Small Telescopes for Big Science from Space

Transcript

SmallTelescopesforBig
SciencefromSpace
IsabellaPagano
INAF
OsservatorioAstrofisicodiCatania
ChiantiTopics2016
13May2016
CHEOPS and PLATO
the ESA S1 & M3 missions
in the Cosmic Vision 2015-25
Solar System
51 Pegasi
Mayor & Queloz 1995
•  ~2300 years after Epicurus
•  ~500 years after Nicolaus Cusanus
• 
more than 400 years after Giordano Bruno
51 Peg: a ~0.5 MJ planet,
orbiting a solar type star in
~4.2 d a~0.05 AU) AWG/SSEWG meeting| A.M. Heras | 22/05/2013 | ESA/SRE | Slide ‹n.›
ESA UNCLASSIFIED – For Official Use
20YearsAfter
51Pegb
1356sistemiplanetari
•  How do planets and planetary systems form and
evolve?
2116pianeti
•  Is our Solar System special or are there other systems
512sistemiconpianetimultipli
like ours?
•  Are there potentially habitable planets?
www.exoplanets.eu
ChiantiTopics2016-13May2016
Inthepast20years
Mass
Jupiter
Neptun
Earth
Jupiter
Neptun
Earth
Radius
Detections
RadialVelocity
Planetsdatafromhttp://exoplanet.eu/uptoMay2016
Detections
RadialVelocityTransits
Detections
RadialVelocityTransitsImaging
Detections
RadialVelocityTransitsImagingTiming
Detections
Massa[M/MGiove]
RadialVelocityTransitsImagingTimingMicrolenses
Distanzastella-pianeta[UA]
TheEP-RATRoadmap
ESA EXOPLANET ROADMAP ADVISORY TEAM – Oct 2010
Timeanddifficulty
Timeanddifficulty
Rome,5Nov2014
RADIALVELOCITYANDTRANSITS
RV&Transits:
thepowerofcomplementarity
TransitMethod
Radialvelocitymethod
•  Orbitparameters
•  Orbitalinclination,i
•  Planetradius,Rp
•  Orbitalparameters
•  Minimumplanetmass,Mpsini
Trueplanetmassandmeandensity
Telescopio
Nazionale
Galileo
HARPS- N
The Kepler revolution
•  Launched in 2009
•  Still working as K2
•  FoV ~100 sqdeg •  (0.25 % of the sky) • 
➡  4706 planet candidates
➡  2326
1041 confirmed planets
http://kepler.nasa.gov
~ 145 000 stelle
Smallplanetsarecommon
SizefromKepler
MassfromRadialVelocitySurvey
are
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onths
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ays
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,
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(Ma
BUTmassandradiusmostlycomefromdifferent
techniques:fewobjectswithbothmeasurements
FromCoRoT,KeplerandMost
➔Diversityofsuper-Earths
ü  Massesvarybya
factorof~4
(withlargeerrors)
ü  Radiivarybya
factorof~3
➔
Accuratemasses&radiiarerequiredtoseparate
terrestrialfrommini-gasplanets
Super-Earths:diversity
andimplicationsonhabitability
SolarSystemplanetsareNOTthegeneralrule:
small≠>rocky,large≠>gaseous
•  Smallexoplanetsareverydiverse:
fromEarth-liketomini-gasplanets
•  Mini-gasplanetsarelikelynothabitable
•  Silicate-ironplanetsareprimetargetsforatmospherespectroscopy
SearchingforHabitabilityrequires:
➢ accuratemeandensitiestoidentifyterrestrialplanets
➢ bulkcharacterizetargetsforatmospherespectroscopyfollow-up
Planetdiversity
Earth 5.5g/cm3
•  PlanetsofEarthmassandbelowremaintobe
detectedandcharacterized
GJ1214b 1.6g/cm3
Minigasplanets
<~1g/cm3
• ➔Needmeandensitiestoseparate
terrestrialplanetsfrommini-gasplanets
Planetdiversityandplanet
formation
Testplanetformation
models:
•  Whatisthe
observedcritical
coremass?How
massivecanasolid
coregrowbefore
accretingvolatiles?
•  Cansuper-massive
rockyplanetsexist?
Howarethey
formed?
•  ArelightplanetswithH2-dominatedatmospherescommon?
