AustralieFrV1, Main, Exploration, bibRecord, 005866

THE RISE TIME OF NORMAL AND SUBLUMINOUS TYPE Ia SUPERNOVAE

Identifieur interne : 005866 ( Main/Exploration ); précédent : 005865; suivant : 005867

THE RISE TIME OF NORMAL AND SUBLUMINOUS TYPE Ia SUPERNOVAE

Auteurs : S. Gonzalez-Gaitan [Canada] ; A. Conley [États-Unis] ; F. B. Bianco [États-Unis] ; D. A. Howell [États-Unis] ; M. Sullivan [Royaume-Uni] ; K. Perrett [Canada] ; R. Carlberg [Canada] ; P. Astier [France] ; D. Balam [Canada] ; C. Balland [France] ; S. Basa [France] ; D. Fouchez [France] ; N. Fourmanoit [France] ; M. L. Graham [États-Unis, Canada] ; J. Guy [France] ; D. Hardin [France] ; I. M. Hook [Royaume-Uni, Italie] ; C. Lidman [Australie] ; R. Pain [France] ; N. Palanque-Delabrouille [France] ; C. J. Pritchet [Canada] ; N. Regnault [France] ; J. Rich [France] ; V. Ruhlmann-Kleider [France]

Source :

The Astrophysical journal [ 0004-637X ] ; 2012.

RBID : Pascal:12-0088502

Descripteurs français

Pascal (Inist)
- Supernova type I, Courbe lumière, Modèle, Paramétrisation.

English descriptors

KwdEn :
- Light curves, Models, Parameterization, Type I supernova.

Abstract

We calculate the average stretch-corrected rise time of Type Ia supernovae (SNe Ia) in the Supernova Legacy Survey. We use the aggregate light curves of spectroscopic and photometrically identified SNe Ia to fit the rising part of the light curve with a simple quadratic model. We obtain a light curve shape corrected, i.e., stretch-corrected, fiducial rise time of 17.02^+0.18_-0.28(stat) days. The measured rise time differs from an earlier finding by the SNLS (Conley et al.) due to the use of different SN Ia templates. We compare it to nearby samples using the same methods and find no evolution in the early part of the light curve of SNe Ia up to z = 1. We search for variations among different populations, particularly subluminous objects, by dividing the sample in stretch. Bright and slow decliners (s > 1.0) have consistent stretch-corrected rise times compared to fainter and faster decliners (0.8 < s ≤ 1.0); they are shorter by 0.57^+0.47_-0.50(stat) days. Subluminous SNe Ia (here defined as objects with s < 0.8), although less constrained, are also consistent, with a rise time of 18.03^+0.81_-1.37(stat) days. We study several systematic biases and find that the use of different fiducial templates may affect the average rise time but not the intrinsic differences between populations. Based on our results, we estimate that subluminous SNe Ia are powered by 0.05-0.35 M_◦. of ⁵⁶Ni synthesized in the explosion. Our conclusions are the same for the single-stretch and two-stretch parameterizations of the light curve.

Affiliations:

