@article{96e17f33a76143ffb06afe7c3c0c6752,
title = "A sample of dust attenuation laws for Dark Energy Survey supernova host galaxies",
abstract = "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 differing star-to-dust geometry for different galaxy orientations, which is significantly different 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.",
keywords = "distance scale, dust, extinction, galaxies: general, supernovae: general, UKRI, MRC, MR/T01881X/1, STFC, ST/R000506/1",
author = "{DES Collaboration} and J. Duarte and S. Gonz{\'a}lez-Gait{\'a}n and A. Mour{\~a}o and A. Paulino-Afonso and P. Guilherme-Garcia and J. {\'A}guas and L. Galbany and L. Kelsey and D. Scolnic and M. Sullivan and D. Brout and A. Palmese and P. Wiseman and M. Aguena and O. Alves and D. Bacon and E. Bertin and S. Bocquet and D. Brooks and Burke, {D. L.} and {Carnero Rosell}, A. and {Carrasco Kind}, M. and J. Carretero and M. Costanzi and Pereira, {M. E.S.} and Davis, {T. M.} and {De Vicente}, J. and S. Desai and Diehl, {H. T.} and P. Doel and S. Everett and I. Ferrero and D. Friedel and J. Frieman and J. Garc{\'i}a-Bellido and M. Gatti and Gerdes, {D. W.} and D. Gruen and Gruendl, {R. A.} and G. Gutierrez and Hinton, {S. R.} and Hollowood, {D. L.} and K. Honscheid and James, {D. J.} and K. Kuehn and N. Kuropatkin and P. Melchior and R. Miquel and F. Paz-Chinch{\'o}n and A. Pieres",
note = "Funding Information: J.D., S.G.G., A.M. and A.P.A. acknowledge support by FCT under Project CRISP PTDC/FIS-AST-31546/2017 and Project No. UIDB/00099/2020. L.G. acknowledges financial support from the Spanish Ministerio de Ciencia e Innovaci{\'o}n (MCIN), the Agencia Estatal de Investigaci{\'o}n (AEI) 10.13039/501100011033, and the European Social Fund (ESF) “Investing in your future” under the 2019 Ram{\'o}n y Cajal program RYC2019-027683-I and the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Cient{\'i}ficas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia Mar{\'i}a de Maeztu CEX2020-001058-M. L.K. thanks the UKRI Future Leaders Fellowship for support through the grant MR/T01881X/1. Computations were performed at the cluster “Baltasar-Sete-S{\'o}is” and supported by the H2020 ERC Consolidator Grant “Matter and strong field gravity: New frontiers in Einstein{\textquoteright}s theory” grant agreement no. MaGRaTh-646597. P.W. acknowledges support from the Science and Technology Facilities Council (STFC) grant ST/R000506/1. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Funda{\c c}{\~a}o Carlos Chagas Filho de Amparo {\'a} Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient{\'i}fico e Tecnol{\'o}gico and the Minist{\'e}rio da Ci{\^e}ncia, Tecnologia e Inova{\c c}{\~a}o, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energ{\'e}ticas, Medioambientales y Tecnol{\'o}gicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgen{\"o}ssische Technische Hochschule (ETH) Z{\"u}rich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ci{\'e}ncies de l{\textquoteright}Espai (IEEC/CSIC), the Institut de F{\'i}sica d{\textquoteright}Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit{\"a}t M{\"u}nchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union{\textquoteright}s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ci{\^e}ncia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. Publisher Copyright: {\textcopyright} The Authors 2023.",
year = "2023",
month = dec,
day = "1",
doi = "10.1051/0004-6361/202346534",
language = "English",
volume = "680",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",
}