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Cited by 55Galaxies: Formation, Evolution, PhenomenaStellar, planetary, and galactic studiesAstrophysics and Star Formation Studies

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emerge – empirical constraints on the formation of passive galaxies

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Moster, Benjamin P, Naab, Thorsten, White, Simon D M·2020·Monthly Notices of the Royal Astronomical Society
DOI 10.1093/mnras/staa3019
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Abstract

We present constraints on the emergence and evolution of passive galaxies with the empirical model emerge, which reproduces the evolution of stellar mass functions (SMFs), specific and cosmic star formation rates since $z$ ≈ 10, ‘quenched’ galaxy fractions, and correlation functions. At fixed halo mass, present-day passive galaxies are more massive than active galaxies, whereas at fixed stellar mass passive galaxies populate more massive haloes in agreement with observations. This effect naturally results from the shape and scatter of the stellar-to-halo mass relation. The stellar mass assembly of present-day passive galaxies is dominated by ‘in situ’ star formation below ∼3 × 1011 M⊙ and by merging and accretion of ‘ex situ’ formed stars at higher mass. The mass dependence is in tension with current cosmological simulations. Lower mass passive galaxies show extended star formation towards low redshift in agreement with IFU surveys. All passive galaxies have main progenitors on the ‘main sequence of star formation’ with the ‘red sequence’ appearing at $z$ ≈ 2. Above this redshift, over 95 per cent of the progenitors of passive galaxies are active. More than 90 per cent of $z$ ≈ 2 ‘main sequence’ galaxies with m* > 1010 M⊙ evolve into present-day passive galaxies. Above redshift 6, more than 80 per cent of the observed SMFs above 109 M⊙ can be accounted for by progenitors of passive galaxies with m* > 1010 M⊙. This implies that high-redshift observations mainly probe the birth of present-day passive galaxies. emerge is available at github.com/bmoster/emerge.

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Research works printed but not linked: 110

