TYPE Ia SUPERNOVA CARBON FOOTPRINTS
Identifieur interne : 001697 ( PascalFrancis/Corpus ); précédent : 001696; suivant : 001698TYPE Ia SUPERNOVA CARBON FOOTPRINTS
Auteurs : R. C. Thomas ; G. Aldering ; P. Antilogus ; C. Aragon ; S. Bailey ; C. Baltay ; S. Bongard ; C. Buton ; A. Canto ; M. Childress ; N. Chotard ; Y. Copin ; H. K. Fakhouri ; E. Gangler ; E. Y. Hsiao ; M. Kerschhaggl ; M. Kowalski ; S. Loken ; P. Nugent ; K. Paech ; R. Pain ; E. Pecontal ; R. Pereira ; S. Perlmutter ; D. Rabinowitz ; M. Rigault ; D. Rubin ; K. Runge ; R. Scalzo ; G. Smadja ; C. Tao ; B. A. Weaver ; C. Wu ; P. J. Brown ; P. A. MilneSource :
- The Astrophysical journal [ 0004-637X ] ; 2011.
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English descriptors
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Abstract
We present convincing evidence of unburned carbon at photospheric velocities in new observations of five Type Ia supernovae (SNe Ia) obtained by the Nearby Supernova Factory. These SNe are identified by examining 346 spectra from 124 SNe obtained before +2.5 days relative to maximum. Detections are based on the presence of relatively strong C II λ6580 absorption "notches" in multiple spectra of each SN, aided by automated fitting with the SYNAPPS code. Four of the five SNe in question are otherwise spectroscopically unremarkable, with ions and ejection velocities typical of SNe Ia, but spectra of the fifth exhibit high-velocity (ù > 20, 000 km s-1) Si II and Ca II features. On the other hand, the light curve properties are preferentially grouped, strongly suggesting a connection between carbon-positivity and broadband light curve/color behavior: three of the five have relatively narrow light curves but also blue colors and a fourth may be a dust-reddened member of this family. Accounting for signal to noise and phase, we estimate that 22+10-6% of SNe Ia exhibit spectroscopic CII signatures as late as -5 days with respect to maximum. We place these new objects in the context of previously recognized carbon-positive SNe Ia and consider reasonable scenarios seeking to explain a physical connection between light curve properties and the presence of photospheric carbon. We also examine the detailed evolution of the detected carbon signatures and the surrounding wavelength regions to shed light on the distribution of carbon in the ejecta. Our ability to reconstruct the C II λ6580 feature in detail under the assumption of purely spherical symmetry casts doubt on a "carbon blobs" hypothesis, but does not rule out all asymmetric models. A low volume filling factor for carbon, combined with line-of-sight effects, seems unlikely to explain the scarcity of detected carbon in SNe Ia by itself.
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Format Inist (serveur)
| NO : | PASCAL 12-0032592 INIST |
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| ET : | TYPE Ia SUPERNOVA CARBON FOOTPRINTS |
| AU : | THOMAS (R. C.); ALDERING (G.); ANTILOGUS (P.); ARAGON (C.); BAILEY (S.); BALTAY (C.); BONGARD (S.); BUTON (C.); CANTO (A.); CHILDRESS (M.); CHOTARD (N.); COPIN (Y.); FAKHOURI (H. K.); GANGLER (E.); HSIAO (E. Y.); KERSCHHAGGL (M.); KOWALSKI (M.); LOKEN (S.); NUGENT (P.); PAECH (K.); PAIN (R.); PECONTAL (E.); PEREIRA (R.); PERLMUTTER (S.); RABINOWITZ (D.); RIGAULT (M.); RUBIN (D.); RUNGE (K.); SCALZO (R.); SMADJA (G.); TAO (C.); WEAVER (B. A.); WU (C.); BROWN (P. J.); MILNE (P. A.) |
| AF : | Computational Cosmology Center, Computational Research Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road MS 50B-4206/Berkeley, CA 94611/Etats-Unis (1 aut., 19 aut.); Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road/Berkeley, CA 94720/Etats-Unis (2 aut., 4 aut., 5 aut., 10 aut., 13 aut., 15 aut., 18 aut., 24 aut., 27 aut., 28 aut.); Laboratoire de Physique Nucléaire et des Hautes Energies, Universite Pierre et Marie Curie Paris 6, Universite Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu/75252 Paris/France (3 aut., 7 aut., 9 aut., 21 aut.); Department of Physics, Yale University/New Haven, CT 06250-8121/Etats-Unis (6 aut., 25 aut.); Physikalisches Institut, Universitat Bonn, Nussallee 12/53115 Bonn/Allemagne (8 aut., 16 aut., 17 aut., 20 aut.); Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300/Berkeley, CA 94720-7300/Etats-Unis (10 aut., 13 aut., 24 aut., 27 aut.); Université de Lyon/69622 Lyon/France (11 aut., 12 aut., 14 aut., 23 aut., 26 aut., 30 aut.); Universite de Lyon 1, Villeurbanne/Lyon/France (22 aut.); CNRS/IN2P3, Institut de Physique Nucléaire de Lyon/Lyon/France (29 aut.); Centre de Recherche Astronomique de Lyon, Université Lyon 1, 9 Avenue Charles Andre/69561 Saint Genis Laval/France (31 aut.); Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University, Cotter Road/Weston ACT 2611/Australie (31 aut.); Centre de Physique des Particules de Marseille, 163, Avenue de Luminy - Case 902/13288 Marseille/France (32 aut.); Tsinghua Center for Astrophysics, Tsinghua University/Beijing 100084/Chine (33 aut.); Center for Cosmology and Particle Physics, New York University, 4 Washington Place/New York, NY 10003/Etats-Unis (34 aut.); National Astronomical Observatories, Chinese Academy of Sciences/Beijing 100012/Chine (35 aut.); Department of Physics and Astronomy, University of Utah/Salt Lake City, UT 84112/Etats-Unis; Steward Observatory, University of Arizona, 933 North Cherry Avenue/Tucson, AZ 85719/Etats-Unis |
