论文标题
在CO排放调查中确定的巨大的，尘土飞扬的高吸收选择的星系大约2.46 $
A Massive, Dusty HI-Absorption-Selected Galaxy at $z \approx 2.46$ Identified in a CO Emission Survey
论文作者
论文摘要
我们报告了一个北部的扩展毫米阵列（NOEMA）和ATACAMA大毫米/毫米/毫米阵列（ALMA）搜索与七个高金属金属相关的星系中的红移CO排放（[m/h] $ \ geq-geq -1.03 $）我们的观察结果通过使用NOEMA从$ z = 2.4604 $从星系发射CO（3-2）发射的新发现，与$ z = 2.4628 $ dla有关to QSO B0201+365。包括以前的搜索，我们的搜索导致CO排放的检测率分别为$ \ of 56^{+38} _ { - 24} $％和$ \ of of11^{+26} _ { - 9} $％，分别在$ {\ rm [m/h]} $ 0.3 $和$ 0.3 $和0.3 $和0.3 $}的DLA领域，此外，与[m/h] $> -0.3 $相关的HI选择星系都具有高分子气体质量，$ \ gtrsim5 \ times10^{10} \ {\ rm m m} _ \ odot $。这表明$ z \ of 2 $的最高金属dlas与最大的星系有关。新近识别的$ z \ 2.4604 $ hi选择的星系，DLA0201+365G，对QSO视线的影响参数约为$ \ of $ \ of $ \ kpc，而暗示的分子气体质量为$（5.04 \ pm0.78）\ pm0.78） co} /4.36）\ times（r_ {31} /0.55）\ {\ rm m} _ \ odot $。档案中的哈勃太空望远镜宽场和行星相机2成像涵盖了该星系中的静止框架（NUV）（NUV）和Far-ultraviolet（FUV）的发射，从该星系中产生了静止式NUV和fuv的非检测，以及2.3 m $ $ _ $ _ $ _ $ $ $ $ $ y y y y y y yr $ y y yr $ y y yr $ yr $ yr $ yr $ yr $ yr $ yr $^$^ - （SFR）。基于NUV低的SFR估计值尽管非常高的分子气体质量，但表明DLA0201+365G是非常灰尘的星系，或者具有分子气体耗尽时间，大约要大约两个数量级，该数量级大于相似的红移的星形星系。
We report a NOrthern Extended Millimeter Array (NOEMA) and Atacama Large Millimeter/submillimeter Array (ALMA) search for redshifted CO emission from the galaxies associated with seven high-metallicity ([M/H] $\geq -1.03$) damped Lyman-$α$ absorbers (DLAs) at $z\approx1.64-2.51$. Our observations yielded one new detection of CO(3-2) emission from a galaxy at $z=2.4604$ using NOEMA, associated with the $z=2.4628$ DLA towards QSO B0201+365. Including previous searches, our search results in detection rates of CO emission of $\approx56^{+38}_{-24}$ % and $\approx11^{+26}_{-9}$ %, respectively, in the fields of DLAs with ${\rm [M/H]}>-0.3$ and ${\rm [M/H]}<-0.3$. Further, the HI-selected galaxies associated with five DLAs with [M/H] $>-0.3$ all have high molecular gas masses, $\gtrsim5\times10^{10}\ {\rm M}_\odot$. This indicates that the highest-metallicity DLAs at $z\approx2$ are associated with the most massive galaxies. The newly-identified $z\approx2.4604$ HI-selected galaxy, DLA0201+365g, has an impact parameter of $\approx7$ kpc to the QSO sightline, and an implied molecular gas mass of $(5.04\pm0.78) \times10^{10}\times(α_{\rm CO}/4.36)\times(r_{31}/0.55)\ {\rm M}_\odot$. Archival Hubble Space Telescope Wide Field and Planetary Camera 2 imaging covering the rest-frame near-ultraviolet (NUV) and far-ultraviolet (FUV) emission from this galaxy yield non-detections of rest-frame NUV and FUV emission, and a $5σ$ upper limit of 2.3 M$_\odot$ yr$^{-1}$ on the unobscured star formation rate (SFR). The low NUV-based SFR estimate, despite the very high molecular gas mass, indicates that DLA0201+365g either is a very dusty galaxy, or has a molecular gas depletion time that is around two orders of magnitude larger than that of star-forming galaxies at similar redshifts.
