1. MATISSE Multi AperTure Mid-Infrared SpectroScopic Experiment Sebastian Wolf MATISSE Project Scientist Emmy Noether Research Group “Evolution of Circumstellar Dust Disks to Planetary Systems” Max Planck Institute for Astronomy, Heidelberg Bruno Lopez PI Observatoire de la Cote d’Azur, Nice + Science Team

2. The Progenitor: MIDI Perfect combination of observing wavelength (~10  m) and spatial resolution (VLTI baselines => 10-20mas) => regions with hot dust can be spatially resolved since 2002 observations of the hot dust in circumstellar disks, AGB stars, winds of hot stars, massive star forming regions, tori of AGNs, … Results: Very successful in interferometric spectroscopy (chemical composition of dust on different spatial scales) Concept of mid-infrared long-baseline interferometry proven to work but … Mid-Infrared Interferometric Instrument

3. MIDI’s limitations a) Small number of visibility points b) Lack of Phase Information Investigation of small-scale structures (= main goal of MIDI) and quantitative analysis of spectroscopic observation strongly limited c) Interpretation of MIDI data: Comparison between modelled and observed visibility points, using 2D models with point-symmetry (usually even rotation symmetry) Approach justified only by large-scale (if at all existing) symmetries, but expected to be strongly misleading or simply wrong on size scales investigated with MIDI

4. Proposed 2 nd Generation VLTI Instrument Specifications: L, M, N, Q band: ~2.7 – 25  m Spectral resolutions: 30 / 100-300 / 500-1000 Simultaneous observations in 2 spectral bands What’s new? Image reconstruction on size scales of 3 / 6 mas (L band) 10 / 20mas (N band) using ATs / UTs Multi-wavelength approach in the mid-infrared 3 new mid-IR observing windows for interferometry (L,M,Q) Improved Spectroscopic Capabilities MATISSE Multi AperTure Mid-Infrared SpectroScopic Experiment High-Resolution Multi-Band Image Reconstruction + Spectroscopy in the Mid-IR

5. MATISSE MATISSE Multi AperTure Mid-Infrared SpectroScopic Experiment AMBER JWST

6. MATISSE Multi AperTure Mid-Infrared SpectroScopic Experiment High-Resolution Multi-Band Image Reconstruction + Spectroscopy in the Mid-IR Successor of MIDI: Imaging Capability in the entire mid-IR accessible from the ground Successor of AMBER: Extension down to 2.7  m + General use of closure phases Ground Precursor of DARWIN Wavelength range 6-18  m

7. The MATISSE Team

8. Individual Contributions Obs. de Lyon, Obs. de Grenoble, Universite de Lille, TLS Tautenburg Letters of Intent Meudon, Torino-INAF

9. Studies: a) Science Cases: Complex Structures Star and Planet Formation Circumstellar Environment:Low / Intermediate mass stars Massive Stars Multiple Stars Protostellar Disks:Planet Formation Disk evolution: Young => Debris Disks Extrasolar Planets AGBs / Evolved Stars / Hot Stars Active Galactic Nuclei b) Image Reconstruction Studies Science Team

10. The circumstellar environment of young low and intermediate mass stars Planet forming region Emission from hot dust from the inner region Earth- 14 mas Jupiter- 74 mas Neptune- 429 mas d=140pc AB Aurigae (Fukagawa, 2004) Complex outer disk structures observed => Complex inner disk structure expected FU Orionis outbursts -- Variability in general (flux, polarization) -- Expected influence from the formation of Jets/Outflows

11. The circumstellar environment of young low and intermediate mass stars Is there indirect or direct evidence for the presence of planets? Protoplanets: Significant influence on the surface density / brightness profile: Hot spot / Gaps Hot Accretion Region around the Planet i=0deg i=60deg 10  m surface brightness profile of a T Tauri disk with an embedded planet ( inner 40AUx40AU, distance: 140pc) [Wolf & Klahr 2005]

12. The circumstellar environment of young low and intermediate mass stars Is there indirect or direct evidence for the presence of planets? Density profile of a 0.05 M sun disk with a Jupiter-mass planet orbiting a solar-mass star [Wolf, Gueth, Henning, Kley 2002]  m image of a) an undisturbed disk and b) a disk with a gap at 4AU Location of the Planet formation region => Gaps are expected to occur in the mid- infrared bright region of disks

13. Massive Star Formation M * >10M sun Butterfly Star (low mass young stellar object) In a typical distance of nearby massive star forming regions.