| DT : | Publication en série; Niveau analytique |
| SO : | The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2011; Vol. 743; No. 1 p. 1; 27.1-27.16; Bibl. 3/4 p. |
| LA : | Anglais |
| EA : | We present convincing evidence of unburned carbon at photospheric velocities in new observations of five Type Ia supernovae (SNe Ia) obtained by the Nearby Supernova Factory. These SNe are identified by examining 346 spectra from 124 SNe obtained before +2.5 days relative to maximum. Detections are based on the presence of relatively strong C II λ6580 absorption "notches" in multiple spectra of each SN, aided by automated fitting with the SYNAPPS code. Four of the five SNe in question are otherwise spectroscopically unremarkable, with ions and ejection velocities typical of SNe Ia, but spectra of the fifth exhibit high-velocity (ù > 20, 000 km s-1) Si II and Ca II features. On the other hand, the light curve properties are preferentially grouped, strongly suggesting a connection between carbon-positivity and broadband light curve/color behavior: three of the five have relatively narrow light curves but also blue colors and a fourth may be a dust-reddened member of this family. Accounting for signal to noise and phase, we estimate that 22+10-6% of SNe Ia exhibit spectroscopic CII signatures as late as -5 days with respect to maximum. We place these new objects in the context of previously recognized carbon-positive SNe Ia and consider reasonable scenarios seeking to explain a physical connection between light curve properties and the presence of photospheric carbon. We also examine the detailed evolution of the detected carbon signatures and the surrounding wavelength regions to shed light on the distribution of carbon in the ejecta. Our ability to reconstruct the C II λ6580 feature in detail under the assumption of purely spherical symmetry casts doubt on a "carbon blobs" hypothesis, but does not rule out all asymmetric models. A low volume filling factor for carbon, combined with line-of-sight effects, seems unlikely to explain the scarcity of detected carbon in SNe Ia by itself. |
| CC : | 001E03 |
| FD : | Supernova type I; Courbe lumière; Courbe couleur; Couleur; Bruit phase; Symétrie sphérique; Modèle; Facteur remplissage |
| ED : | Type I supernova; Light curves; Color curve; Color; Phase noise; Spherical symmetry; Models; Fill factor |
| SD : | Supernova tipo I; Curva color; Simetría esférica; Modelo |
| LO : | INIST-512.354000505946060270 |
| ID : | 12-0032592 |
Links to Exploration step
Pascal:12-0032592Le document en format XML
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Baltay</name><affiliation><inist:fA14 i1="04"><s1>Department of Physics, Yale University</s1><s2>New Haven, CT 06250-8121</s2><s3>USA</s3><sZ>6 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bongard, S" sort="Bongard, S" uniqKey="Bongard S" first="S." last="Bongard">S. Bongard</name><affiliation><inist:fA14 i1="03"><s1>Laboratoire de Physique Nucléaire et des Hautes Energies, Universite Pierre et Marie Curie Paris 6, Universite Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Buton, C" sort="Buton, C" uniqKey="Buton C" first="C." last="Buton">C. Buton</name><affiliation><inist:fA14 i1="05"><s1>Physikalisches Institut, Universitat Bonn, Nussallee 12</s1><s2>53115 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Canto, A" sort="Canto, A" uniqKey="Canto A" first="A." last="Canto">A. Canto</name><affiliation><inist:fA14 i1="03"><s1>Laboratoire de Physique Nucléaire et des Hautes Energies, Universite Pierre et Marie Curie Paris 6, Universite Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Childress, M" sort="Childress, M" uniqKey="Childress M" first="M." last="Childress">M. Childress</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="06"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Chotard, N" sort="Chotard, N" uniqKey="Chotard N" first="N." last="Chotard">N. Chotard</name><affiliation><inist:fA14 i1="07"><s1>Université de Lyon</s1><s2>69622 Lyon</s2><s3>FRA</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ><sZ>23 aut.</sZ><sZ>26 aut.</sZ><sZ>30 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Copin, Y" sort="Copin, Y" uniqKey="Copin Y" first="Y." last="Copin">Y. Copin</name><affiliation><inist:fA14 i1="07"><s1>Université de Lyon</s1><s2>69622 Lyon</s2><s3>FRA</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ><sZ>23 aut.</sZ><sZ>26 aut.</sZ><sZ>30 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Fakhouri, H K" sort="Fakhouri, H K" uniqKey="Fakhouri H" first="H. K." last="Fakhouri">H. K. Fakhouri</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="06"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gangler, E" sort="Gangler, E" uniqKey="Gangler E" first="E." last="Gangler">E. Gangler</name><affiliation><inist:fA14 i1="07"><s1>Université de Lyon</s1><s2>69622 Lyon</s2><s3>FRA</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ><sZ>23 aut.</sZ><sZ>26 aut.