Ionized gas in NGC 4258: Exploring the AGN -- Star formation connection
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| Autores principales: | , , , , , , , , , , , |
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| Formato: | Preprint |
| Publicado: |
2025
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| author | Fernández-Arenas, D. Rousseau-Nepton, L. Robert, C. Drissen, L. Martin, R. P. Amram, P. Epinat, B. Puertas, Duarte Garner III, R. Savard, G. Vicens-Mouret, S. Massé, É. |
| author_facet | Fernández-Arenas, D. Rousseau-Nepton, L. Robert, C. Drissen, L. Martin, R. P. Amram, P. Epinat, B. Puertas, Duarte Garner III, R. Savard, G. Vicens-Mouret, S. Massé, É. |
| contents | NGC 4258 is a prime target for studying feedback in Low-Luminosity Active Galactic Nuclei (LLAGNs) due to its proximity and comprehensive multi-wavelength coverage. Using new Integral Field Spectroscopy (IFS) data from SITELLE at the Canada-France-Hawaii Telescope, we analysed the galaxy's nebular emission lines. Our study focused on spatially resolved line ratios and Baldwin-Phillips-Terlevich diagrams, revealing that the ''anomalous spiral arms'' exhibit intense interactions between the jet and interstellar medium (ISM) extending up to 6 kpc with velocity dispersions peak at 200-250 km/s in these regions, contrasting with star-forming areas showing lower values around of 30-50 km/s. Analysis of covering fractions indicates heightened AGN ionization cones aligned with the radio jet, alongside evidence of shock quenching observed in the lower "anomalous arc". Conversely, jet-induced compression may stimulate star formation in other areas. We derived a galaxy-wide star formation rate of $\sim3 M_{\odot}\mathrm{yr}^{-1}$ decreasing to $0.3 M_{\odot}\mathrm{yr}^{-1}$ within the central $3.4 \mathrm{kpc}^2$. SITELLE's broad field coverage elucidates the galaxy's structural details, confirming that low-power jets significantly influence the host galaxy across parsec and kpc scales. The velocity dispersion map reveals asymmetric or double-peaked emission lines, tracing jet-disk interactions likely responsible for the formation of anomalous arm features. Small-scale ionizing clusters were detected in regions with disrupted gas flows, possibly formed through tidal interactions or shock compression. NGC~4258 thus presents a compelling case for studying LLAGN-driven feedback, illustrating how optical IFS combined with multi-wavelength data clarifies the impact of outflows and shocks on nearby spiral galaxies, providing insights into how these processes shape star formation and ISM conditions. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_16153 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Ionized gas in NGC 4258: Exploring the AGN -- Star formation connection Fernández-Arenas, D. Rousseau-Nepton, L. Robert, C. Drissen, L. Martin, R. P. Amram, P. Epinat, B. Puertas, Duarte Garner III, R. Savard, G. Vicens-Mouret, S. Massé, É. Astrophysics of Galaxies NGC 4258 is a prime target for studying feedback in Low-Luminosity Active Galactic Nuclei (LLAGNs) due to its proximity and comprehensive multi-wavelength coverage. Using new Integral Field Spectroscopy (IFS) data from SITELLE at the Canada-France-Hawaii Telescope, we analysed the galaxy's nebular emission lines. Our study focused on spatially resolved line ratios and Baldwin-Phillips-Terlevich diagrams, revealing that the ''anomalous spiral arms'' exhibit intense interactions between the jet and interstellar medium (ISM) extending up to 6 kpc with velocity dispersions peak at 200-250 km/s in these regions, contrasting with star-forming areas showing lower values around of 30-50 km/s. Analysis of covering fractions indicates heightened AGN ionization cones aligned with the radio jet, alongside evidence of shock quenching observed in the lower "anomalous arc". Conversely, jet-induced compression may stimulate star formation in other areas. We derived a galaxy-wide star formation rate of $\sim3 M_{\odot}\mathrm{yr}^{-1}$ decreasing to $0.3 M_{\odot}\mathrm{yr}^{-1}$ within the central $3.4 \mathrm{kpc}^2$. SITELLE's broad field coverage elucidates the galaxy's structural details, confirming that low-power jets significantly influence the host galaxy across parsec and kpc scales. The velocity dispersion map reveals asymmetric or double-peaked emission lines, tracing jet-disk interactions likely responsible for the formation of anomalous arm features. Small-scale ionizing clusters were detected in regions with disrupted gas flows, possibly formed through tidal interactions or shock compression. NGC~4258 thus presents a compelling case for studying LLAGN-driven feedback, illustrating how optical IFS combined with multi-wavelength data clarifies the impact of outflows and shocks on nearby spiral galaxies, providing insights into how these processes shape star formation and ISM conditions. |
| title | Ionized gas in NGC 4258: Exploring the AGN -- Star formation connection |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2507.16153 |