14. Massive Star Formation M * >10M sun High-mass star forming regions are much more distant (in average) than those of low-mass stars (high-mass: 3-7kpc vs. low-mass: 0.1-0.3 kpc) JHK composite of NGC 3603 from ISAAC data, dimension 25'' x 25'' OB stars - form preferentially in the centre of dense star clusters - seem to live pref. in (tight) binary and higher order systems The Orion BN/KL region at 12.5  m, dimension 10'' x 10'' (distance 450 pc) [Shuping et al. 2004] High number density of objects Enhanced outflow activity Strong stellar winds from the massive stars after ignition

15. Massive Star Formation M * >10M sun What we can do with MIDI … W3: UCHII region Objects of this class are often faint in the near-IR, but bright in the mid-IR! MATISSE will for the first time allow a comprehensive comparison between low and high mass star formation Linz et al. 2004 [Disks, Jets, Multiplicity,…]

16. Image Reconstruction Studies Goal: Justification that MATISSE will indeed be able to answer the questions addressed in the individual Science Case Studies Strategy: Simulation of a realistic observation procedure

17. Image Reconstruction Studies Problem: There are no observed 10  m images of the targets on the size scale to be investigated Solution: Radiative Transfer Simulations (MC3D) 10  m image of a circumstellar disk with an inner hole, radius 4AU (inclination: 60deg; distance 140pc, inner 60AU x 60AU)

18. Image Reconstruction Studies SimVLTI3 : -Based on SimVLTI -Simulation of 3/4 beam combination + closure phases -Location of all AT stations added -Output: OI-FITS format Definition of the Observing Procedure + location of ATs, number of nights, noise, etc, …

19. Image Reconstruction Studies Tracks in the uv plane

20. Image Reconstruction Studies Building Block Method (K.-H. Hofmann) Hybrid Mapping & Self-Calibration (S. Kraus) Difference Mapping (L. Mosoni)

21. Reconstruction with Building Block Method Image Reconstruction Studies

22. All 3 applied image reconstruction techniques allow to reconstruct main features in the considered disk model Best results: Building Block Method (Hofmann & Weigelt) Sufficient uv coverage: 3-5 nights of observations with ATs (at varying locations) Improvement of reconstructed images: 4 telescopes (instead of 3) UT Single-dish data + VLTI (UTs/ATs) interferometric data Conclusions: Image Reconstruction Studies

23. Multiwavelength Imaging (L - M - N - Q) Observations in different bands … trace regions with different characteristic temperatures …provide image with different spatial resolution … allow a comparison with lower-resolution images obtained at large telescopes with adaptive optics – tracing the large scale structure if the targets – in different wavelength regions (L/M: NACO, N/Q: VISIR) L M N Q

24. Multiwavelength Imaging (L - M - N - Q) Depending on the individual band …unique spectral features (dust/gas) are accessible …spectral features can be investigated that correspond to dust species which can also be observed in N band L M N Q

25. L band H 2 O ice broad band feature (2.7-4.0  m) PAHs: 3.3  m, 3.4  m Nanodiamonds: 3.52  m Highest Sensitivity in the MIR (reduced background emission) M band CO fundamental transition series (4.6-4.78  m) CO ice features (4.6-4.7  m) Recombination lines, (e.g., Pf  at 4.65  m)

26. Spectroscopy The 3-25  m spectral region is extremly rich in spectral diagnostics of gas and dust – covering a huge range of physical and chemical conditions Gas strong vibrational lines of abundant molecules (CO, OH, H 2 O, SiO, C 2 H 2 ) Dust oxygen-rich dust amorphous silicates, crystalline silicates (e.g. forsterite) simple oxides (SiO 2, amourphous Al 2 O 3, Spinel – MgAl 2 O 2 ) other dust species FeS (most abundant sulfur bearing solid), … carbon-rich dust TiC, PAHs, Nano-Diamonds volatile dust or ice species H 2 O ice (3.1 / 12  m), CO (4.7  m)