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Le document en format XML

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<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">THE RISE TIME OF NORMAL AND SUBLUMINOUS TYPE Ia SUPERNOVAE</title>
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<sZ>1 aut.</sZ>
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<orgName type="university">Université de Toronto</orgName>
<placeName><settlement type="city">Toronto</settlement>
<region type="state">Ontario</region>
</placeName>
</affiliation>
</author>
<author><name sortKey="Conley, A" sort="Conley, A" uniqKey="Conley A" first="A." last="Conley">A. Conley</name>
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<affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Department of Physics, University of California, Santa Barbara, Broida Hall, Mail Code 9530</s1>
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<author><name sortKey="Sullivan, M" sort="Sullivan, M" uniqKey="Sullivan M" first="M." last="Sullivan">M. Sullivan</name>
<affiliation wicri:level="4"><inist:fA14 i1="05"><s1>Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road</s1>
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<sZ>1 aut.</sZ>
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<author><name sortKey="Carlberg, R" sort="Carlberg, R" uniqKey="Carlberg R" first="R." last="Carlberg">R. Carlberg</name>
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<sZ>1 aut.</sZ>
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<author><name sortKey="Astier, P" sort="Astier, P" uniqKey="Astier P" first="P." last="Astier">P. Astier</name>
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<author><name sortKey="Balam, D" sort="Balam, D" uniqKey="Balam D" first="D." last="Balam">D. Balam</name>
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<sZ>9 aut.</sZ>
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<author><name sortKey="Balland, C" sort="Balland, C" uniqKey="Balland C" first="C." last="Balland">C. Balland</name>
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<country>France</country>
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<affiliation wicri:level="4"><inist:fA14 i1="09"><s1>Université Paris 11</s1>
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<country>France</country>
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<author><name sortKey="Basa, S" sort="Basa, S" uniqKey="Basa S" first="S." last="Basa">S. Basa</name>
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<author><name sortKey="Fouchez, D" sort="Fouchez, D" uniqKey="Fouchez D" first="D." last="Fouchez">D. Fouchez</name>
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<author><name sortKey="Fourmanoit, N" sort="Fourmanoit, N" uniqKey="Fourmanoit N" first="N." last="Fourmanoit">N. Fourmanoit</name>
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<author><name sortKey="Graham, M L" sort="Graham, M L" uniqKey="Graham M" first="M. L." last="Graham">M. L. Graham</name>
<affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Department of Physics, University of California, Santa Barbara, Broida Hall, Mail Code 9530</s1>
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<affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Department of Physics & Astronomy, University of Victoria, P.O. Box 3055, Stn CSC</s1>
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<sZ>14 aut.</sZ>
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<author><name sortKey="Guy, J" sort="Guy, J" uniqKey="Guy J" first="J." last="Guy">J. Guy</name>
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<author><name sortKey="Hook, I M" sort="Hook, I M" uniqKey="Hook I" first="I. M." last="Hook">I. M. Hook</name>
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<sZ>5 aut.</sZ>
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<orgName type="university">Université d'Oxford</orgName>
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<author><name sortKey="Lidman, C" sort="Lidman, C" uniqKey="Lidman C" first="C." last="Lidman">C. Lidman</name>
<affiliation wicri:level="1"><inist:fA14 i1="14"><s1>Australian Astronomical Observatory, P.O. Box 296, Epping</s1>
