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Start Over Author "Xue, Yongquan" Topic fos: physical sciences
12 results on '"Xue, Yongquan"'

1. [OIII] 5007A Emission Line Width as a Surrogate for stellar dispersion in Type 1 AGNs?

Author

Le, Huynh Anh N., Xue, Yongquan, Lin, Xiaozhi, and Wang, Yijun

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract

We present a study of the relation between the [OIII] 5007A emission line width (sigma_{[OIII]}) and stellar velocity dispersion (sigma_{*}), utilizing a sample of 740 type 1 active galactic nuclei (AGNs) with high-quality spectra at redshift z < 1.0. We find the broad correlation between the core component of [OIII] emission line width (sigma_{[OIII,core]}) and sigma_{*} with a scatter of 0.11~dex for the low redshift (z < 0.1) sample; for redshift (0.3 < z < 1.0) AGNs, the scatter is larger, being 0.16~dex. We also find that the Eddington ratio (L_{bol}/L_{Edd}) may play an important role in the discrepancies between sigma_{[OIII,core]} and sigma_{*}. As the L_{bol}/L_{Edd} increases, sigma_{[OIII,core]} tends to be larger than sigma_{*}. By classifying our local sample with different minor-to-major axis ratios, we find that sigma_{*} is larger than sigma_{[OIII,core]} for those edge-on spiral galaxies. In addition, we also find that the effects of outflow strength properties such as maximum outflow velocity (V_{max}) and the broader component of [OIII] emission line width and line shift (sigma_{[OIII,out]} and V_{[OIII,out]}) may play a major role in the discrepancies between sigma_{[OIII,core]} and sigma_{*}. The discrepancies between sigma_{[OIII,core]} and sigma_{*} are larger when V_{max}, V_{[OIII,out]}, and sigma_{[OIII,out]} increase. Our results show that the outflow strengths may have significant effects on the differences between narrow-line region gas and stellar kinematics in AGNs. We suggest that caution should be taken when using sigma_{[OIII,core]} as a surrogate for sigma_{*}. In addition, the substitute of sigma_{[OIII,core]} for sigma_{*} could be used only for low luminosity AGNs., 17 pages, Accepted for publication in ApJ

Published
2023

2. Scientific Objectives of the Hot Universe Baryon Surveyor (HUBS) Mission

Author

Bregman, Joel, Cen, Renyue, Chen, Yang, Cui, Wei, Fang, Taotao, Guo, Fulai, Hodges-Kluck, Edmund, Huang, Rui, Ho, Luis C., Ji, Li, Ji, Suoqing, Kang, Xi, Lai, Xiaoyu, Li, Hui, Li, Jiangtao, Li, Miao, Li, Xiangdong, Li, Yuan, Li, Zhaosheng, Liang, Guiyun, Liu, Helei, Liu, Wenhao, Lu, Fangjun, Mao, Junjie, Ponti, Gabriele, Qu, Zhijie, Shan, Chenxi, Shao, Lijing, Shi, Fangzheng, Shu, Xinwen, Sun, Lei, Sun, Mouyuan, Tong, Hao, Wang, Junfeng, Wang, Junxian, Wang, Q. Daniel, Wang, Song, Wang, Tinggui, Wang, Weiyang, Wang, Zhongxiang, Xu, Dandan, Xu, Haiguang, Xu, Heng, Xu, Renxin, Xu, Xiaojie, Xue, Yongquan, Yang, Hang, Yuan, Feng, Zhang, Shuinai, Zhang, Yuning, Zhang, Zhongli, Zhao, Yuanyuan, Zhou, Enping, and Zhou, Ping

