Home > Publications database > Search for Precursor Eruptions Among Type IIB Supernovae > print

001     293421
005     20250730113911.0
024 7 _ |a 10.1088/0004-637X/811/2/117
|2 doi
024 7 _ |a 0004-637X
|2 ISSN
024 7 _ |a 0004-637x
|2 ISSN
024 7 _ |a 1538-4357
|2 ISSN
024 7 _ |a WOS:000363513800045
|2 WOS
024 7 _ |a 10.3204/PUBDB-2016-00510
|2 datacite_doi
024 7 _ |a inspire:1388686
|2 inspire
024 7 _ |a altmetric:4418856
|2 altmetric
024 7 _ |a openalex:W1868769978
|2 openalex
037 _ _ |a PUBDB-2016-00510
082 _ _ |a 520
100 1 _ |a Strotjohann, Nora L.
|0 P:(DE-H253)PIP1023448
|b 0
|u desy
245 _ _ |a Search for Precursor Eruptions Among Type IIB Supernovae
260 _ _ |a Chicago, Ill. [u.a.]
|c 2015
|b Univ.11032
336 7 _ |a article
|2 DRIVER
336 7 _ |a Output Types/Journal article
|2 DataCite
336 7 _ |a Journal Article
|b journal
|m journal
|0 PUB:(DE-HGF)16
|s 1480948761_895
|2 PUB:(DE-HGF)
336 7 _ |a ARTICLE
|2 BibTeX
336 7 _ |a JOURNAL_ARTICLE
|2 ORCID
336 7 _ |a Journal Article
|0 0
|2 EndNote
500 _ _ |a (c) The American Astronomical Society
520 _ _ |a The progenitor stars of several Type IIb supernovae (SNe) show indications of extended hydrogen envelopes. These envelopes might be the outcome of luminous energetic pre-explosion events, so-called precursor eruptions. We use the Palomar Transient Factory (PTF) pre-explosion observations of a sample of 27 nearby SNe IIb to look for such precursors during the final years prior to the SN explosion. No precursors are found when combining the observations in 15-day bins, and we calculate the absolute-magnitude-dependent upper limit on the precursor rate. At the 90% confidence level, SNe IIb have on average <0.86 precursors as bright as an absolute R-band magnitude of −14 in the final 3.5 years before the explosion and <0.56 events over the final year. In contrast, precursors among SNe IIn have a gsim5 times higher rate. The kinetic energy required to unbind a low-mass stellar envelope is comparable to the radiated energy of a few-weeks-long precursor that would be detectable for the closest SNe in our sample. Therefore, mass ejections, if they are common in such SNe, are radiatively inefficient or have durations longer than months. Indeed, when using 60-day bins, a faint precursor candidate is detected prior to SN 2012cs (~2% false-alarm probability). We also report the detection of the progenitor of SN 2011dh that does not show detectable variability over the final two years before the explosion. The suggested progenitor of SN 2012P is still present, and hence is likely a compact star cluster or an unrelated object.
536 _ _ |a 613 - Matter and Radiation from the Universe (POF3-613)
|0 G:(DE-HGF)POF3-613
|c POF3-613
|f POF III
|x 0
536 _ _ |a COSMICEXPLOSIONS - The nature of cosmic explosions (307260)
|0 G:(EU-Grant)307260
|c 307260
|f ERC-2012-StG_20111012
|x 1
536 _ _ |a SPCND - Supernovae: Physics and Cosmology in the Next Decade (615929)
|0 G:(EU-Grant)615929
|c 615929
|f ERC-2013-CoG
|x 2
588 _ _ |a Dataset connected to CrossRef
693 _ _ |0 EXP:(DE-H253)IceCube-20150101
|5 EXP:(DE-H253)IceCube-20150101
|e IceCube South Pole Neutrino Observatory
|x 0
700 1 _ |a Ofek, Eran O.
|b 1
700 1 _ |a Gal-Yam, Avishay
|b 2
700 1 _ |a Sullivan, Mark
|b 3
700 1 _ |a Kulkarni, Shrinivas R.
|b 4
700 1 _ |a Shaviv, Nir J.
|b 5
700 1 _ |a Fremling, Christoffer
|b 6
700 1 _ |a Kasliwal, Mansi M.
|b 7
700 1 _ |a Nugent, Peter E.
