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Title: The atomic gas sequence and mass–metallicity relation from dwarfs to massive galaxies

Journal Article · · Monthly Notices of the Royal Astronomical Society
ORCiD logo [1]; ORCiD logo [2];  [3]; ORCiD logo [4];  [5]; ORCiD logo [6];  [7];  [8]; ORCiD logo [7];  [9];  [2];  [2];  [7];  [10];  [2]; ORCiD logo [11]; ORCiD logo [2]; ORCiD logo [12]; ORCiD logo [13]; ORCiD logo [7] more »; ORCiD logo [9];  [14];  [7]; ORCiD logo [15];  [7];  [7];  [7];  [16];  [17];  [9];  [2];  [18];  [19];  [5];  [20];  [21]; ORCiD logo [22];  [22]; ORCiD logo [23];  [24];  [7];  [9]; ORCiD logo [25];  [2];  [26]; ORCiD logo [27];  [9] « less
  1. University College London (United Kingdom); University of Edinburgh (United Kingdom)
  2. University College London (United Kingdom)
  3. Siena College, Loudonville, NY (United States)
  4. The University of Western Australia (Australia); ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) (Australia)
  5. Chinese Academy of Sciences, Beijing (China)
  6. University of Pittsburgh, PA (United States)
  7. Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)
  8. Boston University, MA (United States)
  9. NSF NOIRLab, Tucson, AZ (United States)
  10. Universidad Nacional Autonoma´ de Mexico (Mexico)
  11. University College London (United Kingdom); The Ohio State University, Columbus, OH (United States)
  12. The Barcelona Institute of Science and Technology (Spain); Universidad de los Andes, Bogota, (Colombia)
  13. Universidad de los Andes, Bogota, (Colombia); Institut d’Estudis Espacials de Catalunya (IEEC), Barcelona (Spain); University of Portsmouth (United Kingdom)
  14. Southern Methodist University, Dallas, TX (United States)
  15. University of Edinburgh (United Kingdom); The Ohio State University, Columbus, OH (United States)
  16. Institute of Space Sciences, Barcelona (Spain)
  17. The Ohio State University, Columbus, OH (United States); Institució Catalana de Recerca i Estudis Avançats, Barcelona (Spain); The Barcelona Institute of Science and Technology, Bellaterra Barcelona (Spain)
  18. University of Wyoming, Laramie, WY (United States); University of California, Berkeley, CA (United States)
  19. University of California, Berkeley, CA (United States)
  20. Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States); Kansas State University, Manhattan, KS (United States); Sejong University, Seoul (Korea)
  21. CIEMAT, Madrid (Spain)
  22. University of Michigan, Ann Arbor, MI (United States)
  23. University of Cambridge (United Kingdom)
  24. Instituto de Astrofísica de Andalucía (CSIC), Granada (Spain); University of St Andrews (United Kingdom)
  25. Institute of Space Sciences, Barcelona (Spain); University of Wyoming, Laramie, WY (United States)
  26. Instituto de Astrof´ısica de Andaluc´ıa (CSIC), Granada (Spain)
  27. University of St Andrews (United Kingdom)

Galaxy scaling relations provide insights into the processes that drive galaxy evolution. The extension of these scaling relations into the dwarf galaxy regime is of particular interest. This is because dwarf galaxies represent a crucial stage in galaxy evolution, and understanding them could also shed light on their role in reionizing the early Universe. There is currently no consensus on the processes that dominate the evolution of dwarfs. In this work, we constrain the atomic gas sequence (stellar mass versus atomic gas fraction) and mass–metallicity relation (stellar mass versus gas-phase metallicity) from dwarf (⁠106.5 M⁠) to massive (⁠1011.5 M) galaxies in the local Universe. The combined optical and 21-cm spectroscopic observations of the Dark Energy Spectroscopic Instrument and Arecibo Legacy Fast ALFA surveys allow us to constrain both scaling relations simultaneously. We find a slope change of the atomic gas sequence at a stellar mass of ~109 M⁠. We also find that the shape and scatter of the atomic gas sequence and mass–metallicity relation are strongly linked for both dwarfs and more massive galaxies. Consequently, the low-mass slope change of the atomic gas sequence is imprinted onto the mass–metallicity relation of dwarf galaxies. The mass scale of the measured slope change is consistent with a predicted escape velocity threshold below which low-mass galaxies experience significant supernova-driven gas loss, as well as with a reduction in cold gas accretion onto more massive galaxies.

Research Organization:
Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States); Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC); University of Michigan, Ann Arbor, MI (United States)
Sponsoring Organization:
National Key Research and Development Program of China; National Natural Science Foundation of China; U.S. National Science Foundation (NSF), Division of Astronomical Sciences; USDOE Office of Science (SC), High Energy Physics (HEP)
Grant/Contract Number:
AC02-05CH11231; SC0019193; SC0020086
OSTI ID:
2478029
Journal Information:
Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 3 Vol. 535; ISSN 0035-8711; ISSN 1365-2966
Publisher:
Oxford University Press (OUP)Copyright Statement
Country of Publication:
United States
Language:
English

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