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Hot Universe Baryon Surveyor (HUBS) is a proposed space-based X-ray telescope for detecting X-ray emissions from the hot gas content in our universe. With its unprecedented spatially-resolved high-resolution spectroscopy and large field of view, the HUBS mission will be uniquely qualified to measure the physical and chemical properties of the hot gas in the interstellar medium, the circumgalactic medium, the intergalactic medium, and the intracluster medium. These measurements will be valuable for two key scientific goals of HUBS, namely to unravel the AGN and stellar feedback physics that governs the formation and evolution of galaxies, and to probe the baryon budget and multi-phase states from galactic to cosmological scales. In addition to these two goals, the HUBS mission will also help us solve some problems in the fields of galaxy clusters, AGNs, diffuse X-ray backgrounds, supernova remnants, and compact objects. This paper discusses the perspective of advancing these fields using the HUBS telescope., Comment: 52 pages, 22 figures. Accepted for publication in Science China: Physics, Mechanics and Astronomy

Published
2023
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3. Investigation of Stellar Kinematics and Ionized gas Outflows in Local (U)LIRGs

Author

Ayubinia, Ashraf, Xue, Yongquan, Le, Huynh Anh Nguyen, Zou, Fan, Wang, Shu, He, Zhicheng, and Eser, Ece Kilerci

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract

We explore properties of stellar kinematics and ionized gas in a sample of 1106 local (U)LIRGs from the AKARI telescope. We combine data from $Wide-field\ Infrared\ Survey\ Explorer$ (WISE) and Sloan Digital Sky Survey (SDSS) Data Release 13 (DR13) to fit the spectral energy distribution (SED) of each source to constrain the contribution of active galactic nuclei (AGNs) to the total IR luminosity and estimate physical parameters such as stellar mass and star-formation rate (SFR). We split our sample into AGNs and weak/non-AGNs. We find that our sample is considerably above the main sequence. The highest SFRs and stellar masses are associated with ULIRGs. We also fit the H$\beta$ and H$\alpha$ regions to characterize the outflows. We find that the incidence of ionized gas outflows in AGN (U)LIRGs ($\sim$ 72\%) is much higher than that in weak/non-AGN ones ($\sim$ 39\%). The AGN ULIRGs have extreme outflow velocities (up to $\sim$ 2300 km s$^{-1}$) and high mass-outflow rates (up to $\sim$ 60 \solarm~yr$^{-1}$). Our results suggest that starbursts are insufficient to produce such powerful outflows. We explore the correlations of SFR and specific SFR (sSFR) with ionized gas outflows. We find that AGN hosts with the highest SFRs exhibit a negative correlation between outflow velocity and sSFR. Therefore, in AGNs containing large amounts of gas, the negative feedback scenario might be suggested., Comment: revised version for typos, errors in captions of figures 3,4 and 11 fixed, accepted by ApJ

Published
2023
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4. Sciences for The 2.5-meter Wide Field Survey Telescope (WFST)

Author

WFST Collaboration, Wang, Tinggui, Liu, Guilin, Cai, Zhenyi, Gen, Jinjun, Fang, Min, He, Haoning, Jiang, Ji-an, Jiang, Ning, Kong, Xu, Li, Bin, Li, Ye, Luo, Wentao, Pan, Zhizheng, Wu, Xuefeng, Yang, Ji, Yu, Jiming, Zheng, Xianzhong, Zhu, Qingfeng, Cai, Yi-Fu, Chen, YuanYuan, Chen, Zhiwei, Dai, Zigao, Fan, Lulu, Fan, Yizhong, Fang, Wenjuan, He, Zhicheng, Hu, Lei, Hu, Maokai, Jin, Zhiping, Jiang, Zhibo, Li, Guoliang, Li, Fan, Li, Xuzhi, Liang, Runduo, Lin, Zheyu, Liu, Qingzhong, Liu, Wenhao, Liu, Zhengyan, Liu, Wei, Liu, Yao, Lou, Zheng, Qu, Han, Sheng, Zhenfeng, Shi, Jianchun, Shu, Yiping, Su, Zhenbo, Sun, Tianrui, Wang, Hongchi, Wang, Huiyuan, Wang, Jian, Wang, Junxian, Wei, Daming, Wei, Junjie, Xue, Yongquan, Yan, Jingzhi, Yang, Chao, Yuan, Ye, Yuan, Yefei, Zhang, Hongxin, Zhang, Miaomiao, Zhao, Haibin, and Zhao, Wen

