AustralieFrV1, Main, Exploration, bibRecord, 007154

The dependence of Type Ia Supernovae luminosities on their host galaxies

Identifieur interne : 007154 ( Main/Exploration ); précédent : 007153; suivant : 007155

The 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.

RBID : ISTEX:171F7651FBADFA4C4F2307DF89CB4F31FF707EE9

Descripteurs français

Pascal (Inist)
- Calcul erreur, Correction, Cosmologie, Couleur, Courbe lumière, Diagramme Hubble, Déplacement vers le rouge, Echelle distance, Energie sombre, Equation état, Formation stellaire, Galaxies, Incertitude, Luminosité, Magnitude absolue, Masse stellaire, Modèle cosmologique, Métallicité, Paramètre statistique, Supernova type I, Taux formation.
Wicri :
- topic : Cosmologie, Nuisance.

English descriptors

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:

Le document en format XML

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<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" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title>
<idno type="ISSN">0035-8711</idno>
<idno type="eISSN">1365-2966</idno>
<imprint><biblScope unit="vol">406</biblScope>
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<publisher>Blackwell Publishing Ltd</publisher>
<pubPlace>Oxford, UK</pubPlace>
<date type="published" when="2010-08-01">2010-08-01</date>
</imprint>
<idno type="ISSN">0035-8711</idno>
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</seriesStmt>
</fileDesc>
<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Absolute magnitude</term>
<term>Absolute magnitudes</term>
<term>Binned points</term>
<term>Cfht</term>
<term>Color</term>
<term>Colour</term>
<term>Colour corrections</term>
<term>Colours</term>
<term>Conley</term>
<term>Corrections</term>
<term>Cosmological</term>
<term>Cosmological analyses</term>
<term>Cosmological model</term>
<term>Cosmological models</term>
<term>Cosmological parameters</term>
<term>Cosmological results</term>
<term>Cosmology</term>
<term>Dark energy</term>
<term>Della valle</term>
<term>Different values</term>
<term>Distance scale</term>
<term>Elliptical galaxies</term>
<term>Equations of state</term>
<term>Error analysis</term>
<term>Error bars</term>
<term>Extra parameter</term>
<term>Fainter</term>
<term>Formation rate</term>
<term>Galaxies</term>
<term>Galaxy</term>
<term>Gallagher</term>
<term>Hamuy</term>
<term>Hicken</term>
<term>Host</term>
<term>Host dependence</term>
<term>Host galaxies</term>
<term>Host galaxy</term>
<term>Host galaxy mstellar</term>
<term>Host galaxy parameters</term>
<term>Host galaxy photometry</term>
<term>Host galaxy properties</term>
<term>Host galaxy ssfr</term>
<term>Host galaxy type</term>
<term>Host parameter</term>
<term>Host properties</term>
<term>Hosts show</term>
<term>Howell</term>
<term>Hubble</term>
<term>Hubble diagram</term>
<term>Hubble residuals</term>
<term>Journal compilation</term>
<term>Kirshner</term>
<term>Light curves</term>
<term>Lled circles</term>
<term>Luminosity</term>
<term>Luminosity trends</term>
<term>Massive galaxies</term>
<term>Metallicities</term>
<term>Metallicity</term>
<term>Mnras</term>
<term>More metal</term>
<term>Mstellar</term>
<term>National research council</term>
<term>Nuisance</term>
<term>Nuisance parameters</term>
<term>Nuisance variables</term>
<term>Open circles</term>
<term>Parameter</term>
<term>Peak luminosities</term>
<term>Peak magnitudes</term>
<term>Percentage increase</term>
<term>Photometric</term>
<term>Photometry</term>
<term>Progenitor</term>
<term>Red shift</term>
<term>Reddest</term>
<term>Redshift</term>
<term>Residual</term>
<term>Residual axis</term>
<term>Residual error</term>
<term>Riess</term>
<term>Salt2</term>
<term>Same trends</term>
<term>Samples split</term>
<term>Scatter</term>
<term>Selection effect</term>
<term>Selection effects</term>
<term>Sifto</term>
<term>Similar results</term>
<term>Smaller scatter</term>
<term>Snls</term>
<term>Snls data</term>
<term>Snls sample</term>
<term>Spectroscopic</term>
<term>Split point</term>
<term>Split points</term>
<term>Ssfr</term>
<term>Star formation</term>
<term>Statistical errors</term>
<term>Statistical parameter</term>
<term>Stellar</term>
<term>Stellar mass</term>
<term>Stellar masses</term>
<term>Stellar metallicity</term>
<term>Straight line</term>
<term>Supernova</term>
<term>Systematic error</term>
<term>Systematic errors</term>
<term>Tting</term>
<term>Type I supernova</term>
<term>Uncertainty</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Calcul erreur</term>
<term>Correction</term>
<term>Cosmologie</term>
<term>Couleur</term>
<term>Courbe lumière</term>
