1. Molecular Surveys of the Disks Encircling T Tauri/Herbig Ae Stars Geoffrey A. Blake CalTech Chemistry as a Diagnostic of Star Formation Waterloo, Canada 23Aug2002

2. People Really Doing the Work! Caltech: -Jacqueline Kessler, Chunhua Qi (now at the SMA/CfA) -Adwin Boogert Leiden w/Ewine van Dishoeck: -Klaus Pontoppidan, Gerd Jan van Zadelhoff, Wing-Fai Thi (now at UCL) Arizona: -Michiel Hogerheijde SFCHEM 2002 23Aug02

3. Study Isolated Disks (Weak/No Outflow) SFCHEM 2002 23Aug02 Beckwith & Sargent 1996

4. Spectroscopy of “Disk Atmospheres” SFCHEM 2002 23Aug02 IR disk surface within several tens of AU (sub)mm disk surface at large radii, disk interior G.J. van Zadelhoff 2002

5. MM-Wave CO Traces Dynamics, Others? SFCHEM 2002 23Aug02 Dutrey et al. 1997, IRAM 30m Kastner et al. 1997, TW Hya, JCMT M. Simon et al. 2001, PdBI Measure: R_disk M_star Inclination w/resolved images.

6. The Sample (drawn from larger single dish survey) Star Sp Type d(pc) Teff(K) R(Rsun) L(Lsun) M(Msun) Age(Myr) LkCa 15K5:V 140 4365 1.64 0.72 0.81 11.7 GM Aur K5V:e140 4060 1.78 0.8 0.84 1.8 HD 163296 A0 120 9550 2.2 30.2 2.3 6.0 MWC 480 A3 130 8710 2.1 32.4 2.0 4.6 Mannings, Koerner & Sargent 1997 MWC 480 LkCa 15 Koerner & Sargent 1995 OVRO+CSO/JCMT MM-Wave Disk Survey SFCHEM 2002 23Aug02 See also poster #67 (SMA maps)

7. Combine 3/1.3 mm array images w/higher J spectra to constrain OUTER disk properties, chemical networks. van Zadelhoff et al. 2001 OVRO+CSO/JCMT MM-Wave Disk Survey II SFCHEM 2002 23Aug02

8. Disk properties vary widely with radius, height; and depend on accretion rate, etc. (Aikawa et al. 2002, w/ D’Alessio et al. disk models, poster #21). Currently sensitive only to R>100 AU in gas tracers, R<100 AU dust. CO clearly optically thick, other species likely to be as well. Model via 2D Monte Carlo using disk structure and chemical models as input, vary to fit observations (Kessler talk). Disk Ionization Structure: CO and Ions

9. Source L * (L ) CN/HCN H dust /h gas LkCa 15 0.72 ~ 10 1.0 GM Aur 0.80 << 1 4.0 MWC 480 30.2 ~ 4 1.7 HD 163293 35.2 >> 50 - [CN]/[HCN] traces enhanced UV fields ( Fuente et al. 1993, Chiang et al. 2001 ) Molecular distribution ring-like? Photochemistry or desorption? Qi et al., in prep UV Fields: HCN and CN LkCa 15 SFCHEM 2002 23Aug02

10. N T (CS) = 10 13 -10 14 cm -2 Upper limits only for H 2 S,SO,SO 2 CS dominant Reminiscent of “early time” chemistry. LkCa 15 CS 2-1 LkCa 15 C 34 S 5-4 Sulfur Species SFCHEM 2002 23Aug02

11. CH 3 OH, H 2 CO - grain surface production SiO - grain sputtering + gas phase rxn CH 3 OH H 2 CO Si Si + O 2  SiO + O h h H 2 CO CH 3 OH Grain chemistry: CH 3 OH, SiO, H 2 CO SFCHEM 2002 23Aug02

12. Are Even Larger Molecules Present? Observations can test gas/grain models, HIFI and arrays can uniquely access small, dense cores & disks. Laboratory spectra urgently needed, work underway (posters #11,84). SFCHEM 2002 23Aug02 Grain Chemistry Model (Charnley 2001) Glycine

13. MM-continuum surveys do not reveal such large, massive disks in similarly aged clusters (IC348) and clouds (NGC 2024, MBM12). Environment? Need better (sub)mm-wave imaging capabilities. CO, HCO + (and NNH + ) chemistry well predicted by disk models. Other species, esp. CS, CN, HCN, much more intense, with unusual emission patterns in some cases (LkCa 15). Are these large disks unusual? SFCHEM 2002 23Aug02

14. Future of the U.S. University Arrays – CARMA Juniper Flat CARMA = BIMA (9 6.1m) + OVRO (6 10.4m) + SZ Array (8 3.5m) telescopes. SUP submitted 2003 SZA on site 2004 move OVRO 2004 move BIMA 2005 full operations

