First cosmology results using type Ia supernovae from the Dark Energy Survey: the effect of host galaxy properties on supernova luminosity

被引：58

作者：

Smith, M. ^{[1
]}

Sullivan, M. ^{[1
]}

Wiseman, P. ^{[1
]}

Kessler, R. ^{[2
,3
]}

Scolnic, D. ^{[4
]}

Brout, D. ^{[5
]}

D'Andrea, C. B. ^{[5
,6
]}

Davis, T. M. ^{[7
]}

Foley, R. J. ^{[8
]}

Frohmaier, C. ^{[9
]}

Galbany, L. ^{[10
]}

Gupta, R. R. ^{[11
]}

Gutierrez, C. P. ^{[1
]}

Hinton, S. R. ^{[7
]}

Kelsey, L. ^{[1
]}

Lidman, C. ^{[12
,13
]}

Macaulay, E. ^{[9
,14
]}

Moeller, A. ^{[12
,13
,15
]}

Nichol, R. C. ^{[9
]}

Nugent, P. ^{[11
,16
]}

Palmese, A. ^{[3
,17
]}

Pursiainen, M. ^{[1
]}

Sako, M. ^{[5
]}

Swann, E. ^{[9
]}

Thomas, R. C. ^{[11
]}

Tucker, B. E. ^{[12
]}

Vincenzi, M. ^{[9
]}

Carollo, D. ^{[18
]}

Lewis, G. F. ^{[19
]}

Sommer, N. E. ^{[12
]}

Abbott, T. M. C. ^{[20
]}

Aguena, M. ^{[21
,22
]}

Allam, S. ^{[17
]}

Avila, S. ^{[23
]}

Bertin, E. ^{[24
,25
]}

Bhargava, S. ^{[26
]}

Brooks, D. ^{[27
]}

Buckley-Geer, E. ^{[17
]}

Burke, D. L. ^{[28
,29
]}

Rosell, A. Carnero ^{[22
,30
]}

Kind, M. Carrasco ^{[31
,32
]}

Costanzi, M. ^{[33
,34
]}

da Costa, L. N. ^{[22
,35
]}

De Vicente, J. ^{[30
]}

Desai, S. ^{[36
]}

Diehl, H. T. ^{[17
]}

Doel, P. ^{[27
]}

Eifler, T. F. ^{[37
,38
]}

Everett, S. ^{[8
]}

Flaugher, B. ^{[17
]}

机构：

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

[2] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA

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

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

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

[6] Bryn Mawr Coll, Dept Phys, Bryn Mawr, PA 19010 USA

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

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

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

[10] Univ Pittsburgh, PIIT PACC, Dept Phys & Astron, Pittsburgh, PA 15260 USA

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

[12] Australian Natl Univ, Res Sch Astnm & Astrophys, Canberra, ACT 2601, Australia

[13] ARC Ctr Excellence All Sky Astrophys CAASTRO, Canberra, ACT, Australia

[14] Univ North Georgia, Dept Phys & Astron, Dahlonega, GA 30597 USA

[15] Univ Clermont Auvergne, CNRS IN2P3, LPC, F-63000 Clermont Ferrand, France

[16] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA

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

[18] INAF, Astrophys Observ Turin, I-110025 Pino Torinese, Italy

[19] Univ Sydney, Sch Phys, Sydney Inst Astron, A28, Sydney, NSW 2006, Australia

[20] Natl Opt Astron Observ, Cenv Tololo Interamer Observ, Casilla 603, La Serena, Chile

[21] Univ Sao Paulo, Dept Fis Matemat, Inst Fis, CP 66318, BR-05314970 Sao Paulo, SP, Brazil

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

[23] Univ Autonorna Madrid, Inst Fis Teor UAM CSIC, E-28049 Madrid, Spain

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

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

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

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

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

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

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

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

[32] Natl Ctr Supercomp Applicat, 1205 West Clark Str, Urbana, IL 61801 USA

[33] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy

[34] Inst Fundamental Phys Universe, Via Beirut 2, I-34014 Trieste, Italy

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

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

[37] Univ Arizona, Dept Astron Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA

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

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

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

[41] Swinbunre Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia

[42] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA

[43] Swiss Fed Inst Technol, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland

[44] Univ Geneva, Dept Phys Theor, 24 Quai Ernest Ansermet, CH-1211 Geneva, Switzerland

[45] Univ Geneva, Ctr Astroparticle Phys, 24 Quai Ernest Ansermet, CH-1211 Geneva, Switzerland

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

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

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

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

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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2020年 / 494卷 / 03期

基金：

欧盟地平线“2020”; 欧洲研究理事会; 英国科学技术设施理事会; 美国国家科学基金会;

关键词：

surveys; supernovae: general; distance scale; cosmology: observations; transients: supernovae; POPULATION SYNTHESIS; MASS; SEXTRACTOR; SOFTWARE; PEGASE;

D O I：

10.1093/mnras/staa946

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present improved photometric measurements for the host galaxies of 206 spectroscopically confirmed type Ia supernovae discovered by the Dark Energy Survey Supernova Program (DES-SN) and used in the first DES-SN cosmological analysis. For the DES-SN sample, when considering a 5D (z, x(1), c, alpha, beta) bias correction, we find evidence of a Hubble residual 'mass step', where SNe Ia in high-mass galaxies (>10(10)M(circle dot)) are intrinsically more luminous (after correction) than their low-mass counterparts by gamma = 0.040 +/- 0.019 mag. This value is larger by 0.031 mag than the value found in the first DES-SN cosmological analysis. This difference is due to a combination of updated photometric measurements and improved star formation histories and is not from host-galaxy misidentification. When using a 1D (redshift-only) bias correction the inferred mass step is larger, with gamma = 0.066 +/- 0.020 mag. The 1D-5D gamma difference for DES-SN is 0.026 +/- 0.009 mag. We show that this difference is due to a strong correlation between host galaxy stellar mass and the x(1) component of the 5D distance-bias correction. Including an intrinsic correlation between the observed properties of SNe Ia, stretch and colour, and stellar mass in simulated SN Ia samples, we show that a 5D fit recovers gamma with -9 mmag bias compared to a +2 mmag bias for a 1D fit. This difference can explain part of the discrepancy seen in the data. Improvements in modelling correlations between galaxy properties and SN is necessary to ensure unbiased precision estimates of the dark energy equation of state as we enter the era of LSST.

引用

页码：4426 / 4447

页数：22

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