<term>Diagramme Hubble</term>
<term>Déplacement vers le rouge</term>
<term>Echelle distance</term>
<term>Energie sombre</term>
<term>Equation état</term>
<term>Formation stellaire</term>
<term>Galaxies</term>
<term>Incertitude</term>
<term>Luminosité</term>
<term>Magnitude absolue</term>
<term>Masse stellaire</term>
<term>Modèle cosmologique</term>
<term>Métallicité</term>
<term>Paramètre statistique</term>
<term>Supernova type I</term>
<term>Taux formation</term>
</keywords>
<keywords scheme="Teeft" xml:lang="en"><term>Absolute magnitudes</term>
<term>Binned points</term>
<term>Cfht</term>
<term>Colour</term>
<term>Colour corrections</term>
<term>Colours</term>
<term>Conley</term>
<term>Corrections</term>
<term>Cosmological</term>
<term>Cosmological analyses</term>
<term>Cosmological model</term>
<term>Cosmological parameters</term>
<term>Cosmological results</term>
<term>Cosmology</term>
<term>Dark energy</term>
<term>Della valle</term>
<term>Different values</term>
<term>Elliptical galaxies</term>
<term>Error bars</term>
<term>Extra parameter</term>
<term>Fainter</term>
<term>Galaxy</term>
<term>Gallagher</term>
<term>Hamuy</term>
<term>Hicken</term>
<term>Host</term>
<term>Host dependence</term>
<term>Host galaxies</term>
<term>Host galaxy</term>
<term>Host galaxy mstellar</term>
<term>Host galaxy parameters</term>
<term>Host galaxy photometry</term>
<term>Host galaxy properties</term>
<term>Host galaxy ssfr</term>
<term>Host galaxy type</term>
<term>Host parameter</term>
<term>Host properties</term>
<term>Hosts show</term>
<term>Howell</term>
<term>Hubble</term>
<term>Hubble diagram</term>
<term>Hubble residuals</term>
<term>Journal compilation</term>
<term>Kirshner</term>
<term>Light curves</term>
<term>Lled circles</term>
<term>Luminosity</term>
<term>Luminosity trends</term>
<term>Massive galaxies</term>
<term>Metallicities</term>
<term>Metallicity</term>
<term>Mnras</term>
<term>More metal</term>
<term>Mstellar</term>
<term>National research council</term>
<term>Nuisance</term>
<term>Nuisance parameters</term>
<term>Nuisance variables</term>
<term>Open circles</term>
<term>Parameter</term>
<term>Peak luminosities</term>
<term>Peak magnitudes</term>
<term>Percentage increase</term>
<term>Photometric</term>
<term>Photometry</term>
<term>Progenitor</term>
<term>Reddest</term>
<term>Redshift</term>
<term>Residual</term>
<term>Residual axis</term>
<term>Residual error</term>
<term>Riess</term>
<term>Salt2</term>
<term>Same trends</term>
<term>Samples split</term>
<term>Scatter</term>
<term>Selection effect</term>
<term>Selection effects</term>
<term>Sifto</term>
<term>Similar results</term>
<term>Smaller scatter</term>
<term>Snls</term>
<term>Snls data</term>
<term>Snls sample</term>
<term>Spectroscopic</term>
<term>Split point</term>
<term>Split points</term>
<term>Ssfr</term>
<term>Star formation</term>
<term>Statistical errors</term>
<term>Stellar</term>
<term>Stellar mass</term>
<term>Stellar masses</term>
<term>Stellar metallicity</term>
<term>Straight line</term>
<term>Supernova</term>
<term>Systematic error</term>
<term>Systematic errors</term>
<term>Tting</term>
</keywords>
<keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Cosmologie</term>
<term>Nuisance</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">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>Auvergne-Rhône-Alpes</li>
<li>Californie</li>
<li>Colorado</li>
<li>Ontario</li>
<li>Oxfordshire</li>
<li>Provence-Alpes-Côte d'Azur</li>
<li>Rhône-Alpes</li>
<li>Toscane</li>
<li>Île-de-France</li>
</region>
<settlement><li>Gif‐sur‐Yvette</li>
<li>Grenoble</li>
<li>Marseille</li>
<li>Oxford</li>
<li>Paris</li>
<li>Pise</li>
<li>Toronto</li>
</settlement>
<orgName><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="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 Elabrouille, N" sort="Palanque Elabrouille, N" uniqKey="Palanque Elabrouille 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 Leider, V" sort="Ruhlmann Leider, V" uniqKey="Ruhlmann Leider 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. Walker</name>
</country>
<country name="Australie"><noRegion><name sortKey="Lidman, C" sort="Lidman, C" uniqKey="Lidman C" first="C." last="Lidman">C. Lidman</name>
</noRegion>
</country>
</tree>
</affiliations>
</record>

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Serveur d'exploration sur les relations entre la France et l'Australie

The dependence of Type Ia Supernovae luminosities on their host galaxies

The dependence of Type Ia Supernovae luminosities on their host galaxies

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