Volume 625, May 2019
|Number of page(s)||9|
|Section||Interstellar and circumstellar matter|
|Published online||17 May 2019|
Murchison Widefield Array and XMM-Newton observations of the Galactic supernova remnant G5.9+3.1
Department of Astronomy, Faculty of Mathematics, University of Belgrade,
Studentski trg 16,
2 Western Sydney University, Locked Bag 1797, Penrith South DC, NSW, Australia
3 International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth WA 6845, Australia
4 Department of Earth and Space Sciences, Space Science Center, Morehead State University, 235 Martindale Drive, Morehead, KY 40351, USA
5 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, 85748 Garching, Germany
6 School of Physics, The University of New South Wales, Sydney 2052, Australia
7 School of Physical Sciences, The University of Adelaide, Adelaide 5005, Australia
8 University of Technology Sydney, 15 Broadway, Ultimo, NSW 2007, Australia
9 Netherlands Institute for Radio Astronomy (ASTRON), PO Bus 2, 7990AA Dwingeloo, The Netherlands
10 Raman Research Institute, 560080 Bangalore, India
11 International Centre for Radio Astronomy Research (ICRAR), M468, University of Western Australia, Crawley, WA 6009, Australia
12 Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
13 CSIRO Astronomy and Space Science, Marsfield, NSW 1710, Australia
14 Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia
15 School of Physics, The University of Melbourne, Parkville, VIC 3010, Australia
16 Shanghai Astronomical Observatory, 80 Nandan Rd, Xuhui Qu, 200000 Shanghai Shi, PR China,
17 Isaac Newton Institute of Chile, Yugoslavia Branch, Serbia
Accepted: 4 April 2019
Aims. In this paper we discuss the radio continuum and X-ray properties of the so-far poorly studied Galactic supernova remnant (SNR) G5.9 + 3.1.
Methods. We present the radio spectral energy distribution (SED) of the Galactic SNR G5.9 + 3.1 obtained with the Murchison Widefield Array (MWA). Combining these new observations with the surveys at other radio continuum frequencies, we discuss the integrated radio continuum spectrum of this particular remnant. We have also analyzed an archival XMM-Newton observation, which represents the first detection of X-ray emission from this remnant.
Results. The SNR SED is very well explained by a simple power-law relation. The synchrotron radio spectral index of G5.9 + 3.1 is estimated to be 0.42 ± 0.03 and the integrated flux density at 1 GHz to be around 2.7 Jy. Furthermore, we propose that the identified point radio source, located centrally inside the SNR shell, is most probably a compact remnant of the supernova explosion. The shell-like X-ray morphology of G5.9 + 3.1 as revealed by XMM-Newton broadly matches the spatial distribution of the radio emission, where the radio-bright eastern and western rims are also readily detected in the X-ray while the radio-weak northern and southern rims are weak or absent in the X-ray. Extracted MOS1+MOS2+PN spectra from the whole SNR as well as the north, east, and west rims of the SNR are fit successfully with an optically thin thermal plasma model in collisional ionization equilibrium with a column density NH ~ 0.80 × 1022 cm−2 and fitted temperatures spanning the range kT ~ 0.14–0.23 keV for all of the regions. The derived electron number densities ne for the whole SNR and the rims are also roughly comparable (ranging from ~0.20f−1∕2 to ~0.40f−1∕2 cm−3, where f is the volume filling factor). We also estimate the swept-up mass of the X-ray emitting plasma associated with G5.9+3.1 to be ~46f−1∕2 M⊙.
Key words: ISM: individual objects: G5.9+3.1 / ISM: supernova remnants / radio continuum: ISM / radiation mechanisms: general
© ESO 2019
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