Possible Systematic Rotation in the Mature Stellar Population of a z = 9.1 Galaxy
Inoue, Akio K.; Hashimoto, Takuya; Sugahara, Yuma; Tamura, Yoichi; Ellis, Richard S.; Zheng, Wei; Fudamoto, Yoshinobu; Zackrisson, Erik; Matsuo, Hiroshi; Roberts-Borsani, Guido; Laporte, Nicolas; Shimizu, Ikkoh; Yoshida, Naoki; Yamanaka, Satoshi; Tokuoka, Tsuyoshi; Moriwaki, Kana
Japan, United Kingdom, United States, Sweden
Abstract
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 μm emission is detected at 10σ with a spatial resolution of ~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 ΔV obs/2σ tot = 0.84 ± 0.23, where ΔV obs is the observed maximum velocity difference and σ 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 ${V}_{\mathrm{rot}}/{\sigma }_{V}={0.67}_{-0.26}^{+0.73}$ , where V rot and σ V are the rotation velocity and velocity dispersion, respectively, still consistent with rotation. The resulting disk mass of ${0.65}_{-0.40}^{+1.37}\times {10}^{9}$ M ⊙ 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 ~ 15.