The dependence of Type Ia Supernovae luminosities on their host galaxies
Identifieur interne : 000958 ( Istex/Checkpoint ); précédent : 000957; suivant : 000959The dependence of Type Ia Supernovae luminosities on their host galaxies
Auteurs : M. Sullivan [Royaume-Uni] ; A. Conley [États-Unis] ; D. A. Howell [États-Unis] ; J. D. Neill [États-Unis] ; P. Astier [France] ; C. Balland [France] ; S. Basa [France] ; R. G. Carlberg [Canada] ; D. Fouchez [France] ; J. Guy [France] ; D. Hardin [France] ; I. M. Hook [Royaume-Uni, Italie] ; R. Pain [France] ; N. Palanque-Delabrouille [France] ; K. M. Perrett [Canada] ; C. J. Pritchet [Canada] ; N. Regnault [France] ; J. Rich [France] ; V. Ruhlmann-Kleider [France] ; S. Baumont [France] ; E. Hsiao [États-Unis] ; T. Kronborg [France] ; C. Lidman [Australie] ; S. Perlmutter [États-Unis] ; E. S. Walker [Royaume-Uni, Italie]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2010-08-01.
Abstract
Precision cosmology with Type Ia supernovae (SNe Ia) makes use of the fact that SN Ia luminosities depend on their light-curve shapes and colours. Using Supernova Legacy Survey (SNLS) and other data, we show that there is an additional dependence on the global characteristics of their host galaxies: events of the same light-curve shape and colour are, on average, 0.08 mag (≃4.0σ) brighter in massive host galaxies (presumably metal-rich) and galaxies with low specific star formation rates (sSFR). These trends do not depend on any assumed cosmological model, and are independent of the SN light-curve width: both fast and slow-declining events show the same trends. SNe Ia in galaxies with a low sSFR also have a smaller slope (‘β’) between their luminosities and colours with ∼2.7σ significance, and a smaller scatter on SN Ia Hubble diagrams (at 95 per cent confidence), though the significance of these effects is dependent on the reddest SNe. SN Ia colours are similar between low-mass and high-mass hosts, leading us to interpret their luminosity differences as an intrinsic property of the SNe and not of some external factor such as dust. If the host stellar mass is interpreted as a metallicity indicator using galaxy mass–metallicity relations, the luminosity trends are in qualitative agreement with theoretical predictions. We show that the average stellar mass, and therefore the average metallicity, of our SN Ia host galaxies decreases with redshift. The SN Ia luminosity differences consequently introduce a systematic error in cosmological analyses, comparable to the current statistical uncertainties on parameters such as w, the equation of state of dark energy. We show that the use of two SN Ia absolute magnitudes, one for events in high-mass (metal-rich) galaxies and the other for events in low-mass (metal-poor) galaxies, adequately corrects for the differences. Cosmological fits incorporating these terms give a significant reduction in χ2 (3.8σ–4.5σ); linear corrections based on host parameters do not perform as well. We conclude that all future SN Ia cosmological analyses should use a correction of this (or similar) form to control demographic shifts in the underlying galaxy population.
