The Growth of Galaxy Stellar Haloes over 0.2 ≤ z ≤ 1.1
Galaxies are predicted to assemble their stellar haloes through the accretion of stellar material from interactions with their cosmic environment. Observations that trace stellar halo buildup probe the processes that drive galaxy size and stellar mass growth. We investigate stellar halo assembly ove...
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ade9a8 |
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| author | Devin J. Williams Ivana Damjanov Marcin Sawicki Harrison Souchereau Lingjian Chen Guillaume Desprez Angelo George Marianna Annunziatella Stéphane Arnouts Stephen Gwyn Danilo Marchesini Anna Sajina |
| author_facet | Devin J. Williams Ivana Damjanov Marcin Sawicki Harrison Souchereau Lingjian Chen Guillaume Desprez Angelo George Marianna Annunziatella Stéphane Arnouts Stephen Gwyn Danilo Marchesini Anna Sajina |
| author_sort | Devin J. Williams |
| collection | DOAJ |
| description | Galaxies are predicted to assemble their stellar haloes through the accretion of stellar material from interactions with their cosmic environment. Observations that trace stellar halo buildup probe the processes that drive galaxy size and stellar mass growth. We investigate stellar halo assembly over 0.2 ≤ z ≤ 1.1 in a mass-complete ( M _⋆ ≥ 10 ^9.5 M _⊙ ) sample of 242,456 star-forming galaxies (SFGs) and 88,421 quiescent galaxies (QGs) from the CLAUDS and HSC-SSP surveys. We extract galaxy rest-frame g -band surface brightness ( μ _g ) profiles to study faint, extended emission in galaxy outskirts. We examine trends in galaxy assembly by analyzing the median μ _g profiles in different SFG and QG M _⋆ ranges with decreasing redshift and connecting evolution in galaxy μ _g profiles with the underlying stellar mass growth in galaxies. Since z = 1.1, the majority of evolution in the median μ _g profiles of galaxies (∼64% in SFGs and ∼71% in QGs) occurs throughout their stellar halo regions (2–10 R _e ). More-massive galaxies assemble stellar halo material more rapidly at 0.2 ≤ z ≤ 1.1. Over this period, QGs grow a larger fraction of their stellar haloes than SFGs at fixed M _⋆ (factor of ∼1.2). Although star formation can account for the stellar halo growth observed in low-mass SFGs (10 ^9.5 M _⊙ ≤ M _⋆ < 10 ^10.5 M _⊙ ), high-mass SFGs ( M _⋆ ≥ 10 ^10.5 M _⊙ ), and both low- and high-mass QGs require an additional assembly mechanism. Our results suggest accretion via minor mergers drives additional stellar halo growth in these galaxies. The contribution from accretion is larger in more-massive galaxies (over M _⋆ ≥ 10 ^9.5 M _⊙ ), and QGs exhibit larger fractional increases to their ex situ fractions over 0.2 ≤ z ≤ 1.1 than SFGs at fixed M _⋆ . |
| format | Article |
| id | doaj-art-021e372133b343ada1c1922e01a9b287 |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-021e372133b343ada1c1922e01a9b2872025-08-20T04:00:32ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01989110710.3847/1538-4357/ade9a8The Growth of Galaxy Stellar Haloes over 0.2 ≤ z ≤ 1.1Devin J. Williams0Ivana Damjanov1https://orcid.org/0000-0003-4797-5246Marcin Sawicki2https://orcid.org/0000-0002-7712-7857Harrison Souchereau3https://orcid.org/0000-0001-5079-1865Lingjian Chen4Guillaume Desprez5https://orcid.org/0000-0001-8325-1742Angelo George6https://orcid.org/0009-0009-2742-7702Marianna Annunziatella7https://orcid.org/0000-0002-8053-8040Stéphane Arnouts8Stephen Gwyn9https://orcid.org/0000-0001-8221-8406Danilo Marchesini10https://orcid.org/0000-0001-9002-3502Anna Sajina11https://orcid.org/0000-0002-1917-1200Institute for Computational Astrophysics and Department of Astronomy & Physics, Saint Mary’s University , 923 Robie Street, Halifax, NS B3H 3C3, CanadaInstitute for Computational Astrophysics and Department of Astronomy & Physics, Saint Mary’s University , 923 Robie Street, Halifax, NS B3H 3C3, CanadaInstitute for Computational Astrophysics and Department of Astronomy & Physics, Saint Mary’s University , 923 Robie Street, Halifax, NS B3H 3C3, CanadaInstitute for Computational Astrophysics