras,
J.M. Carrasco, [...], C. Cacciari, E. Pancino, A. Bragaglia,
G. Altavilla: (INAF-Bologna Obs); S.C. Trager (Kapteyn Astro. Inst.); C. Soubiran (Obs. Bourdeau), 5 nights, April 2008
(approved in 2007), visitor mode
SPM 1.5m
51. SPM 1.5m+La Ruca, Ground-based photometry for the absolute
flux calibration of Gaia, PI: William J. Schuster B., Barbara
Pichardo, Co–I: F. Figueras, E. Pancino, S.C.Trager, 10+11
nights, January-February, April-May 2008 (approved in 2007),
visitor mode
AZT-24 1.08m
52. AZT-24+SWIRCAM, The infrared JHK light curves of RR Lyr,
PI: C. Cacciari, Co–I: A. Sollima, A. Piersimoni, 7 n, May-July
2007, service mode
220
REM 0.6m
53. REM 0.6m+ROSS, GAIA Calibration Working Group: Monitoring candidate Spectrophotometric Standard Stars against variability (16012 AOT16/07B), PI: E. Pancino(INAF-OA Bologna), Co–I: C. Cacciari, G. Altavilla, A. Bragaglia, M.
Bellazzini, L. Federici et al., 60 hours, from July 2007 to January 2008, service mode
54. REM 0.6m+ROSS, GAIA Calibration Working Group: Monitoring candidate Spectrophotometric Standard Stars against variability (17012 AOT17/08A), PI: E. Pancino(INAF-OA Bologna), Co–I: C. Cacciari, G. Altavilla, A. Bragaglia, M. Bellazzini, L. Federici et al., 60 hours, from February to July 2008
(approved in 2007), service mode
SPACE OBSERVATORIES
HST
55. HST+ACS, Deep photometry of NGC1569: understanding the
closest and strongest starburst of the nearby universe, PI: A.
Aloisi, Co–I: L. Angeretti, D. Romano, M. Tosi et al, 19 orbits,
January 2007,
56. HST+WFPC2, RR Lyrae stars in M31 Globular Clusters: How
did the M31 spiral galaxy form?,, PI: G. Clementini, Co–I:
C. Cacciari, L. Federici, F. Fusi Pecci, M. Marconi, R.
Contreras, M. Catelan, K. Kinemuchi, B. Pritzl, H.A. Smith,
78 orbits, Cycle 15, June-September 2007,
XMM–Newton
57. XMM+, Relics and Halos at intermediate redshifts: testing the
merging paradigm., PI: P. Mazzotta, Co–I: S. Giacintucci, S.
Bardelli, T. Venturi, et al., 58 ksec, August 2007,
221
58. XMM+pn/MOS, The ultradeep survey in the CDFS: an XMMNewton legacy, PI: A. Comastri, Co–I: R. Gilli, G, Zamorani, C. Vignali, K. Iwasawa et al., 1300 ksec, approved in December 2007,
59. XMM+pn/MOS, XMM observations of the most heavily obscured
AGN in the Swift-BAT survey, PI: M. Ajello, Co–I: A. Comastri, R. Gilli, et al., 224 ksec, approved in December 2007,
60. XMM-Newton+PN+MOS, The case of high metallicity in lowtemperature nearby galaxy clusters, PI: S. Ettori, Co–I: F. Gastaldello,
P. Tozzi, I. Balestra, F. Brighenti, S. De Grandi, M. Gitti, D.
Buote, 106 ksec, approved in December 2007,
Chandra
61. Chandra+ACIS–I, The Chandra Deep field south survey: a public Chandra legacy, PI: W.N. Brandt, Co–I: A. Comastri, R.
Gilli, C. Vignali, K. Iwasawa et al., 1000 ksec, approved in July
2007,
62. Chandra+ACIS-S, Towards a Complete Sample: 3CR Extragalactic Radio Sources with z ¡ 0.3, PI: D. Harris, Co–I: R. Gilli,
M. Chiaberge, D. Macchetto, S. Capetti, G. Risaliti, G. Giovannini, W. Sparks, P. Grandi, 224 ksec, Dec 2007 - June 2008,
Suzaku
63. Suzaku+XIS/HXD, Another Compton Thick AGN just around
the corner, PI: R. Gilli, Co–I: A. Comastri, C. Vignali, K.
