From Grism to IFU: Revising the Redshift and Nature of the Massive Dusty Galaxy S1 with JWST and ALMA
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2026
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| author | Xiao, Mengyuan Bing, Longji Brammer, Gabriel Oesch, Pascal A. Elbaz, David Marques-Chaves, Rui Dessauges-Zavadsky, Miroslava Magnelli, Benjamin Bouwens, Rychard Daddi, Emanuele Franco, Maximilien Gu, Qiusheng Herard-Demanche, Thomas Illingworth, Garth Labbe, Ivo Marchesini, Danilo Matthee, Jorryt Meyer, Romain A. Naidu, Rohan P. Shivaei, Irene van Dokkum, Pieter Weibel, Andrea Williams, Christina C. Wuyts, Stijn |
| author_facet | Xiao, Mengyuan Bing, Longji Brammer, Gabriel Oesch, Pascal A. Elbaz, David Marques-Chaves, Rui Dessauges-Zavadsky, Miroslava Magnelli, Benjamin Bouwens, Rychard Daddi, Emanuele Franco, Maximilien Gu, Qiusheng Herard-Demanche, Thomas Illingworth, Garth Labbe, Ivo Marchesini, Danilo Matthee, Jorryt Meyer, Romain A. Naidu, Rohan P. Shivaei, Irene van Dokkum, Pieter Weibel, Andrea Williams, Christina C. Wuyts, Stijn |
| contents | We report a revised spectroscopic redshift for the dusty massive galaxy S1, previously inferred with an exceptionally high baryon-to-star conversion efficiency from NIRCam slitless grism data at $z_{\rm grism}=5.58$. Our new JWST/NIRSpec IFU observations reveal multiple rest-frame optical and NIR emission lines, yielding a secure spectroscopic redshift of $z_{\rm spec}=3.2439\pm0.0002$. We show that the earlier grism-based redshift resulted from contamination by a nearby galaxy whose dispersed spectral trace overlaps with S1, illustrating a known challenge of slitless spectroscopy when only a single dispersion angle and single emission feature are available. In addition, we present new ALMA 1 mm observations, which robustly detect dust emission ($S_{\rm 1mm}=0.99\pm0.03$ mJy) and show a dust half-light radius ($R_{\rm e,1mm}=0.73\pm0.10$ kpc) slightly smaller than the stellar size ($R_{\rm e, F444W} = 0.97\pm0.01$ kpc). Using the revised redshift and compiled multi-wavelength photometry, we update the UV-to-FIR SED and find that S1 is less extreme than previously inferred, yet remains a very massive (log$M_{\star}/M_{\odot}\sim10.6$), heavily obscured star-forming galaxy. The updated SED modeling reveals S1 to be a very dust- and gas-rich system with a moderate star formation rate and a long gas depletion time ($τ_{\rm dep} \sim 1.4$ Gyr), deviating from SMGs and OFGs, but more closely resembling typical massive main-sequence galaxies. We note that, although this revision reduces the number of ultra-massive galaxies reported in Xiao et al. 2024, it does not alter the main conclusions of that work. Overall, our study clarifies the nature of S1 and underscores the importance of multi-line spectroscopic confirmation, slitless observations at multiple position angles, and IFU data for robust redshift and physical characterization of rare massive galaxies in the early Universe. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2602_03030 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | From Grism to IFU: Revising the Redshift and Nature of the Massive Dusty Galaxy S1 with JWST and ALMA Xiao, Mengyuan Bing, Longji Brammer, Gabriel Oesch, Pascal A. Elbaz, David Marques-Chaves, Rui Dessauges-Zavadsky, Miroslava Magnelli, Benjamin Bouwens, Rychard Daddi, Emanuele Franco, Maximilien Gu, Qiusheng Herard-Demanche, Thomas Illingworth, Garth Labbe, Ivo Marchesini, Danilo Matthee, Jorryt Meyer, Romain A. Naidu, Rohan P. Shivaei, Irene van Dokkum, Pieter Weibel, Andrea Williams, Christina C. Wuyts, Stijn Astrophysics of Galaxies We report a revised spectroscopic redshift for the dusty massive galaxy S1, previously inferred with an exceptionally high baryon-to-star conversion efficiency from NIRCam slitless grism data at $z_{\rm grism}=5.58$. Our new JWST/NIRSpec IFU observations reveal multiple rest-frame optical and NIR emission lines, yielding a secure spectroscopic redshift of $z_{\rm spec}=3.2439\pm0.0002$. We show that the earlier grism-based redshift resulted from contamination by a nearby galaxy whose dispersed spectral trace overlaps with S1, illustrating a known challenge of slitless spectroscopy when only a single dispersion angle and single emission feature are available. In addition, we present new ALMA 1 mm observations, which robustly detect dust emission ($S_{\rm 1mm}=0.99\pm0.03$ mJy) and show a dust half-light radius ($R_{\rm e,1mm}=0.73\pm0.10$ kpc) slightly smaller than the stellar size ($R_{\rm e, F444W} = 0.97\pm0.01$ kpc). Using the revised redshift and compiled multi-wavelength photometry, we update the UV-to-FIR SED and find that S1 is less extreme than previously inferred, yet remains a very massive (log$M_{\star}/M_{\odot}\sim10.6$), heavily obscured star-forming galaxy. The updated SED modeling reveals S1 to be a very dust- and gas-rich system with a moderate star formation rate and a long gas depletion time ($τ_{\rm dep} \sim 1.4$ Gyr), deviating from SMGs and OFGs, but more closely resembling typical massive main-sequence galaxies. We note that, although this revision reduces the number of ultra-massive galaxies reported in Xiao et al. 2024, it does not alter the main conclusions of that work. Overall, our study clarifies the nature of S1 and underscores the importance of multi-line spectroscopic confirmation, slitless observations at multiple position angles, and IFU data for robust redshift and physical characterization of rare massive galaxies in the early Universe. |
| title | From Grism to IFU: Revising the Redshift and Nature of the Massive Dusty Galaxy S1 with JWST and ALMA |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2602.03030 |