</sZ><sZ>30 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Hsiao, E Y" sort="Hsiao, E Y" uniqKey="Hsiao E" first="E. Y." last="Hsiao">E. Y. Hsiao</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kerschhaggl, M" sort="Kerschhaggl, M" uniqKey="Kerschhaggl M" first="M." last="Kerschhaggl">M. Kerschhaggl</name><affiliation><inist:fA14 i1="05"><s1>Physikalisches Institut, Universitat Bonn, Nussallee 12</s1><s2>53115 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kowalski, M" sort="Kowalski, M" uniqKey="Kowalski M" first="M." last="Kowalski">M. Kowalski</name><affiliation><inist:fA14 i1="05"><s1>Physikalisches Institut, Universitat Bonn, Nussallee 12</s1><s2>53115 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Loken, S" sort="Loken, S" uniqKey="Loken S" first="S." last="Loken">S. Loken</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Nugent, P" sort="Nugent, P" uniqKey="Nugent P" first="P." last="Nugent">P. Nugent</name><affiliation><inist:fA14 i1="01"><s1>Computational Cosmology Center, Computational Research Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road MS 50B-4206</s1><s2>Berkeley, CA 94611</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Paech, K" sort="Paech, K" uniqKey="Paech K" first="K." last="Paech">K. Paech</name><affiliation><inist:fA14 i1="05"><s1>Physikalisches Institut, Universitat Bonn, Nussallee 12</s1><s2>53115 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Pain, R" sort="Pain, R" uniqKey="Pain R" first="R." last="Pain">R. Pain</name><affiliation><inist:fA14 i1="03"><s1>Laboratoire de Physique Nucléaire et des Hautes Energies, Universite Pierre et Marie Curie Paris 6, Universite Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Pecontal, E" sort="Pecontal, E" uniqKey="Pecontal E" first="E." last="Pecontal">E. Pecontal</name><affiliation><inist:fA14 i1="08"><s1>Universite de Lyon 1, Villeurbanne</s1><s2>Lyon</s2><s3>FRA</s3><sZ>22 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Pereira, R" sort="Pereira, R" uniqKey="Pereira R" first="R." last="Pereira">R. Pereira</name><affiliation><inist:fA14 i1="07"><s1>Université de Lyon</s1><s2>69622 Lyon</s2><s3>FRA</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ><sZ>23 aut.</sZ><sZ>26 aut.</sZ><sZ>30 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Perlmutter, S" sort="Perlmutter, S" uniqKey="Perlmutter S" first="S." last="Perlmutter">S. Perlmutter</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="06"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Rabinowitz, D" sort="Rabinowitz, D" uniqKey="Rabinowitz D" first="D." last="Rabinowitz">D. Rabinowitz</name><affiliation><inist:fA14 i1="04"><s1>Department of Physics, Yale University</s1><s2>New Haven, CT 06250-8121</s2><s3>USA</s3><sZ>6 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Rigault, M" sort="Rigault, M" uniqKey="Rigault M" first="M." last="Rigault">M. Rigault</name><affiliation><inist:fA14 i1="07"><s1>Université de Lyon</s1><s2>69622 Lyon</s2><s3>FRA</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ><sZ>23 aut.</sZ><sZ>26 aut.</sZ><sZ>30 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Rubin, D" sort="Rubin, D" uniqKey="Rubin D" first="D." last="Rubin">D. Rubin</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="06"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Runge, K" sort="Runge, K" uniqKey="Runge K" first="K." last="Runge">K. Runge</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Scalzo, R" sort="Scalzo, R" uniqKey="Scalzo R" first="R." last="Scalzo">R. Scalzo</name><affiliation><inist:fA14 i1="09"><s1>CNRS/IN2P3, Institut de Physique Nucléaire de Lyon</s1><s2>Lyon</s2><s3>FRA</s3><sZ>29 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Smadja, G" sort="Smadja, G" uniqKey="Smadja G" first="G." last="Smadja">G. Smadja</name><affiliation><inist:fA14 i1="07"><s1>Université de Lyon</s1><s2>69622 Lyon</s2><s3>FRA</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ><sZ>23 aut.</sZ><sZ>26 aut.</sZ><sZ>30 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Tao, C" sort="Tao, C" uniqKey="Tao C" first="C." last="Tao">C. Tao</name><affiliation><inist:fA14 i1="10"><s1>Centre de Recherche Astronomique de Lyon, Université Lyon 1, 9 Avenue Charles Andre</s1><s2>69561 Saint Genis Laval</s2><s3>FRA</s3><sZ>31 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="11"><s1>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University, Cotter Road</s1><s2>Weston ACT 2611</s2><s3>AUS</s3><sZ>31 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Weaver, B A" sort="Weaver, B A" uniqKey="Weaver B" first="B. A." last="Weaver">B. A. Weaver</name><affiliation><inist:fA14 i1="12"><s1>Centre de Physique des Particules de Marseille, 163, Avenue de Luminy - Case 902</s1><s2>13288 Marseille</s2><s3>FRA</s3><sZ>32 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wu, C" sort="Wu, C" uniqKey="Wu C" first="C." last="Wu">C. Wu</name><affiliation><inist:fA14 i1="13"><s1>Tsinghua Center for Astrophysics, Tsinghua University</s1><s2>Beijing 100084</s2><s3>CHN</s3><sZ>33 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Brown, P J" sort="Brown, P J" uniqKey="Brown P" first="P. J." last="Brown">P. J. Brown</name><affiliation><inist:fA14 i1="14"><s1>Center for Cosmology and Particle Physics, New York University, 4 Washington Place</s1><s2>New York, NY 10003</s2><s3>USA</s3><sZ>34 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Milne, P A" sort="Milne, P