Modelling the impact of host galaxy dust on type Ia supernova distance measurements

(DES Collaboration)

doi:10.1093/mnras/stae2164

Modelling the impact of host galaxy dust on type Ia supernova distance measurements

(DES Collaboration)

Research output: Contribution to journal › Article › peer-review

Abstract

Type Ia Supernovae (SNe Ia) are a critical tool in measuring the accelerating expansion of the universe. Recent efforts to improve these standard candles have focused on incorporating the effects of dust on distance measurements with SNe Ia. In this paper, we use the state-of-the-art Dark Energy Survey 5 year sample to evaluate two different families of dust models: empirical extinction models derived from SNe Ia data and physical attenuation models from the spectra of galaxies. In this work, we use realistic simulations of SNe Ia to forward-model different models of dust and compare summary statistics in order to test different assumptions and impacts on SNe Ia data. Among the SNe Ia-derived models, we find that a logistic function of the total-to-selective extinction best recreates the correlations between supernova distance measurements and host galaxy properties, though an additional 0.02 mag of grey scatter is needed to fully explain the scatter in SNIa brightness in all cases. These empirically derived extinction distributions are highly incompatible with the physical attenuation models from galactic spectral measurements. From these results, we conclude that SNe Ia must either preferentially select extreme ends of galactic dust distributions, or that the characterization of dust along the SNe Ia line-of-sight is incompatible with that of galactic dust distributions.

Original language	English
Pages (from-to)	2263-2276
Number of pages	14
Journal	Monthly Notices of the Royal Astronomical Society
Volume	534
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stae2164
State	Published - Nov 1 2024
Externally published	Yes

Funding

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\u00E7\u00E3o Carlos Chagas Filho de Amparo \u00E0 Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient\u00EDfico e Tecnol\u00F3gico and the Minist\u00E9rio da Ci\u00EAncia, Tecnologia e Inova\u00E7\u00E3o, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. All authors have read and contributed to the drafting of the manuscript. BP devised the analysis, ran the simulations and drafted the majority of the manuscript. PW, MSu, and MSm provided scientific support throughout the analysis and writing. SG-G and DS internally re vie wed the work and provided extensive feedback. JD, LG, LK, RK, CL, JL, MT, and MV provided comments on the analysis and interpretation. The remaining authors have made contributions to this paper that include, but are not limited to, the construction of DECam and other aspects of collecting the data; data processing and calibration; developing broadly used methods, codes, and simulations; running the pipelines and validation tests; and promoting the science analysis. PW acknowledges support from the Science and Technology Facilities Council (STFC) grant ST/R000506/1. AM is supported by the ARC Disco v ery Early Career Researcher Award (DECRA) project number DE230100055 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\u00E7\u00E3o Carlos Chagas Filho de Amparo \u00E0 Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient\u00EDfico e Tecnol\u00F3gico and the Minist\u00E9rio da Ci\u00EAncia, Tecnologia e Inova\u00E7\u00E3o, the Deutsche Forschungsge-meinschaft 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 Energ\u00E9ticas, Medioambientales y Tecnol\u00F3gicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgen\u00F6ssische Technische Hochschule (ETH) Z\u00FCrich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ci\u00E8ncies de l'Espai (IEEC/CSIC), the Institut de F\u00EDsica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit\u00E4t M\u00FCnchen and the associated Excellence Cluster Universe, the University of Michigan, NSF NOIRLab, the University of Nottingham, The Ohio State University, the Univ ersity 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 NSF Cerro Tololo Inter-American Observatory at NSF 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. 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 MICINN under grants PID2021-123012, PID2021-128989, PID2022-141079, SEV-2016-0588, CEX2020-001058-M, and CEX2020-001007-S, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. We acknowledge support from the Brazilian Instituto Nacional de Ci\u00EAncia e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). SGG and JD acknowledge support by FCT for CENTRA through the Project No. UIDB/00099/2020. JD also acknowledges support by FCT under the PhD grant 2023.01333.BD. 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. We acknowledge support from the Brazilian Instituto Nacional de Ci\u00EAncia e Tecnologia (INCT) do e-Universo (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. 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 MICINN under grants PID2021-123012, PID2021-128989, PID2022-141079, SEV-2016-0588, CEX2020-001058-M, and CEX2020-001007-S, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. PW acknowledges support from the Science and Technology Facilities Council (STFC) grant ST/R000506/1. AM is supported by the ARC Discovery Early Career Researcher Award (DECRA) project number DE230100055 Based in part on observations at NSF Cerro Tololo Inter-American Observatory at NSF 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. SGG and JD acknowledge support by FCT for CENTRA through the Project No. UIDB/00099/2020. JD also acknowledges support by FCT under the PhD grant 2023.01333.BD.

