1. RRI Digital Repository
  2. 04. Astronomy and Astrophysics
  3. Research Papers (A&A)
Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7221
Full metadata record
DC FieldValueLanguage
dc.contributor.authorOni´, D.-
dc.contributor.authorFilipovi´, M. D.-
dc.contributor.authorDwarakanath, K.S.-
dc.contributor.author+27 Co-Authors-
dc.date.accessioned2019-06-06T18:15:12Z-
dc.date.available2019-06-06T18:15:12Z-
dc.date.issued2019-05-
dc.identifier.citationAstronomy & Astrophysics, 2019, Vol.625, p A93en_US
dc.identifier.issn0004-6361-
dc.identifier.issn1432-0746 (Online)-
dc.identifier.urihttp://hdl.handle.net/2289/7221-
dc.descriptionOpen Access.en_US
dc.description.abstractIn 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. 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. 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 1GHz to be around 2.7Jy. 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~0.80x1022 cm−2 and fitted temperatures spanning the range kT~0.14-0.23keV 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 ~0.20f−1/2 cm−3 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−1/2M⊙.en_US
dc.language.isoenen_US
dc.publisherEDP Sciences for European Southern Observatoryen_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2019A%26A...625A..93O/abstracten_US
dc.relation.urihttps://arxiv.org/abs/1904.06541en_US
dc.relation.urihttps://doi.org/10.1051/0004-6361/201834230en_US
dc.rights2019 European Southern Observatoryen_US
dc.subjectISMen_US
dc.subjectindividual objectsen_US
dc.subjectG5.9+3.1 – ISMen_US
dc.subjectsupernova remnants – radio continuumen_US
dc.subjectISM – radiation mechanismsen_US
dc.subjectgeneralen_US
dc.titleMurchison Widefield Array and XMM-Newton observations of the Galactic supernova remnant G5.9+3.1en_US
dc.typeArticleen_US
Appears in Collections:Research Papers (A&A)

Files in This Item:
File Description SizeFormat 
2019_A&A_Vol.625_pA93.pdfOpen Access1.41 MBAdobe PDFView/Open
2019_A&A_Vol.625_pA93.epub
  Restricted Access		Open Access3.34 MBEPUBView/Open Request a copy
Show simple item record


Items in RRI Digital Repository are protected by copyright, with all rights reserved, unless otherwise indicated.