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dc.contributor.authorSand, D. J.
dc.contributor.authorAmaro, R. C.
dc.contributor.authorMoe, M.
dc.contributor.authorGraham, M. L.
dc.contributor.authorAndrews, J. E.
dc.contributor.authorBurke, J.
dc.contributor.authorCartier, R.
dc.contributor.authorEweis, Y.
dc.contributor.authorGalbany, L.
dc.contributor.authorHiramatsu, D.
dc.contributor.authorHowell, D. A.
dc.contributor.authorJha, S. W.
dc.contributor.authorLundquist, M.
dc.contributor.authorMatheson, T.
dc.contributor.authorMcCully, C.
dc.contributor.authorMilne, P.
dc.contributor.authorSMITH, NATHAN
dc.contributor.authorValenti, S.
dc.contributor.authorWyatt, S.
dc.date.accessioned2019-08-30T23:12:07Z
dc.date.available2019-08-30T23:12:07Z
dc.date.issued2019-05-20
dc.identifier.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.en_US
dc.identifier.issn2041-8205
dc.identifier.doi10.3847/2041-8213/ab1eaf
dc.identifier.urihttp://hdl.handle.net/10150/634042
dc.description.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.en_US
dc.description.sponsorshipKorea 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 Washingtonen_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.rights© 2019. The American Astronomical Society. All rights reserved.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectsupernovae: generalen_US
dc.titleNebular Hα Limits for Fast Declining SNe Iaen_US
dc.typeArticleen_US
dc.identifier.eissn2041-8213
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.identifier.journalASTROPHYSICAL JOURNAL LETTERSen_US
dc.description.collectioninformationThis 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 repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.volume877
dc.source.issue1
dc.source.beginpageL4
refterms.dateFOA2019-08-30T23:12:07Z


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