  1. Baugh, 2006, Rep. Prog. Phys., 69, 3101, 10.1088/0034-4885/69/12/R02 · DOI
  2. Beare, 2019, ApJ, 873, 78, 10.3847/1538-4357/ab041a · DOI
  3. Behroozi, 2010, ApJ, 717, 379, 10.1088/0004-637X/717/1/379 · DOI
  4. Behroozi, 2013, ApJ, 762, 109, 10.1088/0004-637X/762/2/109 · DOI
  5. Behroozi, 2013, ApJ, 763, 18, 10.1088/0004-637X/763/1/18 · DOI
  6. Bernardi, 2003, AJ, 125, 1849, 10.1086/374256 · DOI
  7. Bernardi, 2011, MNRAS, 412, L6, 10.1111/j.1745-3933.2010.00982.x · DOI
  8. Bernardi, 2019, MNRAS, 489, 5633, 10.1093/mnras/stz2413 · DOI
  9. Bhatawdekar, 2019, MNRAS, 486, 3805, 10.1093/mnras/stz866 · DOI
  10. Blaizot, 2004, MNRAS, 352, 571, 10.1111/j.1365-2966.2004.07947.x · DOI
  11. Blumenthal, 1984, Nature, 311, 517, 10.1038/311517a0 · DOI
  12. Boogaard, 2018, A&A, 619, A27, 10.1051/0004-6361/201833136 · DOI
  13. Boylan-Kolchin, 2008, MNRAS, 383, 93, 10.1111/j.1365-2966.2007.12530.x · DOI
  14. Boylan-Kolchin, 2009, MNRAS, 398, 1150, 10.1111/j.1365-2966.2009.15191.x · DOI
  15. Bryan, 1998, ApJ, 495, 80, 10.1086/305262 · DOI
  16. Cappellari, 2004, PASP, 116, 138, 10.1086/381875 · DOI
  17. Cappellari, 2011, MNRAS, 413, 813, 10.1111/j.1365-2966.2010.18174.x · DOI
  18. Cattaneo, 2006, MNRAS, 370, 1651, 10.1111/j.1365-2966.2006.10608.x · DOI
  19. Cattaneo, 2008, MNRAS, 389, 567, 10.1111/j.1365-2966.2008.13562.x · DOI
  20. Cattaneo, 2011, A&A, 533, A5, 10.1051/0004-6361/201015780 · DOI
  21. Cattaneo, 2013, MNRAS, 430, 686, 10.1093/mnras/sts668 · DOI
  22. Chabrier, 2003, PASP, 115, 763, 10.1086/376392 · DOI · Paper page
  23. Choi, 2015, MNRAS, 449, 4105, 10.1093/mnras/stv575 · DOI
  24. Cole, 1994, MNRAS, 271, 781, 10.1093/mnras/271.4.781 · DOI
  25. Conroy, 2009, ApJ, 696, 620, 10.1088/0004-637X/696/1/620 · DOI
  26. Conroy, 2006, ApJ, 647, 201, 10.1086/503602 · DOI
  27. Cowie, 1996, AJ, 112, 839, 10.1086/118058 · DOI
  28. Davé, 2017, MNRAS, 471, 1671, 10.1093/mnras/stx1693 · DOI
  29. Davidzon, 2018, ApJ, 852, 107, 10.3847/1538-4357/aaa19e · DOI
  30. Dekel, 2006, MNRAS, 368, 2, 10.1111/j.1365-2966.2006.10145.x · DOI
  31. De Lucia, 2006, MNRAS, 366, 499, 10.1111/j.1365-2966.2005.09879.x · DOI
  32. Dolence, 2008, 9th LCI International Conference on High-Performance Clustered Computing
  33. D’Souza, 2014, MNRAS, 443, 1433, 10.1093/mnras/stu1194 · DOI
  34. Dubois, 2014, MNRAS, 444, 1453, 10.1093/mnras/stu1227 · DOI
  35. Duc, 2011, MNRAS, 417, 863, 10.1111/j.1365-2966.2011.19137.x · DOI
  36. Elson, 2007, A&A, 464, 1167, 10.1051/0004-6361:20065081 · DOI
  37. Faber, 2007, ApJ, 665, 265, 10.1086/519294 · DOI
  38. Fall, 1980, MNRAS, 193, 189, 10.1093/mnras/193.2.189 · DOI
  39. Gavazzi, 2002, ApJ, 576, 135, 10.1086/341730 · DOI
  40. Genzel, 2006, Nature, 442, 786, 10.1038/nature05052 · DOI
  41. Genzel, 2008, ApJ, 687, 59, 10.1086/591840 · DOI
  42. Goodman, 2010, Commun. Appl. Math. Comput. Sci., 5, 65, 10.2140/camcos.2010.5.65 · DOI
  43. Grylls, 2020, MNRAS, 491, 634, 10.1093/mnras/stz2956 · DOI
  44. Guo, 2010, MNRAS, 404, 1111, 10.1111/j.1365-2966.2010.16341.x · DOI
  45. Hahn, 2011, MNRAS, 415, 2101, 10.1111/j.1365-2966.2011.18820.x · DOI
  46. Heavens, 2004, Nature, 428, 625, 10.1038/nature02474 · DOI
  47. Henriques, 2019, MNRAS, 485, 3446, 10.1093/mnras/stz577 · DOI
  48. Hirschmann, 2014, MNRAS, 442, 2304, 10.1093/mnras/stu1023 · DOI
  49. Hopkins, 2014, MNRAS, 445, 581, 10.1093/mnras/stu1738 · DOI
  50. Hubble, 1926, ApJ, 64, 321, 10.1086/143018 · DOI
  51. Katsianis, 2017, MNRAS, 464, 4977, 10.1093/mnras/stw2680 · DOI
  52. Kauffmann, 1993, MNRAS, 264, 201, 10.1093/mnras/264.1.201 · DOI
  53. Knobel, 2015, ApJ, 800, 24, 10.1088/0004-637X/800/1/24 · DOI
  54. Lacey, 1993, MNRAS, 262, 627, 10.1093/mnras/262.3.627 · DOI
  55. Lange, 2019, MNRAS, 487, 3112, 10.1093/mnras/stz1466 · DOI
