论文标题
[oiii] 88 $μ$ m和1.2 mm连续排放的上限
An upper limit on [OIII] 88 $μ$m and 1.2 mm continuum emission from a JWST $z \approx 12-13$ galaxy candidate with ALMA
论文作者
论文摘要
最近，根据公共James Webb太空望远镜（JWST）NIRCAM观察，确定了许多新的$ Z> 11美元的Galaxy候选人。这些候选者的光谱证实是必须稳健地衡量其红移，并将它们置于对早期宇宙中星系积聚的背景下。 Glass-Z13是这些候选人之一，报告的光度红移$ z> 11.9 $。我提出了公开可用的Atacama大毫米/毫米/毫米阵列（ALMA）Band 6 Direction董事的酌处时间观察（Project 2021.A.00020.S; Pi T. Bakx），通过在搜索[OIIII]线发射的Redshift promiss-Z13中获得光谱红移，以获取glass-Z13的红色速度。在玻璃-Z13周围的光圈中提取的集成光谱中，也未检测到[OIII]发射，也没有在使用自动线查找算法（对成像应用不同的UV加权策略）时检测到。也未检测到与玻璃-Z13相关的1.2 mM连续发射。如果Glass-Z13在Z $ \ $ 12-13处，这意味着[OIII]和REST-FRAME $ \ sim $ 90 $ 90 $ 90 $ 90 $ $ m $ m Continum $ \ sim1 \ times10^8 \，\ rm {lmm {l} _ \ odot $和10.8 $ $ Jy， [OIII]和连续发射的未检测并不一定意味着玻璃Z13不在$ z \ of12-13 $上。它也可以通过低金属性（$ \ sim 0.2 \，\ rm {z} _ \ odot $或较低）和/或高密度（至少100 $ \ rm {cm}^{ - 3} $）。这项工作证明了Alma和JWST之间研究第一个星系性能的协同作用，尽管JWST/NIRSPEC光谱对于确认或拒绝玻璃-Z13的高光度光度降射是必需的。
A number of new $z>11$ galaxy candidates have recently been identified based on public James Webb Space Telescope (JWST) NIRCam observations. Spectroscopic confirmation of these candidates is necessary to robustly measure their redshift and put them in the context of our understanding of the buildup of galaxies in the early Universe. GLASS-z13 is one of these candidates, with a reported photometric redshift $z>11.9$. I present publicly available Atacama Large Millimeter/submillimeter Array (ALMA) band 6 Director's Discretionary Time observations (project 2021.A.00020.S; PI T. Bakx), taken to acquire a spectroscopic redshift for GLASS-z13 by searching for [OIII] line emission in the redshift range $z=11.9-13.5$. No [OIII] emission is detected in integrated spectra extracted within an aperture around GLASS-z13, nor when using an automated line finding algorithm (applying different uv-weighting strategies for the imaging). 1.2 mm continuum emission associated to GLASS-z13 is not detected either. If GLASS-z13 is at z$\approx$12-13, this implies a 3-$σ$ upper limit on the [OIII] and rest-frame $\sim$90 $μ$m continuum emission of $\sim1\times10^8\,\rm{L}_\odot$ and 10.8 $μ$Jy, respectively. The non-detection of [OIII] and continuum emission does not necessarily imply that GLASS-z13 is not at $z\approx12-13$. It can also be explained by a low metallicity ($\sim 0.2\,\rm{Z}_\odot$ or lower) and/or high-density (at least 100 $\rm{cm}^{-3}$) interstellar medium. This work demonstrates the synergy between ALMA and JWST to study the properties of the first galaxies, although JWST/NIRSpec spectroscopy will be necessary to confirm or reject the high photometric-redshift of GLASS-z13.
