A large-scale ring galaxy at z = 2.2 revealed by JWST/NIRCam: kinematic observations and analytical modelling
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2025
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| author | Shachar, A. Nestor Sternberg, A. Genzel, R. Liu, D. Price, S. H. Pulsoni, C. Tacconi, L. J. Herrera-Camus, R. Schreiber, N. M. Forster Burkert, A. Jolly, J. B. Lutz, D. Wuyts, S. Barfety, C. Cao, Y. Chen, J. Davies, R. Eisenhauer, F. Salcedo, J. M. Espejo Lee, L. L. Lee, M. Naab, T. Pastras, S. Shimizu, T. T. Sturm, E. Tozzi, G. Ubler, H. |
| author_facet | Shachar, A. Nestor Sternberg, A. Genzel, R. Liu, D. Price, S. H. Pulsoni, C. Tacconi, L. J. Herrera-Camus, R. Schreiber, N. M. Forster Burkert, A. Jolly, J. B. Lutz, D. Wuyts, S. Barfety, C. Cao, Y. Chen, J. Davies, R. Eisenhauer, F. Salcedo, J. M. Espejo Lee, L. L. Lee, M. Naab, T. Pastras, S. Shimizu, T. T. Sturm, E. Tozzi, G. Ubler, H. |
| contents | A unique galaxy at z = 2.2, zC406690, has a striking clumpy large-scale ring structure that persists from rest UV to near-infrared, yet has an ordered rotation and lies on the star-formation main sequence. We combine new JWST/NIRCam and ALMA band 4 observations, together with previous VLT/SINFONI integral field spectroscopy and HST imaging to re-examine its nature. The high-resolution H$α$ kinematics are best fitted if the mass is distributed within a ring with total mass $M_{\rm{ring}} = 2 \times 10^{10} M_\odot$ and radius $R_{ring}$ = 4.6 kpc, together with a central undetected mass component (e.g., a "bulge") with a dynamical mass of $M_{bulge} = 8 \times 10^{10} M_\odot$. We also consider a purely flux emitting ring superposed over a faint exponential disk, or a highly "cuspy" dark matter halo, both disfavored against a massive ring model. The low-resolution CO(4-3) line and 142GHz continuum emission imply a total molecular and dust gas masses of $M_{mol,gas} = 7.1 \times 10^{10}M_\odot$ and $M_{dust} = 3 \times 10^8 M_\odot$ over the entire galaxy, giving a dust-to-mass ratio of 0.7%. We estimate that roughly half the gas and dust mass lie inside the ring, and that $\sim 10\%$ of the total dust is in a foreground screen that attenuates the stellar light of the bulge in the rest-UV to near-infrared. Sensitive high-resolution ALMA observations will be essential to confirm this scenario and study the gas and dust distribution. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_00839 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A large-scale ring galaxy at z = 2.2 revealed by JWST/NIRCam: kinematic observations and analytical modelling Shachar, A. Nestor Sternberg, A. Genzel, R. Liu, D. Price, S. H. Pulsoni, C. Tacconi, L. J. Herrera-Camus, R. Schreiber, N. M. Forster Burkert, A. Jolly, J. B. Lutz, D. Wuyts, S. Barfety, C. Cao, Y. Chen, J. Davies, R. Eisenhauer, F. Salcedo, J. M. Espejo Lee, L. L. Lee, M. Naab, T. Pastras, S. Shimizu, T. T. Sturm, E. Tozzi, G. Ubler, H. Astrophysics of Galaxies A unique galaxy at z = 2.2, zC406690, has a striking clumpy large-scale ring structure that persists from rest UV to near-infrared, yet has an ordered rotation and lies on the star-formation main sequence. We combine new JWST/NIRCam and ALMA band 4 observations, together with previous VLT/SINFONI integral field spectroscopy and HST imaging to re-examine its nature. The high-resolution H$α$ kinematics are best fitted if the mass is distributed within a ring with total mass $M_{\rm{ring}} = 2 \times 10^{10} M_\odot$ and radius $R_{ring}$ = 4.6 kpc, together with a central undetected mass component (e.g., a "bulge") with a dynamical mass of $M_{bulge} = 8 \times 10^{10} M_\odot$. We also consider a purely flux emitting ring superposed over a faint exponential disk, or a highly "cuspy" dark matter halo, both disfavored against a massive ring model. The low-resolution CO(4-3) line and 142GHz continuum emission imply a total molecular and dust gas masses of $M_{mol,gas} = 7.1 \times 10^{10}M_\odot$ and $M_{dust} = 3 \times 10^8 M_\odot$ over the entire galaxy, giving a dust-to-mass ratio of 0.7%. We estimate that roughly half the gas and dust mass lie inside the ring, and that $\sim 10\%$ of the total dust is in a foreground screen that attenuates the stellar light of the bulge in the rest-UV to near-infrared. Sensitive high-resolution ALMA observations will be essential to confirm this scenario and study the gas and dust distribution. |
| title | A large-scale ring galaxy at z = 2.2 revealed by JWST/NIRCam: kinematic observations and analytical modelling |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2503.00839 |