The GECKOS Survey: Resolved, multiphase observations of mass-loading and gas density in the galactic wind of NGC 4666
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| Format: | Preprint |
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2025
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| author | Ciraulo, Barbara Mazzilli Fisher, D. B. Elliott, R. Fraser-McKelvie, A. Hayden, M. R. Martig, M. van de Sande, J. Battisti, A. J. Bland-Hawthorn, J. Bolatto, A. D. Brown, T. H. Catinella, B. Combes, F. Cortese, L. Davis, T. A. Emsellem, E. Gadotti, D. A. Lagos, C. del P. Lin, X. Marasco, A. Peng, E. Pinna, F. Puzia, T. H. Silva-Lima, L. A. Valenzuela, L. M. van de Ven, G. Wang, J. |
| author_facet | Ciraulo, Barbara Mazzilli Fisher, D. B. Elliott, R. Fraser-McKelvie, A. Hayden, M. R. Martig, M. van de Sande, J. Battisti, A. J. Bland-Hawthorn, J. Bolatto, A. D. Brown, T. H. Catinella, B. Combes, F. Cortese, L. Davis, T. A. Emsellem, E. Gadotti, D. A. Lagos, C. del P. Lin, X. Marasco, A. Peng, E. Pinna, F. Puzia, T. H. Silva-Lima, L. A. Valenzuela, L. M. van de Ven, G. Wang, J. |
| contents | We present a multiphase, resolved study of the galactic wind extending from the nearby starburst galaxy NGC 4666. For this we use VLT/MUSE observations from the GECKOS program and HI data from the WALLABY survey. We identify both ionised and HI gas in a biconical structure extending to at least $z\sim$8 kpc from the galaxy disk, with increasing velocity offsets above the midplane in both phases, consistent with a multiphase wind. The measured electron density, using [SII], differs significantly from standard expectations of galactic winds. We find electron density declines from the galaxy centre to $\sim2$ kpc, then rises again, remaining high ($\sim100-300$ cm$^{-3}$) out to $\sim$5 kpc. We find that HI dominates the mass loading. The total HI mass outflow rate (above $z~>2$ kpc) is between $5-13~M_{\odot}~\rm yr^{-1}$, accounting for uncertainties from disk-blurring and group interactions. The total ionised mass outflow rate (traced by H$α$) is between $0.5~M_{\odot}~\rm yr^{-1}$ and $5~M_{\odot}~\rm yr^{-1}$, depending on $n_e(z)$ assumptions. From ALMA/ACA observations, we place an upper-limit on CO flux in the outflow which correlates to $\lesssim2.9~M_{\odot}~\rm yr^{-1}$. We also show that the entire outflow is not limited to the bicone, but a secondary starburst at the edge generates a more widespread outflow, which should be included in simulations. The cool gas in NGC 4666 wind has insufficient velocity to escape the halo of a galaxy of its mass, especially because most of the mass is present in the slower atomic phase. This strong biconical wind contributes to gas cycling around the galaxy. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2509_17560 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The GECKOS Survey: Resolved, multiphase observations of mass-loading and gas density in the galactic wind of NGC 4666 Ciraulo, Barbara Mazzilli Fisher, D. B. Elliott, R. Fraser-McKelvie, A. Hayden, M. R. Martig, M. van de Sande, J. Battisti, A. J. Bland-Hawthorn, J. Bolatto, A. D. Brown, T. H. Catinella, B. Combes, F. Cortese, L. Davis, T. A. Emsellem, E. Gadotti, D. A. Lagos, C. del P. Lin, X. Marasco, A. Peng, E. Pinna, F. Puzia, T. H. Silva-Lima, L. A. Valenzuela, L. M. van de Ven, G. Wang, J. Astrophysics of Galaxies We present a multiphase, resolved study of the galactic wind extending from the nearby starburst galaxy NGC 4666. For this we use VLT/MUSE observations from the GECKOS program and HI data from the WALLABY survey. We identify both ionised and HI gas in a biconical structure extending to at least $z\sim$8 kpc from the galaxy disk, with increasing velocity offsets above the midplane in both phases, consistent with a multiphase wind. The measured electron density, using [SII], differs significantly from standard expectations of galactic winds. We find electron density declines from the galaxy centre to $\sim2$ kpc, then rises again, remaining high ($\sim100-300$ cm$^{-3}$) out to $\sim$5 kpc. We find that HI dominates the mass loading. The total HI mass outflow rate (above $z~>2$ kpc) is between $5-13~M_{\odot}~\rm yr^{-1}$, accounting for uncertainties from disk-blurring and group interactions. The total ionised mass outflow rate (traced by H$α$) is between $0.5~M_{\odot}~\rm yr^{-1}$ and $5~M_{\odot}~\rm yr^{-1}$, depending on $n_e(z)$ assumptions. From ALMA/ACA observations, we place an upper-limit on CO flux in the outflow which correlates to $\lesssim2.9~M_{\odot}~\rm yr^{-1}$. We also show that the entire outflow is not limited to the bicone, but a secondary starburst at the edge generates a more widespread outflow, which should be included in simulations. The cool gas in NGC 4666 wind has insufficient velocity to escape the halo of a galaxy of its mass, especially because most of the mass is present in the slower atomic phase. This strong biconical wind contributes to gas cycling around the galaxy. |
| title | The GECKOS Survey: Resolved, multiphase observations of mass-loading and gas density in the galactic wind of NGC 4666 |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2509.17560 |