PTF10ops – a subluminous, normal‐width light curve Type Ia supernova in the middle of nowhere
Identifieur interne : 002D17 ( Istex/Corpus ); précédent : 002D16; suivant : 002D18PTF10ops – a subluminous, normal‐width light curve Type Ia supernova in the middle of nowhere
Auteurs : K. Maguire ; M. Sullivan ; R. C. Thomas ; P. Nugent ; D. A. Howell ; A. Gal-Yam ; I. Arcavi ; S. Ben-Ami ; S. Blake ; J. Botyanszki ; C. Buton ; J. Cooke ; R. S. Ellis ; I. M. Hook ; M. M. Kasliwal ; Y. Pan ; R. Pereira ; P. Podsiadlowski ; A. Sternberg ; N. Suzuki ; D. Xu ; O. Yaron ; J. S. Bloom ; S. B. Cenko ; S. R. Kulkarni ; N. Law ; E. O. Ofek ; D. Poznanski ; R. M. QuimbySource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-12-01.
English descriptors
- KwdEn :
- Absolute magnitude, Absolute magnitude limit, Absorption features, Benetti, Bolometric, Bolometric luminosity, California institute, Centre, Colour terms, Cool photosphere, Cool spectra, Cumbres observatory, Distance modulus, Equivalent widths, Exotic explosion, Explosion mechanism, Extinction, Faint group, Faint host galaxies, Galactic extinction, Galaxy, Globular, Globular cluster, Globular clusters, Halo, Host galaxies, Host galaxy, Host galaxy extinction, Host velocities, Howell, Hubble space telescope, Input parameters, July, Large distance, Large distances, Lawrence berkeley, Light curve, Light curve width, Light curves, Luminosity, Magnitude space, Massive galaxies, Massive galaxy, Massive spiral galaxy, Massive star, Maximum light, Maximum magnitude, Metallicity, Mnras, Monthly notices, More detail, More details, Nancial support, National aeronautics, Nearby spiral galaxy, Nearby supernova factory, Normal luminosity, Normal template, Normal templates, Optical magnitudes, Optical spectra, Palomar observatory, Pasp, Peak bband magnitude, Peak luminosity, Peak magnitude, Photometry, Photospheric, Photospheric phase spectra, Physique nucl, Progenitor, Progenitor model, Progenitor star, Redshift, Rest frame, Rise time, Same redshift, Samuel oschin telescope, Santa barbara, Sdss system, Secondary maxima, Secondary peak, Sifto, Similar properties, Space administration, Space telescope science institute, Spanish observatorio, Spectral, Spectral features, Spectral properties, Spectral template, Spectrum, Spiral galaxy, Stellar, Stellar population, Stellar populations, Stretch value, Stretch values, Strong lines, Subluminous, Subluminous events, Subluminous objects, Subluminous template, Substantial host galaxy extinction, Supernova, Synapps, Taubenberger, Technology facilities council, Telescope, Template, Template spectrum, Tertiary standards, Third epochs, Tting, Tting code synapps, Velocity gradient group, Weizmann institute.
- Teeft :
- Absolute magnitude, Absolute magnitude limit, Absorption features, Benetti, Bolometric, Bolometric luminosity, California institute, Centre, Colour terms, Cool photosphere, Cool spectra, Cumbres observatory, Distance modulus, Equivalent widths, Exotic explosion, Explosion mechanism, Extinction, Faint group, Faint host galaxies, Galactic extinction, Galaxy, Globular, Globular cluster, Globular clusters, Halo, Host galaxies, Host galaxy, Host galaxy extinction, Host velocities, Howell, Hubble space telescope, Input parameters, July, Large distance, Large distances, Lawrence berkeley, Light curve, Light curve width, Light curves, Luminosity, Magnitude space, Massive galaxies, Massive galaxy, Massive spiral galaxy, Massive star, Maximum light, Maximum magnitude, Metallicity, Mnras, Monthly notices, More detail, More details, Nancial support, National aeronautics, Nearby spiral galaxy, Nearby supernova factory, Normal luminosity, Normal template, Normal templates, Optical magnitudes, Optical spectra, Palomar observatory, Pasp, Peak bband magnitude, Peak luminosity, Peak magnitude, Photometry, Photospheric, Photospheric phase spectra, Physique nucl, Progenitor, Progenitor model, Progenitor star, Redshift, Rest frame, Rise time, Same redshift, Samuel oschin telescope, Santa barbara, Sdss system, Secondary maxima, Secondary peak, Sifto, Similar properties, Space administration, Space telescope science institute, Spanish observatorio, Spectral, Spectral features, Spectral properties, Spectral template, Spectrum, Spiral galaxy, Stellar, Stellar population, Stellar populations, Stretch value, Stretch values, Strong lines, Subluminous, Subluminous events, Subluminous objects, Subluminous template, Substantial host galaxy extinction, Supernova, Synapps, Taubenberger, Technology facilities council, Telescope, Template, Template spectrum, Tertiary standards, Third epochs, Tting, Tting code synapps, Velocity gradient group, Weizmann institute.
Abstract
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.
Url:
DOI: 10.1111/j.1365-2966.2011.19526.x
Links to Exploration step
ISTEX:EF4AA392C829B78146F1F0FCD6D4E82C0261078BLe document en format XML
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Howell</name><affiliation><mods:affiliation>Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117, USA</mods:affiliation></affiliation><affiliation><mods:affiliation>Department of Physics, University of California at Santa Barbara, Santa Barbara, CA 93196, USA</mods:affiliation></affiliation></author><author><name sortKey="Gal Am, A" sort="Gal Am, A" uniqKey="Gal Am A" first="A." last="Gal-Yam">A. Gal-Yam</name><affiliation><mods:affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</mods:affiliation></affiliation></author><author><name sortKey="Arcavi, I" sort="Arcavi, I" uniqKey="Arcavi I" first="I." last="Arcavi">I. 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Botyanszki</name><affiliation><mods:affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</mods:affiliation></affiliation><affiliation><mods:affiliation>Department of Physics, University of California, Berkeley, CA 94720‐3411, USA</mods:affiliation></affiliation></author><author><name sortKey="Buton, C" sort="Buton, C" uniqKey="Buton C" first="C." last="Buton">C. Buton</name><affiliation><mods:affiliation>Physikalisches Institut Universitat Bonn, Nussallee 12 53115 Bonn, Germany</mods:affiliation></affiliation></author><author><name sortKey="Cooke, J" sort="Cooke, J" uniqKey="Cooke J" first="J." last="Cooke">J. Cooke</name><affiliation><mods:affiliation>Swinburne University of Technology, Melbourne, Victoria 3122, Australia</mods:affiliation></affiliation></author><author><name sortKey="Ellis, R S" sort="Ellis, R S" uniqKey="Ellis R" first="R. S." last="Ellis">R. S. 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Pan</name><affiliation><mods:affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</mods:affiliation></affiliation></author><author><name sortKey="Pereira, R" sort="Pereira, R" uniqKey="Pereira R" first="R." last="Pereira">R. Pereira</name><affiliation><mods:affiliation>Université de Lyon, F‐69622 France; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, France</mods:affiliation></affiliation></author><author><name sortKey="Podsiadlowski, P" sort="Podsiadlowski, P" uniqKey="Podsiadlowski P" first="P." last="Podsiadlowski">P. Podsiadlowski</name><affiliation><mods:affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</mods:affiliation></affiliation></author><author><name sortKey="Sternberg, A" sort="Sternberg, A" uniqKey="Sternberg A" first="A." last="Sternberg">A. Sternberg</name><affiliation><mods:affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</mods:affiliation></affiliation></author><author><name sortKey="Suzuki, N" sort="Suzuki, N" uniqKey="Suzuki N" first="N." last="Suzuki">N. Suzuki</name><affiliation><mods:affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</mods:affiliation></affiliation></author><author><name sortKey="Xu, D" sort="Xu, D" uniqKey="Xu D" first="D." last="Xu">D. Xu</name><affiliation><mods:affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</mods:affiliation></affiliation></author><author><name sortKey="Yaron, O" sort="Yaron, O" uniqKey="Yaron O" first="O." last="Yaron">O. Yaron</name><affiliation><mods:affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</mods:affiliation></affiliation></author><author><name sortKey="Bloom, J S" sort="Bloom, J S" uniqKey="Bloom J" first="J. S." last="Bloom">J. S. Bloom</name><affiliation><mods:affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</mods:affiliation></affiliation></author><author><name sortKey="Cenko, S B" sort="Cenko, S B" uniqKey="Cenko