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dc.creatorCrockett, R. Marken_US
dc.creatorMaund, Justyn R.en_US
dc.creatorSmartt, Steven J.en_US
dc.creatorMattila, Seppoen_US
dc.creatorPastorello, Andreaen_US
dc.creatorSmoker, Jonathanen_US
dc.creatorStephens, Andrew W.en_US
dc.creatorFynbo, Johanen_US
dc.creatorEldridge, John J.en_US
dc.creatorDanziger, I. Johnen_US
dc.creatorBenn, Christopher R.en_US
dc.date.accessioned2016-10-28T19:34:48Z
dc.date.available2016-10-28T19:34:48Z
dc.date.issued2008-01en_US
dc.identifierdoi:10.15781/T2804XN4P
dc.identifier.citationCrockett, R. Mark, Justyn R. Maund, Stephen J. Smartt, Seppo Mattila, Andrea Pastorello, Jonathan Smoker, Andrew W. Stephens et al. "The birth place of the type Ic supernova 2007gr." The Astrophysical Journal Letters, Vol. 672, No. 2 (Jan., 2008): L99.en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/2152/42942
dc.description.abstractWe report our attempts to locate the progenitor of the peculiar Type Ic SN 2007gr in Hubble Space Telescope (HST) preexplosion images of the host galaxy, NGC 1058. Aligning adaptive optics Altair/NIRI imaging of SN 2007gr from the Gemini ( North) Telescope with the preexplosion HST WFPC2 images, we identify the supernova (SN) position on the HST frames with an accuracy of 20 mas. Although nothing is detected at the SN position, we show that it lies on the edge of a bright source 134 +/- 23 mas (6.9 pc) from its nominal center. On the basis of its luminosity, we suggest that this object is possibly an unresolved, compact, and coeval cluster and that the SN progenitor was a cluster member, although we note that model profile fitting favors a single bright star. We find two solutions for the age of this assumed cluster: 7 -/+ 0.5 Myr and 20 - 30 Myr, with turnoff masses of 28 +/- M(circle dot) and 12 - 9 M(circle dot), respectively. Preexplosion ground-based K- band images marginally favor the younger cluster 4 age/higher turnoff mass. Assuming the SN progenitor was a cluster member, the turnoff mass provides the best estimate for its initial mass. More detailed observations, after the SN has faded, should determine whether the progenitor was indeed part of a cluster and, if so, allow an age estimate to within similar to 2 Myr, thereby favoring either a high-mass single star or lower-mass interacting binary progenitor.en_US
dc.description.sponsorshipEURYIen_US
dc.description.sponsorshipESFen_US
dc.description.sponsorshipNSF/NASA AST04-06740/NNG 04GL00en_US
dc.description.sponsorshipAcademy of Finland project 8120503en_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.subjectgalaxies : individual (ngc 1058)en_US
dc.subjectstars : evolutionen_US
dc.subjectsupernovae :en_US
dc.subjectgeneralen_US
dc.subjectsupernovae : individual (2007gr)en_US
dc.subjectred supergiant progenitoren_US
dc.subjectcore-collapse supernovaeen_US
dc.subjectimage subtractionen_US
dc.subjectnearby galaxiesen_US
dc.subjectstar-Formationen_US
dc.subjectclustersen_US
dc.subjectspectroscopyen_US
dc.subjectsearchen_US
dc.subject2004djen_US
dc.subject2005csen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleThe Birth Place of the Type Ic Supernova 2007Gren_US
dc.typeArticleen_US
dc.description.departmentAstronomyen_US
dc.rights.restrictionOpenen_US
dc.identifier.doi10.1086/527299en_US
dc.contributor.utaustinauthorDanziger, I. Johnen_US
dc.relation.ispartofserialAstrophysical Journal Lettersen_US


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