A Morphological Study of the Supernova Remnant RX J0852.0-4622 (Vela Jr.)
We conduct a multi-wavelength morphological study of the Galactic supernova remnant RXJ0852.0-4622 (also known as Vela Jr., Vela Z and G266.2-1.2). RX J0852.0-4622 is coincident with the edge of the larger Vela supernova remnant causing confusion in the attribution of some filamentary structures to...
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| creator | Maxted, Nigel I Filipovic, M D Sano, H Allen, G E Pannuti, T G Rowell, G P Grech, A Roper, Q Wong, G F Galvin, T J Fukui, Y Collier, J D Crawford, E J Grieve, K Horta, A D Manojlovic, P O'Brien, A |
| description | We conduct a multi-wavelength morphological study of the Galactic supernova remnant RXJ0852.0-4622 (also known as Vela Jr., Vela Z and G266.2-1.2). RX J0852.0-4622 is coincident with the edge of the larger Vela supernova remnant causing confusion in the attribution of some filamentary structures to either RX J0852.0-4622 or its larger sibling. We find that the RX J0852.0-4622 radio continuum emission can be characterised by a 2-dimensional shell with a radius of 0.90+/-0.01deg (or 11.8+/-0.6pc at an assumed distance of 750pc) centred at (l,b)=(133.08+/-0.01 deg,-46.34+/-0.01deg) (or RA=8h52m19.2s, Dec=-46deg20'24.0'', J2000), consistent with X-ray and gamma-ray emission. Although [OIII] emission features are generally associated with the Vela SNR, one particular [OIII] emission feature, which we denote as "the Vela Claw", morphologically matches a molecular clump that is thought to have been stripped by the stellar progenitor of the RX J0852.0-4622 SNR. We argue that the Vela Claw feature is possibly associated with RX J0852.0-4622. Towards the north-western edge of RX J0852.0-4622, we find a flattening of the radio spectral index towards another molecular clump also thought to be associated with RX J0852.0-4622. It is currently unclear whether this feature and the Vela Claw result from interactions between the RX J0852.0-4622 shock and the ISM. |
| doi_str_mv | 10.48550/arxiv.1809.02249 |
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RX J0852.0-4622 is coincident with the edge of the larger Vela supernova remnant causing confusion in the attribution of some filamentary structures to either RX J0852.0-4622 or its larger sibling. We find that the RX J0852.0-4622 radio continuum emission can be characterised by a 2-dimensional shell with a radius of 0.90+/-0.01deg (or 11.8+/-0.6pc at an assumed distance of 750pc) centred at (l,b)=(133.08+/-0.01 deg,-46.34+/-0.01deg) (or RA=8h52m19.2s, Dec=-46deg20'24.0'', J2000), consistent with X-ray and gamma-ray emission. Although [OIII] emission features are generally associated with the Vela SNR, one particular [OIII] emission feature, which we denote as "the Vela Claw", morphologically matches a molecular clump that is thought to have been stripped by the stellar progenitor of the RX J0852.0-4622 SNR. We argue that the Vela Claw feature is possibly associated with RX J0852.0-4622. Towards the north-western edge of RX J0852.0-4622, we find a flattening of the radio spectral index towards another molecular clump also thought to be associated with RX J0852.0-4622. It is currently unclear whether this feature and the Vela Claw result from interactions between the RX J0852.0-4622 shock and the ISM.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1809.02249</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Continuum radiation ; Emission ; Gamma ray astronomy ; Gamma rays ; Morphology ; Physics - High Energy Astrophysical Phenomena ; Supernova remnants ; Supernovae</subject><ispartof>arXiv.org, 2018-09</ispartof><rights>2018. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). 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RX J0852.0-4622 is coincident with the edge of the larger Vela supernova remnant causing confusion in the attribution of some filamentary structures to either RX J0852.0-4622 or its larger sibling. We find that the RX J0852.0-4622 radio continuum emission can be characterised by a 2-dimensional shell with a radius of 0.90+/-0.01deg (or 11.8+/-0.6pc at an assumed distance of 750pc) centred at (l,b)=(133.08+/-0.01 deg,-46.34+/-0.01deg) (or RA=8h52m19.2s, Dec=-46deg20'24.0'', J2000), consistent with X-ray and gamma-ray emission. Although [OIII] emission features are generally associated with the Vela SNR, one particular [OIII] emission feature, which we denote as "the Vela Claw", morphologically matches a molecular clump that is thought to have been stripped by the stellar progenitor of the RX J0852.0-4622 SNR. We argue that the Vela Claw feature is possibly associated with RX J0852.0-4622. Towards the north-western edge of RX J0852.0-4622, we find a flattening of the radio spectral index towards another molecular clump also thought to be associated with RX J0852.0-4622. It is currently unclear whether this feature and the Vela Claw result from interactions between the RX J0852.0-4622 shock and the ISM.