Rates and properties of Type Ia supernovae in galaxy clusters within the dark energy survey

被引：3

作者：

Toy, M. ^{[1
]}

Wiseman, P. ^{[1
]}

Sullivan, M. ^{[1
]}

Frohmaier, C. ^{[1
,16
]}

Graur, O. ^{[2
,3
]}

Palmese, A. ^{[4
]}

Popovic, B. ^{[5
]}

Davis, T. M. ^{[6
]}

Galbany, L. ^{[7
,8
]}

Kelsey, L. ^{[2
]}

Lidman, C. ^{[9
,10
]}

Scolnic, D. ^{[5
]}

Allam, S. ^{[11
]}

Desai, S. ^{[12
]}

Abbott, T. M. C. ^{[13
]}

Aguena, M. ^{[14
]}

Alves, O. ^{[15
]}

Annis, J. ^{[11
]}

Bacon, D.

Bertin, E. ^{[16
,17
]}

Brooks, D. ^{[18
]}

Burke, D. L. ^{[19
,20
]}

Rosell, A. Carnero ^{[21
,22
]}

Kind, M. Carrasco ^{[23
,24
]}

Carretero, J. ^{[25
]}

Castander, F. J. ^{[7
,8
]}

Conselice, C. ^{[26
,27
]}

da Costa, L. N.

Pereira, M. E. S. ^{[28
]}

De Vicente, J. ^{[29
]}

Diehl, H. T. ^{[11
]}

Doel, P. ^{[18
]}

Everett, S. ^{[30
]}

Ferrero, I ^{[31
]}

Frieman, J. ^{[11
,32
]}

Gerdes, D. W. ^{[15
,33
]}

Gruen, D. ^{[34
]}

Gruendl, R. A. ^{[23
,24
]}

Gutierrez, G. ^{[11
]}

Hinton, S. R. ^{[6
]}

Hollowood, D. L. ^{[35
]}

Honscheid, K. ^{[36
,37
]}

James, D. J. ^{[38
]}

Kuehn, K. ^{[39
,40
]}

Kuropatkin, N. ^{[11
]}

Marshall, J. L. ^{[41
,42
]}

Melchior, P. ^{[43
]}

Mena-Fernandez, J.

Menanteau, F. ^{[23
,24
]}

Miquel, R. ^{[25
,44
]}

机构：

[1] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, England

[2] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, England

[3] Amer Museum Nat Hist, Dept Astrophys, Cent Pk West & 79th St, New York, NY 10024 USA

[4] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15312 USA

[5] Duke Univ, Dept Phys, Durham, NC 27708 USA

[6] Univ Queensland, Sch Math & Phys, Brisbane, QLD 4072, Australia

[7] Inst Estudis Espacials Catalunya IEEC, E-08034 Barcelona, Spain

[8] CSIC, Inst Space Sci ICE, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain

[9] Australian Natl Univ, Coll Sci, Ctr Gravitat Astrophys, Canberra, ACT 2601, Australia

[10] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2601, Australia

[11] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA

[12] IIT Hyderabad, Dept Phys, Kandi 502285, Telangana, India

[13] NSFs Natl Opt Infrared Astron Res Lab, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile

[14] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[15] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[16] Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France

[17] UPMC Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France

[18] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England

[19] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol KIPAC, POB 2450, Stanford, CA 94305 USA

[20] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA

[21] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Tenerife, Spain

[22] Univ La Laguna, Dept Astrofis, E-38206 San Cristobal la Laguna, Tenerife, Spain

[23] Natl Ctr Supercomp Applicat, Ctr Astrophys Surveys, 1205 West Clark St, Urbana, IL 61801 USA

[24] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA

[25] Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain

[26] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Oxford Rd, Manchester M13 9PL, England

[27] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England

[28] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany

[29] Ctr Invest Energet Medioambientales & Tecnol CIEM, 40, E-28040 Madrid, Spain

[30] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[31] Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, N-0315 Oslo, Norway

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

[33] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[34] Ludwig Maximilians Univ Munchen, Univ Observ, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany

[35] Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA

[36] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[37] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA

[38] Ctr Astrophys Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138 USA

[39] Macquarie Univ, Australian Astron Opt, N Ryde, NSW 2113, Australia

[40] Lowell Observ, 1400 Mars Hill Rd, Flagstaff, AZ 86001 USA

[41] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA

[42] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA

[43] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA

[44] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain

[45] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[46] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, England

[47] Univ Claude Bernard Lyon 1, Univ Lyon, CNRS, IP2I Lyon IN2P3,IMR 5822, F-69622 Villeurbanne, France

[48] Oak Ridge Natl Lab, Comp Sci & Math Div, Oak Ridge, TN 37831 USA

[49] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 526卷 / 04期

关键词：

supernovae: general; galaxies: clusters: general; transients: supernovae; STELLAR MASS FUNCTION; SDSS-IV MANGA; STAR-FORMATION; HOST-GALAXY; ENVIRONMENTAL DEPENDENCE; RICH CLUSTERS; LUMINOSITY; EVOLUTION; FIELD; CALIBRATION;

D O I：

10.1093/mnras/stad2982

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We identify 66 photometrically classified Type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) that have occurred within red-sequence selected galaxy clusters. We compare light-curve and host galaxy properties of the cluster SNe to 1024 DES SNe Ia located in field galaxies, the largest comparison of two such samples at high redshift (z > 0.1). We find that cluster SN light curves decline faster than those in the field (97.7 per cent confidence). However, when limiting these samples to host galaxies of similar colour and mass, there is no significant difference in the SN light-curve properties. Motivated by previous detections of a higher-normalized SN Ia delay-time distribution in galaxy clusters, we measure the intrinsic rate of SNe Ia in cluster and field environments. We find the average ratio of the SN Ia rate per galaxy between high-mass (10 <= log (M-& lowast;/M-circle dot) <= 11.25) cluster and field galaxies to be 0.594 +/- 0.068. This difference is mass-dependent, with the ratio declining with increasing mass, which suggests that the stellar populations in cluster hosts are older than those in field hosts. We show that the mass-normalized rate (or SNe per unit mass) in massive-passive galaxies is consistent between cluster and field environments. Additionally, both of these rates are consistent with rates previously measured in clusters at similar redshifts. We conclude that in massive-passive galaxies, which are the dominant hosts of cluster SNe, the cluster delay-time distribution is comparable to the field.

引用

页码：5292 / 5305

页数：14

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