Optical and Near-infrared Observations of the Nearby SN Ia 2017cbv

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 2017c...

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Veröffentlicht in:The Astrophysical journal 2020-11, Vol.904 (1), p.14
Hauptverfasser: Wang, Lingzhi, Contreras, Carlos, Hu, Maokai, Hamuy, Mario A., Hsiao, Eric Y., Sand, David J., Anderson, Joseph P., Ashall, Chris, Burns, Christopher R., Chen, Juncheng, Diamond, Tiara R., Davis, Scott, Förster, Francisco, Galbany, Lluís, González-Gaitán, Santiago, Gromadzki, Mariusz, Hoeflich, Peter, Li, Wenxiong, Marion, G. H., Morrell, Nidia, Pignata, Giuliano, Prieto, Jose L., Phillips, Mark M., Shahbandeh, Melissa, Suntzeff, Nicholas B., Valenti, Stefano, Wang, Lifan, Wang, Xiaofeng, Young, D. R., Yu, Lixin, Zhang, Jujia
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Sprache:eng
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Zusammenfassung: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 0.006 mag, 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 = 30.58 0.05 mag and assuming H0 = 72 km s−1 Mpc−1, we found that 0.73 M 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 well-observed 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.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/abba82