Optical and Near-Infrared Observations of the Nearby Type Ia Supernova 2017cbv

Autor: 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, Valenti, Stefano, Wang, Lifan, Wang, Xiaofeng, Young, D. R., Yu, Lixin, Zhang, Jujia
Rok vydání: 2020
Předmět:
Druh dokumentu: Working Paper
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.
Comment: 20 figures, Accepted for publication in The Astrophysical Journal
Databáze: arXiv
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