|b 8
700 1 _ |a Cao, Yi
|b 9
700 1 _ |a Arcavi, Iair
|b 10
700 1 _ |a Sollerman, Jesper
|b 11
700 1 _ |a Filippenko, Alexei V.
|b 12
700 1 _ |a Yaron, Ofer
|b 13
700 1 _ |a Laher, Russ
|b 14
700 1 _ |a Surace, Jason
|b 15
773 _ _ |a 10.1088/0004-637X/811/2/117
|g Vol. 811, no. 2, p. 117 -
|0 PERI:(DE-600)1473835-1
|n 2
|p 117 -
|t The astrophysical journal / 1
|v 811
|y 2015
|x 1538-4357
856 4 _ |y OpenAccess
|u https://bib-pubdb1.desy.de/record/293421/files/APJ811.pdf
856 4 _ |y OpenAccess
|x icon
|u https://bib-pubdb1.desy.de/record/293421/files/APJ811.gif?subformat=icon
856 4 _ |y OpenAccess
|x icon-1440
|u https://bib-pubdb1.desy.de/record/293421/files/APJ811.jpg?subformat=icon-1440
856 4 _ |y OpenAccess
|x icon-180
|u https://bib-pubdb1.desy.de/record/293421/files/APJ811.jpg?subformat=icon-180
856 4 _ |y OpenAccess
|x icon-640
|u https://bib-pubdb1.desy.de/record/293421/files/APJ811.jpg?subformat=icon-640
856 4 _ |y OpenAccess
|x pdfa
|u https://bib-pubdb1.desy.de/record/293421/files/APJ811.pdf?subformat=pdfa
909 C O |o oai:bib-pubdb1.desy.de:293421
|p openaire
|p open_access
|p driver
|p VDB
|p ec_fundedresources
|p dnbdelivery
910 1 _ |a Deutsches Elektronen-Synchrotron
|0 I:(DE-588b)2008985-5
|k DESY
|b 0
|6 P:(DE-H253)PIP1023448
913 1 _ |a DE-HGF
|b Forschungsbereich Materie
|l Materie und Universum
|1 G:(DE-HGF)POF3-610
|0 G:(DE-HGF)POF3-613
|2 G:(DE-HGF)POF3-600
|v Matter and Radiation from the Universe
|x 0
|4 G:(DE-HGF)POF
|3 G:(DE-HGF)POF3
914 1 _ |y 2015
915 _ _ |a DBCoverage
|0 StatID:(DE-HGF)0200
|2 StatID
|b SCOPUS
915 _ _ |a Free to read
|0 LIC:(DE-HGF)PublisherOA
|2 HGFVOC
915 _ _ |a JCR
|0 StatID:(DE-HGF)0100
|2 StatID
|b ASTROPHYS J : 2014
915 _ _ |a DBCoverage
|0 StatID:(DE-HGF)1150
|2 StatID
|b Current Contents - Physical, Chemical and Earth Sciences
915 _ _ |a DBCoverage
|0 StatID:(DE-HGF)0150
|2 StatID
|b Web of Science Core Collection
915 _ _ |a WoS
|0 StatID:(DE-HGF)0110
|2 StatID
|b Science Citation Index
915 _ _ |a WoS
|0 StatID:(DE-HGF)0111
|2 StatID
|b Science Citation Index Expanded
915 _ _ |a OpenAccess
|0 StatID:(DE-HGF)0510
|2 StatID
915 _ _ |a IF >= 5
|0 StatID:(DE-HGF)9905
|2 StatID
|b ASTROPHYS J : 2014
915 _ _ |a DBCoverage
|0 StatID:(DE-HGF)0300
|2 StatID
|b Medline
915 _ _ |a DBCoverage
|0 StatID:(DE-HGF)0199
|2 StatID
|b Thomson Reuters Master Journal List
920 1 _ |0 I:(DE-H253)ZEU-ICE-20160806
|k ZEU-ICE
|l Neutrinoteleskop
|x 0
980 _ _ |a journal
980 _ _ |a VDB
980 _ _ |a UNRESTRICTED
980 _ _ |a I:(DE-H253)ZEU-ICE-20160806
980 1 _ |a FullTexts

LibraryCollectionCLSMajorCLSMinorLanguageAuthor
Marc 21