盖亚 CRF3 来源的光学变异性与鲁棒统计以及 5000 颗变异最大的类星体

Valeri V. Makarov
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引用次数: 0

摘要

利用 Gaia Data Release 3 中公布的 1170 多万个可变源的光曲线时间序列数据,计算了 83.6 万 Gaia CRF 天体的平均星等、颜色和可变性参数,这些天体主要是类星体和活动星系核(AGN)。为了减小数据中偶尔出现的异常现象的影响,我们采用了稳健的统计方法:即中位数、中位数绝对偏差和斯皮尔曼相关性。我们发现,大多数 CRF 来源在 Gaia G 波段的变异幅度适中,略低于 0.1 马格。变率振幅的重尾分布(以稳健标准偏差量化)并没有找到单一的分析形式,但更接近于麦克斯韦分布,尺度为 0.078 马格。大多数CRF源的G等和GBP-GRP颜色呈正相关,这意味着这些类星体和AGN在变亮时会变得更蓝。GBP波段和GRP波段的变化也大多呈正相关。对于红移 0.7 以上的更精确估计,所有变率参数与宇宙学红移的关系都相当平缓,而中值颜色则显示出强烈的系统性红移变化。利用一个稳健的量级偏差归一化分数,选出并公布了 5000 个变率最大的类星体样本。该样本与ICRF3星表的交集显示,ICRF3星表中强变类星体(主要是类星体)的比例要高得多。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Optical Variability of Gaia CRF3 Sources with Robust Statistics and the 5000 Most Variable Quasars
Using the light-curve time-series data for more than 11.7 million variable sources published in the Gaia Data Release 3, the average magnitudes, colors, and variability parameters have been computed for 0.836 million Gaia CRF objects, which are mostly quasars and active galactic nuclei (AGNs). To mitigate the effects of occasional flukes in the data, robust statistical measures have been employed: namely, the median, median absolute deviation, and Spearman correlation. We find that the majority of the CRF sources have moderate amplitudes of variability in the Gaia G band just below 0.1 mag. The heavy-tailed distribution of variability amplitudes (quantified as robust standard deviations) does not find a single analytical form, but is closer to Maxwell distribution with a scale of 0.078 mag. The majority of CRF sources have positive correlations between G magnitude and GBP−GRP colors, meaning that these quasars and AGNs become bluer when they are brighter. The variations in the GBP and GRP bands are also mostly positively correlated. Dependencies of all variability parameters with cosmological redshift are fairly flat for the more accurate estimates above redshift 0.7, while the median color shows strong systematic variations with redshift. Using a robust normalized score of magnitude deviations, a sample of the 5000 most variable quasars is selected and published. The intersection of this sample with the ICRF3 catalog shows a much higher rate of strongly variable quasars (mostly blazars) in ICRF3.
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