Constraints on compact objects from the Dark Energy Survey 5-yr supernova sample

被引：1

作者：

Shah, P. ^{[1
]}

Davis, T. M. ^{[2
]}

Vincenzi, M. ^{[3
]}

Armstrong, P. ^{[4
]}

Brout, D. ^{[5
]}

Camilleri, R. ^{[2
]}

Galbany, L. ^{[6
,7
]}

Garcia-Bellido, J. ^{[8
]}

Gill, M. S. S. ^{[9
]}

Lahav, O. ^{[1
]}

Lee, J. ^{[10
]}

Lidman, C. ^{[11
]}

Moeller, A. ^{[12
]}

Sako, M.

Sanchez, B. O. ^{[13
,14
]}

Sullivan, M. ^{[15
]}

Whiteway, L.

Wiseman, P. ^{[15
]}

Allam, S. ^{[16
]}

Aguena, M. ^{[17
]}

Bocquet, S. ^{[18
]}

Brooks, D. ^{[1
]}

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

Rosell, A. Carnero ^{[17
,20
]}

da Costa, L. N. ^{[17
]}

Pereira, M. E. S. ^{[21
]}

Desai, S. ^{[22
,34
]}

Dodelson, S. ^{[23
,24
]}

Doel, P.

Ferrero, I ^{[25
]}

Flaugher, B. ^{[16
]}

Frieman, J. ^{[16
,26
]}

Gaztanaga, E. ^{[3
,6
,7
]}

Gruen, D.

Gruendl, R. A. ^{[27
,28
]}

Gutierrez, G.

Herner, K.

Hinton, S. R. ^{[2
]}

Hollowood, D. L. ^{[29
]}

Honscheid, K. ^{[30
,31
]}

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

Kuehn, K. ^{[32
,33
]}

Lee, S.

Marshall, J. L. ^{[35
,36
]}

Mena-Fernandez, J. ^{[37
]}

Miquel, R. ^{[38
,39
]}

Myles, J. ^{[40
]}

Palmese, A.

Pieres, A. ^{[17
,41
]}

Malagon, A. A. Plazas ^{[9
]}

机构：

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

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

[3] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England

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

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

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

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

[8] Univ Autonoma Madrid, Inst Fis Teor UAM CSIC, E-28049 Madrid, Spain

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

[10] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

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

[12] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia

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

[14] Univ Grenoble Alpes, Dept Astrophys, CNRS, LPSC IN2P3, F-38000 Grenoble, France

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

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

[17] Lab Interinst eAstron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

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

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

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

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

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

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

[24] Carnegie Mellon Univ, NSF AI Planning Inst Phys Future, Pittsburgh, PA 15213 USA

[25] Univ Oslo, Inst Theoret Astrophys, PO Box 1029 Blindern, NO-0315 Oslo, Norway

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

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

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

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

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

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

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

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

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

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

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

[37] LPSC, 53 Ave Martyrs, F-38026 Grenoble, France

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

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

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

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

[42] Northeastern Univ, Dept Phys, Boston, MA 02115 USA

[43] Ctr Invest Energet Medioambientales & Tecnol CIEMA, Madrid, Spain

[44] Univ Lancaster, Phys Dept, Lancaster LA1 4YB, England

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

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

[47] Argonne Natl Lab, Lemont, IL 60439 USA

[48] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA

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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2024年 / 536卷 / 01期

基金：

欧洲研究理事会; 美国国家科学基金会; 英国科学技术设施理事会; 澳大利亚研究理事会;

关键词：

gravitational lensing: weak; stars: black holes; cosmology: cosmological parameters; cosmology: dark matter; transients: supernovae; GRAVITATIONAL MICROLENSING MAGNIFICATION; SPECTROSCOPIC SURVEY MEASUREMENT; CHALLENGE LIGHTCONE SIMULATION; DISTANCE-REDSHIFT RELATION; GALAXY SAMPLE; OBSERVATIONAL EVIDENCE; BLACK-HOLES; GROWTH-RATE; TIME-DELAY; MASS;

D O I：

10.1093/mnras/stae2614

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Gravitational lensing magnification of Type Ia supernovae (SNe Ia) allows information to be obtained about the distribution of matter on small scales. In this paper, we derive limits on the fraction alpha of the total matter density in compact objects (which comprise stars, stellar remnants, small stellar groupings, and primordial black holes) of mass M > 0.03 M-circle dot over cosmological distances. Using 1532 SNe Ia from the Dark Energy Survey Year 5 sample (DES-SN5YR) combined with a Bayesian prior for the absolute magnitude M, we obtain alpha < 0.12 at the 95 per cent confidence level after marginalization over cosmological parameters, lensing due to large-scale structure, and intrinsic non-Gaussianity. Similar results are obtained using priors from the cosmic microwave background, baryon acoustic oscillations, and galaxy weak lensing, indicating our results do not depend on the background cosmology. We argue our constraints are likely to be conservative (in the sense of the values we quote being higher than the truth), but discuss scenarios in which they could be weakened by systematics of the order of Delta alpha similar to 0.04.

引用

页码：946 / 961

页数：16

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