Murchison Widefield Array and XMM-Newton observations of the Galactic supernova remnant G5.9+3.1

D. Onic, M. D. Filipovic, I. Bojicic, N. Hurley-Walker, B. Arbutina, T. G. Pannuti, C. Maitra, D. Urosevic, F. Haberl, N. Maxted, G. F. Wong, G. Rowell, M. E. Bell, J. R. Callingham, K. S. Dwarakanath, B. -Q. For, P. J. Hancock, L. Hindson, M. Johnston-Hollitt, A. D. Kapinska & 10 others E. Lenc, B. McKinley, J. Morgan, A. R. Offringa, L. E. Porter, P. Procopio, L. Staveley-Smith, R. B. Wayth, C. Wu, Q. Zheng

Research output: Contribution to journalArticle

Abstract

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 N-H similar to 0.80 +/- 10(22) cm(-2) and fitted temperatures spanning the range kT similar to 0.14-0.23 keV for all of the regions. The derived electron number densities n(e) for the whole SNR and the rims are also roughly comparable (ranging from similar to 0.20 f(-1/2) to similar to 0.40 f(-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 similar to 46 f(-1/2) M-circle dot.

Original languageEnglish
Article number93
Number of pages9
JournalASTRONOMY & ASTROPHYSICS
Volume625
DOIs
Publication statusPublished - 17 May 2019

Cite this

Onic, D., Filipovic, M. D., Bojicic, I., Hurley-Walker, N., Arbutina, B., Pannuti, T. G., ... Zheng, Q. (2019). Murchison Widefield Array and XMM-Newton observations of the Galactic supernova remnant G5.9+3.1. ASTRONOMY & ASTROPHYSICS, 625, [93]. https://doi.org/10.1051/0004-6361/201834230
Onic, D. ; Filipovic, M. D. ; Bojicic, I. ; Hurley-Walker, N. ; Arbutina, B. ; Pannuti, T. G. ; Maitra, C. ; Urosevic, D. ; Haberl, F. ; Maxted, N. ; Wong, G. F. ; Rowell, G. ; Bell, M. E. ; Callingham, J. R. ; Dwarakanath, K. S. ; For, B. -Q. ; Hancock, P. J. ; Hindson, L. ; Johnston-Hollitt, M. ; Kapinska, A. D. ; Lenc, E. ; McKinley, B. ; Morgan, J. ; Offringa, A. R. ; Porter, L. E. ; Procopio, P. ; Staveley-Smith, L. ; Wayth, R. B. ; Wu, C. ; Zheng, Q. / Murchison Widefield Array and XMM-Newton observations of the Galactic supernova remnant G5.9+3.1. In: ASTRONOMY & ASTROPHYSICS. 2019 ; Vol. 625.
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title = "Murchison Widefield Array and XMM-Newton observations of the Galactic supernova remnant G5.9+3.1",
abstract = "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 N-H similar to 0.80 +/- 10(22) cm(-2) and fitted temperatures spanning the range kT similar to 0.14-0.23 keV for all of the regions. The derived electron number densities n(e) for the whole SNR and the rims are also roughly comparable (ranging from similar to 0.20 f(-1/2) to similar to 0.40 f(-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 similar to 46 f(-1/2) M-circle dot.",
keywords = "ISM: individual objects: G5.9+3.1, ISM: supernova remnants, radio continuum: ISM, radiation mechanisms: general, RADIO-CONTINUUM SURVEY, PARTICLE-ACCELERATION, COSMIC-RAYS, DISCOVERY, SPECTRA, PLANE",
author = "D. Onic and Filipovic, {M. D.} and I. Bojicic and N. Hurley-Walker and B. Arbutina and Pannuti, {T. G.} and C. Maitra and D. Urosevic and F. Haberl and N. Maxted and Wong, {G. F.} and G. Rowell and Bell, {M. E.} and Callingham, {J. R.} and Dwarakanath, {K. S.} and For, {B. -Q.} and Hancock, {P. J.} and L. Hindson and M. Johnston-Hollitt and Kapinska, {A. D.} and E. Lenc and B. McKinley and J. Morgan and Offringa, {A. R.} and Porter, {L. E.} and P. Procopio and L. Staveley-Smith and Wayth, {R. B.} and C. Wu and Q. Zheng",
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language = "English",
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journal = "ASTRONOMY & ASTROPHYSICS",
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Onic, D, Filipovic, MD, Bojicic, I, Hurley-Walker, N, Arbutina, B, Pannuti, TG, Maitra, C, Urosevic, D, Haberl, F, Maxted, N, Wong, GF, Rowell, G, Bell, ME, Callingham, JR, Dwarakanath, KS, For, B-Q, Hancock, PJ, Hindson, L, Johnston-Hollitt, M, Kapinska, AD, Lenc, E, McKinley, B, Morgan, J, Offringa, AR, Porter, LE, Procopio, P, Staveley-Smith, L, Wayth, RB, Wu, C & Zheng, Q 2019, 'Murchison Widefield Array and XMM-Newton observations of the Galactic supernova remnant G5.9+3.1' ASTRONOMY & ASTROPHYSICS, vol. 625, 93. https://doi.org/10.1051/0004-6361/201834230

