The dependence of Type Ia Supernovae luminosities on their host galaxies

被引：401

作者：

Sullivan, M. ^{[1
]}

Conley, A. ^{[2
]}

Howell, D. A. ^{[3
,4
]}

Neill, J. D. ^{[5
]}

Astier, P. ^{[6
]}

Balland, C. ^{[7
,8
]}

Basa, S. ^{[8
]}

Carlberg, R. G. ^{[9
]}

Fouchez, D. ^{[10
]}

Guy, J. ^{[6
]}

Hardin, D. ^{[6
]}

Hook, I. M. ^{[1
,11
]}

Pain, R. ^{[6
]}

Palanque-Delabrouille, N. ^{[12
]}

Perrett, K. M. ^{[9
,13
]}

Pritchet, C. J. ^{[14
]}

Regnault, N. ^{[6
]}

Rich, J. ^{[12
]}

Ruhlmann-Kleider, V. ^{[12
]}

Baumont, S. ^{[6
,15
]}

Hsiao, E. ^{[16
]}

Kronborg, T. ^{[6
]}

Lidman, C. ^{[17
]}

Perlmutter, S. ^{[16
,18
]}

Walker, E. S. ^{[1
,19
]}

机构：

[1] Univ Oxford, Dept Phys Astrophys, DWB, Oxford OX1 3RH, England

[2] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA

[3] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA

[4] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[5] CALTECH, Pasadena, CA 91125 USA

[6] Univ Paris 07, Univ Paris 06, LPNHE, CNRS,IN2P3, F-75252 Paris 05, France

[7] Univ Paris 11, F-91405 Orsay, France

[8] LAM, F-13388 Marseille 13, France

[9] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada

[10] Aix Marseille Univ, CPPM, CNRS, IN2P3, F-13288 Marseille 9, France

[11] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy

[12] CEA Saclay, DSM Irfu Spp, F-91191 Gif Sur Yvette, France

[13] DRDC Ottawa, Network Informat Operat, Ottawa, ON K1A 0Z4, Canada

[14] Univ Victoria, Dept Phys & Astron, Victoria, BC V8T 1M8, Canada

[15] CNRS IN2P3, LPSC, F-38026 Grenoble, France

[16] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA

[17] Anglo Australian Observ, Epping, NSW 1710, Australia

[18] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[19] Scuola Normale Super Pisa, I-56126 Pisa, Italy

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2010年 / 406卷 / 02期

基金：

加拿大自然科学与工程研究理事会;

关键词：

supernovae: general; cosmology: observations; distance scale; MASS-METALLICITY RELATION; HUBBLE-SPACE-TELESCOPE; BVRI LIGHT CURVES; DEEP SURVEY; STAR-FORMATION; LEGACY SURVEY; CONSTRAINTS; EVOLUTION; DIAGRAM; AGE;

D O I：

10.1111/j.1365-2966.2010.16731.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Precision cosmology with Type la 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 (similar or equal to 4.0 sigma) 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 ('beta') between their luminosities and colours with similar to 2.7 sigma significance, and a smaller scatter on SN la 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 la luminosity differences consequently introduce a systematic error in cosmological analyses, comparable to the current statistical uncertainties on parameters such as in, 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 chi(2) (3.8 sigma-4.5 sigma); linear corrections based on host parameters do not perform as well. We conclude that all future SN la cosmological analyses should use a correction of this (or similar) form to control demographic shifts in the underlying galaxy population.

引用

页码：782 / 802

页数：21

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