S" first="S. B." last="Cenko">S. B. Cenko</name><affiliation><mods:affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</mods:affiliation></affiliation></author><author><name sortKey="Kulkarni, S R" sort="Kulkarni, S R" uniqKey="Kulkarni S" first="S. R." last="Kulkarni">S. R. Kulkarni</name><affiliation><mods:affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</mods:affiliation></affiliation></author><author><name sortKey="Law, N" sort="Law, N" uniqKey="Law N" first="N." last="Law">N. Law</name><affiliation><mods:affiliation>Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto M5S 3H4, Ontario, Canada</mods:affiliation></affiliation></author><author><name sortKey="Ofek, E O" sort="Ofek, E O" uniqKey="Ofek E" first="E. O." last="Ofek">E. O. Ofek</name><affiliation><mods:affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</mods:affiliation></affiliation></author><author><name sortKey="Poznanski, D" sort="Poznanski, D" uniqKey="Poznanski D" first="D." last="Poznanski">D. Poznanski</name><affiliation><mods:affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</mods:affiliation></affiliation><affiliation><mods:affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</mods:affiliation></affiliation></author><author><name sortKey="Quimby, R M" sort="Quimby, R M" uniqKey="Quimby R" first="R. M." last="Quimby">R. M. Quimby</name><affiliation><mods:affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</mods:affiliation></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:EF4AA392C829B78146F1F0FCD6D4E82C0261078B</idno><date when="2011" year="2011">2011</date><idno type="doi">10.1111/j.1365-2966.2011.19526.x</idno><idno type="url">https://api.istex.fr/document/EF4AA392C829B78146F1F0FCD6D4E82C0261078B/fulltext/pdf</idno><idno type="wicri:Area/Istex/Corpus">002D17</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">002D17</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a" type="main">PTF10ops – a subluminous, normal‐width light curve Type Ia supernova in the middle of nowhere</title><author><name sortKey="Maguire, K" sort="Maguire, K" uniqKey="Maguire K" first="K." last="Maguire">K. Maguire</name><affiliation><mods:affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: kate.maguire@astro.ox.ac.uk</mods:affiliation></affiliation></author><author><name sortKey="Sullivan, M" sort="Sullivan, M" uniqKey="Sullivan M" first="M." last="Sullivan">M. Sullivan</name><affiliation><mods:affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</mods:affiliation></affiliation></author><author><name sortKey="Thomas, R C" sort="Thomas, R C" uniqKey="Thomas R" first="R. C." last="Thomas">R. C. Thomas</name><affiliation><mods:affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</mods:affiliation></affiliation><affiliation><mods:affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</mods:affiliation></affiliation></author><author><name sortKey="Nugent, P" sort="Nugent, P" uniqKey="Nugent P" first="P." last="Nugent">P. Nugent</name><affiliation><mods:affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</mods:affiliation></affiliation><affiliation><mods:affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</mods:affiliation></affiliation></author><author><name sortKey="Howell, D A" sort="Howell, D A" uniqKey="Howell D" first="D. A." last="Howell">D. A. Howell</name><affiliation><mods:affiliation>Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117, USA</mods:affiliation></affiliation><affiliation><mods:affiliation>Department of Physics, University of California at Santa Barbara, Santa Barbara, CA 93196, USA</mods:affiliation></affiliation></author><author><name sortKey="Gal Am, A" sort="Gal Am, A" uniqKey="Gal Am A" first="A." last="Gal-Yam">A. Gal-Yam</name><affiliation><mods:affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</mods:affiliation></affiliation></author><author><name sortKey="Arcavi, I" sort="Arcavi, I" uniqKey="Arcavi I" first="I." last="Arcavi">I. Arcavi</name><affiliation><mods:affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</mods:affiliation></affiliation></author><author><name sortKey="Ben Mi, S" sort="Ben Mi, S" uniqKey="Ben Mi S" first="S." last="Ben-Ami">S. Ben-Ami</name><affiliation><mods:affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</mods:affiliation></affiliation></author><author><name sortKey="Blake, S" sort="Blake, S" uniqKey="Blake S" first="S." last="Blake">S. Blake</name><affiliation><mods:affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</mods:affiliation></affiliation></author><author><name sortKey="Botyanszki, J" sort="Botyanszki, J" uniqKey="Botyanszki J" first="J." last="Botyanszki">J. Botyanszki</name><affiliation><mods:affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</mods:affiliation></affiliation><affiliation><mods:affiliation>Department of Physics, University of California, Berkeley, CA 94720‐3411, USA</mods:affiliation></affiliation></author><author><name sortKey="Buton, C" sort="Buton, C" uniqKey="Buton C" first="C." last="Buton">C. Buton</name><affiliation><mods:affiliation>Physikalisches Institut Universitat Bonn, Nussallee 12 53115 Bonn, Germany</mods:affiliation></affiliation></author><author><name sortKey="Cooke, J" sort="Cooke, J" uniqKey="Cooke J" first="J." last="Cooke">J. Cooke</name><affiliation><mods:affiliation>Swinburne University of Technology, Melbourne, Victoria 3122, Australia</mods:affiliation></affiliation></author><author><name sortKey="Ellis, R S" sort="Ellis, R S" uniqKey="Ellis R" first="R. S." last="Ellis">R. S. Ellis</name><affiliation><mods:affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</mods:affiliation></affiliation></author><author><name sortKey="Hook, I M" sort="Hook, I M" uniqKey="Hook I" first="I. M." last="Hook">I. M. Hook</name><affiliation><mods:affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</mods:affiliation></affiliation><affiliation><mods:affiliation>INAF – Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy</mods:affiliation></affiliation></author><author><name sortKey="Kasliwal, M M" sort="Kasliwal, M M" uniqKey="Kasliwal M" first="M. M." last="Kasliwal">M. M. Kasliwal</name><affiliation><mods:affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</mods:affiliation></affiliation></author><author><name sortKey="Pan, Y" sort="Pan, Y" uniqKey="Pan Y" first="Y." last="Pan">Y. Pan</name><affiliation><mods:affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</mods:affiliation></affiliation></author><author><name sortKey="Pereira, R" sort="Pereira, R" uniqKey="Pereira R" first="R." last="Pereira">R. Pereira</name><affiliation><mods:affiliation>Université de Lyon, F‐69622 France; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, France</mods:affiliation></affiliation></author><author><name sortKey="Podsiadlowski, P" sort="Podsiadlowski, P" uniqKey="Podsiadlowski P" first="P." last="Podsiadlowski">P. Podsiadlowski</name><affiliation><mods:affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</mods:affiliation></affiliation></author><author><name sortKey="Sternberg, A" sort="Sternberg, A" uniqKey="Sternberg A" first="A." last="Sternberg">A. Sternberg</name><affiliation><mods:affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</mods:affiliation></affiliation></author><author><name sortKey="Suzuki, N" sort="Suzuki, N" uniqKey="Suzuki N" first="N." last="Suzuki">N. Suzuki</name><affiliation><mods:affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</mods:affiliation></affiliation></author><author><name sortKey="Xu, D" sort="Xu, D" uniqKey="Xu D" first="D." last="Xu">D. Xu</name><affiliation><mods:affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</mods:affiliation></affiliation></author><author><name sortKey="Yaron, O" sort="Yaron, O" uniqKey="Yaron O" first="O." last="Yaron">O. Yaron</name><affiliation><mods:affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</mods:affiliation></affiliation></author><author><name sortKey="Bloom, J S" sort="Bloom, J S" uniqKey="Bloom J" first="J. S." last="Bloom">J. S. Bloom</name><affiliation><mods:affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</mods:affiliation></affiliation></author><author><name sortKey="Cenko, S B" sort="Cenko, S B" uniqKey="Cenko S" first="S. B." last="Cenko">S. B. Cenko</name><affiliation><mods:affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</mods:affiliation></affiliation></author><author><name sortKey="Kulkarni, S R" sort="Kulkarni, S R" uniqKey="Kulkarni