Long-period variable stars (LPVs) are pulsating red giants, primarily in the asymptotic giant branch phase, and they include both Miras and semi-regular variables (SRVs). Their period-age and period-luminosity relations enable us to trace different stellar populations, as they are intrinsically very bright and cover a wide range in distances and ages. The purpose of this study is to establish a census of LPV stars in a region close to the Galactic center, using the six-year database of the Vista Variables in the Vía Láctea (VVV) ESO Public Survey, as well as to describe the methodology that was employed to search for and characterize LPVs using VVV data. Near-IR surveys such as VVV provide a unique opportunity to probe the high-extinction innermost regions of the Milky Way. The detection and analysis of the intrinsically bright Miras in this region could provide us with an excellent probe of the properties of the Milky Way far behind its bulge. We used point-spread function photometry for all available $K_{s}$-band images in ten VVV tiles, covering $16.4~°^2$ in total, overlapping fields observed in the course of the Optical Gravitational Lensing Experiment (OGLE)-III survey. We designed a method to select LPV candidates, and we used the known variables from OGLE-III and other known variables from the literature to test our approach. The reduced $χ^2$ statistic, along with the flux-independent index $K_{(fi)}$, were used in our analysis. The Lomb-Scargle period search method, Fourier analysis, template fitting, and visual inspection were then performed to refine our sample and characterize the properties of the stars included in our catalog. A final sample of 130 Mira candidates, of which 129 are new discoveries, was thus obtained, with periods in the range between about 80 and 1400~days.
An Automated tool to detect variable sources in the Vista Variables in the V\'ıa Láctea Survey. The VVV Variables (V$^{4}$) catalog of tiles d001 and d002
Three Ultra-short Period Contact Eclipsing Binary Systems Mined from Massive Astronomical Surveys
本文介绍了从大量天文观测中发现的三颗接触型超短周期全食双星CRTS_J172718.0+431624、OGLE-BLG-ECL-000104和OGLE-BLG-ECL-000012的光度分析结果。利用VVV、OGLE、ZTF和CSS等天文观测资料，以及Helmos天文台2.3 m Aristarchos望远镜的多波段光度观测资料，计算了它们的相对物理参数。我们探索的参数空间，使用PIKAIA遗传算法优化。通过对全局最优值的MCMC抽样，对每个系统采用最佳光度解决方案和误差预算估计。采用经验质光关系，推导出每个接触系统的近似绝对参数。所有三个系统的质量比均低于0.5。2016-2022年期间，CRTS_J172718.0+431624的原生深度和次生深度之间的交换可能是由于现货活动。此外，我们提出了一个详细的分析，第一个良好的特点最短周期接触食双星与全食已知的（OGLE-BLG-ECL-000104）。由于VVV和OGLE LC，使用经验周期光度关系推导出OGLE-BLG-ECL-000104和OGLE-BLG-ECL-000012的新距离。在拆离双星形成通道的背景下，对这三个超短周期接触双星的起源和演化状态进行了深入的讨论。
Identification of unresolved binaries in the VVV b294 tile: A Pro-Am collaboration using the Virtual Observatory
Universidad Complutense de Madrid（马德里康普顿斯大学）；Centro de Astrobiología (CSIC-INTA)（天体生物学中心（西班牙国家研究委员会-国家航空航天技术研究所））；Asociación Astronómica AstroHenares（AstroHenares天文协会）；Agrupación Astronómica de Córdoba（科尔多瓦天文团）；Agrupación Astronómica de Sabadell（萨巴德尔天文团）
Automatic Catalog of RRLyrae from $\sim$ 14 million VVV Light Curves: How far can we go with traditional machine-learning?
Centro Internacional Franco Argentino de Ciencias de la Información y de Sistemas (CIFASIS, CONICET–UNR)（法国-阿根廷信息与系统科学国际中心（CIFASIS，CONICET–UNR））；Instituto De Astronomía Teórica y Experimental – Observatorio Astronómico Córdoba (IATE–OAC–UNC–CONICET)（理论与实验天文学研究所 – 科尔多瓦天文台（IATE–OAC–UNC–CONICET））；Western Sydney University (WSU)（西悉尼大学（WSU））
The Galactic Bulge exploration I.: The period-absolute\,magnitude-metallicity relations for RR~Lyrae stars for $G_{\rm BP}$, $V$, $G$, $G_{\rm RP}$, $I$, $J$, $H$, and $K_{\rm s}$ passbands using $Gaia$ DR3 parallaxes
