KECK OBSERVATIONS OF THE YOUNG METAL-POOR HOST GALAXY OF THE SUPER-CHANDRASEKHAR-MASS TYPE Ia SUPERNOVA SN 2007if
Identifieur interne : 001D18 ( PascalFrancis/Corpus ); précédent : 001D17; suivant : 001D19KECK OBSERVATIONS OF THE YOUNG METAL-POOR HOST GALAXY OF THE SUPER-CHANDRASEKHAR-MASS TYPE Ia SUPERNOVA SN 2007if
Auteurs : M. Childress ; G. Aldering ; C. Aragon ; P. Antilogus ; S. Bailey ; C. Baltay ; S. Bongard ; C. Buton ; A. Canto ; N. Chotard ; Y. Copin ; H. K. Fakhouri ; E. Gangler ; M. Kerschhaggl ; M. Kowalski ; E. Y. Hsiao ; S. Loken ; P. Nugent ; K. Paech ; R. Pain ; E. Pecontal ; R. Pereira ; S. Perlmutter ; D. Rabinowitz ; K. Runge ; R. Scalzo ; R. C. Thomas ; G. Smadja ; C. Tao ; B. A. Weaver ; C. WuSource :
- The Astrophysical journal [ 0004-637X ] ; 2011.
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- Pascal (Inist)
English descriptors
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Abstract
We present Keck LRIS spectroscopy and g-band photometry of the metal-poor, low-luminosity host galaxy of the super-Chandrasekhar-mass Type Ia supernova SN 2007if. Deep imaging of the host reveals its apparent magnitude to be mg = 23.15 ± 0.06, which at the spectroscopically measured redshift of Zhelio = 0.07450 ± 0.00015 corresponds to an absolute magnitude of Mg = -14.45 ± 0.06. Galaxy g - r color constrains the mass-to-light ratio, giving a host stellar mass estimate of log(M*/M◦.) = 7.32 ± 0.17. Balmer absorption in the stellar continuum, along with the strength of the 4000 Å break, constrains the age of the dominant starburst in the galaxy to be tburst = 123±165-77 Myr, corresponding to a main-sequence turnoff mass of M/M◦. = 4.6+2.6-1.4. Using the R23 method of calculating metallicity from the fluxes of strong emission lines, we determine the host oxygen abundance to be 12 + log(O/H)KK04 = 8.01 ± 0.09, significantly lower than any previously reported spectroscopically measured Type Ia supernova host galaxy metallicity. Our data show that SN 2007if is very likely to have originated from a young, metal-poor progenitor.
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Format Inist (serveur)
| NO : | PASCAL 11-0258003 INIST |
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| ET : | KECK OBSERVATIONS OF THE YOUNG METAL-POOR HOST GALAXY OF THE SUPER-CHANDRASEKHAR-MASS TYPE Ia SUPERNOVA SN 2007if |
| AU : | CHILDRESS (M.); ALDERING (G.); ARAGON (C.); ANTILOGUS (P.); BAILEY (S.); BALTAY (C.); BONGARD (S.); BUTON (C.); CANTO (A.); CHOTARD (N.); COPIN (Y.); FAKHOURI (H. K.); GANGLER (E.); KERSCHHAGGL (M.); KOWALSKI (M.); HSIAO (E. Y.); LOKEN (S.); NUGENT (P.); PAECH (K.); PAIN (R.); PECONTAL (E.); PEREIRA (R.); PERLMUTTER (S.); RABINOWITZ (D.); RUNGE (K.); SCALZO (R.); THOMAS (R. C.); SMADJA (G.); TAO (C.); WEAVER (B. A.); WU (C.) |
| AF : | Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road/Berkeley, CA 94720/Etats-Unis (1 aut., 2 aut., 3 aut., 5 aut., 12 aut., 16 aut., 17 aut., 23 aut., 25 aut.); Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300/Berkeley, CA 94720-7300/Etats-Unis (1 aut., 12 aut., 23 aut.); Laboratoire de Physique Nucleaire et des Hautes Energies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu/75252 Paris/France (4 aut., 7 aut., 9 aut., 20 aut., 31 aut.); Department of Physics, Yale University/New Haven, CT 06250-8121/Etats-Unis (6 aut., 24 aut., 26 aut.); Physikalisches Institut, Universitat Bonn, Nussallee 12/531 15 Bonn/Allemagne (8 aut., 14 aut., 15 aut., 19 aut.); Université de Lyon, 69622, Lyon; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucleaire de Lyon/France (10 aut., 11 aut., 13 aut., 22 aut., 28 aut.); Computational Cosmology Center, Computational Research Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road MS 50B-4206/Berkeley, CA 94611/Etats-Unis (18 aut., 27 aut.); Centre de Recherche Astronomique de Lyon, Université Lyon 1, 9 Avenue Charles André/69561 Saint Genis Laval/France (21 aut.); Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, The Australian National University, Cotter Road/Weston ACT 2611/Australie (26 aut.); Centre de Physique des Particules de Marseille, 163, avenue de Luminy, Case 902/13288 Marseille/France (29 aut.); Tsinghua Center for Astrophysics, Tsinghua University/Beijing 100084/Chine (29 aut.); New York University, Center for Cosmology & Particle Physics, 4 Washington Place/New York, NY 10003/Etats-Unis (30 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2011; Vol. 733; No. 1 p. 1; 7333.1-7333.15; Bibl. 3/4 p. |
| LA : | Anglais |
