EDGE : What shapes the relationship between H i and stellar observables in faint dwarf galaxies?
(2022) In Monthly Notices of the Royal Astronomical Society 511(4). p.5672-5681- Abstract
We show how the interplay between feedback and mass-growth histories introduces scatter in the relationship between stellar and neutral gas properties of field faint dwarf galaxies (M∗ 106, M⊙). Across a suite of cosmological, high-resolution zoomed simulations, we find that dwarf galaxies of stellar masses 105 ≤ M∗ ≤ 106, M⊙ are bimodal in their cold gas content, being either H i-rich or H i-deficient. This bimodality is generated through the coupling between (i) the modulation of H i contents by the background of ultraviolet radiation (UVB) at late times and (ii) the significant scatter in the stellar-to-halo mass relationship induced by reionization. Furthermore, our H i-rich dwarfs exhibit disturbed and time-variable neutral gas... (More)
We show how the interplay between feedback and mass-growth histories introduces scatter in the relationship between stellar and neutral gas properties of field faint dwarf galaxies (M∗ 106, M⊙). Across a suite of cosmological, high-resolution zoomed simulations, we find that dwarf galaxies of stellar masses 105 ≤ M∗ ≤ 106, M⊙ are bimodal in their cold gas content, being either H i-rich or H i-deficient. This bimodality is generated through the coupling between (i) the modulation of H i contents by the background of ultraviolet radiation (UVB) at late times and (ii) the significant scatter in the stellar-to-halo mass relationship induced by reionization. Furthermore, our H i-rich dwarfs exhibit disturbed and time-variable neutral gas distributions primarily due to stellar feedback. Over the last four billion years, we observe order-of-magnitude changes around the median M H,\small I, factor-of-a-few variations in H i spatial extents, and spatial offsets between H i and stellar components regularly exceeding the galaxies' optical sizes. Time variability introduces further scatter in the M∗-M H, small I relation and affects a galaxy's detectability in H i at any given time. These effects will need to be accounted for when interpreting observations of the population of faint, H i-bearing dwarfs by the combination of optical and radio wide, deep surveys.
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- author
- Rey, Martin P. LU ; Pontzen, Andrew ; Agertz, Oscar LU ; Orkney, Matthew D.A. ; Read, Justin I. ; Saintonge, Amelie ; Kim, Stacy Y. and Das, Payel
- organization
- publishing date
- 2022-04
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- Galaxies: dwarf, Galaxies: evolution, Galaxies: haloes, Galaxies: structure, Methods: numerical
- in
- Monthly Notices of the Royal Astronomical Society
- volume
- 511
- issue
- 4
- pages
- 10 pages
- publisher
- Oxford University Press
- external identifiers
-
- scopus:85127448895
- ISSN
- 0035-8711
- DOI
- 10.1093/mnras/stac502
- language
- English
- LU publication?
- yes
- id
- 467e9b62-6ada-4255-a6f7-94c1f7cbe137
- date added to LUP
- 2022-06-02 11:03:34
- date last changed
- 2024-04-18 10:48:37
@article{467e9b62-6ada-4255-a6f7-94c1f7cbe137, abstract = {{<p>We show how the interplay between feedback and mass-growth histories introduces scatter in the relationship between stellar and neutral gas properties of field faint dwarf galaxies (M∗ 106, M⊙). Across a suite of cosmological, high-resolution zoomed simulations, we find that dwarf galaxies of stellar masses 105 ≤ M∗ ≤ 106, M⊙ are bimodal in their cold gas content, being either H i-rich or H i-deficient. This bimodality is generated through the coupling between (i) the modulation of H i contents by the background of ultraviolet radiation (UVB) at late times and (ii) the significant scatter in the stellar-to-halo mass relationship induced by reionization. Furthermore, our H i-rich dwarfs exhibit disturbed and time-variable neutral gas distributions primarily due to stellar feedback. Over the last four billion years, we observe order-of-magnitude changes around the median M H,\small I, factor-of-a-few variations in H i spatial extents, and spatial offsets between H i and stellar components regularly exceeding the galaxies' optical sizes. Time variability introduces further scatter in the M∗-M H, small I relation and affects a galaxy's detectability in H i at any given time. These effects will need to be accounted for when interpreting observations of the population of faint, H i-bearing dwarfs by the combination of optical and radio wide, deep surveys. </p>}}, author = {{Rey, Martin P. and Pontzen, Andrew and Agertz, Oscar and Orkney, Matthew D.A. and Read, Justin I. and Saintonge, Amelie and Kim, Stacy Y. and Das, Payel}}, issn = {{0035-8711}}, keywords = {{Galaxies: dwarf; Galaxies: evolution; Galaxies: haloes; Galaxies: structure; Methods: numerical}}, language = {{eng}}, number = {{4}}, pages = {{5672--5681}}, publisher = {{Oxford University Press}}, series = {{Monthly Notices of the Royal Astronomical Society}}, title = {{EDGE : What shapes the relationship between H i and stellar observables in faint dwarf galaxies?}}, url = {{http://dx.doi.org/10.1093/mnras/stac502}}, doi = {{10.1093/mnras/stac502}}, volume = {{511}}, year = {{2022}}, }