Abiasedview
Ourknowledgeonplanetnatureislimitedto
close-inplanetssofar.
Allplanets
PlanetswithP>80days
Super-Earthsinthehabitable
zone
Detectedsuper-Earths
•  Goal:Detectand
characterizesuperEarthsinhabitable
zones
•  Status:veryfewsmall/
lightplanetsin
habitablezones
detected
Super-Earthsinthehabitable
zone
Super-Earthswithmeasuredradiusandmass
•  Goal:Detectand
characterizesuperEarthsinhabitable
zones
•  Status:veryfewsmall/
lightplanetsin
habitablezones
detected
No„super-Earths“
withknownmean
densityinthe
habitablezone!
Theneedforbrightstars
Knownplanetsfromradialvelocityandtransitsurveys
Whyhavesofewtargetsbeen
characterized?
-Transitsurveystargetedfaintand
distantstarstomaximizedetection
performance.
- Radialvelocitysurveysneedbright
stars(≤11mag)tokeeptelescope
resourceslimited.
Lessonslearned:
Futuretransitmissionsmusttargetbrightstars!
MissionsandObservatoriesfor
Exoplanets
CoRoT
PLATO
Survey
Kepler
K2
GAIA
Spitzer
GAIA
LBT
HST
TESS
E-ELT
CHEOPS
JWST
Characterization
Ariel?
Spica?
GAIA
Biased toward massive, cool planets
hosted by low-mass, nearby stars
(a poorly explored region, so far)
GAIA is expected
to discover
~25,000 such
planets, of which
25-40 transiting
(Perryman+ 2014);
~1,000 will be
brighter than G~8.
Transitmissions:What’snext?
K-2(Kepler2)
(NASA)
observefieldsintheeclipticplane
for~80days/field
CHEOPS
(ESA,launch2018):
follow-up,radiiofdetected(RV)
planets,
TESS
(NASA,launch2017):
scanthewholesky,~1month/
field,~2%ofskyatpolesfor1year
PLATO
(ESA,launch2024)
detectandcharacterize(density,
age)terrestrialplanetsaround
solar-likestarsuptothehabitable
zone
–  Sclassmission(S1)
–  Budgetenvelope<150M€(≤50M€fromESA)
–  Launch:endof2018=>fastdevelopment(TRL5whenselected)
–  Operation:3.5(+1.5)yrs-sharedlaunch
Mirrordiameter:33cm
PayloadWeight:60kg
Totalweight:250Kg
CHEOPSmainsciencegoals
Ø  Perform1st-stepcharacterisationofsuper-earths&
neptunes
bymeasuringaccurateradii&bulkdensitiesforsuchplanetsorbiting
brightstars
Ø  Providegoldentargetsforfuture
atmosphericcharacterisation
Howitworks
ü  High-precisionphotometry
ü  Achieveaphotometricprecision
similartoKepler
ü  Observingbrighterstarsanywhereinthe
sky
©CHEOPSConsortium
byfindingtheplanetsmostamenabletodeepatmosphericstudies
CHEOPS strategy: Follow-up!
TESS
(2017)
Ground-basedtransitsurveys
NGTS(2014)
nown
k
f
o
t
i
s
n
etra
Detectth s
th
super-Ear
Ground-basedRVsurveys
HARPS,HARPS-N,HIRES,SOPHIE(ongoing)
ESPRESSO(2017)
20%opentime
(3.5-yrmission)
©CHEOPSConsortium
K2
(2014)
CHEOPS legacy & synergy!
TESS
JWST
2018
©CHEOPSConsortium
E-ELT,
GMT,TMT
>=2024
CHEOPS The Telescope
telescope
internalbaffle radiators
primary
baffle
baffle cover secondarybaffle
vanes
telescope
structure
CCD
300mm
startracker
©CHEOPSConsortium
focalplane
module
back-end
optics
secondarymirror
primarymirror
Mirrordiameter:33cm-Weight:60kg
OpticsmadeinItaly
•  INAF
•  Oss. Astronomico Padova
•  Oss. Astrofisico di Catania
•  SELEX ES
•  Thalenia Alenia Space
•  Medialario
STM1
PFM
STM2
PFM
STM
STMTVtests
PLATO
PLAnetaryTransits&OscillationsofStars
– Mclassmission(M3)
– Budgetenvelope~650M€(≤500M€fromESA)
– Launch:2024–LauncherSoyuzFregatfrom
Kourou
– Operation:6.25(+2)yrs
©PLATO@INAF
LargeFoVconcept
Searchingfor
transitsofBright
Stars➔
➔ largeFoV!
