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

  • Nigel I. Maxted (a1), Gavin P. Rowell (a1), Bruce R. Dawson (a1), Michael G. Burton (a2), Yasuo Fukui (a3), Jasmina Lazendic (a4), Akiko Kawamura (a3), Hirotaka Horachi (a3), Hidetoshi Sano (a3), Andrew J. Walsh (a5), Satoshi Yoshiike (a3) and Tatsuya Fukuda (a3)...

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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