A" uniqKey="Milne P" first="P. A." last="Milne">P. A. Milne</name><affiliation><inist:fA14 i1="15"><s1>National Astronomical Observatories, Chinese Academy of Sciences</s1><s2>Beijing 100012</s2><s3>CHN</s3><sZ>35 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">12-0032592</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 12-0032592 INIST</idno><idno type="RBID">Pascal:12-0032592</idno><idno type="wicri:Area/PascalFrancis/Corpus">001697</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">TYPE Ia SUPERNOVA CARBON FOOTPRINTS</title><author><name sortKey="Thomas, R C" sort="Thomas, R C" uniqKey="Thomas R" first="R. C." last="Thomas">R. C. Thomas</name><affiliation><inist:fA14 i1="01"><s1>Computational Cosmology Center, Computational Research Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road MS 50B-4206</s1><s2>Berkeley, CA 94611</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="16"><s1>Department of Physics and Astronomy, University of Utah</s1><s2>Salt Lake City, UT 84112</s2><s3>USA</s3></inist:fA14></affiliation><affiliation><inist:fA14 i1="17"><s1>Steward Observatory, University of Arizona, 933 North Cherry Avenue</s1><s2>Tucson, AZ 85719</s2><s3>USA</s3></inist:fA14></affiliation></author><author><name sortKey="Aldering, G" sort="Aldering, G" uniqKey="Aldering G" first="G." last="Aldering">G. Aldering</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Antilogus, P" sort="Antilogus, P" uniqKey="Antilogus P" first="P." last="Antilogus">P. Antilogus</name><affiliation><inist:fA14 i1="03"><s1>Laboratoire de Physique Nucléaire et des Hautes Energies, Universite Pierre et Marie Curie Paris 6, Universite Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Aragon, C" sort="Aragon, C" uniqKey="Aragon C" first="C." last="Aragon">C. Aragon</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bailey, S" sort="Bailey, S" uniqKey="Bailey S" first="S." last="Bailey">S. Bailey</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Baltay, C" sort="Baltay, C" uniqKey="Baltay C" first="C." last="Baltay">C. Baltay</name><affiliation><inist:fA14 i1="04"><s1>Department of Physics, Yale University</s1><s2>New Haven, CT 06250-8121</s2><s3>USA</s3><sZ>6 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bongard, S" sort="Bongard, S" uniqKey="Bongard S" first="S." last="Bongard">S. Bongard</name><affiliation><inist:fA14 i1="03"><s1>Laboratoire de Physique Nucléaire et des Hautes Energies, Universite Pierre et Marie Curie Paris 6, Universite Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Buton, C" sort="Buton, C" uniqKey="Buton C" first="C." last="Buton">C. Buton</name><affiliation><inist:fA14 i1="05"><s1>Physikalisches Institut, Universitat Bonn, Nussallee 12</s1><s2>53115 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Canto, A" sort="Canto, A" uniqKey="Canto A" first="A." last="Canto">A. Canto</name><affiliation><inist:fA14 i1="03"><s1>Laboratoire de Physique Nucléaire et des Hautes Energies, Universite Pierre et Marie Curie Paris 6, Universite Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Childress, M" sort="Childress, M" uniqKey="Childress M" first="M." last="Childress">M. Childress</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="06"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Chotard, N" sort="Chotard, N" uniqKey="Chotard N" first="N." last="Chotard">N. Chotard</name><affiliation><inist:fA14 i1="07"><s1>Université de Lyon</s1><s2>69622 Lyon</s2><s3>FRA</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ><sZ>23 aut.</sZ><sZ>26 aut.</sZ><sZ>30 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Copin, Y" sort="Copin, Y" uniqKey="Copin Y" first="Y." last="Copin">Y. Copin</name><affiliation><inist:fA14 i1="07"><s1>Université de Lyon</s1><s2>69622 Lyon</s2><s3>FRA</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ><sZ>23 aut.</sZ><sZ>26 aut.</sZ><sZ>30 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Fakhouri, H K" sort="Fakhouri, H K" uniqKey="Fakhouri H" first="H. K." last="Fakhouri">H. K. Fakhouri</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="06"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gangler, E" sort="Gangler, E" uniqKey="Gangler E" first="E." last="Gangler">E. Gangler</name><affiliation><inist:fA14 i1="07"><s1>Université de Lyon</s1><s2>69622 Lyon</s2><s3>FRA</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ><sZ>23 aut.</sZ><sZ>26 aut.</sZ><sZ>30 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Hsiao, E Y" sort="Hsiao, E Y" uniqKey="Hsiao E" first="E. Y." last="Hsiao">E. Y. Hsiao</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kerschhaggl, M" sort="Kerschhaggl, M" uniqKey="Kerschhaggl M" first="M." last="Kerschhaggl">M. Kerschhaggl</name><affiliation><inist:fA14 i1="05"><s1>Physikalisches Institut, Universitat Bonn, Nussallee 12</s1><s2>53115 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Kowalski, M" sort="Kowalski, M" uniqKey="Kowalski M" first="M." last="Kowalski">M. Kowalski</name><affiliation><inist:fA14 i1="05"><s1>Physikalisches Institut, Universitat Bonn, Nussallee 12</s1><s2>53115 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Loken, S" sort="Loken, S" uniqKey="Loken S" first="S." last="Loken">S. Loken</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Nugent, P" sort="Nugent, P" uniqKey="Nugent