A guided tour to VLTI
Transcript
A guided tour to VLTI
er et m ro fe er e nt cop s ele ge ar y er r ne bi om ec am l ca ti ul mi no ro st Data and calibration of A M BE R / V L T I Florentin Millour ( ) And the A.M.BE.R. consortium Osservatorio Astrofisico di Arcetri Consortium website : http://amber.obs.ujfgrenoble.fr Accardo Matteo, Acke Bram, Agabi Karim, Altariba Evelyne, Antonelli Pierre, Arezki Brahim, Aristidi Eric, Baffa Carlo, Beckmann Udo, Behrend Jan, Blöcker Thomas, Bonhomme Serge, Bresson Yves, Busoni Simone, Casoli Fabienne, Cassaing Frédéric, Chelli Alain, Clausse JeanMichel, Colin Jacques, Connot Claus, Debouzy Geneviève, Delboulbé Alain, Domiciano de Souza Armando, Dugué Michel, Duvert Gilles, Driebe Thomas, Exertier Pierre, Feautrier Philippe, Ferruzzi Debora, Forveille Thierry, Fossat Eric, Foy Renaud, FraixBurnet Didier, Gallardo Agustin, Gennari Sandro, Giani Elisabetta, Gil Carla, Glentzlin André, Glück Laurence, Heiden Manfred, Heininger Matthias, Hernandez Oscar, Hofmann KarlHeinz, Kamm Daniel, Kern Pierre, Lagarde Stéphane, Lagrange AnneMarie, Le Coarer Étienne, Le Contel Danielle, Lecontel JeanMichel, Lisi Franco, Lopez Bruno, Malbet Fabien, Magnard Yves, Marconi Alessandro, Mars Gilbert, MartinotLagarde Grégoire, Mathias Philippe, Mège Pierre, Millour Florentin, Monin JeanLouis, Montmerle Thierry, Mouillet David, Mourard Denis, Nussbaum Edmund, Ohnaka Keiichi, Pacheco José, Pacini Franco, Perraut Karine, Perrier Christian, Petrov Romain, Puget Pascal, Rabbia Yves, Rebattu Sylvestre, Reynaud François, Richichi Andrea, Robbe Sylvie, Roussel Alain, Sacchettini Michel, Salinari Piero, Salvati Marco, Schertl Dieter, Solscheid Walter, Stee Philippe, Stefanini Paolo, TallonBosc Isabelle, Tallon Michel, Tasso Daniel, Tatulli Éric, Testi Leonardo, Vakili Farrokh, Valtier JeanClaude, van der Lühe Oskar, Vannier Martin, Ventura Noël, Weigelt Gerd, Zins Gérard Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Cophased and collimated beams from telescopes Detector Telescopes “Basic” interferometer Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Detector Telescopes 3T monomode spectrointerferometer Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 AMBER Spectrograph and detector VLTI Calibration and alignment units Osservatorio Astrofisico di Arcetri Spatial filters (optical fibers) F. Millour, ESO, 26/01/07 The AMBER raw data Photometric beams Interferometric beam Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Spectral calibration ² Vel Atype star Telluric lines Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Spectral calibration Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Spectral calibration d e d u l c n n i a l y p l t n n o e i r t r a u r c b i t l a o c N e h t in Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Flux (e) Flux (e) The P2VM algorithm #Pixel #Pixel Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Flux (e) Flux (e) The P2VM algorithm #Pixel #Pixel Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 The P2VM algorithm X = P2VM "Instrumental fringes" "cleaned" data Matrix multiplication Osservatorio Astrofisico di Arcetri Observables (Complex coherent flux) F. Millour, ESO, 26/01/07 AMBER observables Complex coherent flux : i, j C =2 N V T measured on M frames Photometric beams Interferometric beam Spectrum : S = N() Visibility : Vi,j = |Ci,j()| / N() Phase closure : 123 = atan<C1,2C2,3C*1,3> Diff. phase : i,jdiff Diff. visibility : Vi,jdiff “Phase closure” of diff. phases : 123diff 1,2diff2,3diff3,1diff Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 The amdlib library Handles all the data reduction steps, both online and offline GUI : Gasgano, ammYorick, GreG Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 The P2VM algorithm Is valid IF : the instrument is stable enough between calibration and observations SNR on the P2VM is enough The spectral channels are thin enough The detector cosmetics is well enough known The wavelength calibration is OK Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 The P2VM algorithm Is valid IF : the instrument is stable enough between calibration and observations SNR on the P2VM is enough The spectral channels are thin enough The detector cosmetics is well enough known The wavelength calibration is OK Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 The P2VM algorithm Is valid IF : the instrument is stable enough between calibration and observations SNR on the P2VM is enough The spectral channels are thin enough The detector cosmetics is well enough known The wavelength calibration is OK Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 The P2VM algorithm Is valid IF : the instrument is stable enough between calibration and observations SNR on the P2VM is enough The spectral channels are thin enough The detector cosmetics is well enough known The wavelength calibration is OK Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 The P2VM algorithm Is valid IF : the instrument is stable enough between calibration and observations SNR on the P2VM is enough The spectral