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    Dense Gas Towards the RX J1713.7–3946 Supernova Remnant

    199553_99588_Dense_gas.pdf (2.791Mb)
    Access Status
    Open access
    Authors
    Maxted, N.
    Rowell, G.
    Dawson, B.
    Burton, M.
    Fukui, Y.
    Lazendic, J.
    Kawamura, A.
    Horachi, H.
    Sano, H.
    Walsh, Andrew
    Yoshiike, S.
    Fukuda, T.
    Date
    2013
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Maxted, N. and Rowell, G. and Dawson, B. and Burton, M. and Fukui, Y. and Lazendic, J. and Kawamura, A. et al. 2013. Dense Gas Towards the RX J1713.7–3946 Supernova Remnant. Publications of the Astronomical Society of Australia. 30: Article ID e055.
    Source Title
    Publications of the Astronomical Society of Australia
    DOI
    10.1017/pasa.2013.35
    ISSN
    1323-3580
    URI
    http://hdl.handle.net/20.500.11937/38909
    Collection
    • Curtin Research Publications
    Abstract

    We present results from a Mopra 7 mm-wavelength survey that targeted the dense gas-tracing CS(1-0) transition towards the young γ-ray-bright supernova remnant, RX J1713.7–3946 (SNR G 347.3−0.5). In a hadronic γ-ray emission scenario, where cosmic ray (CR) protons interact with gas to produce the observed γ-ray emission, the mass of potential CR target material is an important factor. We summarise newly discovered dense gas components, towards Cores G and L, and Clumps N1, N2, N3, and T1, which have masses of 1 – 104 M ☉. We argue that these components are not likely to contribute significantly to γ-ray emission in a hadronic γ-ray emission scenario. This would be the case if RX J1713.7–3946 were at either the currently favoured distance of ~1 kpc or an alternate distance (as suggested in some previous studies) of ~6 kpc. This survey also targeted the shock-tracing SiO molecule. Although no SiO emission corresponding to the RX J1713.7–3946 shock was observed, vibrationally excited SiO(1-0) maser emission was discovered towards what may be an evolved star. Observations taken 1 yr apart confirmed a transient nature, since the intensity, line-width, and central velocity of SiO(J = 1-0,v = 1,2) emission varied significantly.

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