15. (pre-ALMA) The size scales are too small even for the largest current near-IR arrays… Spectroscopy to the rescue! Simulation G. Bryden How can we probe the planet-forming region? Theory Observation? Jupiter (5 AU): V_doppler = 13 m/s V_orbit = 20 km/s

16. High Resolution IR Spectroscopy & Disks CO M-band fundamental VLT Keck NIRSPEC R=25000 R=10,000-100,000 (30-3 km/s) echelle spectrographs (ISAAC,MICHELLE, NIRSPEC, PHOENIX,TEXES) on 8-10m telescopes can now probe “typical” T Tauri/Herbig Ae stars:

17. L1489: Gas/Ice~10/1, accretion. CRBR2422.8: Gas/Ice~1/1, velocity field? Elias 18 Gas/Ice<1/10 (Shuping et al.) Edge-on absorption. Orientation is Pivotal in the IR! H 3 + in absorption? SFCHEM 2002 23Aug02 Poster #79

18. Edge-on Disks & Comets? IR studies of edge on disks could map out both gas phase & grain mantle composition, compare to that found in massive YSOs, comets. N7538 W33A Hale-Bopp Water 100 100 100 CO 10 1 23 CO 2 16 3 6 CH 4 1 0.7 0.6 H 2 CO 3 2 1 CH 3 OH 9 10 2 HCOOH 2 0.5 0.1 NH 3 10 4 0.7 OCS 0.1 0.05 0.4 SFCHEM 2002 23Aug02

19. GSS30 – Class I T Tauri star, accretion shock emission? Broad H I from accretion/outflow, narrow CO from disk. Gap tracer (Carr et al. 2001, DQ Tau)? More typically, emission is seen in M-band Pontoppidan et al. 2002 (ISAAC, R~5000, poster #66) (NIRSPEC, R~25000) SFCHEM 2002 23Aug02

20. CO and 13 CO rotation diagrams show two components, but even the “hot” component is <500 K. Very small amounts of gas. Collisional excitation unimportant at these temperatures, Resonant scattering! Need detailed radiative transfer models (similar effects seen in massive YSOs, Mitchell et al., van der Tak et al.). How is the CO excited in these disks? SFCHEM 2002 23Aug02

21. Explanation: Dust sublimation near the star exposes the inner disk to direct stellar radiation, heating the dust and “puffing up” the disk. Flared disk models often possess 2-5 micron deficiency in model SEDs, where a “bump” is often observed for Herbig Ae stars. Where does the CO emission come from? Dullemond et al. 2002 SFCHEM 2002 23Aug02

22. This model can now be directly tested via YSO size determinations with K-band interferometry. Intense dust emission pumps CO, rim “shadowing” can produce moderate T_rot. Fits to AB Aur SED yield an inner radius of ~0.5 AU (and 0.06 AU for T Tau). SED Fits versus IR Interferometry (Monnier & Millan-Gabet 2002, astro-ph/0207292) Dullemond et al. 2002

23. Many other species and disk types (transitional, debris, etc.) should be examined in both absorption (edge on disks) and emission: H 3 +, CH 4, H 2 O, OCS... Future “Near”-IR (1-5 um) Spectroscopy SFCHEM 2002 23Aug02 Brittain & Rettig 2002, poster #10

24. Rotational H 2 lines potentially provide direct measure of gas mass w/o need for abundance calibrations. Additional studies/confirmation in optically thick, “transitional” pivotal. Difficult, but doable, from the ground. Mid-IR Spectroscopy – Unique access to “warm” H 2 Thi et al. 2001 SFCHEM 2002 23Aug02

25. SIRTF - IRAC (mid-IR cameras, 3.6 4.5, 5.8, 8.0  m) - MIPS (far-IR cameras, 24, 70 160  m, R=20 SED mode) - IRS (5-40  m long slit,R=150, 10-38  m echelle, R=600) 09 Jan 2003 launch - GTO observations - Legacy program - General observations SFCHEM 2002 23Aug02

26. ISO SWS data on A stars, SIRTF can do sun-like stars, high spectral resolution needed for gas phase features. Evans et al., c2d ~170 sources first look + follow up of mapping (poster #46). Meyer et al. Photometry~350 sources, IRS follow up (Class III). SIRTF – Spectroscopy of Dust and Ice SFCHEM 2002 23Aug02

27. (Sub)mm-wave instruments can only study the outer reaches of large disks at present. Expanded arrays (CARMA, eSMA, ALMA) will provide access to much smaller scales. HIFI will enable first assault on water in the cold regions of disks, and may provide a new window on molecular complexity. High resolution IR spectroscopy just starting, is immensely powerful, and will provide unique access to the 1-10 AU region until the advent of ALMA, large IR interferometers. SIRTF will provide many new targets! Disk Spectroscopy - Conclusions SFCHEM 2002 23Aug02