来自TNG50模拟的大质量星系在$3 \leq z \leq 6$尺度演化的预期：CEERS/JWST视角
Expectations of the size evolution of massive galaxies at $3 \leq z \leq 6$ from the TNG50 simulation: the CEERS/JWST view
Luca Costantin, Pablo G. Pérez-González, Jesús Vega-Ferrero, Marc Huertas-Company, Laura Bisigello, Fernando Buitrago, Micaela B. Bagley, Nikko J. Cleri, Michae… 展开作者
Luca Costantin, Pablo G. Pérez-González, Jesús Vega-Ferrero, Marc Huertas-Company, Laura Bisigello, Fernando Buitrago, Micaela B. Bagley, Nikko J. Cleri, Michael C. Cooper, Steven L. Finkelstein, Benne Holwerda, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Dylan Nelson, Casey Papovich, Annalisa Pillepich, Nor Pirzkal, Sandro Tacchella, L. Y. Aaron Yung
我们呈现了一个来自TNG50宇宙学模拟的约25,000张大质量（$M_{\star} \ge 10^9 M_{\odot}$）星系在红移$3 \leq z \leq 6$处的图像目录，这些图像专为JWST在多个波长上进行的观测而定制。合成图像使用SKIRT辐射传输代码生成，包含尘埃衰减和散射效应。无噪声图像经过mirage模拟器处理，以模拟宇宙演化早期发布科学（CEERS）巡天的近红外相机（NIRCam）观测策略（例如噪声、抖动模式等）。在本文中，我们分析了TNG50模拟对$3 \leq z \leq 6$处星系尺度演化的预测，以及CEERS探测该演化的预期。我们特别研究了尺度如何依赖于波长、红移、质量和图像角分辨率。我们发现有效半径准确描述了TNG50星系的三维半质量半径。在2~$\mu$m处观测到的尺度与在3.56~$\mu$m处测量的尺度在所有红移和质量上均一致。在所有质量下，较高红移星系群体比较低红移对应体更致密。然而，对于最大质量星系，尤其是在$z \lesssim 4$处，本征尺度小于模拟观测尺度。质量分布与光分布之间的这种差异可能表明在$z$=4-5处星系形态发生转变，大质量致密系统开始发展更延展的恒星结构。
英文摘要：
We present a catalog of about 25,000 images of massive ($M_{\star} \ge 10^9 M_{\odot}$) galaxies at redshift $3 \leq z \leq 6$ from the TNG50 cosmological simulation, tailored for observations at multiple wavelengths carried out with JWST. The synthetic images were created with the SKIRT radiative transfer code, including the effects of dust attenuation and scattering. The noiseless images were processed with the mirage simulator to mimic the Near Infrared Camera (NIRCam) observational strategy (e.g., noise, dithering pattern, etc.) of the Cosmic Evolution Early Release Science (CEERS) survey. In this paper, we analyze the predictions of the TNG50 simulation for the size evolution of galaxies at $3 \leq z \leq 6$ and the expectations for CEERS to probe that evolution. In particular, we investigate how sizes depend on wavelength, redshift, mass, and angular resolution of the images. We find that the effective radius accurately describes the three-dimensional half-mass radius of TNG50 galaxies. Sizes observed at 2~$μ$m are consistent with those measured at 3.56~$μ$m at all redshifts and masses. At all masses, the population of higher-$z$ galaxies is more compact than their lower-$z$ counterparts. However, the intrinsic sizes are smaller than the mock observed sizes for the most massive galaxies, especially at $z \lesssim 4$. This discrepancy between the mass and light distribution may point to a transition in the galaxy morphology at $z$=4-5, where massive compact systems start to develop more extended stellar structures.
Galaxy-scale lens search in the PEARLS NEP TDF and CEERS JWST fields
University of Melbourne（墨尔本大学）；ARC Centre of Excellence for All-Sky Astrophysics in 3 Dimensions (ASTRO 3D)（三维全天空天体物理学卓越研究中心）；Arizona State University（亚利桑那州立大学）；Instituto de Fisica de Cantabria (CSIC-UC)（坎塔布里亚物理研究所）；Space Telescope Science Institute（太空望远镜科学研究所）
Adding Value to JWST Spectra and Photometry: Stellar Population and Star Formation Properties of Spectroscopically Confirmed JADES and CEERS Galaxies at $z > 7$
本文分析 43 个 JADES/CEERS 经光谱证认的 $z>7$ JWST 星系，联合 SED 拟合、光谱线、测光与形态信息，揭示其上升的恒星形成历史、测光 EW 偏差及近期星暴贡献。
JWST Identification of Extremely Low C/N Galaxies with [N/O]$\gtrsim 0.5$ at $z\sim 6-10$ Evidencing the Early CNO-Cycle Enrichment and a Connection with Globular Cluster Formation
Direct T_e-based Metallicities of z=2-9 Galaxies with JWST/NIRSpec: Empirical Metallicity Calibrations Applicable from Reionization to Cosmic Noon
University of Kentucky（肯塔基大学）；University of California, Davis（加州大学戴维斯分校）；University of California, Los Angeles（加州大学洛杉矶分校）；University of Arizona（亚利桑那大学）；University of California, Riverside（加州大学河滨分校）；Cosmic Dawn Center (DAWN)（宇宙黎明中心）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）