S" first="S. R." last="Kulkarni">S. R. Kulkarni</name><affiliation><mods:affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</mods:affiliation></affiliation></author><author><name sortKey="Law, N" sort="Law, N" uniqKey="Law N" first="N." last="Law">N. Law</name><affiliation><mods:affiliation>Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto M5S 3H4, Ontario, Canada</mods:affiliation></affiliation></author><author><name sortKey="Ofek, E O" sort="Ofek, E O" uniqKey="Ofek E" first="E. O." last="Ofek">E. O. Ofek</name><affiliation><mods:affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</mods:affiliation></affiliation></author><author><name sortKey="Poznanski, D" sort="Poznanski, D" uniqKey="Poznanski D" first="D." last="Poznanski">D. Poznanski</name><affiliation><mods:affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</mods:affiliation></affiliation><affiliation><mods:affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</mods:affiliation></affiliation></author><author><name sortKey="Quimby, R M" sort="Quimby, R M" uniqKey="Quimby R" first="R. M." last="Quimby">R. M. Quimby</name><affiliation><mods:affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">418</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="747">747</biblScope><biblScope unit="page" to="758">758</biblScope><biblScope unit="page-count">12</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2011-12-01">2011-12-01</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Absolute magnitude</term><term>Absolute magnitude limit</term><term>Absorption features</term><term>Benetti</term><term>Bolometric</term><term>Bolometric luminosity</term><term>California institute</term><term>Centre</term><term>Colour terms</term><term>Cool photosphere</term><term>Cool spectra</term><term>Cumbres observatory</term><term>Distance modulus</term><term>Equivalent widths</term><term>Exotic explosion</term><term>Explosion mechanism</term><term>Extinction</term><term>Faint group</term><term>Faint host galaxies</term><term>Galactic extinction</term><term>Galaxy</term><term>Globular</term><term>Globular cluster</term><term>Globular clusters</term><term>Halo</term><term>Host galaxies</term><term>Host galaxy</term><term>Host galaxy extinction</term><term>Host velocities</term><term>Howell</term><term>Hubble space telescope</term><term>Input parameters</term><term>July</term><term>Large distance</term><term>Large distances</term><term>Lawrence berkeley</term><term>Light curve</term><term>Light curve width</term><term>Light curves</term><term>Luminosity</term><term>Magnitude space</term><term>Massive galaxies</term><term>Massive galaxy</term><term>Massive spiral galaxy</term><term>Massive star</term><term>Maximum light</term><term>Maximum magnitude</term><term>Metallicity</term><term>Mnras</term><term>Monthly notices</term><term>More detail</term><term>More details</term><term>Nancial support</term><term>National aeronautics</term><term>Nearby spiral galaxy</term><term>Nearby supernova factory</term><term>Normal luminosity</term><term>Normal template</term><term>Normal templates</term><term>Optical magnitudes</term><term>Optical spectra</term><term>Palomar observatory</term><term>Pasp</term><term>Peak bband magnitude</term><term>Peak luminosity</term><term>Peak magnitude</term><term>Photometry</term><term>Photospheric</term><term>Photospheric phase spectra</term><term>Physique nucl</term><term>Progenitor</term><term>Progenitor model</term><term>Progenitor star</term><term>Redshift</term><term>Rest frame</term><term>Rise time</term><term>Same redshift</term><term>Samuel oschin telescope</term><term>Santa barbara</term><term>Sdss system</term><term>Secondary maxima</term><term>Secondary peak</term><term>Sifto</term><term>Similar properties</term><term>Space administration</term><term>Space telescope science institute</term><term>Spanish observatorio</term><term>Spectral</term><term>Spectral features</term><term>Spectral properties</term><term>Spectral template</term><term>Spectrum</term><term>Spiral galaxy</term><term>Stellar</term><term>Stellar population</term><term>Stellar populations</term><term>Stretch value</term><term>Stretch values</term><term>Strong lines</term><term>Subluminous</term><term>Subluminous events</term><term>Subluminous objects</term><term>Subluminous template</term><term>Substantial host galaxy extinction</term><term>Supernova</term><term>Synapps</term><term>Taubenberger</term><term>Technology facilities council</term><term>Telescope</term><term>Template</term><term>Template spectrum</term><term>Tertiary standards</term><term>Third epochs</term><term>Tting</term><term>Tting code synapps</term><term>Velocity gradient group</term><term>Weizmann institute</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Absolute magnitude</term><term>Absolute magnitude limit</term><term>Absorption features</term><term>Benetti</term><term>Bolometric</term><term>Bolometric luminosity</term><term>California institute</term><term>Centre</term><term>Colour terms</term><term>Cool photosphere</term><term>Cool spectra</term><term>Cumbres observatory</term><term>Distance modulus</term><term>Equivalent widths</term><term>Exotic explosion</term><term>Explosion mechanism</term><term>Extinction</term><term>Faint group</term><term>Faint host galaxies</term><term>Galactic extinction</term><term>Galaxy</term><term>Globular</term><term>Globular cluster</term><term>Globular clusters</term><term>Halo</term><term>Host galaxies</term><term>Host galaxy</term><term>Host galaxy extinction</term><term>Host velocities</term><term>Howell</term><term>Hubble space telescope</term><term>Input parameters</term><term>July</term><term>Large distance</term><term>Large distances</term><term>Lawrence berkeley</term><term>Light curve</term><term>Light curve width</term><term>Light curves</term><term>Luminosity</term><term>Magnitude space</term><term>Massive galaxies</term><term>Massive galaxy</term><term>Massive spiral galaxy</term><term>Massive star</term><term>Maximum light</term><term>Maximum magnitude</term><term>Metallicity</term><term>Mnras</term><term>Monthly notices</term><term>More detail</term><term>More details</term><term>Nancial support</term><term>National aeronautics</term><term>Nearby spiral galaxy</term><term>Nearby supernova factory</term><term>Normal luminosity</term><term>Normal template</term><term>Normal templates</term><term>Optical magnitudes</term><term>Optical spectra</term><term>Palomar observatory</term><term>Pasp</term><term>Peak bband magnitude</term><term>Peak luminosity</term><term>Peak magnitude</term><term>Photometry</term><term>Photospheric</term><term>Photospheric phase spectra</term><term>Physique nucl</term><term>Progenitor</term><term>Progenitor model</term><term>Progenitor star</term><term>Redshift</term><term>Rest frame</term><term>Rise time</term><term>Same redshift</term><term>Samuel oschin telescope</term><term>Santa barbara</term><term>Sdss system</term><term>Secondary maxima</term><term>Secondary peak</term><term>Sifto</term><term>Similar properties</term><term>Space administration</term><term>Space telescope science institute</term><term>Spanish observatorio</term><term>Spectral</term><term>Spectral features</term><term>Spectral properties</term><term>Spectral template</term><term>Spectrum</term><term>Spiral galaxy</term><term>Stellar</term><term>Stellar population</term><term>Stellar populations</term><term>Stretch value</term><term>Stretch values</term><term>Strong lines</term><term>Subluminous</term><term>Subluminous events</term><term>Subluminous objects</term><term>Subluminous template</term><term>Substantial host galaxy extinction</term><term>Supernova</term><term>Synapps</term><term>Taubenberger</term><term>Technology facilities council</term><term>Telescope</term><term>Template</term><term>Template spectrum</term><term>Tertiary standards</term><term>Third epochs</term><term>Tting</term><term>Tting code synapps</term><term>Velocity gradient group</term><term>Weizmann institute</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">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.