论文标题
解释JWST超级星系的Alma非检测
Interpreting ALMA non-detections of JWST super-early galaxies
论文作者
论文摘要
最近试图检测[OIII] 88 $μ$ m从JWST观察到的超级（$ z> 10 $）的星系候选者的排放量未成功。通过使用Zoom-In模拟，我们表明这些星系是微弱的，并且主要落在本地金属贫困$ \ rm [OIII] -SFR $下方，因为它们的低电离参数，$ u _ {\ rm ion} \ rm ion} \ sillsim 10^{ - 3} $。如此低的$ u _ {\ rm ion} $值是在早期组装阶段的星系中发现的，其恒星仍然嵌入高密度的出生云中。但是，我们的样品中最发光的星系（$ \ rm {log} [l _ {\ rm {[[oiii]}}}/l_ \ odot] = 8.4 $，$ _ {\ rm ion} \ rm ion} \ yout 0.1 $）可以在Alma中以$ 2.8 $ 2.8 $ hrs的价格检测到。
Recent attempts to detect [OIII] 88$μ$m emission from super-early ($z>10$) galaxy candidates observed by JWST have been unsuccessful. By using zoom-in simulations, we show that these galaxies are faint, and mostly fall below the local metal-poor $\rm [OIII]-SFR$ relation as a result of their low ionization parameter, $U_{\rm ion}\lesssim 10^{-3}$. Such low $U_{\rm ion}$ values are found in galaxies that are in an early assembly stage, and whose stars are still embedded in high-density natal clouds. However, the most luminous galaxy in our sample ($\rm{log}[L_{\rm{[OIII]}}/L_\odot] = 8.4$, $U_{\rm ion} \approx 0.1$) could be detected by ALMA in only $2.8$ hrs.
