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Identification of Volatiles Toward Young Stellar Objects

Identification of Volatiles Toward Young Stellar Objects. Kari A. Van Brunt University of MO—St. Louis Advisor: Dr. Erika Gibb. How Did We Get Here?. Key to understanding our solar system Study other solar systems Did ours form in a region with low mass YSOs?

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Identification of Volatiles Toward Young Stellar Objects

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  1. Identification of Volatiles Toward Young Stellar Objects Kari A. Van Brunt University of MO—St. Louis Advisor: Dr. Erika Gibb

  2. How Did We Get Here? • Key to understanding our solar system • Study other solar systems • Did ours form in a region with low mass YSOs? • Or did ours form in a region with massive stars nearby? • Study composition around YSOs in low mass regions and mixed regions and compare to the composition of our own solar system

  3. Studying Star Forming Regions • Studied at long wavelengths, in the radio and infrared regions • Regions are cold, thus emit radiation at longer wavelengths • Regions are filled with gas and dust, so the wavelength of radiation must be longer than the diameter of the dust particle, or in the submicron region, to be seen • The spectrograph on the space-based telescope, Spitzer covers the >5 µm region

  4. Model of a YSO Outflow Outer Disk Accretion/Inflow Inner Disk

  5. Observations • Used SpeX on IRTF (3m telescope) on Mauna Kea to study ices • Used a spectral range of 2.1-5µm • Resolving power was about 1,700 • Data reduced using Spextool • Used NIRSPEC on Keck (10m telescope) to study gases • Used a spectral range of 1-5µm • Resolving power was about 25,000 • Data reduced using command line IDL

  6. Ices in GV Tau

  7. Shape of ice feature is dependent on composition, temperature, and dust grain size Find the optical depth, fit a mixture of lab ices to the feature, giving the temperature and composition Find the column density (abundance) by integrating over the optical depth Ices in GV Tau

  8. HCN Gas at ~3µm in GV Tau

  9. Population Diagram • Assume LTE and that the profile is optically thin • Use the Boltzmann Equation to find T:

  10. Discussion • Water ice and carbon monoxide ice have been found in several sources • Analysis is underway • Further observations will be done in June to look for ices in other objects • Observation time has been applied for to obtain better signal-to-noise for the current objects so that the carbon monoxide ice feature can be better resolved • A quick look at the temperature indicates the ice is probably located in the disk rather than in the envelope. • HCN gas has been found in a pilot study of GV Tau • Preliminary results show a temperature of 550 K of the gas • This temperature indicates the gas may be in the disk, accreting onto the star, or in an outflow • Further analysis is ongoing • We will be applying for more time in the fall to characterize gas in other objects

  11. Questions? • Acknowledgments • Missouri-Space Grant Consortium for another year of support! • Dr. Erika Gibb and Dr. Bruce Wilking • Our collaborators, Terrence Rettig and Sean Brittain

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