AuthorSand, D. J.
Amaro, R. C.
Graham, M. L.
Andrews, J. E.
Howell, D. A.
Jha, S. W.
AffiliationUniv Arizona, Steward Observ
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationSand, D. J., Amaro, R. C., Moe, M., Graham, M. L., Andrews, J. E., Burke, J., ... & Howell, D. A. (2019). Nebular Hα Limits for Fast Declining SNe Ia. The Astrophysical Journal Letters, 877(1), L4.
JournalASTROPHYSICAL JOURNAL LETTERS
Rights© 2019. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractOne clear observational prediction of the single-degenerate progenitor scenario as the origin of type Ia supernovae (SNe) is the presence of relatively narrow (approximate to 1000 km s(-1)) H alpha emission at nebular phases, although this feature is rarely seen. We present a compilation of nebular phase H alpha limits for SN Ia in the literature and demonstrate that this heterogenous sample has been biased toward SN Ia with relatively high luminosities and slow decline rates, as parameterized by Delta m(15)(B), the difference in B-band magnitude between maximum light and 15 days afterward. Motivated by the need to explore the full parameter space of SN Ia and their subtypes, we present two new and six previously published nebular spectra of SN Ia with Delta m(15)(B) > 1.3 mag (including members of the transitional and SN1991bg-like subclasses) and measure nondetection limits of L-H alpha < 0.85-9.9 x 10(36) erg s(-1), which we confirmed by implanting simulated H alpha emission into our data. Based on the latest models of swept-up material stripped from a nondegenerate companion star, these L-H alpha values correspond to hydrogen mass limits of M-H less than or similar to 1-3 x 10(-4) M-circle dot, which are roughly three orders of magnitude below that expected for the systems modeled, although we note that no simulations of H alpha nebular emission in such weak explosions have yet been performed. Despite the recent detection of strong H alpha in ASASSN-18tb (SN 2018fhw; Delta m(15)(B) = 2.0 mag), we see no evidence that fast-declining systems are more likely to have late time H alpha emission, although a larger sample is needed to confirm this result.
VersionFinal published version
SponsorsKorea Astronomy and Space Science Institute (Republic of Korea) [GN-2008A-Q-17, GS-2018A-Q-315]; NSF [AST-1615455, AST-1821987, 1821967, AST-1515559]; NASA grant [ADAP-80NSSC19K0578]; DIRAC Institute in the Department of Astronomy at the University of Washington