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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>μ</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>eff</mml:mi> <mml:mo>,</mml:mo> <mml:mi mathvariant="italic">g</mml:mi> </mml:mrow> </mml:msub> <mml:mo>&gt;</mml:mo> <mml:mn>24.2</mml:mn> <mml:mspace width="0.25em"/> <mml:mi>mag</mml:mi> <mml:mspace width="0.25em"/> <mml:msup> <mml:mrow> <mml:mi>arcsec</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2</mml:mn> </mml:mrow> </mml:msup> </mml:math> are drawn from the Dark Energy Survey Year 3 catalog while the hosts with masses <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>9.0</mml:mn> <mml:mo>&lt;</mml:mo> <mml:mi>log</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi class="MJX-tex-calligraphic" mathvariant="script">M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⋆</mml:mo> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo stretchy="false">)</mml:mo> <mml:mo>&lt;</mml:mo> <mml:mn>11.0</mml:mn> </mml:math> 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.

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Journal
The Astrophysical Journal
Published
2024-11-01
DOI
https://doi.org/10.3847/1538-4357/ad79fe
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1
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Galaxies: Formation, Evolution, Phenomena
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article
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article

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

A. Pieres, Ting-Yun Cheng, D. J. James, I. Ferrero et al.
1 citations
The Astrophysical Journal
Galaxies: Formation, Evolution, Phenomena
0.33
article

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

A. Pieres, Ting-Yun Cheng, D. J. James, I. Ferrero, S. R. Hinton, Paul Martini, J. Carretero, J. García-Bellido, J. L. Marshall, L. N. da Costa, M. R. Smith, Dimitrios Tanoglidis, Michael S. Schubnell, A. Palmese, D. Gruen, A. A. Plazas, E. Suchyta, G. Giannini, O. Alves, P. Wiseman, A. R. Walker, J. C. Bhattacharyya, N. Weaverdyck, Andrew B. Pace, Eusebio Sanchez, Louis E. Strigari, J. Mena-Fernández, Burçı̇n Mutlu-Pakdı̇l, A. Carnero Rosell, K. Kuehn, R. A. Gruendl, J. García-Bellido, David Bacon, K. Honscheid, Annika H. G. Peter, M. Vincenzi, A. Drlica-Wagner, T. M. Davis, M. E. C. Swanson, R. Miquel, M. E. S. Pereira, S. Desai, F. Andrade-Oliveira, M. Aguena, I. Sevilla-Noarbe, Dar A. Roberts, B. X. Santiago, G. Tarle, Peter Doel, D. Brooks
article en
1 citations

Abstract

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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>μ</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>eff</mml:mi> <mml:mo>,</mml:mo> <mml:mi mathvariant="italic">g</mml:mi> </mml:mrow> </mml:msub> <mml:mo>&gt;</mml:mo> <mml:mn>24.2</mml:mn> <mml:mspace width="0.25em"/> <mml:mi>mag</mml:mi> <mml:mspace width="0.25em"/> <mml:msup> <mml:mrow> <mml:mi>arcsec</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2</mml:mn> </mml:mrow> </mml:msup> </mml:math> are drawn from the Dark Energy Survey Year 3 catalog while the hosts with masses <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>9.0</mml:mn> <mml:mo>&lt;</mml:mo> <mml:mi>log</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi class="MJX-tex-calligraphic" mathvariant="script">M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⋆</mml:mo> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo stretchy="false">)</mml:mo> <mml:mo>&lt;</mml:mo> <mml:mn>11.0</mml:mn> </mml:math> 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.

The Astrophysical JournalVol. 975(2)
Dartmouth College (US), Institució Catalana de Recerca i Estudis Avançats (ES), Oak Ridge National Laboratory (US), Universidade Federal do Rio Grande do Sul (BR), Fermi National Accelerator Laboratory (US), Lawrence Berkeley National Laboratory (US), University of Illinois Urbana-Champaign (US), Universidad de La Laguna (ES), Universität Hamburg (DE), The University of Queensland (AU), University of Oslo (NO), Institute for High Energy Physics (ES), Durham University (GB), University of Michigan (US), Lowell Observatory (US), Mitchell Institute (US), SLAC National Accelerator Laboratory (US), Australian Astronomical Observatory (AU), Institute for Advanced Study (US), University of Chicago (US), Valongo Observatory (BR), Kavli Institute for Particle Astrophysics and Cosmology (US), Center for Astrophysics Harvard & Smithsonian (US), National Observatory (BR), Instituto de Astrofísica de Canarias (ES), National Center for Supercomputing Applications (US), Cerro Tololo Inter-American Observatory (CL), Laboratoire de Physique Subatomique et de Cosmologie (FR), Laboratório Interinstitucional de e-Astronomia (BR), Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (ES), University of Southampton (GB), University College London (GB), The Ohio State University (US), University of Portsmouth (GB), Universidad Autónoma de Madrid (ES), Indian Institute of Technology Hyderabad (IN), Carnegie Mellon University (US), Ludwig-Maximilians-Universität München (DE), Texas A&M University (US), Stanford University (US), Macquarie University (AU)
National Science Foundation, U.S. Department of Energy, University of Pennsylvania, Ohio State University, University of Chicago, University of Portsmouth, Centres de Recerca de Catalunya, University College London, European Commission, University of Sussex, Deutsche Forschungsgemeinschaft, Generalitat de Catalunya, Ministério da Ciência, Tecnologia e Inovação, Conselho Nacional de Desenvolvimento Científico e Tecnológico, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Financiadora de Estudos e Projetos, Ministerio de Ciencia e Innovación, Institut de Física d'Altes Energies, University of Illinois at Urbana-Champaign, Office of Science, Science and Technology Facilities Council, European Regional Development Fund, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, High Energy Physics, Integrated Electronics Engineering Center, Binghamton University, Argonne National Laboratory, Fermilab, Lawrence Berkeley National Laboratory, SLAC National Accelerator Laboratory
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Galaxies: Formation, Evolution, Phenomena
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