You are here

Nebular Spectroscopy Of The "blue Bump" Type Ia Supernova 2017cbv

Title: Nebular Spectroscopy Of The "blue Bump" Type Ia Supernova 2017cbv.
Name(s): Sand, D. J., author
Graham, M. L., author
Botyanszki, J., author
Hiramatsu, D., author
McCully, C., author
Valenti, S., author
Hosseinzadeh, G., author
Howell, D. A., author
Burke, J., author
Cartier, R., author
Diamond, T., author
Hsiao, E. Y., author
Jha, S. W., author
Kasen, D., author
Kumar, S., author
Marion, G. H., author
Suntzeff, N., author
Tartaglia, L., author
Wheeler, J. C., author
Wyatt, S., author
Type of Resource: text
Genre: Journal Article
Journal Article
Date Issued: 2018-08-10
Physical Form: computer
online resource
Extent: 1 online resource
Language(s): English
Abstract/Description: We present nebular phase optical and near-infrared spectroscopy of the Type Ia supernova (SN) 2017cbv. The early light curves of SN 2017cbv showed a prominent blue bump in the U, B, and g bands lasting for similar to 5 days. One interpretation of the early light curve is that the excess blue light is due to shocking of the SN ejecta against a nondegenerate companion star-a signature of the single degenerate scenario. If this is the correct interpretation, the interaction between the SN ejecta and the companion star could result in significant Ha (or helium) emission at late times, possibly along with other species, depending on the companion star and its orbital separation. A search for Ha emission in our +302 d spectrum yields a nondetection, with a L-H alpha < 8.0 x 10(35) erg s(-1) (given an assumed distance of D = 12.3 Mpc), which we verified by implanting simulated Ha emission into our data. We make a quantitative comparison to models of swept-up material stripped from a nondegenerate companion star and limit the mass of hydrogen that might remain undetected to M-H < 1 x 10(-4) M-circle dot. A similar analysis of helium star related lines yields a M-He < 5 x 10(-4) M-circle dot. Taken at face value, these results argue against a nondegenerate H- or He-rich companion in Roche lobe overflow as the progenitor of SN 2017cbv. Alternatively, there could be weaknesses in the envelope-stripping and radiative transfer models necessary to interpret the strong H and He flux limits.
Identifier: FSU_libsubv1_wos_000441126000010 (IID), 10.3847/1538-4357/aacde8 (DOI)
Keywords: hydrogen, spectra, impact, supernovae: general, helium, star, companion, supernovae: individual (SN 2017cbv), progenitor, ejecta, binaries, main-sequence
Publication Note: The publisher’s version of record is available at
Persistent Link to This Record:
Host Institution: FSU
Is Part Of: Astrophysical Journal.
Issue: iss. 1, vol. 863

Choose the citation style.
Sand, D. J., Graham, M. L., Botyanszki, J., Hiramatsu, D., McCully, C., Valenti, S., … Wyatt, S. (2018). Nebular Spectroscopy Of The "blue Bump" Type Ia Supernova 2017cbv. Astrophysical Journal. Retrieved from