  56. Lewis, 2000, ApJ, 538, 473, 10.1086/309179 · DOI · Paper page
  57. Lilly, 1995, ApJ, 455, 108, 10.1086/176560 · DOI
  58. Liu, 2018, ApJ, 853, 172, 10.3847/1538-4357/aaa600 · DOI
  59. Macciò, 2008, MNRAS, 391, 1940, 10.1111/j.1365-2966.2008.14029.x · DOI
  60. McDermid, 2015, MNRAS, 448, 3484, 10.1093/mnras/stv105 · DOI
  61. Mandelbaum, 2006, MNRAS, 368, 715, 10.1111/j.1365-2966.2006.10156.x · DOI · Paper page
  62. Mandelbaum, 2016, MNRAS, 457, 3200, 10.1093/mnras/stw188 · DOI
  63. Mo, 1996, MNRAS, 282, 347, 10.1093/mnras/282.2.347 · DOI
  64. Moore, 2001, Mining the Sky, 71, 10.1007/10849171_5 · DOI
  65. More, 2011, MNRAS, 410, 210, 10.1111/j.1365-2966.2010.17436.x · DOI
  66. Moster, 2010, ApJ, 710, 903, 10.1088/0004-637X/710/2/903 · DOI
  67. Moster, 2013, MNRAS, 428, 3121, 10.1093/mnras/sts261 · DOI · Paper page
  68. Moster, 2018, MNRAS, 477, 1822, 10.1093/mnras/sty655 · DOI
  69. Mutch, 2013, MNRAS, 435, 2445, 10.1093/mnras/stt1453 · DOI
  70. Naab, 2017, ARA&A, 55, 59, 10.1146/annurev-astro-081913-040019 · DOI
  71. Oser, 2010, ApJ, 725, 2312, 10.1088/0004-637X/725/2/2312 · DOI
  72. Peacock, 2000, MNRAS, 318, 1144, 10.1046/j.1365-8711.2000.03779.x · DOI
  73. Pérez-González, 2008, ApJ, 675, 234, 10.1086/523690 · DOI
  74. Pillepich, 2018, MNRAS, 475, 648, 10.1093/mnras/stx3112 · DOI
  75. Planck Collaboration VI, 2020, A&A, A6
  76. Renzini, 2015, ApJ, 801, L29, 10.1088/2041-8205/801/2/L29 · DOI
  77. Ruiz, 2015, MNRAS, 454, 1605, 10.1093/mnras/stv2030 · DOI
  78. Salmon, 2015, ApJ, 799, 183, 10.1088/0004-637X/799/2/183 · DOI
  79. Sheth, 2004, MNRAS, 349, 1464, 10.1111/j.1365-2966.2004.07622.x · DOI
  80. Somerville, 2015, ARA&A, 53, 51, 10.1146/annurev-astro-082812-140951 · DOI
  81. Somerville, 1999, MNRAS, 310, 1087, 10.1046/j.1365-8711.1999.03032.x · DOI
  82. Springel, 2005, MNRAS, 364, 1105, 10.1111/j.1365-2966.2005.09655.x · DOI · Paper page
  83. Springel, 2005, MNRAS, 361, 776, 10.1111/j.1365-2966.2005.09238.x · DOI
  84. Tacchella, 2015, Science, 348, 314, 10.1126/science.1261094 · DOI
  85. Tacchella, 2019, MNRAS, 487, 5416, 10.1093/mnras/stz1657 · DOI
  86. Tacconi, 2013, ApJ, 768, 74, 10.1088/0004-637X/768/1/74 · DOI
  87. Teyssier, 2013, MNRAS, 429, 3068, 10.1093/mnras/sts563 · DOI
  88. Thomas, 2005, ApJ, 621, 673, 10.1086/426932 · DOI
  89. Thomas, 2010, MNRAS, 404, 1775, 10.1111/j.1365-2966.2010.16427.x · DOI
  90. Tinker, 2012, ApJ, 755, L5, 10.1088/2041-8205/755/1/L5 · DOI
  91. Trujillo, 2006, ApJ, 650, 18, 10.1086/506464 · DOI
  92. Tweed, 2018, MNRAS, 477, 1427, 10.1093/mnras/sty507 · DOI
  93. Vale, 2004, MNRAS, 353, 189, 10.1111/j.1365-2966.2004.08059.x · DOI
  94. van der Wel, 2014, ApJ, 788, 28, 10.1088/0004-637X/788/1/28 · DOI
  95. van Dokkum, 2008, ApJ, 677, L5, 10.1086/587874 · DOI
  96. Vogelsberger, 2014, MNRAS, 444, 1518, 10.1093/mnras/stu1536 · DOI
  97. Wang, 2015, MNRAS, 454, 83, 10.1093/mnras/stv1937 · DOI
  98. Wechsler, 2018, ARA&A, 56, 435, 10.1146/annurev-astro-081817-051756 · DOI
  99. Wechsler, 1998, ApJ, 506, 19, 10.1086/306229 · DOI
  100. Wechsler, 2002, ApJ, 568, 52, 10.1086/338765 · DOI
  101. Wetzel, 2013, MNRAS, 432, 336, 10.1093/mnras/stt469 · DOI
  102. Whitaker, 2014, ApJ, 795, 104, 10.1088/0004-637X/795/2/104 · DOI
  103. Whitaker, 2012, ApJ, 754, L29, 10.1088/2041-8205/754/2/L29 · DOI
  104. White, 1991, ApJ, 379, 52, 10.1086/170483 · DOI
  105. White, 1978, MNRAS, 183, 341, 10.1093/mnras/183.3.341 · DOI · Paper page
  106. Wojtak, 2013, MNRAS, 428, 2407, 10.1093/mnras/sts203 · DOI
  107. Wright, 2018, MNRAS, 480, 3491, 10.1093/mnras/sty2136 · DOI
  108. Yang, 2003, MNRAS, 339, 1057, 10.1046/j.1365-8711.2003.06254.x · DOI
  109. Zehavi, 2004, ApJ, 608, 16, 10.1086/386535 · DOI
  110. Zehavi, 2018, ApJ, 853, 84, 10.3847/1538-4357/aaa54a · DOI