Segmentationistheonly
possiblesolution
OnePLATOtelescope
©PLATO2.0 @INAF
FoV~∼1200sqdeg(12timesKepler)–likeacircleof39degdiameter
Telescopesonthesatellite
Ø  32 “Normal” telescopes: 4 sets of 8 telescopes
Ø  2 “Fast” telescopes
FastandNormalTelescopes
«normal»
NORMAL
FullframeCCD
4510×451018μmsqpx
mV > 8
t=25s
«fast»
FAST
FrametransferCCD
4510×225518μmsqpx
mV ~4–8
t=2.5sAOCS
ü 
ü 
ü 
ü 
132CCDs➔~0.95sqmeter
1FEE/camera;
1DPU/2cameras;
2ICUsincoldredundancy
PLATO–thesetof34telescopes
24timesKepler
©PLATO@INAF
OverlappingFoV∼2250sqdeg,equivalenttoacircleof~53degdiameter
PLATOScienceGoals
fromtheSMP
• 
Determineplanetbulkproperties(mass,radiusandmeandensity)
• 
Studyhowplanetsandplanetsystemsevolvewithage
• 
Studythetypicalarchitecturesofplanetarysystems
• 
Analysethecorrelationofplanetpropertiesandtheirfrequencieswith
stellarparameters(e.g.,stellarmetallicity,stellartype)
• 
Analysecorrelationswiththeenvironmentinwhichtheyformed
• 
Identifytargetsforspectroscopytoinvestigateplanetaryatmospheres
• 
Studytheinternalstructureofstarsandhowitevolveswithage
• 
+guestobserverprogram(complementaryandlegacysciencetopics).
TheMethod
Photometrictransit
▪  radius~2%
RV–follow-up
▪  Mass~10%
▪  Age~10%
Example:Kepler-10b(V=11.5mag)
©PLATO2.0Consortium
Asteroseismology
ExoplanetsandStars
Characterizationofexoplanets…needscharacterizationofstars
•  Mass+radiusèmeandensity
•  Stellarmass,radius
gaseousvs.rocky,composition,structure deriveplanetmass,radius
•  Stellartype,luminosity,activity
planetinsolation
•  Age
•  Stellarage
planetandplanetarysystemevolution
definesplanetage
©PLATO2.0
Consortium
•  Orbitaldistance,atmosphere
habitability
ObservingStrategy
The observing duty cycle will be at least 95%.
ThePLATOsky
à~50%skycoverage
PLATOSatellite
•  Threecompetativeindustrystudiesongoinguntilend2016.
Ø  3-axis stabilised
Ø  Mass ~ 2000 kg
Ø  Pointing error: 0.2 arcsec Hz-1/2 over time scales of 25 s to 14 hours.
Astrium
TAS
OHB
Groundstations
New Norcia
(Australia, 35 m)
Cebreros
(Spagna, 35 m)
Ø  K-band telecommunications,
Ø  downlink telemetry ~400 Gbit per day
Malargüe
(Argentina, 35 m)
Whodoeswhat
ESA
• 
• 
• 
• 
Satellite
MissionOperationCenter(MOC)
ScienceOperationCenter(SOC)
Launcherandlaunchfacilities
PLATOMissionConsortium:
•  Payload
•  DataCenter(PDC)
•  PlatoScienceManagement(PSM)
Organization
ThePLATOCommunity
PLATOinItalia
Accordo ASI-INAF "PLATO Fasi B2/C” - n.2015-019-R0del29luglio2015
ü  INAF
–  OACatania(Science,Payload)
–  OAPadova(Science,Payload)
–  OABrera(Science,Payload)
–  IAPS-Roma(Science,Payload)
–  FGG(Payload)
–  OAPalermo(Science)
–  OATorino(Science)
–  OACapodimonte(Science)
–  OARoma(+Teramo)(Science)
–  OAArcetri(Science)
ü  PaduaUniversity,Physics&AstronomyDep.(Science)
ü  ASI-ASDC(PDC,Science)
Ø Italian Scientific Responsible: I. Pagano
Ø Members of the Advisory Science Team: G. Piotto, R. Ragazzoni
Ø Members of the PMC Board: I. Pagano, G. Piotto
www.plato-mission.eu
www.oact.inaf.it/plato/Plato-Italia/
PLATOItalianTeam
E. Antonello (INAF-OAB), L. Affer (INAF-OAPA), M. Barbieri (Univ. Padova), St. Basso (INAFOAB), L. Bedin (INAF-OAPD), A. Bellini (Univ. Padova), S. Benatti (INAF OAPD), M. Bergomi
(INAF-OAPD), A. Bonanno (INAF-OACT), F. Borsa (INAF-OAB), R. Bonito (Univ. Palermo), G.
