论文标题
VST ATLAS类星体调查I：目录
The VST ATLAS Quasar Survey I: Catalogue
论文作者
论文摘要
我们介绍VST ATLAS类星体调查，包括$ \ sim1,229,000 $ quasar（QSO）候选人，$ 16 <g <g <22.5 $超过$ \ sim4700 $ deg $^2 $。该目录基于VST Atlas $+$ neowise Imaging Surveys，旨在达到$ z <2.2 $和$ z <2.2 $和$ \ sim30 $ deg $^{ - 2} $ $ z <2.2 $ $ 130 $ v $^{ - 2} $的QSO天空密度。该目录的目的之一是为4个宇宙学红移调查选择QSO目标。为了指导我们的选择，我们在扩展的William Herschel Deep Field（WHDF）中使用X射线/UV/Optical/Mir数据，在此我们找到$ G <22.5 $ broad Line QSO密度为$ 269 \ pm67 $ deg $^{ - 2} $，与预期的$ \ sim196 $ deg $^$^$^{ - 2} $一致。我们还发现，$ \ sim25 $％的QSO在形态上分类为光学扩展。总体而言，我们发现，在这些深度数据中，MiR，UV和X射线选择都是$ \ sim70-90 $％完整的，而X射线的污染物比Mir和UV少。但是，mir比X射线或紫外线至$ z> 2.2 $ QSO更敏感，$ g <22.5 $和EROSITA限制。然后，我们调整了以前2QDE试验调查的选择标准，并优先考虑显示紫外线和mir过量的VST ATLAS候选者，同时还选择最初归类为扩展的候选者。我们使用DESI的数据（将在DR1中发布）和2DF测试我们的选择，以估计选择的效率和完整性，最后我们使用ANNZ2来确定QSO候选目录的光度红移。 Applying over the $\sim4700$ deg$^2$ ATLAS area gives us $\sim917,000$ $z<2.2$ QSO candidates of which 472,000 are likely to be $z<2.2$ QSOs, implying a sky density of $\sim$100 deg$^{-2}$, which our WHDF analysis suggests will rise to at least 130 deg$^{-2}$ when eROSITA包括X射线候选人。在$ z> 2.2 $时，我们找到了$ \ sim310,000 $候选人，其中169,000可能是$ \ sim36 $ deg $^{ - 2} $的QSO。
We present the VST ATLAS Quasar Survey, consisting of $\sim1,229,000$ quasar (QSO) candidates with $16<g<22.5$ over $\sim4700$ deg$^2$. The catalogue is based on VST ATLAS$+$NEOWISE imaging surveys and aims to reach a QSO sky density of $130$ deg$^{-2}$ for $z<2.2$ and $\sim30$ deg$^{-2}$ for $z>2.2$. One of the aims of this catalogue is to select QSO targets for the 4MOST Cosmology Redshift Survey. To guide our selection, we use X-ray/UV/optical/MIR data in the extended William Herschel Deep Field (WHDF) where we find a $g<22.5$ broad-line QSO density of $269\pm67$ deg$^{-2}$, roughly consistent with the expected $\sim196$ deg$^{-2}$. We also find that $\sim25$% of our QSOs are morphologically classed as optically extended. Overall, we find that in these deep data, MIR, UV and X-ray selections are all $\sim70-90$% complete while X-ray suffers less contamination than MIR and UV. MIR is however more sensitive than X-ray or UV to $z>2.2$ QSOs at $g<22.5$ and the eROSITA limit. We then adjust the selection criteria from our previous 2QDES pilot survey and prioritise VST ATLAS candidates that show both UV and MIR excess, while also selecting candidates initially classified as extended. We test our selections using data from DESI (which will be released in DR1) and 2dF to estimate the efficiency and completeness of our selections, and finally we use ANNz2 to determine photometric redshifts for the QSO candidate catalogue. Applying over the $\sim4700$ deg$^2$ ATLAS area gives us $\sim917,000$ $z<2.2$ QSO candidates of which 472,000 are likely to be $z<2.2$ QSOs, implying a sky density of $\sim$100 deg$^{-2}$, which our WHDF analysis suggests will rise to at least 130 deg$^{-2}$ when eROSITA X-ray candidates are included. At $z>2.2$, we find $\sim310,000$ candidates, of which 169,000 are likely to be QSOs for a sky density of $\sim36$ deg$^{-2}$.
