论文标题
XGAPS：一个亚弧形的银河平面调查
XGAPS: a sub-arcsecond cross-match of Galactic Plane Surveys
论文作者
论文摘要
我们提出了针对INT银河飞机调查（IGAP）和英国红外深色Sky Survey（UKIDSS）的GAIA数据版本3（DR3）的近距离交叉匹配。由此产生的交叉匹配的银河飞机调查（XGAPS）为GAIA光度法提供了其他精确的光度法（$ u_ {rgo} $，$ g $，$ r $，$ r $，$ i $，$ i $，$ i $，$ i $，$ i $，$ i $，$ i $，$ i $，$ i $，$ i $，$ i $，$ i $，$ i $，$ i $，$ j $，$ j $，$ h $和$ k $）。在构建目录时，Gaia DR3中给出的适当动作会恢复到与Igaps组成的调查相匹配的时期（对北银河平面的Int光度测量\ HA调查，IPHAST和UV-Excess对北部银河平面的uv-Excess调查，uvex，uvex，uvevex）和ukidss，确保了高正确的运动对象。该目录包含33,987,180个来源。每一个列出的来源的$>3σ$视差检测的要求意味着覆盖了1--1.5 kpc的距离。在生产XGAP时，我们还训练了一个随机的森林分类器，以辨别出有问题的星体解决方案的目标。基于分类器结果的选择切割可用于以受控和合理的方式清洁颜色尺度和颜色彩色图，并生产出天文统计的可靠目标子集。我们提供XGAP作为111列表。目录的用途包括选择用于多对象光谱调查的银河系目标以及对特定银河种群的识别。
We present a sub-arcsecond cross-match of Gaia Data Release 3 (DR3) against the INT Galactic Plane Surveys (IGAPS) and the United Kingdom Infrared Deep Sky Survey (UKIDSS). The resulting cross-match of Galactic Plane Surveys (XGAPS) provides additional precise photometry ($U_{RGO}$, $g$, $r$, $i$, H$α$, $J$, $H$ and $K$) to the Gaia photometry. In building the catalogue, proper motions given in Gaia DR3 are wound back to match the epochs of the IGAPS constituent surveys (INT Photometric \ha Survey of the Northern Galactic Plane, IPHAS, and the UV-Excess Survey of the northern Galactic plane, UVEX) and UKIDSS, ensuring high proper motion objects are appropriately cross-matched. The catalogue contains 33,987,180 sources. The requirement of $>3σ$ parallax detection for every included source means that distances out to 1--1.5 kpc are well covered. In producing XGAPS we have also trained a Random Forest classifier to discern targets with problematic astrometric solutions. Selection cuts based on the classifier results can be used to clean colour-magnitude and colour-colour diagrams in a controlled and justified manner, as well as producing subsets of astrometrically reliable targets. We provide XGAPS as a 111 column table. Uses of the catalogue include the selection of Galactic targets for multi-object spectroscopic surveys as well as identification of specific Galactic populations.
