Environmental Quenching of Low-surface-brightness Galaxies Near Hosts from Large Magellanic Cloud to Milky Way Mass Scales

Dark Energy Survey Collaboration

doi:10.3847/1538-4357/ad79fe

Environmental Quenching of Low-surface-brightness Galaxies Near Hosts from Large Magellanic Cloud to Milky Way Mass Scales

Dark Energy Survey Collaboration

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Abstract

Low-surface-brightness galaxies (LSBGs) are excellent probes of quenching and other environmental processes near massive galaxies. We study an extensive sample of LSBGs near massive hosts in the local universe that are distributed across a diverse range of environments. The LSBGs with surface-brightness m_{eff, g} > 24.2 mag arcsec^-2 are drawn from the Dark Energy Survey Year 3 catalog while the hosts with masses 9.0 < log(M_* M_☉) < 11.0 comparable to the Milky Way and the Large Magellanic Cloud are selected from the z0MGS sample. We study the projected radial density profiles of LSBGs as a function of their color and surface brightness around hosts in both the rich Fornax-Eridanus cluster environment and the low-density field. We detect an overdensity with respect to the background density, out to 2.5 times the virial radius for both hosts in the cluster environment and the isolated field galaxies. When the LSBG sample is split by g − i color or surface brightness μ_{eff, g}, we find the LSBGs closer to their hosts are significantly redder and brighter, like their high-surface-brightness counterparts. The LSBGs form a clear “red sequence” in both the cluster and isolated environments that is visible beyond the virial radius of the hosts. This suggests preprocessing of infalling LSBGs and a quenched backsplash population around both host samples. More so, the relative prominence of the “blue cloud” feature implies that preprocessing is ongoing near the isolated hosts compared to the cluster environment where the LSBGs are already well processed.

Original language	English
Article number	244
Journal	Astrophysical Journal
Volume	975
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/ad79fe
State	Published - Nov 1 2024

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. 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\u2019Espai (IEEC/CSIC), the Institut de F\u00EDsica d\u2019Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit\u00E4t M\u00FCnchen and the associated Excellence Cluster Universe, the University of Michigan, NSF\u2019s NOIRLab, 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 at NSF\u2019s 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 Nos. 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\u2019s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. 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. This paper has gone through internal review by the DES collaboration. We thank the anonymous reviewer for the useful feedback that improved this paper. The authors would also like to thank Adam Leroy, Jenny E. Greene, and Benedikt Diemer for their valuable input. J.B. and A.H.G.P. are supported by National Science Foundation grant No. AST-2008110. 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. 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 DESBrazil 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\u2019Espai (IEEC/CSIC), the Institut de F\u00EDsica d\u2019Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit\u00E4t M\u00FCnchen and the associated Excellence Cluster Universe, the University of Michigan, NSF\u2019s NOIRLab, 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 at NSF\u2019s 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 Nos. 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\u2019s Seventh Framework Program (FP7/ 2007-2013) including ERC grant agreements 240672, 291329, and 306478. 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. Software: NumPy (C. R. Harris et al. 2020), Matplotlib (J. D. Hunter 2007), SciPy (P. Virtanen et al. 2020), astropy (Astropy Collaboration et al. 2013, 2018), Source Extractor (E. Bertin & S. Arnouts 1996). This paper has gone through internal review by the DES collaboration. We thank the anonymous reviewer for the useful feedback that improved this paper. The authors would also like to thank Adam Leroy, Jenny E. Greene, and Benedikt Diemer for their valuable input. J.B. and A.H.G.P. are supported by National Science Foundation grant No. AST-2008110.

