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Article: Multiwavelength study of a new Galactic SNR G332.5-5.6

TitleMultiwavelength study of a new Galactic SNR G332.5-5.6
Authors
KeywordsSurveys
Radio continuum: general
Supernova remnants
Issue Date2007
Citation
Monthly Notices of the Royal Astronomical Society, 2007, v. 381, n. 1, p. 377-388 How to Cite?
AbstractWe present compelling evidence for confirmation of a Galactic supernova remnant (SNR) candidate, G332.5-5.6, based initially on identification of new, filamentary, optical emission-line nebulosity seen in the arcsecond resolution images from the Anglo Australian Observatory (AAO)/United Kingdom Schmidt Telescope (UKST) Hα survey. The extant radio observations and X-ray data which we have independently re-reduced, together with new optical spectroscopy of the large-scale fragmented nebulosity, confirm the identification. Optical spectra, taken across five different, widely separated nebula regions of the remnant as seen in the Hα images, show average ratios of [N ii]/Hα = 2.42, [S ii]/Hα = 2.10 and [S ii] 6717/6731 = 1.23, as well as strong [O i] 6300, 6364 Å and [O ii] 3727 Å emission. These ratios are firmly 3within those typical of SNRs. Here, we also present the radio-continuum detection of the SNR at 20/13 cm from observations with the Australia Telescope Compact Array (ATCA). Radio emission is also seen at 4850 MHz, in the Parkes-MIT-NRAO (PMN) survey and at 843 MHz from the Sydney University Molonglo Sky Survey (SUMSS) survey. We estimate an angular diameter of ∼30 arcmin and obtain an average radio spectral index of α = -0.6 ± 0.1 which indicates the non-thermal nature of G332.5-5.6. Fresh analysis of existing ROSAT X-ray data in the vicinity also confirms the existence of the SNR. The distance to G332.5-5.6 has been independently estimated by Reynoso and Green as 3.4 kpc based on measurements of the H i λ21-cm line seen in absorption against the continuum emission. Our cruder estimates via assumptions on the height of the dust layer (3.1 kpc) and using the Σ-D relation (4 kpc) are in good agreement. © 2007 RAS.
Persistent Identifierhttp://hdl.handle.net/10722/208798
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806

 

DC FieldValueLanguage
dc.contributor.authorStupar, Milorad-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorFilipovíc, Miroslav D.-
dc.contributor.authorFrew, David J.-
dc.contributor.authorBojičić, Ivan S.-
dc.contributor.authorAschenbach, Bernd R.-
dc.date.accessioned2015-03-23T02:01:44Z-
dc.date.available2015-03-23T02:01:44Z-
dc.date.issued2007-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2007, v. 381, n. 1, p. 377-388-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/208798-
dc.description.abstractWe present compelling evidence for confirmation of a Galactic supernova remnant (SNR) candidate, G332.5-5.6, based initially on identification of new, filamentary, optical emission-line nebulosity seen in the arcsecond resolution images from the Anglo Australian Observatory (AAO)/United Kingdom Schmidt Telescope (UKST) Hα survey. The extant radio observations and X-ray data which we have independently re-reduced, together with new optical spectroscopy of the large-scale fragmented nebulosity, confirm the identification. Optical spectra, taken across five different, widely separated nebula regions of the remnant as seen in the Hα images, show average ratios of [N ii]/Hα = 2.42, [S ii]/Hα = 2.10 and [S ii] 6717/6731 = 1.23, as well as strong [O i] 6300, 6364 Å and [O ii] 3727 Å emission. These ratios are firmly 3within those typical of SNRs. Here, we also present the radio-continuum detection of the SNR at 20/13 cm from observations with the Australia Telescope Compact Array (ATCA). Radio emission is also seen at 4850 MHz, in the Parkes-MIT-NRAO (PMN) survey and at 843 MHz from the Sydney University Molonglo Sky Survey (SUMSS) survey. We estimate an angular diameter of ∼30 arcmin and obtain an average radio spectral index of α = -0.6 ± 0.1 which indicates the non-thermal nature of G332.5-5.6. Fresh analysis of existing ROSAT X-ray data in the vicinity also confirms the existence of the SNR. The distance to G332.5-5.6 has been independently estimated by Reynoso and Green as 3.4 kpc based on measurements of the H i λ21-cm line seen in absorption against the continuum emission. Our cruder estimates via assumptions on the height of the dust layer (3.1 kpc) and using the Σ-D relation (4 kpc) are in good agreement. © 2007 RAS.-
dc.languageeng-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.subjectSurveys-
dc.subjectRadio continuum: general-
dc.subjectSupernova remnants-
dc.titleMultiwavelength study of a new Galactic SNR G332.5-5.6-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1111/j.1365-2966.2007.12296.x-
dc.identifier.scopuseid_2-s2.0-35148887183-
dc.identifier.volume381-
dc.identifier.issue1-
dc.identifier.spage377-
dc.identifier.epage388-
dc.identifier.eissn1365-2966-

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