Identifying Periodic Variable Stars and Eclipsing Binary Systems with Long-term Las Cumbres Observatory Photometric Monitoring of ZTF J0139+5245
Identifying Periodic Variable Stars and Eclipsing Binary Systems with Long-term Las Cumbres Observatory Photometric Monitoring of ZTF J0139+5245
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DOI：
10.3847/1538-3881/ac18be
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发表时间：
2021-07
期刊：
影响因子：
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通讯作者：
A. Sanghi;Z. Vanderbosch;M. Montgomery
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文献类型：
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作者：
A. Sanghi;Z. Vanderbosch;M. Montgomery
利用位于McDonald天文台的两个1.0 m望远镜节点，利用Sinistro成像仪对白色矮星ZTF J0139+5245进行了长期观测。在这次搜索中，我们发现了38个可变源，其中27个是新发现的或新分类的（71%），根据与以前公布的目录的比较，从而增加了在考虑中的视场中的检测数量的一个因素的2.5倍。我们发现，由于LCO图像的曝光时间较长，加上LCO测光的时间采样更长，每次曝光的测光精度提高，使我们能够增加在这个视野中的检测总数。每一张LCO图像覆盖的视场为26′ × 26′，观测的区域靠近银道面（B = −9.°4），恒星密度平均为108弧分−2。我们进行孔径测光和傅立叶分析超过2000颗恒星跨越1560 LCO图像跨越537天，找到28个候选人天龙座变星，三个候选人食双星的EA型，和7个候选人食双星的EW型。在分配初步的分类，我们的检测，我们证明了盖亚色星等图作为一个强大的分类工具，变星研究的适用性。
We present the results of our search for variable stars using the long-term Las Cumbres Observatory (LCO) monitoring of white dwarf ZTF J0139+5245 with the two 1.0 m telescope nodes located at McDonald Observatory using the Sinistro imaging instrument. In this search, we find 38 variable sources, of which 27 are newly discovered or newly classified (71%) based on comparisons with previously published catalogs, thereby increasing the number of detections in the field of view under consideration by a factor of ≈2.5. We find that the improved photometric precision per exposure due to longer exposure time for LCO images combined with the greater time sampling of LCO photometry enables us to increase the total number of detections in this field of view. Each LCO image covers a field of view of 26′ × 26′ and observes a region close to the Galactic plane (b = −9.°4) abundant in stars with an average stellar density of ≈8 arcmin−2. We perform aperture photometry and Fourier analysis on over 2000 stars across 1560 LCO images spanning 537 days to find 28 candidate BY Draconis variables, three candidate eclipsing binaries of type EA, and seven candidate eclipsing binaries of type EW. In assigning preliminary classifications to our detections, we demonstrate the applicability of the Gaia color–magnitude diagram as a powerful classification tool for variable-star studies.