论文标题
改善SDSS条纹的阻尼随机步行参数82 pan-Starrs1
Improving Damped Random Walk parameters for SDSS Stripe 82 Quasars with Pan-STARRS1
论文作者
论文摘要
我们使用全景调查望远镜和快速响应系统1调查（Pan-Starrs1，PS1）数据来扩展Sloan数字天空调查（SDSS）条纹82 Quasar Light曲线。 PS1和SDSS光曲线的结合提供了15年基线的9248类品牌 - 比仅使用SDS的先前研究长5年。我们使用阻尼的随机步行（DRW）模型拟合光曲线 - 其可变性的统计描述。我们关联所得的DRW模型参数：渐近可变性幅度sf $ _ {\ infty} $和特征时间尺度$τ$，带有类星体物理属性 - 黑洞质量，冲击量度亮度和红移。使用模拟的光曲线，我们发现较长的基线使我们能够更好地约束DRW参数。添加PS1数据后，可变性幅度是黑洞质量的强大功能，并且对类星体发光度的依赖性较弱。另外，特征时间尺度$τ$依赖于类星体光度的略有弱弱。当Zwicky瞬态设施（ZTF）和Rubin Observator遗产调查时空（LSST）数据时，我们还对DRW模型参数检索的保真度进行了预测。最后，我们展示了更新的DRW参数如何提供一种独立的方法来发现更改外观的Quasar候选（CLQSO）。在SDS和PS1段之间的幅度和散射方面，候选人是异常值。我们识别40个对象（35个新报告），SDSS和SDSS-PS1数据之间的变异时间尺度增加了十倍，这是由于亮度发生较大（超过0.5 mag） - CLQSOS的特征。
We use the Panoramic Survey Telescope and Rapid Response System 1 Survey (Pan-STARRS1, PS1) data to extend the Sloan Digital Sky Survey (SDSS) Stripe 82 quasar light curves. Combining PS1 and SDSS light curves provides a 15 yr baseline for 9248 quasars - 5 yr longer than prior studies that used only SDSS. We fit the light curves with the damped random walk (DRW) model model - a statistical description of their variability. We correlate the resulting DRW model parameters: asymptotic variability amplitude SF$_{\infty}$, and characteristic timescale $τ$, with quasar physical properties - black hole mass, bolometric luminosity, and redshift. Using simulated light curves, we find that a longer baseline allows us to better constrain the DRW parameters. After adding PS1 data, the variability amplitude is a stronger function of the black hole mass, and has a weaker dependence on quasar luminosity. In addition, the characteristic timescale $τ$ dependence on quasar luminosity is marginally weaker. We also make predictions for the fidelity of DRW model parameter retrieval when light curves will be further extended with Zwicky Transient Facility (ZTF) and the Rubin Observatory Legacy Survey of Space and Time (LSST) data. Finally, we show how updated DRW parameters offer an independent method of discovering changing-look quasar candidates (CLQSOs). The candidates are outliers in terms of differences in magnitude and scatter between SDSS and PS1 segments. We identify 40 objects (35 newly reported) with tenfold increase in variability timescale between SDSS and SDSS--PS1 data, which is due to a large change in brightness (over 0.5 mag) - characteristic for CLQSOs.
