The planet-forming zones of disks around solar-mass stars: a CRIRES evolutionary study

VLT Large Program 24 nights

Major questions

Structure of disks? E.g., size, flat vs. flared, inner holes

How and when is gas lost from disks => timescale for giant planet formation? Mechanisms: photoevaporation, winds, …

How and when is dust lost from disks? How, when and where are planets formed? Chemical composition of material for forming

planets (H2O, biogenic molecules, …)?

Inspiration and guidance from Keck

Cold gas Hot gas

CO v=1-0 band at 4.7 m in disks around Herbig stars

Blake & Boogert 2004

R=25000

CO vibration-rotation spectra

Inspiration from VLT-ISAAC

Pontoppidan et al 2003

CO ice

CO gas

- Increase in CO gas/solid ratios- Change in solid CO band profile

VLT-ISAACR=10,000

T

Q: what are gas-phase abundances? CO emission from young disks?

Importance of velocity information

- Hot HCN and CO blue-shifted by 25 km/s =>Base of MHD wind?

Keck HCN 3 m and CO 4.7 m

IRS 46

Lahuis, Boogertet al. 2006

CRIRES on VLT

1-5 m spectroscopy up to R=100000 with 0.2’’ slit, AO assistedFour 1024 x 512 InSb Aladdin III arrays => large instantaneous wavelength coverage

CRIRES goals and questions Do all disks show hot gas in the inner AU?

Gas dissipation timescales and mechanism Gas temperature and turbulent width CO emitting layer? Departures from Keplerian rotation on <10 AU scales? Comparison gas disk structures (size, position, inclination) with dust

disk CO excitation mechanism as function of radius (UV vs. thermal) Temperature structure of inner envelope and disks in embedded

phase? CO isotope selective photodissociation H3

+ as probe of ionization

Hot chemistry in inner disk? H2O, CH4, HCN, H2CO, …

CO kinematics in disksNeed for high spectral resolution and instrument stability

12CO low J 12CO low J

13CO low J

Note different profiles andnarrow absorption of coldgas in outer disk

CO excitation

Spectroastrometry works!SR 21 disk

-Note accuracy: down to 0.1 AU rms (~200 arcsec, comparable or better than VLTI!)

-Offset is relative to continuum at 4.7m

P lines

Need to work on press release

Pontoppidan et al. 2008

Asymmetries

- slight asymmetries in gas, or in underlying dust continuum in opposite direction

CRIRES sources

Classical T Tauri stars (35) Largely drawn from Keck M-band survey Spectroastrometry on subsample

Cold / transitional disks (20) Bruno’s sample Lucas wTT sample

Embedded Class I sources (20) Largely drawn from VLT-ISAAC survey

Absorption + emission sources Chemistry on subsample

Goals of today

Inventory of results from first four observing runs

Status of data reduction pipeline Status of modeling tools Plans for final runs

Which projects to emphasize? For which sources do we need 2 epochs?

Science analysis + papers Next papers Who will work on what

CO in disks: first results

Edge-on disk: i~60 Face-on disk: i~15o