Late-time Flattening of Type Ia Supernova Light Curves: Constraints from SN 2014J in M82
The very nearby Type Ia supernova 2014J in M82 offers a rare opportunity to study the physics of thermonuclear supernovae at extremely late phases ( 800 days). Using the Hubble Space Telescope, we obtained 6 epochs of high-precision photometry for SN 2014J from 277 days to 1181 days past the B-band...
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| Veröffentlicht in: | The Astrophysical journal 2018-01, Vol.852 (2), p.89 |
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| creator | Yang, Yi Wang, Lifan Baade, Dietrich Brown, Peter. J. Cikota, Aleksandar Cracraft, Misty Höflich, Peter A. Maund, Justyn R. Patat, Ferdinando Sparks, William B. Spyromilio, Jason Stevance, Heloise F. Wang, Xiaofeng Wheeler, J. Craig |
| description | The very nearby Type Ia supernova 2014J in M82 offers a rare opportunity to study the physics of thermonuclear supernovae at extremely late phases ( 800 days). Using the Hubble Space Telescope, we obtained 6 epochs of high-precision photometry for SN 2014J from 277 days to 1181 days past the B-band maximum light. The reprocessing of electrons and X-rays emitted by the radioactive decay chain is needed to explain the significant flattening of both the F606W-band and the pseudo-bolometric light curves. The flattening confirms previous predictions that the late-time evolution of type Ia supernova luminosities requires additional energy input from the decay of 57Co. By assuming the F606W-band luminosity scales with the bolometric luminosity at ∼500 days after the B-band maximum light, a mass ratio is required. This mass ratio is roughly ∼3 times the solar ratio and favors a progenitor white dwarf with a mass near the Chandrasekhar limit. A similar fit using the constructed pseudo-bolometric luminosity gives a mass ratio . Astrometric tests based on the multi-epoch HST ACS/WFC images reveal no significant circumstellar light echoes in between 0.3 and 100 pc from the supernova. |
| doi_str_mv | 10.3847/1538-4357/aa9e4c |
| format | Article |
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J. ; Cikota, Aleksandar ; Cracraft, Misty ; Höflich, Peter A. ; Maund, Justyn R. ; Patat, Ferdinando ; Sparks, William B. ; Spyromilio, Jason ; Stevance, Heloise F. ; Wang, Xiaofeng ; Wheeler, J. Craig</creator><creatorcontrib>Yang, Yi ; Wang, Lifan ; Baade, Dietrich ; Brown, Peter. J. ; Cikota, Aleksandar ; Cracraft, Misty ; Höflich, Peter A. ; Maund, Justyn R. ; Patat, Ferdinando ; Sparks, William B. ; Spyromilio, Jason ; Stevance, Heloise F. ; Wang, Xiaofeng ; Wheeler, J. Craig</creatorcontrib><description>The very nearby Type Ia supernova 2014J in M82 offers a rare opportunity to study the physics of thermonuclear supernovae at extremely late phases ( 800 days). Using the Hubble Space Telescope, we obtained 6 epochs of high-precision photometry for SN 2014J from 277 days to 1181 days past the B-band maximum light. The reprocessing of electrons and X-rays emitted by the radioactive decay chain is needed to explain the significant flattening of both the F606W-band and the pseudo-bolometric light curves. The flattening confirms previous predictions that the late-time evolution of type Ia supernova luminosities requires additional energy input from the decay of 57Co. By assuming the F606W-band luminosity scales with the bolometric luminosity at ∼500 days after the B-band maximum light, a mass ratio is required. This mass ratio is roughly ∼3 times the solar ratio and favors a progenitor white dwarf with a mass near the Chandrasekhar limit. A similar fit using the constructed pseudo-bolometric luminosity gives a mass ratio . Astrometric tests based on the multi-epoch HST ACS/WFC images reveal no significant circumstellar light echoes in between 0.3 and 100 pc from the supernova.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/aa9e4c</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Astrophysics ; Bolometers ; Echoes ; Flattening ; Hubble Space Telescope ; Light curve ; Luminosity ; nuclear reactions, nucleosynthesis, abundances ; Radioactive decay ; Reprocessing ; Space telescopes ; Stellar evolution ; Supernova ; Supernovae ; supernovae: individual (SN 2014J) ; White dwarf stars</subject><ispartof>The Astrophysical journal, 2018-01, Vol.852 (2), p.89</ispartof><rights>2018. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Jan 10, 2018</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c445t-6eb5572c028103f76d4db5b0118391dfdbd61c92865b57a31c4e4701ed5157003</citedby><cites>FETCH-LOGICAL-c445t-6eb5572c028103f76d4db5b0118391dfdbd61c92865b57a31c4e4701ed5157003</cites><orcidid>0000-0003-1349-6538 ; 0000-0002-0537-3573 ; 0000-0003-0733-7215 ; 0000-0002-0504-4323 ; 0000-0001-6815-4055 ; 0000-0001-6272-5507 ; 0000-0002-7698-3002 ; 0000-0002-7334-2357 ; 0000-0002-6535-8500 ; 0000-0002-9011-6829</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/aa9e4c/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>314,776,780,27901,27902,38867,53842</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4357/aa9e4c$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc></links><search><creatorcontrib>Yang, Yi</creatorcontrib><creatorcontrib>Wang, Lifan</creatorcontrib><creatorcontrib>Baade, Dietrich</creatorcontrib><creatorcontrib>Brown, Peter. J.