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    Radio continuum observations of Class I protostellar discs in Taurus: constraining the greybody tail at centimetre wavelengths

    245649_245649.pdf (918.7Kb)
    Access Status
    Open access
    Authors
    Scaife, A.
    Buckle, J.
    Ainsworth, R.
    Davies, M.
    Franzen, Thomas
    Grainge, K.
    Hobson, M.
    Hurley-Walker, Natasha
    Lasenby, A.
    Olamaie, M.
    Perrott, Y.
    Pooley, G.
    Ray, T.
    Richer, J.
    Rodriguez-Gonzalvez, C.
    Saunders, R.
    Schammel, M.
    Scott, P.
    Shimwell, T.
    Titterington, D.
    Waldram, E.
    Date
    2012
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Scaife, A. and Buckle, J. and Ainsworth, R. and Davies, M. and Franzen, T. and Grainge, K. and Hobson, M. et al. 2012. Radio continuum observations of Class I protostellar discs in Taurus: constraining the greybody tail at centimetre wavelengths. Monthly Notices of the Royal Astronomical Society. 420 (4): pp. 3334-3343.
    Source Title
    Monthly Notices of the Royal Astronomical Society
    DOI
    10.1111/j.1365-2966.2011.20254.x
    ISSN
    0035-8711
    Remarks

    Copyright © 2012 The Authors. Published by Oxford University Press on behalf of Royal Astronomical Society. All rights reserved.

    URI
    http://hdl.handle.net/20.500.11937/25549
    Collection
    • Curtin Research Publications
    Abstract

    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 submm to near-infrared range and their spectral energy distributions modelled to provide reliable physical and geometrical parameters. We use these 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 disc. 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 discs. We use spectra fitted jointly to radio and submm data to separate the contributions from thermal dust and radio emission at 1.8 cm and derive disc masses directly from the cm-wave dust contribution. We find that disc masses derived from these flux densities under assumptions consistent with the literature are systematically higher than those calculated from submm data, and meet the criteria for giant planet formation in a number of cases.

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