Nebular Spectroscopy of the "Blue Bump" Type Ia Supernova 2017cbv
We present nebular phase optical and near-infrared spectroscopy of the Type Ia supernova (SN) 2017cbv. The early light curves of SN 2017cbv showed a prominent blue bump in the U, B, and g bands lasting for ∼5 days. One interpretation of the early light curve is that the excess blue light is due to s...
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| Veröffentlicht in: | The Astrophysical journal 2018-08, Vol.863 (1), p.24 |
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| creator | Sand, D. J. Graham, M. L. Botyánszki, J. Hiramatsu, D. McCully, C. Valenti, S. Hosseinzadeh, G. Howell, D. A. Burke, J. Cartier, R. Diamond, T. Hsiao, E. Y. Jha, S. W. Kasen, D. Kumar, S. Marion, G. H. Suntzeff, N. Tartaglia, L. Wheeler, J. C. Wyatt, S. |
| description | We present nebular phase optical and near-infrared spectroscopy of the Type Ia supernova (SN) 2017cbv. The early light curves of SN 2017cbv showed a prominent blue bump in the U, B, and g bands lasting for ∼5 days. One interpretation of the early light curve is that the excess blue light is due to shocking of the SN ejecta against a nondegenerate companion star-a signature of the single degenerate scenario. If this is the correct interpretation, the interaction between the SN ejecta and the companion star could result in significant H (or helium) emission at late times, possibly along with other species, depending on the companion star and its orbital separation. A search for H emission in our +302 d spectrum yields a nondetection, with a LH < 8.0 × 1035 erg s−1 (given an assumed distance of D = 12.3 Mpc), which we verified by implanting simulated H emission into our data. We make a quantitative comparison to models of swept-up material stripped from a nondegenerate companion star and limit the mass of hydrogen that might remain undetected to MH < 1 × 10−4 M . A similar analysis of helium star related lines yields a MHe < 5 × 10−4 M . Taken at face value, these results argue against a nondegenerate H- or He-rich companion in Roche lobe overflow as the progenitor of SN 2017cbv. Alternatively, there could be weaknesses in the envelope-stripping and radiative transfer models necessary to interpret the strong H and He flux limits. |
| doi_str_mv | 10.3847/1538-4357/aacde8 |
| format | Article |
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J. ; Graham, M. L. ; Botyánszki, J. ; Hiramatsu, D. ; McCully, C. ; Valenti, S. ; Hosseinzadeh, G. ; Howell, D. A. ; Burke, J. ; Cartier, R. ; Diamond, T. ; Hsiao, E. Y. ; Jha, S. W. ; Kasen, D. ; Kumar, S. ; Marion, G. H. ; Suntzeff, N. ; Tartaglia, L. ; Wheeler, J. C. ; Wyatt, S.</creator><creatorcontrib>Sand, D. J. ; Graham, M. L. ; Botyánszki, J. ; Hiramatsu, D. ; McCully, C. ; Valenti, S. ; Hosseinzadeh, G. ; Howell, D. A. ; Burke, J. ; Cartier, R. ; Diamond, T. ; Hsiao, E. Y. ; Jha, S. W. ; Kasen, D. ; Kumar, S. ; Marion, G. H. ; Suntzeff, N. ; Tartaglia, L. ; Wheeler, J. C. ; Wyatt, S.</creatorcontrib><description>We present nebular phase optical and near-infrared spectroscopy of the Type Ia supernova (SN) 2017cbv. The early light curves of SN 2017cbv showed a prominent blue bump in the U, B, and g bands lasting for ∼5 days. One interpretation of the early light curve is that the excess blue light is due to shocking of the SN ejecta against a nondegenerate companion star-a signature of the single degenerate scenario. If this is the correct interpretation, the interaction between the SN ejecta and the companion star could result in significant H (or helium) emission at late times, possibly along with other species, depending on the companion star and its orbital separation. A search for H emission in our +302 d spectrum yields a nondetection, with a LH < 8.0 × 1035 erg s−1 (given an assumed distance of D = 12.3 Mpc), which we verified by implanting simulated H emission into our data. We make a quantitative comparison to models of swept-up material stripped from a nondegenerate companion star and limit the mass of hydrogen that might remain undetected to MH < 1 × 10−4 M . A similar analysis of helium star related lines yields a MHe < 5 × 10−4 M . Taken at face value, these results argue against a nondegenerate H- or He-rich companion in Roche lobe overflow as the progenitor of SN 2017cbv. Alternatively, there could be weaknesses in the envelope-stripping and radiative transfer models necessary to interpret the strong H and He flux limits.