A sample of dust attenuation laws for Dark Energy Survey supernova host galaxies

被引：6

作者：

Duarte, J. ^{[1
]}

Gonzalez-Gaitan, S. ^{[1
]}

Mourao, A. ^{[1
]}

Paulino-Afonso, A. ^{[1
]}

Guilherme-Garcia, P. ^{[2
]}

Aguas, J. ^{[1
]}

Galbany, L. ^{[3
,4
]}

Kelsey, L. ^{[5
,6
]}

Scolnic, D. ^{[7
]}

Sullivan, M. ^{[6
]}

Brout, D. ^{[8
]}

Palmese, A. ^{[9
]}

Wiseman, P. ^{[6
]}

Aguena, M. ^{[10
]}

Alves, O. ^{[11
]}

Bacon, D. ^{[5
]}

Bertin, E. ^{[12
,13
]}

Bocquet, S. ^{[14
]}

Brooks, D. ^{[15
]}

Burke, D. L. ^{[16
,17
]}

Carnero Rosell, A. ^{[10
,18
,19
]}

Kind, M. Carrasco ^{[20
,21
]}

Carretero, J. ^{[22
]}

Costanzi, M. ^{[23
,24
,25
]}

Pereira, M. E. S. ^{[26
]}

Davis, T. M. ^{[27
]}

De Vicente, J. ^{[28
]}

Desai, S. ^{[29
]}

Diehl, H. T. ^{[30
]}

Doel, P. ^{[15
]}

Everett, S. ^{[31
]}

Ferrero, I. ^{[32
]}

Friedel, D. ^{[20
]}

Frieman, J. ^{[30
,33
]}

Garcia-Bellido, J. ^{[34
]}

Gatti, M. ^{[35
]}

Gerdes, D. W. ^{[36
]}

Gruen, D. ^{[14
]}

Gruendl, R. A. ^{[20
]}

Gutierrez, G. ^{[30
]}

Hinton, S. R. ^{[27
]}

Hollowood, D. L. ^{[37
]}

Honscheid, K. ^{[38
,39
]}

James, D. J.

Kuehn, K. ^{[40
,41
]}

Kuropatkin, N. ^{[30
]}

Melchior, P.

Miquel, R. ^{[42
,43
]}

Paz-Chinchon, F. ^{[20
,44
]}

Pieres, A. ^{[45
]}

机构：

[1] Univ Lisbon, CENTRA, Inst Super Tecn, Av Rovisco Pais 1, P-1049001 Lisbon, Portugal

[2] Univ Lisbon, Fac Ciencias, CENTRA, Ed C8,Campo Grande, P-1749016 Lisbon, Portugal

[3] Inst Estudis Espacials Catalunya IEEC, Barcelona 08034, Spain

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[18] Inst Astrofis Canarias, Tenerife 38205, Spain

[19] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Spain

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

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

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

[23] Univ Trieste, Astron Unit, Dept Phys, Via Tiepolo 11, I-34131 Trieste, Italy

[24] INAF Osservat Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy

[25] Inst Fundamental Phys Univ, Via Beirut 2, I-34014 Trieste, Italy

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

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

[28] Ctr Invest Energet Medioambient & Tecnol CIEMAT, Madrid, Spain

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

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

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

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

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

[34] Univ Autonoma Madrid, Inst Fis Teor, UAM CSIC, Madrid 28049, Spain

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

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

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

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

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

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

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

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

[43] Inst Catalana Rec & Estudis Avancats, Barcelona 08010, Spain

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

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

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 680卷

基金：

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

关键词：

dust; extinction; supernovae: general; distance scale; galaxies: general; MILKY-WAY DISK; NEUTRON-CAPTURE ELEMENTS; ROTATING MASSIVE STARS; CHEMICAL EVOLUTION; SPIRAL STRUCTURE; ABUNDANCE GRADIENTS; OXYGEN-ABUNDANCE; S-PROCESS; TRIGONOMETRIC PARALLAXES; METALLICITY DISTRIBUTION;

D O I：

10.1051/0004-6361/202346534

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Type Ia supernovae (SNe Ia) are useful distance indicators in cosmology, provided their luminosity is standardized by applying empirical corrections based on light-curve properties. One factor behind these corrections is dust extinction, which is accounted for in the color-luminosity relation of the standardization. This relation is usually assumed to be universal, which can potentially introduce systematics into the standardization. The "mass step" observed for SN Ia Hubble residuals has been suggested as one such systematic. Aims. We seek to obtain a more complete view of dust attenuation properties for a sample of 162 SN Ia host galaxies and to probe their link to the mass step. Methods. We inferred attenuation laws toward hosts from both global and local (4 kpc) Dark Energy Survey photometry and composite stellar population model fits. Results. We recovered a relation between the optical depth and the attenuation slope, best explained by di ffering star-to-dust geometry for di fferent galaxy orientations, which is significantly di fferent from the optical depth and extinction slope relation observed directly for SNe. We obtain a large variation of attenuation slopes and confirm these change with host properties, such as the stellar mass and age, meaning a universal SN Ia correction should ideally not be assumed. Analyzing the cosmological standardization, we find evidence for a mass step and a two-dimensional "dust step", both more pronounced for red SNe. Although comparable, the two steps are not found to be completely analogous. Conclusions. We conclude that host galaxy dust data cannot fully account for the mass step, using either an alternative SN standardization with extinction proxied by host attenuation or a dust-step approach.

引用

页数：28

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