| EA : | We present Keck LRIS spectroscopy and g-band photometry of the metal-poor, low-luminosity host galaxy of the super-Chandrasekhar-mass Type Ia supernova SN 2007if. Deep imaging of the host reveals its apparent magnitude to be mg = 23.15 ± 0.06, which at the spectroscopically measured redshift of Zhelio = 0.07450 ± 0.00015 corresponds to an absolute magnitude of Mg = -14.45 ± 0.06. Galaxy g - r color constrains the mass-to-light ratio, giving a host stellar mass estimate of log(M*/M◦.) = 7.32 ± 0.17. Balmer absorption in the stellar continuum, along with the strength of the 4000 Å break, constrains the age of the dominant starburst in the galaxy to be tburst = 123±165-77 Myr, corresponding to a main-sequence turnoff mass of M/M◦. = 4.6+2.6-1.4. Using the R23 method of calculating metallicity from the fluxes of strong emission lines, we determine the host oxygen abundance to be 12 + log(O/H)KK04 = 8.01 ± 0.09, significantly lower than any previously reported spectroscopically measured Type Ia supernova host galaxy metallicity. Our data show that SN 2007if is very likely to have originated from a young, metal-poor progenitor. |
| CC : | 001E03 |
| FD : | Galaxies à flambée; Supernova type I; Spectrométrie; Photométrie; Luminosité; Déplacement vers le rouge; Magnitude absolue; Couleur; Rapport masse luminosité; Masse stellaire; Continuum; Age; Métallicité; Raie émission; Abondance; Galaxies naines |
| ED : | Starburst galaxies; Type I supernova; Spectroscopy; Photometry; Luminosity; Red shift; Absolute magnitude; Color; Mass to light ratio; Stellar mass; Continuum; Age; Metallicity; Emission line; Abundance; Dwarf galaxies |
| SD : | Galaxias llamarada estelar; Supernova tipo I; Magnitud absoluta; Relación masa luminosidad; Continuo; Edad; Metalicidad; Raya emisión |
| LO : | INIST-512.354000191605310030 |
| ID : | 11-0258003 |
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Pascal:11-0258003Le document en format XML
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Childress</name><affiliation><inist:fA14 i1="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="02"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>12 aut.</sZ><sZ>23 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Aldering, G" sort="Aldering, G" uniqKey="Aldering G" first="G." last="Aldering">G. 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Antilogus</name><affiliation><inist:fA14 i1="03"><s1>Laboratoire de Physique Nucleaire et des Hautes Energies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>31 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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 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>24 aut.</sZ><sZ>26 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 Nucleaire et des Hautes Energies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>31 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>531 15 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>19 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 Nucleaire et des Hautes Energies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>31 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="06"><s1>Université de Lyon, 69622, Lyon; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucleaire de Lyon</s1><s3>FRA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>13 aut.</sZ><sZ>22 aut.</sZ><sZ>28 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="06"><s1>Université de Lyon, 69622, Lyon; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucleaire de Lyon</s1><s3>FRA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>13 aut.</sZ><sZ>22 aut.</sZ><sZ>28 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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="02"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>12 aut.</sZ><sZ>23 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="06"><s1>Université de Lyon, 69622, Lyon; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucleaire de Lyon</s1><s3>FRA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>13 aut.</sZ><sZ>22 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>531 15 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>19 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>531 15 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>19 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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 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="07"><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>18 aut.