Iwasawa, P. Ranalli, 90 ksec, approved in May 2007,
64. Suzaku+XIS/HXD, The powerful starburst and the COmpton
Thick pbscured AGN in NGC 6240, PI: P. Ranalli, Co–I: A.
Comastri, R. Gilli, C. Vignali, K. Iwasawa, et al , 150 ksec,
approved in May 2007,
222
65. Suzaku+XIS+HXD, The outskirts of NGC 1550 and MKW 4,
PI: F. Gastaldello, Co–I: D. Buote, F. Brighenti, S. Ettori, P.
Humphrey, B. Mathews, L. Zappacosta, 142 ksec, approved in
May 2007,
INTEGRAL
66. INTEGRAL+ISGRI, The ultra-deep INTEGRAL legacy hard Xray survey (amendment), PI: M. Ajello, Co–I: A. Comastri, R.
Gilli, et al, 2000 ksec, approved in December 2007,
223
11
Positions Held in Working Groups
and Science Policy Committees
• Bragaglia A.
Member of the Time Allocation Committee for TNG
Visiting Astronomer (Oct-Nov 2007) as part of the “Scientific
Visitor Programme” at ESO-Chile in Santiago
• Buzzoni A.
- Comisión Dictaminadora Externa dell’Instituto Nacional de
Astrofı́sica, Optica y Electrónica (Mexico): effective member
- RCEA (Registro Evaluadores Acreditados) del CONACyT (Mexico): effective member
- PRIN-INAF project “Un laboratorio per lo studio teorico delle
popolazioni stellari: nuove modellistiche e strumenti di indagine”:
National Coordinator
- Universitá di Bologna, corso di “Evoluzione delle popolazioni
stellari nelle galassie” (Laurea Specialistica in Astrofisica e Cosmologia): Professore a contratto
- CONICET (Buenos Aires, Argentina): Investigador Correspondiente
• Cacciari C.
- Science Committee for the Fondazione Osservatorio Astrofisico
di Castelgrande: member
- Management Team for the GAIA Coordination Unit 5 (CU5):
member
- GAIA CU5/DU14 (Instrument absolute response characterisation: definition and application): manager
224
• Clementini G.
- Supplementary Observations workpackage and Cepheids/RR
Lyrae of the Specific Object Studies workpackage, within GAIA
Coordination Unit 7 (CU7): manager
- PRIN-INAF project “From Local to Cosmological Distances”:
National Coordinator
• Comastri A.
- ESA XEUS (X-ray Evolving Universe Spectroscopy) Astrophysics Working Group: member
- NASA Chandra Cycle 8 TAC panel member
- COSMOS AGN Working Group: chair
- INAF Macroarea 1 “Galassie e Cosmologia”: Elected member
and coordinator
- INAF Unità operativa di programmazione: member
- Università di Ferrara: Professore a contratto
• de Ruiter H.R.
- Marie Curie Initial Training Network (ITN) (FP7 of the European Union): Expert Evaluator
- ESO OPC: Panel member
• Diolaiti E.
- Extremely Large Telescope Design Study (funded by the European Community under contract No 011863), “Novel Adaptive
Optics Concepts”: Workpackage manager
- LBT Near Infrared Adaptive Optics Test Cameras: Coordinator
- INAF, OABo & Bologna University, Phase A study of a multi–
conjugate adaptive optics module for the European ELT: Coordinator
225
• Ettori S.
- Chandra Cycle 10 TAC panel: member
- EDGE mission: responsable for science on galaxy clusters
- Contrattro ASI I/088/06/0: national PI
- PRIN-INAF 2006 e contratto ASI I/023/05/0: local PI
- Observatory “Thursday Seminars”: organizer
• Fusi Pecci F.
- Director of the Bologna Observatory
- INAF Dip.1: member of the Board
- INAF Dip.3: member of the TS Committee
- Cagliari Astronomical Observatory: member of the Board
- Sardinia Radio Telescope: member of the Board
- Consiglio Fondazione TT1 (Telescopio Toppo): member
• Gruppioni C.
