QSO的MUSEUM：与$z\sim$ 3类星体相关的分子气藏及其与扩展的Ly $α$发射的联系
APEX at the QSO MUSEUM: molecular gas reservoirs associated with $z\sim$3 quasars and their link to the extended Ly$α$ emission
摘要：
在$z\sim3$类星体周围经常可以探测到由氢Ly $α$辐射示踪的冷气体（T $\sim$ 10 $^{4}$ ~K），但对它们的分子气藏却知之甚少。本文介绍了类星体博物馆巡天中9个类星体的CO（6-5），CO（7-6）和[CI]（2-1）发射线的APEX光谱巡天，这些类星体具有相似的紫外光度，但非常不同的Ly $α$星云。这些观测（300 km~s $^{-1}$中的$\langle~\rm rms~\rangle=2.6$ ~mJy）探测到3条CO（6-5）谱线，其$\leq I_{\rm CO(6-5)} \leq$为5.1~Jy ~ s，620 $\leq$ FWHM $\leq$为707~km~s，以及3条[CI]（2-1）谱线，其$\leq I_{\rm [CI](2-1)} \leq$为2.3 $\leq I_{\rm [CI](2-1)} \leq$ 15.7~Jy ~s，329 $\leq$ FWHM $\leq$为943~km~s。对于检测到的CO和[CI]源，我们将分子气藏限制为$\rm M_{H_{2}} = (0.4-6.9) \times 10^{11} M_{\odot}$，而未检测到的则意味着$\rm M_{H_{2}} < 1.1\times 10^{11} M_{\odot}$。我们将我们的观察与扩展的Ly $α$性质进行比较，以了解冷态和分子气相之间的联系。我们发现在五个源（从$\sim$-400到$\sim+$ 1200~km~ sPDMATHABMR）中，Ly $α$的体相速度与分子气体系统红移之间有很大的位移.具有最大位移的源在样本中具有最大的Ly $α$线宽，这表明这些类星体周围存在更多的湍流气体条件和/或大规模的流入/流出。我们还发现，最亮（$I_{\rm[CI](2-1)}=15.7\pm3.7~\rm Jy~km~s^{-1}$）和最宽（FWHM $\sim$ 900~km~s $^{-1}$）的谱线分别出现在最小和最暗的Ly $α$星云中。从这一点上，我们推测，宿主星系遮蔽可以发挥重要作用，减少电离和Ly $α$光子能够逃脱晕尺度，和/或这些系统是由更大规模的晕主办。
英文摘要：
Cool gas (T$\sim$10$^{4}$~K) traced by hydrogen Ly$α$ emission is now routinely detected around $z\sim3$ quasars, but little is known about their molecular gas reservoirs. Here, we present an APEX spectroscopic survey of the CO(6-5), CO(7-6) and [CI](2-1) emission lines for 9 quasars from the QSO MUSEUM survey which have similar UV luminosities, but very diverse Ly$α$ nebulae. These observations ($\langle~\rm rms~\rangle=2.6$~mJy in 300~km~s$^{-1}$) detected three CO(6-5) lines with 3.4$\leq I_{\rm CO(6-5)} \leq$5.1~Jy~km~s$^{-1}$, 620$\leq$FWHM$\leq$707~km~s$^{-1}$, and three [CI](2-1) lines with 2.3$\leq I_{\rm [CI](2-1)} \leq$15.7~Jy~km~s$^{-1}$, 329$\leq$FWHM$\leq$943~km~s$^{-1}$. For the CO and [CI] detected sources, we constrain the molecular gas reservoirs to be $\rm M_{H_{2}} = (0.4-6.9) \times 10^{11} M_{\odot}$, while the non-detections imply $\rm M_{H_{2}} < 1.1\times 10^{11} M_{\odot}$. We compare our observations with the extended Ly$α$ properties to understand the link between the cool and the molecular gas phases. We find large velocity shifts between the bulk of Ly$α$ and the molecular gas systemic redshift in five sources (from $\sim$-400 to $\sim+$1200~km~s$^{-1}$). The sources with the largest shifts have the largest Ly$α$ line widths in the sample, suggesting more turbulent gas conditions and/or large-scale inflows/outflows around these quasars. We also find that the brightest ($I_{\rm[CI](2-1)}=15.7\pm3.7~\rm Jy~km~s^{-1}$) and the widest (FWHM$\sim$900~km~s$^{-1}$) lines are detected for the smallest and dimmest Ly$α$ nebulae. From this, we speculate that host galaxy obscuration can play an important role in reducing the ionizing and Ly$α$ photons able to escape to halo scales, and/or that these systems are hosted by more massive halos.
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