Gas and star formation in satellites of Milky Way analogs
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| Main Authors: | , , , , , , , , , , , |
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| Format: | Preprint |
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2023
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| _version_ | 1866914701665894400 |
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| author | Jones, Michael G. Sand, David J. Karunakaran, Ananthan Spekkens, Kristine Oman, Kyle A. Bennet, Paul Besla, Gurtina Crnojevic, Denija Cuillandre, Jean-Charles Fielder, Catherine E. Gwyn, Stephen Mutlu-Pakdil, Burcin |
| author_facet | Jones, Michael G. Sand, David J. Karunakaran, Ananthan Spekkens, Kristine Oman, Kyle A. Bennet, Paul Besla, Gurtina Crnojevic, Denija Cuillandre, Jean-Charles Fielder, Catherine E. Gwyn, Stephen Mutlu-Pakdil, Burcin |
| contents | We have imaged the entirety of eight (plus one partial) Milky Way-like satellite systems, a total of 42 (45) satellites, from the Satellites Around Galactic Analogs (SAGA) II catalog in both H$α$ and HI with the Canada-France-Hawaii Telescope and the Jansky Very Large Array. In these eight systems we have identified four cases where a satellite appears to be currently undergoing ram pressure stripping (RPS) as its HI gas collides with the circumgalactic medium (CGM) of its host. We also see a clear suppression of gas fraction ($M_\mathrm{HI}/M_\ast$) with decreasing (projected) satellite--host separation; to our knowledge, the first time this has been observed in a sample of Milky Way-like systems. Comparisons to the Auriga, APOSTLE, and TNG50 cosmological zoom-in simulations show consistent global behavior, but they systematically under-predict gas fractions across all satellites by roughly 0.5 dex. Using a simplistic RPS model we estimate the average peak CGM density that satellites in these systems have encountered to be $\log ρ_\mathrm{cgm}/\mathrm{g\,cm^{-3}} \approx -27.3$. Furthermore, we see tentative evidence that these satellites are following a specific star formation rate-to-gas fraction relation that is distinct from field galaxies. Finally, we detect one new gas-rich satellite in the UGC903 system with an optical size and surface brightness meeting the standard criteria to be considered an ultra-diffuse galaxy. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2311_02152 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Gas and star formation in satellites of Milky Way analogs Jones, Michael G. Sand, David J. Karunakaran, Ananthan Spekkens, Kristine Oman, Kyle A. Bennet, Paul Besla, Gurtina Crnojevic, Denija Cuillandre, Jean-Charles Fielder, Catherine E. Gwyn, Stephen Mutlu-Pakdil, Burcin Astrophysics of Galaxies We have imaged the entirety of eight (plus one partial) Milky Way-like satellite systems, a total of 42 (45) satellites, from the Satellites Around Galactic Analogs (SAGA) II catalog in both H$α$ and HI with the Canada-France-Hawaii Telescope and the Jansky Very Large Array. In these eight systems we have identified four cases where a satellite appears to be currently undergoing ram pressure stripping (RPS) as its HI gas collides with the circumgalactic medium (CGM) of its host. We also see a clear suppression of gas fraction ($M_\mathrm{HI}/M_\ast$) with decreasing (projected) satellite--host separation; to our knowledge, the first time this has been observed in a sample of Milky Way-like systems. Comparisons to the Auriga, APOSTLE, and TNG50 cosmological zoom-in simulations show consistent global behavior, but they systematically under-predict gas fractions across all satellites by roughly 0.5 dex. Using a simplistic RPS model we estimate the average peak CGM density that satellites in these systems have encountered to be $\log ρ_\mathrm{cgm}/\mathrm{g\,cm^{-3}} \approx -27.3$. Furthermore, we see tentative evidence that these satellites are following a specific star formation rate-to-gas fraction relation that is distinct from field galaxies. Finally, we detect one new gas-rich satellite in the UGC903 system with an optical size and surface brightness meeting the standard criteria to be considered an ultra-diffuse galaxy. |
| title | Gas and star formation in satellites of Milky Way analogs |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2311.02152 |