</sZ><sZ>27 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>531 15 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>19 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 Nucleaire et des Hautes Energies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>31 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>Centre de Recherche Astronomique de Lyon, Université Lyon 1, 9 Avenue Charles André</s1><s2>69561 Saint Genis Laval</s2><s3>FRA</s3><sZ>21 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="06"><s1>Université de Lyon, 69622, Lyon; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucleaire de Lyon</s1><s3>FRA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>13 aut.</sZ><sZ>22 aut.</sZ><sZ>28 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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="02"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>12 aut.</sZ><sZ>23 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>24 aut.</sZ><sZ>26 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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 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="04"><s1>Department of Physics, Yale University</s1><s2>New Haven, CT 06250-8121</s2><s3>USA</s3><sZ>6 aut.</sZ><sZ>24 aut.</sZ><sZ>26 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="09"><s1>Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, The Australian National University, Cotter Road</s1><s2>Weston ACT 2611</s2><s3>AUS</s3><sZ>26 aut.</sZ></inist:fA14></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><inist:fA14 i1="07"><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>18 aut.</sZ><sZ>27 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="06"><s1>Université de Lyon, 69622, Lyon; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucleaire de Lyon</s1><s3>FRA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>13 aut.</sZ><sZ>22 aut.</sZ><sZ>28 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 Physique des Particules de Marseille, 163, avenue de Luminy, Case 902</s1><s2>13288 Marseille</s2><s3>FRA</s3><sZ>29 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="11"><s1>Tsinghua Center for Astrophysics, Tsinghua University</s1><s2>Beijing 100084</s2><s3>CHN</s3><sZ>29 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>New York University, Center for Cosmology & Particle Physics, 4 Washington Place</s1><s2>New York, NY 10003</s2><s3>USA</s3><sZ>30 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="03"><s1>Laboratoire de Physique Nucleaire et des Hautes Energies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>31 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0258003</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 11-0258003 INIST</idno><idno type="RBID">Pascal:11-0258003</idno><idno type="wicri:Area/PascalFrancis/Corpus">001D18</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">KECK OBSERVATIONS OF THE YOUNG METAL-POOR HOST GALAXY OF THE SUPER-CHANDRASEKHAR-MASS TYPE Ia SUPERNOVA SN 2007if</title><author><name sortKey="Childress, M" sort="Childress, M" uniqKey="Childress M" first="M." last="Childress">M. Childress</name><affiliation><inist:fA14 i1="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="02"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>12 aut.</sZ><sZ>23 aut.</sZ></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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 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 Nucleaire et des Hautes Energies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>31 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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 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>24 aut.</sZ><sZ>26 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 Nucleaire et des Hautes Energies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>31 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>531 15 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>19 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 Nucleaire et des Hautes Energies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>31 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="06"><s1>Université de Lyon, 69622, Lyon; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucleaire de Lyon</s1><s3>FRA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>13 aut.</sZ><sZ>22 aut.</sZ><sZ>28 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="06"><s1>Université de Lyon, 69622, Lyon; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucleaire de Lyon</s1><s3>FRA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>13 aut.