Funders	Funder number
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
University of Illinois at Urbana-Champaign
Brazilian Instituto Nacional de Ciência e Tecnologia
Univ ersity of Pennsylvania
University of Nottingham
University of Sussex
High Energy Physics
University of Edinburgh
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Ohio State University
Stanford University
University of Chicago
Generalitat de Catalunya
Higher Education Funding Council for England
Financiadora de Estudos e Projetos
Collaborating Institutions in the Dark Energy Surv e y
Ministry of Education and Science of Ukraine
Eidgenössische Technische Hochschule Zürich
University of California, Santa Cruz
Deutsche Forschungsgemeinschaft
Neurosciences Foundation
European Commission
Instituto Nacional de Ciência e Tecnologia para Excitotoxicidade e Neuroproteção
SLAC National Accelerator Laboratory
U.S. Department of Energy
Lawrence Berkeley National Laboratory
Fermilab
Collaborating Institutions are Argonne National Laboratory
University College London
University of Portsmouth
Science and Technology Facilities Council of the United Kingdom
Ministério da Ciência, Tecnologia e Inovação
Office of Science
National Centre for Supercomputing Applications
European Regional Development Fund
University of Michigan
Institut de Física d'Altes Energies
DECam
Collaborating Institutions in the Dark Energy Survey
Ludwig-Maximilians-Universität München
Institut de Ciències de l'Espai
Conselho Nacional de Desenvolvimento Científico e Tecnológico	465376/2014-2
Conselho Nacional de Desenvolvimento Científico e Tecnológico
Science and Technology Facilities Council	ST/R000506/1
Science and Technology Facilities Council
Australian Research Council	DE230100055
Australian Research Council
Ministerio de Ciencia e Innovación	CEX2020-001007-S, SEV-2016-0588, PID2021-123012, PID2022-141079, CEX2020-001058-M, PID2021-128989
Ministerio de Ciencia e Innovación
Fermi Research Alliance, LLC	DE-AC02-07CH11359
National Science Foundation	AST-1138766, AST-1536171
National Science Foundation
Texas A and M University	2012B-0001
Texas A and M University
Fundação para a Ciência e a Tecnologia	2023.01333, UIDB/00099/2020
Fundação para a Ciência e a Tecnologia

Keywords

ISM: dust, extinction
cosmology: distance scale
supernovae: general

Access to Document

10.1093/mnras/stae2164

Cite this

@article{7d3b77ab1eef46daa174efe67263c172,

title = "Modelling the impact of host galaxy dust on type Ia supernova distance measurements",

abstract = "Type Ia Supernovae (SNe Ia) are a critical tool in measuring the accelerating expansion of the universe. Recent efforts to improve these standard candles have focused on incorporating the effects of dust on distance measurements with SNe Ia. In this paper, we use the state-of-the-art Dark Energy Survey 5 year sample to evaluate two different families of dust models: empirical extinction models derived from SNe Ia data and physical attenuation models from the spectra of galaxies. In this work, we use realistic simulations of SNe Ia to forward-model different models of dust and compare summary statistics in order to test different assumptions and impacts on SNe Ia data. Among the SNe Ia-derived models, we find that a logistic function of the total-to-selective extinction best recreates the correlations between supernova distance measurements and host galaxy properties, though an additional 0.02 mag of grey scatter is needed to fully explain the scatter in SNIa brightness in all cases. These empirically derived extinction distributions are highly incompatible with the physical attenuation models from galactic spectral measurements. From these results, we conclude that SNe Ia must either preferentially select extreme ends of galactic dust distributions, or that the characterization of dust along the SNe Ia line-of-sight is incompatible with that of galactic dust distributions.",

keywords = "ISM: dust, extinction, cosmology: distance scale, supernovae: general",

author = "{(DES Collaboration)} and B. Popovic and P. Wiseman and M. Sullivan and M. Smith and S. Gonz{\'a}lez-Gait{\'a}n and D. Scolnic and J. Duarte and P. Armstrong and J. Asorey and D. Brout and D. Carollo and L. Galbany and K. Glazebrook and L. Kelsey and R. Kessler and C. Lidman and J. Lee and Lewis, {G. F.} and A. M{\"o}ller and Nichol, {R. C.} and S{\'a}nchez, {B. O.} and M. Toy and Tucker, {B. E.} and M. Vincenzi and Abbott, {T. M.C.} and M. Aguena and F. Andrade-Oliveira and D. Bacon and D. Brooks and Burke, {D. L.} and {Carnero Rosell}, A. and J. Carretero and Castander, {F. J.} and {Da Costa}, {L. N.} and Pereira, {M. E.S.} and Davis, {T. M.} and S. Desai and S. Everett and I. Ferrero and B. Flaugher and J. Garc{\'i}a-Bellido and E. Gaztanaga 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 E. Suchyta",

note = "Publisher Copyright: {\textcopyright} 2024 The Author(s).",

year = "2024",

month = nov,

day = "1",

doi = "10.1093/mnras/stae2164",

language = "English",

volume = "534",

pages = "2263--2276",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

TY - JOUR

T1 - Modelling the impact of host galaxy dust on type Ia supernova distance measurements

AU - (DES Collaboration)

AU - Popovic, B.

