Protoplanetary seen through the eyes of new-generation high-resolution instruments - Rome, June 6, 08 Revealing the evolution of at 0.0-0 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
What happens in the blind side? From Garufi et al. 07, MSGR Pinilla et al 08
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 4 0 6 wavelength (um) 8 IR spectroscopy Spitzer VLT Keck ALMA & Direct Imaging Main Belt spatially resolved by ALMA @ kpc hot-jupiters super-earths exo-jupiters spatially resolved by ALMA @ 40 pc 0.0 au 0. au distance from host star au 0 au 00 au
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.0 0-3 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,
How to get spatial information at 0.0-0 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 4 0 6 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 0.0-0 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)
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
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) HD4569 3 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!
(Banzatti et al. 0, 05a) Intermezzo: the interesting case of EXLupi
Water vapor evolution and chemical gradients Data: IR spectroscopy (VLT-CRIRES, Spitzer-IRS) Resolution: low + high (Δv ~ 3-450 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 35 35 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
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 <.
Summary Molecular spectroscopy at infrared wavelengths provides a unique probe of protoplanetary at ~0.05-0 au, complementary to imaging (limited to > ~5 au @ 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 HD4569 3 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