Bono (INFN), A.S. Bonomo (INAF-OATO), L. Borsato (Univ. Padova), E. Brocato (INAF-OAR),
A. Bressan (INAF-OAPD), R. Buonanno (INAF-OACTe, INFN), D. Cardini (INAF-IAPS), E.
Carolo (INAF-OAPD), S. Cassisi (INAF-OACTe), M. Castellani (INAF-OAR), R. Claudi (INAFOAPD), R. Cosentino (INAF-OACT, FGG), G. Cutispoto (INAF-OACT), M. Damasso (INAFOATO), D. De Martino (INAF-OAC), S. Desidera (INAF-OAPD), S. Di Franco (Univ. Florence),
M. Dima (INAF-OAPD), A.M. Di Giorgio (INAF-IAPS), M.P. Di Mauro (INAF-IAPS), J. Farinato
(INAF-OAPD), E. Flaccomio (INAF-OAPA), M. Focardi (Univ. Florence), P. Giommi (ASDC), L.
Girardi (INAF-OAPD), G. Giuffrida (ASDC), G. Giusi (INAF-IAPS), M. Ghigo (INAF-OAB), V.
Granata (Univ. Padova), D. Greggio (INAF-OAPD), A.F. Lanza (INAF-OACT), A.C. Lanzafame
(UNICT), M.G. Lattanzi (INAF-OATO), G. Leto (INAF-OACT), C. Maceroni (INAF-OAR), D.
Magrin (INAF-OAPD), L. Malavolta (Univ. Padova), L. Marafatto (INAF-OAPD), M. Marconi
(INAF-OAC), P. Marigo (Univ. Padova), P.M. Marrese (ASDC), F. Marzari (Univ. Padova), D.
Mesa (INAF-OAPD), S. Messina (INAF-OACT), J. Montalban (Univ. Padova), M. Munari (INAFOACT), U. Munari (INAF-OAPD), I. Musella (INAF-OAC), V. Nascimbeni (OAPD-INAF), R. Orfei
(INAF-IAPS), S. Ortolani (Univ. Padova), E. Pace (Univ. Florence), I. Pagano (INAF-OACT), F.
Palla (INAF-OAA), M. Pancrazzi (Univ. Florence), St. Pezzuto (INAF-IAPS), G. Picogna (Univ.
Padova), A. Pietrinferni (INAF–OACTe), G. Piotto (Univ. Padova), E. Poretti (INAF-OAB), L.
Prisinzano (INAF-OAPA), R. Ragazzoni (INAF-OAPD), G. Raimondo (INAF – OACTe), M.
Rainer (INAF-OAB), V. Ripepi (INAF-OAC), G. Scandariato (INAF-OACT), S. Scuderi (INAFOACT), R. Silvotti (INAF-OATO), R. Smart (INAF–OATO), A. Sozzetti (INAF-OATO), D. Spiga
(INAF-OAB), P. Ventura (INAF-OAR), V. Viotto (INAF-OAPD)
SciencePreparation
FieldCharacterizationand
TargetSelection
• 
• 
2"long-duration"(LD)fields+"step&stare"(S&S)fields
Scientificrequirements:5stellar(dwarfs&giants)samples(P1–P5)
– 
– 
– 
– 
– 
• 
P1≥20000starsinLDfields(spectraltype>F5;V<11)
P2≥1000starsinLDfields(V<8)
P3≥3000stars(extensionofP2)inLDand/orS&Sfields
P4≥10000Mstars(5000inLD+5000inS&S)
P5≥245000starsinLDfields(V<13)
PLATOwillnotdownloadtheimages
– 
– 
P1–P5selectedinadvance
Spectral-typeselection
• 
Nosuitableall-skycatalogsexistforstellarparameters
Ø 
Gaia:intermediatecatalogreleasein2017
1. 