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The Wide Field Survey Telescope (WFST) is a dedicated photometric survey facility under construction jointly by the University of Science and Technology of China and Purple Mountain Observatory. It is equipped with a primary mirror of 2.5m in diameter, an active optical system, and a mosaic CCD camera of 0.73 Gpix on the main focus plane to achieve high-quality imaging over a field of view of 6.5 square degrees. The installation of WFST in the Lenghu observing site is planned to happen in the summer of 2023, and the operation is scheduled to commence within three months afterward. WFST will scan the northern sky in four optical bands (u, g, r, and i) at cadences from hourly/daily to semi-weekly in the deep high-cadence survey (DHS) and the wide field survey (WFS) programs, respectively. WFS reaches a depth of 22.27, 23.32, 22.84, and 22.31 in AB magnitudes in a nominal 30-second exposure in the four bands during a photometric night, respectively, enabling us to search tremendous amount of transients in the low-z universe and systematically investigate the variability of Galactic and extragalactic objects. Intranight 90s exposures as deep as 23 and 24 mag in u and g bands via DHS provide a unique opportunity to facilitate explorations of energetic transients in demand for high sensitivity, including the electromagnetic counterparts of gravitational-wave events detected by the second/third-generation GW detectors, supernovae within a few hours of their explosions, tidal disruption events and luminous fast optical transients even beyond a redshift of 1. Meanwhile, the final 6-year co-added images, anticipated to reach g about 25.5 mag in WFS or even deeper by 1.5 mag in DHS, will be of significant value to general Galactic and extragalactic sciences. The highly uniform legacy surveys of WFST will also serve as an indispensable complement to those of LSST which monitors the southern sky., Comment: 46 pages, submitted to SCMPA

Published
2023
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5. The $\textit{NuSTAR}$ Extragalactic Surveys: Source Catalogs from the Extended $\textit{Chandra}$ Deep Field-South and the $\textit{Chandra}$ Deep Field-North

Author

Zhang, Tianyi and Xue, Yongquan

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

We present a routinized and reliable method to obtain source catalogs from the $\textit{Nuclear Spectroscopic Telescope Array}$ ($\textit{NuSTAR}$) extragalactic surveys of the Extended $\textit{Chandra}$ Deep Field-South (E-CDF-S) and $\textit{Chandra}$ Deep Field-North (CDF-N). The $\textit{NuSTAR}$ E-CDF-S survey covers a sky area of $\approx30'\times30'$ to a maximum depth of $\sim$ 230 ks corrected for vignetting in the 3--24 keV band, with a total of 58 sources detected in our E-CDF-S catalog; the $\textit{NuSTAR}$ CDF-N survey covers a sky area of $\approx7'\times10'$ to a maximum depth of $\sim$ 440 ks corrected for vignetting in the 3--24 keV band, with a total of 42 sources detected in our CDF-N catalog that is produced for the first time. We verify the reliability of our two catalogs by crossmatching them with the relevant catalogs from the $\textit{Chandra}$ X-ray observatory, and find that the fluxes of our $\textit{NuSTAR}$ sources are generally consistent with that of their $\textit{Chandra}$ counterparts. Our two catalogs are produced following the exactly same method and made publicly available, thereby providing a uniform platform that facilitates further studies involving these two fields. Our source-detection method provides a systematic approach for source cataloging in other $\textit{NuSTAR}$ extragalactic surveys., Comment: 26 pages, 7 figures, accepted for publication in JUSTC; click "Full text" & "Supplements" for catalogs in https://doi.org/10.52396/JUSTC-2023-0032

