MATISSE - Rencontre projet Fizeau Nov. 2010

Schedule

Dec2010

PD

R

June2011

OF

DR

Dec2011

FD

R

Mar2013

N C

old

Op

tics

Apr2013

N C

ryo

stat

Jun2013

Inte

gra

tio

n N

Co

ld

Op

tics

, Cry

ost

at,

Det

ecto

r

Apr2014

Jul2013

L C

ryo

stat

Aug2013

L C

old

Op

tics

Nov2013

Inte

gra

tio

n L

Co

ld

Op

tics

, Cry

ost

at,

Det

ecto

r

Fin

al in

teg

rati

on

N

ban

d a

t O

CA

Fin

al in

teg

rati

on

N

ban

d a

t O

CA

Sep2014

Mar2015

Tes

t P

lan

, PA

E

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 6

reimager

photometricchannels

anamorphic optics

Interferometricchannels

photometricslider

wheelscamera

detector

shutter

coldstop

slit

reimager

From January 2010 to now

Matisse June 2010 Slide 7

reimager

photometricchannels

anamorphic optics

Interferometric channels

photometricslider

wheels

camera

detectorshutter

Cold Optics & Cryostats

Warm Optics

BEAM COMPRESSOR UNIT2100x2400

MATISSE WARM OPTICS

680

U=52050V=-32025

UV

U=49800V=-32275

680

V=-28945FOCAL 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=-35675FOCAL LAB WALL

SWITCHYARD2100x2100U=52050

V=-35325

LEONARDO

PRIMA-12100x2100

PRIMA-22190x2300

U=44800V=-32725

U=44800V=-35325

GRAVITY

1500x5690HARDWARE VOLUME

640

U=47540V=-35315

500

550

870

U=51130V=-34575

900x1800

2000x1500

1200x2400U=49910V=-35325

RE

FE

RE

NC

E T

AR

GE

T

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

=50

215

IP3-

L U

=50

135

IP5-

L U

=50

055

IP7-

L U

=49

975

IP1-

N U

=51

640

IP3-

N U

=51

560

IP5-

N U

=51

480

IP7-

N U

=51

400

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=

5098

7.5

U=

5076

2.5

U=

5053

7.5

U=

5031

2.5

U

VWarm 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 ATs38 sources >=1Jy, observable with UTs

L band : 18 sources >=2Jy, observable with ATs53 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 ATs38 sources >=1Jy, observable with UTs

L band : 18 sources >=2Jy, observable with ATs53 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 contents

Scenario 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 AU

Scenario 3 = scenario 1 with a disk inclination of 35°

Scenario 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 <= 6 AU.

Scenario 7 : a puffed inner region as an alternative to Scenario 1.

Scenario 8 : a case with the presence of water ice grains (to be compared with scenario 1), disk without ice grains).

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-tracking MR blind recording New ideas for coherencing

High dynamic range : Urgent need to open the AMBER BCD

Vers une ANR 2011

Formation et Evolution des Systèmes Planétaires

2 Axes afin d’apporter de nouveau résultats dans le domaines :

a) R&D codes Astrophysiques (différent types poussière, région puffed-up, …)

b) R&D Traitement du signal (cas objet faible en régime ‘fond thermique’)

Projets : MIDI, AMBER (déjà utilisables), SPHERE (à court terme), …,

MATISSE & SPICA dont on a intérêt à préparer au mieux les programmes

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

Imaginé demandé : 2 post-doc, 2 Thèses, 50-100 k€ MATISSE & SPICA

Interface avec recherche et/ou ANR : corps mineurs, simulation dynamique, reconstruction d’image

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. Dugué1, 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 Côte d'Azur, Nice, France, 2- Max Planck Institut für Astronomie, Heidelberg, Germany, 3- Leiden Observatory, the Netherlands, 4- ASTRON-NOVA, Dwingeloo, the Netherlands, 5- Max Planck Institut für 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- Thüringer 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. Gonté (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 Imaging

Model Image,diam. 90 mas

Building block reconstruction with Phase References

Building block reconstruction with Closure Phases

30 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 Imaging

Model Images

Building block reconstruction with Phase References

Building block reconstruction with Closure Phases

60 mas 90 mas 120 mas 150 mas 180 mas 210 mas

MATISSE

Successor of MIDI:Imaging capability in the entire mid-IR

Successor of AMBER:Extension down to 2.8 m + General use of closure phases

Complement to ALMA + ELT

Ground Precursor of space mission to characterize Earth like planets

Wavelength range 6-18m

Multi-AperTure Mid-Infrared SpectroScopic Experiment

Towards the Imaging in the mid-IR domain

Towards the Opening of New Spectral Windows

3 4 5L M N Q

Present MIDI Instrument

Towards the Opening of New Spectral Windows

3 4 5L M N Q

MATISSE Instrument

Science Programs and their key Issues

Science Programs and their key Issues

Mineralogy of Proto-Planetary Disks Grain Evolution towards Planetesimals

“The building blocks of planets within the terrestrial region of protoplanetary disks”

van Boekel et al. 2004, Nature, 432, 479

No

rma

lize

d f

lux

Science Programs and their key Issues

???????

MATISSE Characteristics

Number 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 <R<40 in L&M at 3.5 mm; 20<R<40 in N at 10.5 mm. Medium : 350<R<550 in L&M at 3.5 mm; 150<R<250 in N at 10.5 mm. High : 800<R<1000 in L at 3.5 mm

The simultaneous coverage of the L&M bands in low and medium resolutions, and the full coverage of the L band in high spectral resolution require an external fringe tracker.

MATISSE will measure: coherent flux, visibilities, closure phases and differential phases. Differential visibilities can also be derived.

2 main modes

High sensitivity Mode (High Sens) :- 2T, 3T or 4T- With dedicated sequence of photometry: the photometry is evaluated by two

means,• In the Fourier domain, by the low frequency peak,• Using dedicated long sequences of photometric recording.

- Without photometry => Phase Oriented Mode

Simultaneous Photometry Mode (Si Phot) :- 2T, 3T or 4T- Photometric channels are used, individual photometry is estimated frame by frame for

bright targets, or binned relatively to the chopping frequency.

MATISSE Observing Modes

Specifications on sensitivity on the coherent flux

With the current VLTI infrastructure (within 300 ms and 50ms) :

Specifications on sensitivity on the coherent flux

With the current VLTI infrastructure (within 300 ms and 50ms) :

For information assuming a Fringe Tracking

With 10 minutes of total observing time