Url:
DOI: 10.1111/j.1365-2966.2010.16731.x
Affiliations:
- Australie, Canada, France, Italie, Royaume-Uni, États-Unis
- Angleterre, Californie, Colorado, Ontario, Oxfordshire, Provence-Alpes-Côte d'Azur, Toscane, Île-de-France
- Gif-sur-Yvette, Marseille, Oxford, Paris, Pise, Toronto
- Université d'Aix-Marseille, Université d'Oxford, Université de Toronto
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Pritchet</name><affiliation wicri:level="1"><country xml:lang="fr">Canada</country><wicri:regionArea>Department of Physics and Astronomy, University of Victoria, PO Box 3055 STN CSC, Victoria BC V8T 1M8</wicri:regionArea><wicri:noRegion>Victoria BC V8T 1M8</wicri:noRegion></affiliation></author><author><name sortKey="Regnault, N" sort="Regnault, N" uniqKey="Regnault N" first="N." last="Regnault">N. Regnault</name><affiliation wicri:level="3"><country xml:lang="fr">France</country><wicri:regionArea>LPNHE, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu, 75252 Paris Cedex 05</wicri:regionArea><placeName><region type="region" nuts="2">Île-de-France</region><settlement type="city">Paris</settlement></placeName></affiliation></author><author><name sortKey="Rich, J" sort="Rich, J" uniqKey="Rich J" first="J." last="Rich">J. Rich</name><affiliation wicri:level="1"><country xml:lang="fr">France</country><wicri:regionArea>CEA/Saclay, DSM/Irfu/Spp, 91191 Gif-sur-Yvette Cedex</wicri:regionArea><wicri:noRegion>91191 Gif-sur-Yvette Cedex</wicri:noRegion><wicri:noRegion>91191 Gif-sur-Yvette Cedex</wicri:noRegion></affiliation></author><author><name sortKey="Ruhlmann Kleider, V" sort="Ruhlmann Kleider, V" uniqKey="Ruhlmann Kleider V" first="V." last="Ruhlmann-Kleider">V. Ruhlmann-Kleider</name><affiliation wicri:level="3"><country xml:lang="fr">France</country><wicri:regionArea>CEA/Saclay, DSM/Irfu/Spp, 91191 Gif-sur-Yvette Cedex</wicri:regionArea><placeName><region type="region" nuts="2">Île-de-France</region><settlement type="city">Gif-sur-Yvette</settlement></placeName></affiliation></author><author><name sortKey="Baumont, S" sort="Baumont, S" uniqKey="Baumont S" first="S." last="Baumont">S. Baumont</name><affiliation wicri:level="1"><country xml:lang="fr">France</country><wicri:regionArea>LPNHE, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu, 75252 Paris Cedex 05</wicri:regionArea><wicri:noRegion>75252 Paris Cedex 05</wicri:noRegion><wicri:noRegion>75252 Paris Cedex 05</wicri:noRegion></affiliation><affiliation wicri:level="1"><country xml:lang="fr">France</country><wicri:regionArea>LPSC, CNRS-IN2P3, 53 rue des Martyrs, 38026 Grenoble Cedex</wicri:regionArea><wicri:noRegion>38026 Grenoble Cedex</wicri:noRegion><wicri:noRegion>38026 Grenoble Cedex</wicri:noRegion></affiliation></author><author><name sortKey="Hsiao, E" sort="Hsiao, E" uniqKey="Hsiao E" first="E." last="Hsiao">E. Hsiao</name><affiliation wicri:level="2"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Lawrence Berkeley National Laboratory, Mail Stop 50-232, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720</wicri:regionArea><placeName><region type="state">Californie</region></placeName></affiliation></author><author><name sortKey="Kronborg, T" sort="Kronborg, T" uniqKey="Kronborg T" first="T." last="Kronborg">T. Kronborg</name><affiliation wicri:level="3"><country xml:lang="fr">France</country><wicri:regionArea>LPNHE, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu, 75252 Paris Cedex 05</wicri:regionArea><placeName><region type="region" nuts="2">Île-de-France</region><settlement type="city">Paris</settlement></placeName></affiliation></author><author><name sortKey="Lidman, C" sort="Lidman, C" uniqKey="Lidman C" first="C." last="Lidman">C. Lidman</name><affiliation wicri:level="1"><country xml:lang="fr">Australie</country><wicri:regionArea>Anglo-Australian Observatory, PO Box 296, Epping, NSW 1710</wicri:regionArea><wicri:noRegion>NSW 1710</wicri:noRegion></affiliation></author><author><name sortKey="Perlmutter, S" sort="Perlmutter, S" uniqKey="Perlmutter S" first="S." last="Perlmutter">S. Perlmutter</name><affiliation wicri:level="2"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Lawrence Berkeley National Laboratory, Mail Stop 