The dark energy survey: detection of weak lensing magnification of supernovae and constraints on dark matter haloes

被引：1

作者：

Shah, P. ^{[1
]}

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

Bacon, D. ^{[3
]}

Brout, D. ^{[4
]}

Frieman, J. ^{[5
,6
]}

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

Kessler, R. ^{[6
,9
]}

Lahav, O. ^{[1
]}

Lee, J. ^{[10
]}

Lidman, C. ^{[11
,12
]}

Nichol, R. C. ^{[3
]}

Sako, M. ^{[10
]}

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

Scolnic, D. ^{[13
]}

Sullivan, M. ^{[15
]}

Vincenzi, M. ^{[3
,15
]}

Wiseman, P.

Allam, S.

Abbott, T. M. C. ^{[16
]}

Aguena, M. ^{[17
]}

Alves, O. ^{[18
]}

Andrade-Oliveira, F. ^{[18
]}

Annis, J. ^{[5
]}

Bechtol, K. ^{[19
]}

Bertin, E. ^{[20
,21
]}

Bocquet, S. ^{[22
]}

Brooks, D.

Rosell, A. Carnero ^{[17
,23
]}

Carretero, J. ^{[24
]}

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

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

Pereira, M. E. S. ^{[25
]}

Diehl, H. T.

Doel, P. ^{[1
]}

Doux, C. ^{[26
]}

Everett, S. ^{[27
]}

Ferrero, I ^{[28
]}

Flaugher, B. ^{[5
]}

Friedel, D. ^{[29
]}

Gatti, M.

Gruen, D.

Gruendl, R. A. ^{[29
,30
]}

Gutierrez, G. ^{[5
]}

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

Hollowood, D. L. ^{[31
]}

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

Huterer, D.

James, D. J. ^{[34
]}

Kuehn, K. ^{[35
,36
]}

Lee, S. ^{[27
]}

机构：

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

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

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

[4] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA

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

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

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

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

[9] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 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] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2601, Australia

[13] Duke Univ, Dept Math, 120 Sci Dr, Durham, NC 27710 USA

[14] Univ Aix Marseille, CPPM, IN2P3, CNRS, F-13007 Marseille, France

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

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

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

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

[19] Univ Wisconsin Madison, Phys Dept, 2320 Chamberlin Hall,1150 Univ Ave Madison, Madison, WI 53706 USA

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

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

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

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

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

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

[26] Univ Grenoble Alpes, CNRS, IPAG, IN2P3, F-38000 Grenoble, France

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

[28] Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, NO-0315 Oslo, Norway

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

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

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

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

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

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

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

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

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

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

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

[40] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain

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

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

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

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

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

[46] Ctr Invest Energet Medioambientales & Tecnol CIEMA, Madrid 28040, Spain

[47] Oak Ridge Natl Lab, Comp Sci & Math Div, Oak Ridge, TN 37831 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 / 532卷 / 01期

基金：

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

关键词：

gravitational lensing: weak; galaxies: haloes; cosmological parameters; dark matter; transients: supernovae; IA SUPERNOVAE; COSMOLOGICAL CONSTRAINTS; HUBBLE CONSTANT; TIME-DELAY; SNE IA; GALAXY; MASS; LUMINOSITIES; SIMULATIONS; IMAGES;

D O I：

10.1093/mnras/stae1515

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The residuals of the distance moduli of Type Ia supernovae (SNe Ia) relative to a Hubble diagram fit contain information about the inhomogeneity of the Universe, due to weak lensing magnification by foreground matter. By correlating the residuals of the Dark Energy Survey Year 5 SN Ia sample (DES-SN5YR) with extragalactic foregrounds from the DES Y3 Gold catalogue, we detect the presence of lensing at $6.0 \sigma$ significance. This is the first detection with a significance level above $5\sigma$. Constraints on the effective mass-to-light ratios and radial profiles of dark matter haloes surrounding individual galaxies are also obtained. We show that the scatter of SNe Ia around the Hubble diagram is reduced by modifying the standardization of the distance moduli to include an easily calculable de-lensing (i.e. environmental) term. We use the de-lensed distance moduli to recompute cosmological parameters derived from SN Ia, finding in Flat wcold dark matter a difference of Delta Omega M=+0.036and Delta w=-0.056 compared to the unmodified distance moduli, a change of $\sim 0.3\sigma$. We argue that our modelling of SN Ia lensing will lower systematics on future surveys with higher statistical power. We use the observed dispersion of lensing in DES-SN5YR to constrain $\sigma _8$, but caution that the fit is sensitive to uncertainties at small scales. Nevertheless, our detection of SN Ia lensing opens a new pathway to study matter inhomogeneity that complements galaxy-galaxy lensing surveys and has unrelated systematics.

引用

页码：932 / 944

页数：13

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