Corvus A: A low-mass, isolated galaxy at 3.5 Mpc
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| Main Authors: | , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| author | Jones, Michael G. Sand, David J. Mutlu-Pakdil, Burcin Fielder, Catherine E. Crnojevic, Denija Bennet, Paul Spekkens, Kristine Donnerstein, Richard Doliva-Dolinsky, Amandine Karunakaran, Ananthan Strader, Jay Zaritsky, Dennis |
| author_facet | Jones, Michael G. Sand, David J. Mutlu-Pakdil, Burcin Fielder, Catherine E. Crnojevic, Denija Bennet, Paul Spekkens, Kristine Donnerstein, Richard Doliva-Dolinsky, Amandine Karunakaran, Ananthan Strader, Jay Zaritsky, Dennis |
| contents | We report the discovery of Corvus A, a low-mass, gas-rich galaxy at a distance of approximately 3.5 Mpc, identified in DR10 of the Dark Energy Camera Legacy Imaging Survey during the initial phase of our ongoing SEmi-Automated Machine LEarning Search for Semi-resolved galaxies (SEAMLESS). Jansky Very Large Array observations of Corvus A detect HI line emission at a radial velocity of $523\pm2$ km/s. Magellan/Megacam imaging reveals an irregular and complex stellar population with both young and old stars. We detect UV emission in Neil Gehrels Swift observations, indicative of recent star formation. However, there are no signs of HII regions in H$α$ imaging from Steward Observatory's Kuiper telescope. Based on the Megacam color magnitude diagram we measure the distance to Corvus A via the tip-of-the-red-giant-branch standard candle as $3.48\pm0.24$ Mpc. This makes Corvus A remarkably isolated, with no known galaxy within $\sim$1 Mpc. Based on this distance, we estimate the HI and stellar mass of Corvus A to be $\log M_\mathrm{HI}/\mathrm{M_\odot} = 6.59$ and $\log M_\ast/\mathrm{M_\odot} = 6.0$. Although there are some signs of rotation, the HI distribution of Corvus A appears to be close to face-on, analogous to that of Leo T, and we therefore do not attempt to infer a dynamical mass from its HI line width. Higher resolution synthesis imaging is required to confirm this morphology and to draw robust conclusions from its gas kinematics. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2407_03393 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Corvus A: A low-mass, isolated galaxy at 3.5 Mpc Jones, Michael G. Sand, David J. Mutlu-Pakdil, Burcin Fielder, Catherine E. Crnojevic, Denija Bennet, Paul Spekkens, Kristine Donnerstein, Richard Doliva-Dolinsky, Amandine Karunakaran, Ananthan Strader, Jay Zaritsky, Dennis Astrophysics of Galaxies We report the discovery of Corvus A, a low-mass, gas-rich galaxy at a distance of approximately 3.5 Mpc, identified in DR10 of the Dark Energy Camera Legacy Imaging Survey during the initial phase of our ongoing SEmi-Automated Machine LEarning Search for Semi-resolved galaxies (SEAMLESS). Jansky Very Large Array observations of Corvus A detect HI line emission at a radial velocity of $523\pm2$ km/s. Magellan/Megacam imaging reveals an irregular and complex stellar population with both young and old stars. We detect UV emission in Neil Gehrels Swift observations, indicative of recent star formation. However, there are no signs of HII regions in H$α$ imaging from Steward Observatory's Kuiper telescope. Based on the Megacam color magnitude diagram we measure the distance to Corvus A via the tip-of-the-red-giant-branch standard candle as $3.48\pm0.24$ Mpc. This makes Corvus A remarkably isolated, with no known galaxy within $\sim$1 Mpc. Based on this distance, we estimate the HI and stellar mass of Corvus A to be $\log M_\mathrm{HI}/\mathrm{M_\odot} = 6.59$ and $\log M_\ast/\mathrm{M_\odot} = 6.0$. Although there are some signs of rotation, the HI distribution of Corvus A appears to be close to face-on, analogous to that of Leo T, and we therefore do not attempt to infer a dynamical mass from its HI line width. Higher resolution synthesis imaging is required to confirm this morphology and to draw robust conclusions from its gas kinematics. |
| title | Corvus A: A low-mass, isolated galaxy at 3.5 Mpc |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2407.03393 |