</description><identifier>ISSN: 0004-637X</identifier><identifier>ISSN: 1538-4357</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/aacde8</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Astrophysics ; Companion stars ; Computer simulation ; Ejecta ; H alpha line ; Helium ; Hydrogen ; Infrared spectra ; Infrared spectroscopy ; Light curve ; Near infrared radiation ; Near infrared spectroscopy ; Overflow ; Radiative transfer ; Radiative transfer models ; Spectrum analysis ; Supernova ; supernovae: general ; supernovae: individual (SN 2017cbv)</subject><ispartof>The Astrophysical journal, 2018-08, Vol.863 (1), p.24</ispartof><rights>2018. The American Astronomical Society. 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J.</creatorcontrib><creatorcontrib>Graham, M. L.</creatorcontrib><creatorcontrib>Botyánszki, J.</creatorcontrib><creatorcontrib>Hiramatsu, D.</creatorcontrib><creatorcontrib>McCully, C.</creatorcontrib><creatorcontrib>Valenti, S.</creatorcontrib><creatorcontrib>Hosseinzadeh, G.</creatorcontrib><creatorcontrib>Howell, D. A.</creatorcontrib><creatorcontrib>Burke, J.</creatorcontrib><creatorcontrib>Cartier, R.</creatorcontrib><creatorcontrib>Diamond, T.</creatorcontrib><creatorcontrib>Hsiao, E. Y.</creatorcontrib><creatorcontrib>Jha, S. W.</creatorcontrib><creatorcontrib>Kasen, D.</creatorcontrib><creatorcontrib>Kumar, S.</creatorcontrib><creatorcontrib>Marion, G. H.</creatorcontrib><creatorcontrib>Suntzeff, N.</creatorcontrib><creatorcontrib>Tartaglia, L.</creatorcontrib><creatorcontrib>Wheeler, J. C.</creatorcontrib><creatorcontrib>Wyatt, S.</creatorcontrib><title>Nebular Spectroscopy of the "Blue Bump" Type Ia Supernova 2017cbv</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>We present nebular phase optical and near-infrared spectroscopy of the Type Ia supernova (SN) 2017cbv. The early light curves of SN 2017cbv showed a prominent blue bump in the U, B, and g bands lasting for ∼5 days. One interpretation of the early light curve is that the excess blue light is due to shocking of the SN ejecta against a nondegenerate companion star-a signature of the single degenerate scenario. If this is the correct interpretation, the interaction between the SN ejecta and the companion star could result in significant H (or helium) emission at late times, possibly along with other species, depending on the companion star and its orbital separation. A search for H emission in our +302 d spectrum yields a nondetection, with a LH < 8.0 × 1035 erg s−1 (given an assumed distance of D = 12.3 Mpc), which we verified by implanting simulated H emission into our data. We make a quantitative comparison to models of swept-up material stripped from a nondegenerate companion star and limit the mass of hydrogen that might remain undetected to MH < 1 × 10−4 M . A similar analysis of helium star related lines yields a MHe < 5 × 10−4 M . Taken at face value, these results argue against a nondegenerate H- or He-rich companion in Roche lobe overflow as the progenitor of SN 2017cbv. Alternatively, there could be weaknesses in the envelope-stripping and radiative transfer models necessary to interpret the strong H and He flux limits.</description><subject>Astrophysics</subject><subject>Companion stars</subject><subject>Computer simulation</subject><subject>Ejecta</subject><subject>H alpha line</subject><subject>Helium</subject><subject>Hydrogen</subject><subject>Infrared spectra</subject><subject>Infrared spectroscopy</subject><subject>Light curve</subject><subject>Near infrared radiation</subject><subject>Near infrared spectroscopy</subject><subject>Overflow</subject><subject>Radiative transfer</subject><subject>Radiative transfer models</subject><subject>Spectrum analysis</subject><subject>Supernova</subject><subject>supernovae: general</subject><subject>supernovae: individual (SN 2017cbv)</subject><issn>0004-637X</issn><issn>1538-4357</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNp1kEtPwzAQhC0EEqVw52gVjoT6ldg5tuVVqYJDC-JmObEDqdra2ElR_z2Jglpx4LTa1bejmQHgEqNbKhgf4piKiNGYD5XKtRFHoLc_HYMeQohFCeXvp-AshGW7kjTtgdGzyeqV8nDuTF55G3LrdtAWsPo0cDBe1QaO67UbwMXOGThVcF474zd2qyBBmOfZ9hycFGoVzMXv7IPXh_vF5CmavTxOJ6NZlDNBqogTjVCccsxFWmQZwpnWORKxUoyxhKYppQgXcYY1LrhWSGsiksIwTDhWiiraBzedbvg2rs6k8-Va-Z20qpR35dtIWv8hQy1xgnCTvA-uOtx5-1WbUMmlrf2mcSgJTWJBRWO_oVBH5U304E2xl8VItr3KtkTZlii7XpuX6-6ltO6gqdxSioRKLAmTThcHu3-wf1V_AMryhDk</recordid><startdate>20180810</startdate><enddate>20180810</enddate><creator>Sand, D. J.