Revealing the evolution of disks at au from high-resolution IR spectroscopy

Transcription

1 Protoplanetary seen through the eyes of new-generation high-resolution instruments - Rome, June 6, 08 Revealing the evolution of at au from high-resolution IR spectroscopy VLT IR interferometry (not included in this talk) ~ 0.0 au IR spectroscopy ~ 5 au Spitzer VLT Keck IRTF JWST ~ 0 au VLT ALMA Dr. Andrea Banzatti

2 What happens in the blind side? From Garufi et al. 07, MSGR Pinilla et al 08

3 N/MIR molecular spectroscopy to study inner Wavelengths: ~-40 micron (different ranges covered by different instruments) Molecules: CO, HO, OH, HCN, CH, CO (mostly, plus some other species) Spectral Resolution: some very high (3 km/s), some only moderate (450 km/s) but large coverage Science: structure (from gas kinematics), chemistry, evolution of planet-forming regions at < 0 au CO hot H O Molecular spectra of inner cold H O organics: C H HCN CO wavelength (um) 8 IR spectroscopy Spitzer VLT Keck ALMA & Direct Imaging Main Belt spatially resolved by kpc hot-jupiters super-earths exo-jupiters spatially resolved by 40 pc 0.0 au 0. au distance from host star au 0 au 00 au

4 Mostly small sample sizes &/or low spectral resolution 990-0: CO gas NIR emission probes Keplerian inner Keck-NIRSPEC -5 um R~5,000 ~00 A brief history of N/MIR molecular spectroscopy of planetforming regions 008-today: Large sample sizes (~00 ) high spectral resolution (R = 75,000-00,000) Particularly promising: combined datasets (wavelengths, tracers, molecules, samples) to obtain global view of evolving planet-forming regions Carr+ 00 Carr, Najita, Blake, Brittain, Salyk 008-0: Water and organics discovered in inner Carr & Najita 008 (Salyk+ 008) Spitzer-IRS 0-37 um R~700 ~00 VLT-CRIRES (+) -5 um R~00,000 ~00 VLT-VISIR um R~5,000 ~50 IRTF-ISHELL -5 um R~75,000 >0 Carr, Najita, Pontoppidan, Salyk, Fedele Some references: Najita, Carr, Pontoppidan, Salyk, Brittain, Fedele, Carmona, Banzatti, Doppmann, Blake, Mandell, Pascucci, Brown, Herczeg, van der Plas, Bast, Hein Bertelsen,

5 How to get spatial information at au log flux optical 6000 K star infrared (IR) ~500 K CO hot H O Molecular spectra from inner organics: C H HCN CO cold H O disk dust emission millimeter < 00 K wavelength (um) 8 (e.g. Carr & Najita 008; Salyk et al. 0; Banzatti et al. 0, 03, 07) log wavelength Doppler broadening of CO emission lines: flux ~5 AU vel R au ~0.4 AU resolution element vel towards the star IR spectroscopy 0. super- ALMA Velocity shift (km/s) (e.g. Brittain et al. 007; Pontoppidan et al. 0; Banzatti et al., 05a,b, 07)

6 High-res. CO spectra to study inner Data: IR spectroscopy (VLT-CRIRES, IRTF-iSHELL) Resolution: high (Δv ~ 3-5 km/s) Sample size: > 50, spanning evolutionary stages Goals: resolve gas kinematics and radial structure at < 5 AU, detect gas-depleted zones, measure gas temperature and density, reconstruct inner disk evolution phases Several observing programs (mostly a LP by vdishoeck &Pontoppidan) CRIRES on VLT (8-m) ~30 nights of data (more than 4 papers published to date) Part of the ro-vibrational spectrum of carbon monoxide (CO): RATIO > vibrational temperature FWHM > emitting radius on face-on disk: R Banzatti et al. 05a, 07, 08, Banzatti & Pontoppidan 05

7 Gas temperature and evolution/depletion Data: IR spectroscopy (VLT-CRIRES, IRTF-iSHELL) Resolution: high (Δv ~ 3-5 km/s) Sample size: > 50, spanning evolutionary stages Goals: resolve gas kinematics and radial structure at < 5 AU, detect gas-depleted zones, measure gas temperature and density, reconstruct inner disk evolution phases SR primordial (full) HD DRTau devoid inner partly devoid Jupiter s orbit (~5 AU) Beta Pic! (upper lim.) TWHya The high-velocity gas is gone (Banzatti & Pontoppidan 05) (Banzatti & Pontoppidan 05) 4 HD35344B! (SAO0646) end of primordial gas FWHM > emitting radius UV pumping regime RATIO > vibrational temperature HD00546 debris!