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>subluminous</json:string><json:string>light curve</json:string><json:string>progenitor</json:string><json:string>mnras</json:string><json:string>sifto</json:string><json:string>galaxy</json:string><json:string>redshift</json:string><json:string>pasp</json:string><json:string>monthly notices</json:string><json:string>july</json:string><json:string>supernova</json:string><json:string>host galaxy</json:string><json:string>globular</json:string><json:string>luminosity</json:string><json:string>photometry</json:string><json:string>rise time</json:string><json:string>bolometric</json:string><json:string>taubenberger</json:string><json:string>light curves</json:string><json:string>host galaxies</json:string><json:string>photospheric</json:string><json:string>rest frame</json:string><json:string>benetti</json:string><json:string>maximum light</json:string><json:string>tting</json:string><json:string>metallicity</json:string><json:string>spectral features</json:string><json:string>synapps</json:string><json:string>subluminous template</json:string><json:string>bolometric luminosity</json:string><json:string>secondary maxima</json:string><json:string>normal template</json:string><json:string>absolute magnitude</json:string><json:string>host galaxy extinction</json:string><json:string>photospheric phase spectra</json:string><json:string>california institute</json:string><json:string>subluminous events</json:string><json:string>massive galaxies</json:string><json:string>normal luminosity</json:string><json:string>large distances</json:string><json:string>galactic extinction</json:string><json:string>massive star</json:string><json:string>massive spiral galaxy</json:string><json:string>globular cluster</json:string><json:string>optical spectra</json:string><json:string>absorption features</json:string><json:string>template</json:string><json:string>stellar</json:string><json:string>howell</json:string><json:string>faint host galaxies</json:string><json:string>globular clusters</json:string><json:string>stellar populations</json:string><json:string>spiral galaxy</json:string><json:string>physique nucl</json:string><json:string>lawrence berkeley</json:string><json:string>peak magnitude</json:string><json:string>massive galaxy</json:string><json:string>normal templates</json:string><json:string>equivalent widths</json:string><json:string>extinction</json:string><json:string>spectrum</json:string><json:string>halo</json:string><json:string>centre</json:string><json:string>telescope</json:string><json:string>palomar observatory</json:string><json:string>more details</json:string><json:string>samuel oschin telescope</json:string><json:string>nearby supernova factory</json:string><json:string>maximum magnitude</json:string><json:string>progenitor star</json:string><json:string>large distance</json:string><json:string>stretch values</json:string><json:string>more detail</json:string><json:string>magnitude space</json:string><json:string>spectral template</json:string><json:string>strong lines</json:string><json:string>cumbres observatory</json:string><json:string>subluminous objects</json:string><json:string>peak bband magnitude</json:string><json:string>similar properties</json:string><json:string>substantial host galaxy extinction</json:string><json:string>peak luminosity</json:string><json:string>light curve width</json:string><json:string>optical magnitudes</json:string><json:string>space telescope science institute</json:string><json:string>secondary peak</json:string><json:string>template spectrum</json:string><json:string>cool spectra</json:string><json:string>progenitor model</json:string><json:string>spectral properties</json:string><json:string>host velocities</json:string><json:string>explosion mechanism</json:string><json:string>santa barbara</json:string><json:string>same redshift</json:string><json:string>tting code synapps</json:string><json:string>input parameters</json:string><json:string>third epochs</json:string><json:string>velocity gradient group</json:string><json:string>faint group</json:string><json:string>hubble space telescope</json:string><json:string>cool photosphere</json:string><json:string>absolute magnitude limit</json:string><json:string>nearby spiral galaxy</json:string><json:string>weizmann institute</json:string><json:string>tertiary standards</json:string><json:string>exotic explosion</json:string><json:string>colour terms</json:string><json:string>space administration</json:string><json:string>distance modulus</json:string><json:string>stellar population</json:string><json:string>sdss system</json:string><json:string>technology facilities council</json:string><json:string>spanish observatorio</json:string><json:string>nancial support</json:string><json:string>national aeronautics</json:string><json:string>stretch value</json:string><json:string>spectral</json:string></teeft></keywords><author><json:item><name>K. Maguire</name><affiliations><json:string>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</json:string><json:string>E-mail: kate.maguire@astro.ox.ac.uk</json:string></affiliations></json:item><json:item><name>M. Sullivan</name><affiliations><json:string>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</json:string></affiliations></json:item><json:item><name>R. C. Thomas</name><affiliations><json:string>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</json:string><json:string>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</json:string></affiliations></json:item><json:item><name>P. Nugent</name><affiliations><json:string>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</json:string><json:string>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</json:string></affiliations></json:item><json:item><name>D. A. Howell</name><affiliations><json:string>Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117, USA</json:string><json:string>Department of Physics, University of California at Santa Barbara, Santa Barbara, CA 93196, USA</json:string></affiliations></json:item><json:item><name>A. Gal‐Yam</name><affiliations><json:string>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</json:string></affiliations></json:item><json:item><name>I. Arcavi</name><affiliations><json:string>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</json:string></affiliations></json:item><json:item><name>S. Ben‐Ami</name><affiliations><json:string>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</json:string></affiliations></json:item><json:item><name>S. Blake</name><affiliations><json:string>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</json:string></affiliations></json:item><json:item><name>J. Botyanszki</name><affiliations><json:string>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</json:string><json:string>Department of Physics, University of California, Berkeley, CA 94720‐3411, USA</json:string></affiliations></json:item><json:item><name>C. Buton</name><affiliations><json:string>Physikalisches Institut Universitat Bonn, Nussallee 12 53115 Bonn, Germany</json:string></affiliations></json:item><json:item><name>J. Cooke</name><affiliations><json:string>Swinburne University of Technology, Melbourne, Victoria 3122, Australia</json:string></affiliations></json:item><json:item><name>R. S. Ellis</name><affiliations><json:string>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</json:string></affiliations></json:item><json:item><name>I. M. Hook</name><affiliations><json:string>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</json:string><json:string>INAF – Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy</json:string></affiliations></json:item><json:item><name>M. M. Kasliwal</name><affiliations><json:string>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</json:string></affiliations></json:item><json:item><name>Y.