</sZ><sZ>22 aut.</sZ><sZ>28 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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="02"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>12 aut.</sZ><sZ>23 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="06"><s1>Université de Lyon, 69622, Lyon; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucleaire de Lyon</s1><s3>FRA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>13 aut.</sZ><sZ>22 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>531 15 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>19 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>531 15 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>19 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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 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="07"><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>18 aut.</sZ><sZ>27 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>531 15 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>19 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 Nucleaire et des Hautes Energies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>31 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>Centre de Recherche Astronomique de Lyon, Université Lyon 1, 9 Avenue Charles André</s1><s2>69561 Saint Genis Laval</s2><s3>FRA</s3><sZ>21 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="06"><s1>Université de Lyon, 69622, Lyon; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucleaire de Lyon</s1><s3>FRA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>13 aut.</sZ><sZ>22 aut.</sZ><sZ>28 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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="02"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>12 aut.</sZ><sZ>23 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>24 aut.</sZ><sZ>26 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="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 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="04"><s1>Department of Physics, Yale University</s1><s2>New Haven, CT 06250-8121</s2><s3>USA</s3><sZ>6 aut.</sZ><sZ>24 aut.</sZ><sZ>26 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="09"><s1>Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, The Australian National University, Cotter Road</s1><s2>Weston ACT 2611</s2><s3>AUS</s3><sZ>26 aut.</sZ></inist:fA14></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><inist:fA14 i1="07"><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>18 aut.</sZ><sZ>27 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="06"><s1>Université de Lyon, 69622, Lyon; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucleaire de Lyon</s1><s3>FRA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>13 aut.</sZ><sZ>22 aut.</sZ><sZ>28 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 Physique des Particules de Marseille, 163, avenue de Luminy, Case 902</s1><s2>13288 Marseille</s2><s3>FRA</s3><sZ>29 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="11"><s1>Tsinghua Center for Astrophysics, Tsinghua University</s1><s2>Beijing 100084</s2><s3>CHN</s3><sZ>29 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>New York University, Center for Cosmology & Particle Physics, 4 Washington Place</s1><s2>New York, NY 10003</s2><s3>USA</s3><sZ>30 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="03"><s1>Laboratoire de Physique Nucleaire et des Hautes Energies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>31 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>Absolute magnitude</term><term>Abundance</term><term>Age</term><term>Color</term><term>Continuum</term><term>Dwarf galaxies</term><term>Emission line</term><term>Luminosity</term><term>Mass to light ratio</term><term>Metallicity</term><term>Photometry</term><term>Red shift</term><term>Spectroscopy</term><term>Starburst galaxies</term><term>Stellar mass</term><term>Type I supernova</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Galaxies à flambée</term><term>Supernova type I</term><term>Spectrométrie</term><term>Photométrie</term><term>Luminosité</term><term>Déplacement vers le rouge</term><term>Magnitude absolue</term><term>Couleur</term><term>Rapport masse luminosité</term><term>Masse stellaire</term><term>Continuum</term><term>Age</term><term>Métallicité</term><term>Raie émission</term><term>Abondance</term><term>Galaxies naines</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present Keck LRIS spectroscopy and g-band photometry of the metal-poor, low-luminosity host galaxy of the super-Chandrasekhar-mass Type Ia supernova SN 2007if. Deep imaging of the host reveals its apparent magnitude to be mg = 23.15 ± 0.06, which at the spectroscopically measured redshift of Z<sub>helio</sub> = 0.07450 ± 0.00015 corresponds to an absolute magnitude of M<sub>g </sub>= -14.45 ± 0.06. Galaxy g - r color constrains the mass-to-light ratio, giving a host stellar mass estimate of log(M<sub>*</sub>/M<sub>◦.