Evaluating cosmological biases using photometric redshifts for Type Ia Supernova cosmology with the Dark Energy Survey Supernova Program

DES Collaboration

doi:10.1093/mnras/stae2703

Evaluating cosmological biases using photometric redshifts for Type Ia Supernova cosmology with the Dark Energy Survey Supernova Program

DES Collaboration

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Abstract

Cosmological analyses with Type Ia Supernovae (SNe Ia) have traditionally been reliant on spectroscopy for both classifying the type of supernova and obtaining reliable redshifts to measure the distance-redshift relation. While obtaining a host-galaxy spectroscopic redshift for most SNe is feasible for small-area transient surveys, it will be too resource intensive for upcoming large-area surveys such as the Vera Rubin Observatory Legacy Survey of Space and Time, which will observe on the order of millions of SNe. Here, we use data from the Dark Energy Survey (DES) to address this problem with photometric redshifts (photo-z) inferred directly from the SN light curve in combination with Gaussian and full priors from host-galaxy photo-z estimates. Using the DES 5-yr photometrically classified SN sample, we consider several photo-z algorithms as host-galaxy photo-z priors, including the Self-Organizing Map redshifts (SOMPZ), Bayesian Photometric Redshifts (BPZ), and Directional-Neighbourhood Fitting (DNF) redshift estimates employed in the DES 3 × 2 point analyses. With detailed catalogue-level simulations of the DES 5-yr sample, we find that the simulated w can be recovered within when using SN+SOMPZ or DNF prior photo-z, smaller than the average statistical uncertainty for these samples of 0.03. With data, we obtain biases in w consistent with simulations within ∼1 σ for three of the five photo-z variants. We further evaluate how photo-z systematics interplay with photometric classification and find classification introduces a subdominant systematic component. This work lays the foundation for next-generation fully photometric SNe Ia cosmological analyses.

Original language	English
Pages (from-to)	1948-1966
Number of pages	19
Journal	Monthly Notices of the Royal Astronomical Society
Volume	536
Issue number	2
DOIs	https://doi.org/10.1093/mnras/stae2703
State	Published - Jan 1 2025

Funding

This paper has gone through internal review by the DES collaboration. 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, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the DES. This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of Workforce Development for Teachers and Scientists, Office of Science Graduate Student Research (SCGSR) program. The SCGSR program is administered by the Oak Ridge Institute for Science and Education for the DOE under contract number DE-SC0014664. 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 ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, 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’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). Author contributions: RC developed and performed the analysis and wrote the manuscript. DS, MV, ER, JM, RK, and BP assisted in developing the project and provided useful discussion and insight.MSa and MSm served as internal re vie wers. All authors contributed to this paper and/or carried out infrastructure work that made this analysis possible. Additional highlighted contributions include: Construction and validation of the DES-SN5YR data and Hubble diagram : AM, BP, BS, CL, DB, DS, GQ, JL, LG, MSa, MSm, MSu, P A, PW, MV. Contributed to the internal re vie w process : AM, CL, HQ, JL, LG, MSa, MSm, MSu, PW, TD. Development and/or maintenance of software : PA, RK. 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. This material is based upon work supported by the U.S. Depart- ment of Energy, Office of Science, Office of Workforce Development for Teachers and Scientists, Office of Science Graduate Student Research (SCGSR) program. The SCGSR program is administered by the Oak Ridge Institute for Science and Education for the DOE under contract number DE-SC0014664. DS is supported by Department of Energy grant DESC0010007, the David and Lucile Packard Foundation, the Templeton Foun- dation, and Sloan Foundation. LG acknowledges financial support from the Spanish Ministerio de Ciencia e Innovacion (MCIN) and the Agencia Estatal de Investigacion (AEI) 10.13039/501100011033 under the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Cientýficas (CSIC) under the PIE project 20215AT016 and the program Unidad de Excelencia Marýa de Maeztu CEX2020-001058-M, and from the Departament de Recerca i Universitats de la Generalitat de Catalunya through the 2021-SGR-01270 grant. This paper has gone through internal re vie w by the DES collab- oration. 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 cao 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 DES. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cam- bridge, 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 Urbana- Champaign, 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 Michi- gan, NFS'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. Based in part on data acquired at the AAT, under program A/2013B/012. We acknowledge the traditional owners of the land on which the AAT stands, the Gamilaraay people, and pay our respects to elders past and present. The DES data management system is supported by the Na- tional Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016- 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's Se venth Frame work Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This w ork w as completed in part with resources provided by the University of Chicago's Research Computing Center. DS is supported by Department of Energy grant DESC0010007, the David and Lucile Packard Foundation, the Templeton Foundation, and Sloan Foundation. LG acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación (MCIN) and the Agencia Estatal de Investigación (AEI) 10.13039/501100011033 under the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016 and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M, and from the Departament de Recerca i Universitats de la Generalitat de Catalunya through the 2021-SGR-01270 grant.