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<author><name sortKey="Pain, R" sort="Pain, R" uniqKey="Pain R" first="R." last="Pain">R. Pain</name>
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<author><name sortKey="Palanque Delabrouille, N" sort="Palanque Delabrouille, N" uniqKey="Palanque Delabrouille N" first="N." last="Palanque-Delabrouille">N. Palanque-Delabrouille</name>
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<author><name sortKey="Pritchet, C J" sort="Pritchet, C J" uniqKey="Pritchet C" first="C. J." last="Pritchet">C. J. Pritchet</name>
<affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Department of Physics & Astronomy, University of Victoria, P.O. Box 3055, Stn CSC</s1>
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<s3>CAN</s3>
<sZ>14 aut.</sZ>
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<author><name sortKey="Regnault, N" sort="Regnault, N" uniqKey="Regnault N" first="N." last="Regnault">N. Regnault</name>
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<author><name sortKey="Rich, J" sort="Rich, J" uniqKey="Rich J" first="J." last="Rich">J. Rich</name>
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<sZ>20 aut.</sZ>
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<author><name sortKey="Ruhlmann Kleider, V" sort="Ruhlmann Kleider, V" uniqKey="Ruhlmann Kleider V" first="V." last="Ruhlmann-Kleider">V. Ruhlmann-Kleider</name>
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<series><title level="j" type="main">The Astrophysical journal</title>
<title level="j" type="abbreviated">Astrophys. j.</title>
<idno type="ISSN">0004-637X</idno>
<imprint><date when="2012">2012</date>
</imprint>
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</sourceDesc>
<seriesStmt><title level="j" type="main">The Astrophysical journal</title>
<title level="j" type="abbreviated">Astrophys. j.</title>
<idno type="ISSN">0004-637X</idno>
</seriesStmt>
</fileDesc>
<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Light curves</term>
<term>Models</term>
<term>Parameterization</term>
<term>Type I supernova</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Supernova type I</term>
<term>Courbe lumière</term>
<term>Modèle</term>
<term>Paramétrisation</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">We calculate the average stretch-corrected rise time of Type Ia supernovae (SNe Ia) in the Supernova Legacy Survey. We use the aggregate light curves of spectroscopic and photometrically identified SNe Ia to fit the rising part of the light curve with a simple quadratic model. We obtain a light curve shape corrected, i.e., stretch-corrected, fiducial rise time of 17.02<sup>+0.18</sup>
<sub>-0.28 </sub>
(stat) days. The measured rise time differs from an earlier finding by the SNLS (Conley et al.) due to the use of different SN Ia templates. We compare it to nearby samples using the same methods and find no evolution in the early part of the light curve of SNe Ia up to z = 1. We search for variations among different populations, particularly subluminous objects, by dividing the sample in stretch. Bright and slow decliners (s > 1.0) have consistent stretch-corrected rise times compared to fainter and faster decliners (0.8 < s ≤ 1.0); they are shorter by 0.57<sup>+0.47</sup>
<sub>-0.50 </sub>
(stat) days. Subluminous SNe Ia (here defined as objects with s < 0.8), although less constrained, are also consistent, with a rise time of 18.03<sup>+0.81</sup>
<sub>-1.37 </sub>
(stat) days. We study several systematic biases and find that the use of different fiducial templates may affect the average rise time but not the intrinsic differences between populations. Based on our results, we estimate that subluminous SNe Ia are powered by 0.05-0.35 M<sub>◦.</sub>
 of <sup>56</sup>
Ni synthesized in the explosion. Our conclusions are the same for the single-stretch and two-stretch parameterizations of the light curve.</div>
</front>
</TEI>
<affiliations><list><country><li>Australie</li>
<li>Canada</li>
<li>France</li>
<li>Italie</li>
<li>Royaume-Uni</li>
<li>États-Unis</li>
</country>
<region><li>Angleterre</li>
<li>Ontario</li>
<li>Oxfordshire</li>
<li>Provence-Alpes-Côte d'Azur</li>
<li>Île-de-France</li>
</region>
<settlement><li>Marseille</li>