</creatorcontrib><creatorcontrib>Cikota, Aleksandar</creatorcontrib><creatorcontrib>Cracraft, Misty</creatorcontrib><creatorcontrib>Höflich, Peter A.</creatorcontrib><creatorcontrib>Maund, Justyn R.</creatorcontrib><creatorcontrib>Patat, Ferdinando</creatorcontrib><creatorcontrib>Sparks, William B.</creatorcontrib><creatorcontrib>Spyromilio, Jason</creatorcontrib><creatorcontrib>Stevance, Heloise F.</creatorcontrib><creatorcontrib>Wang, Xiaofeng</creatorcontrib><creatorcontrib>Wheeler, J. Craig</creatorcontrib><title>Late-time Flattening of Type Ia Supernova Light Curves: Constraints from SN 2014J in M82</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>The very nearby Type Ia supernova 2014J in M82 offers a rare opportunity to study the physics of thermonuclear supernovae at extremely late phases ( 800 days). Using the Hubble Space Telescope, we obtained 6 epochs of high-precision photometry for SN 2014J from 277 days to 1181 days past the B-band maximum light. The reprocessing of electrons and X-rays emitted by the radioactive decay chain is needed to explain the significant flattening of both the F606W-band and the pseudo-bolometric light curves. The flattening confirms previous predictions that the late-time evolution of type Ia supernova luminosities requires additional energy input from the decay of 57Co. By assuming the F606W-band luminosity scales with the bolometric luminosity at ∼500 days after the B-band maximum light, a mass ratio is required. This mass ratio is roughly ∼3 times the solar ratio and favors a progenitor white dwarf with a mass near the Chandrasekhar limit. A similar fit using the constructed pseudo-bolometric luminosity gives a mass ratio . Astrometric tests based on the multi-epoch HST ACS/WFC images reveal no significant circumstellar light echoes in between 0.3 and 100 pc from the supernova.</description><subject>Astrophysics</subject><subject>Bolometers</subject><subject>Echoes</subject><subject>Flattening</subject><subject>Hubble Space Telescope</subject><subject>Light curve</subject><subject>Luminosity</subject><subject>nuclear reactions, nucleosynthesis, abundances</subject><subject>Radioactive decay</subject><subject>Reprocessing</subject><subject>Space telescopes</subject><subject>Stellar evolution</subject><subject>Supernova</subject><subject>Supernovae</subject><subject>supernovae: individual (SN 2014J)</subject><subject>White dwarf stars</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNp1kM9LwzAYhoMoOKd3jwE9WpefTeJNhtNJ1cMm7BbSNp0dW1uTdLD_3paKXvT08X087_vBA8AlRrdUMjHBnMqIUS4mxijLsiMw-jkdgxFCiEUxFatTcOb9pl-JUiOwSkywUSh3Fs62JgRbldUa1gVcHhoL5wYu2sa6qt4bmJTrjwCnrdtbfwendeWDM2UVPCxcvYOLV0gQZs-wrOCLJOfgpDBbby--5xi8zx6W06coeXucT--TKGOMhyi2KeeCZIhIjGgh4pzlKU8RxpIqnBd5msc4U0TGPOXCUJwxywTCNueYC4ToGFwNvY2rP1vrg97Urau6l5rQmCsklVQdhQYqc7X3zha6ceXOuIPGSPf-dC9L97L04K-LXA-Rsm5-O02z0ZITTbRUusmLDrv5A_u39QuBW3tI</recordid><startdate>20180110</startdate><enddate>20180110</enddate><creator>Yang, Yi</creator><creator>Wang, Lifan</creator><creator>Baade, Dietrich</creator><creator>Brown, Peter. 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J. ; Cikota, Aleksandar ; Cracraft, Misty ; Höflich, Peter A. ; Maund, Justyn R. ; Patat, Ferdinando ; Sparks, William B. ; Spyromilio, Jason ; Stevance, Heloise F. ; Wang, Xiaofeng ; Wheeler, J. 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Craig</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Late-time Flattening of Type Ia Supernova Light Curves: Constraints from SN 2014J in M82</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2018-01-10</date><risdate>2018</risdate><volume>852</volume><issue>2</issue><spage>89</spage><pages>89-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>The very nearby Type Ia supernova 2014J in M82 offers a rare opportunity to study the physics of thermonuclear supernovae at extremely late phases ( 800 days). Using the Hubble Space Telescope, we obtained 6 epochs of high-precision photometry for SN 2014J from 277 days to 1181 days past the B-band maximum light. The reprocessing of electrons and X-rays emitted by the radioactive decay chain is needed to explain the significant flattening of both the F606W-band and the pseudo-bolometric light curves. The flattening confirms previous predictions that the late-time evolution of type Ia supernova luminosities requires additional energy input from the decay of 57Co. By assuming the F606W-band luminosity scales with the bolometric luminosity at ∼500 days after the B-band maximum light, a mass ratio is required. This mass ratio is roughly ∼3 times the solar ratio and favors a progenitor white dwarf with a mass near the Chandrasekhar limit. A similar fit using the constructed pseudo-bolometric luminosity gives a mass ratio . 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| source | Institute of Physics Open Access Journal Titles |
| subjects | Astrophysics Bolometers Echoes Flattening Hubble Space Telescope Light curve Luminosity nuclear reactions, nucleosynthesis, abundances Radioactive decay Reprocessing Space telescopes Stellar evolution Supernova Supernovae supernovae: individual (SN 2014J) White dwarf stars |
| title | Late-time Flattening of Type Ia Supernova Light Curves: Constraints from SN 2014J in M82 |
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