AU - Wiseman, P.

AU - Sullivan, M.

AU - Smith, M.

AU - González-Gaitán, S.

AU - Scolnic, D.

AU - Duarte, J.

AU - Armstrong, P.

AU - Asorey, J.

AU - Brout, D.

AU - Carollo, D.

AU - Galbany, L.

AU - Glazebrook, K.

AU - Kelsey, L.

AU - Kessler, R.

AU - Lidman, C.

AU - Lee, J.

AU - Lewis, G. F.

AU - Möller, A.

AU - Nichol, R. C.

AU - Sánchez, B. O.

AU - Toy, M.

AU - Tucker, B. E.

AU - Vincenzi, M.

AU - Abbott, T. M.C.

AU - Aguena, M.

AU - Andrade-Oliveira, F.

AU - Bacon, D.

AU - Brooks, D.

AU - Burke, D. L.

AU - Carnero Rosell, A.

AU - Carretero, J.

AU - Castander, F. J.

AU - Da Costa, L. N.

AU - Pereira, M. E.S.

AU - Davis, T. M.

AU - Desai, S.

AU - Everett, S.

AU - Ferrero, I.

AU - Flaugher, B.

AU - García-Bellido, J.

AU - Gaztanaga, E.

AU - Gruendl, R. A.

AU - Gutierrez, G.

AU - Hinton, S. R.

AU - Hollowood, D. L.

AU - Honscheid, K.

AU - James, D. J.

AU - Kuehn, K.

AU - Suchyta, E.

PY - 2024/11/1

Y1 - 2024/11/1

N2 - Type Ia Supernovae (SNe Ia) are a critical tool in measuring the accelerating expansion of the universe. Recent efforts to improve these standard candles have focused on incorporating the effects of dust on distance measurements with SNe Ia. In this paper, we use the state-of-the-art Dark Energy Survey 5 year sample to evaluate two different families of dust models: empirical extinction models derived from SNe Ia data and physical attenuation models from the spectra of galaxies. In this work, we use realistic simulations of SNe Ia to forward-model different models of dust and compare summary statistics in order to test different assumptions and impacts on SNe Ia data. Among the SNe Ia-derived models, we find that a logistic function of the total-to-selective extinction best recreates the correlations between supernova distance measurements and host galaxy properties, though an additional 0.02 mag of grey scatter is needed to fully explain the scatter in SNIa brightness in all cases. These empirically derived extinction distributions are highly incompatible with the physical attenuation models from galactic spectral measurements. From these results, we conclude that SNe Ia must either preferentially select extreme ends of galactic dust distributions, or that the characterization of dust along the SNe Ia line-of-sight is incompatible with that of galactic dust distributions.

AB - Type Ia Supernovae (SNe Ia) are a critical tool in measuring the accelerating expansion of the universe. Recent efforts to improve these standard candles have focused on incorporating the effects of dust on distance measurements with SNe Ia. In this paper, we use the state-of-the-art Dark Energy Survey 5 year sample to evaluate two different families of dust models: empirical extinction models derived from SNe Ia data and physical attenuation models from the spectra of galaxies. In this work, we use realistic simulations of SNe Ia to forward-model different models of dust and compare summary statistics in order to test different assumptions and impacts on SNe Ia data. Among the SNe Ia-derived models, we find that a logistic function of the total-to-selective extinction best recreates the correlations between supernova distance measurements and host galaxy properties, though an additional 0.02 mag of grey scatter is needed to fully explain the scatter in SNIa brightness in all cases. These empirically derived extinction distributions are highly incompatible with the physical attenuation models from galactic spectral measurements. From these results, we conclude that SNe Ia must either preferentially select extreme ends of galactic dust distributions, or that the characterization of dust along the SNe Ia line-of-sight is incompatible with that of galactic dust distributions.

KW - ISM: dust, extinction

KW - cosmology: distance scale

KW - supernovae: general

UR - http://www.scopus.com/inward/record.url?scp=85207007887&partnerID=8YFLogxK

U2 - 10.1093/mnras/stae2164

DO - 10.1093/mnras/stae2164

M3 - Article

AN - SCOPUS:85207007887

SN - 0035-8711

VL - 534

SP - 2263

EP - 2276

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

Modelling the impact of host galaxy dust on type Ia supernova distance measurements

Abstract

Funding

Keywords

Access to Document

Other files and links

Fingerprint

Cite this