Статья

PTF10ops - a subluminous, normal-width light curve Type Ia supernova in the middle of nowhere

K. MaguireDepartment of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RHM. SullivanDepartment of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RHR. C. ThomasComputational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USAP. NugentComputational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USAD. A. HowellDepartment of Physics, University of California at Santa Barbara, Santa Barbara, CA 93196, USAA. Gal‐YamDepartment of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, IsraelI. ArcaviDepartment of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, IsraelSagi Ben-AmiDepartment of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, IsraelS. BlakeDepartment of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RHJ. BotyánszkiComputational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USAC. ButonPhysikalisches Institut Universitat Bonn, Nussallee 12 53115 Bonn, GermanyJeff CookeSwinburne University of Technology, Melbourne, Victoria 3122, AustraliaRichard S. EllisCahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USAI. HookDepartment of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RHM. M. KasliwalCahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USAY. C. PanDepartment of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RHR. PereiraUniversité de Lyon, F-69622 France; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, FrancePhilipp PodsiadlowskiDepartment of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RHA. SternbergDepartment of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, IsraelN. SuzukiComputational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USAD. XuDepartment of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, IsraelO. YaronDepartment of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, IsraelJ. S. BloomDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAS. B. CenkoDepartment of Astronomy, University of California, Berkeley, CA 94720-3411, USAS. R. KulkarniCahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USANicholas M. LawDunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto M5S 3H4, Ontario, CanadaE. O. OfekCahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USAD. PoznanskiComputational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USAR. M. QuimbyCahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA

2011en

ABI

Аннотация

PTF10ops is a Type Ia supernova (SN Ia), whose light curve and spectral properties place it outside the current SN Ia subtype classifications. Its spectra display the characteristic lines of subluminous SNe Ia, but it has a normal-width light curve with a long rise time, typical of normal-luminosity SNe Ia. The early-time optical spectra of PTF10ops were modelled using a spectral fitting code and found to have all the lines typically seen in subluminous SNe Ia, without the need to invoke more uncommon elements. The host galaxy environment of PTF10ops is also unusual with no galaxy detected at the position of the SN down to an absolute limiting magnitude of r≥−12.0 mag, but a very massive galaxy is present at a separation of ∼148 kpc and at the same redshift as suggested by the SN spectral features. The progenitor of PTF10ops is most likely a very old star, possibly in a low-metallicity environment, which affects its explosion mechanism and observational characteristics. PTF10ops does not easily fit into any of the current models of either subluminous or normal SN Ia progenitor channels.

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Идентификаторы

DOI: 10.1111/j.1365-2966.2011.19526.x

Цитирования и источники

Цитирований: 2Использованных источников: 0

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