channels are thin enough The detector cosmetics is well enough known The wavelength calibration is OK Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 The P2VM algorithm Is valid IF : the instrument is stable enough between calibration and observations SNR on the P2VM is enough The spectral channels are thin enough The detector cosmetics is well enough known The wavelength calibration is OK Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 The P2VM algorithm Is valid IF : the instrument is stable enough between calibration and observations SNR on the P2VM is enough The spectral channels are thin enough The detector cosmetics is well enough known The wavelength calibration is OK Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 The P2VM algorithm Is valid IF : the instrument is stable enough between calibration and observations SNR on the P2VM is enough The spectral channels are thin enough The detector cosmetics is well enough known The wavelength calibration is OK G. Li Causi 2006 Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 The P2VM algorithm Is valid IF : the instrument is stable enough between calibration and observations SNR on the P2VM is enough The spectral channels are thin enough The detector cosmetics is well enough known The wavelength calibration is OK Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 The P2VM algorithm Is valid IF : the instrument is stable enough between calibration and observations SNR on the P2VM is enough The spectral channels are thin enough The detector cosmetics is well enough known The wavelength calibration is OK Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 The P2VM algorithm Is valid IF : the instrument is stable enough between calibration and observations SNR on the P2VM is enough The spectral channels are thin enough The detector cosmetics is well enough known The wavelength calibration is OK Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Instrumental contrast on the sky Lab visibility : On sky exp. visibility (FSU) : On sky exp. visibility (no FSU) : 0.85 0.85 0.60 NO FINITO ! : Average onsky UT visibility : Average onsky AT visibility : 0.20 0.60 “VLTI / UT vibrations" OPD modulation between 0.2 & 1m Frequency >20Hz We have a problem Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Instrumental contrast on the sky Lab visibility : On sky exp. visibility (FSU) : On sky exp. visibility (no FSU) : 0.85 0.85 0.60 NO FINITO ! : Average onsky UT visibility : Average onsky AT visibility : 0.20 0.60 “VLTI / UT vibrations" OPD modulation between 0.2 & 1m Frequency >20Hz We have a problem Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 30 micron RMS OPD measurements Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Puissance (m2) Conan & co. 1995 Puissance (normalisée) Vibrations and OPD Fréquence (Hz) Kervella 2005 Fréquence (Hz) 2/3 8/3 Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Puissance (m2) Conan & co. 1995 Puissance (normalisée) Vibrations and flux Fréquence (Hz) Kervella 2005 Fréquence (Hz) 2/3 11/3 Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Puissance (m2) Conan & co. 1995 Puissance (normalisée) Vibrations and flux Kervella 2005 r e n t t o i i j t f c e o r r e o c c n a d t r n o a p t n Im me e r u s a e m Fréquence (Hz) Fréquence (Hz) 2/3 11/3 Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 0,40 0,05 “transfert function” Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 0,40 0,05 “transfert function” Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 0,40 0,05 “transfert function” Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 0,40 0,05 “transfert function” Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 0,40 0,05 “transfert function” Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 “transfert function” 0,40 0,05 d e t 7 a 0 . r 0 b i : l a n c o i " t s i s c e e b r " p y t i l i b i s i v Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Differential phase bias Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 “Today's” performances Medium spectral resolution (R=1500) Bright star (K=3.5) Typical uncertainties Today Visibility 0.05 Differential visibility 0.01 Phase closure (rad) 0.05 Differential phase (rad) 0.01 Osservatorio Astrofisico di Arcetri Specs 0.01 0.01 0.02 0.01 F. Millour, ESO, 26/01/07 “Today's” performances Low resolution (R=35) See poster Cruzalèbes et al Bright star (K=5) Typical uncertainties Today Visibility ? Differential visibility ? Phase closure (rad) 0.01 Differential phase (rad) 0.001* Specs 0.01 0.01 0.002 0.001 * chromatic dispersion : amplitude ~ from 0.1 rad to 1 rad Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 What could be improved AMBER side : − Jitter estimation/correction − Detector fringe pattern − LR data − Closure phase and differential phase high accuracy VLTI side − VIBRATIONS ! − FINITO − Time delay between measurements Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Osservatorio Astrofisico di Arcetri F. Millour, ESO, 26/01/07 Thank you for your attention Any question ? F. Millour, ESO, 26/01/07