</sub>) = 7.32 ± 0.17. Balmer absorption in the stellar continuum, along with the strength of the 4000 Å break, constrains the age of the dominant starburst in the galaxy to be t<sub>burst</sub> = 123±<sup>165</sup><sub>-77</sub> Myr, corresponding to a main-sequence turnoff mass of M/M<sub>◦.</sub> = 4.6<sup>+2.6</sup><sub>-1.4</sub>. Using the R<sub>23</sub> method of calculating metallicity from the fluxes of strong emission lines, we determine the host oxygen abundance to be 12 + log(O/H)<sub>KK04</sub> = 8.01 ± 0.09, significantly lower than any previously reported spectroscopically measured Type Ia supernova host galaxy metallicity. Our data show that SN 2007if is very likely to have originated from a young, metal-poor progenitor.</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>733</s2></fA05><fA06><s2>1</s2><s3>p. 1</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>KECK OBSERVATIONS OF THE YOUNG METAL-POOR HOST GALAXY OF THE SUPER-CHANDRASEKHAR-MASS TYPE Ia SUPERNOVA SN 2007if</s1></fA08><fA11 i1="01" i2="1"><s1>CHILDRESS (M.)</s1></fA11><fA11 i1="02" i2="1"><s1>ALDERING (G.)</s1></fA11><fA11 i1="03" i2="1"><s1>ARAGON (C.)</s1></fA11><fA11 i1="04" i2="1"><s1>ANTILOGUS (P.)</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>CHOTARD (N.)</s1></fA11><fA11 i1="11" i2="1"><s1>COPIN (Y.)</s1></fA11><fA11 i1="12" i2="1"><s1>FAKHOURI (H. K.)</s1></fA11><fA11 i1="13" i2="1"><s1>GANGLER (E.)</s1></fA11><fA11 i1="14" i2="1"><s1>KERSCHHAGGL (M.)</s1></fA11><fA11 i1="15" i2="1"><s1>KOWALSKI (M.)</s1></fA11><fA11 i1="16" i2="1"><s1>HSIAO (E. Y.)</s1></fA11><fA11 i1="17" i2="1"><s1>LOKEN (S.)</s1></fA11><fA11 i1="18" i2="1"><s1>NUGENT (P.)</s1></fA11><fA11 i1="19" i2="1"><s1>PAECH (K.)</s1></fA11><fA11 i1="20" i2="1"><s1>PAIN (R.)</s1></fA11><fA11 i1="21" i2="1"><s1>PECONTAL (E.)</s1></fA11><fA11 i1="22" i2="1"><s1>PEREIRA (R.)</s1></fA11><fA11 i1="23" i2="1"><s1>PERLMUTTER (S.)</s1></fA11><fA11 i1="24" i2="1"><s1>RABINOWITZ (D.)</s1></fA11><fA11 i1="25" i2="1"><s1>RUNGE (K.)</s1></fA11><fA11 i1="26" i2="1"><s1>SCALZO (R.)</s1></fA11><fA11 i1="27" i2="1"><s1>THOMAS (R. C.)</s1></fA11><fA11 i1="28" i2="1"><s1>SMADJA (G.)</s1></fA11><fA11 i1="29" i2="1"><s1>TAO (C.)</s1></fA11><fA11 i1="30" i2="1"><s1>WEAVER (B. A.)</s1></fA11><fA11 i1="31" i2="1"><s1>WU (C.)</s1></fA11><fA14 i1="01"><s1>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ><sZ>23 aut.</sZ><sZ>25 aut.</sZ></fA14><fA14 i1="02"><s1>Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300</s1><s2>Berkeley, CA 94720-7300</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>12 aut.</sZ><sZ>23 aut.</sZ></fA14><fA14 i1="03"><s1>Laboratoire de Physique Nucleaire et des Hautes Energies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu</s1><s2>75252 Paris</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>7 aut.</sZ><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>31 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>24 aut.</sZ><sZ>26 aut.</sZ></fA14><fA14 i1="05"><s1>Physikalisches Institut, Universitat Bonn, Nussallee 12</s1><s2>531 15 Bonn</s2><s3>DEU</s3><sZ>8 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ><sZ>19 aut.</sZ></fA14><fA14 i1="06"><s1>Université de Lyon, 69622, Lyon; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucleaire de Lyon</s1><s3>FRA</s3><sZ>10 aut.</sZ><sZ>11 aut.</sZ><sZ>13 aut.</sZ><sZ>22 aut.</sZ><sZ>28 aut.</sZ></fA14><fA14 i1="07"><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>18 aut.</sZ><sZ>27 aut.</sZ></fA14><fA14 i1="08"><s1>Centre de Recherche Astronomique de Lyon, Université Lyon 1, 9 Avenue Charles André</s1><s2>69561 Saint Genis Laval</s2><s3>FRA</s3><sZ>21 aut.</sZ></fA14><fA14 i1="09"><s1>Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, The Australian National University, Cotter Road</s1><s2>Weston ACT 2611</s2><s3>AUS</s3><sZ>26 aut.</sZ></fA14><fA14 i1="10"><s1>Centre de Physique des Particules de Marseille, 163, avenue de Luminy, Case 902</s1><s2>13288 Marseille</s2><s3>FRA</s3><sZ>29 aut.