THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. II. THE TYPE Ia SUPERNOVA RATE IN HIGH-REDSHIFT GALAXY CLUSTERS

被引：38

作者：

Barbary, K. ^{[1
,2
]}

Aldering, G. ^{[2
]}

Amanullah, R. ^{[1
,3
]}

Brodwin, M. ^{[4
]}

Connolly, N. ^{[5
]}

Dawson, K. S. ^{[2
,6
]}

Doi, M. ^{[7
]}

Eisenhardt, P. ^{[8
]}

Faccioli, L. ^{[2
]}

Fadeyev, V. ^{[9
]}

Fakhouri, H. K. ^{[1
,2
]}

Fruchter, A. S. ^{[10
]}

Gilbank, D. G. ^{[11
]}

Gladders, M. D. ^{[12
]}

Goldhaber, G. ^{[1
,2
]}

Goobar, A. ^{[3
,13
]}

Hattori, T. ^{[14
]}

Hsiao, E. ^{[2
]}

Huang, X. ^{[1
]}

Ihara, Y. ^{[7
]}

Kashikawa, N. ^{[15
]}

Koester, B. ^{[12
,16
]}

Konishi, K. ^{[17
]}

Kowalski, M. ^{[18
]}

Lidman, C. ^{[19
]}

Lubin, L. ^{[20
]}

Meyers, J. ^{[1
,2
]}

Morokuma, T. ^{[7
,15
]}

Oda, T. ^{[21
]}

Panagia, N. ^{[10
]}

Perlmutter, S. ^{[1
,2
]}

Postman, M. ^{[10
]}

Ripoche, P. ^{[2
]}

Rosati, P. ^{[22
]}

Rubin, D. ^{[1
,2
]}

Schlegel, D. J. ^{[2
]}

Spadafora, A. L. ^{[2
]}

Stanford, S. A. ^{[20
,23
]}

Strovink, M. ^{[1
,2
]}

Suzuki, N. ^{[2
]}

Takanashi, N. ^{[15
]}

Tokita, K. ^{[7
]}

Yasuda, N. ^{[17
]}

机构：

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

[2] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA

[3] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden

[4] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[5] Hamilton Coll, Dept Phys, Clinton, NY 13323 USA

[6] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA

[7] Univ Tokyo, Grad Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan

[8] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[9] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 94064 USA

[10] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[11] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada

[12] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA

[13] Stockholm Univ, Albanova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden

[14] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA

[15] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan

[16] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[17] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan

[18] Univ Bonn, Inst Phys, Bonn, Germany

[19] Australian Astron Observ, Epping, NSW 1710, Australia

[20] Univ Calif Davis, Dept Phys, Davis, CA 95618 USA

[21] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan

[22] ESO, D-85748 Garching, Germany

[23] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 745卷 / 01期

基金：

澳大利亚研究理事会; 日本学术振兴会;

关键词：

cosmology: observations; supernovae: general; white dwarfs; DELAY-TIME DISTRIBUTION; DIGITAL SKY SURVEY; INTRACLUSTER PLANETARY-NEBULAE; DIFFUSE OPTICAL LIGHT; SIMILAR-TO; X-RAY; LUMINOSITY FUNCTION; RED-SEQUENCE; STELLAR MASS; XMMXCS J2215.9-1738;

D O I：

10.1088/0004-637X/745/1/32

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report a measurement of the Type Ia supernova (SN Ia) rate in galaxy clusters at 0.9 < z < 1.46 from the Hubble Space Telescope Cluster Supernova Survey. This is the first cluster SN Ia rate measurement with detected z > 0.9 SNe. Finding 8 +/- 1 cluster SNe Ia, we determine an SN Ia rate of 0.50(-0.19)(+0.23) (stat) (+0.10)(-0.09) (sys) h(70)(2) SNuB (SNuB equivalent to 10(-12) SNe (L-1)circle dot(,B) yr(-1)). In units of stellar mass, this translates to 0.36(-0.13)(+0.16) (stat) (+0.07)(-0.06) (sys) h(70)(2) SNuM (SNuM = 10(-12) SNe M-1 circle dot yr(-1)). This represents a factor of approximate to 5 +/- 2 increase over measurements of the cluster rate at z < 0.2. We parameterize the late-time SN Ia delay time distribution (DTD) with a power law: Psi(t) t(s). Under the approximation of a single-burst cluster formation redshift of z(f) = 3, our rate measurement in combination with lower-redshift cluster SN Ia rates constrains s = -1.41(-0.40)(+0.47), consistent with measurements of the DTD in the field. This measurement is generally consistent with expectations for the "double degenerate" scenario and inconsistent with some models for the "single degenerate" scenario predicting a steeper DTD at large delay times. We check for environmental dependence and the influence of younger stellar populations by calculating the rate specifically in cluster red-sequence galaxies and in morphologically early-type galaxies, finding results similar to the full cluster rate. Finally, the upper limit of one hostless cluster SN Ia detected in the survey implies that the fraction of stars in the intra-cluster medium is less than 0.47 (95% confidence), consistent with measurements at lower redshifts.

引用

页数：28

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