Correction to: Optical variability of quasars with 20-year photometric light curves
Correction to: Optical variability of quasars with 20-year photometric light curves
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DOI：
10.1093/mnras/stac1259
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发表时间：
2022-01
影响因子：
4.8
通讯作者：
Zach Stone;Yue Shen;C. J. Burke;Yu-Ching Chen;Qian Yang;Xin Liu;R. Gruendl;M. Adamów;F. Andrade-Oliveira;J. Annis;D. Bacon;E. Bertin;S. Bocquet;D. Brooks;D. Burke;A. Rosell;M. Kind;J. Carretero;L. Costa;M. Pereira;J. Vicente;S. Desai;H. Diehl;P. Doel;I. Ferrero;D. Friedel;J. Frieman;J. Garc'ia-Bellido;E. Gaztañaga;D. Gruen;G. Gutiérrez;S. Hinton;D. Hollowood;K. Honscheid;K. Kuehn;N. Kuropatkin;C. Lidman;M. Maia;F. Menanteau;R. Miquel;R. Morgan;F. Paz-Chinch'on;A. Pieres;A. P. Malag'on;M. Rodríguez-Monroy;E. Sanchez;V. Scarpine;S. Serrano;I. Sevilla-Noarbe;E. Suchyta;M. Swanson;G. Tarlé;C. B. D. O. Astronomy;U. I. Urbana-Champaign;National Center for Supercomputing Applications;Center for Astrophysical Surveys;H. C. F. Astrophysics;Instituto de F'isica Te'orica;Universidade Estadual Paulista;L. LIneA;F. N. Laboratory;Institute of Cosmology;Gravitation;U. Portsmouth;Cnrs;Umr 7095;I. Paris;Sorbonne Universit'es;06 UPMCUnivParis;F. O. Physics;Ludwig-Maximilians-Universitat;D. PhysicsAstronomy;University College London;Kavli Institute for Particle AstrophysicsCosmology;S. N. Laboratory;Institut de F'isica d'Altes Energies;T. Z. F. O. Science;Technology;O. Nacional;D. Physics;U. Michigan;A. Arbor;H. Sternwarte;U. Hamburg;Centro de Investigaciones Energ'eticas;Medioambientales y Tecnol'ogicas;Iit Hyderabad;Institute of Theoretical Astrophysics;U. Oslo;Instituto de Fisica Teorica Uamcsic;U. A. D. Madrid;I. D. E. D. Catalunya-I.-D.-E.-D.-Catalunya-152160569;Institute of Space Sciences;Campus Uab;S. O. Mathematics;Physics;U. Queensland;Santa Cruz Institute for Particle Physics;Center for Cosmology;Astro-particle Physics;T. O. S. University;Australian Astronomical Optics;M. University;L. Observatory;Centre for Gravitational Astrophysics;College of Materials Science;The Australian National University;T. D. O. Astronomy;Astrophysics;A. N. University;I. C. D. R. I. E. Avanccats-I.-C.-D.-R.-I.-E.-Avanccats-1387885964;P. Department;U. Wisconsin--Madison-U.-Wisconsin--Madison-1387898181;I. O. Astronomy;U. Cambridge;D. Sciences;P. University;Computer Science;M. Division;Oak Ridge National Laboratory;Waldorf High School of Massachusetts Bay
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文献类型：
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作者：
Zach Stone;Yue Shen;C. J. Burke;Yu-Ching Chen;Qian Yang;Xin Liu;R. Gruendl;M. Adamów;F. Andrade-Oliveira;J. Annis;D. Bacon;E. Bertin;S. Bocquet;D. Brooks;D. Burke;A. Rosell;M. Kind;J. Carretero;L. Costa;M. Pereira;J. Vicente;S. Desai;H. Diehl;P. Doel;I. Ferrero;D. Friedel;J. Frieman;J. Garc'ia-Bellido;E. Gaztañaga;D. Gruen;G. Gutiérrez;S. Hinton;D. Hollowood;K. Honscheid;K. Kuehn;N. Kuropatkin;C. Lidman;M. Maia;F. Menanteau;R. Miquel;R. Morgan;F. Paz-Chinch'on;A. Pieres;A. P. Malag'on;M. Rodríguez-Monroy;E. Sanchez;V. Scarpine;S. Serrano;I. Sevilla-Noarbe;E. Suchyta;M. Swanson;G. Tarlé;C. B. D. O. Astronomy;U. I. Urbana-Champaign;National Center for Supercomputing Applications;Center for Astrophysical Surveys;H. C. F. Astrophysics;Instituto de F'isica Te'orica;Universidade Estadual Paulista;L. LIneA;F. N. Laboratory;Institute of Cosmology;Gravitation;U. Portsmouth;Cnrs;Umr 7095;I. Paris;Sorbonne