‐C. Pan</name><affiliations><json:string>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</json:string></affiliations></json:item><json:item><name>R. Pereira</name><affiliations><json:string>Université de Lyon, F‐69622 France; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, France</json:string></affiliations></json:item><json:item><name>P. Podsiadlowski</name><affiliations><json:string>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</json:string></affiliations></json:item><json:item><name>A. Sternberg</name><affiliations><json:string>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</json:string></affiliations></json:item><json:item><name>N. Suzuki</name><affiliations><json:string>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</json:string></affiliations></json:item><json:item><name>D. Xu</name><affiliations><json:string>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</json:string></affiliations></json:item><json:item><name>O. Yaron</name><affiliations><json:string>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</json:string></affiliations></json:item><json:item><name>J. S. Bloom</name><affiliations><json:string>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</json:string></affiliations></json:item><json:item><name>S. B. Cenko</name><affiliations><json:string>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</json:string></affiliations></json:item><json:item><name>S. R. Kulkarni</name><affiliations><json:string>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</json:string></affiliations></json:item><json:item><name>N. Law</name><affiliations><json:string>Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto M5S 3H4, Ontario, Canada</json:string></affiliations></json:item><json:item><name>E. O. Ofek</name><affiliations><json:string>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</json:string></affiliations></json:item><json:item><name>D. Poznanski</name><affiliations><json:string>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</json:string><json:string>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</json:string></affiliations></json:item><json:item><name>R. M. Quimby</name><affiliations><json:string>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>supernovae: general</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>supernovae: individual: PTF10ops</value></json:item></subject><articleId><json:string>MNR19526</json:string></articleId><arkIstex>ark:/67375/WNG-9VKHV5ZQ-Z</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>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.</abstract><qualityIndicators><refBibsNative>true</refBibsNative><abstractWordCount>179</abstractWordCount><abstractCharCount>1103</abstractCharCount><keywordCount>2</keywordCount><score>9.148</score><pdfWordCount>9718</pdfWordCount><pdfCharCount>51634</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>12</pdfPageCount><pdfPageSize>595.274 x 782.286 pts</pdfPageSize></qualityIndicators><title>PTF10ops – a subluminous, normal‐width light curve Type Ia supernova in the middle of nowhere</title><genre><json:string>article</json:string></genre><host><title>Monthly Notices of the Royal Astronomical Society</title><language><json:string>unknown</json:string></language><doi><json:string>10.1111/(ISSN)1365-2966</json:string></doi><issn><json:string>0035-8711</json:string></issn><eissn><json:string>1365-2966</json:string></eissn><publisherId><json:string>MNR</json:string></publisherId><volume>418</volume><issue>2</issue><pages><first>747</first><last>758</last><total>12</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>2011</json:string></date><geogName></geogName><orgName><json:string>University of Toronto</json:string><json:string>California Institute of Technology, Columbia Unversity, La Cumbres Observatory, the Lawrence Berkeley National Laboratory, the National Energy Research Scienti</json:string><json:string>Department of Astronomy, University of California, Berkeley, CA</json:string><json:string>Department of Physics, University of California, Berkeley, CA</json:string><json:string>University of Oxford</json:string><json:string>Swinburne University</json:string><json:string>Weizmann Institute of Science</json:string><json:string>Lawrence Berkeley National Laboratory, Yale University, University of Bonn, Max Planck Institute for Astrophysics, Tsinghua Center for Astrophysics, and the Centre</json:string><json:string>TABASGO Foundation, and NSF</json:string><json:string>Astronomy, Inc.</json:string><json:string>California Institute of Technology, Pasadena, CA</json:string><json:string>Department of Particle Physics and Astrophysics</json:string><json:string>Lawrence Berkeley National Laboratory</json:string><json:string>Israeli Science Foundation</json:string><json:string>California Institute of Technology, the University of California</json:string><json:string>University of Hawaii</json:string><json:string>Liverpool John Moores University</json:string><json:string>Keck Foundation</json:string><json:string>Cahill Center for Astrophysics</json:string><json:string>BSF</json:string><json:string>Jet Propulsion Laboratory, California Institute of Technology</json:string><json:string>Weizmann Institute of Science, Rehovot</json:string><json:string>Dunlap Institute for Astronomy and Astrophysics</json:string><json:string>Binational Science Foundation</json:string><json:string>Department of Physics, University of California</json:string><json:string>ISF</json:string><json:string>National Aeronautics and Space</json:string><json:string>Computing Center</json:string><json:string>UK Science and Technology</json:string><json:string>RH Cosmology Center</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>Sky Survey</json:string><json:string>Robert Hubbard</json:string><json:string>S. R. Kulkarni</json:string><json:string>S. Ellis</json:string><json:string>D. A. Howell</json:string><json:string>C. Pan</json:string><json:string>Sarah Zahorchak</json:string><json:string>E. O. Ofek</json:string><json:string>Giovanni Iezzi</json:string><json:string>Henryk Krawczyk</json:string><json:string>A. Gal-Yam</json:string><json:string>S. B. Cenko</json:string><json:string>La Palma</json:string><json:string>Julian Date</json:string><json:string>Cynthia Bengier</json:string><json:string>Marie Curie</json:string><json:string>The</json:string><json:string>P. Nugent</json:string><json:string>R. M. Quimby</json:string><json:string>D. Xu</json:string><json:string>I. M. Hook</json:string><json:string>S. Bloom</json:string><json:string>D. Poznanski</json:string><json:string>S. Blake</json:string><json:string>Samuel Oschin</json:string><json:string>M. Kasliwal</json:string><json:string>I. Arcavi</json:string><json:string>S. Ben-Ami</json:string><json:string>K. Maguire</json:string><json:string>Elisabeth Baeten</json:string><json:string>Graham Dungworth</json:string><json:string>A. Sternberg</json:string><json:string>George Street</json:string><json:string>P. Podsiadlowski</json:string><json:string>C. Thomas</json:string></persName><placeName><json:string>Germany</json:string><json:string>Santa Barbara</json:string><json:string>Australia</json:string><json:string>Bonn</json:string><json:string>Metallicity</json:string><json:string>UK</json:string><json:string>Canada</json:string><json:string>Melbourne</json:string><json:string>Toronto</json:string><json:string>Frascati</json:string><json:string>Liverpool</json:string><json:string>CA</json:string><json:string>Israel</json:string><json:string>Velocity</json:string><json:string>France</json:string><json:string>Cortona</json:string><json:string>Marseille</json:string><json:string>Italy</json:string><json:string>Lyon</json:string><json:string>Los Muchachos</json:string><json:string>Las Cumbres</json:string></placeName><ref_url><json:string>http://www.lbl.gov/</json:string><json:string>http://supernova.galaxyzoo.org/authors</json:string><json:string>http://www.weizmann.ac.il/ astrophysics/wiseass</json:string></ref_url><ref_bibl><json:string>Foley et al. 2010</json:string><json:string>Filippenko et al. 1992</json:string><json:string>Conley et al. 2008</json:string><json:string>Taubenberger et al. (2008)</json:string><json:string>Arcavi et al. (2010)</json:string><json:string>Hammer et al. 2007</json:string><json:string>Perlmutter et al. 1999</json:string><json:string>K. Maguire et al.</json:string><json:string>Pskovskii (1984)</json:string><json:string>Strolger, Smith & Suntzeff 2002</json:string><json:string>Arnett 1982</json:string><json:string>Howell et al. (2009)</json:string><json:string>Schlegel et al. (1998)</json:string><json:string>Nugent et al. (1995b)</json:string><json:string>Oke et al. 1995</json:string><json:string>Perets et al. 2010</json:string><json:string>Schlegel, Finkbeiner & Davis 1998</json:string><json:string>Rau et al. 2009</json:string><json:string>Hsiao et al. (2007)</json:string><json:string>Kalirai et al. 2006</json:string><json:string>Kasliwal et al. (2008)</json:string><json:string>Hayden et al. 2010</json:string><json:string>Sullivan et al. 2010</json:string><json:string>Stanishev et al. 2007</json:string><json:string>Riess et al. 1998, 2007</json:string><json:string>Hicken et al. (2009)</json:string><json:string>Martin et al. 2006</json:string><json:string>Kessler et al. 2009</json:string><json:string>Foley et al. (2010)</json:string><json:string>Richmond et al. 1995</json:string><json:string>Sullivan et al. 2011b</json:string><json:string>Kasliwal et al.