Published
2023
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6. Identification and Characterization of a Large Sample of Distant Active Dwarf Galaxies in XMM-SERVS

Author

Zou, Fan, Brandt, W. N., Ni, Qingling, Zhu, Shifu, Alexander, David M., Bauer, Franz E., Chen, Chien-Ting J., Luo, Bin, Sun, Mouyuan, Vignali, Cristian, Vito, Fabio, Xue, Yongquan, and Yan, Wei

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract

Active dwarf galaxies are important because they contribute to the evolution of dwarf galaxies and can reveal their hosted massive black holes. However, the sample size of such sources beyond the local universe is still highly limited. In this work, we search for active dwarf galaxies in the recently completed XMM-Spitzer Extragalactic Representative Volume Survey (XMM-SERVS). XMM-SERVS is currently the largest medium-depth X-ray survey covering 13 $\mathrm{deg}^2$ in three extragalactic fields, which all have well-characterized multi-wavelength information. After considering several factors that may lead to misidentifications, we identify 73 active dwarf galaxies at $z, 34 pages, 21 figures, 6 tables, accepted for publication in ApJ

Published
2023
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7. Accretion in strong field gravity with eXTP

Author

De Rosa, Alessandra, Uttley, Phil, Gou, Lijun, Liu, Yuan, Bambi, Cosimo, Barret, Didier, Belloni, Tomaso, Berti, Emanuele, Bianchi, Stefano, Caiazzo, Ilaria, Casella, Piergiorgio, Feroci, Marco, Ferrari, Valeria, Gualtieri, Leonardo, Heyl, Jeremy, Ingram, Adam, Karas, Vladimir, Lu, Fangjun, Luo, Bin, Matt, Giorgio, Motta, Sara, Neilsen, Joseph, Pani, Paolo, Santangelo, Andrea, Shu, Xinwen, Wang, Junfeng, Wang, Jian-Min, Xue, Yongquan, Xu, Yupeng, Yuan, Weimin, Yuan, Yefei, Zhang, Shuang-Nan, Zhang, Shu, Agudo, Ivan, Amati, Lorenzo, Andersson, Nils, Baglio, Cristina, Bakala, Pavel, Baykal, Altan, Bhattacharyya, Sudip, Bombaci, Ignazio, Bucciantini, Niccolò, Capitanio, Fiamma, Ciolfi, Riccardo, Cui, Wei K., D'Ammando, Filippo, Dauser, Thomas, Del Santo, Melania, De Marco, Barbara, Di Salvo, Tiziana, Done, Chris, Dovčiak, Michal, Fabian, Andrew C., Falanga, Maurizio, Gambino, Angelo Francesco, Gendre, Bruce, Grinberg, Victoria, Heger, Alexander, Homan, Jeroen, Iaria, Rosario, Jiang, Jiachen, Jin, Chichuan, Koerding, Elmar, Linares, Manu, Liu, Zhu, Maccarone, Thomas J., Malzac, Julien, Manousakis, Antonios, Marin, Frédéric, Marinucci, Andrea, Mehdipour, Missagh, Méndez, Mariano, Migliari, Simone, Miller, Cole, Miniutti, Giovanni, Nardini, Emanuele, O'Brien, Paul T., Osborne, Julian P., Petrucci, Pierre Olivier, Possenti, Andrea, Riggio, Alessandro, Rodriguez, Jerome, Sanna, Andrea, Shao, Lijing, Sobolewska, Malgosia, Sramkova, Eva, Stevens, Abigail L., Stiele, Holger, Stratta, Giulia, Stuchlik, Zdenek, Svoboda, Jiri, Tamburini, Fabrizio, Tauris, Thomas M., Tombesi, Francesco, Török, Gabriel, Urbanec, Martin, Vincent, Frederic, Wu, Qingwen, Yuan, Feng, in't Zand, Jean J. M., Zdziarski, Andrzej A., Zhou, Xinlin, Rosa, Alessandra De, Cui, Wei, D’Ammando, Filippo, Fabian, Andrew, Maccarone, Thomas, O’Brien, Paul, Osborne, Julian, Stevens, Abigail, Tauris, Thomas, in’ t Zand, Jean, Zdziarski, Andrzej, School of Physics and Astronomy [Southampton], University of Southampton, Sécurité des Données et des Systèmes (SDS), Laboratoire d'Informatique Fondamentale d'Orléans (LIFO), Université d'Orléans (UO)-Institut National des Sciences Appliquées - Centre Val de Loire (INSA CVL), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université