- Scientist Associate to the Herschel-PACS Guaranteed Time
Extragalactic Surveys Consortium;
- Member of the Extragalactic Herschel Open Time Surveys
(“Extra-Hot”) Consortium;
- PRIN-INAF 2006 Galaxy Evolution from the Early Phases to
the Actual Universe: the IR and sub-millimeter view and Preparation for Herschel: PI
• Meneghetti M.
- EUCLID/DUNE mission: responsible of the italian pipeline for
image simulations used for preparing the DUNE proposal
226
• Origlia L.
- GIANO project: Principal Investigator
- ESO Instrument Science Team of X-shooter: member
- LBT Scientific and Technical Committee: member
- Member of Collegio dei Docenti di Dottorato del Dipartimento
di Astronomia dell’Università di Bologna, XXIII Ciclo
• Pancino E.
- DU13 (Instrument absolute response characterization: groundbased observations) within the GAIA DPAC (Data Processing and Analysis Consortium) CU5 (Photometry Coordination
Unit): manager
• Tosi M.
- Deputy Director of the Bologna Observatory
- INAF Committee for Macroarea 2 (Stellar populations and
interstellar medium): elected member and coordinator
- INAF Unità Operativa di Programmazione: member
- Bologna University, Collegio dei Docenti for the Astronomy
PhD: member
- Institute Visiting Committee of the Space Telescope Science
Institute (Baltimore USA): ESA member
- ESO Observing Program Committee: panel chair
- ESO ELT Standing Review Committee: member
- IAU Commission 37 (Open Clusters): member
- ASI: member of the Guppo di Lavoro per Cosmologia e Fisica
Fondamentale
• Zamorani G.
- zCOSMOS management team : member
227
- ESA Time Allocation Committee for Herschel : member
- ESA Concept Advisory Team for a European Dark Energy
Mission: member
- EUCLID-NIS WP3000 (Science): coordinator
• Zitelli V.
- Loiano telescopes: coordinator
- INAF Commission ”Piccoli telescopi ottici nazionali”: member
- Contract FP7 Science Access: member
228
12
Organization of Workshops
Bolzonella M.
- Member of LOC and editor of the proceedings of the conference
”A century of Cosmology”, San Servolo, Venice, August 27-31, 2007.
- International Referee of the Ph.D. Thesis of Florence Ienna, ”Evolution des propriétés globales des galaxies dans le Canada-FranceHawaii Telescope Legacy Survey”, defended on November 9, 2007,
supervisor Roser Pelló, Université Toulouse III - Observatoire MidiPyrénées.
Buzzoni A.
- Member of SOC of the international conference “New quests in
stellar astrophysics. II. Ultraviolet properties of evolved stellar populations” (Puerto Vallarta, Messico - Apr 2007)
Cacciari C.
- Member of the selection board for the INAF position of Astronomer at the OA Torino
- Member of the selection board for the INAF position of Astronomer at the OA Torino
- Member of the selection board for the contract (AR) to work on
Gaia absolute photometric calibration at the OA Bologna
- Member of the selection board for the contract (AR) to work on
Gaia absolute photometric calibration at the OA Bologna
- Contract to G. Altavilla, to work in GAIA CU5/DU13
- JAVA Workshop for the preparation of the Gaia pipeline, 11-13
June 2007, at the OA Bologna: organizer
Meneghetti M.