</sZ></fA14><fA14 i1="11"><s1>Tsinghua Center for Astrophysics, Tsinghua University</s1><s2>Beijing 100084</s2><s3>CHN</s3><sZ>29 aut.</sZ></fA14><fA14 i1="12"><s1>New York University, Center for Cosmology & Particle Physics, 4 Washington Place</s1><s2>New York, NY 10003</s2><s3>USA</s3><sZ>30 aut.</sZ></fA14><fA20><s2>7333.1-7333.15</s2></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>512</s2><s5>354000191605310030</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>11-0258003</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 Keck LRIS spectroscopy and g-band photometry of the metal-poor, low-luminosity host galaxy of the super-Chandrasekhar-mass Type Ia supernova SN 2007if. Deep imaging of the host reveals its apparent magnitude to be mg = 23.15 ± 0.06, which at the spectroscopically measured redshift of Z<sub>helio</sub> = 0.07450 ± 0.00015 corresponds to an absolute magnitude of M<sub>g </sub>= -14.45 ± 0.06. Galaxy g - r color constrains the mass-to-light ratio, giving a host stellar mass estimate of log(M<sub>*</sub>/M<sub>◦.</sub>) = 7.32 ± 0.17. Balmer absorption in the stellar continuum, along with the strength of the 4000 Å break, constrains the age of the dominant starburst in the galaxy to be t<sub>burst</sub> = 123±<sup>165</sup><sub>-77</sub> Myr, corresponding to a main-sequence turnoff mass of M/M<sub>◦.</sub> = 4.6<sup>+2.6</sup><sub>-1.4</sub>. Using the R<sub>23</sub> method of calculating metallicity from the fluxes of strong emission lines, we determine the host oxygen abundance to be 12 + log(O/H)<sub>KK04</sub> = 8.01 ± 0.09, significantly lower than any previously reported spectroscopically measured Type Ia supernova host galaxy metallicity. Our data show that SN 2007if is very likely to have originated from a young, metal-poor progenitor.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Galaxies à flambée</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Starburst galaxies</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Galaxias llamarada estelar</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Supernova type I</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Type I supernova</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Supernova tipo I</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Spectrométrie</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Spectroscopy</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Photométrie</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Photometry</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Luminosité</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Luminosity</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Déplacement vers le rouge</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Red shift</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Magnitude absolue</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Absolute magnitude</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Magnitud absoluta</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Couleur</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Color</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Rapport masse luminosité</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Mass to light ratio</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Relación masa luminosidad</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Masse stellaire</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Stellar mass</s0><s5>35</s5></fC03><fC03 i1="11" i2="X" l="FRE"><s0>Continuum</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="ENG"><s0>Continuum</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="SPA"><s0>Continuo</s0><s5>36</s5></fC03><fC03 i1="12" i2="X" l="FRE"><s0>Age</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="ENG"><s0>Age</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="SPA"><s0>Edad</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Métallicité</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Metallicity</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Metalicidad</s0><s5>38</s5></fC03><fC03 i1="14" i2="X" l="FRE"><s0>Raie émission</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="ENG"><s0>Emission line</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="SPA"><s0>Raya emisión</s0><s5>39</s5></fC03><fC03 i1="15" i2="3" l="FRE"><s0>Abondance</s0><s5>40</s5></fC03><fC03 i1="15" i2="3" l="ENG"><s0>Abundance</s0><s5>40</s5></fC03><fC03 i1="16" i2="3" l="FRE"><s0>Galaxies