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Possible Systematic Rotation in the Mature Stellar Population of a z=9.1 Galaxy

Tokuoka, Tsuyoshi (författare)
Waseda Univ, Fac Sci & Engn, Grad Sch Adv Sci & Engn, Dept Pure & Appl Phys, 3-4-1 Okubo, Tokyo 1698555, Japan.
Inoue, Akio K. (författare)
Waseda Univ, Fac Sci & Engn, Grad Sch Adv Sci & Engn, Dept Pure & Appl Phys, 3-4-1 Okubo, Tokyo 1698555, Japan.;Waseda Univ, Fac Sci & Engn, Waseda Res Inst Sci & Engn, 3-4-1 Okubo, Tokyo 1698555, Japan.
Hashimoto, Takuya (författare)
Univ Tsukuba, Fac Pure & Appl Sci, Tomonaga Ctr Hist Universe TCHoU, Tsukuba, Ibaraki 3058571, Japan.
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Ellis, Richard S. (författare)
UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
Laporte, Nicolas (författare)
Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England.;Univ Cambridge, Cavendish Lab, 19 JJ Thomson Ave, Cambridge CB3 0HE, England.
Sugahara, Yuma (författare)
Waseda Univ, Fac Sci & Engn, Waseda Res Inst Sci & Engn, 3-4-1 Okubo, Tokyo 1698555, Japan.;Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
Matsuo, Hiroshi (författare)
Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
Tamura, Yoichi (författare)
Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan.
Fudamoto, Yoshinobu (författare)
Waseda Univ, Fac Sci & Engn, Waseda Res Inst Sci & Engn, 3-4-1 Okubo, Tokyo 1698555, Japan.;Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
Moriwaki, Kana (författare)
Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
Roberts-Borsani, Guido (författare)
Univ Calif Los Angeles, Dept Phys & Astron, 430 Portola Plaza, Los Angeles, CA 90095 USA.
Shimizu, Ikkoh (författare)
Shikoku Gakuin Univ, Dept Literature, 3-2-1 Bunkyocho, Zentsuji, Kagawa 7658505, Japan.
Yamanaka, Satoshi (författare)
Toba Coll, Natl Inst Technol, Gen Educ Dept, 1-1 Ikegami Cho, Toba, Mie 5178501, Japan.
Yoshida, Naoki (författare)
Univ Tokyo, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.;Univ Tokyo, UT Inst Adv Study, Kavli Inst Phys & Math Universe WPI, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan.;Univ Tokyo, Sch Sci, Res Ctr Early Universe, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.;Univ Tokyo, Sch Sci, Inst Phys Intelligence, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
Zackrisson, Erik (författare)
Uppsala universitet,Observationell astrofysik
Zheng, Wei (författare)
Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
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Waseda Univ, Fac Sci & Engn, Grad Sch Adv Sci & Engn, Dept Pure & Appl Phys, 3-4-1 Okubo, Tokyo 1698555, Japan Waseda Univ, Fac Sci & Engn, Grad Sch Adv Sci & Engn, Dept Pure & Appl Phys, 3-4-1 Okubo, Tokyo 1698555, Japan.;Waseda Univ, Fac Sci & Engn, Waseda Res Inst Sci & Engn, 3-4-1 Okubo, Tokyo 1698555, Japan. (creator_code:org_t)
2022-07-01
2022
Engelska.
Ingår i: Astrophysical Journal Letters. - : Institute of Physics Publishing (IOPP). - 2041-8205 .- 2041-8213. ; 933:1
Relaterad länk:
https://doi.org/10.3...
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https://uu.diva-port... (primary) (Raw object)
https://urn.kb.se/re...
https://doi.org/10.3...
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  • Tidskriftsartikel (refereegranskat)
Abstract Ämnesord
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  • We present new observations with the Atacama Large Millimeter/submillimeter Array for a gravitationally lensed galaxy at z = 9.1, MACS1149-JD1. [O III] 88 mu m emission is detected at 10 sigma with a spatial resolution of similar to 0.3 kpc in the source plane, enabling the most distant morphokinematic study of a galaxy. The [O iii] emission is distributed smoothly without any resolved clumps and shows a clear velocity gradient with Delta V-obs/2 sigma(tot) = 0.84 +/- 0.23, where Delta V-obs is the observed maximum velocity difference and sigma(tot) is the velocity dispersion measured in the spatially integrated line profile, suggesting a rotating system. Assuming a geometrically thin self-gravitating rotation disk model, we obtain V-rot/sigma(V)=0.67-0.26+0.73, where V-rot and sigma (V) are the rotation velocity and velocity dispersion, respectively, still consistent with rotation. The resulting disk mass of 0.65-0.40+1.37x10(9) M-circle dot is consistent with being associated with the stellar mass identified with a 300 Myr old stellar population independently indicated by a Balmer break in the spectral energy distribution. We conclude that the most of the dynamical mass is associated with the previously identified mature stellar population that formed at z similar to 15.

Ämnesord

NATURVETENSKAP  -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
NATURAL SCIENCES  -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)

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