A galaxy-driven model of type Ia supernova luminosity variations

Wiseman, P and Vincenzi, M and Desai, Shantanu and et al, . (2022) A galaxy-driven model of type Ia supernova luminosity variations. Monthly Notices of the Royal Astronomical Society. pp. 1-19. ISSN 0035-8711

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Abstract

Type Ia supernovae (SNe Ia) are used as standardizable candles to measure cosmological distances, but differences remain in their corrected luminosities which display a magnitude step as a function of host galaxy properties such as stellar mass and rest-frame U-R colour. Identifying the cause of these steps is key to cosmological analyses and provides insight into SN physics. Here we investigate the effects of SN progenitor ages on their light-curve properties using a galaxy-based forward model that we compare to the Dark Energy Survey 5-yr SN Ia sample. We trace SN Ia progenitors through time and draw their light-curve width parameters from a bimodal distribution according to their age. We find that an intrinsic luminosity difference between SNe of different ages cannot explain the observed trend between step size and SN colour. The data split by stellar mass are better reproduced by following recent work implementing a step in total-to-selective dust extinction ratio (RV) between low- and high-mass hosts, although an additional intrinsic luminosity step is still required to explain the data split by host galaxy U-R. Modelling the RV step as a function of galaxy age provides a better match overall. Additional age versus luminosity steps marginally improve the match to the data, although most of the step is absorbed by the width versus luminosity coefficient α. Furthermore, we find no evidence that α varies with SN age. © 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.

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IITH Creators:

IITH Creators	ORCiD
Desai, Shantanu	http://orcid.org/0000-0002-0466-3288

Item Type:

Article

Additional Information:

We thank the referee Mickael Rigault for comments which significantly impro v ed this paper. P.W. acknowledges support from the Science and Technology Facilities Council (STFC) grant ST/R000506/1. MS acknowledges support from EU/FP7-ERC grant 615929. LK thanks the UKRI Future Leaders Fellowship for support through the grant MR/T01881X/1. LG acknowledges financial support from the Spanish Ministerio de Ciencia e Innovacion (MCIN), the Agencia Estatal de Investigacion (AEI) 10.13039/501100011033, and the European Social Fund (ESF) 'Investing in your future' under the 2019 Ramon y Cajal program RYC2019-027683-I and the PID2020115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Cientýficas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia Marýa de Maeztu CEX2020001058-M. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement number 759194 USNAC). 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 Te xas A&M Univ ersity, Financiadora de Estudos e Projetos, Fundaçao Carlos Chagas Filho de Amparo `a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientýfico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovaçao, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Surv e y. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgen ¨ossische Technische Hochschule (ETH) Z ¨urich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ci `encies de l'Espai (IEEC/CSIC), the Institut de Fýsica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit ¨at M ¨unchen and the associated Excellence Cluster Universe, the University of Michigan, NSF's NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford Uni versity, the Uni versity of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF's NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation.

Uncontrolled Keywords:

cosmology: observations; dust, extinction; galaxies: evolution; supernovae: general

Subjects:

Physics

Divisions:

Department of Physics

Depositing User:

. LibTrainee 2021

Date Deposited:

12 Nov 2022 09:53

Last Modified:

12 Nov 2022 09:53