50-232, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720</wicri:regionArea><placeName><region type="state">Californie</region></placeName></affiliation><affiliation wicri:level="2"><country xml:lang="fr">États-Unis</country><wicri:regionArea>Department of Physics, University of California, 366 LeConte Hall MC 7300, Berkeley, CA 94720-7300</wicri:regionArea><placeName><region type="state">Californie</region></placeName></affiliation></author><author><name sortKey="Walker, E S" sort="Walker, E S" uniqKey="Walker E" first="E. S." last="Walker">E. S. Walker</name><affiliation wicri:level="4"><orgName type="university">Université d'Oxford</orgName><country>Royaume-Uni</country><placeName><settlement type="city">Oxford</settlement><region type="nation">Angleterre</region><region type="région" nuts="1">Oxfordshire</region></placeName></affiliation><affiliation wicri:level="1"><country xml:lang="fr">Italie</country><wicri:regionArea>Scuola Normale Superiore, Piazza dei Cavalieri 7, 56126 Pisa</wicri:regionArea><placeName><settlement type="city">Pise</settlement><region nuts="2">Toscane</region></placeName></affiliation></author></analytic><monogr></monogr><series><title level="j">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbrev">Monthly Notices of the Royal Astronomical Society</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2010-08-01">2010-08-01</date><biblScope unit="volume">406</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="782">782</biblScope><biblScope unit="page" to="802">802</biblScope></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass></textClass></profileDesc></teiHeader><front><div type="abstract">Precision cosmology with Type Ia supernovae (SNe Ia) makes use of the fact that SN Ia luminosities depend on their light-curve shapes and colours. Using Supernova Legacy Survey (SNLS) and other data, we show that there is an additional dependence on the global characteristics of their host galaxies: events of the same light-curve shape and colour are, on average, 0.08 mag (≃4.0σ) brighter in massive host galaxies (presumably metal-rich) and galaxies with low specific star formation rates (sSFR). These trends do not depend on any assumed cosmological model, and are independent of the SN light-curve width: both fast and slow-declining events show the same trends. SNe Ia in galaxies with a low sSFR also have a smaller slope (‘β’) between their luminosities and colours with ∼2.7σ significance, and a smaller scatter on SN Ia Hubble diagrams (at 95 per cent confidence), though the significance of these effects is dependent on the reddest SNe. SN Ia colours are similar between low-mass and high-mass hosts, leading us to interpret their luminosity differences as an intrinsic property of the SNe and not of some external factor such as dust. If the host stellar mass is interpreted as a metallicity indicator using galaxy mass–metallicity relations, the luminosity trends are in qualitative agreement with theoretical predictions. We show that the average stellar mass, and therefore the average metallicity, of our SN Ia host galaxies decreases with redshift. The SN Ia luminosity differences consequently introduce a systematic error in cosmological analyses, comparable to the current statistical uncertainties on parameters such as w, the equation of state of dark energy. We show that the use of two SN Ia absolute magnitudes, one for events in high-mass (metal-rich) galaxies and the other for events in low-mass (metal-poor) galaxies, adequately corrects for the differences. Cosmological fits incorporating these terms give a significant reduction in χ2 (3.8σ–4.5σ); linear corrections based on host parameters do not perform as well. We conclude that all future SN Ia cosmological analyses should use a correction of this (or similar) form to control demographic shifts in the underlying galaxy population.