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| Main Authors: | , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| Online Access: | https://arxiv.org/abs/2409.16345 |
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| _version_ | 1866912149042888704 |
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| author | Sand, D. J. Mutlu-Pakdil, B. Jones, M. G. Karunakaran, A. Andrews, J. E. Bennet, P. Crnojevic, D. Donatiello, G. Drlica-Wagner, A. Fielder, C. Martinez-Delgado, D. Martinez-Vazquez, C. E. Spekkens, K. Doliva-Dolinsky, A. Hunter, L. C. Carlin, J. L. Cerny, W. Hai, T. N. McQuinn, K. B. W Pace, A. B. Smercina, A. |
| author_facet | Sand, D. J. Mutlu-Pakdil, B. Jones, M. G. Karunakaran, A. Andrews, J. E. Bennet, P. Crnojevic, D. Donatiello, G. Drlica-Wagner, A. Fielder, C. Martinez-Delgado, D. Martinez-Vazquez, C. E. Spekkens, K. Doliva-Dolinsky, A. Hunter, L. C. Carlin, J. L. Cerny, W. Hai, T. N. McQuinn, K. B. W Pace, A. B. Smercina, A. |
| contents | We report the discovery of three faint and ultra-faint dwarf galaxies -- Sculptor A, Sculptor B and Sculptor C -- in the direction of NGC 300 (D=2.0 Mpc), a Large Magellanic Cloud-mass galaxy. Deep ground-based imaging with Gemini/GMOS resolves all three dwarf galaxies into stars, each displaying a red giant branch indicative of an old, metal-poor stellar population. No young stars or HI gas are apparent, and the lack of a GALEX UV detection suggests that all three systems are quenched. Sculptor C (D=2.04$^{+0.10}_{-0.13}$ Mpc; $M_V$=$-$9.1$\pm$0.1 mag or $L_V$=(3.7$^{+0.4}_{-0.3}$)$\times$10$^5$ $L_{\odot}$) is consistent with being a satellite of NGC 300. Sculptor A (D=1.35$^{+0.22}_{-0.08}$ Mpc; $M_V$=$-$6.9$\pm$0.3 mag or $L_V$=(5$^{+1}_{-1}$)$\times$10$^4$ $L_{\odot}$) is likely in the foreground of NGC 300 and at the extreme edge of the Local Group, analogous to the recently discovered ultra-faint Tucana B in terms of its physical properties and environment. Sculptor B (D=2.48$^{+0.21}_{-0.24}$ Mpc; $M_V$=$-$8.1$\pm$0.3 mag or $L_V$=(1.5$^{+0.5}_{-0.4}$)$\times$10$^5$ $L_{\odot}$) is likely in the background, but future distance measurements are necessary to solidify this statement. It is also of interest due to its quiescent state and low stellar mass. Both Sculptor A and B are $\gtrsim$2-4 $r_{vir}$ from NGC 300 itself. The discovery of three dwarf galaxies in isolated or low-density environments offers an opportunity to study the varying effects of ram pressure stripping, reionization and internal feedback in influencing the star formation history of the faintest stellar systems. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2409_16345 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Three Quenched, Faint Dwarf Galaxies in the Direction of NGC 300: New Probes of Reionization and Internal Feedback Sand, D. J. Mutlu-Pakdil, B. Jones, M. G. Karunakaran, A. Andrews, J. E. Bennet, P. Crnojevic, D. Donatiello, G. Drlica-Wagner, A. Fielder, C. Martinez-Delgado, D. Martinez-Vazquez, C. E. Spekkens, K. Doliva-Dolinsky, A. Hunter, L. C. Carlin, J. L. Cerny, W. Hai, T. N. McQuinn, K. B. W Pace, A. B. Smercina, A. Astrophysics of Galaxies We report the discovery of three faint and ultra-faint dwarf galaxies -- Sculptor A, Sculptor B and Sculptor C -- in the direction of NGC 300 (D=2.0 Mpc), a Large Magellanic Cloud-mass galaxy. Deep ground-based imaging with Gemini/GMOS resolves all three dwarf galaxies into stars, each displaying a red giant branch indicative of an old, metal-poor stellar population. No young stars or HI gas are apparent, and the lack of a GALEX UV detection suggests that all three systems are quenched. Sculptor C (D=2.04$^{+0.10}_{-0.13}$ Mpc; $M_V$=$-$9.1$\pm$0.1 mag or $L_V$=(3.7$^{+0.4}_{-0.3}$)$\times$10$^5$ $L_{\odot}$) is consistent with being a satellite of NGC 300. Sculptor A (D=1.35$^{+0.22}_{-0.08}$ Mpc; $M_V$=$-$6.9$\pm$0.3 mag or $L_V$=(5$^{+1}_{-1}$)$\times$10$^4$ $L_{\odot}$) is likely in the foreground of NGC 300 and at the extreme edge of the Local Group, analogous to the recently discovered ultra-faint Tucana B in terms of its physical properties and environment. Sculptor B (D=2.48$^{+0.21}_{-0.24}$ Mpc; $M_V$=$-$8.1$\pm$0.3 mag or $L_V$=(1.5$^{+0.5}_{-0.4}$)$\times$10$^5$ $L_{\odot}$) is likely in the background, but future distance measurements are necessary to solidify this statement. It is also of interest due to its quiescent state and low stellar mass. Both Sculptor A and B are $\gtrsim$2-4 $r_{vir}$ from NGC 300 itself. The discovery of three dwarf galaxies in isolated or low-density environments offers an opportunity to study the varying effects of ram pressure stripping, reionization and internal feedback in influencing the star formation history of the faintest stellar systems. |
| title | Three Quenched, Faint Dwarf Galaxies in the Direction of NGC 300: New Probes of Reionization and Internal Feedback |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2409.16345 |