P" first="P." last="Nugent">P. Nugent</name><affiliation><inist:fA14 i1="01"><s1>Computational Cosmology Center, Computational Research Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road MS 50B-4206</s1><s2>Berkeley, CA 94611</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>19 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Paech, K" sort="Paech, K" uniqKey="Paech K" first="K." last="Paech">K. Paech</name><affiliation><inist:fA14 i1="05"><s1>Physikalisches Institut, Universitat Bonn, Nussallee 12</s1><s2>53115 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Pain, R" sort="Pain, R" uniqKey="Pain R" first="R." last="Pain">R. Pain</name><affiliation><inist:fA14 i1="03"><s1>Laboratoire de Physique Nucléaire et des Hautes Energies, Universite Pierre et Marie Curie Paris 6, Universite Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Pecontal, E" sort="Pecontal, E" uniqKey="Pecontal E" first="E." last="Pecontal">E. Pecontal</name><affiliation><inist:fA14 i1="08"><s1>Universite de Lyon 1, Villeurbanne</s1><s2>Lyon</s2><s3>FRA</s3><sZ>22 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Pereira, R" sort="Pereira, R" uniqKey="Pereira R" first="R." last="Pereira">R. Pereira</name><affiliation><inist:fA14 i1="07"><s1>Université de Lyon</s1><s2>69622 Lyon</s2><s3>FRA</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ><sZ>23 aut.</sZ><sZ>26 aut.</sZ><sZ>30 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Perlmutter, S" sort="Perlmutter, S" uniqKey="Perlmutter S" first="S." last="Perlmutter">S. Perlmutter</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="06"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Rabinowitz, D" sort="Rabinowitz, D" uniqKey="Rabinowitz D" first="D." last="Rabinowitz">D. Rabinowitz</name><affiliation><inist:fA14 i1="04"><s1>Department of Physics, Yale University</s1><s2>New Haven, CT 06250-8121</s2><s3>USA</s3><sZ>6 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Rigault, M" sort="Rigault, M" uniqKey="Rigault M" first="M." last="Rigault">M. Rigault</name><affiliation><inist:fA14 i1="07"><s1>Université de Lyon</s1><s2>69622 Lyon</s2><s3>FRA</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ><sZ>23 aut.</sZ><sZ>26 aut.</sZ><sZ>30 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Rubin, D" sort="Rubin, D" uniqKey="Rubin D" first="D." last="Rubin">D. Rubin</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="06"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Runge, K" sort="Runge, K" uniqKey="Runge K" first="K." last="Runge">K. Runge</name><affiliation><inist:fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Scalzo, R" sort="Scalzo, R" uniqKey="Scalzo R" first="R." last="Scalzo">R. Scalzo</name><affiliation><inist:fA14 i1="09"><s1>CNRS/IN2P3, Institut de Physique Nucléaire de Lyon</s1><s2>Lyon</s2><s3>FRA</s3><sZ>29 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Smadja, G" sort="Smadja, G" uniqKey="Smadja G" first="G." last="Smadja">G. Smadja</name><affiliation><inist:fA14 i1="07"><s1>Université de Lyon</s1><s2>69622 Lyon</s2><s3>FRA</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ><sZ>23 aut.</sZ><sZ>26 aut.</sZ><sZ>30 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Tao, C" sort="Tao, C" uniqKey="Tao C" first="C." last="Tao">C. Tao</name><affiliation><inist:fA14 i1="10"><s1>Centre de Recherche Astronomique de Lyon, Université Lyon 1, 9 Avenue Charles Andre</s1><s2>69561 Saint Genis Laval</s2><s3>FRA</s3><sZ>31 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="11"><s1>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University, Cotter Road</s1><s2>Weston ACT 2611</s2><s3>AUS</s3><sZ>31 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Weaver, B A" sort="Weaver, B A" uniqKey="Weaver B" first="B. A." last="Weaver">B. A. Weaver</name><affiliation><inist:fA14 i1="12"><s1>Centre de Physique des Particules de Marseille, 163, Avenue de Luminy - Case 902</s1><s2>13288 Marseille</s2><s3>FRA</s3><sZ>32 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wu, C" sort="Wu, C" uniqKey="Wu C" first="C." last="Wu">C. Wu</name><affiliation><inist:fA14 i1="13"><s1>Tsinghua Center for Astrophysics, Tsinghua University</s1><s2>Beijing 100084</s2><s3>CHN</s3><sZ>33 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Brown, P J" sort="Brown, P J" uniqKey="Brown P" first="P. J." last="Brown">P. J. Brown</name><affiliation><inist:fA14 i1="14"><s1>Center for Cosmology and Particle Physics, New York University, 4 Washington Place</s1><s2>New York, NY 10003</s2><s3>USA</s3><sZ>34 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Milne, P A" sort="Milne, P A" uniqKey="Milne P" first="P. A." last="Milne">P. A. Milne</name><affiliation><inist:fA14 i1="15"><s1>National Astronomical Observatories, Chinese Academy of Sciences</s1><s2>Beijing 100012</s2><s3>CHN</s3><sZ>35 aut.