TY - JOUR
T1 - SN 2000cx and SN 2013bh
T2 - Extremely rare, nearly twin type ia supernovae
AU - Silverman, Jeffrey M.
AU - Vinko, Jozsef
AU - Kasliwal, Mansi M.
AU - Fox, Ori D.
AU - Cao, Yi
AU - Johansson, Joel
AU - Perley, Daniel A.
AU - Tal, David
AU - Wheeler, J. Craig
AU - Amanullah, Rahman
AU - Arcavi, Iair
AU - Bloom, Joshua S.
AU - Gal-Yam, Avishay
AU - Goobar, Ariel
AU - Kulkarni, Shrinivas R.
AU - Laher, Russ
AU - Lee, William H.
AU - Marion, G. H.
AU - Nugent, Peter E.
AU - Shivvers, Isaac
N1 - W. M. Keck Foundation; NASA [NNX09AH71G, NNX09AT02G, NNX10AI27G, NNX12AE66G]; CONACyT [INFR-2009-01-122785]; UNAM PAPIIT [IN113810]; UC MEXUS-CONACyT; Alfred P. Sloan Foundation; NSF; US Department of Energy Office of Science; NSF [AST-1302771, AST 11-09801, PHY-1066293]; Hungarian OTKA [NN 107637]; Hubble Fellowship; Carnegie-Princeton Fellowship; CDI from the National Science Foundation [0941742]We would like to thank M. Ganeshalingam, P. Kelly and E. Ofek for helpful discussions, J. Caldwell, S. Odewahn and S. Rostopchin for their assistance with some of the observations, as well as the PESSTO and CRTS collaborations for making some of their data on SN 2013bh publicly available. The HET is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universitat Munchen and Georg-August-Universitat Gottingen. The HET is named in honour of its principal benefactors, William P. Hobby and Robert E. Eberly. The Marcario Low Resolution Spectrograph is named for Mike Marcario of High Lonesome Optics who fabricated several optics for the instrument but died before its completion. The LRS is a joint project of the HET partnership and the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico. 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 the National Aeronautics and Space Administration (NASA); the observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain. This work is partially based on observations made with the Nordic Optical
PY - 2013/12
Y1 - 2013/12
N2 - The Type Ia supernova (SN Ia) SN 2000cx was one of the most peculiar transients ever discovered, with a rise to maximum brightness typical of a SN Ia, but a slower decline and a higher photospheric temperature. 13 yr later SN 2013bh (also known as iPTF13abc), a near identical twin, was discovered and we obtained optical and near-infrared photometry and low-resolution optical spectroscopy from discovery until about 1 month past r-band maximum brightness. The spectra of both objects show iron-group elements [Co II, Ni II, FeII, Fe III and high-velocity features (HVFs) of Ti II], intermediate-mass elements (Si II, Si III and S II) and separate normal velocity features (~12 000 km s-1) and HVFs (~24 000 km s-1) of Ca II. Persistent absorption from Fe III and Si III, along with the colour evolution, implies high blackbody temperatures for SNe 2013bh and 2000cx (~12 000 K). Both objects lack narrow Na I D absorption and exploded in the outskirts of their hosts, indicating that the SN environments were relatively free of interstellar or circumstellar material and may imply that the progenitors came from a relatively old and low-metallicity stellar population. Models of SN 2000cx, seemingly applicable to SN 2013bh, imply the production of up to 1 M of 56Ni and (4.3-5.5) × 10-3 M⊙ of fast-moving Ca ejecta.
AB - The Type Ia supernova (SN Ia) SN 2000cx was one of the most peculiar transients ever discovered, with a rise to maximum brightness typical of a SN Ia, but a slower decline and a higher photospheric temperature. 13 yr later SN 2013bh (also known as iPTF13abc), a near identical twin, was discovered and we obtained optical and near-infrared photometry and low-resolution optical spectroscopy from discovery until about 1 month past r-band maximum brightness. The spectra of both objects show iron-group elements [Co II, Ni II, FeII, Fe III and high-velocity features (HVFs) of Ti II], intermediate-mass elements (Si II, Si III and S II) and separate normal velocity features (~12 000 km s-1) and HVFs (~24 000 km s-1) of Ca II. Persistent absorption from Fe III and Si III, along with the colour evolution, implies high blackbody temperatures for SNe 2013bh and 2000cx (~12 000 K). Both objects lack narrow Na I D absorption and exploded in the outskirts of their hosts, indicating that the SN environments were relatively free of interstellar or circumstellar material and may imply that the progenitors came from a relatively old and low-metallicity stellar population. Models of SN 2000cx, seemingly applicable to SN 2013bh, imply the production of up to 1 M of 56Ni and (4.3-5.5) × 10-3 M⊙ of fast-moving Ca ejecta.
KW - Supernovae:general
KW - Supernovae:individual:SN 2000cx
KW - Supernovae:individual:SN 2013bh
UR - http://www.scopus.com/inward/record.url?scp=84888061704&partnerID=8YFLogxK
U2 - 10.1093/mnras/stt1647
DO - 10.1093/mnras/stt1647
M3 - مقالة
SN - 0035-8711
VL - 436
SP - 1225
EP - 1237
JO - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
JF - MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
IS - 2
ER -