Early Blue Excess from the Type Ia Supernova 2017cbv and Implications for Its Progenitor
We present very early, high-cadence photometric observations of the nearby Type Ia SN 2017cbv. The light curve is unique in that it has a blue bump during the first five days of observations in the U, B, and g bands, which is clearly resolved given our photometric cadence of 5.7 hr during that time...
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| Published in | Astrophysical journal. Letters Vol. 845; no. 2; p. L11 |
|---|---|
| Main Authors | , , , , , , , , , , , , , |
| Format | Journal Article |
| Language | English |
| Published |
Austin
The American Astronomical Society
20.08.2017
IOP Publishing |
| Subjects | |
| Online Access | Get full text |
| ISSN | 2041-8205 2041-8213 |
| DOI | 10.3847/2041-8213/aa8402 |
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| Abstract | We present very early, high-cadence photometric observations of the nearby Type Ia SN 2017cbv. The light curve is unique in that it has a blue bump during the first five days of observations in the U, B, and g bands, which is clearly resolved given our photometric cadence of 5.7 hr during that time span. We model the light curve as the combination of early shocking of the supernova ejecta against a nondegenerate companion star plus a standard SN Ia component. Our best-fit model suggests the presence of a subgiant star 56 R☉ from the exploding white dwarf, although this number is highly model-dependent. While this model matches the optical light curve well, it overpredicts the observed flux in the ultraviolet bands. This may indicate that the shock is not a blackbody, perhaps because of line blanketing in the UV. Alternatively, it could point to another physical explanation for the optical blue bump, such as interaction with circumstellar material or an unusual nickel distribution. Early optical spectra of SN 2017cbv show strong carbon (C ii λ6580) absorption up through day −13 with respect to maximum light, suggesting that the progenitor system contains a significant amount of unburned material. These early results on SN 2017cbv illustrate the power of early discovery and intense follow-up of nearby supernovae to resolve standing questions about the progenitor systems and explosion mechanisms of SNe Ia. |
|---|---|
| AbstractList | We present very early, high-cadence photometric observations of the nearby Type Ia SN 2017cbv. The light curve is unique in that it has a blue bump during the first five days of observations in the U , B , and g bands, which is clearly resolved given our photometric cadence of 5.7 hr during that time span. We model the light curve as the combination of early shocking of the supernova ejecta against a nondegenerate companion star plus a standard SN Ia component. Our best-fit model suggests the presence of a subgiant star 56 R {sub ☉} from the exploding white dwarf, although this number is highly model-dependent. While this model matches the optical light curve well, it overpredicts the observed flux in the ultraviolet bands. This may indicate that the shock is not a blackbody, perhaps because of line blanketing in the UV. Alternatively, it could point to another physical explanation for the optical blue bump, such as interaction with circumstellar material or an unusual nickel distribution. Early optical spectra of SN 2017cbv show strong carbon (C ii λ 6580) absorption up through day −13 with respect to maximum light, suggesting that the progenitor system contains a significant amount of unburned material. These early results on SN 2017cbv illustrate the power of early discovery and intense follow-up of nearby supernovae to resolve standing questions about the progenitor systems and explosion mechanisms of SNe Ia. We present very early, high-cadence photometric observations of the nearby Type Ia SN 2017cbv. The light curve is unique in that it has a blue bump during the first five days of observations in the U , B , and g bands, which is clearly resolved given our photometric cadence of 5.7 hr during that time span. We model the light curve as the combination of early shocking of the supernova ejecta against a nondegenerate companion star plus a standard SN Ia component. Our best-fit model suggests the presence of a subgiant star 56 R ☉ from the exploding white dwarf, although this number is highly model-dependent. While this model matches the optical light curve well, it overpredicts the observed flux in the ultraviolet bands. This may indicate that the shock is not a blackbody, perhaps because of line blanketing in the UV. Alternatively, it could point to another physical explanation for the optical blue bump, such as interaction with circumstellar material or an unusual nickel distribution. Early optical spectra of SN 2017cbv show strong carbon (C ii λ 6580) absorption up through day −13 with respect to maximum light, suggesting that the progenitor system contains a significant amount of unburned material. These early results on SN 2017cbv illustrate the power of early discovery and intense follow-up of nearby supernovae to resolve standing questions about the progenitor systems and explosion mechanisms of SNe Ia. We present very early, high-cadence photometric observations of the nearby Type Ia SN 2017cbv. The light curve is unique in that it has a blue bump during the first five days of observations in the U, B, and g bands, which is clearly resolved given our photometric cadence of 5.7 hr during that time span. We model the light curve as the combination of early shocking of the supernova ejecta against a nondegenerate companion star plus a standard SN Ia component. Our best-fit model suggests the presence of a subgiant star 56 R ☉ from the exploding white dwarf, although this number is highly model-dependent. While this model matches the optical light curve well, it overpredicts the observed flux in the ultraviolet bands. This may indicate that the shock is not a blackbody, perhaps because of line blanketing in the UV. Alternatively, it could point to another physical explanation for the optical blue bump, such as interaction with circumstellar material or an