</sZ></inist:fA14></affiliation></author></analytic><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="2011">2011</date></imprint></series></biblStruct></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>Color</term><term>Color curve</term><term>Fill factor</term><term>Light curves</term><term>Models</term><term>Phase noise</term><term>Spherical symmetry</term><term>Type I supernova</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Supernova type I</term><term>Courbe lumière</term><term>Courbe couleur</term><term>Couleur</term><term>Bruit phase</term><term>Symétrie sphérique</term><term>Modèle</term><term>Facteur remplissage</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present convincing evidence of unburned carbon at photospheric velocities in new observations of five Type Ia supernovae (SNe Ia) obtained by the Nearby Supernova Factory. These SNe are identified by examining 346 spectra from 124 SNe obtained before +2.5 days relative to maximum. Detections are based on the presence of relatively strong C II λ6580 absorption "notches" in multiple spectra of each SN, aided by automated fitting with the SYNAPPS code. Four of the five SNe in question are otherwise spectroscopically unremarkable, with ions and ejection velocities typical of SNe Ia, but spectra of the fifth exhibit high-velocity (ù > 20, 000 km s<sup>-1</sup>) Si II and Ca II features. On the other hand, the light curve properties are preferentially grouped, strongly suggesting a connection between carbon-positivity and broadband light curve/color behavior: three of the five have relatively narrow light curves but also blue colors and a fourth may be a dust-reddened member of this family. Accounting for signal to noise and phase, we estimate that 22<sup>+10</sup><sub>-6</sub>% of SNe Ia exhibit spectroscopic CII signatures as late as -5 days with respect to maximum. We place these new objects in the context of previously recognized carbon-positive SNe Ia and consider reasonable scenarios seeking to explain a physical connection between light curve properties and the presence of photospheric carbon. We also examine the detailed evolution of the detected carbon signatures and the surrounding wavelength regions to shed light on the distribution of carbon in the ejecta. Our ability to reconstruct the C II λ6580 feature in detail under the assumption of purely spherical symmetry casts doubt on a "carbon blobs" hypothesis, but does not rule out all asymmetric models. A low volume filling factor for carbon, combined with line-of-sight effects, seems unlikely to explain the scarcity of detected carbon in SNe Ia by itself.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-637X</s0></fA01><fA02 i1="01"><s0>ASJOAB</s0></fA02><fA03 i2="1"><s0>Astrophys. j.</s0></fA03><fA05><s2>743</s2></fA05><fA06><s2>1</s2><s3>p. 1</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>TYPE Ia SUPERNOVA CARBON FOOTPRINTS</s1></fA08><fA11 i1="01" i2="1"><s1>THOMAS (R. C.)</s1></fA11><fA11 i1="02" i2="1"><s1>ALDERING (G.)</s1></fA11><fA11 i1="03" i2="1"><s1>ANTILOGUS (P.)</s1></fA11><fA11 i1="04" i2="1"><s1>ARAGON (C.)</s1></fA11><fA11 i1="05" i2="1"><s1>BAILEY (S.)</s1></fA11><fA11 i1="06" i2="1"><s1>BALTAY (C.)</s1></fA11><fA11 i1="07" i2="1"><s1>BONGARD (S.)</s1></fA11><fA11 i1="08" i2="1"><s1>BUTON (C.)</s1></fA11><fA11 i1="09" i2="1"><s1>CANTO (A.)</s1></fA11><fA11 i1="10" i2="1"><s1>CHILDRESS (M.)</s1></fA11><fA11 i1="11" i2="1"><s1>CHOTARD (N.)</s1></fA11><fA11 i1="12" i2="1"><s1>COPIN (Y.)</s1></fA11><fA11 i1="13" i2="1"><s1>FAKHOURI (H. K.)</s1></fA11><fA11 i1="14" i2="1"><s1>GANGLER (E.)</s1></fA11><fA11 i1="15" i2="1"><s1>HSIAO (E. Y.)</s1></fA11><fA11 i1="16" i2="1"><s1>KERSCHHAGGL (M.)</s1></fA11><fA11 i1="17" i2="1"><s1>KOWALSKI (M.)</s1></fA11><fA11 i1="18" i2="1"><s1>LOKEN (S.)</s1></fA11><fA11 i1="19" i2="1"><s1>NUGENT (P.)</s1></fA11><fA11 i1="20" i2="1"><s1>PAECH (K.)</s1></fA11><fA11 i1="21" i2="1"><s1>PAIN (R.)</s1></fA11><fA11 i1="22" i2="1"><s1>PECONTAL (E.)</s1></fA11><fA11 i1="23" i2="1"><s1>PEREIRA (R.)</s1></fA11><fA11 i1="24" i2="1"><s1>PERLMUTTER (S.)</s1></fA11><fA11 i1="25" i2="1"><s1>RABINOWITZ (D.)</s1></fA11><fA11 i1="26" i2="1"><s1>RIGAULT (M.)</s1></fA11><fA11 i1="27" i2="1"><s1>RUBIN (D.)</s1></fA11><fA11 i1="28" i2="1"><s1>RUNGE (K.)</s1></fA11><fA11 i1="29" i2="1"><s1>SCALZO (R.)</s1></fA11><fA11 i1="30" i2="1"><s1>SMADJA (G.)</s1></fA11><fA11 i1="31" i2="1"><s1>TAO (C.)</s1></fA11><fA11 i1="32" i2="1"><s1>WEAVER (B. A.)</s1></fA11><fA11 i1="33" i2="1"><s1>WU (C.)</s1></fA11><fA11 i1="34" i2="1"><s1>BROWN (P. J.)</s1></fA11><fA11 i1="35" i2="1"><s1>MILNE (P. A.)</s1></fA11><fA14 i1="01"><s1>Computational Cosmology Center, Computational Research Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road MS 50B-4206</s1><s2>Berkeley, CA 94611</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>19 aut.</sZ></fA14><fA14 i1="02"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>15 aut.</sZ><sZ>18 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ><sZ>28 aut.</sZ></fA14><fA14 i1="03"><s1>Laboratoire de Physique Nucléaire et des Hautes Energies, Universite Pierre et Marie Curie Paris 6, Universite Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>21 aut.</sZ></fA14><fA14 i1="04"><s1>Department of Physics, Yale University</s1><s2>New Haven, CT 06250-8121</s2><s3>USA</s3><sZ>6 aut.</sZ><sZ>25 aut.</sZ></fA14><fA14 i1="05"><s1>Physikalisches Institut, Universitat Bonn, Nussallee 12</s1><s2>53115 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>20 aut.</sZ></fA14><fA14 i1="06"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>10 aut.</sZ><sZ>13 aut.</sZ><sZ>24 aut.</sZ><sZ>27 aut.