Murchison Widefield Array and XMM-Newton observations of the Galactic supernova remnant G5.9+3.1. / Onic, D.; Filipovic, M. D.; Bojicic, I.; Hurley-Walker, N.; Arbutina, B.; Pannuti, T. G.; Maitra, C.; Urosevic, D.; Haberl, F.; Maxted, N.; Wong, G. F.; Rowell, G.; Bell, M. E.; Callingham, J. R.; Dwarakanath, K. S.; For, B. -Q.; Hancock, P. J.; Hindson, L.; Johnston-Hollitt, M.; Kapinska, A. D.; Lenc, E.; McKinley, B.; Morgan, J.; Offringa, A. R.; Porter, L. E.; Procopio, P.; Staveley-Smith, L.; Wayth, R. B.; Wu, C.; Zheng, Q.

In: ASTRONOMY & ASTROPHYSICS, Vol. 625, 93, 17.05.2019.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Murchison Widefield Array and XMM-Newton observations of the Galactic supernova remnant G5.9+3.1

AU - Onic, D.

AU - Filipovic, M. D.

AU - Bojicic, I.

AU - Hurley-Walker, N.

AU - Arbutina, B.

AU - Pannuti, T. G.

AU - Maitra, C.

AU - Urosevic, D.

AU - Haberl, F.

AU - Maxted, N.

AU - Wong, G. F.

AU - Rowell, G.

AU - Bell, M. E.

AU - Callingham, J. R.

AU - Dwarakanath, K. S.

AU - For, B. -Q.

AU - Hancock, P. J.

AU - Hindson, L.

AU - Johnston-Hollitt, M.

AU - Kapinska, A. D.

AU - Lenc, E.

AU - McKinley, B.

AU - Morgan, J.

AU - Offringa, A. R.

AU - Porter, L. E.

AU - Procopio, P.

AU - Staveley-Smith, L.

AU - Wayth, R. B.

AU - Wu, C.

AU - Zheng, Q.

PY - 2019/5/17

Y1 - 2019/5/17

N2 - 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 N-H similar to 0.80 +/- 10(22) cm(-2) and fitted temperatures spanning the range kT similar to 0.14-0.23 keV for all of the regions. The derived electron number densities n(e) for the whole SNR and the rims are also roughly comparable (ranging from similar to 0.20 f(-1/2) to similar to 0.40 f(-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 similar to 46 f(-1/2) M-circle dot.

AB - 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 N-H similar to 0.80 +/- 10(22) cm(-2) and fitted temperatures spanning the range kT similar to 0.14-0.23 keV for all of the regions. The derived electron number densities n(e) for the whole SNR and the rims are also roughly comparable (ranging from similar to 0.20 f(-1/2) to similar to 0.40 f(-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 similar to 46 f(-1/2) M-circle dot.

KW - ISM: individual objects: G5.9+3.1

KW - ISM: supernova remnants

KW - radio continuum: ISM

KW - radiation mechanisms: general

KW - RADIO-CONTINUUM SURVEY

KW - PARTICLE-ACCELERATION

KW - COSMIC-RAYS

KW - DISCOVERY

KW - SPECTRA

KW - PLANE

U2 - 10.1051/0004-6361/201834230

DO - 10.1051/0004-6361/201834230

M3 - Article

VL - 625

JO - ASTRONOMY & ASTROPHYSICS

JF - ASTRONOMY & ASTROPHYSICS

SN - 0004-6361

M1 - 93

ER -