Further Characterizing the Planet Forming Region Around V1331 Cyg

Details Further Characterizing the Planet Forming Region Around V1331 Cyg Further Characterizing the Planet Forming Region Around V1331 Cyg

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21931405d&link_type=abstract

American Astronomical Society, AAS Meeting #219, #314.05

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High resolution L-band (3.0-3.9 μm) spectra of young stars with circumstellar disks provide a key window for probing the physical conditions and pre-biotic chemistry within the inner disk region where terrestrial-like planets are thought to form. Rich with transitions due to water, OH, and key organic compounds of biological interest, L-band spectra at high resolution (R > 18,000) are critical to elucidate the properties of each molecular component present. Well-suited for this purpose, our NIRSPEC/Keck observations of V1331 Cyg, an intermediate mass young stellar object (spectral type A8-G5), show strong OH and water emission at 1500K. At R=24,000, our spectra resolve individual lines in the crowded emission spectrum that is dominated by water, and enable us to also characterize the accompanying OH emission. By comparing the observed spectra with synthetic disk models we (1) probe the nature of the accretion mechanism in the inner disk from the temperature, column density, and line broadening of the water emission that is present, (2) examine the disk photochemistry from the abundance ratio of OH to water, and (3) employ the new HITEMP line list to make empirical improvements to the water line list and thereby detect or set detection limits on organic emission (e.g., C2H2, HCN, C2H6, H2CO, NH3, and CH4) that may underly the L-band water spectrum. Support for this research was provided in part by the NASA Origins of Solar Systems program NNH10A0061.

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