</json:string><json:string>Benetti et al. (2005)</json:string><json:string>Howell 2001</json:string><json:string>Fisher 2000</json:string><json:string>Nugent et al. 1995b</json:string><json:string>Sullivan et al. (2011a)</json:string><json:string>Rosswog et al. 2009</json:string><json:string>Garnavich et al. 2004</json:string><json:string>Kasliwal et al. 2010</json:string><json:string>Taubenberger et al. 2008</json:string><json:string>Riess et al. (1999)</json:string><json:string>Sullivan et al. 2011a</json:string><json:string>Poznanski et al. 2011</json:string><json:string>Nugent et al. 1995a</json:string><json:string>Oke & Gunn 1983</json:string><json:string>Thomas, Nugent & Meza 2011</json:string><json:string>Dan et al. (2011)</json:string><json:string>Cooke et al. 2011</json:string><json:string>Pakmor et al. (2010)</json:string><json:string>Sullivan et al. (2010)</json:string><json:string>Gallagher et al. 2005</json:string><json:string>Leibundgut et al. 1993</json:string><json:string>2006, 2009</json:string><json:string>Lantz et al. 2004</json:string><json:string>Richardson et al. 2011</json:string><json:string>Law et al. 2009</json:string><json:string>Branch et al. (2009)</json:string><json:string>York et al. 2000</json:string><json:string>Phillips et al. (1987)</json:string><json:string>Smith et al. 2011</json:string><json:string>Howell et al. 2005</json:string><json:string>Nugent, Kim & Perlmutter 2002</json:string><json:string>Miller & Stone 1993</json:string><json:string>Pakmor et al. 2010</json:string><json:string>Nugent et al. (1995a)</json:string><json:string>Perets et al. (2010)</json:string><json:string>van den Bergh 1991</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-9VKHV5ZQ-Z</json:string></ark><categories><wos><json:string>1 - science</json:string><json:string>2 - astronomy & astrophysics</json:string></wos><scienceMetrix><json:string>1 - natural sciences</json:string><json:string>2 - physics & astronomy</json:string><json:string>3 - astronomy & astrophysics</json:string></scienceMetrix><scopus><json:string>1 - Physical Sciences</json:string><json:string>2 - Earth and Planetary Sciences</json:string><json:string>3 - Space and Planetary Science</json:string><json:string>1 - Physical Sciences</json:string><json:string>2 - Physics and Astronomy</json:string><json:string>3 - Astronomy and Astrophysics</json:string></scopus><inist><json:string>1 - sciences appliquees, technologies et medecines</json:string><json:string>2 - sciences biologiques et medicales</json:string><json:string>3 - sciences biologiques fondamentales et appliquees. psychologie</json:string></inist></categories><publicationDate>2011</publicationDate><copyrightDate>2011</copyrightDate><doi><json:string>10.1111/j.1365-2966.2011.19526.x</json:string></doi><id>EF4AA392C829B78146F1F0FCD6D4E82C0261078B</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/EF4AA392C829B78146F1F0FCD6D4E82C0261078B/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/EF4AA392C829B78146F1F0FCD6D4E82C0261078B/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/EF4AA392C829B78146F1F0FCD6D4E82C0261078B/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">PTF10ops – a subluminous, normal‐width light curve Type Ia supernova in the middle of nowhere</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><availability><licence>© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</licence></availability><date type="published" when="2011-12-01"></date></publicationStmt><notesStmt><note type="content-type" subtype="article" source="article" scheme="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</note><note type="publication-type" subtype="journal" scheme="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</note></notesStmt><sourceDesc><biblStruct type="article"><analytic><title level="a" type="main">PTF10ops – a subluminous, normal‐width light curve Type Ia supernova in the middle of nowhere</title><title level="a" type="short">PTF10ops: A subluminous, normal‐width SN Ia</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">K.</forename><surname>Maguire</surname></persName><affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</affiliation><affiliation>E‐mail: kate.maguire@astro.ox.ac.uk</affiliation></author><author xml:id="author-0001"><persName><forename type="first">M.</forename><surname>Sullivan</surname></persName><affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</affiliation></author><author xml:id="author-0002"><persName><forename type="first">R. C.</forename><surname>Thomas</surname></persName><affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA<address><country key="US"></country></address></affiliation><affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0003"><persName><forename type="first">P.</forename><surname>Nugent</surname></persName><affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA<address><country key="US"></country></address></affiliation><affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0004"><persName><forename type="first">D. A.</forename><surname>Howell</surname></persName><affiliation>Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117, USA<address><country key="US"></country></address></affiliation><affiliation>Department of Physics, University of California at Santa Barbara, Santa Barbara, CA 93196, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0005"><persName><forename type="first">A.</forename><surname>Gal‐Yam</surname></persName><affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel<address><country key="IL"></country></address></affiliation></author><author xml:id="author-0006"><persName><forename type="first">I.</forename><surname>Arcavi</surname></persName><affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel<address><country key="IL"></country></address></affiliation></author><author xml:id="author-0007"><persName><forename type="first">S.</forename><surname>Ben‐Ami</surname></persName><affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel<address><country key="IL"></country></address></affiliation></author><author xml:id="author-0008"><persName><forename type="first">S.</forename><surname>Blake</surname></persName><affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</affiliation></author><author xml:id="author-0009"><persName><forename type="first">J.</forename><surname>Botyanszki</surname></persName><affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA<address><country key="US"></country></address></affiliation><affiliation>Department of Physics, University of California, Berkeley, CA 94720‐3411, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0010"><persName><forename type="first">C.</forename><surname>Buton</surname></persName><affiliation>Physikalisches Institut Universitat Bonn, Nussallee 12 53115 Bonn, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0011"><persName><forename type="first">J.</forename><surname>Cooke</surname></persName><affiliation>Swinburne University of Technology, Melbourne, Victoria 3122, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0012"><persName><forename type="first">R. S.</forename><surname>Ellis</surname></persName><affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0013"><persName><forename type="first">I. M.</forename><surname>Hook</surname></persName><affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</affiliation><affiliation>INAF – Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0014"><persName><forename type="first">M. M.</forename><surname>Kasliwal</surname></persName><affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0015"><persName><forename type="first">Y.‐C.</forename><surname>Pan</surname></persName><affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</affiliation></author><author xml:id="author-0016"><persName><forename type="first">R.</forename><surname>Pereira</surname></persName><affiliation>Université de Lyon, F‐69622 France; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0017"><persName><forename type="first">P.</forename><surname>Podsiadlowski</surname></persName><affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</affiliation></author><author xml:id="author-0018"><persName><forename type="first">A.