Funders	Funder number
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
University of Illinois at Urbana-Champaign
Institut de Ciències de l’Espai
Brazilian Instituto Nacional de Ciência e Tecnologia
University of Nottingham
University of Sussex
University of Edinburgh
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Seventh Framework Programme
Ohio State University
Stanford University
University of Chicago
Generalitat de Catalunya
Higher Education Funding Council for England
Financiadora de Estudos e Projetos
DESBrazil Consortium
Ministry of Education and Science of Ukraine
Eidgenössische Technische Hochschule Zürich
University of California, Santa Cruz
Deutsche Forschungsgemeinschaft
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 Research Council
European Regional Development Fund
University of Michigan
Institut de Física d'Altes Energies
University of Pennsylvania
Collaborating Institutions in the Dark Energy Survey
Ludwig-Maximilians-Universität München
National Science Foundation	AST-1138766, AST-2008110, AST-1536171
National Science Foundation
Texas A and M University	2012B-0001
Texas A and M University
Fermi Research Alliance, LLC	DE-AC02-07CH11359
Engineering Research Centers	240672, 306478, 291329
Engineering Research Centers
High Energy Physics	2020
High Energy Physics
Ministerio de Ciencia e Innovación	SEV-2016-0588, SEV-2016-0597, MDM-2015-0509, PGC2018-094773, PGC2018-102021, ESP2017-89838
Ministerio de Ciencia e Innovación
Conselho Nacional de Desenvolvimento Científico e Tecnológico	465376/2014-2
Conselho Nacional de Desenvolvimento Científico e Tecnológico

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10.3847/1538-4357/ad79fe

Cite this

@article{e737e9e444e44d30813f708a275122a1,

title = "Environmental Quenching of Low-surface-brightness Galaxies Near Hosts from Large Magellanic Cloud to Milky Way Mass Scales",

abstract = "Low-surface-brightness galaxies (LSBGs) are excellent probes of quenching and other environmental processes near massive galaxies. We study an extensive sample of LSBGs near massive hosts in the local universe that are distributed across a diverse range of environments. The LSBGs with surface-brightness meff, g > 24.2 mag arcsec-2 are drawn from the Dark Energy Survey Year 3 catalog while the hosts with masses 9.0 < log(M* M☉) < 11.0 comparable to the Milky Way and the Large Magellanic Cloud are selected from the z0MGS sample. We study the projected radial density profiles of LSBGs as a function of their color and surface brightness around hosts in both the rich Fornax-Eridanus cluster environment and the low-density field. We detect an overdensity with respect to the background density, out to 2.5 times the virial radius for both hosts in the cluster environment and the isolated field galaxies. When the LSBG sample is split by g − i color or surface brightness μeff, g, we find the LSBGs closer to their hosts are significantly redder and brighter, like their high-surface-brightness counterparts. The LSBGs form a clear “red sequence” in both the cluster and isolated environments that is visible beyond the virial radius of the hosts. This suggests preprocessing of infalling LSBGs and a quenched backsplash population around both host samples. More so, the relative prominence of the “blue cloud” feature implies that preprocessing is ongoing near the isolated hosts compared to the cluster environment where the LSBGs are already well processed.",

author = "{Dark Energy Survey Collaboration} and J. Bhattacharyya and Peter, {A. H.G.} and P. Martini and B. Mutlu-Pakdil and A. Drlica-Wagner and Pace, {A. B.} and Strigari, {L. E.} and Cheng, {T. Y.} and D. Roberts and D. Tanoglidis and M. Aguena and O. Alves and F. Andrade-Oliveira and D. Bacon and D. Brooks and {Carnero Rosell}, A. and J. Carretero and {da Costa}, {L. N.} and Pereira, {M. E.S.} and Davis, {T. M.} and S. Desai and P. Doel and I. Ferrero and J. Frieman and J. Garc{\'i}a-Bellido and G. Giannini and D. Gruen and Gruendl, {R. A.} and Hinton, {S. R.} and Hollowood, {D. L.} and K. Honscheid and James, {D. J.} and K. Kuehn and Marshall, {J. L.} and J. Mena-Fern{\'a}ndez and R. Miquel and A. Palmese and A. Pieres and {Plazas Malag{\'o}n}, {A. A.} and E. Sanchez and B. Santiago and M. Schubnell and I. Sevilla-Noarbe and M. Smith and E. Suchyta and Swanson, {M. E.C.} and G. Tarle and M. Vincenzi and Walker, {A. R.} and N. Weaverdyck",

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

year = "2024",

month = nov,

day = "1",

doi = "10.3847/1538-4357/ad79fe",

language = "English",

volume = "975",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2",

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TY - JOUR

T1 - Environmental Quenching of Low-surface-brightness Galaxies Near Hosts from Large Magellanic Cloud to Milky Way Mass Scales

AU - Dark Energy Survey Collaboration

AU - Bhattacharyya, J.

AU - Peter, A. H.G.

AU - Martini, P.

AU - Mutlu-Pakdil, B.

AU - Drlica-Wagner, A.

AU - Pace, A. B.

AU - Strigari, L. E.