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    “…been identified), implying that the total accreted stellar mass is likely to be close to the sum of the five satellites discussed here (which is on the low side of, but consistent with the predictions for Milky Way-mass galaxies by Behroozi et al. 2019 and Moster et al. 2019, who find 1−5× 109 M ).”
    Result

Metadata

Authors
Moster, B. P., Naab, T., & White, S. D. M.
Affiliations
Max Planck Institute for Astrophysics (DE)
Corresponding author
Moster, Benjamin P
ORCID
Venue
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Published
2020-10-05
Volume
499
Issue
4
Pages
4748-4767
ISSN
  • 0035-8711 (ISSN-L)
  • 1365-2966
DOI
10.1093/mnras/staa3019
OpenAlex
W2982082610
Cited by
55
References
2
Citations by year
2026: 2 · 2025: 9 · 2024: 8 · 2023: 10 · 2022: 7 · 2021: 14 · 2020: 4
FWCI
3.90
Type
journal article
Language
en
Open access
Licence
academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model (vor)
Locations
  • Monthly Notices of the Royal Astronomical Society (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • MPG.PuRe (Max Planck Society) (submittedVersion)
  • arXiv (Cornell University)
Funders
Deutsche Forschungsgemeinschaft (MO 2979/1-1, 390783311)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
Keywords
quiescent galaxies, galaxy quenching, galaxy evolution, stellar mass function, star formation rate, stellar mass-halo mass relation, galaxy mergers, in situ star formation, galaxy progenitors, star-forming main sequence, red sequence, galaxy halo mass

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