Optical and near-infrared observations of the nearby SN Ia 2017cbv

Lingzhi Wang; Carlos Contreras; Maokai Hu; Mario A. Hamuy; Eric Y. Hsiao; David J. Sand; Joseph P. Anderson; Chris Ashall; Christopher R. Burns; Juncheng Chen; Tiara R. Diamond; Scott Davis; Francisco Förster; Lluís Galbany; Santiago González-Gaitán; Mariusz Gromadzki; Peter Hoeflich; Wenxiong Li; G. H. Marion; Nidia Morrell; Giuliano Pignata; Jose L. Prieto; Mark M. Phillips; Melissa Shahbandeh; Nicholas B. Suntzeff; Stefano Valenti; Lifan Wang; Xiaofeng Wang; D. R. Young; Lixin Yu; Jujia Zhang

doi:10.3847/1538-4357/abba82

Optical and near-infrared observations of the nearby SN Ia 2017cbv

Lingzhi Wang, Carlos Contreras, Maokai Hu, Mario A. Hamuy, Eric Y. Hsiao, David J. Sand, Joseph P. Anderson, Chris Ashall, Christopher R. Burns, Juncheng Chen, Tiara R. Diamond, Scott Davis, Francisco Förster, Lluís Galbany, Santiago González-Gaitán, Mariusz Gromadzki, Peter Hoeflich, Wenxiong Li, G. H. Marion, Nidia MorrellGiuliano Pignata, Jose L. Prieto, Mark M. Phillips, Melissa Shahbandeh, Nicholas B. Suntzeff, Stefano Valenti, Lifan Wang, Xiaofeng Wang, D. R. Young, Lixin Yu, Jujia Zhang

Astronomy

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Abstract

Supernova (SN) 2017cbv in NGC 5643 is one of a handful of Type Ia supernovae (SNe Ia) reported to have excess blue emission at early times. This paper presents extensive BVRIYJHKs-band light curves of SN 2017cbv, covering the phase from -16 to +125 days relative to B-band maximum light. The SN 2017cbv reached a B-band maximum of 11.710 ± 0.006mag, with a postmaximum magnitude decline of Δm15(B) = 0.990 ± 0.013 mag. The SN suffered no host reddening based on Phillips intrinsic color, the Lira-Phillips relation, and the CMAGIC diagram. By employing the CMAGIC distance modulus μ = 30.58 ± 0.05 mag and assuming H0 = 72 km s-1 Mpc-1, we found that 0.73M⊙ 56Ni was synthesized during the explosion of SN 2017cbv, which is consistent with estimates using reddening- and distance-free methods via the phases of the secondary maximum of the near-IR- (NIR-) band light curves. We also present 14 NIR spectra from -18 to +49 days relative to the B-band maximum light, providing constraints on the amount of swept-up hydrogen from the companion star in the context of the single degenerate progenitor scenario. No Paβ emission feature was detected from our postmaximum NIR spectra, placing a hydrogen mass upper limit of 0.1 M⊙. The overall optical/NIR photometric and NIR spectral evolution of SN 2017cbv is similar to that of a normal SN Ia, even though its early evolution is marked by a flux excess not seen in most other wellobserved normal SNe Ia. We also compare the exquisite light curves of SN 2017cbv with some Mch delayed detonation models and sub-Mch double detonation models.

Original language	English (US)
Article number	abba82
Journal	Astrophysical Journal
Volume	904
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/abba82
State	Published - Nov 20 2020

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4357/abba82

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Wang, L., Contreras, C., Hu, M., Hamuy, M. A., Hsiao, E. Y., Sand, D. J., Anderson, J. P., Ashall, C., Burns, C. R., Chen, J., Diamond, T. R., Davis, S., Förster, F., Galbany, L., González-Gaitán, S., Gromadzki, M., Hoeflich, P., Li, W., Marion, G. H., ... Zhang, J. (2020). Optical and near-infrared observations of the nearby SN Ia 2017cbv. Astrophysical Journal, 904(1), Article abba82. https://doi.org/10.3847/1538-4357/abba82