8 (Banzatti et al. 0, 05a) Intermezzo: the interesting case of EXLupi

9 Water vapor evolution and chemical gradients Data: IR spectroscopy (VLT-CRIRES, Spitzer-IRS) Resolution: low + high (Δv ~ km/s) Sample size: > 50, spanning evolutionary stages Goals: combined analysis of multiple molecular tracers (CO, HO, OH), to study the thermo-chemical structure and evolution CO and HO emission broad lines (broad emission lines) broad lines < Rsnow.9,.5, 33Rµm co lines water-vapor-rich disk.9,.5, 33 µm line vable obser Rco < Rsnow water-vapor-rich OH/HO ratio (Walsh et al. 05) C/O stellar accretion full gas C/O (Walsh et al. 05) water-vapor-poor planetesimal and planetary accretion and migration CO emission only (narrow lines) narrow lines Rco R cavity snow inner disk (depleted zone) narrow lines Rco Rsnow water-vapor-poor disk winds water-vapor-poor (Rsnow) disk temperature increases closer to the star ~50 K ~500 K b (Banzatti et al. 07)c CO and HO emission c CO and HO emission winds stellar accretion Line Line detections: detections: at 3-30 at 3-30 umum only only at > at > umum only only at >at30 > 30 umum water water depleted depleted winds water-vapor-rich water-vapor-poor CO emission only (narrow lines) 3 M3sol Msol Msol M (Walsh et al. 05) sol Msol Msol water-vapor-poor imprints water-vapor-poor planet atmosphere composition CO emission only (narrow lines) Stellar Stellar mass: mass: Stellar mass: mass: inner disk cavity (depletedstellar zone) inner disk cavity (depleted zone) 3 M3sol Msol Msol Msol Msol Msol Models: imprints planet stellar core composition accretion planetesimal and planetary planetesimal and planetary accretion and migration accretion and migration water-vapor-rich temperature first trends observed in disk gas (broad emission lines) (broad emission lines) nsion depletes depletes from from 3Measurements: to3 to water water vapor emission emission depletes depletes from from 3 to3with towith known dustdust with with known known dustdust ission fades away water asvapor vapor emission fades away asknown aps r form form form in in um um as larger as larger form form in in.9,.5, 33 µm line form in inner.9,.5, 33 µm lines in inner larger cavities water-vapor-poor <5 K

10 The powerful synergy of gas and dust tracers high-res optical spectroscopy of stellar photosphere (Folsom+ 0, Kama+ 05) DUST optical-to-ir photometry SED (a) (c) HD3648 HD4443S HD04 HD6396 no/small cavities HD457 HD457 HD44604 HD35344B HD35344B HD4666 HD989 high-nir cavities HD393 HD3964 HD36 HD393 HD3964 high-nir cavities all have spirals! HD37806 HD5093 HD989 HD4443S HD9588 HD3648 HD44668 HD4666 HD04 HD6396 HD36 HD00546 HD90073 HD798 HD694 HD694 low-nir cavities HD4569 HD97048 HD00546 HD97048 HD798 HD4569 solar HD50550 (b) (d) HD457 HD457 HD36 HD35344B HD00453 HD393 HD393 HD35344B HD36 HD0437 HD989 GI split in high-nir and low-nir HD37806 HD4443S HD989 HD6396 HD3648 HD4443S HD4666 HD04 HD694 HD6396 HD4666 HD3648 HD694 HD97048 HD97048 HD798 HD3964 HD348 HD00546 HD798 HD00546 HD3964 F30/F3 <. (GII) F30/F3 >. (GI) solar HD4569 HD4569 GAS high-res infrared spectroscopy of disk molecular emission GAS (Banzatti, Garufi, Kama et al. 08) No/small cavity Large cavity Gas-poor The evolution and depletion of gas & dust are tightly connected in inner Large GII (HD6396) Small GII (HD5093) CO gas, Hot dust, Cold dust High-NIR GI (HD35344B) Low-NIR GI (HD00546) Gas-poor GI (HD4569) Gas-poor GII (HD4563) F30/F3 >. F30/F3 <.

11 Summary Molecular spectroscopy at infrared wavelengths provides a unique probe of protoplanetary at ~ au, complementary to imaging (limited to > ~5 40 pc) An escalation of discoveries in recent years: ) CO kinematics and excitation reveal the formation and evolution of inner disk cavities ) as inner evolve, HO is depleted in the terrestrial planet zone 3) dust and molecular gas are depleted simultaneously, by planet-formation processes or disk winds (?) 4) next: links between complementary techniques, to link evolving inner and exoplanet populations.. SR primordial (full) molecular disk wind / photoevaporative wind? NC BC HD DRTau devoid inner partly devoid HD00546 (NC/) (BC) migration Beta Pic! (upper lim.) TWHya disk dissipation SC photoevaporative gap formation? end of primordial gas debris! hot Jupiters formation & migration 4 HD35344B! (SAO0646) UV pumping regime By combining high spectral resolution (R = 5,000-00,000), multiple molecules (CO, HO, OH), large samples (50-00 ), and multiple disk tracers (gas, dust, winds), we are working our way towards obtaining a global view of the evolution of inner planet-forming. formation & migration stellar UV radiation SC 3 exo-jupiters largely devoid inner disk 4 CO gas from dust grains