2. 
3. 
4. 
Single-catalogdependenceisarisk
GaiawillbeaffectedbycrowdingatlowGalacticlatitudes
Degeneracybetweenparameters(temperatureandinterstellarextinction)
Complementarycatalogs
Ø 
Analysisofavailablecatalogsinliterature(UCAC4,RAVE,…)
Ø 
Analysisoftheoreticalmodels(GUMS)andavailabletechniques
Ø 
UCAC4-RPM:anewad-hocall-skydatabaseforFGKMstars,basedon
alreadyknowntoolsandcatalogs
l. in preparation
tto, et a
Nascimbeni, Pio
ItalianTOUTeam
e-mail:[email protected]
•  INAF-OAB:StefanoBasso,FrancescoBorsa,Mauro
Ghigo,DanieleSpiga;
•  INAF-OACT:MatteoMunari,IsabellaPagano,Gaetano
Scandariato,DanielaSicilia;
•  INAF-OAPD:MariaBergomi,SimonettaChinmellato,
MarioDima,DavideGreggio,JacopoFarinato,
DemetrioMagrin,LucaMarafatto,RobertoRagazzoni,
ValentinaViotto.
TelescopeBreadboards
©PLATO@INAF
Testingthetelescopebreadboardinto
thespaceenvironment…
Workinprogress
Selection of prime contractor almost
completed
ItalianICUTeam
e-mail:[email protected]
•  INAF-FGG:R.Cosentino;
•  INAF-IFSI:S.Pezzuto,M.Benedettini,D.
Biondi,A.DiGiorgio,G.Giusi,G.LiCausi,J.Liu,
R.Orfei;
•  INAF-OAA:M.Focardi,M.Pancrazzi,E.Pace,
S.DiFranco.
Dataproducts
ü 
ü 
ü 
ü 
Imagettes
Light curves and centroids
Housekeeping
Quality data
L0
L1
ü  Planetary transit candidates and
their parameters
ü  asteroseismological analysis
ü  stellar rotation periods and stellar
activity properties
ü  seismically-determined stellar
masses, radii and ages of stars
ü  TTV planetary systems
L2
Lg
L3
Calibrated Light curves
Next slide
Processed imagetttes
Ancillary data
ü  list of confirmed planetary systems, which will
Quality data
be fully characterised by combining
information from the planetary transits, the
seismology of the planet-hosting stars, and
the results of ground-based observations.
ü 
ü 
ü 
ü 
Ground-basedobservationsdata(Lg)
•  Ground-basedobservationsforfilteringfalseplanet
transits:
– 
– 
– 
– 
– 
Low-precisionspectroscopy(1-2mtelescopes);
High-resolutionimaging(2mtelescopes);
Onandofftransitphotometry(1-2mtelescopes);
High-resolutionspectroscopy(4-8mtelescopes);
Rossiter-McLaughlin(RM)observations(8mtelescopes).
•  Ground-basedobservationsforthecharacterisationof
planets:
–  High-resolutionspectroscopy(1-2m,4mand8m
telescopes);
–  Rossiter-McLaughlin(RM)observations(8mtelescopes).
Ground-basedObservation
Programme
ing
g
a
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a
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s
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sampl ESO Large
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or mo
Fewhardestcases(e.g.,faintesthostswithEarthsinthehabitablezone)
willneedE-ELT
FlowdiagramofPLATO
operations
PLATOStatus
✓  PHASEB2inprogress
✓  MissionAdoptionReview:ongoing
✓  PDR:summer2017
AdoptioninNov2016
Launchin2024
Planetyields
Prospectsforcharacterized
super-Earthsinthehabitablezone
„Super-Earths“withmeasuredradiusandmass
TESSeclipticpoles
TESS,CHEOPS,K2willmainlycoverorbitalperiodsupto~80days
PLATOmisureràladensitàdei
pianetipiccoliconP>80g
„Super-Earths“withmeasuredradiusandmass
PLATOuniqueness
Allplanets
Ourknowledgeonplanet
natureislimitedtoclose-in
planetssofar.