Universit'es;06 UPMCUnivParis;F. O. Physics;Ludwig-Maximilians-Universitat;D. PhysicsAstronomy;University College London;Kavli Institute for Particle AstrophysicsCosmology;S. N. Laboratory;Institut de F'isica d'Altes Energies;T. Z. F. O. Science;Technology;O. Nacional;D. Physics;U. Michigan;A. Arbor;H. Sternwarte;U. Hamburg;Centro de Investigaciones Energ'eticas;Medioambientales y Tecnol'ogicas;Iit Hyderabad;Institute of Theoretical Astrophysics;U. Oslo;Instituto de Fisica Teorica Uamcsic;U. A. D. Madrid;I. D. E. D. Catalunya-I.-D.-E.-D.-Catalunya-152160569;Institute of Space Sciences;Campus Uab;S. O. Mathematics;Physics;U. Queensland;Santa Cruz Institute for Particle Physics;Center for Cosmology;Astro-particle Physics;T. O. S. University;Australian Astronomical Optics;M. University;L. Observatory;Centre for Gravitational Astrophysics;College of Materials Science;The Australian National University;T. D. O. Astronomy;Astrophysics;A. N. University;I. C. D. R. I. E. Avanccats-I.-C.-D.-R.-I.-E.-Avanccats-1387885964;P. Department;U. Wisconsin--Madison-U.-Wisconsin--Madison-1387898181;I. O. Astronomy;U. Cambridge;D. Sciences;P. University;Computer Science;M. Division;Oak Ridge National Laboratory;Waldorf High School of Massachusetts Bay
我们利用SDSS、PanSTARRS-1、暗能量调查和Blanco 4M/DECAM专门的跟踪监测，研究了SDSS条纹82区域内190个类星体的光学光度变率，这些类星体在1998年至2020年期间有长期的光度测量覆盖。在每个滤光片平均每类星体200$夜间历元的情况下，我们改进了一个阻尼式随机游走(DRW)模型的参数约束，该模型与以往研究中的光曲线相吻合，基线为10-15年，历元为100个历元。我们发现，随着基线的增加，类星体的平均衰减时间标度继续上升，在这些类星体的20年光曲线中，中位数达到了750天($g$波段)。一些类星体的光曲线可能具有渐进的、长期的趋势，这表明要么DRW拟合需要非常长的基线才能收敛，要么潜在的变化比这些类星体的单个DRW过程更复杂。使用约束较好的类星体子集$tau{rmDRW}$(小于基线的20%)，我们确认弱波长依赖于$tau{rmdrw}\proto\lambda^{0.51\pm0.20}$。我们使用结构函数(SF)和功率谱密度(PSD)分析进一步量化了这些类星体在几天到几十年的时间尺度上的光学可变性。SF和PSD测量定性地确认了从DRW拟合测得的(数百天)衰减时间尺度。然而，对于这些发光类星体来说，在每月小于$sim$的时间尺度上，集合PSD比DRW的PSD更陡峭，并且这个第二突变点与较长的DRW衰减时间尺度相关。
We study the optical $gri$ photometric variability of a sample of 190 quasars within the SDSS Stripe 82 region that have long-term photometric coverage during $\sim 1998-2020$ with SDSS, PanSTARRS-1, the Dark Energy Survey, and dedicated follow-up monitoring with Blanco 4m/DECam. With on average $\sim 200$ nightly epochs per quasar per filter band, we improve the parameter constraints from a Damped Random Walk (DRW) model fit to the light curves over previous studies with 10-15 yr baselines and $\lesssim 100$ epochs. We find that the average damping timescale $\tau_{\rm DRW}$ continues to rise with increased baseline, reaching a median value of $\sim 750$ days ($g$ band) in the rest-frame of these quasars using the 20-yr light curves. Some quasars may have gradual, long-term trends in their light curves, suggesting that either the DRW fit requires very long baselines to converge, or that the underlying variability is more complex than a single DRW process for these quasars. Using a subset of quasars with better-constrained $\tau_{\rm DRW}$ (less than 20\% of the baseline), we confirm a weak wavelength dependence of $\tau_{\rm DRW}\propto \lambda^{0.51\pm0.20}$. We further quantify optical variability of these quasars over days to decades timescales using structure function (SF) and power spectrum density (PSD) analyses. The SF and PSD measurements qualitatively confirm the measured (hundreds of days) damping timescales from the DRW fits. However, the ensemble PSD is steeper than that of a DRW on timescales less than $\sim$ a month for these luminous quasars, and this second break point correlates with the longer DRW damping timescale.