naines</s0><s5>41</s5></fC03><fC03 i1="16" i2="3" l="ENG"><s0>Dwarf galaxies</s0><s5>41</s5></fC03><fN21><s1>178</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 11-0258003 INIST</NO><ET>KECK OBSERVATIONS OF THE YOUNG METAL-POOR HOST GALAXY OF THE SUPER-CHANDRASEKHAR-MASS TYPE Ia SUPERNOVA SN 2007if</ET><AU>CHILDRESS (M.); ALDERING (G.); ARAGON (C.); ANTILOGUS (P.); BAILEY (S.); BALTAY (C.); BONGARD (S.); BUTON (C.); CANTO (A.); CHOTARD (N.); COPIN (Y.); FAKHOURI (H. K.); GANGLER (E.); KERSCHHAGGL (M.); KOWALSKI (M.); HSIAO (E. Y.); LOKEN (S.); NUGENT (P.); PAECH (K.); PAIN (R.); PECONTAL (E.); PEREIRA (R.); PERLMUTTER (S.); RABINOWITZ (D.); RUNGE (K.); SCALZO (R.); THOMAS (R. C.); SMADJA (G.); TAO (C.); WEAVER (B. A.); WU (C.)</AU><AF>Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road/Berkeley, CA 94720/Etats-Unis (1 aut., 2 aut., 3 aut., 5 aut., 12 aut., 16 aut., 17 aut., 23 aut., 25 aut.); Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300/Berkeley, CA 94720-7300/Etats-Unis (1 aut., 12 aut., 23 aut.); Laboratoire de Physique Nucleaire et des Hautes Energies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu/75252 Paris/France (4 aut., 7 aut., 9 aut., 20 aut., 31 aut.); Department of Physics, Yale University/New Haven, CT 06250-8121/Etats-Unis (6 aut., 24 aut., 26 aut.); Physikalisches Institut, Universitat Bonn, Nussallee 12/531 15 Bonn/Allemagne (8 aut., 14 aut., 15 aut., 19 aut.); Université de Lyon, 69622, Lyon; Université de Lyon 1, Villeurbanne; CNRS/IN2P3, Institut de Physique Nucleaire de Lyon/France (10 aut., 11 aut., 13 aut., 22 aut., 28 aut.); Computational Cosmology Center, Computational Research Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road MS 50B-4206/Berkeley, CA 94611/Etats-Unis (18 aut., 27 aut.); Centre de Recherche Astronomique de Lyon, Université Lyon 1, 9 Avenue Charles André/69561 Saint Genis Laval/France (21 aut.); Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, The Australian National University, Cotter Road/Weston ACT 2611/Australie (26 aut.); Centre de Physique des Particules de Marseille, 163, avenue de Luminy, Case 902/13288 Marseille/France (29 aut.); Tsinghua Center for Astrophysics, Tsinghua University/Beijing 100084/Chine (29 aut.); New York University, Center for Cosmology & Particle Physics, 4 Washington Place/New York, NY 10003/Etats-Unis (30 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2011; Vol. 733; No. 1 p. 1; 7333.1-7333.15; Bibl. 3/4 p.</SO><LA>Anglais</LA><EA>We present Keck LRIS spectroscopy and g-band photometry of the metal-poor, low-luminosity host galaxy of the super-Chandrasekhar-mass Type Ia supernova SN 2007if. Deep imaging of the host reveals its apparent magnitude to be mg = 23.15 ± 0.06, which at the spectroscopically measured redshift of Z<sub>helio</sub> = 0.07450 ± 0.00015 corresponds to an absolute magnitude of M<sub>g </sub>= -14.45 ± 0.06. Galaxy g - r color constrains the mass-to-light ratio, giving a host stellar mass estimate of log(M<sub>*</sub>/M<sub>◦.</sub>) = 7.32 ± 0.17. Balmer absorption in the stellar continuum, along with the strength of the 4000 Å break, constrains the age of the dominant starburst in the galaxy to be t<sub>burst</sub> = 123±<sup>165</sup><sub>-77</sub> Myr, corresponding to a main-sequence turnoff mass of M/M<sub>◦.</sub> = 4.6<sup>+2.6</sup><sub>-1.4</sub>. Using the R<sub>23</sub> method of calculating metallicity from the fluxes of strong emission lines, we determine the host oxygen abundance to be 12 + log(O/H)<sub>KK04</sub> = 8.01 ± 0.09, significantly lower than any previously reported spectroscopically measured Type Ia supernova host galaxy metallicity. Our data show that SN 2007if is very likely to have originated from a young, metal-poor progenitor.</EA><CC>001E03</CC><FD>Galaxies à flambée; Supernova type I; Spectrométrie; Photométrie; Luminosité; Déplacement vers le rouge; Magnitude absolue; Couleur; Rapport masse luminosité; Masse stellaire; Continuum; Age; Métallicité; Raie émission; Abondance; Galaxies naines</FD><ED>Starburst galaxies; Type I supernova; Spectroscopy; Photometry; Luminosity; Red shift; Absolute magnitude; Color; Mass to light ratio; Stellar mass; Continuum; Age; Metallicity; Emission line; Abundance; Dwarf galaxies</ED><SD>Galaxias llamarada estelar; Supernova tipo I; Magnitud absoluta; Relación masa luminosidad; Continuo; Edad; Metalicidad; Raya emisión</SD><LO>INIST-512.354000191605310030</LO><ID>11-0258003</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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