论文标题
$ z \ sim $ 11-17的Ultra High-Redshift Galaxy候选人的Alma Fir视图：蓝色怪物还是低$ Z $ RED RED INTELLOPERS？
ALMA FIR View of Ultra High-redshift Galaxy Candidates at $z\sim$ 11-17: Blue Monsters or Low-$z$ Red Interlopers?
论文作者
论文摘要
We present ALMA Band~7 observations of a remarkably bright galaxy candidate at $z_{\rm phot}$=$16.7^{+1.9}_{-0.3}$ ($M_{\rm UV}$=$-21.6$), S5-z17-1, identified in JWST Early Release Observation data of Stephen's Quintet.我们没有在866〜 $μ$ m处检测到尘埃连续体，排除了\ targb \是低 - $ z $ dusty starburst的可能性，其星形成率为$ \ gtrsim 30 $〜$〜$ m m _ {\ odot} $ 〜yr $^yr $^yr $^{ - 1} $。我们在$ 338.726 \ pm0.007 $ 〜GHz恰好与JWST源位置相吻合的5.1 $σ$线功能，其信号的可能性为2 \％。最有可能的线标识是[OIII] 52 $μ$ m，$ z = 16.01 $或[CII] 158 $ $ m at $ z = 4.61 $，其线路亮度并不违反两种情况下的灰尘连续性的未检测。连同其他三个$ Z \ gtrsim $ 11--13候选星系最近在Alma观察到，我们进行了ALMA和JWST Spectral Energy分布（SED）分析，发现高$ Z $解决方案以$ Z \ sim $ 11--17在每个候选人中都受到青睐（非常蓝色的canteruum canteruum slope of $ \ simeq-2 $ simeq-2 $），以及lum simeq-2 $ num pum {$ simeq-2 $ s），并且ry num pum num pum num n um pum num n um pum num n um pum num n um pum {$ m。 uv} \ simeq [ - $ 24：$ - 21] $）系统。 Still, we find in several candidates that reasonable SED fits ($Δ$ $χ^{2}\lesssim4$) are reproduced by type-II quasar and/or quiescent galaxy templates with strong emission lines at $z\sim3$--5, where such populations predicted from their luminosity functions and EW([OIII]+H$β$) distributions are abundant in survey volumes used为了标识$ z \ sim $ 11--17候选人。尽管这些最近的ALMA观察结果加强了高$ Z $解决方案的可能性，但在$ z \ sim $ 11--17个候选人中的几个中，较低的$ z $可能性并不完全排除，这表明需要考虑在Ultra High-$ z $ Galaxy搜索中较低$ Z $污染物的相对表面密度。
We present ALMA Band~7 observations of a remarkably bright galaxy candidate at $z_{\rm phot}$=$16.7^{+1.9}_{-0.3}$ ($M_{\rm UV}$=$-21.6$), S5-z17-1, identified in JWST Early Release Observation data of Stephen's Quintet. We do not detect the dust continuum at 866~$μ$m, ruling out the possibility that \targb\ is a low-$z$ dusty starburst with a star-formation rate of $\gtrsim 30$~$M_{\odot}$~yr$^{-1}$. We detect a 5.1$σ$ line feature at $338.726\pm0.007$~GHz exactly coinciding with the JWST source position, with a 2\% likelihood of the signal being spurious. The most likely line identification would be [OIII]52$μ$m at $z=16.01$ or [CII]158$μ$m at $z=4.61$, whose line luminosities do not violate the non-detection of the dust continuum in both cases. Together with three other $z\gtrsim$ 11--13 candidate galaxies recently observed with ALMA, we conduct a joint ALMA and JWST spectral energy distribution (SED) analysis and find that the high-$z$ solution at $z\sim$11--17 is favored in every candidate as a very blue (UV continuum slope of $\simeq-2.3$) and luminous ($M_{\rm UV}\simeq[-$24:$-21]$) system. Still, we find in several candidates that reasonable SED fits ($Δ$ $χ^{2}\lesssim4$) are reproduced by type-II quasar and/or quiescent galaxy templates with strong emission lines at $z\sim3$--5, where such populations predicted from their luminosity functions and EW([OIII]+H$β$) distributions are abundant in survey volumes used for the identification of the $z\sim$11--17 candidates. While these recent ALMA observation results have strengthened the likelihood of the high-$z$ solutions, lower-$z$ possibilities are not completely ruled out in several of the $z\sim$11--17 candidates, indicating the need to consider the relative surface densities of the lower-$z$ contaminants in the ultra high-$z$ galaxy search.