unusual nickel distribution. Early optical spectra of SN 2017cbv show strong carbon (C ii λ6580) absorption up through day −13 with respect to maximum light, suggesting that the progenitor system contains a significant amount of unburned material. These early results on SN 2017cbv illustrate the power of early discovery and intense follow-up of nearby supernovae to resolve standing questions about the progenitor systems and explosion mechanisms of SNe Ia. We present very early, high-cadence photometric observations of the nearby Type Ia SN 2017cbv. The light curve is unique in that it has a blue bump during the first five days of observations in the U, B, and g bands, which is clearly resolved given our photometric cadence of 5.7 hr during that time span. We model the light curve as the combination of early shocking of the supernova ejecta against a nondegenerate companion star plus a standard SN Ia component. Our best-fit model suggests the presence of a subgiant star 56 R☉ from the exploding white dwarf, although this number is highly model-dependent. While this model matches the optical light curve well, it overpredicts the observed flux in the ultraviolet bands. This may indicate that the shock is not a blackbody, perhaps because of line blanketing in the UV. Alternatively, it could point to another physical explanation for the optical blue bump, such as interaction with circumstellar material or an unusual nickel distribution. Early optical spectra of SN 2017cbv show strong carbon (C ii λ6580) absorption up through day −13 with respect to maximum light, suggesting that the progenitor system contains a significant amount of unburned material. These early results on SN 2017cbv illustrate the power of early discovery and intense follow-up of nearby supernovae to resolve standing questions about the progenitor systems and explosion mechanisms of SNe Ia. |
| Author | Hosseinzadeh, Griffin Hsiao, Eric Y. Kasen, Daniel McCully, Curtis Stritzinger, Maximilian D. Sand, David J. Arcavi, Iair Tartaglia, Leonardo Davis, Scott Brown, Peter Shahbandeh, Melissa Valenti, Stefano Howell, D. Andrew Bostroem, K. Azalee |
| Author_xml | – sequence: 1 givenname: Griffin orcidid: 0000-0002-0832-2974 surname: Hosseinzadeh fullname: Hosseinzadeh, Griffin email: griffin@lco.global organization: University of California Department of Physics, Santa Barbara, CA 93106-9530, USA – sequence: 2 givenname: David J. orcidid: 0000-0003-4102-380X surname: Sand fullname: Sand, David J. organization: Texas Tech University Department of Physics & Astronomy, Box 41051, Lubbock, TX 79109-1051, USA – sequence: 3 givenname: Stefano orcidid: 0000-0001-8818-0795 surname: Valenti fullname: Valenti, Stefano organization: University of California Department of Physics, 1 Shields Avenue, Davis, CA 95616-5270, USA – sequence: 4 givenname: Peter orcidid: 0000-0001-6272-5507 surname: Brown fullname: Brown, Peter organization: Texas A&M University Mitchell Institute for Fundamental Physics and Astronomy, College Station, TX 77843-4242, USA – sequence: 5 givenname: D. Andrew orcidid: 0000-0003-4253-656X surname: Howell fullname: Howell, D. Andrew organization: University of California Department of Physics, Santa Barbara, CA 93106-9530, USA – sequence: 6 givenname: Curtis orcidid: 0000-0001-5807-7893 surname: McCully fullname: McCully, Curtis organization: University of California Department of Physics, Santa Barbara, CA 93106-9530, USA – sequence: 7 givenname: Daniel orcidid: 0000-0002-5981-1022 surname: Kasen fullname: Kasen, Daniel organization: University of California Departments of Physics and Astronomy, Berkeley, CA 94720-7300, USA – sequence: 8 givenname: Iair orcidid: 0000-0001-7090-4898 surname: Arcavi fullname: Arcavi, Iair organization: University of California Department of Physics, Santa Barbara, CA 93106-9530, USA – sequence: 9 givenname: K. Azalee orcidid: 0000-0002-4924-444X surname: Bostroem fullname: Bostroem, K. Azalee organization: University of California Department of Physics, 1 Shields Avenue, Davis, CA 95616-5270, USA – sequence: 10 givenname: Leonardo orcidid: 0000-0003-3433-1492 surname: Tartaglia fullname: Tartaglia, Leonardo organization: University of California Department of Physics, 1 Shields Avenue, Davis, CA 95616-5270, USA – sequence: 11 givenname: Eric Y. orcidid: 0000-0003-1039-2928 surname: Hsiao fullname: Hsiao, Eric Y. organization: Florida State University Department of Physics, 77 Chieftain Way, Tallahassee, FL 32306-4350, USA – sequence: 12 givenname: Scott surname: Davis fullname: Davis, Scott organization: Florida State University Department of Physics, 77 Chieftain Way, Tallahassee, FL 32306-4350, USA – sequence: 13 givenname: Melissa surname: Shahbandeh fullname: Shahbandeh, Melissa organization: Florida State University Department of Physics, 77 Chieftain Way, Tallahassee, FL 32306-4350, USA – sequence: 14 givenname: Maximilian D. orcidid: 0000-0002-5571-1833 surname: Stritzinger fullname: Stritzinger, Maximilian D. organization: Aarhus University Department of Physics and Astronomy, Ny Munkegade 120, DK-8000 Aarhus C, Denmark |
| BackLink | https://www.osti.gov/biblio/22654411$$D View this record in Osti.gov |
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| Copyright | 2017. The American Astronomical Society. All rights reserved. Copyright IOP Publishing Aug 20, 2017 |
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| Snippet | We present very early, high-cadence photometric observations of the nearby Type Ia SN 2017cbv. The light curve is unique in that it has a blue bump during the... |
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| SubjectTerms | ABSORPTION ASTROPHYSICS, COSMOLOGY AND ASTRONOMY Blackbody Blanketing CARBON Companion stars DISTRIBUTION Ejecta EXPLOSIONS INTERACTIONS Light curve NICKEL Photometric observations Photometry SPECTRA Subgiant stars Supernova SUPERNOVAE supernovae: general supernovae: individual (SN 2017cbv) ULTRAVIOLET RADIATION VISIBLE RADIATION WHITE DWARF STARS |
| Title | Early Blue Excess from the Type Ia Supernova 2017cbv and Implications for Its Progenitor |
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