</creator><creator>Graham, M. L.</creator><creator>Botyánszki, J.</creator><creator>Hiramatsu, D.</creator><creator>McCully, C.</creator><creator>Valenti, S.</creator><creator>Hosseinzadeh, G.</creator><creator>Howell, D. A.</creator><creator>Burke, J.</creator><creator>Cartier, R.</creator><creator>Diamond, T.</creator><creator>Hsiao, E. Y.</creator><creator>Jha, S. W.</creator><creator>Kasen, D.</creator><creator>Kumar, S.</creator><creator>Marion, G. H.</creator><creator>Suntzeff, N.</creator><creator>Tartaglia, L.</creator><creator>Wheeler, J. C.</creator><creator>Wyatt, S.</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>ADTPV</scope><scope>AOWAS</scope><scope>DG7</scope><orcidid>https://orcid.org/0000-0003-4102-380X</orcidid><orcidid>https://orcid.org/0000-0001-8818-0795</orcidid><orcidid>https://orcid.org/0000-0003-4253-656X</orcidid><orcidid>https://orcid.org/0000-0002-9154-3136</orcidid><orcidid>https://orcid.org/0000-0002-0805-1908</orcidid><orcidid>https://orcid.org/0000-0003-1039-2928</orcidid><orcidid>https://orcid.org/0000-0003-1349-6538</orcidid><orcidid>https://orcid.org/0000-0002-5719-1560</orcidid><orcidid>https://orcid.org/0000-0001-8738-6011</orcidid><orcidid>https://orcid.org/0000-0003-3433-1492</orcidid><orcidid>https://orcid.org/0000-0001-5807-7893</orcidid><orcidid>https://orcid.org/0000-0002-0832-2974</orcidid></search><sort><creationdate>20180810</creationdate><title>Nebular Spectroscopy of the "Blue Bump" Type Ia Supernova 2017cbv</title><author>Sand, D. J. ; Graham, M. L. ; Botyánszki, J. ; Hiramatsu, D. ; McCully, C. ; Valenti, S. ; Hosseinzadeh, G. ; Howell, D. A. ; Burke, J. ; Cartier, R. ; Diamond, T. ; Hsiao, E. Y. ; Jha, S. W. ; Kasen, D. ; Kumar, S. ; Marion, G. H. ; Suntzeff, N. ; Tartaglia, L. ; Wheeler, J. 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W.</au><au>Kasen, D.</au><au>Kumar, S.</au><au>Marion, G. H.</au><au>Suntzeff, N.</au><au>Tartaglia, L.</au><au>Wheeler, J. C.</au><au>Wyatt, S.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Nebular Spectroscopy of the "Blue Bump" Type Ia Supernova 2017cbv</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2018-08-10</date><risdate>2018</risdate><volume>863</volume><issue>1</issue><spage>24</spage><pages>24-</pages><issn>0004-637X</issn><issn>1538-4357</issn><eissn>1538-4357</eissn><abstract>We present nebular phase optical and near-infrared spectroscopy of the Type Ia supernova (SN) 2017cbv. The early light curves of SN 2017cbv showed a prominent blue bump in the U, B, and g bands lasting for ∼5 days. One interpretation of the early light curve is that the excess blue light is due to shocking of the SN ejecta against a nondegenerate companion star-a signature of the single degenerate scenario. If this is the correct interpretation, the interaction between the SN ejecta and the companion star could result in significant H (or helium) emission at late times, possibly along with other species, depending on the companion star and its orbital separation. A search for H emission in our +302 d spectrum yields a nondetection, with a LH < 8.0 × 1035 erg s−1 (given an assumed distance of D = 12.3 Mpc), which we verified by implanting simulated H emission into our data. We make a quantitative comparison to models of swept-up material stripped from a nondegenerate companion star and limit the mass of hydrogen that might remain undetected to MH < 1 × 10−4 M . A similar analysis of helium star related lines yields a MHe < 5 × 10−4 M . Taken at face value, these results argue against a nondegenerate H- or He-rich companion in Roche lobe overflow as the progenitor of SN 2017cbv. 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| subjects | Astrophysics Companion stars Computer simulation Ejecta H alpha line Helium Hydrogen Infrared spectra Infrared spectroscopy Light curve Near infrared radiation Near infrared spectroscopy Overflow Radiative transfer Radiative transfer models Spectrum analysis Supernova supernovae: general supernovae: individual (SN 2017cbv) |
| title | Nebular Spectroscopy of the "Blue Bump" Type Ia Supernova 2017cbv |
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