and Department of Astronomy & Physics, Saint Mary’s University , 923 Robie Street, Halifax, NS B3H 3C3, Canada; Department of Astronomy, Yale University , New Haven, CT 06511, USAInstitute for Computational Astrophysics and Department of Astronomy & Physics, Saint Mary’s University , 923 Robie Street, Halifax, NS B3H 3C3, CanadaInstitute for Computational Astrophysics and Department of Astronomy & Physics, Saint Mary’s University , 923 Robie Street, Halifax, NS B3H 3C3, CanadaInstitute for Computational Astrophysics and Department of Astronomy & Physics, Saint Mary’s University , 923 Robie Street, Halifax, NS B3H 3C3, CanadaCentro de Astrobiología (CSIC-INTA) , Ctra de Torrejón a Ajalvir, km 4, E-28850 Torrejón de Ardoz, Madrid, SpainAix Marseille Université , CNRS, CNES, LAM, 38 rue Frédéric Joliot-Curie, Marseille 13388 cedex 13, FranceNRC Herzberg Astronomy and Astrophysics , 5071 West Saanich Road, Victoria, BC V9E 2E7, CanadaDepartment of Physics and Astronomy, Tufts University , Medford, MA 02155, USADepartment of Physics and Astronomy, Tufts University , Medford, MA 02155, USAGalaxies are predicted to assemble their stellar haloes through the accretion of stellar material from interactions with their cosmic environment. Observations that trace stellar halo buildup probe the processes that drive galaxy size and stellar mass growth. We investigate stellar halo assembly over 0.2 ≤ z ≤ 1.1 in a mass-complete ( M _⋆ ≥ 10 ^9.5 M _⊙ ) sample of 242,456 star-forming galaxies (SFGs) and 88,421 quiescent galaxies (QGs) from the CLAUDS and HSC-SSP surveys. We extract galaxy rest-frame g -band surface brightness ( μ _g ) profiles to study faint, extended emission in galaxy outskirts. We examine trends in galaxy assembly by analyzing the median μ _g profiles in different SFG and QG M _⋆ ranges with decreasing redshift and connecting evolution in galaxy μ _g profiles with the underlying stellar mass growth in galaxies. Since z = 1.1, the majority of evolution in the median μ _g profiles of galaxies (∼64% in SFGs and ∼71% in QGs) occurs throughout their stellar halo regions (2–10 R _e ). More-massive galaxies assemble stellar halo material more rapidly at 0.2 ≤ z ≤ 1.1. Over this period, QGs grow a larger fraction of their stellar haloes than SFGs at fixed M _⋆ (factor of ∼1.2). Although star formation can account for the stellar halo growth observed in low-mass SFGs (10 ^9.5 M _⊙ ≤ M _⋆ < 10 ^10.5 M _⊙ ), high-mass SFGs ( M _⋆ ≥ 10 ^10.5 M _⊙ ), and both low- and high-mass QGs require an additional assembly mechanism. Our results suggest accretion via minor mergers drives additional stellar halo growth in these galaxies. The contribution from accretion is larger in more-massive galaxies (over M _⋆ ≥ 10 ^9.5 M _⊙ ), and QGs exhibit larger fractional increases to their ex situ fractions over 0.2 ≤ z ≤ 1.1 than SFGs at fixed M _⋆ .https://doi.org/10.3847/1538-4357/ade9a8Galaxy evolutionGalaxy photometryGalaxy interactionsGalaxy mergersGalaxy stellar halosGalaxy structure |
| spellingShingle | Devin J. Williams Ivana Damjanov Marcin Sawicki Harrison Souchereau Lingjian Chen Guillaume Desprez Angelo George Marianna Annunziatella Stéphane Arnouts Stephen Gwyn Danilo Marchesini Anna Sajina The Growth of Galaxy Stellar Haloes over 0.2 ≤ z ≤ 1.1 The Astrophysical Journal Galaxy evolution Galaxy photometry Galaxy interactions Galaxy mergers Galaxy stellar halos Galaxy structure |
| title | The Growth of Galaxy Stellar Haloes over 0.2 ≤ z ≤ 1.1 |
| title_full | The Growth of Galaxy Stellar Haloes over 0.2 ≤ z ≤ 1.1 |
| title_fullStr | The Growth of Galaxy Stellar Haloes over 0.2 ≤ z ≤ 1.1 |
| title_full_unstemmed | The Growth of Galaxy Stellar Haloes over 0.2 ≤ z ≤ 1.1 |
| title_short | The Growth of Galaxy Stellar Haloes over 0.2 ≤ z ≤ 1.1 |
| title_sort | growth of galaxy stellar haloes over 0 2 ≤ z ≤ 1 1 |
| topic | Galaxy evolution Galaxy photometry Galaxy interactions Galaxy mergers Galaxy stellar halos Galaxy structure |
| url | https://doi.org/10.3847/1538-4357/ade9a8 |
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