1. The planet-forming zones of disks around solar- mass stars: a CRIRES evolutionary study VLT Large Program 24 nights

2. 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 (H 2 O, biogenic molecules, …)?

3. Inspiration and guidance from Keck Cold gasHot gas CO v=1-0 band at 4.7  m in disks around Herbig stars Blake & Boogert 2004 R=25000

4. CO vibration-rotation spectra

5. 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-ISAAC R=10,000 T Q: what are gas-phase abundances? CO emission from young disks?

6. 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, Boogert et al. 2006

7. CRIRES on VLT 1-5  m spectroscopy up to R=100000 with 0.2’’ slit, AO assisted Four 1024 x 512 InSb Aladdin III arrays => large instantaneous wavelength coverage

8. 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  H 3 + as probe of ionization  Hot chemistry in inner disk?  H 2 O, CH 4, HCN, H 2 CO, …

9. CO kinematics in disks Need for high spectral resolution and instrument stability 12 CO low J 13 CO low J Note different profiles and narrow absorption of cold gas in outer disk

10. CO excitation

11. 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 4.7  m P lines Need to work on press release Pontoppidan et al. 2008

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

13. 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

14. 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

16. CO in disks: first results Edge-on disk: i~60 Face-on disk: i~15 o