</sZ></fA14><fA14 i1="07"><s1>Université de Lyon</s1><s2>69622 Lyon</s2><s3>FRA</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ><sZ>14 aut.</sZ><sZ>23 aut.</sZ><sZ>26 aut.</sZ><sZ>30 aut.</sZ></fA14><fA14 i1="08"><s1>Universite de Lyon 1, Villeurbanne</s1><s2>Lyon</s2><s3>FRA</s3><sZ>22 aut.</sZ></fA14><fA14 i1="09"><s1>CNRS/IN2P3, Institut de Physique Nucléaire de Lyon</s1><s2>Lyon</s2><s3>FRA</s3><sZ>29 aut.</sZ></fA14><fA14 i1="10"><s1>Centre de Recherche Astronomique de Lyon, Université Lyon 1, 9 Avenue Charles Andre</s1><s2>69561 Saint Genis Laval</s2><s3>FRA</s3><sZ>31 aut.</sZ></fA14><fA14 i1="11"><s1>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University, Cotter Road</s1><s2>Weston ACT 2611</s2><s3>AUS</s3><sZ>31 aut.</sZ></fA14><fA14 i1="12"><s1>Centre de Physique des Particules de Marseille, 163, Avenue de Luminy - Case 902</s1><s2>13288 Marseille</s2><s3>FRA</s3><sZ>32 aut.</sZ></fA14><fA14 i1="13"><s1>Tsinghua Center for Astrophysics, Tsinghua University</s1><s2>Beijing 100084</s2><s3>CHN</s3><sZ>33 aut.</sZ></fA14><fA14 i1="14"><s1>Center for Cosmology and Particle Physics, New York University, 4 Washington Place</s1><s2>New York, NY 10003</s2><s3>USA</s3><sZ>34 aut.</sZ></fA14><fA14 i1="15"><s1>National Astronomical Observatories, Chinese Academy of Sciences</s1><s2>Beijing 100012</s2><s3>CHN</s3><sZ>35 aut.</sZ></fA14><fA14 i1="16"><s1>Department of Physics and Astronomy, University of Utah</s1><s2>Salt Lake City, UT 84112</s2><s3>USA</s3></fA14><fA14 i1="17"><s1>Steward Observatory, University of Arizona, 933 North Cherry Avenue</s1><s2>Tucson, AZ 85719</s2><s3>USA</s3></fA14><fA20><s2>27.1-27.16</s2></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>512</s2><s5>354000505946060270</s5></fA43><fA44><s0>0000</s0><s1>© 2012 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>12-0032592</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>The Astrophysical journal</s0></fA64><fA66 i1="01"><s0>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>We present convincing evidence of unburned carbon at photospheric velocities in new observations of five Type Ia supernovae (SNe Ia) obtained by the Nearby Supernova Factory. These SNe are identified by examining 346 spectra from 124 SNe obtained before +2.5 days relative to maximum. Detections are based on the presence of relatively strong C II λ6580 absorption "notches" in multiple spectra of each SN, aided by automated fitting with the SYNAPPS code. Four of the five SNe in question are otherwise spectroscopically unremarkable, with ions and ejection velocities typical of SNe Ia, but spectra of the fifth exhibit high-velocity (ù > 20, 000 km s<sup>-1</sup>) Si II and Ca II features. On the other hand, the light curve properties are preferentially grouped, strongly suggesting a connection between carbon-positivity and broadband light curve/color behavior: three of the five have relatively narrow light curves but also blue colors and a fourth may be a dust-reddened member of this family. Accounting for signal to noise and phase, we estimate that 22<sup>+10</sup><sub>-6</sub>% of SNe Ia exhibit spectroscopic CII signatures as late as -5 days with respect to maximum. We place these new objects in the context of previously recognized carbon-positive SNe Ia and consider reasonable scenarios seeking to explain a physical connection between light curve properties and the presence of photospheric carbon. We also examine the detailed evolution of the detected carbon signatures and the surrounding wavelength regions to shed light on the distribution of carbon in the ejecta. Our ability to reconstruct the C II λ6580 feature in detail under the assumption of purely spherical symmetry casts doubt on a "carbon blobs" hypothesis, but does not rule out all asymmetric models. A low volume filling factor for carbon, combined with line-of-sight effects, seems unlikely to explain the scarcity of detected carbon in SNe Ia by itself.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Supernova type I</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Type I supernova</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Supernova tipo I</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Courbe lumière</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Light curves</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Courbe couleur</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Color curve</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Curva color</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Couleur</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Color</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Bruit phase</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Phase noise</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Symétrie sphérique</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Spherical symmetry</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Simetría esférica</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Modèle</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Models</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Modelo</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Facteur remplissage</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Fill factor</s0><s5>33</s5></fC03><fN21><s1>016</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 12-0032592 INIST</NO><ET>TYPE Ia SUPERNOVA CARBON FOOTPRINTS</ET><AU>THOMAS (R. C.); ALDERING (G.); ANTILOGUS (P.); ARAGON (C.); BAILEY (S.); BALTAY (C.); BONGARD (S.); BUTON (C.); CANTO (A.); CHILDRESS (M.); CHOTARD (N.); COPIN (Y.); FAKHOURI (H. K.); GANGLER (E.); HSIAO (E. Y.); KERSCHHAGGL (M.); KOWALSKI (M.); LOKEN (S.); NUGENT (P.); PAECH (K.); PAIN (R.); PECONTAL (E.); PEREIRA (R.); PERLMUTTER (S.); RABINOWITZ (D.); RIGAULT (M.); RUBIN (D.); RUNGE (K.); SCALZO (R.); SMADJA (G.); TAO (C.); WEAVER (B. A.); WU (C.); BROWN (P. J.); MILNE (P. A.)