Dense Gas Towards the RXJ1713.7-3946 Supernova Remnant
Abstract
We present results from a Mopra 7mm-wavelength survey that targeted the dense gas-tracing CS(1-0) transition towards the young gamma-ray-bright supernova remnant, RXJ1713.7-3946 (SNR G347.3-0.5). In a hadronic gamma-ray emission scenario, where cosmic ray protons interact with gas to produce the observed gamma-ray emission, the mass of potential cosmic ray 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 1-10^4 solar masses. We argue that these components are not likely to contribute significantly to gamma-ray emission in a hadronic gamma-ray emission scenario. This would be the case if RXJ1713.7-3946 were at either the currently favoured distance of ~1kpc or an alternate distance (as suggested in some previous studies) of ~6kpc. This survey also targeted the shock-tracing SiO molecule. Although no SiO emission corresponding to the RXJ1713.7-3946 shock was observed, vibrationally-excited SiO(1-0) maser emission was discovered towards what may be an evolved star. Observations taken one year apart confirmed a transient nature, since the intensity, line-width and central velocity of SiO(J=1-0,v=1,2) emission varied significantly.
Keywords
Cite
@article{arxiv.1310.7017,
title = {Dense Gas Towards the RXJ1713.7-3946 Supernova Remnant},
author = {Nigel I. Maxted and Gavin P. Rowell and Bruce R. Dawson and Michael G. Burton and Yasuo Fukui and Jasmina Lazendic and Akiko Kawamura and Hirotaka Horachi and Hidetoshi Sano and Andrew J. Walsh and Satoshi Yoshiike and Tatsuya Fukuda},
journal= {arXiv preprint arXiv:1310.7017},
year = {2015}
}
Comments
19 pages, 11 figures, accepted for publication in PASA