Optical and Near-infrared Observations of the Nearby SN Ia 2017cbv
| Autor: | Scott C. Davis, Lixin Yu, Christopher R. Burns, T. R. Diamond, G. H. Marion, Xiaofeng Wang, Lingzhi Wang, Lifan Wang, David J. Sand, Giuliano Pignata, Joseph P. Anderson, Peter Hoeflich, Stefano Valenti, Lluís Galbany, F. Forster, Nidia Morrell, Carlos Contreras, J. L. Prieto, D. R. Young, Wenxiong Li, Melissa Shahbandeh, Mario Hamuy, Maokai Hu, Mark M. Phillips, Eric Hsiao, Mariusz Gromadzki, Juncheng Chen, Santiago González-Gaitán, Nicholas B. Suntzeff, Chris Ashall, Jujia Zhang |
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| Rok vydání: | 2020 |
| Předmět: |
Physics
010308 nuclear & particles physics Near-infrared spectroscopy Flux Astronomy and Astrophysics Context (language use) Astrophysics Type (model theory) Light curve 01 natural sciences Spectral line Supernova Distance modulus Space and Planetary Science 0103 physical sciences 010303 astronomy & astrophysics |
| Zdroj: | The Astrophysical Journal |
| ISSN: | 1538-4357 |
| DOI: | 10.3847/1538-4357/abba82 |
| Popis: | 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 $BVRIYJHK_s$-band light curves of SN 2017cbv, covering the phase from $-16$ to $+125$ days relative to $B$-band maximum light. SN 2017cbv reached a $B$-band maximum of 11.710$\pm$0.006~mag, with a post-maximum magnitude decline $\Delta m_{15}(B)$=0.990$\pm$0.013 mag. The supernova suffered no host reddening based on Phillips intrinsic color, Lira-Phillips relation, and the CMAGIC diagram. By employing the CMAGIC distance modulus $\mu=30.58\pm0.05$~mag and assuming $H_0$=72~$\rm km \ s^{-1} \ Mpc^{-1}$, we found that 0.73~\msun $^{56}$Ni was synthesized during the explosion of SN 2017cbv, which is consistent with estimates using reddening-free and distance-free methods via the phases of the secondary maximum of the NIR-band light curves. We also present 14 near-infrared 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 $Pa{\beta}$ emission feature was detected from our post-maximum NIR spectra, placing a hydrogen mass upper limit of 0.1 $M_{\odot}$. 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 no seen in most other well-observed normal SNe~Ia. We also compare the exquisite light curves of SN 2017cbv with some $M_{ch}$ DDT models and sub-$M_{ch}$ double detonation models. |
| Databáze: | OpenAIRE |
| Externí odkaz: |
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