论文标题
Glass-JWST的早期结果。 V：星系$ z> 7 $的第一个休息框的光学尺寸亮度关系
Early results from GLASS-JWST. V: the first rest-frame optical size-luminosity relation of galaxies at $z>7$
论文作者
论文摘要
我们使用Glass James Webb太空望远镜早期发行科学（Glass-JWST-ERS）计划获得的NIRCAM成像数据，介绍了$ z> 7 $的第一个$ z> 7 $的星系的休息式光学尺寸亮度关系，提供了ERS活动的最深层核外层次数据。我们的样本由19个光学选择的明亮星系组成，$ m_ \ text {f444w} \ leq27.8 $ at $ 7 <z <9 $和$ m_ \ text {f444w} <28.2 $ at $ z \ sim99-15 $。 We measure the size of the galaxies in 5 bands, from the rest-frame optical ($\sim4800\,{\rm Å}$) to the ultra-violet (UV; $\sim1600\,{\rm Å}$) based on the Sérsic model, and analyze the size-luminosity relation as a function of wavelength.值得注意的是，NIRCAM成像的数据质量足以探测半灯半径$ r_e $降低到$ \ sim 100 $ pc $ z> 7 $。鉴于样本量和幅度范围有限，我们首先将斜率固定在使用HST样品中的REST框架紫外线中观察到的较大样品的斜率。参考光度时的中值$ r_0 $ $ m = -21 $从REST-FRAME光学（$ 600 \ pm80 $ pc）略微降低到UV（$ 450 \ pm130 $ pc）。然后，我们重新拟合尺寸亮度的关系，使斜率变化。除F150W以外的所有频段，该坡度与$β\ sim0.2 $一致，我们发现$β= 0.53 \ pm0.15 $的陡峭斜率更陡峭。陡峭的紫外线主要由最小，最微弱的星系驱动。如果用较大的样品确认，则意味着紫外线尺寸 - 露光关系朝向微弱的末端，如镜头研究所暗示的那样。
We present the first rest-frame optical size-luminosity relation of galaxies at $z>7$, using the NIRCam imaging data obtained by the GLASS James Webb Space Telescope Early Release Science (GLASS-JWST-ERS) program, providing the deepest extragalactic data of the ERS campaign. Our sample consist of 19 photometrically selected bright galaxies with $m_\text{F444W}\leq27.8$ at $7<z<9$ and $m_\text{F444W}<28.2$ at $z\sim9-15$. We measure the size of the galaxies in 5 bands, from the rest-frame optical ($\sim4800\,{\rm Å}$) to the ultra-violet (UV; $\sim1600\,{\rm Å}$) based on the Sérsic model, and analyze the size-luminosity relation as a function of wavelength. Remarkably, the data quality of NIRCam imaging is sufficient to probe the half-light radius $r_e$ down to $\sim 100$ pc at $z>7$. Given the limited sample size and magnitude range, we first fix the slope to that observed for larger samples in rest-frame UV using HST samples. The median size $r_0$ at the reference luminosity $M=-21$ decreases slightly from rest-frame optical ($600\pm80$ pc) to UV ($450\pm130$ pc). We then re-fit the size-luminosity relation allowing the slope to vary. The slope is consistent with $β\sim0.2$ for all bands except F150W, where we find a marginally steeper slope of $β=0.53\pm0.15$. The steep UV slope is mainly driven by the smallest and faintest galaxies. If confirmed by larger samples, it implies that the UV size-luminosity relation breaks toward the faint end as suggested by lensing studies.