- Lecturer at the University ”Tor Vergata”, Rome, May 2007
229
13
Seminars and Visiting Astronomers
1. January 11 - Peter Coles (Nottingham University)
The Axis of Evil and Other Cosmic Anomalies
2. January 16 - Laura Ferrarese (Herzberg Institute of Astrophysics,
Canada)
The Inner Workings of Early-Type Galaxies: Supermassive Black
Holes and Stellar Nuclei
3. January 18 - Bianca Poggianti (INAF-OA Padova)
The evolution of the star formation activity and the galaxy environment
4. January 25 - Monica Colpi (University of Milano Bicocca)
Binary black holes in merging galaxies
5. February 1 - Raphael Hirschi (University of Basel)
The evolution of the first stellar generations
6. February 6 - Francesca Civano (PhD Bologna)
The co-evolution of Black Holes and their host galaxies: the high
energy perspective
7. February 8 - Jacopo Fritz (INAF-OA Bologna)
Star Formation Histories and stellar masses in Cluster Galaxies:
A Spectrophotometric Model Applied to the WINGS dataset
8. February 15 - Davide Grassi (LESIA Observatoire de Paris –
Meudon)
Infrared Spectroscopy of Planetary Atmospheres: General Concepts and Recent Achievements
9. February 22 - Giuseppina Battaglia (Kapteyn Institute, Gronigen)
Chemo-dynamical modelling of Dwarf Spheroidal Galaxies in the
Local Group
10. March 1 - Francesco Vissani (INFN GranSasso)
Neutrino masses, oscillations and implications for neutrino astronomy
230
11. March 8 - Fabrice Lamareille (INAF-OA Bologna)
The formation and evolution of galaxies as seen with the massmetallicity relation
12. March 15 - Alejo Martinez Sansigre (Max-Planck Heidelberg)
Obscured quasars at high redshift
13. March 22 - Scott Trager (Kapteyn Astr. Inst.)
Is downsizing universal? Stellar populations in the Coma Cluster
14. March 29 - Michele Cignoni (INAF-OA Bologna)
Recovering the star formation rate in the solar neighborhood
15. April 12 - Alessandro De Angelis (INFN, Università di Udine)
Gamma astroparticle physics: the MAGIC telescope and the
future
16. April 19 - John R. Brucato (INAF-OA Napoli)
Dall’astrochimica all’astrobiologia: cosa abbiamo imparato da
Stardust
17. April 26 - Mariachiara Rossetti (INAF-IASF Milano)
Looking at merging clusters in X-Rays
18. May 3 - Stefan Gottlber (AIP Potsdam)
The MareNostrum Universe
19. May 10 - Silvano Massaglia (Univ. Torino)
Stellar jets: Comparison between observations and models
20. May 17 - Paolo Padoan (Univ. of California, San Diego)
The Stellar IMF Now and Then
21. May 22 - Antonio Lazcano (Universidad Nacional Autonoma de
Mexico)
The emergence of life on Earth: recent advances, old problems
22. May 24 - Andrea Marcolini (University of Central Lancashire,
UK)
About the chemical enrichment of dSphs and Omega Centauri
231
23. May 31 - Katrien Uytterhoeven (INAF-OAB Brera-Merate)
The ground-based follow up of asteroseismic targets for the COROT
space mission
24. June 4 - Kenji Bekki (University of New South Wales, Australia)
Globular cluster systems and galaxy formation
25. June 8 - Art Wolfe (University of California, San Diego)
Bimodality in Damped Lyman alpha Absorption Systems
26. June 12 - Massimo Stiavelli (STScI)
Studio dell’epoca della reionizzazione con HST e JWST
27. June 21 - Brian McNamara (University of Waterloo, Canada)
Heating Hot Halos with Active Galactic Nuclei
28. June 22 - Brian McNamara (University of Waterloo, Canada)
Lecture 1: General Introduction to X-ray Clusters: Scaling Relations; Lecture 2: The Cosmic Cooling Problem and Galaxy
