A Morphological Study of the Supernova Remnant Rx J0852.0-4622 (Vela Jr.)
We conduct a multiwavelength morphological study of the Galactic supernova remnant (SNR) RX J0852.0-4622 (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 SNR causing confusion in the attribution of some filamentary structures to either...
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| Veröffentlicht in: | The Astrophysical journal 2018-10, Vol.866 (2), p.76 |
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| creator | Maxted, Nigel I. Filipovi, 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. Manojlovi, P. O'Brien, A. |
| description | We conduct a multiwavelength morphological study of the Galactic supernova remnant (SNR) RX J0852.0-4622 (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 SNR 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 characterized by a two-dimensional shell with a radius of 0 90 0 01 (or 11.8 0.6 pc at an assumed distance of 750 pc) centered at (l, b) = (133 08 0 01,−46 34 0 01) (or R.A. = 8h52m19 2, decl. = −46°20′24 0, J2000), consistent with X-ray and gamma-ray emission. Although [O iii] emission features are generally associated with the Vela SNR, one particular [O iii] 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. Toward the northwestern edge of RX J0852.0-4622 , we find a flattening of the radio spectral index toward 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 interstellar medium gas. |
| doi_str_mv | 10.3847/1538-4357/aae082 |
| format | Article |
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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. ; Manojlovi, P. ; O'Brien, A.</creator><creatorcontrib>Maxted, Nigel I. ; Filipovi, 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. ; Manojlovi, P. ; O'Brien, A.</creatorcontrib><description>We conduct a multiwavelength morphological study of the Galactic supernova remnant (SNR) RX J0852.0-4622 (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 SNR 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 characterized by a two-dimensional shell with a radius of 0 90 0 01 (or 11.8 0.6 pc at an assumed distance of 750 pc) centered at (l, b) = (133 08 0 01,−46 34 0 01) (or R.A. = 8h52m19 2, decl. = −46°20′24 0, J2000), consistent with X-ray and gamma-ray emission. Although [O iii] emission features are generally associated with the Vela SNR, one particular [O iii] 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. Toward the northwestern edge of RX J0852.0-4622 , we find a flattening of the radio spectral index toward 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 interstellar medium gas.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/aae082</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>acceleration of particles ; Astrophysics ; Continuum radiation ; Emission ; Gamma emission ; Gamma rays ; gamma rays: ISM ; Interstellar gas ; Interstellar matter ; Interstellar medium ; ISM: supernova remnants ; Morphology ; radio continuum: ISM ; Supernova ; Supernova remnants</subject><ispartof>The Astrophysical journal, 2018-10, Vol.866 (2), p.76</ispartof><rights>2018. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Oct 20, 2018</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c445t-a05e9e49a49ca11966e599bc51851b57df6e386b62963bf9d98b0001fe73ce143</citedby><cites>FETCH-LOGICAL-c445t-a05e9e49a49ca11966e599bc51851b57df6e386b62963bf9d98b0001fe73ce143</cites><orcidid>0000-0003-2062-5692 ; 0000-0001-7658-1065 ; 0000-0002-2144-6912 ; 0000-0002-9516-1581 ; 0000-0003-2762-8378 ; 0000-0002-4990-9288</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/aae082/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>314,776,780,27901,27902,38867,53842</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/aae082$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc></links><search><creatorcontrib>Maxted, Nigel I.</creatorcontrib><creatorcontrib>Filipovi, 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>Manojlovi, P.</creatorcontrib><creatorcontrib>O'Brien, A.</creatorcontrib><title>A Morphological Study of the Supernova Remnant Rx J0852.0-4622 (Vela Jr.)</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>We conduct a multiwavelength morphological study of the Galactic supernova remnant (SNR) RX J0852.0-4622 (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 SNR 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 characterized by a two-dimensional shell with a radius of 0 90 0 01 (or 11.8 0.6 pc at an assumed distance of 750 pc) centered at (l, b) = (133 08 0 01,−46 34 0 01) (or R.A. = 8h52m19 2, decl. = −46°20′24 0, J2000), consistent with X-ray and gamma-ray emission. Although [O iii] emission features are generally associated with the Vela SNR, one particular [O iii] 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. Toward the northwestern edge of RX J0852.0-4622 , we find a flattening of the radio spectral index toward 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 interstellar medium gas.</description><subject>acceleration of particles</subject><subject>Astrophysics</subject><subject>Continuum radiation</subject><subject>Emission</subject><subject>Gamma emission</subject><subject>Gamma rays</subject><subject>gamma rays: ISM</subject><subject>Interstellar gas</subject><subject>Interstellar matter</subject><subject>Interstellar medium</subject><subject>ISM: supernova remnants</subject><subject>Morphology</subject><subject>radio continuum: ISM</subject><subject>Supernova</subject><subject>Supernova remnants</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNp1kE1Lw0AQhhdRsFbvHhf0oGDa_c7usRQ_WhShVfG2bJJd25Jm4yYR--9NiOhFT8MMz7wzPACcYjSiksVjzKmMGOXx2BiLJNkDg5_RPhgghFgkaPx6CI6qatO1RKkBmE3ggw_lyuf-bZ2aHC7rJttB72C9snDZlDYU_sPAhd0Wpqjh4hPOkeRkhCImCIEXLzY3cB5Gl8fgwJm8siffdQieb66fpnfR_ePtbDq5j1LGeB0ZxK2yTBmmUoOxEsJypZKUY8lxwuPMCUulSARRgiZOZUom7bfY2ZimFjM6BGd9bhn8e2OrWm98E4r2pCZUcMk4krilUE-lwVdVsE6XYb01Yacx0p0w3dnRnR3dC2tXzvuVtS9_M0250VIITXQsdJm5Frv6A_s39Qu7KXSD</recordid><startdate>20181020</startdate><enddate>20181020</enddate><creator>Maxted, Nigel I.</creator><creator>Filipovi, M. 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D.</au><au>Manojlovi, 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>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2018-10-20</date><risdate>2018</risdate><volume>866</volume><issue>2</issue><spage>76</spage><pages>76-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>We conduct a multiwavelength morphological study of the Galactic supernova remnant (SNR) RX J0852.0-4622 (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 SNR 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 characterized by a two-dimensional shell with a radius of 0 90 0 01 (or 11.8 0.6 pc at an assumed distance of 750 pc) centered at (l, b) = (133 08 0 01,−46 34 0 01) (or R.A. = 8h52m19 2, decl. = −46°20′24 0, J2000), consistent with X-ray and gamma-ray emission. Although [O iii] emission features are generally associated with the Vela SNR, one particular [O iii] 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. Toward the northwestern edge of RX J0852.0-4622 , we find a flattening of the radio spectral index toward 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 interstellar medium gas.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/aae082</doi><tpages>9</tpages><orcidid>https://orcid.org/0000-0003-2062-5692</orcidid><orcidid>https://orcid.org/0000-0001-7658-1065</orcidid><orcidid>https://orcid.org/0000-0002-2144-6912</orcidid><orcidid>https://orcid.org/0000-0002-9516-1581</orcidid><orcidid>https://orcid.org/0000-0003-2762-8378</orcidid><orcidid>https://orcid.org/0000-0002-4990-9288</orcidid><oa>free_for_read</oa></addata></record> |
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| subjects | acceleration of particles Astrophysics Continuum radiation Emission Gamma emission Gamma rays gamma rays: ISM Interstellar gas Interstellar matter Interstellar medium ISM: supernova remnants Morphology radio continuum: ISM Supernova Supernova remnants |
| title | A Morphological Study of the Supernova Remnant Rx J0852.0-4622 (Vela Jr.) |
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