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dc.creatorSilverman, Jeffrey M.en_US
dc.creatorNugent, Peter E.en_US
dc.creatorGal-Yam, Avishayen_US
dc.creatorSullivan, Marken_US
dc.creatorHowell, D. Andrewen_US
dc.creatorFilippenko, Alexei V.en_US
dc.creatorPan, Yen-Chenen_US
dc.creatorCenko, S. Bradleyen_US
dc.creatorHook, Isobel M.en_US
dc.date.accessioned2016-04-28T19:36:21Z
dc.date.available2016-04-28T19:36:21Z
dc.date.issued2013-08en
dc.identifierdoi:10.15781/T2PZ32
dc.identifier.citationSilverman, Jeffrey M., Peter E. Nugent, Avishay Gal-Yam, Mark Sullivan, D. Andrew Howell, Alexei V. Filippenko, Yen-Chen Pan, S. Bradley Cenko, and Isobel M. Hook. "Late-time Spectral Observations of the Strongly Interacting Type Ia Supernova PTF11kx." The Astrophysical Journal, Vol. 772, No. 2 (Aug., 2013): 125.en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/34883
dc.description.abstractPTF11kx was a Type Ia supernova (SN Ia) that showed time-variable absorption features, including saturated Ca II H and K lines that weakened and eventually went into emission. The strength of the emission component of H alpha gradually increased, implying that the SN was undergoing significant interaction with its circumstellar medium (CSM). These features, and many others, were blueshifted slightly and showed a P-Cygni profile, likely indicating that the CSM was directly related to, and probably previously ejected by, the progenitor system itself. These and other observations led Dilday et al. to conclude that PTF11kx came from a symbiotic nova progenitor like RS Oph. In this work we extend the spectral coverage of PTF11kx to 124-680 rest-frame days past maximum brightness. The late-time spectra of PTF11kx are dominated by Ha emission (with widths of full width at half-maximum intensity approximate to 2000 km s(-1)), strong Ca II emission features (similar to 10,000 km s(-1) wide), and a blue "quasi-continuum" due to many overlapping narrow lines of Fe II. Emission from oxygen, He I, and Balmer lines higher than Ha is weak or completely absent at all epochs, leading to large observed H alpha/H beta intensity ratios. The H alpha emission appears to increase in strength with time for similar to 1 yr, but it subsequently decreases significantly along with the Ca II emission. Our latest spectrum also indicates the possibility of newly formed dust in the system as evidenced by a slight decrease in the red wing of H alpha. During the same epochs, multiple narrow emission features from the CSM temporally vary in strength. The weakening of the H alpha and Ca II emission at late times is possible evidence that the SN ejecta have overtaken the majority of the CSM and agrees with models of other strongly interacting SNe Ia. The varying narrow emission features, on the other hand, may indicate that the CSM is clumpy or consists of multiple thin shells.en_US
dc.description.sponsorshipW. M. Keck Foundationen_US
dc.description.sponsorshipNASAen_US
dc.description.sponsorshipAlfred P. Sloan Foundationen_US
dc.description.sponsorshipNational Science Foundation (NSF)en_US
dc.description.sponsorshipU.S. Department of Energy Office of Scienceen_US
dc.description.sponsorshipRichard and Rhoda Goldman Funden_US
dc.description.sponsorshipChristopher R. Redlich Funden_US
dc.description.sponsorshipTABASGO Foundationen_US
dc.description.sponsorshipNSF AST-0908886, AST-1211916en_US
dc.description.sponsorshipISFen_US
dc.description.sponsorshipBSFen_US
dc.description.sponsorshipGIFen_US
dc.description.sponsorshipMinerva, an FP7/ERC granten_US
dc.description.sponsorshipHelen and Martin Kimmel Award for Innovative Investigationen_US
dc.description.sponsorshipRoyal Societyen_US
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectcircumstellar matteren_US
dc.subjectsupernovae: generalen_US
dc.subjectsupernovae: individualen_US
dc.subject(ptf11kx)en_US
dc.subjectdark-energy constraintsen_US
dc.subjectwhite-dwarf staren_US
dc.subjectiin supernovaen_US
dc.subjectcircumstellaren_US
dc.subjectinteractionen_US
dc.subjectsodium-absorptionen_US
dc.subjectlegacy surveyen_US
dc.subjectsn 2011feen_US
dc.subjectprogenitoren_US
dc.subject2009dcen_US
dc.subject2010jlen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleLate-Time Spectral Observations Of The Strongly Interacting Type Ia Supernova PTF11Kxen_US
dc.typeArticleen_US
dc.description.departmentAstronomyen_US
dc.identifier.Filename2013_08_latetimespectral.pdfen_US
dc.rights.restrictionOpenen_US
dc.identifier.doi10.1088/0004-637x/772/2/125en_US
dc.contributor.utaustinauthorSilverman, Jeffrey M.en_US
dc.relation.ispartofserialAstrophysical Journalen_US


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