MATISSE - Rencontre projet Fizeau Nov. 2010. Schedule

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Transcript of MATISSE - Rencontre projet Fizeau Nov. 2010. Schedule

  • MATISSE - Rencontre projet Fizeau Nov. 2010

  • Schedule

    Dec2010

    PDR

    June2011

    OFDR

    Dec2011

    FDR

    Mar2013

    N Cold Optics

    Apr2013

    N Cryostat

    Jun2013

    Integration N Cold Optics, Cryostat, Detector

    Jul2013

    L Cryostat

    Aug2013

    L Cold Optics

    Nov2013

    Integration L Cold Optics, Cryostat, Detector

    Apr2014

    Final integration N band at OCA

    Final integration N band at OCA

    Sep2014

    Mar2015

    Test Plan, PAE

  • Contribution de Caroline Daire pour la gestion

    Total FTEs pour OCA : 48.8 sur 124.5.

  • From January 2010 to June

  • From January 2010 to June

    Matisse September 2010

    Slide *reimagerphotometricchannelsanamorphic opticsInterferometricchannelsphotometricslider wheelscameradetectorshuttercoldstopslitreimager

  • From January 2010 to now

    Matisse June 2010

    Slide *reimagerphotometricchannelsanamorphic opticsInterferometric channelsphotometricsliderwheels cameradetectorshutter

    Cold Optics & CryostatsWarm Optics

    BEAM COMPRESSOR UNIT

    2100x2400

    MATISSE WARM OPTICS

    680

    U=52050V=-32025

    U

    V

    U=49800V=-32275

    680

    V=-28945

    FOCAL LAB WALL

    CRANE ACCESS

    V=-30050

    SWD-1-I / V=-33495

    SWD-2-I / V=-33735

    SWD-3-I / V=-33975

    SWD-4-I / V=-34215

    MATISSE FEEDING OPTICS

    V=-35675

    FOCAL LAB WALL

    SWITCHYARD

    2100x2100

    U=52050V=-35325

    LEONARDO

    PRIMA-1

    2100x2100

    PRIMA-2

    2190x2300

    U=44800V=-32725

    U=44800V=-35325

    GRAVITY

    1500x5690

    HARDWARE VOLUME

    640

    U=47540V=-35315

    500

    550

    870

    U=51130V=-34575

    900x1800

    2000x1500

    1200x2400

    U=49910V=-35325

    REFERENCE TARGET

    640

    SCP#35700x440

    760

    250

    750x1105

    MATISSE L BAND CRYOSTAT

    MATISSE N BAND CRYOSTAT

    750x1105

    650

    500

    660

    U=49700V=-30730

    U=51125V=-30730

    175

    675

    360

    680

    IP1-L U=50215

    IP3-L U=50135

    IP5-L U=50055

    IP7-L U=49975

    IP1-N U=51640

    IP3-N U=51560

    IP5-N U=51480

    IP7-N U=51400

    IP7 = ex-SWD-1-I / V=-33495

    IP5 = ex-SWD-2-I / V=-33735

    IP3 = ex-SWD-3-I / V=-33975

    IP1 = ex-SWD-4-I / V=-34215

    IP7

    IP5

    IP3

    IP1

    U=50987.5

    U=50762.5

    U=50537.5

    U=50312.5

    U

    V

    Warm optics Table

    L band Cryostat

    N band Cryostat

    ESO feeding optics

    100

    100

  • Young Stellar Objects From Circumstellar.org catalogue

  • Young Stellar Objects N band : 4-7 sources >=18-20Jy, observable with ATs 38 sources >=1Jy, observable with UTs L band : 18 sources >=2Jy, observable with ATs 53 sources >=0.1Jy, observable with UTs

    By an increase of the sensitivity to the coherent flux by a factor of 5 : N band AT : 20 sources instead of 2-4N band UT : 70 sources instead of 38L band AT : 40 sources instead of 18L band UT : 61 sources instead of 53

  • Young Stellar Objects N band : 4-7 sources >=18-20Jy, observable with ATs 38 sources >=1Jy, observable with UTs L band : 18 sources >=2Jy, observable with ATs 53 sources >=0.1Jy, observable with UTs

    By an increase of the sensitivity to the coherent flux by a factor of 5 : N band AT : 20 sources instead of 2-4N band UT : 70 sources instead of 38L band AT : 40 sources instead of 18L band UT : 61 sources instead of 53

  • Several Scenarios studied for different disk structures and dust contentsScenario 1. Flared disk, inner radius of 3 AU. Herbig source. The disk inclination is 45. Scenario similar to the one used during Phase A for reconstructing an image.

    Scenario 2 = scenario 1 with a disk inner radius of 4 AUScenario 3 = scenario 1 with a disk inclination of 35Scenario 4 = scenario 1 with a maximum grain size three times larger.Scenario 5 = scenario 1 where the dust grains are made up also with 10% of crystalline olivine + Forsterite material. Images for several wavelengths are computed.Scenario 6 = scenario 5, the same case as previously where the dust grains are made up also with a percentage of crystalline material but now the olivine composed grains are distributed for R

  • 7 nights, 4 telescopes, N band

    Case 1: 10 % error on V, 0.1 rad on the closure phases.Case 2: 2-3% error on V, 0.01 rad on the closure phases.

  • 7 nights, 4 telescopes, N band

    Case 1: 10 % error on V, 0.1 rad on the closure phases.Case 2: 2-3% error on V, 0.01 rad on the closure phases.

  • Improvement of VLTI sensitivity and accuracy.

    Sensitivities with MATISSE will be improved by :- the use of an external Fringe Tracking, On and Off Axis,- the continuation of the effort made to reduce the fast OPD jitters/ vibrations.