</forename><surname>Sternberg</surname></persName><affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel<address><country key="IL"></country></address></affiliation></author><author xml:id="author-0019"><persName><forename type="first">N.</forename><surname>Suzuki</surname></persName><affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0020"><persName><forename type="first">D.</forename><surname>Xu</surname></persName><affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel<address><country key="IL"></country></address></affiliation></author><author xml:id="author-0021"><persName><forename type="first">O.</forename><surname>Yaron</surname></persName><affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel<address><country key="IL"></country></address></affiliation></author><author xml:id="author-0022"><persName><forename type="first">J. S.</forename><surname>Bloom</surname></persName><affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0023"><persName><forename type="first">S. B.</forename><surname>Cenko</surname></persName><affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0024"><persName><forename type="first">S. R.</forename><surname>Kulkarni</surname></persName><affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0025"><persName><forename type="first">N.</forename><surname>Law</surname></persName><affiliation>Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto M5S 3H4, Ontario, Canada<address><country key="CA"></country></address></affiliation></author><author xml:id="author-0026"><persName><forename type="first">E. O.</forename><surname>Ofek</surname></persName><affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0027"><persName><forename type="first">D.</forename><surname>Poznanski</surname></persName><affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA<address><country key="US"></country></address></affiliation><affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0028"><persName><forename type="first">R. M.</forename><surname>Quimby</surname></persName><affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA<address><country key="US"></country></address></affiliation></author><idno type="istex">EF4AA392C829B78146F1F0FCD6D4E82C0261078B</idno><idno type="ark">ark:/67375/WNG-9VKHV5ZQ-Z</idno><idno type="DOI">10.1111/j.1365-2966.2011.19526.x</idno><idno type="unit">MNR19526</idno><idno type="toTypesetVersion">file:MNR.MNR19526.pdf</idno></analytic><monogr><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="pISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><idno type="book-DOI">10.1111/(ISSN)1365-2966</idno><idno type="book-part-DOI">10.1111/mnr.2011.418.issue-2</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">418</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="747">747</biblScope><biblScope unit="page" to="758">758</biblScope><biblScope unit="page-count">12</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2011-12-01"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>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 <hi rend="italic">r</hi>≥−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.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">supernovae: general</term><term xml:id="k2">supernovae: individual: PTF10ops</term></keywords><keywords rend="tocHeading1"><term>Papers</term></keywords></textClass><langUsage><language ident="en"></language></langUsage></profileDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/EF4AA392C829B78146F1F0FCD6D4E82C0261078B/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration><istex:document><component version="2.0" type="serialArticle" xml:lang="en"><header><publicationMeta level="product"><publisherInfo><publisherName>Blackwell Publishing Ltd</publisherName><publisherLoc>Oxford, UK</publisherLoc></publisherInfo><doi origin="wiley" registered="yes">10.1111/(ISSN)1365-2966</doi><issn type="print">0035-8711</issn><issn type="electronic">1365-2966</issn><idGroup><id type="product" value="MNR"></id><id type="publisherDivision" value="ST"></id></idGroup><titleGroup><title type="main" sort="MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY">Monthly Notices of the Royal Astronomical Society</title></titleGroup></publicationMeta><publicationMeta level="part" position="12102"><doi origin="wiley">10.1111/mnr.2011.418.issue-2</doi><numberingGroup><numbering type="journalVolume" number="418">418</numbering><numbering type="journalIssue" number="2">2</numbering></numberingGroup><coverDate startDate="2011-12-01">December 2011</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="3" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2011.19526.x</doi><idGroup><id type="unit" value="MNR19526"></id></idGroup><countGroup><count type="pageTotal" number="12"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><copyright>© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</copyright><eventGroup><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:3.0 mode:FullText" date="2011-11-16"></event><event type="publishedOnlineEarlyUnpaginated" date="2011-09-26"></event><event type="firstOnline" date="2011-09-26"></event><event type="publishedOnlineFinalForm" date="2011-11-16"></event><event type="xmlConverted" agent="Converter:WILEY_ML3G_TO_WILEY_ML3GV2 version:3.8.8" date="2014-02-03"></event><event type="xmlConverted" agent="Converter:WML3G_To_WML3G version:4.1.7 mode:FullText,remove_FC" date="2014-10-31"></event></eventGroup><numberingGroup><numbering type="pageFirst" number="747">747</numbering><numbering type="pageLast" number="758">758</numbering></numberingGroup><correspondenceTo>
E‐mail: <email>kate.maguire@astro.ox.ac.uk</email></correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR19526.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2011 July 27. Received 2011 July 27; in original form 2011 July 13</unparsedEditorialHistory><countGroup><count type="figureTotal" number="9"></count><count type="tableTotal" number="4"></count><count type="formulaTotal" number="24"></count><count type="referenceTotal" number="66"></count><count type="linksCrossRef" number="162"></count></countGroup><titleGroup><title type="main">PTF10ops – a subluminous, normal‐width light curve Type Ia supernova in the middle of nowhere</title><title type="shortAuthors"><i>K. Maguire et al.</i></title><title type="short"><i>PTF10ops: A subluminous, normal‐width SN Ia</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>K.</givenNames><familyName>Maguire</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a1"><personName><givenNames>M.</givenNames><familyName>Sullivan</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a2 #a3"><personName><givenNames>R. C.</givenNames><familyName>Thomas</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a2 #a3"><personName><givenNames>P.</givenNames><familyName>Nugent</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a4 #a5"><personName><givenNames>D. 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S.</givenNames><familyName>Bloom</familyName></personName></creator><creator creatorRole="author" xml:id="cr24" affiliationRef="#a3"><personName><givenNames>S. B.</givenNames><familyName>Cenko</familyName></personName></creator><creator creatorRole="author" xml:id="cr25" affiliationRef="#a10"><personName><givenNames>S. R.</givenNames><familyName>Kulkarni</familyName></personName></creator><creator creatorRole="author" xml:id="cr26" affiliationRef="#a13"><personName><givenNames>N.</givenNames><familyName>Law</familyName></personName></creator><creator creatorRole="author" xml:id="cr27" affiliationRef="#a10"><personName><givenNames>E. O.</givenNames><familyName>Ofek</familyName></personName></creator><creator creatorRole="author" xml:id="cr28" affiliationRef="#a2 #a3"><personName><givenNames>D.</givenNames><familyName>Poznanski</familyName></personName></creator><creator creatorRole="author" xml:id="cr29" affiliationRef="#a10"><personName><givenNames>R. M.