Keywords

(cosmology:) dark energy
transients: supernovae

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10.1093/mnras/stae2703

Cite this

@article{fc9b93ede97340019eda9a637c508dda,

title = "Evaluating cosmological biases using photometric redshifts for Type Ia Supernova cosmology with the Dark Energy Survey Supernova Program",

abstract = "Cosmological analyses with Type Ia Supernovae (SNe Ia) have traditionally been reliant on spectroscopy for both classifying the type of supernova and obtaining reliable redshifts to measure the distance-redshift relation. While obtaining a host-galaxy spectroscopic redshift for most SNe is feasible for small-area transient surveys, it will be too resource intensive for upcoming large-area surveys such as the Vera Rubin Observatory Legacy Survey of Space and Time, which will observe on the order of millions of SNe. Here, we use data from the Dark Energy Survey (DES) to address this problem with photometric redshifts (photo-z) inferred directly from the SN light curve in combination with Gaussian and full priors from host-galaxy photo-z estimates. Using the DES 5-yr photometrically classified SN sample, we consider several photo-z algorithms as host-galaxy photo-z priors, including the Self-Organizing Map redshifts (SOMPZ), Bayesian Photometric Redshifts (BPZ), and Directional-Neighbourhood Fitting (DNF) redshift estimates employed in the DES 3 × 2 point analyses. With detailed catalogue-level simulations of the DES 5-yr sample, we find that the simulated w can be recovered within when using SN+SOMPZ or DNF prior photo-z, smaller than the average statistical uncertainty for these samples of 0.03. With data, we obtain biases in w consistent with simulations within ∼1 σ for three of the five photo-z variants. We further evaluate how photo-z systematics interplay with photometric classification and find classification introduces a subdominant systematic component. This work lays the foundation for next-generation fully photometric SNe Ia cosmological analyses.",

keywords = "(cosmology:) dark energy, transients: supernovae",

author = "\{DES Collaboration\} and Chen, \{R. C.\} and D. Scolnic and M. Vincenzi and Rykoff, \{E. S.\} and J. Myles and R. Kessler and B. Popovic and M. Sako and M. Smith and P. Armstrong and D. Brout and Davis, \{T. M.\} and L. Galbany and J. Lee and C. Lidman and A. M{\"o}ller and S{\'a}nchez, \{B. O.\} and M. Sullivan and H. Qu and P. Wiseman and Abbott, \{T. M.C.\} and M. Aguena and S. Allam and O. Alves and F. Andrade-Oliveira and J. Annis and D. Bacon and D. Brooks and \{Carnero Rosell\}, A. and J. Carretero and A. Choi and C. Conselice and \{Da Costa\}, \{L. N.\} and Pereira, \{M. E.S.\} and Diehl, \{H. T.\} and P. Doel and S. Everett and I. Ferrero and B. Flaugher and J. Frieman and J. Garc{\'i}a-Bellido and M. Gatti and E. Gaztanaga and G. Giannini and D. Gruen and Gruendl, \{R. A.\} and G. Gutierrez and K. Herner and Hinton, \{S. R.\} and E. Suchyta",

note = "Publisher Copyright: {\textcopyright} 2024 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.",

year = "2025",

month = jan,

day = "1",

doi = "10.1093/mnras/stae2703",

language = "English",

volume = "536",

pages = "1948--1966",

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

issn = "0035-8711",

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TY - JOUR

T1 - Evaluating cosmological biases using photometric redshifts for Type Ia Supernova cosmology with the Dark Energy Survey Supernova Program

AU - DES Collaboration

AU - Chen, R. C.

AU - Scolnic, D.

AU - Vincenzi, M.

AU - Rykoff, E. S.

AU - Myles, J.

AU - Kessler, R.

AU - Popovic, B.

AU - Sako, M.

AU - Smith, M.

AU - Armstrong, P.

AU - Brout, D.

AU - Davis, T. M.

AU - Galbany, L.

AU - Lee, J.

AU - Lidman, C.

AU - Möller, A.