Wang, L, Contreras, C, Hu, M, Hamuy, MA, Hsiao, EY, Sand, DJ, Anderson, JP, Ashall, C, Burns, CR, Chen, J, Diamond, TR, Davis, S, Förster, F, Galbany, L, González-Gaitán, S, Gromadzki, M, Hoeflich, P, Li, W, Marion, GH, Morrell, N, Pignata, G, Prieto, JL, Phillips, MM, Shahbandeh, M, Suntzeff, NB, Valenti, S, Wang, L, Wang, X, Young, DR, Yu, L & Zhang, J 2020, 'Optical and near-infrared observations of the nearby SN Ia 2017cbv', Astrophysical Journal, vol. 904, no. 1, abba82. https://doi.org/10.3847/1538-4357/abba82

@article{00b13374ad9f4d69b2ffd1992308e5f4,

title = "Optical and near-infrared observations of the nearby SN Ia 2017cbv",

abstract = "Supernova (SN) 2017cbv in NGC 5643 is one of a handful of Type Ia supernovae (SNe Ia) reported to have excess blue emission at early times. This paper presents extensive BVRIYJHKs-band light curves of SN 2017cbv, covering the phase from -16 to +125 days relative to B-band maximum light. The SN 2017cbv reached a B-band maximum of 11.710 ± 0.006mag, with a postmaximum magnitude decline of Δm15(B) = 0.990 ± 0.013 mag. The SN suffered no host reddening based on Phillips intrinsic color, the Lira-Phillips relation, and the CMAGIC diagram. By employing the CMAGIC distance modulus μ = 30.58 ± 0.05 mag and assuming H0 = 72 km s-1 Mpc-1, we found that 0.73M⊙ 56Ni was synthesized during the explosion of SN 2017cbv, which is consistent with estimates using reddening- and distance-free methods via the phases of the secondary maximum of the near-IR- (NIR-) band light curves. We also present 14 NIR spectra from -18 to +49 days relative to the B-band maximum light, providing constraints on the amount of swept-up hydrogen from the companion star in the context of the single degenerate progenitor scenario. No Paβ emission feature was detected from our postmaximum NIR spectra, placing a hydrogen mass upper limit of 0.1 M⊙. The overall optical/NIR photometric and NIR spectral evolution of SN 2017cbv is similar to that of a normal SN Ia, even though its early evolution is marked by a flux excess not seen in most other wellobserved normal SNe Ia. We also compare the exquisite light curves of SN 2017cbv with some Mch delayed detonation models and sub-Mch double detonation models.",

author = "Lingzhi Wang and Carlos Contreras and Maokai Hu and Hamuy, {Mario A.} and Hsiao, {Eric Y.} and Sand, {David J.} and Anderson, {Joseph P.} and Chris Ashall and Burns, {Christopher R.} and Juncheng Chen and Diamond, {Tiara R.} and Scott Davis and Francisco F{\"o}rster and Llu{\'i}s Galbany and Santiago Gonz{\'a}lez-Gait{\'a}n and Mariusz Gromadzki and Peter Hoeflich and Wenxiong Li and Marion, {G. H.} and Nidia Morrell and Giuliano Pignata and Prieto, {Jose L.} and Phillips, {Mark M.} and Melissa Shahbandeh and Suntzeff, {Nicholas B.} and Stefano Valenti and Lifan Wang and Xiaofeng Wang and Young, {D. R.} and Lixin Yu and Jujia Zhang",

note = "Publisher Copyright: {\textcopyright} 2020. The American Astronomical Society.",

year = "2020",

month = nov,

day = "20",

doi = "10.3847/1538-4357/abba82",

language = "English (US)",

volume = "904",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1",

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TY - JOUR

T1 - Optical and near-infrared observations of the nearby SN Ia 2017cbv

AU - Wang, Lingzhi

AU - Contreras, Carlos

AU - Hu, Maokai

AU - Hamuy, Mario A.

AU - Hsiao, Eric Y.

AU - Sand, David J.

AU - Anderson, Joseph P.

AU - Ashall, Chris

AU - Burns, Christopher R.

AU - Chen, Juncheng

AU - Diamond, Tiara R.

