A closer look at dwarf galaxies exhibiting MIR variability: AGN confirmation and comparison with non-variable dwarf galaxies
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arXiv
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| Format: | Preprint |
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2024
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| author | Aravindan, Archana Canalizo, Gabriela Secrest, Nathan Satyapal, Shobita Bohn, Thomas |
| author_facet | Aravindan, Archana Canalizo, Gabriela Secrest, Nathan Satyapal, Shobita Bohn, Thomas |
| contents | Detecting active black holes in dwarf galaxies has proven to be a challenge due to their small size and weak electromagnetic signatures. Mid-infrared variability has emerged as a promising tool that can be used to detect active low-mass black holes in dwarf galaxies. We analyzed 10.4 years of photometry from the ALL$WISE$/NEO$WISE$ multi-epoch catalogs, identifying 25 objects with AGN-like variability. Independent confirmation of AGN activity was found in 68% of these objects using optical and near-infrared diagnostics. Notably, we discovered a near-infrared coronal line [S IX] $λ$ 1.252 $μ$m in J1205, the galaxy with the lowest stellar mass (log M$_{*}$ = 7.5 M$_{\odot}$) and low metallicity (12 + log(O/H) = 7.46) in our sample. Additionally, we found broad Pa$α$ potentially from the BLR in two targets, and their implied black hole masses are consistent with black hole-stellar mass relations. Comparing non-variable galaxies with similar stellar masses and $WISE$ $W1-W2$ colors, we found no clear trends between variability and large-scale galaxy properties. However, we found that AGN activity likely causes redder $W1-W2$ colors in variable targets, while for the non-variable galaxies, the contribution stems from strong star formation activity. A high incidence of optical broad lines was also observed in variable targets. Our results suggest that mid-infrared variability is an effective method for detecting AGN activity in low-mass galaxies and can help uncover a larger sample of active low-mass ($<$ 10$^{6}$ M$_{\odot}$) black holes in the universe. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_00666 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | A closer look at dwarf galaxies exhibiting MIR variability: AGN confirmation and comparison with non-variable dwarf galaxies Aravindan, Archana Canalizo, Gabriela Secrest, Nathan Satyapal, Shobita Bohn, Thomas Astrophysics of Galaxies Detecting active black holes in dwarf galaxies has proven to be a challenge due to their small size and weak electromagnetic signatures. Mid-infrared variability has emerged as a promising tool that can be used to detect active low-mass black holes in dwarf galaxies. We analyzed 10.4 years of photometry from the ALL$WISE$/NEO$WISE$ multi-epoch catalogs, identifying 25 objects with AGN-like variability. Independent confirmation of AGN activity was found in 68% of these objects using optical and near-infrared diagnostics. Notably, we discovered a near-infrared coronal line [S IX] $λ$ 1.252 $μ$m in J1205, the galaxy with the lowest stellar mass (log M$_{*}$ = 7.5 M$_{\odot}$) and low metallicity (12 + log(O/H) = 7.46) in our sample. Additionally, we found broad Pa$α$ potentially from the BLR in two targets, and their implied black hole masses are consistent with black hole-stellar mass relations. Comparing non-variable galaxies with similar stellar masses and $WISE$ $W1-W2$ colors, we found no clear trends between variability and large-scale galaxy properties. However, we found that AGN activity likely causes redder $W1-W2$ colors in variable targets, while for the non-variable galaxies, the contribution stems from strong star formation activity. A high incidence of optical broad lines was also observed in variable targets. Our results suggest that mid-infrared variability is an effective method for detecting AGN activity in low-mass galaxies and can help uncover a larger sample of active low-mass ($<$ 10$^{6}$ M$_{\odot}$) black holes in the universe. |
| title | A closer look at dwarf galaxies exhibiting MIR variability: AGN confirmation and comparison with non-variable dwarf galaxies |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2408.00666 |