</givenNames><familyName>Quimby</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1"><unparsedAffiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="US"><unparsedAffiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="US"><unparsedAffiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="US"><unparsedAffiliation>Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117, USA</unparsedAffiliation></affiliation><affiliation xml:id="a5" countryCode="US"><unparsedAffiliation>Department of Physics, University of California at Santa Barbara, Santa Barbara, CA 93196, USA</unparsedAffiliation></affiliation><affiliation xml:id="a6" countryCode="IL"><unparsedAffiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</unparsedAffiliation></affiliation><affiliation xml:id="a7" countryCode="US"><unparsedAffiliation>Department of Physics, University of California, Berkeley, CA 94720‐3411, USA</unparsedAffiliation></affiliation><affiliation xml:id="a8" countryCode="DE"><unparsedAffiliation>Physikalisches Institut Universitat Bonn, Nussallee 12 53115 Bonn, Germany</unparsedAffiliation></affiliation><affiliation xml:id="a9" countryCode="AU"><unparsedAffiliation>Swinburne University of Technology, Melbourne, Victoria 3122, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a10" countryCode="US"><unparsedAffiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</unparsedAffiliation></affiliation><affiliation xml:id="a11" countryCode="IT"><unparsedAffiliation>INAF – Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy</unparsedAffiliation></affiliation><affiliation xml:id="a12" countryCode="FR"><unparsedAffiliation>Université de Lyon, F‐69622 France; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, France</unparsedAffiliation></affiliation><affiliation xml:id="a13" countryCode="CA"><unparsedAffiliation>Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto M5S 3H4, Ontario, Canada</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">supernovae: general</keyword><keyword xml:id="k2">supernovae: individual: PTF10ops</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>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 <i>r</i>≥−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.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>PTF10ops – a subluminous, normal‐width light curve Type Ia supernova in the middle of nowhere</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>PTF10ops: A subluminous, normal‐width SN Ia</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>PTF10ops – a subluminous, normal‐width light curve Type Ia supernova in the middle of nowhere</title></titleInfo><name type="personal"><namePart type="given">K.</namePart><namePart type="family">Maguire</namePart><affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</affiliation><affiliation>E-mail: kate.maguire@astro.ox.ac.uk</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Sullivan</namePart><affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. C.</namePart><namePart type="family">Thomas</namePart><affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</affiliation><affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">P.</namePart><namePart type="family">Nugent</namePart><affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</affiliation><affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D. A.</namePart><namePart type="family">Howell</namePart><affiliation>Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117, USA</affiliation><affiliation>Department of Physics, University of California at Santa Barbara, Santa Barbara, CA 93196, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Gal‐Yam</namePart><affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">I.</namePart><namePart type="family">Arcavi</namePart><affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S.</namePart><namePart type="family">Ben‐Ami</namePart><affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S.</namePart><namePart type="family">Blake</namePart><affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Botyanszki</namePart><affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</affiliation><affiliation>Department of Physics, University of California, Berkeley, CA 94720‐3411, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">C.</namePart><namePart type="family">Buton</namePart><affiliation>Physikalisches Institut Universitat Bonn, Nussallee 12 53115 Bonn, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Cooke</namePart><affiliation>Swinburne University of Technology, Melbourne, Victoria 3122, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. S.</namePart><namePart type="family">Ellis</namePart><affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">I. M.</namePart><namePart type="family">Hook</namePart><affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</affiliation><affiliation>INAF – Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M. M.</namePart><namePart type="family">Kasliwal</namePart><affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Y.‐C.</namePart><namePart type="family">Pan</namePart><affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R.</namePart><namePart type="family">Pereira</namePart><affiliation>Université de Lyon, F‐69622 France; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">P.</namePart><namePart type="family">Podsiadlowski</namePart><affiliation>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Sternberg</namePart><affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">N.</namePart><namePart type="family">Suzuki</namePart><affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="family">Xu</namePart><affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">O.</namePart><namePart type="family">Yaron</namePart><affiliation>Department of Particle Physics and Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J. S.</namePart><namePart type="family">Bloom</namePart><affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S. B.</namePart><namePart type="family">Cenko</namePart><affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S. R.</namePart><namePart type="family">Kulkarni</namePart><affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">N.</namePart><namePart type="family">Law</namePart><affiliation>Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St George Street, Toronto M5S 3H4, Ontario, Canada</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">E. O.</namePart><namePart type="family">Ofek</namePart><affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="family">Poznanski</namePart><affiliation>Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Rd., Berkeley, CA 94720, USA</affiliation><affiliation>Department of Astronomy, University of California, Berkeley, CA 94720‐3411, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. M.</namePart><namePart type="family">Quimby</namePart><affiliation>Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article" authority="ISTEX" authorityURI="https://content-type.data.istex.fr" valueURI="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2011-12-01</dateIssued><edition>Accepted 2011 July 27. Received 2011 July 27; in original form 2011 July 13</edition><copyrightDate encoding="w3cdtf">2011</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">9</extent><extent unit="tables">4</extent><extent unit="formulas">24</extent><extent unit="references">66</extent><extent unit="linksCrossRef">162</extent></physicalDescription><abstract lang="en">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.</abstract><subject lang="en"><genre>keywords</genre><topic>supernovae: general</topic><topic>supernovae: individual: PTF10ops</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre><identifier type="ISSN">0035-8711</identifier><identifier type="eISSN">1365-2966</identifier><identifier type="DOI">10.1111/(ISSN)1365-2966</identifier><identifier type="PublisherID">MNR</identifier><part><date>2011</date><detail type="volume"><caption>vol.</caption><number>418</number></detail><detail type="issue"><caption>no.</caption><number>2</number></detail><extent unit="pages"><start>747</start><end>758</end><total>12</total></extent></part></relatedItem><identifier type="istex">EF4AA392C829B78146F1F0FCD6D4E82C0261078B</identifier><identifier type="ark">ark:/67375/WNG-9VKHV5ZQ-Z</identifier><identifier type="DOI">10.1111/j.1365-2966.2011.19526.x</identifier><identifier type="ArticleID">MNR19526</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</accessCondition><recordInfo><recordContentSource authority="ISTEX" authorityURI="https://loaded-corpus.data.istex.fr" valueURI="https://loaded-corpus.data.istex.fr/ark:/67375/XBH-L0C46X92-X">wiley</recordContentSource><recordOrigin>Blackwell Publishing Ltd</recordOrigin></recordInfo></mods><json:item><extension>json</extension><original>false</original><mimetype>application/json</mimetype><uri>https://api.istex.fr/document/EF4AA392C829B78146F1F0FCD6D4E82C0261078B/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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