Formation in Cooling
29. June 28 - Guido Risaliti (INAF-OA Arcetri)
Infrared diagnostics of starbursts and AGNs in local and high-z
galaxies
30. September 6 - Vernesa Smolčić (MPIA, Heidelberg)
The dust-unbiased cosmic star formation history derived from
the faint radio population
31. September 13 - Luca Amendola (INAF/OA Roma)
The dark side of gravity
32. September 20 - Giuliana Fiorentino (INAF-OA Bologna)
Classical Cepheids: from theory to observation
33. September 27 - Eugenio Carretta (INAF-OA Bologna)
Evolving evolution: the not-so-simple Simple Stellar Populations
of Globular Clusters
34. October 11 - Andrea Cattaneo (AIP Potsdam)
Il ruolo dei buchi neri nella formazione e nell’evoluzione delle
galassie
232
35. October 18 - Luca Gasperini (ISMAR-CNR)
A possible impact crater for the 1908 Tunguska Event
36. October 23 - Nino Panagia (STScI, INAF & SN Ltd.)
SN1987A: twenty years later
37. October 25 - Luigi Stella (INAF-OA Roma)
The Giant Flare of 2004 Dec 27 and Fundamental Physics from
Magnetars
38. November 8 - Luca Tornatore (SISSA Trieste)
Cosmic structures in numerical simulations
39. November 13 - Federico Marulli (PhD Bologna)
Modeling the cosmological co-evolution of supermassive black
holes and galaxies
40. November 15 - Carlo Nipoti (Univ. Bologna)
The role of thermal evaporation in galaxy formation
41. November 22 - Alessio Mucciarelli (PhD Bologna)
Spectroscopic and photometric study of the stellar populations
in the Magellanic Clouds
42. November 29 - Andrea Morandi (PhD Bologna)
Properties of the gas and of the dark matter in X-ray galaxy
clusters with Sunyaev Zel’dovic measurements
43. December 6 - Gabriele Cocozza (PhD Bologna)
Searching for optical counterparts of Millisecond Pulsars in Globular Clusters
44. December 7 - Gregori Beskin (Special Astrophysical Observatory
- Russia)
Optical SETI at 6-meter telescope
45. December 11 - Simone Recchi (INAF-OA Trieste)
The early evolution of Tidal Dwarf Galaxies
46. December 13 - Vincenzo Antonuccio (INAF-OA Catania)
Physical models of AGN feedback: Simulations of jet-ISM/IGM
interactions
233
47. December 18 - Matteo Barnabè (Kapteyn Astronomical Inst,
Groningen)
Joint Gravitational Lensing and Stellar Dynamics Analysis of
Early-Type Galaxies
48. December 20 - Mattia Righi (MPA Garching)
Dust emission from merging galaxies as CMB foreground
Visiting Astronomers
1. Alessandra Aloisi (STSCI, Baltimore, USA) January 2007 [Tosi]
2. Laura Ferrarese (Herzberg Institute of Astrophysics, Victoria,
Canada) January 2007 [Tosi]
3. Katharina Glatt (University of Basel, CH) January 2007 [Tosi]
4. Raphael Hirschi (University of Basel, CH) February 2007 [Tosi]
5. Nino Panagia (STSCI, Baltimore, USA) October 2007 [Tosi]
6. Elena Sabbi (STSCI, Baltimore, USA) January and December
2007 [Tosi]
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14
“Laurea” thesis
1. Salvatore Giannetto, Proprietà spettrali dalla banda X al lontano infrarosso di un campione di AGN nella survey XMM/ELAISS1 (G. Palumbo, C. Gruppioni, A. Comastri, C. Vignali),
Marzo 2007
2. Gerardo Tomasulo, Analisi di un campione di spettri ad alta
risoluzione in ω Centauri (F.R. Ferraro, Elena Pancino), Marzo
2007
3. Enrica Bellocchi, Quasar oscurati: emissione infrarossa con
il satellite Spitzer (B. Marano, A. Comastri, F. Pozzi, C. Vignali), Luglio 2007
4. Laura Malagoli, Ottica adattiva multi-coniugata per LBT: un
sensore di fronte d’onda per LINC-NIRVANA (B. Marano, E.
Diolaiti), 2007
5. Veronica Biffi, The spherical collapse in Dark Energy models:
application to Galaxy Clusters (L. Moscardini, S. Ettori) Luglio
2008
6. Julian Merten (University of Heidelberg) Combined strong and
weak lensing mass reconstructions of galaxy clusters Bartelmann,
Meneghetti M.
235
15
PhD theses
1. Gabriele Cocozza, Binary Milli-Second Pulsars in Globular
clusters, XX cycle (advisors: F.R. Ferraro, F. Fusi Pecci)
2. Andrea Morandi, Effetto Sunyaev-Zeldovich di ammassi di
galassie selezionati nella banda X, XX cycle (advisors: L. Moscardini, S. Ettori)
3. Alessio Mucciarelli, Photometric and spectroscopic study of
the stellar populations in the Large Magellanic Cloud, XX cycle
(advisor: F.R. Ferraro, L. Origlia)
4. Emanuele Dalessandro, Multiwavelength observations of stellar populations in globular clusters, XXI cycle (advisors: F.R.
