Radio continuum observations of Class I protostellar discs in Taurus: constraining the greybody tail at centimetre wavelengths★
| Autor: | Paul F. Scott, Michael P. Hobson, Timothy W. Shimwell, Rachael E. Ainsworth, Tom Ray, Carmen Rodríguez-Gonzálvez, Thomas M. O. Franzen, Natasha Hurley-Walker, Elizabeth Waldram, Anthony Lasenby, David Titterington, Keith Grainge, John Richer, Malak Olamaie, Yvette C. Perrott, Anna M. M. Scaife, Michel P. Schammel, Richard D. E. Saunders, Jane V. Buckle, Guy G. Pooley, Matthew L. Davies |
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| Rok vydání: | 2012 |
| Předmět: |
Physics
education.field_of_study 010504 meteorology & atmospheric sciences Opacity Young stellar object Molecular cloud Population Continuum (design consultancy) Giant planet Flux Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics 01 natural sciences Spectral line Space and Planetary Science 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics education 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics 0105 earth and related environmental sciences |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 420:3334-3343 |
| ISSN: | 0035-8711 |
| Popis: | We present deep 1.8 cm (16 GHz) radio continuum imaging of seven young stellar objects in the Taurus molecular cloud. These objects have previously been extensively studied in the sub-mm to NIR range and their SEDs modelled to provide reliable physical and geometrical parametres.We use this new data to constrain the properties of the long-wavelength tail of the greybody spectrum, which is expected to be dominated by emission from large dust grains in the protostellar disk. We find spectra consistent with the opacity indices expected for such a population, with an average opacity index of beta = 0.26+/-0.22 indicating grain growth within the disks. We use spectra fitted jointly to radio and sub-mm data to separate the contributions from thermal dust and radio emission at 1.8 cm and derive disk masses directly from the cm-wave dust contribution. We find that disk masses derived from these flux densities under assumptions consistent with the literature are systematically higher than those calculated from sub-mm data, and meet the criteria for giant planet formation in a number of cases. |
| Databáze: | OpenAIRE |
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