COMBINED ANALYSIS OF IMAGES AND SPECTRAL ENERGY DISTRIBUTIONS OF TAURUS PROTOSTARS
| Autor: | Thomas P. Robitaille, Mercedes Gomez, Barbara A. Whitney, L. V. Gramajo |
|---|---|
| Rok vydání: | 2010 |
| Předmět: |
Physics
Molecular cloud Young stellar object Astronomy Spectral density Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics Spectral line Luminosity Space and Planetary Science Radiative transfer Astrophysics::Solar and Stellar Astrophysics Protostar Astrophysics::Earth and Planetary Astrophysics Stellar evolution Astrophysics::Galaxy Astrophysics |
| Zdroj: | The Astronomical Journal. 139:2504-2524 |
| ISSN: | 1538-3881 0004-6256 |
| DOI: | 10.1088/0004-6256/139/6/2504 |
| Popis: | We present an analysis of spectral energy distributions (SEDs), near- and mid-infrared images, and Spitzer spectra of eight embedded Class I/II objects in the Taurus-Auriga molecular cloud. The initial model for each source was chosen using the grid of young stellar objects (YSOs) and SED fitting tool of Robitaille et al. Then the models were refined using the radiative transfer code of Whitney et al. to fit both the spectra and the infrared images of these objects. In general, our models agree with previous published analyses. However, our combined models should provide more reliable determinations of the physical and geometrical parameters since they are derived from SEDs, including the Spitzer spectra, covering the complete spectral range; and high-resolution near-infrared and Spitzer IRAC images. The combination of SED and image modeling better constrains the different components (central source, disk, envelope) of the YSOs. Our derived luminosities are higher, on average, than previous estimates because we account for the viewing angles (usually nearly edge-on) of most of the sources. Our analysis suggests that the standard rotating collapsing protostar model with disks and bipolar cavities works well for the analyzed sample of objects in the Taurus molecular cloud. |
| Databáze: | OpenAIRE |
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