AU - Cheng, T. Y.

AU - Roberts, D.

AU - Tanoglidis, D.

AU - Aguena, M.

AU - Alves, O.

AU - Andrade-Oliveira, F.

AU - Bacon, D.

AU - Brooks, D.

AU - Carnero Rosell, A.

AU - Carretero, J.

AU - da Costa, L. N.

AU - Pereira, M. E.S.

AU - Davis, T. M.

AU - Desai, S.

AU - Doel, P.

AU - Ferrero, I.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Giannini, G.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Hinton, S. R.

AU - Hollowood, D. L.

AU - Honscheid, K.

AU - James, D. J.

AU - Kuehn, K.

AU - Marshall, J. L.

AU - Mena-Fernández, J.

AU - Miquel, R.

AU - Palmese, A.

AU - Pieres, A.

AU - Plazas Malagón, A. A.

AU - Sanchez, E.

AU - Santiago, B.

AU - Schubnell, M.

AU - Sevilla-Noarbe, I.

AU - Smith, M.

AU - Suchyta, E.

AU - Swanson, M. E.C.

AU - Tarle, G.

AU - Vincenzi, M.

AU - Walker, A. R.

AU - Weaverdyck, N.

PY - 2024/11/1

Y1 - 2024/11/1

N2 - Low-surface-brightness galaxies (LSBGs) are excellent probes of quenching and other environmental processes near massive galaxies. We study an extensive sample of LSBGs near massive hosts in the local universe that are distributed across a diverse range of environments. The LSBGs with surface-brightness meff, g > 24.2 mag arcsec-2 are drawn from the Dark Energy Survey Year 3 catalog while the hosts with masses 9.0 < log(M* M☉) < 11.0 comparable to the Milky Way and the Large Magellanic Cloud are selected from the z0MGS sample. We study the projected radial density profiles of LSBGs as a function of their color and surface brightness around hosts in both the rich Fornax-Eridanus cluster environment and the low-density field. We detect an overdensity with respect to the background density, out to 2.5 times the virial radius for both hosts in the cluster environment and the isolated field galaxies. When the LSBG sample is split by g − i color or surface brightness μeff, g, we find the LSBGs closer to their hosts are significantly redder and brighter, like their high-surface-brightness counterparts. The LSBGs form a clear “red sequence” in both the cluster and isolated environments that is visible beyond the virial radius of the hosts. This suggests preprocessing of infalling LSBGs and a quenched backsplash population around both host samples. More so, the relative prominence of the “blue cloud” feature implies that preprocessing is ongoing near the isolated hosts compared to the cluster environment where the LSBGs are already well processed.

AB - Low-surface-brightness galaxies (LSBGs) are excellent probes of quenching and other environmental processes near massive galaxies. We study an extensive sample of LSBGs near massive hosts in the local universe that are distributed across a diverse range of environments. The LSBGs with surface-brightness meff, g > 24.2 mag arcsec-2 are drawn from the Dark Energy Survey Year 3 catalog while the hosts with masses 9.0 < log(M* M☉) < 11.0 comparable to the Milky Way and the Large Magellanic Cloud are selected from the z0MGS sample. We study the projected radial density profiles of LSBGs as a function of their color and surface brightness around hosts in both the rich Fornax-Eridanus cluster environment and the low-density field. We detect an overdensity with respect to the background density, out to 2.5 times the virial radius for both hosts in the cluster environment and the isolated field galaxies. When the LSBG sample is split by g − i color or surface brightness μeff, g, we find the LSBGs closer to their hosts are significantly redder and brighter, like their high-surface-brightness counterparts. The LSBGs form a clear “red sequence” in both the cluster and isolated environments that is visible beyond the virial radius of the hosts. This suggests preprocessing of infalling LSBGs and a quenched backsplash population around both host samples. More so, the relative prominence of the “blue cloud” feature implies that preprocessing is ongoing near the isolated hosts compared to the cluster environment where the LSBGs are already well processed.

UR - http://www.scopus.com/inward/record.url?scp=85209365964&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/ad79fe

DO - 10.3847/1538-4357/ad79fe

M3 - Article

AN - SCOPUS:85209365964

SN - 0004-637X

VL - 975

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 244

ER -

Environmental Quenching of Low-surface-brightness Galaxies Near Hosts from Large Magellanic Cloud to Milky Way Mass Scales

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