We consider photometric reverberation mapping, where the nuclear continuum variations are monitored via a broad-band filter and the echo of emission line clouds of the broad line region (BLR) is measured with a suitable narrow-band (NB) filter. We investigate how an incomplete emission-line coverage by the NB filter influences the BLR size determination. This includes two basic cases: 1) a symmetric cut of the blue and red part of the line wings, and 2) the filter positioned asymmetrically to the line centre so that essentially a complete half of the emission line is contained in the NB filter. Under the assumption that the BLR size is dominated by circular Keplerian orbits, we find that symmetric cutting of line wings may lead to overestimating the BLR size by less than 5%. The case of asymmetric half-line coverage, similar as for our data of the Seyfert 1 galaxy 3C120, yields the BLR size with a bias of less than 1%. Our results suggest that any BLR size bias due to narrow-band line cut in photometric reverberation mapping is small and in most cases negligible. We used well sampled photometric reverberation mapping light curves with sharp variation features in both the continuum and the Hbeta light curves to determine the geometry type of the Hbeta BLR for 3C120. Modelling of the light curve, under the assumption that the BLR is essentially virialised, argues against a spherical geometry and favours a nearly face-on disk-like geometry with inclination i = 10 +/- 4 deg and extension from 22 to 28 light days. The low inclination may lead to a larger black hole mass than the derived when using the average geometry scaling factor f=5.5. We discuss deviations of Seyfert 1 galaxies from the M_BH - sigma relation.
HALO I: Photometric continuum reverberation mapping of Fairall 9
Center for Theoretical Physics, Polish Academy of Sciences（波兰科学院理论物理中心）；Heidelberg Institute for Theoretical Studies（海德堡理论研究所）；Institut d’Astrophysique et de Géophysique, Université de Liège（列日大学天体物理学与地球物理研究所）；International Gemini Observatory/NSF NOIRLab（国际双子座天文台/NSF NOIRLab）；Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文中心）；Universidad de Concepción（孔塞普西翁大学）；Aryabhatta Research Institute of Observational Sciences（阿亚波达观测科学研究所）；Department of Applied Physics/Physics, Mahatma Jyotiba Phule Rohilkhand University（马哈特玛·乔蒂巴·富勒罗希尔坎德大学应用物理/物理系）；Department of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk University（马萨里克大学理学院理论与天体物理学系）
Mass of the black hole in the Seyfert 1.5 galaxy H 0507+164 from reverberation mapping
我们提出了我们的X射线源H 0507+164，一个低光度塞弗特1.5星系在红移z = 0.018的光学监测活动的结果。光谱观测在2007年11月21日至12月26日的22个夜晚进行。在同一时期还获得了13个夜晚的R波段光度观测。在我们的监测期间，发现银河系的连续谱和宽线通量发生了变化。R波段相对于伴星的微分光变曲线也显示出类似的变化。使用互相关分析，我们估计的时间延迟为3.01天（在休息帧），在5100埃的光学连续谱中的变化的宽H-β线通量的响应。利用这个时间延迟和H β谱线的宽度，我们估计宽线区（BLR）的半径为2.53 x 10^{-3}秒差距，黑洞的质量为9.62 x 10^{6}太阳质量。
The Lick AGN Monitoring Project: Photometric Light Curves and Optical Variability Characteristics
Lick AGN监测项目以13个邻近的Seyfert 1星系为目标，目的是使用反射映射来测量它们中央黑洞的质量。样本包括12个被选中的星系，它们的黑洞质量大约在10^6-10^7太阳质量之间，以及经过充分研究的AGN NGC 5548。结合光谱监测活动，我们从2008年2月到2008年5月的大多数夜晚获得了宽带B和V图像。成像观测由四台望远镜进行：0.76米卡茨曼自动成像望远镜（KAIT）、2米多色活动星系核监测望远镜（MAGNUM）、帕洛玛60英寸（1.5米）望远镜和0.80米特纳格拉II望远镜。在几个月的时间里获得良好采样的光变曲线对于获得宽线混响滞后和黑洞质量是有用的，也使我们能够检查连续谱可变性的特征。本文讨论了活动星系核的观测方法和光度测量，给出了活动星系核的连续光变曲线。我们测量每个光变曲线的各种变化特性。我们没有发现B波段和V波段变化之间存在时滞的任何证据，也没有发现我们样本中活动星系核的显着颜色变化。
Discovery of a Luminosity-dependent Continuum Lag in NGC 4151 from Photometric and Spectroscopic Continuum Reverberation Mapping
Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences（中国科学院天体结构与演化重点实验室）；Center for Astronomical Mega-Science, Chinese Academy of Sciences（中国科学院天文大科学研究中心）；Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences（中国科学院射电天文与技术重点实验室）；Department of Astronomy, Xiamen University（厦门大学天文学系）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（IEE-CSIC））；Jeremiah Horrocks Institute, University of Central Lancashire（中央兰开夏大学杰里迈亚·霍罗克斯研究所）；School of Physics and Astronomy, Sun Yat-sen University（中山大学物理与天文学院）；CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area（粤港澳大湾区空间站科学中心）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）
Effects of heterogeneous data sets and time-lag measurement techniques on cosmological parameter constraints from MgII and CIV reverberation-mapped quasar data
The Radius-Luminosity Relationship for Active Galactic Nuclei with Hierarchical Bayesian Reverberation Mapping
University of Queensland（昆士兰大学）；Macquarie University（麦考瑞大学）；Astrophysics and Space Technologies Research Centre, Macquarie University（麦考瑞大学天体物理与空间技术中心）；The Ohio State University（俄亥俄州立大学）；Kavli Institute for Particle Astrophysics and Cosmology, Stanford University（斯坦福大学卡弗里粒子天体物理学与宇宙学研究所）；Australian National University（澳大利亚国立大学）；Sydney Institute for Astronomy, School of Physics, A28, University of Sydney（悉尼大学A28物理学院悉尼天文研究所）
BayeSN $\times$ Dovekie: Joint Photometric Cross-calibration and SED Modelling of Type Ia Supernovae
Institute of Astronomy and Kavli Institute for Cosmology, University of Cambridge（剑桥大学天体物理研究所与卡弗里宇宙学研究所）；School of Physics and Astronomy, University of Southampton（南安普顿大学物理与天文学院）
