TY - JOUR
T1 - The type IIb supernova 2013df and its cool supergiant progenitor
AU - Van Dyk, Schuyler D.
AU - Zheng, Weikang
AU - Fox, Ori D.
AU - Cenko, S. Bradley
AU - Clubb, Kelsey I.
AU - Filippenko, Alexei V.
AU - Foley, Ryan J.
AU - Miller, Adam A.
AU - Smith, Nathan
AU - Kelly, Patrick L.
AU - Lee, William H.
AU - Ben-Ami, Sagi
AU - Gal-Yam, Avishay
N1 - W. M. Keck Foundation; NASA [NNX09AH71G, NNX09AT02G, NNX10AI27G, NNX12AE66G, GO-12888, GO-13030, HST-HF-51325.01]; CONACyT [INFR2009- 01-122785]; UNAM PAPIIT [IN113810]; UC MEXUS-CONACyT grant; Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST1211916]; EU/FP7 via ERC [307260]; ISAThis work is based in part on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS5-26555. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. KAIT and its ongoing research were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia and Jim Katzman Foundation, and the TABASGO Foundation. We thank the RATIR instrument team and the staff of the Observatorio Astron omico Nacional on Sierra San Pedro Martir. RATIR is a collaboration between the University of California, the Universidad Nacional Autonoma de Mexico, NASA Goddard Space Flight Center, and Arizona State University, benefiting from the loan of an H2RG detector from Teledyne Scientific and Imaging. RATIR, the automation of the Harold L. Johnson Telescope of the Observatorio Astronomico Nacional on Sierra San Pedro Martir, and the operation of both are funded by the partner institutions and through NASA grants NNX09AH71G, NNX09AT02G, NNX10AI27G, and NNX12AE66G, CONACyT grants INFR2009- 01-122785, UNAM PAPIIT grant IN113810, and a UC MEXUS-CONACyT grant. Support for this research was provid
PY - 2014/2
Y1 - 2014/2
N2 - We have obtained early-time photometry and spectroscopy of supernova (SN) 2013df in NGC 4414. The SN is clearly of Type IIb, with notable similarities to SN 1993J. From its luminosity at secondary maximum light, it appears that less 56Ni (≲ 0.06 M ·) was synthesized in the SN 2013df explosion than was the case for the SNe IIb 1993J, 2008ax, and 2011dh. Based on a comparison of the light curves, the SN 2013df progenitor must have been more extended in radius prior to explosion than the progenitor of SN 1993J. The total extinction for SN 2013df is estimated to be AV = 0.30 mag. The metallicity at the SN location is likely to be solar. We have conducted Hubble Space Telescope (HST) Target of Opportunity observations of the SN with the Wide Field Camera 3, and from a precise comparison of these new observations to archival HST observations of the host galaxy obtained 14 yr prior to explosion, we have identified the progenitor of SN 2013df to be a yellow supergiant, somewhat hotter than a red supergiant progenitor for a normal Type II-Plateau SN. From its observed spectral energy distribution, assuming that the light is dominated by one star, the progenitor had effective temperature T eff = 4250 ± 100 K and a bolometric luminosity L bol = 104.94 ± 0.06 L ·. This leads to an effective radius R eff = 545 ± 65 R . The star likely had an initial mass in the range of 13-17 M ·; however, if it was a member of an interacting binary system, detailed modeling of the system is required to estimate this mass more accurately. The progenitor star of SN 2013df appears to have been relatively similar to the progenitor of SN 1993J.
AB - We have obtained early-time photometry and spectroscopy of supernova (SN) 2013df in NGC 4414. The SN is clearly of Type IIb, with notable similarities to SN 1993J. From its luminosity at secondary maximum light, it appears that less 56Ni (≲ 0.06 M ·) was synthesized in the SN 2013df explosion than was the case for the SNe IIb 1993J, 2008ax, and 2011dh. Based on a comparison of the light curves, the SN 2013df progenitor must have been more extended in radius prior to explosion than the progenitor of SN 1993J. The total extinction for SN 2013df is estimated to be AV = 0.30 mag. The metallicity at the SN location is likely to be solar. We have conducted Hubble Space Telescope (HST) Target of Opportunity observations of the SN with the Wide Field Camera 3, and from a precise comparison of these new observations to archival HST observations of the host galaxy obtained 14 yr prior to explosion, we have identified the progenitor of SN 2013df to be a yellow supergiant, somewhat hotter than a red supergiant progenitor for a normal Type II-Plateau SN. From its observed spectral energy distribution, assuming that the light is dominated by one star, the progenitor had effective temperature T eff = 4250 ± 100 K and a bolometric luminosity L bol = 104.94 ± 0.06 L ·. This leads to an effective radius R eff = 545 ± 65 R . The star likely had an initial mass in the range of 13-17 M ·; however, if it was a member of an interacting binary system, detailed modeling of the system is required to estimate this mass more accurately. The progenitor star of SN 2013df appears to have been relatively similar to the progenitor of SN 1993J.
UR - http://www.scopus.com/inward/record.url?scp=84892724882&partnerID=8YFLogxK
U2 - https://doi.org/10.1088/0004-6256/147/2/37
DO - https://doi.org/10.1088/0004-6256/147/2/37
M3 - مقالة
SN - 0004-6256
VL - 147
JO - Astronomical Journal
JF - Astronomical Journal
IS - 2
M1 - 37
ER -