The early optical afterglow and non-thermal components of GRB 060218
Abstract We re-examine the UV/optical and X-ray observations of GRB 060218 during the prompt and afterglow phases. We present evidence in the UV/optical spectra that there is a synchrotron component contributing to the observed flux in the initial 1350 s. This result suggests that GRB 060218 is prod...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2019-04, Vol.484 (4), p.5484-5498 |
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| container_title | Monthly notices of the Royal Astronomical Society |
| container_volume | 484 |
| creator | Emery, S W K Page, M J Breeveld, A A Brown, P J Kuin, N P M Oates, S R De Pasquale, M |
| description | Abstract
We re-examine the UV/optical and X-ray observations of GRB 060218 during the prompt and afterglow phases. We present evidence in the UV/optical spectra that there is a synchrotron component contributing to the observed flux in the initial 1350 s. This result suggests that GRB 060218 is produced from a low-luminosity jet, which penetrates through its progenitor envelope after core collapse. The jet interacts with the surrounding medium to generate the UV/optical external shock synchrotron emission. After 1350 s, the thermal radiation in the UV/optical and X-ray becomes the dominant contribution to the observed flux. The UV/optical and X-ray spectra at 1350–10 000 s can be fitted with a spherically outflowing blackbody model, with an additional power-law component to the model at X-ray energies. |
| doi_str_mv | 10.1093/mnras/stz373 |
| format | Article |
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We re-examine the UV/optical and X-ray observations of GRB 060218 during the prompt and afterglow phases. We present evidence in the UV/optical spectra that there is a synchrotron component contributing to the observed flux in the initial 1350 s. This result suggests that GRB 060218 is produced from a low-luminosity jet, which penetrates through its progenitor envelope after core collapse. The jet interacts with the surrounding medium to generate the UV/optical external shock synchrotron emission. After 1350 s, the thermal radiation in the UV/optical and X-ray becomes the dominant contribution to the observed flux. The UV/optical and X-ray spectra at 1350–10 000 s can be fitted with a spherically outflowing blackbody model, with an additional power-law component to the model at X-ray energies.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stz373</identifier><language>eng</language><publisher>Oxford University Press</publisher><ispartof>Monthly notices of the Royal Astronomical Society, 2019-04, Vol.484 (4), p.5484-5498</ispartof><rights>2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society 2019</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c371t-997ca0fa4d7b7b620e48576e299ded8742f411ca7307741ca882d6ab1c06b9163</citedby><cites>FETCH-LOGICAL-c371t-997ca0fa4d7b7b620e48576e299ded8742f411ca7307741ca882d6ab1c06b9163</cites><orcidid>0000-0002-6689-6271 ; 0000-0001-6313-6616</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,1604,27924,27925</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stz373$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Emery, S W K</creatorcontrib><creatorcontrib>Page, M J</creatorcontrib><creatorcontrib>Breeveld, A A</creatorcontrib><creatorcontrib>Brown, P J</creatorcontrib><creatorcontrib>Kuin, N P M</creatorcontrib><creatorcontrib>Oates, S R</creatorcontrib><creatorcontrib>De Pasquale, M</creatorcontrib><title>The early optical afterglow and non-thermal components of GRB 060218</title><title>Monthly notices of the Royal Astronomical Society</title><description>Abstract
We re-examine the UV/optical and X-ray observations of GRB 060218 during the prompt and afterglow phases. We present evidence in the UV/optical spectra that there is a synchrotron component contributing to the observed flux in the initial 1350 s. This result suggests that GRB 060218 is produced from a low-luminosity jet, which penetrates through its progenitor envelope after core collapse. The jet interacts with the surrounding medium to generate the UV/optical external shock synchrotron emission. After 1350 s, the thermal radiation in the UV/optical and X-ray becomes the dominant contribution to the observed flux. The UV/optical and X-ray spectra at 1350–10 000 s can be fitted with a spherically outflowing blackbody model, with an additional power-law component to the model at X-ray energies.</description><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2019</creationdate><recordtype>article</recordtype><recordid>eNp9kE9LwzAchoMoWKc3P0BuXoz75U-T5qhzTmEgyDyXNE3cpE1KUpH56a3Os6f3hffhPTwIXVK4oaD5vA_J5Hkev7jiR6igXJaEaSmPUQHAS1IpSk_RWc7vACA4kwW632wddiZ1exyHcWdNh40fXXrr4ic2ocUhBjJuXeqnxcZ-iMGFMePo8erlDoMERqtzdOJNl93FX87Q68Nys3gk6-fV0-J2TSxXdCRaK2vAG9GqRjWSgRNVqaRjWreurZRgXlBqjeKglJhKVbFWmoZakI2mks_Q9eHXpphzcr4e0q43aV9TqH8M1L8G6oOBCb864PFj-J_8Bg4wXOs</recordid><startdate>20190421</startdate><enddate>20190421</enddate><creator>Emery, S W K</creator><creator>Page, M J</creator><creator>Breeveld, A A</creator><creator>Brown, P J</creator><creator>Kuin, N P M</creator><creator>Oates, S R</creator><creator>De Pasquale, M</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><orcidid>https://orcid.org/0000-0002-6689-6271</orcidid><orcidid>https://orcid.org/0000-0001-6313-6616</orcidid></search><sort><creationdate>20190421</creationdate><title>The early optical afterglow and non-thermal components of GRB 060218</title><author>Emery, S W K ; Page, M J ; Breeveld, A A ; Brown, P J ; Kuin, N P M ; Oates, S R ; De Pasquale, M</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c371t-997ca0fa4d7b7b620e48576e299ded8742f411ca7307741ca882d6ab1c06b9163</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2019</creationdate><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Emery, S W K</creatorcontrib><creatorcontrib>Page, M J</creatorcontrib><creatorcontrib>Breeveld, A A</creatorcontrib><creatorcontrib>Brown, P J</creatorcontrib><creatorcontrib>Kuin, N P M</creatorcontrib><creatorcontrib>Oates, S R</creatorcontrib><creatorcontrib>De Pasquale, M</creatorcontrib><collection>CrossRef</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Emery, S W K</au><au>Page, M J</au><au>Breeveld, A A</au><au>Brown, P J</au><au>Kuin, N P M</au><au>Oates, S R</au><au>De Pasquale, M</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The early optical afterglow and non-thermal components of GRB 060218</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2019-04-21</date><risdate>2019</risdate><volume>484</volume><issue>4</issue><spage>5484</spage><epage>5498</epage><pages>5484-5498</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>Abstract
We re-examine the UV/optical and X-ray observations of GRB 060218 during the prompt and afterglow phases. We present evidence in the UV/optical spectra that there is a synchrotron component contributing to the observed flux in the initial 1350 s. This result suggests that GRB 060218 is produced from a low-luminosity jet, which penetrates through its progenitor envelope after core collapse. The jet interacts with the surrounding medium to generate the UV/optical external shock synchrotron emission. After 1350 s, the thermal radiation in the UV/optical and X-ray becomes the dominant contribution to the observed flux. The UV/optical and X-ray spectra at 1350–10 000 s can be fitted with a spherically outflowing blackbody model, with an additional power-law component to the model at X-ray energies.</abstract><pub>Oxford University Press</pub><doi>10.1093/mnras/stz373</doi><tpages>15</tpages><orcidid>https://orcid.org/0000-0002-6689-6271</orcidid><orcidid>https://orcid.org/0000-0001-6313-6616</orcidid><oa>free_for_read</oa></addata></record> |
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| title | The early optical afterglow and non-thermal components of GRB 060218 |
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