Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback
We investigate the dynamics of GN-z11, a luminous galaxy at z = 10.60, carefully analyzing the public deep integral field spectroscopy (IFS) data taken with the JWST NIRSpec integral field unit. While the observations of the IFS data originally targeted an He ii clump near GN-z11, we find that the C...
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2024-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ad82dd |
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| author | Yi Xu Masami Ouchi Hidenobu Yajima Hajime Fukushima Yuichi Harikane Yuki Isobe Kimihiko Nakajima Minami Nakane Yoshiaki Ono Hiroya Umeda Hiroto Yanagisawa Yechi Zhang |
| author_facet | Yi Xu Masami Ouchi Hidenobu Yajima Hajime Fukushima Yuichi Harikane Yuki Isobe Kimihiko Nakajima Minami Nakane Yoshiaki Ono Hiroya Umeda Hiroto Yanagisawa Yechi Zhang |
| author_sort | Yi Xu |
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| description | We investigate the dynamics of GN-z11, a luminous galaxy at z = 10.60, carefully analyzing the public deep integral field spectroscopy (IFS) data taken with the JWST NIRSpec integral field unit. While the observations of the IFS data originally targeted an He ii clump near GN-z11, we find that the C iii ] λ λ 1907, 1909 emission from ionized gas at GN-z11 is bright and spatially extended significantly beyond the point-spread function (PSF). The spatially extended C iii ] emission of GN-z11 shows a velocity gradient with red- and blueshifted components in the north and south directions, respectively, which cannot be explained by the variation of the [C iii ] λ 1907/C iii ] λ 1909 line ratios. Assuming the velocity gradient is produced by disk rotation, we perform forward modeling with GalPak ^3D , including the effects of PSF smearing and line blending, and obtain a rotation velocity of ${v}_{\mathrm{rot}}={257}_{-117}^{+138}$ km s ^−1 , a velocity dispersion of ${\sigma }_{v}={91}_{-32}^{+18}$ km s ^−1 , and a ratio of ${v}_{\mathrm{rot}}/{\sigma }_{v}={2.83}_{-1.41}^{+1.82}$ . The v _rot / σ _v value would suggest a rotation-dominated disk existing at z > 10, albeit with large uncertainties. The rotation velocity agrees with those of numerical simulations predicting a rotating disk formed in the early Universe under the conditions of mass compaction and weak feedback. While the velocity gradient is consistent with the rotating-disk solution, we recognize that galactic outflows can also explain the velocity gradient, as well as the extended morphology and the high velocity dispersion found in the outskirts. Higher-signal-to-noise-ratio and higher-resolution data are necessary to conclude the physical origin of the velocity gradient in GN-z11. |
| format | Article |
| id | doaj-art-16f824e7918543f7b9c0c26cb65a7091 |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-16f824e7918543f7b9c0c26cb65a70912024-11-19T06:16:26ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01976114210.3847/1538-4357/ad82ddDynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak FeedbackYi Xu0https://orcid.org/0000-0002-5768-8235Masami Ouchi1https://orcid.org/0000-0002-1049-6658Hidenobu Yajima2https://orcid.org/0000-0002-1319-3433Hajime Fukushima3https://orcid.org/0000-0002-0547-3208Yuichi Harikane4https://orcid.org/0000-0002-6047-430XYuki Isobe5https://orcid.org/0000-0001-7730-8634Kimihiko Nakajima6https://orcid.org/0000-0003-2965-5070Minami Nakane7https://orcid.org/0009-0000-1999-5472Yoshiaki Ono8https://orcid.org/0000-0001-9011-7605Hiroya Umeda9https://orcid.org/0009-0008-0167-5129Hiroto Yanagisawa10https://orcid.org/0009-0006-6763-4245Yechi Zhang11https://orcid.org/0000-0003-3817-8739Institute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; xuyi@icrr.u-tokyo.ac.jp; Department of Astronomy, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; xuyi@icrr.u-tokyo.ac.jp; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Graduate University for Advanced Studies (SOKENDAI) , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba, 277-8583, JapanCenter for Computational Sciences, University of Tsukuba , Tennodai, 1-1-1 Tsukuba, Ibaraki 305-8577, JapanCenter for Computational Sciences, University of Tsukuba , Tennodai, 1-1-1 Tsukuba, Ibaraki 305-8577, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; xuyi@icrr.u-tokyo.ac.jpWaseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1, Okubo, Shinjuku, Tokyo 169-8555, JapanNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; xuyi@icrr.u-tokyo.ac.jp; Department of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; xuyi@icrr.u-tokyo.ac.jpInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; xuyi@icrr.u-tokyo.ac.jp; Department of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; xuyi@icrr.u-tokyo.ac.jp; Department of Physics, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanInstitute for Cosmic Ray Research, The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan ; xuyi@icrr.u-tokyo.ac.jp; Department of Astronomy, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan; National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo , 5-1-5 Kashiwanoha, Kashiwa, Chiba, 277-8583, JapanWe investigate the dynamics of GN-z11, a luminous galaxy at z = 10.60, carefully analyzing the public deep integral field spectroscopy (IFS) data taken with the JWST NIRSpec integral field unit. While the observations of the IFS data originally targeted an He ii clump near GN-z11, we find that the C iii ] λ λ 1907, 1909 emission from ionized gas at GN-z11 is bright and spatially extended significantly beyond the point-spread function (PSF). The spatially extended C iii ] emission of GN-z11 shows a velocity gradient with red- and blueshifted components in the north and south directions, respectively, which cannot be explained by the variation of the [C iii ] λ 1907/C iii ] λ 1909 line ratios. Assuming the velocity gradient is produced by disk rotation, we perform forward modeling with GalPak ^3D , including the effects of PSF smearing and line blending, and obtain a rotation velocity of ${v}_{\mathrm{rot}}={257}_{-117}^{+138}$ km s ^−1 , a velocity dispersion of ${\sigma }_{v}={91}_{-32}^{+18}$ km s ^−1 , and a ratio of ${v}_{\mathrm{rot}}/{\sigma }_{v}={2.83}_{-1.41}^{+1.82}$ . The v _rot / σ _v value would suggest a rotation-dominated disk existing at z > 10, albeit with large uncertainties. The rotation velocity agrees with those of numerical simulations predicting a rotating disk formed in the early Universe under the conditions of mass compaction and weak feedback. While the velocity gradient is consistent with the rotating-disk solution, we recognize that galactic outflows can also explain the velocity gradient, as well as the extended morphology and the high velocity dispersion found in the outskirts. Higher-signal-to-noise-ratio and higher-resolution data are necessary to conclude the physical origin of the velocity gradient in GN-z11.https://doi.org/10.3847/1538-4357/ad82ddGalaxy formationGalaxy evolutionGalaxy disksGalaxy rotationGalaxy kinematicsEarly universe |
| spellingShingle | Yi Xu Masami Ouchi Hidenobu Yajima Hajime Fukushima Yuichi Harikane Yuki Isobe Kimihiko Nakajima Minami Nakane Yoshiaki Ono Hiroya Umeda Hiroto Yanagisawa Yechi Zhang Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback The Astrophysical Journal Galaxy formation Galaxy evolution Galaxy disks Galaxy rotation Galaxy kinematics Early universe |
| title | Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback |
| title_full | Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback |
| title_fullStr | Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback |
| title_full_unstemmed | Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback |
| title_short | Dynamics of a Galaxy at z > 10 Explored by JWST Integral Field Spectroscopy: Hints of Rotating Disk Suggesting Weak Feedback |
| title_sort | dynamics of a galaxy at z 10 explored by jwst integral field spectroscopy hints of rotating disk suggesting weak feedback |
| topic | Galaxy formation Galaxy evolution Galaxy disks Galaxy rotation Galaxy kinematics Early universe |
| url | https://doi.org/10.3847/1538-4357/ad82dd |
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