AU - Davis, Scott

AU - Förster, Francisco

AU - Galbany, Lluís

AU - González-Gaitán, Santiago

AU - Gromadzki, Mariusz

AU - Hoeflich, Peter

AU - Li, Wenxiong

AU - Marion, G. H.

AU - Morrell, Nidia

AU - Pignata, Giuliano

AU - Prieto, Jose L.

AU - Phillips, Mark M.

AU - Shahbandeh, Melissa

AU - Suntzeff, Nicholas B.

AU - Valenti, Stefano

AU - Wang, Lifan

AU - Wang, Xiaofeng

AU - Young, D. R.

AU - Yu, Lixin

AU - Zhang, Jujia

PY - 2020/11/20

Y1 - 2020/11/20

N2 - Supernova (SN) 2017cbv in NGC 5643 is one of a handful of Type Ia supernovae (SNe Ia) reported to have excess blue emission at early times. This paper presents extensive BVRIYJHKs-band light curves of SN 2017cbv, covering the phase from -16 to +125 days relative to B-band maximum light. The SN 2017cbv reached a B-band maximum of 11.710 ± 0.006mag, with a postmaximum magnitude decline of Δm15(B) = 0.990 ± 0.013 mag. The SN suffered no host reddening based on Phillips intrinsic color, the Lira-Phillips relation, and the CMAGIC diagram. By employing the CMAGIC distance modulus μ = 30.58 ± 0.05 mag and assuming H0 = 72 km s-1 Mpc-1, we found that 0.73M⊙ 56Ni was synthesized during the explosion of SN 2017cbv, which is consistent with estimates using reddening- and distance-free methods via the phases of the secondary maximum of the near-IR- (NIR-) band light curves. We also present 14 NIR spectra from -18 to +49 days relative to the B-band maximum light, providing constraints on the amount of swept-up hydrogen from the companion star in the context of the single degenerate progenitor scenario. No Paβ emission feature was detected from our postmaximum NIR spectra, placing a hydrogen mass upper limit of 0.1 M⊙. The overall optical/NIR photometric and NIR spectral evolution of SN 2017cbv is similar to that of a normal SN Ia, even though its early evolution is marked by a flux excess not seen in most other wellobserved normal SNe Ia. We also compare the exquisite light curves of SN 2017cbv with some Mch delayed detonation models and sub-Mch double detonation models.

AB - Supernova (SN) 2017cbv in NGC 5643 is one of a handful of Type Ia supernovae (SNe Ia) reported to have excess blue emission at early times. This paper presents extensive BVRIYJHKs-band light curves of SN 2017cbv, covering the phase from -16 to +125 days relative to B-band maximum light. The SN 2017cbv reached a B-band maximum of 11.710 ± 0.006mag, with a postmaximum magnitude decline of Δm15(B) = 0.990 ± 0.013 mag. The SN suffered no host reddening based on Phillips intrinsic color, the Lira-Phillips relation, and the CMAGIC diagram. By employing the CMAGIC distance modulus μ = 30.58 ± 0.05 mag and assuming H0 = 72 km s-1 Mpc-1, we found that 0.73M⊙ 56Ni was synthesized during the explosion of SN 2017cbv, which is consistent with estimates using reddening- and distance-free methods via the phases of the secondary maximum of the near-IR- (NIR-) band light curves. We also present 14 NIR spectra from -18 to +49 days relative to the B-band maximum light, providing constraints on the amount of swept-up hydrogen from the companion star in the context of the single degenerate progenitor scenario. No Paβ emission feature was detected from our postmaximum NIR spectra, placing a hydrogen mass upper limit of 0.1 M⊙. The overall optical/NIR photometric and NIR spectral evolution of SN 2017cbv is similar to that of a normal SN Ia, even though its early evolution is marked by a flux excess not seen in most other wellobserved normal SNe Ia. We also compare the exquisite light curves of SN 2017cbv with some Mch delayed detonation models and sub-Mch double detonation models.

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U2 - 10.3847/1538-4357/abba82

DO - 10.3847/1538-4357/abba82

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JO - Astrophysical Journal

JF - Astrophysical Journal

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ER -

Optical and near-infrared observations of the nearby SN Ia 2017cbv

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Optical and near-infrared observations of the nearby SN Ia 2017cbv

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