</div></front></TEI><affiliations><list><country><li>Australie</li><li>Canada</li><li>France</li><li>Italie</li><li>Royaume-Uni</li><li>États-Unis</li></country><region><li>Angleterre</li><li>Californie</li><li>Colorado</li><li>Ontario</li><li>Oxfordshire</li><li>Provence-Alpes-Côte d'Azur</li><li>Toscane</li><li>Île-de-France</li></region><settlement><li>Gif-sur-Yvette</li><li>Marseille</li><li>Oxford</li><li>Paris</li><li>Pise</li><li>Toronto</li></settlement><orgName><li>Université d'Aix-Marseille</li><li>Université d'Oxford</li><li>Université de Toronto</li></orgName></list><tree><country name="Royaume-Uni"><region name="Angleterre"><name sortKey="Sullivan, M" sort="Sullivan, M" uniqKey="Sullivan M" first="M." last="Sullivan">M. Sullivan</name></region><name sortKey="Hook, I M" sort="Hook, I M" uniqKey="Hook I" first="I. M." last="Hook">I. M. Hook</name><name sortKey="Sullivan, M" sort="Sullivan, M" uniqKey="Sullivan M" first="M." last="Sullivan">M. Sullivan</name><name sortKey="Sullivan, M" sort="Sullivan, M" uniqKey="Sullivan M" first="M." last="Sullivan">M. Sullivan</name><name sortKey="Walker, E S" sort="Walker, E S" uniqKey="Walker E" first="E. S." last="Walker">E. S. Walker</name></country><country name="États-Unis"><region name="Colorado"><name sortKey="Conley, A" sort="Conley, A" uniqKey="Conley A" first="A." last="Conley">A. Conley</name></region><name sortKey="Howell, D A" sort="Howell, D A" uniqKey="Howell D" first="D. A." last="Howell">D. A. Howell</name><name sortKey="Howell, D A" sort="Howell, D A" uniqKey="Howell D" first="D. A." last="Howell">D. A. Howell</name><name sortKey="Hsiao, E" sort="Hsiao, E" uniqKey="Hsiao E" first="E." last="Hsiao">E. Hsiao</name><name sortKey="Neill, J D" sort="Neill, J D" uniqKey="Neill J" first="J. D." last="Neill">J. D. Neill</name><name sortKey="Perlmutter, S" sort="Perlmutter, S" uniqKey="Perlmutter S" first="S." last="Perlmutter">S. Perlmutter</name><name sortKey="Perlmutter, S" sort="Perlmutter, S" uniqKey="Perlmutter S" first="S." last="Perlmutter">S. Perlmutter</name></country><country name="France"><noRegion><name sortKey="Astier, P" sort="Astier, P" uniqKey="Astier P" first="P." last="Astier">P. Astier</name></noRegion><name sortKey="Balland, C" sort="Balland, C" uniqKey="Balland C" first="C." last="Balland">C. Balland</name><name sortKey="Balland, C" sort="Balland, C" uniqKey="Balland C" first="C." last="Balland">C. Balland</name><name sortKey="Basa, S" sort="Basa, S" uniqKey="Basa S" first="S." last="Basa">S. Basa</name><name sortKey="Baumont, S" sort="Baumont, S" uniqKey="Baumont S" first="S." last="Baumont">S. Baumont</name><name sortKey="Baumont, S" sort="Baumont, S" uniqKey="Baumont S" first="S." last="Baumont">S. Baumont</name><name sortKey="Fouchez, D" sort="Fouchez, D" uniqKey="Fouchez D" first="D." last="Fouchez">D. Fouchez</name><name sortKey="Guy, J" sort="Guy, J" uniqKey="Guy J" first="J." last="Guy">J. Guy</name><name sortKey="Hardin, D" sort="Hardin, D" uniqKey="Hardin D" first="D." last="Hardin">D. Hardin</name><name sortKey="Kronborg, T" sort="Kronborg, T" uniqKey="Kronborg T" first="T." last="Kronborg">T. Kronborg</name><name sortKey="Pain, R" sort="Pain, R" uniqKey="Pain R" first="R." last="Pain">R. Pain</name><name sortKey="Palanque Delabrouille, N" sort="Palanque Delabrouille, N" uniqKey="Palanque Delabrouille N" first="N." last="Palanque-Delabrouille">N. Palanque-Delabrouille</name><name sortKey="Regnault, N" sort="Regnault, N" uniqKey="Regnault N" first="N." last="Regnault">N. Regnault</name><name sortKey="Rich, J" sort="Rich, J" uniqKey="Rich J" first="J." last="Rich">J. Rich</name><name sortKey="Ruhlmann Kleider, V" sort="Ruhlmann Kleider, V" uniqKey="Ruhlmann Kleider V" first="V." last="Ruhlmann-Kleider">V. Ruhlmann-Kleider</name></country><country name="Canada"><region name="Ontario"><name sortKey="Carlberg, R G" sort="Carlberg, R G" uniqKey="Carlberg R" first="R. G." last="Carlberg">R. G. Carlberg</name></region><name sortKey="Perrett, K M" sort="Perrett, K M" uniqKey="Perrett K" first="K. M." last="Perrett">K. M. Perrett</name><name sortKey="Perrett, K M" sort="Perrett, K M" uniqKey="Perrett K" first="K. M." last="Perrett">K. M. Perrett</name><name sortKey="Pritchet, C J" sort="Pritchet, C J" uniqKey="Pritchet C" first="C. J." last="Pritchet">C. J. Pritchet</name></country><country name="Italie"><noRegion><name sortKey="Hook, I M" sort="Hook, I M" uniqKey="Hook I" first="I. M." last="Hook">I. M. Hook</name></noRegion><name sortKey="Walker, E S" sort="Walker, E S" uniqKey="Walker E" first="E. S." last="Walker">E. S. 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