<li>Orsay</li>
<li>Oxford</li>
<li>Paris</li>
<li>Toronto</li>
</settlement>
<orgName><li>Université Paris-Sud</li>
<li>Université d'Oxford</li>
<li>Université de Toronto</li>
</orgName>
</list>
<tree><country name="Canada"><region name="Ontario"><name sortKey="Gonzalez Gaitan, S" sort="Gonzalez Gaitan, S" uniqKey="Gonzalez Gaitan S" first="S." last="Gonzalez-Gaitan">S. Gonzalez-Gaitan</name>
</region>
<name sortKey="Balam, D" sort="Balam, D" uniqKey="Balam D" first="D." last="Balam">D. Balam</name>
<name sortKey="Carlberg, R" sort="Carlberg, R" uniqKey="Carlberg R" first="R." last="Carlberg">R. Carlberg</name>
<name sortKey="Graham, M L" sort="Graham, M L" uniqKey="Graham M" first="M. L." last="Graham">M. L. Graham</name>
<name sortKey="Perrett, K" sort="Perrett, K" uniqKey="Perrett K" first="K." last="Perrett">K. Perrett</name>
<name sortKey="Perrett, K" sort="Perrett, K" uniqKey="Perrett K" first="K." last="Perrett">K. Perrett</name>
<name sortKey="Pritchet, C J" sort="Pritchet, C J" uniqKey="Pritchet C" first="C. J." last="Pritchet">C. J. Pritchet</name>
</country>
<country name="États-Unis"><noRegion><name sortKey="Conley, A" sort="Conley, A" uniqKey="Conley A" first="A." last="Conley">A. Conley</name>
</noRegion>
<name sortKey="Bianco, F B" sort="Bianco, F B" uniqKey="Bianco F" first="F. B." last="Bianco">F. B. Bianco</name>
<name sortKey="Bianco, F B" sort="Bianco, F B" uniqKey="Bianco F" first="F. B." last="Bianco">F. B. Bianco</name>
<name sortKey="Graham, M L" sort="Graham, M L" uniqKey="Graham M" first="M. L." last="Graham">M. L. Graham</name>
<name sortKey="Howell, D A" sort="Howell, D A" uniqKey="Howell D" first="D. A." last="Howell">D. A. Howell</name>
<name sortKey="Howell, D A" sort="Howell, D A" uniqKey="Howell D" first="D. A." last="Howell">D. A. Howell</name>
</country>
<country name="Royaume-Uni"><region name="Angleterre"><name sortKey="Sullivan, M" sort="Sullivan, M" uniqKey="Sullivan M" first="M." last="Sullivan">M. Sullivan</name>
</region>
<name sortKey="Hook, I M" sort="Hook, I M" uniqKey="Hook I" first="I. M." last="Hook">I. M. Hook</name>
</country>
<country name="France"><region name="Île-de-France"><name sortKey="Astier, P" sort="Astier, P" uniqKey="Astier P" first="P." last="Astier">P. Astier</name>
</region>
<name sortKey="Balland, C" sort="Balland, C" uniqKey="Balland C" first="C." last="Balland">C. Balland</name>
<name sortKey="Balland, C" sort="Balland, C" uniqKey="Balland C" first="C." last="Balland">C. Balland</name>
<name sortKey="Basa, S" sort="Basa, S" uniqKey="Basa S" first="S." last="Basa">S. Basa</name>
<name sortKey="Fouchez, D" sort="Fouchez, D" uniqKey="Fouchez D" first="D." last="Fouchez">D. Fouchez</name>
<name sortKey="Fourmanoit, N" sort="Fourmanoit, N" uniqKey="Fourmanoit N" first="N." last="Fourmanoit">N. Fourmanoit</name>
<name sortKey="Guy, J" sort="Guy, J" uniqKey="Guy J" first="J." last="Guy">J. Guy</name>
<name sortKey="Hardin, D" sort="Hardin, D" uniqKey="Hardin D" first="D." last="Hardin">D. Hardin</name>
<name sortKey="Pain, R" sort="Pain, R" uniqKey="Pain R" first="R." last="Pain">R. Pain</name>
<name sortKey="Palanque Delabrouille, N" sort="Palanque Delabrouille, N" uniqKey="Palanque Delabrouille N" first="N." last="Palanque-Delabrouille">N. Palanque-Delabrouille</name>
<name sortKey="Regnault, N" sort="Regnault, N" uniqKey="Regnault N" first="N." last="Regnault">N. Regnault</name>
<name sortKey="Rich, J" sort="Rich, J" uniqKey="Rich J" first="J." last="Rich">J. Rich</name>
<name sortKey="Ruhlmann Kleider, V" sort="Ruhlmann Kleider, V" uniqKey="Ruhlmann Kleider V" first="V." last="Ruhlmann-Kleider">V. Ruhlmann-Kleider</name>
</country>
<country name="Italie"><noRegion><name sortKey="Hook, I M" sort="Hook, I M" uniqKey="Hook I" first="I. M." last="Hook">I. M. Hook</name>
</noRegion>
</country>
<country name="Australie"><noRegion><name sortKey="Lidman, C" sort="Lidman, C" uniqKey="Lidman C" first="C." last="Lidman">C. Lidman</name>
</noRegion>
</country>
</tree>
</affiliations>
</record>

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THE RISE TIME OF NORMAL AND SUBLUMINOUS TYPE Ia SUPERNOVAE

THE RISE TIME OF NORMAL AND SUBLUMINOUS TYPE Ia SUPERNOVAE

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