Exploring organic chemistry in planet-forming zones
  Over the last few years, the chemistry of molecules other than CO in the planet-forming zones of disks is starting to be explored with Spitzer and high-resolution ground-based data. However, these studies have focused only on a few simple molecules. The aim of this study is to put observational constraints on the presence of more complex organic and sulfur-bearing molecules predicted to be abundant in chemical models of disks and to simulate high resolution spectra in view of future missions. High S/N Spitzer spectra at 10-30 micron of the near edge-on disks IRS46 and GVTau are used to search for mid-infrared absorption bands of various molecules. These disks are good laboratories because absorption studies do not suffer from low line/continuum ratios that plague emission data. Simple LTE slab models are used to infer column densities (or upper limits) and excitation temperatures. Bands of HCN, C2H2 and CO2 are clearly detected toward both sources. The HCN and C2H2 absorption arises in warm gas with Tex of 400-700 K, whereas the CO2 absorption originates in cooler gas of app. 250 K (as in Lahuis 2006). No other absorption features are detected. Limits of those molecules are determined and compared with disk models. The inferred ratios wrt. C2H2 and HCN are roughly consistent with models of the chemistry in high-T gas. Models of UV irradiated disk surfaces generally agree better than pure X-ray models. The limit on NH3/HCN implies that evaporation of NH3 containing ices is only a minor contributor. The inferred ratios also compare well with those found in comets, suggesting that part of the cometary material may derive from warm inner disk gas. High resolution simulations show that future instruments on JWST, ELTs, SOFIA and SPICA can probe up to an order of magnitude lower ratios and put important new constraints on the models, especially if pushed to high S/N ratios. 
Jeanette E. Bast, Fred Lahuis, Ewine F. van Dishoeck, and Alexander   G.G.M. Tielens
astro-ph.SR astro-ph.EP astro-ph.GA