AU - Sánchez, B. O.

AU - Sullivan, M.

AU - Qu, H.

AU - Wiseman, P.

AU - Abbott, T. M.C.

AU - Aguena, M.

AU - Allam, S.

AU - Alves, O.

AU - Andrade-Oliveira, F.

AU - Annis, J.

AU - Bacon, D.

AU - Brooks, D.

AU - Carnero Rosell, A.

AU - Carretero, J.

AU - Choi, A.

AU - Conselice, C.

AU - Da Costa, L. N.

AU - Pereira, M. E.S.

AU - Diehl, H. T.

AU - Doel, P.

AU - Everett, S.

AU - Ferrero, I.

AU - Flaugher, B.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gatti, M.

AU - Gaztanaga, E.

AU - Giannini, G.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Gutierrez, G.

AU - Herner, K.

AU - Hinton, S. R.

AU - Suchyta, E.

PY - 2025/1/1

Y1 - 2025/1/1

N2 - Cosmological analyses with Type Ia Supernovae (SNe Ia) have traditionally been reliant on spectroscopy for both classifying the type of supernova and obtaining reliable redshifts to measure the distance-redshift relation. While obtaining a host-galaxy spectroscopic redshift for most SNe is feasible for small-area transient surveys, it will be too resource intensive for upcoming large-area surveys such as the Vera Rubin Observatory Legacy Survey of Space and Time, which will observe on the order of millions of SNe. Here, we use data from the Dark Energy Survey (DES) to address this problem with photometric redshifts (photo-z) inferred directly from the SN light curve in combination with Gaussian and full priors from host-galaxy photo-z estimates. Using the DES 5-yr photometrically classified SN sample, we consider several photo-z algorithms as host-galaxy photo-z priors, including the Self-Organizing Map redshifts (SOMPZ), Bayesian Photometric Redshifts (BPZ), and Directional-Neighbourhood Fitting (DNF) redshift estimates employed in the DES 3 × 2 point analyses. With detailed catalogue-level simulations of the DES 5-yr sample, we find that the simulated w can be recovered within when using SN+SOMPZ or DNF prior photo-z, smaller than the average statistical uncertainty for these samples of 0.03. With data, we obtain biases in w consistent with simulations within ∼1 σ for three of the five photo-z variants. We further evaluate how photo-z systematics interplay with photometric classification and find classification introduces a subdominant systematic component. This work lays the foundation for next-generation fully photometric SNe Ia cosmological analyses.

AB - Cosmological analyses with Type Ia Supernovae (SNe Ia) have traditionally been reliant on spectroscopy for both classifying the type of supernova and obtaining reliable redshifts to measure the distance-redshift relation. While obtaining a host-galaxy spectroscopic redshift for most SNe is feasible for small-area transient surveys, it will be too resource intensive for upcoming large-area surveys such as the Vera Rubin Observatory Legacy Survey of Space and Time, which will observe on the order of millions of SNe. Here, we use data from the Dark Energy Survey (DES) to address this problem with photometric redshifts (photo-z) inferred directly from the SN light curve in combination with Gaussian and full priors from host-galaxy photo-z estimates. Using the DES 5-yr photometrically classified SN sample, we consider several photo-z algorithms as host-galaxy photo-z priors, including the Self-Organizing Map redshifts (SOMPZ), Bayesian Photometric Redshifts (BPZ), and Directional-Neighbourhood Fitting (DNF) redshift estimates employed in the DES 3 × 2 point analyses. With detailed catalogue-level simulations of the DES 5-yr sample, we find that the simulated w can be recovered within when using SN+SOMPZ or DNF prior photo-z, smaller than the average statistical uncertainty for these samples of 0.03. With data, we obtain biases in w consistent with simulations within ∼1 σ for three of the five photo-z variants. We further evaluate how photo-z systematics interplay with photometric classification and find classification introduces a subdominant systematic component. This work lays the foundation for next-generation fully photometric SNe Ia cosmological analyses.

KW - (cosmology:) dark energy

KW - transients: supernovae

UR - https://www.scopus.com/pages/publications/105012370754

U2 - 10.1093/mnras/stae2703

DO - 10.1093/mnras/stae2703

M3 - Article

AN - SCOPUS:105012370754

SN - 0035-8711

VL - 536

SP - 1948

EP - 1966

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 2

ER -

Evaluating cosmological biases using photometric redshifts for Type Ia Supernova cosmology with the Dark Energy Survey Supernova Program

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