ZTF SN Ia DR2: Study of Type Ia supernova light-curve fits

被引：3

作者：

Rigault, M. ^{[1
]}

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

Regnault, N. ^{[3
]}

Kenworthy, W. D. ^{[4
]}

Maguire, K. ^{[5
]}

Goobar, A. ^{[4
]}

Dimitriadis, G. ^{[5
]}

Johansson, J. ^{[4
]}

Amenouche, M. ^{[6
]}

Aubert, M. ^{[7
]}

Barjou-Delayre, C. ^{[7
]}

Bellm, E. C. ^{[8
]}

Burgaz, U. ^{[5
]}

Carreres, B. ^{[9
,10
]}

Copin, Y. ^{[1
]}

Deckers, M. ^{[5
]}

de Jaeger, T. ^{[3
]}

Dhawan, S. ^{[11
,12
]}

Feinstein, F. ^{[9
]}

Fouchez, D. ^{[9
]}

Galbany, L. ^{[13
,14
]}

Ginolin, M. ^{[1
]}

Graham, M. J. ^{[15
]}

Kim, Y. -l. ^{[2
]}

Kowalski, M. ^{[16
,17
]}

Kuhn, D. ^{[3
]}

Kulkarni, S. R. ^{[15
]}

Muller-Bravo, T. E. ^{[13
,14
]}

Nordin, J. ^{[17
]}

Popovic, B. ^{[1
]}

Purdum, J. ^{[18
]}

Rosnet, P. ^{[7
]}

Rosselli, D. ^{[9
]}

Racine, B. ^{[9
]}

Ruppin, F. ^{[1
]}

Sollerman, J. ^{[19
]}

Terwel, J. H. ^{[5
,20
]}

Townsend, A. ^{[17
]}

机构：

[1] UNIV CLAUDE BERNARD LYON 1, CNRS, IMR 5822, IP2I Lyon,IN2P3, F-69622 VILLEURBANNE, France

[2] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, Lancs, England

[3] Univ Paris, LPNHE, IN2P3, CNRS, Paris, France

[4] AlbaNova, Oskar Klein Ctr, Dept Phys, S-10691 Stockholm, Sweden

[5] Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland

[6] Natl Res Council Canada, Herzberg Astron & Astrophys Res Ctr, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada

[7] Univ Clermont Auvergne, CNRS, IN2P3, LPCA, F-63000 Clermont Ferrand, France

[8] Univ Washington, DIRAC Inst, Dept Astron, 3910 15th Ave NE, Seattle, WA 98195 USA

[9] Aix Marseille Univ, CNRS, CPPM, IN2P3, Marseille, France

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

[11] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[12] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England

[13] CSIC, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain

[14] Inst Estudis Espacials Catalunya IEEC, Castelldefels 08860, Barcelona, Spain

[15] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA

[16] Deutsch Elektronen Synchrotron DESY, Platanenallee 6, D-15738 Zeuthen, Germany

[17] Univ Berlin, Inst Phys Humboldt, Newtonstr 15, D-12489 Berlin, Germany

[18] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA

[19] Stockholm Univ, Oskar Klein Ctr, Dept Astron, AlbaNova, SE-10691 Stockholm, Sweden

[20] Nord Opt Telescope, Rambla Jose Ana Fernandez Perez 7, Brena Baja 38711, Spain

来源：

ASTRONOMY & ASTROPHYSICS | 2025年 / 694卷

基金：

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

关键词：

supernovae: general; cosmology: observations; dark energy; distance scale; HUBBLE CONSTANT; DEPENDENCE; DISTANCES; MODEL; LUMINOSITIES; SPECTRA; MAXIMUM; LEGACY; SAMPLE; SALT2;

D O I：

10.1051/0004-6361/202450377

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Type Ia supernova (SN Ia) cosmology relies on the estimation of light-curve parameters to derive precision distances, which are used to infer cosmological parameters such as H0, Omega M, Omega Lambda, and w. The empirical SALT2 light-curve modeling that relies on only two parameters, a stretch x1 and a color c, has been used by the community for almost two decades. We study the ability of the SALT2 model to fit the nearly 3000 cosmology-grade SN Ia light curves from the second release of the Zwicky Transient Facility (ZTF) cosmology science working group. While the ZTF data were not used to train SALT2, the algorithm models the ZTF SN Ia optical light curves remarkably well, except for light-curve points prior to -10 d from maximum, where the training critically lacks data. We find that the light-curve fitting is robust against the considered choice of phase range, but we show that the [ - 10; +40] d range is optimal in terms of statistics and accuracy. We do not detect any significant features in the light-curve fit residuals that could be connected to the host environment. Potential systematic uncertainties associated tp population differences related to the SN Ia host properties might thus not be accountable for by the inclusion of addition of light-curve parameters. However, a small but significant inconsistency between residuals of blue and red SN Ia strongly suggests the existence of a phase-dependent color term, with potential implications for the use of SNe Ia in precision cosmology. We thus encourage further work in this area to explore this possibility, and we emphasize that SN Ia cosmology must include a SALT2 retraining to accurately model the light curves and avoid biasing the derivation of cosmological parameters.

引用

页数：10

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