    Accuracies with MATISSE will be improved by :- the use of an external Fringe Tracking,- the effort made to reduce the fast OPD jitters/ vibrations,- the pupil lateral motion monitoring,- the use of OPD jitter residuals, tip-tilt residual, pupil lateral motion information when analysing the data.

    High limiting magnitude: Urgent need to develop and test exotic modes:H-K blind + N fringe-trackingMR blind recordingNew ideas for coherencingHigh dynamic range: Urgent need to open the AMBER BCD

  • Vers une ANR 2011 Formation et Evolution des Systmes Plantaires

    2 Axes afin dapporter de nouveau rsultats dans le domaines : a) R&D codes Astrophysiques (diffrent types poussire, rgion puffed-up, )b) R&D Traitement du signal (cas objet faible en rgime fond thermique)

    Projets : MIDI, AMBER (dj utilisables), SPHERE ( court terme), ,MATISSE & SPICA dont on a intrt prparer au mieux les programmes

    Date de soumission : 10 (?) Janvier 2011, ANR sur 4 ans nous conduisant lintgration finale et aux tests de MATISSE.

    Imagin demand : 2 post-doc, 2 Thses, 50-100 k MATISSE & SPICA

    Interface avec recherche et/ou ANR : corps mineurs, simulation dynamique, reconstruction dimage

  • B. Lopez1, P. Antonelli1, S. Wolf2, W. Jaffe3, R. Petrov1, S. Lagarde1, P. Berio1, R. Navarro4, U. Graser2, U. Beckman4, G. Weigelt5 , F. Vakili1, T. Henning2, J.C. Augereau9, C. Bailet1, J. Behrend5, N. Berruyer1, Y. Bresson1, O. Chesneau1, J.M. Clausse1, C. Connot5, K. Demyk6, W.C. Danchi7, M. Dugu1, E. Elswijk4, S. Flament1, H. Hanenburg4, K.H. Hofmann5, M. Heininger5, R. t. Horst4, J. Hron14, R. Matthar3, J. Kragt4, G. Kroes8, W. Laun2, Ch. Leinert2, H. Linz2, A. Matter1, Ph. Mathias1, K. Meisenheimer2, J.L. Menut1, F. Millour5, U. Neumann2, E. Nussbaum5, A. Niedzielski10, M. Mellein2, L. Mosoni8, S. Ottogalli1, J. Olofsson9, Y. Rabbia1, T. Ratzka2, S. Robbe-Dubois1, A. Roussel1, F. Rigal4, D. Schertl4, F.-X. Schmider1, B. Stecklum11, E. Thiebaut12, M. Vannier1, L. Venema4, K. Wagner2, L.B.F.M. Waters13.

    1- Observatoire de la Cte d'Azur, Nice, France, 2- Max Planck Institut fr Astronomie, Heidelberg, Germany, 3- Leiden Observatory, the Netherlands, 4- ASTRON-NOVA, Dwingeloo, the Netherlands, 5- Max Planck Institut fr Radioastronomie, Bonn, Germany,6- CETP, Toulouse, France,7- NASA Goddard Flight Center, Baltimore, USA,8- Konkoly Observatory Budapest, Hungary,9- Observatoire de Grenoble, Grenoble, France,10- Torun Center for Astronomy, Torun, Poland,11- Thringer Landessternwarte Tautenburg, Germany, 12- Observatoire de Lyon, France,13- Astronomical Institute Amsterdam, the Netherlands,14- Vienna University Austria.

    With the support of ESO in the frame of the second generation VLTI instruments : A. Richichi (ESO Instrument Scientist of MATISSE), F. Gont (ESO VLTI System Engineer as MATISSE contact), G. Finger, J.L. Lizon, I. Derek, I. Percheron, G. Ruppretch, P. Haguenhauer, P. Gitton, S. Morel, Participants and Institutes

  • Fundings

    Comparison of the Potential of MATISSE Phase-Referenced Imaging with Closure-Phase ImagingModel Image,diam. 90 masBuilding block reconstruction with Phase ReferencesBuilding block reconstruction with Closure Phases30 Jy 20 Jy 12 Jy 8 Jy 6 Jy 4 Jy Simulated uv coverage, 4 ATs, 3 configurations

    Comparison of the Potential of MATISSE Phase-Referenced Imaging with Closure-Phase ImagingModel ImagesBuilding block reconstruction with Phase ReferencesBuilding block reconstruction with Closure Phases 60 mas 90 mas 120 mas 150 mas 180 mas 210 mas

    MATISSE

    Multi-AperTure Mid-Infrared SpectroScopic Experiment

    Towards the Imaging in the mid-IR domain

    Towards the Opening of New Spectral Windows3 4 5LMNQPresent MIDI Instrument

    Towards the Opening of New Spectral Windows3 4 5LMNQMATISSE Instrument

    Science Programs and their key Issues

    Science Programs and their key Issues

    Mineralogy of Proto-Planetary Disks Grain Evolution towards PlanetesimalsThe building blocks of planets within the terrestrial region of protoplanetary disksvanBoekel et al. 2004, Nature, 432, 479Normalized flux

    Science Programs and their key Issues ???????

    MATISSE CharacteristicsNumber of beams : four, two and three also possible.

    Spectral coverage : L, M, N, possible also simultaneously. Optimized for L and N.

    Spectral resolution : low : 20

  • 2 main modes

    High sensitivity Mode (High Sens) :2T, 3T or 4TWith dedicated sequence of photometry: the photometry is evaluated by two means, In the Fourier domain, by the low freque