AI 中文总结
利用JWST/NIRCam成像研究z = 2.16时蛛网原星系团中星系结构，通过多波长参数建模分析星系质量-大小关系等，发现被动分数与局部密度有关，支持淬火和结构转变推进、大小增长仍在进行的观点。
AI 中文摘要
我们利用JWST/NIRCam的F115W、F182M和F410M成像（静止帧约3500Å至1.4μm）研究了在红移z = 2.16时环境如何影响蛛网原星系团中的星系结构。对JWST视场内1周3个星系的蛛网成员样本进行了单Sérsic和 bulge - disc分解的均匀多波长参数建模。形成恒星的星系遵循的质量-大小关系与场大致一致，在高质量端趋势稍陡。被动星系呈现更平缓的质量-大小关系，其典型大小介于同时期场星系和星团被动星系之间。在形成恒星和被动星系系统中，核球都比盘更紧凑。星系大小随波长增加略有减小，而ALMA探测到的尘埃形成恒星星系呈现更陡的波长依赖性。被动分数主要取决于局部密度，在低密度时类似场星系，在高密度时升至约60%。还发现局部密度与Sérsic指数有弱但显著的相关性，与有效半径或恒星形成率面密度无明显相关性。这些结果支持了淬火和结构转变已推进而大小增长仍在进行的图景。
英文摘要
We investigate how the environment affects galaxy structure in the Spiderweb protocluster at $z=2.16$ using JWST/NIRCam F115W, F182M, and F410M imaging (rest-frame $\sim 3500$Å to $1.4\,μ$m). We perform homogeneous multi-wavelength parametric modelling of the single-Sérsic and bulge--disc decomposition for the Spiderweb member sample of 103 galaxies within the JWST field of view (up to $\sim 2\times R_{200}$). Star-forming galaxies follow a mass--size relation broadly consistent with the field, with a mildly steeper trend at the high-mass end within uncertainties. Passive galaxies exhibit a flatter mass--size relation, and their typical size (intercept at fixed stellar mass) lies between that of the coeval field and cluster passive populations, indicating an intermediate evolutionary stage. In both star-forming and passive systems, bulges are systematically more compact than discs. Galaxy sizes decrease slightly with increasing wavelength, whereas ALMA-detected dusty star-forming galaxies exhibit a much steeper wavelength dependence, consistent with centrally concentrated, obscured star formation. The passive fraction depends primarily on local density: it resembles the field at $Σ\lesssim 100$--$200\,{\rm gal\,Mpc^{-2}}$ and rises to $\sim60\%$ at $Σ\gtrsim 1000\,{\rm gal\,Mpc^{-2}}$, although with relatively large uncertainties due to the small number of galaxies in the highest-density bins, with no significant additional dependence on clustercentric distance. We also find a weak but significant correlation between local density and Sérsic index (strongest in F410M), but no clear correlation with effective radius or the star-formation rate surface density $Σ_{\rm SFR}$. These results support a picture in which quenching and structural transformation are already advanced, while the size growth is still ongoing.
Comments12 pages, 7 figures, accepted in A&A