</AU><AF>Computational Cosmology Center, Computational Research Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road MS 50B-4206/Berkeley, CA 94611/Etats-Unis (1 aut., 19 aut.); Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road/Berkeley, CA 94720/Etats-Unis (2 aut., 4 aut., 5 aut., 10 aut., 13 aut., 15 aut., 18 aut., 24 aut., 27 aut., 28 aut.); Laboratoire de Physique Nucléaire et des Hautes Energies, Universite Pierre et Marie Curie Paris 6, Universite Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu/75252 Paris/France (3 aut., 7 aut., 9 aut., 21 aut.); Department of Physics, Yale University/New Haven, CT 06250-8121/Etats-Unis (6 aut., 25 aut.); Physikalisches Institut, Universitat Bonn, Nussallee 12/53115 Bonn/Allemagne (8 aut., 16 aut., 17 aut., 20 aut.); Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300/Berkeley, CA 94720-7300/Etats-Unis (10 aut., 13 aut., 24 aut., 27 aut.); Université de Lyon/69622 Lyon/France (11 aut., 12 aut., 14 aut., 23 aut., 26 aut., 30 aut.); Universite de Lyon 1, Villeurbanne/Lyon/France (22 aut.); CNRS/IN2P3, Institut de Physique Nucléaire de Lyon/Lyon/France (29 aut.); Centre de Recherche Astronomique de Lyon, Université Lyon 1, 9 Avenue Charles Andre/69561 Saint Genis Laval/France (31 aut.); Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University, Cotter Road/Weston ACT 2611/Australie (31 aut.); Centre de Physique des Particules de Marseille, 163, Avenue de Luminy - Case 902/13288 Marseille/France (32 aut.); Tsinghua Center for Astrophysics, Tsinghua University/Beijing 100084/Chine (33 aut.); Center for Cosmology and Particle Physics, New York University, 4 Washington Place/New York, NY 10003/Etats-Unis (34 aut.); National Astronomical Observatories, Chinese Academy of Sciences/Beijing 100012/Chine (35 aut.); Department of Physics and Astronomy, University of Utah/Salt Lake City, UT 84112/Etats-Unis; Steward Observatory, University of Arizona, 933 North Cherry Avenue/Tucson, AZ 85719/Etats-Unis</AF><DT>Publication en série; Niveau analytique</DT><SO>The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2011; Vol. 743; No. 1 p. 1; 27.1-27.16; Bibl. 3/4 p.</SO><LA>Anglais</LA><EA>We present convincing evidence of unburned carbon at photospheric velocities in new observations of five Type Ia supernovae (SNe Ia) obtained by the Nearby Supernova Factory. These SNe are identified by examining 346 spectra from 124 SNe obtained before +2.5 days relative to maximum. Detections are based on the presence of relatively strong C II λ6580 absorption "notches" in multiple spectra of each SN, aided by automated fitting with the SYNAPPS code. Four of the five SNe in question are otherwise spectroscopically unremarkable, with ions and ejection velocities typical of SNe Ia, but spectra of the fifth exhibit high-velocity (ù > 20, 000 km s<sup>-1</sup>) Si II and Ca II features. On the other hand, the light curve properties are preferentially grouped, strongly suggesting a connection between carbon-positivity and broadband light curve/color behavior: three of the five have relatively narrow light curves but also blue colors and a fourth may be a dust-reddened member of this family. Accounting for signal to noise and phase, we estimate that 22<sup>+10</sup><sub>-6</sub>% of SNe Ia exhibit spectroscopic CII signatures as late as -5 days with respect to maximum. We place these new objects in the context of previously recognized carbon-positive SNe Ia and consider reasonable scenarios seeking to explain a physical connection between light curve properties and the presence of photospheric carbon. We also examine the detailed evolution of the detected carbon signatures and the surrounding wavelength regions to shed light on the distribution of carbon in the ejecta. Our ability to reconstruct the C II λ6580 feature in detail under the assumption of purely spherical symmetry casts doubt on a "carbon blobs" hypothesis, but does not rule out all asymmetric models. A low volume filling factor for carbon, combined with line-of-sight effects, seems unlikely to explain the scarcity of detected carbon in SNe Ia by itself.</EA><CC>001E03</CC><FD>Supernova type I; Courbe lumière; Courbe couleur; Couleur; Bruit phase; Symétrie sphérique; Modèle; Facteur remplissage</FD><ED>Type I supernova; Light curves; Color curve; Color; Phase noise; Spherical symmetry; Models; Fill factor</ED><SD>Supernova tipo I; Curva color; Simetría esférica; Modelo</SD><LO>INIST-512.354000505946060270</LO><ID>12-0032592</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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