论文标题
VVV红外可变性目录（Viva-I）
The VVV Infrared Variability Catalog (VIVA-I)
论文作者
论文摘要
得益于Via Lactea（VVV）ESO公共调查中的Vista变量，现在可以探索这些地区的大量对象。本文介绍了使用新方法在VVVDR4中具有10个以上观测值的所有VVV点源的可变性分析。总的来说，使用新的洞察力分析项目中开发的方法分析了288,378,769个来源的近红外光曲线。结果，我们提出了一个完整的样本，具有44、998、752个可变星候选物（VVV-CVSC），其中包括精确的单个坐标，近IIR大小（ZYJHKS），灭绝A（ks），可变性索引，周期，周期，时期，振幅等参数来评估科学。不幸的是，具有高度完整样本的副作用也具有不可变化的高水平污染（非变异与变量的污染比略高于10：1）。为了解决这个问题，我们还提供了一些标志和参数，社区可以使用这些标志和参数来消除可变候选者的数量，而不会大大降低样本的完整性。特别是，我们与SIMBAD和AAVSO数据库交叉识别339,601个来源，这些数据库为我们提供了其他浪潮中这些对象的信息。该子样本构成了一个独特的资源，用于研究已知来源的相应近IR变异性以及评估与X射线和伽马射线源相关的IR变异性。另一方面，我们的样本中的其他99.5％的来源构成了许多潜在的新物体，这些对象具有可变性信息，用于银河平面和凸起的大量拥挤和变红的区域。目前的结果还提供了重要的查询资源，以执行可变性分析并表征诸如TESS和LSST等正在进行的和未来的调查。
Thanks to the VISTA Variables in the Via Lactea (VVV) ESO Public Survey it is now possible to explore a large number of objects in those regions. This paper addresses the variability analysis of all VVV point sources having more than 10 observations in VVVDR4 using a novel approach. In total, the near-IR light curves of 288,378,769 sources were analysed using methods developed in the New Insight Into Time Series Analysis project. As a result, we present a complete sample having 44, 998, 752 variable star candidates (VVV-CVSC), which include accurate individual coordinates, near-IR magnitudes (ZYJHKs), extinctions A(Ks), variability indices, periods, amplitudes, among other parameters to assess the science. Unfortunately, a side effect of having a highly complete sample, is also having a high level of contamination by non-variable (contamination ratio of non-variables to variables is slightly over 10:1). To deal with this, we also provide some flags and parameters that can be used by the community to de-crease the number of variable candidates without heavily decreasing the completeness of the sample. In particular, we cross-identified 339,601 of our sources with Simbad and AAVSO databases, which provide us with information for these objects at other wavelegths. This sub-sample constitutes a unique resource to study the corresponding near-IR variability of known sources as well as to assess the IR variability related with X-ray and Gamma-Ray sources. On the other hand, the other 99.5% sources in our sample constitutes a number of potentially new objects with variability information for the heavily crowded and reddened regions of the Galactic Plane and Bulge. The present results also provide an important queryable resource to perform variability analysis and to characterize ongoing and future surveys like TESS and LSST.
