We investigate the contribution of reprocessed continuum emission (1000A - 10,000A) originating in broad line region (BLR) gas, the diffuse continuum (DC), to the wavelength-dependent continuum delays measured in AGN disk reverberation mapping experiments. Assuming a spherical BLR geometry, we adopt a Local Optimally-emitting Cloud (LOC) model for the BLR that approximately reproduces the broad emission-line strengths of the strongest UV lines (Ly-alpha and C IV) in NGC 5548. Within this LOC framework, we explore how assumptions about the gas hydrogen density and column density distributions influence flux and delay spectra of the DC. We find that: (i) models which match well measured emission line luminosities and time delays also produce a significant DC component, (ii) increased nH and/or NH, particularly at smaller BLR radii, result in larger DC luminosities and reduced DC delays, (iii) in a given continuum band the relative importance of the DC component to the measured inter-band delays is proportional (though not 1:1) to its fractional contribution to the total light in that band, (iv) the measured DC delays and DC variability amplitude depends also on the variability amplitude and characteristic variability timescale of the driving continuum, (v) the DC radial surface emissivity distributions F(r) approximate power-laws in radius with indices close to -2 (approximately 1:1 response to variations in the driving continuum flux), thus their physics is relatively simple and less sensitive to the unknown geometry and uncertainties in radiative transfer. Finally, we provide a simple recipe for estimating the DC contribution in disk reverberation mapping experiments.
Evidence of a diffuse, extended continuum source in quasars from the relative sizes of the broad line region and the UV-optical continuum source measured with microlensing
The Sloan Digital Sky Survey Reverberation Mapping Project: Investigation of Continuum Lag Dependence on Broad-Line Contamination and Quasar Properties
Physically motivated AGN emissivity profiles and their effects on quasar microlensing signatures. 1. Multi-epoch accretion disc size inference
IFPU - Institute for Fundamental Physics of the Universe（基础物理宇宙研究所）；SISSA - International School for Advanced Studies（国际高等研究院）；INAF - Osservatorio Astronomico di Trieste（的里雅斯特天文台）；Center for Astrophysics and Cosmology, University of Nova Gorica（新戈里察大学天体物理学与宇宙学中心）
AGN Variability with Rubin Observatory in the 2030s
International Gemini Observatory/NSF NOIRLab（国际双子星天文台/美国国家光学红外天文实验室）；Heidelberg Institute for Theoretical Studies（海德堡理论研究所）；Departamento de Astronomia, Instituto de Física, Universidade Federal do Rio Grande do Sul（南里奥格兰德联邦大学物理学院天文学系）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学卡尔·格利夫天体物理学研究所）；Center for Theoretical Physics, Polish Academy of Sciences（波兰科学院理论物理中心）；Instituto de Astrofísica de Andalucía (IAA-CSIC)（安达卢西亚天体物理学研究所（西班牙高等科学研究委员会））；Istituto Nazionale di Astrofisica, Osservatorio di Padova（意大利国家天体物理研究所帕多瓦观测站）
Emission-Line and Continuum Reverberation Mapping of the NLS1 Galaxy WPVS 48
Institut für Astrophysik und Geophysik, Universität Göttingen（哥廷根大学物理与天体物理研究所）；Department of Physics, Faculty of Natural Sciences, University of Haifa（海法大学自然科学学院物理系）；Haifa Research Center for Theoretical Physics and Astrophysics, University of Haifa（海法大学海法理论物理与天体物理学研究中心）；Ruhr University Bochum, Faculty of Physics and Astronomy, Astronomical Institute (AIRUB)（波鸿鲁尔大学物理与天文学院天文研究所）；School of Physics & Astronomy and the Wise Observatory, Tel-Aviv University（特拉维夫大学物理与天文学院及怀斯天文台）
Broad line regions behind haze: Intrinsic shape of Br$γ$ line and its origin in a type-1 Seyfert galaxy
Kagoshima University, Graduate School of Science and Engineering（鹿儿岛大学理工学部）；Ehime University, Research Center for Space and Cosmic Evolution（爱媛大学宇宙演化研究中心）；Hokkaido University, Faculty of Science（北海道大学理学部）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）；De La Salle University（德拉萨大学）；Kavli Institute for Astronomy and Astrophysics at Peking University（北京大学科维理天文与天体物理研究所）
The unusually red delay spectrum of the low-mass black hole AGN NGC\,4051 as revealed by intensive continuum reverberation mapping with the Las Cumbres Observatory
Wayne State University（韦恩州立大学）；University of St Andrews（圣安德鲁斯大学）；Durham University（杜伦大学）；Spectral Sciences Inc.（光谱科学公司）；University of Johannesburg（约翰内斯堡大学）；University of California, Irvine（加州大学尔湾分校）；University of Leicester（莱斯特大学）
NGC 4051低质量黑洞的异常红色延迟光谱通过密集连续反照率测绘揭示，其i和z_s波段延迟显著超出预期，可能由尘埃reddening或连续贡献解释。
