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dc.contributor.authorKochanek, CSen
dc.contributor.authorFraser, Morganen
dc.contributor.authorAdams, SMen
dc.contributor.authorSukhbold, Ten
dc.contributor.authorPrieto, JLen
dc.contributor.authorMuller, Ten
dc.contributor.authorBock, Gen
dc.contributor.authorBrown, JSen
dc.contributor.authorDong, Sen
dc.contributor.authorHoloien, TW-Sen
dc.contributor.authorKhan, Ren
dc.contributor.authorShappee, BJen
dc.contributor.authorStanek, KZen
dc.date.accessioned2017-04-21T09:11:05Z
dc.date.available2017-04-21T09:11:05Z
dc.date.issued2017-06-01en
dc.identifier.issn0035-8711
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/263741
dc.description.abstractWe identify a pre-explosion counterpart to the nearby Type IIP supernova ASASSN-16fq (SN 2016cok) in archival $\textit{Hubble Space Telescope}$ data. The source appears to be a blend of several stars that prevents obtaining accurate photometry. However, with reasonable assumptions about the stellar temperature and extinction, the progenitor almost certainly had an initial mass $M_*$ $\lesssim$ 17 M$_\odot$, and was most likely in the mass range of $M_*$ = 8–12 M$_\odot$. Observations once ASASSN-16fq has faded will have no difficulty accurately determining the properties of the progenitor. In 8 yr of Large Binocular Telescope (LBT) data, no significant progenitor variability is detected to rms limits of roughly 0.03 mag. Of the six nearby supernova (SN) with constraints on the low-level variability, SN 1987A, SN 1993J, SN 2008cn, SN 2011dh, SN 2013ej and ASASSN-16fq, only the slowly fading progenitor of SN 2011dh showed clear evidence of variability. Excluding SN 1987A, the 90 per cent confidence limit implied by these sources on the number of outbursts over the last decade before the SN that last longer than 0.1 yr (full width at half-maximum) and are brighter than $M_R$ < −8 mag is approximately $N_\text{out}$ $\lesssim$ 3. Our continuing LBT monitoring programme will steadily improve constraints on pre-SN progenitor variability at amplitudes far lower than achievable by SN surveys.
dc.description.sponsorshipCSK, KZS, JSB, SMA and TWSH are supported by NSF grants AST-1515876 and AST-1515927. BJS is supported by NASA through Hubble Fellowship grant HF-51348.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. TW-SH is supported by the DOE Computational Science Graduate Fellowship, grant number DE-FG02- 97ER25308. TS is partly supported by NSF grant PHY-1404311 to J. Beacom. This work was partly supported by the European Union FP7 programme through ERC grant number 320360. Support for JLP is provided in part by FONDECYT through the grant 1151445 and by the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. SD is supported by the Strategic Priority Research Program ‘The Emergence of Cosmological Structures’ of the Chinese Academy of Sciences (Grant No. XDB09000000) and NSFC project 11573003. Some of the observations were carried out using the LBT at Mt Graham, AZ. The LBT is an international collaboration among institutions in the United States, Italy and Germany. LBT Corporation partners are the University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max–Planck Society, the Astrophysical Institute Potsdam and Heidelberg University; the Ohio State University; and The Research Corporation, on behalf of the University of Notre Dame, University of Minnesota and University of Virginia. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA, and in part on observations made with the NASA/ESA HST obtained at the Space Telescope Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Some observations were obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA).
dc.language.isoenen
dc.publisherOxford University Press
dc.subjectstars: massiveen
dc.subjectsupernovae: generalen
dc.subjectsupernovae: individual: SN 2016coken
dc.subjectgalaxies: individual: M 66en
dc.titleSupernova progenitors, their variability and the Type IIP Supernova ASASSN-16fq in M66en
dc.typeArticle
prism.endingPage3360
prism.issueIdentifier3en
prism.publicationDate2017en
prism.publicationNameMonthly Notices of the Royal Astronomical Societyen
prism.startingPage3347
prism.volume467en
dc.identifier.doi10.17863/CAM.9107
dcterms.dateAccepted2017-01-31en
rioxxterms.versionofrecord10.1093/mnras/stx291en
rioxxterms.versionVoRen
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserveden
rioxxterms.licenseref.startdate2017-06-01en
dc.contributor.orcidFraser, Morgan [0000-0003-2191-1674]
dc.identifier.eissn1365-2966
dc.publisher.urlhttp://dx.doi.org/10.1093/mnras/stx291en
rioxxterms.typeJournal Article/Reviewen
cam.issuedOnline2017-02-24en
dc.identifier.urlhttp://dx.doi.org/10.1093/mnras/stx291en
cam.orpheus.successThu Jan 30 12:54:01 GMT 2020 - The item has an open VoR version.*
rioxxterms.freetoread.startdate2100-01-01


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