The VVV Infrared Variability Catalog (VIVA-I). (arXiv:2005.05404v1 [astro-ph.SR])

The VVV Infrared Variability Catalog (VIVA-I). (arXiv:2005.05404v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lopes_C/0/1/0/all/0/1">C. E. Ferreira Lopes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cross_N/0/1/0/all/0/1">N. J. G. Cross</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Catelan_M/0/1/0/all/0/1">M. Catelan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Minniti_D/0/1/0/all/0/1">D. Minniti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hempel_M/0/1/0/all/0/1">M. Hempel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lucas_P/0/1/0/all/0/1">P. W. Lucas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angeloni_R/0/1/0/all/0/1">R. Angeloni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jablonsky_F/0/1/0/all/0/1">F. Jablonsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Braga_V/0/1/0/all/0/1">V. F. Braga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leao_I/0/1/0/all/0/1">I. C. Leao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herpich_F/0/1/0/all/0/1">F. R. Herpich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alonso_Garcia_J/0/1/0/all/0/1">J. Alonso-Garcia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Papageorgiou_A/0/1/0/all/0/1">A. Papageorgiou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pichara_K/0/1/0/all/0/1">K. Pichara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saito_R/0/1/0/all/0/1">R. K. Saito</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bradley_A/0/1/0/all/0/1">A. Bradley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beamin_J/0/1/0/all/0/1">J. C. Beamin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cortes_C/0/1/0/all/0/1">C. Cortes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Medeiros_J/0/1/0/all/0/1">J. R. De Medeiros</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Russell_C/0/1/0/all/0/1">Christopher. M. P. Russell</a>

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.

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