We present the rest-frame optical and UV surface brightness (SB) profiles for 149 galaxies with Mopt < −19.4 mag at z = 4–10 (29 of which are spectroscopically confirmed with JWST NIRSpec), securing high signal-to-noise ratios of 10–135 with deep JWST NIRCam 1–$5\, \mu$m images obtained by the CEERS survey. We derive morphologies of our high-z galaxies, carefully evaluating the systematics of SB profile measurements with Monte Carlo simulations as well as the impacts of a) AGNs, b) multiple clumps including galaxy mergers, c) spatial resolution differences with previous HST studies, and d) strong emission lines, e.g., Hα and [O iii], on optical morphologies with medium-band F410M images. Conducting Sérsic profile fitting for our high-z galaxy SBs with GALFIT, we obtain effective radius ranges for optical re,opt and UV re,UV wavelengths of re, opt = 0.05–1.6 kpc and re,UV = 0.03–1.7 kpc that are consistent with previous results within large scatters in the size–luminosity relations. However, we find that the effective radius ratio, re,opt$/$re,UV, is almost unity, $1.01^{+0.35}_{-0.22}$, over z = 4–10 with no signatures of past inside-out star formation such as found at z ∼ 0–2. There are no spatial offsets exceeding 3σ between the optical and UV morphology centers in cases of no mergers, indicative of major star-forming activity only being found near mass centers of galaxies at z ≳ 4 probably experiencing the first phase of inside-out galaxy formation.

中文翻译：

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z = 4–10 处星系的静止框架光学和紫外形态普查：由内而外星系形成的第一阶段

我们展示了 149 个星系的静止框架光学和 UV 表面亮度 (SB) 剖面，其中 Mopt < z = 4–10 时为 −19.4 mag（其中 29 个通过 JWST NIRSpec 进行光谱证实），通过深部 JWST NIRCam 1–$5\, \mu$m 获得的图像确保 10–135 的高信噪比CEERS 调查。我们推导出高 z 星系的形态，通过蒙特卡罗模拟仔细评估 SB 剖面测量的系统性，以及 a) AGN、b) 包括星系合并在内的多个团块、c) 与之前 HST 研究的空间分辨率差异的影响， d) 中波段 F410M 图像光学形态上的强发射线，例如 Hα 和 [O iii]。使用 GALFIT 对我们的高 z 星系 SB 进行 Sérsic 剖面拟合，我们获得了 re,opt = 0.05–1.6 kpc 和 re,UV = 0.03–1.7 kpc 的光学 re,opt 和 UV re,UV 波长的有效半径范围，即与先前在尺寸-光度关系的大分散范围内的结果一致。然而，我们发现有效半径比 re,opt$/$re,UV 几乎是统一的，$1.01^{+0.35}_{-0.22}$，在 z = 4–10 上，没有过去内部的签名恒星的形成，例如在 z ∼ 0–2 处发现的。在没有合并的情况下，光学和紫外形态中心之间没有超过 3σ 的空间偏移，表明主要的恒星形成活动仅在 z ≳ 4 处的星系质量中心附近发现，可能正在经历由内而外的星系形成的第一阶段。