Ferraro, B. Lanzoni)
5. Francesco Paci, Spettri della polarizzazione della radiazione
cosmica di fondo, XXI cycle (advisors: L. Moscardini, F. Finelli)
6. Gianluca Lombardi, Valutazione sinottica dei parametri meteorologici e loro impatto sulle osservazioni astronomiche, XXI
cycle (advisors: V. Zitelli, B. Marano)
7. Rodrigo Contreras, Variable stars in the field and globular
clusters of the Andromeda galaxy (M31), XXII cycle (Advisors:
B. Marano, G. Clementini)
8. Graziano Coppa, The cosmic mass assembly history of galaxies: a multi-dimensional study bas ed on deep redshift surveys,
XXII cycle (advisors: B. Marano, M. Mignoli, G. Zamorani)
9. Matteo Correnti, Stellar relics of the hierarchical assembly of
the Galaxy, XXII cycle (advisors: F.R. Ferraro, M. Bellazzini)
10. Annamaria Donnarumma, Testing the consistency of lensing
and X-ray mass estimates in galaxy clusters, XXII cycle (advisors: L. Moscardini, S. Ettori, M. Meneghetti)
11. Sara Fabbri, Studio della perdita di massa nelle stelle giganti di
Popolazione II con osservazioni SPITZER, XXII cycle (advisors:
F.R. Ferraro, L. Origlia, F. Fusi Pecci)
236
12. Vincenzo Guido, Development and optimization of graphic
user interfaces for infrared spectr ometers at TNG, XXII cycle
(advisors: B. Marano, L. Origlia)
13. Silvia Marinoni, Calibration plan, quality control and optimization of data analysis for red and infrared spectroscopic observations from TNG and other ground-based telesco pes, XXII
cycle (advisors: B. Marano, L. Origlia)
14. John Morgan, The application of grid technology to radioastronomy data reduction and ana lysis, XXII cycle (advisors: D.
Dallacasa, H.R. de Ruiter)
15. Sibilla Perina, Peculiar star clusters in M31: an HST view,
XXII cycle (advisors: F.R. Ferraro, M. Bellazzini, L. Federici )
16. Cristiano De Boni X-ray properties of galaxy clusters in cosmologies with dynamical dark energy, XXIII cycle (advisors: L.
Moscardini, S. Ettori)
17. Metteo Lombini Progetto di un modulo di ottica adattiva multiconiugata per il telescopio E–ELT, XXIII cycle (advisors: B.
Marano, E. Diolaiti)
18. Elisabetta Lusso A panchromatic vew of the evolution of supermassive black holes, XXIII cycle (advisors: L. Ciotti, A. Comastri)
19. Giulia Macario Storia della formazione stellare in galassie
risolte, XXIII cycle (advisors: B. Marano, M. Tosi)
20. Michele Moresco Vincoli sull’energia oscura dalle età di galassie
ellittiche, XXIII cycle (advisors: A. Cimatti, L. Pozzetti)
21. Rashmi Verma Software development to carry out sky surveys
with a 20 GHz 7–horns multibeam, XXIII cycle (advisors: L.
Gregorini, I. Prandoni, H. de Ruiter)
237
16
Post-Doctoral, Post-Laurea fellowships
and Contracts
1. Altavilla, Giuseppe
2. Angeretti, Luca
3. Beccari, Giacomo
4. Cignoni, Michele
5. Cocozza, Gabriele
6. Contreras, Rodrigo
7. Coppa, Graziano
8. Fiorentino, Giuliana
9. Fritz, Jacopo
10. Galleti, Silvia
11. Gastaldello Fabio
12. Gitti, Myriam
13. Greco, Claudia
14. Lamareille, Fabrice
15. Lanzoni, Barbara
16. Lombardi, Gianluca
17. Melioli, Claudio
18. Montemaggi, Matteo
19. Perina, Sibilla
20. Poppi, Francesco
21. Romano, Donatella
22. Rossetti, Emanuel
238