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MATISSE M ulti A per T ure Mid- I nfrared S pectro S copic E xperiment

MATISSE M ulti A per T ure Mid- I nfrared S pectro S copic E xperiment. 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

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MATISSE M ulti A per T ure Mid- I nfrared S pectro S copic E xperiment

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  1. MATISSEMulti 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 Mid-Infrared Interferometric Instrument • Perfect combination of observing wavelength (~10mm) 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 …

  3. MIDI’s limitations • a) Small number of visibility pointsb) 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. MATISSEMulti AperTure Mid-Infrared SpectroScopic Experiment High-Resolution Multi-Band Image Reconstruction + Spectroscopy in the Mid-IR • Proposed 2nd Generation VLTI Instrument • Specifications: • L, M, N, Q band: ~2.7 – 25 mm • 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

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

  6. MATISSEMulti 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 2.7mm + General use of closure phases Ground Precursor of DARWIN Wavelength range 6-18mm

  7. The MATISSE Team

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

  9. Science Team • 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

  10. Earth - 14 mas Jupiter - 74 mas Neptune - 429 mas The circumstellar environment of young low and intermediate mass stars • Planet forming region • Emission from hot dust from the inner region d=140pc 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 AB Aurigae (Fukagawa, 2004)

  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 10mm surface brightness profile of a T Tauri disk with an embedded planet ( inner 40AUx40AU, distance: 140pc) [Wolf & Klahr 2005] i=60deg i=0deg

  12. The circumstellar environment of young low and intermediate mass stars • Is there indirect or direct evidence for the presence of planets? Location of the Planet formation region => Gaps are expected to occur in the mid-infrared bright region of disks Density profile of a 0.05 Msun disk with a Jupiter-mass planet orbiting a solar-mass star [Wolf, Gueth, Henning, Kley 2002] 10mm image of a) an undisturbed disk and b) a disk with a gap at 4AU

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

  14. Massive Star FormationM*>10Msun • 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) OB stars - form preferentially in the centre of dense star clusters - seem to live pref. in (tight) binary and higher order systems High number density of objects Enhanced outflow activity Strong stellar winds from the massive stars after ignition The Orion BN/KL region at 12.5mm, dimension 10'' x 10'' (distance 450 pc) [Shuping et al. 2004] JHK composite of NGC 3603 from ISAAC data, dimension 25'' x 25''

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

  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 10mm images of the targets on the size scale to be investigated • Solution: • Radiative Transfer Simulations (MC3D) 10mm 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. Image Reconstruction Studies • Reconstruction with Building Block Method

  22. Conclusions: Image Reconstruction Studies • 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

  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) Q N L M

  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 Q N L M

  25. L band • H2O ice broad band feature (2.7-4.0mm) • PAHs: 3.3mm, 3.4mm • Nanodiamonds: 3.52mm • Highest Sensitivity in the MIR (reduced background emission) • M band • CO fundamental transition series (4.6-4.78mm) • CO ice features (4.6-4.7mm) • Recombination lines, (e.g., Pfb at 4.65mm)

  26. Spectroscopy The 3-25mm 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, H2O, SiO, C2H2) Dust oxygen-rich dust amorphous silicates, crystalline silicates (e.g. forsterite) simple oxides (SiO2, amourphous Al2O3, Spinel – MgAl2O2) other dust species FeS (most abundant sulfur bearing solid), … volatile dust or ice species H2O ice (3.1 / 12mm), CO (4.7mm) carbon-rich dust TiC, PAHs, Nano-Diamonds

  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. Poster by B. Lopez et al. Summary Multi AperTure Mid-Infrared SpectroScopic Experiment High-Resolution Multi-Band Image Reconstruction + Spectroscopy in the Mid-IR • Specifications: • L, M, N, Q band: ~2.7 – 25 mm • 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

  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 • Case Study: Close young binary/multiple systems: • Do we find binary/multiple stars with individual / circumbinary disks? • What is the spatial distribution of the circumstellar material within the system? • How do Binary/Multiple Systems evolve during the formation process? Binary evolution, low angular momentum [Bate et al. 1997] MIDI measures the auto-correlation function only!

  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 Msun) • => 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: • Dust geometry in Carbon Wolf-Rayet Binaries • Conditions of dust formation in B[e] stars • Dust core of Eta Car Deconvolved MIDI acquisition image at 8.7mm [Chesneau et al. 2005] Two epochs of near-infrared images of WR 104, tracing the rotation of the spiral nebula [Monnier at el. 1999]

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