</description><subject>Continuum radiation</subject><subject>Emission</subject><subject>Gamma ray astronomy</subject><subject>Gamma rays</subject><subject>Morphology</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Supernova remnants</subject><subject>Supernovae</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotj01PAjEURRsTEwnyA1zZxI0uZnx9nZZ2SYgfEIwJEONu0qGtQIbp2Jkh8u9FcHU3J_feQ8gNgzRTQsCjiT-bfcoU6BQQM31Besg5S1SGeEUGTbMFAJRDFIL3yGRE30Ks16EMX5uVKemi7eyBBk_btaOLrnaxCntD525Xmaql8086BSUwhSSTiPT-w5WGTmP6cE0uvSkbN_jPPlk-Py3Hr8ns_WUyHs0SIxCT46zTIjMF2IxpqZmwyitUcigLD25oJbNaWGG5Qlj5gmnupfQSfQHM-xXvk9tz7ckzr-NmZ-Ih__PNT75H4u5M1DF8d65p823oYnX8lCMDJpVmDPkvhtNUDg</recordid><startdate>20180906</startdate><enddate>20180906</enddate><creator>Maxted, Nigel I</creator><creator>Filipovic, M D</creator><creator>Sano, H</creator><creator>Allen, G E</creator><creator>Pannuti, T G</creator><creator>Rowell, G P</creator><creator>Grech, A</creator><creator>Roper, Q</creator><creator>Wong, G F</creator><creator>Galvin, T J</creator><creator>Fukui, Y</creator><creator>Collier, J D</creator><creator>Crawford, E J</creator><creator>Grieve, K</creator><creator>Horta, A D</creator><creator>Manojlovic, P</creator><creator>O'Brien, A</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20180906</creationdate><title>A Morphological Study of the Supernova Remnant RX J0852.0-4622 (Vela Jr.)</title><author>Maxted, Nigel I ; Filipovic, M D ; Sano, H ; Allen, G E ; Pannuti, T G ; Rowell, G P ; Grech, A ; Roper, Q ; Wong, G F ; Galvin, T J ; Fukui, Y ; Collier, J D ; Crawford, E J ; Grieve, K ; Horta, A D ; Manojlovic, P ; O'Brien, A</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a522-725e954ab0d4196915d8f828676bf0e7d61d95d5d3820cfb193f66f62fb01ffc3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2018</creationdate><topic>Continuum radiation</topic><topic>Emission</topic><topic>Gamma ray astronomy</topic><topic>Gamma rays</topic><topic>Morphology</topic><topic>Physics - High Energy Astrophysical Phenomena</topic><topic>Supernova remnants</topic><topic>Supernovae</topic><toplevel>online_resources</toplevel><creatorcontrib>Maxted, Nigel I</creatorcontrib><creatorcontrib>Filipovic, M D</creatorcontrib><creatorcontrib>Sano, H</creatorcontrib><creatorcontrib>Allen, G E</creatorcontrib><creatorcontrib>Pannuti, T G</creatorcontrib><creatorcontrib>Rowell, G P</creatorcontrib><creatorcontrib>Grech, A</creatorcontrib><creatorcontrib>Roper, Q</creatorcontrib><creatorcontrib>Wong, G F</creatorcontrib><creatorcontrib>Galvin, T J</creatorcontrib><creatorcontrib>Fukui, Y</creatorcontrib><creatorcontrib>Collier, J D</creatorcontrib><creatorcontrib>Crawford, E J</creatorcontrib><creatorcontrib>Grieve, K</creatorcontrib><creatorcontrib>Horta, A D</creatorcontrib><creatorcontrib>Manojlovic, P</creatorcontrib><creatorcontrib>O'Brien, A</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Maxted, Nigel I</au><au>Filipovic, M D</au><au>Sano, H</au><au>Allen, G E</au><au>Pannuti, T G</au><au>Rowell, G P</au><au>Grech, A</au><au>Roper, Q</au><au>Wong, G F</au><au>Galvin, T J</au><au>Fukui, Y</au><au>Collier, J D</au><au>Crawford, E J</au><au>Grieve, K</au><au>Horta, A D</au><au>Manojlovic, P</au><au>O'Brien, A</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>A Morphological Study of the Supernova Remnant RX J0852.0-4622 (Vela Jr.)</atitle><jtitle>arXiv.org</jtitle><date>2018-09-06</date><risdate>2018</risdate><eissn>2331-8422</eissn><abstract>We conduct a multi-wavelength morphological study of the Galactic supernova remnant RXJ0852.0-4622 (also known as Vela Jr., Vela Z and G266.2-1.2). RX J0852.0-4622 is coincident with the edge of the larger Vela supernova remnant causing confusion in the attribution of some filamentary structures to either RX J0852.0-4622 or its larger sibling. We find that the RX J0852.0-4622 radio continuum emission can be characterised by a 2-dimensional shell with a radius of 0.90+/-0.01deg (or 11.8+/-0.6pc at an assumed distance of 750pc) centred at (l,b)=(133.08+/-0.01 deg,-46.34+/-0.01deg) (or RA=8h52m19.2s, Dec=-46deg20'24.0'', J2000), consistent with X-ray and gamma-ray emission. Although [OIII] emission features are generally associated with the Vela SNR, one particular [OIII] emission feature, which we denote as "the Vela Claw", morphologically matches a molecular clump that is thought to have been stripped by the stellar progenitor of the RX J0852.0-4622 SNR. We argue that the Vela Claw feature is possibly associated with RX J0852.0-4622. Towards the north-western edge of RX J0852.0-4622, we find a flattening of the radio spectral index towards another molecular clump also thought to be associated with RX J0852.0-4622. It is currently unclear whether this feature and the Vela Claw result from interactions between the RX J0852.0-4622 shock and the ISM.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1809.02249</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Continuum radiation Emission Gamma ray astronomy Gamma rays Morphology Physics - High Energy Astrophysical Phenomena Supernova remnants Supernovae |
| title | A Morphological Study of the Supernova Remnant RX J0852.0-4622 (Vela Jr.) |
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