27. Example Application Planet Formation - Protoplanetary Disks Critical tests of models for the radial distribution of different dust species Dust evolution in disks? Determination of crystallization region / processes? - Radial Mixing Efficiency? Origin of nano-diamonds in meteorites + IPD? Distribution of Volatiles Key importance for understanding the complex disk chemistry: Many (organic) molecules are formed in ice mantles – Transport to inner disk region – Sublimation / Release to the gas phase Spatial distribution of water / CO ice? - Where is the snowline?

28. Specifications: L, M, N, Q band: ~2.7 – 25  m Spectral resolutions: 30 / 100-300 / 500-1000 Simultaneous observations in 2 spectral bands Image reconstruction on size scales of 3 / 6 mas (L band) 10 / 20mas (N band) using ATs / UTs Multi-wavelength approach in the mid-infrared 3 new mid-IR observing windows for interferometry (L,M,Q) Improved Spectroscopic Capabilities Key Science Programs can be performed in 3-5 AT nights Perfect complement to high-resolution facilities in the near-IR and mm Summary Multi AperTure Mid-Infrared SpectroScopic Experiment High-Resolution Multi-Band Image Reconstruction + Spectroscopy in the Mid-IR Poster by B. Lopez et al.

29. extra slides

30. Active Galactic Nuclei ~1% of all Galaxies hosts an AGN Dust Torus => Obscuration in the optical (=> Seyfert I/II) Structure of the Torus? Preparatory Studies: MIDI What is the size of the torus? How does it depend on luminosity? What is the overall shape of the torus? Emission of the Tori of Seyfert I/II galaxies compatible with the unified scheme? MATISSE In how far is the torus structure regulated by outflow phenomena (supersonic winds, jets)? What fraction of the dust emission from the inner few parsecs of an AGN is emitted by the torus? Is the torus just the inner, AGN heated part of the central molecular disk in the host galaxy? Can we find direct evidence for the clumpiness of torii?

31. The circumstellar environment of young low and intermediate mass multiple stars Degree of Multiplicity ~ 40% - 60% (depending on SpT) Multiplicity observed in all stages of stellar evolution Multiplicity plays explicit role in the evolution of the companions MIDI measures the auto-correlation function only! Case Study: Close young binary/multiple systems: 1.Do we find binary/multiple stars with individual / circumbinary disks? 2.What is the spatial distribution of the circumstellar material within the system? 3.How do Binary/Multiple Systems evolve during the formation process? Binary evolution, low angular momentum [Bate et al. 1997]

32. Dust and Winds from AGB / Evolved Stars Low/Intermediate Mass Stars => Cool Late Type Stars => Develop dense dusty stellar wind (10 -8 -10 -4 M sun ) => Loose up to 80% of their initial mass => Contribute significantly to the replenishment of the ISM Mechanism (stellar pulsation + radiation pressure) poorly understood Red Super Giants: Bipolar Outflows? Asymmetric Envelopes? Asymptotic Giant Branch Stars: Clumpy Environment? R Coronae Borealis: Localization of the Dust Cloud Formation? Post-AGB, RV Tau: Geometry of the disk torus? Symbiotic Stars / Novae: Role of Binarity? Planetary Nebulae: Disk Geometry?

33. Hot Stars Stellar Winds from Hot Stars strongly affect the ISM by many aspects but: Nature of these Winds still poorly understood. How can dust be formed in this hostile environment? Goals: 1.Dust geometry in Carbon Wolf-Rayet Binaries 2.Conditions of dust formation in B[e] stars 3.Dust core of Eta Car Deconvolved MIDI acquisition image at 8.7  m [Chesneau et al. 2005] Two epochs of near-infrared images of WR 104, tracing the rotation of the spiral nebula [Monnier at el. 1999]