PLATOwillfilltheparameterrange
forlongorbitalperiods
Studyplanetswheretheyform!
©PLATO2.0
Consortium
PlanetswithP>80days
Planets,planetarysystemsand
theirhoststarsevolve
Formationinprotoplanetarydisk,
migration
Lossofprimary
atmosphere
PLATOwillforthefirsttimeprovideaccurate
Stellarradiation,windand
agesforalargesampleofplanetarysystems
magneticfield
Cooling,
Planetaryevolutionstudieswillbepossible!
Cooling,
differentiation
Secondary
atmosphere
©H.Rauer(DLR)
life
(plate)-
tectonics
differentiation
ApossibleHR-likediagram
forplanets?
TheEP-RATRoadmap
ESA EXOPLANET ROADMAP ADVISORY TEAM – Oct 2010
Timeanddifficulty
Timeanddifficulty
Rome,5Nov2014
TESS
nominal
??
CHEOPS
goal
JWST
PLATO
E-ELT
??
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PLATO 2.0 (PLAnetary Transits and Oscillations of stars) is a medium class (M class)
mission studied in the framework of the ESA Cosmic Vision 2015-2025 program.
The scientific goals of PLATO 2.0 are:
• reveal the interior of planets and stars
• detect planets over the whole sky, including
terrestrial planets in the habitable zone
• constrain planet formation and evolution
• provide accurate ages of planetary systems
• provide targets for atmosphere spectroscopy
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@PLATOMissionCon
12 Jan
NEWS
PLATO sui Media
Clicca su News per saperne di più (in inglese).
ESA Cosmic Vision. Presentation of the
#M3competition, January 21st Paris
sci.esa.int/M3missions2014 come and
support #PLATO 2.0
ESA/SRE(2011)13 - Red Book
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s
u
e
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e
t
p
i
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http://www.plato-mission.eu
wo
web
Expand
Key strategy for PLATO 2.0 is the observation of a
large sample of bright stars. In this way PLATO 2.0
is able to completely characterize the discovered
planets and their hosting stars. Specifically, the
characterization includes the seismic analysis of the
parent stars in order to precisely determine their
mass, radius and age, i.e. those fundamental
parameters that are required to precisely derive the
same quantities for the hosted planets.
ESA Cosmic Vision #PLATO Preliminary
Requirement Review Report
sci.esa.int/plato/53525-pl…
#M3competition
PLATO ESA website
ESA Cosmic Vision #PLATO 2.0 Yellow
Book sci.esa.int/plato/53450-pl…
@PLATOMissionCon
11 Jan
Expand
@PLATOMissionCon
Le attività PLATO in ITALIA sono finanziate
dall’Agenzia Spaziale Italiana.
Durante lo studio di definizione con
contratto ASI-Univ. di Padova No.
I/044/10/0 del 25/10/2010.
11 Jan
Moreover, the planetary systems discovered by PLATO 2.0, being bright, can be followed-
PLATO (PLAnetary Transits and Oscillations of stars) è una
missione di classe media (classe M) studiata nell’ambito del
programma ESA Cosmic Vision 2015-2025.
Scopo scientifico principale della missione è la scoperta e lo
studio di sistemi planetari extrasolari tramite l’identificazione
e l’analisi dei transiti.
PLATO osserverà un grande campione di stelle brillanti e
permetterà la completa caratterizzazione dei pianeti e delle
loro stelle ospiti. In particolare, la caratterizzazione include
l’analisi sismica delle stelle ospitanti pianeti dalla quale
ottenere una precisa misura di masse, raggi ed età, parametri
fondamentali per poi ricavare una precisa misura delle stesse
quantità per i pianeti ospitati.
L’acronimo PLATO
coincide con il
nome inglese del
filosofo PLATONE.
Secondo la
testimonianza di
Simplicio (VI secolo
d.C.), Platone
avrebbe proposto
agli astronomi
http://www.oact.inaf.it/plato/Plato-Italia/Home.html
ChiantiTopics 2016 - 13 May
2016

Small Telescopes for Big Science from Space

Transcript

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