d'Orléans (UO)-Institut National des Sciences Appliquées - Centre Val de Loire (INSA CVL), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Fudan University [Shanghai], Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Osservatorio Astronomico di Brera, Istituto Nazionale di Astrofisica (INAF), Department of Physics and Astronomy [U Mississippi], The University of Mississippi [Oxford], IASF, Area di Ricerca di Tor Vergata, Astronomical Institute of the Czech Academy of Sciences, Czech Academy of Sciences [Prague] (ASCR), Key Laboratory of Western China's Environmental Systems (Ministry of Education), Lanzhou University, Dipartimento de Fisica Roma Tre (DF-Roma3), Università degli Studi Roma Tre, Sichuan University, U.S. Department of Energy (DOE), Medical School (University of Nanjing), Nanjing University (NJU), Faculty of Philosophy and Science, Silesian University in Opava, INAF - Osservatorio Astrofisico di Arcetri (OAA), Instituto di Astrofisica (IASF), Consiglio Nazionale delle Ricerche (CNR), Istituto di Radioastronomia (IRA), Department of Physics, Durham University, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Eberhard Karls Universität Tübingen, State Key Laboratory of Magnetic Resonance and Atomic and Molecular Physics, Wuhan Institute of Physics and Mathematics, Chinese Academy of Sciences, Wuhan, 430071 China, Chinese Academy of Sciences [Wuhan Branch], Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), Biogéosciences [UMR 6282] [Dijon] (BGS), Centre National de la Recherche Scientifique (CNRS)-Université de Bourgogne (UB)-AgroSup Dijon - Institut National Supérieur des Sciences Agronomiques, de l'Alimentation et de l'Environnement, European Space Astronomy Centre (ESAC), European Space Agency (ESA), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Cagliari (OAC), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Ethoikos, Radicondoli, ASI Science Data Center (ASDC), Italian Space Agency, Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Technologie de Belfort-Montbeliard (UTBM), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Applied Biology and Chemical Technology, The Hong Kong Polytechnic University [Hong Kong] (POLYU), Max-Planck-Institut für Radioastronomie (MPIFR), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), eXTP, Institut National des Sciences Appliquées - Centre Val de Loire (INSA CVL), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université d'Orléans (UO), Université de Bourgogne (UB)-AgroSup Dijon - Institut National Supérieur des Sciences Agronomiques, de l'Alimentation et de l'Environnement-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institute of High Energy Physics [Beijing], Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Brera (OAB), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Università degli Studi Roma Tre = Roma Tre University (ROMA TRE), Sichuan University [Chengdu] (SCU), U.S. Department of Energy [Washington] (DOE), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Istituto di Radioastronomia [Bologna] (IRA), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Biogéosciences [UMR 6282] (BGS), Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), De Rosa, Alessandra, Uttley, Phil, Gou, LiJun, Liu, Yuan, Bambi, Cosimo, Barret, Didier, Belloni, Tomaso, Berti, Emanuele, Bianchi, Stefano, Caiazzo, Ilaria, Casella, Piergiorgio, Feroci, Marco, Ferrari, Valeria, Gualtieri, Leonardo, Heyl, Jeremy, Ingram, Adam, Karas, Vladimir, Lu, FangJun, Luo, Bin, Matt, Giorgio, Motta, Sara, Neilsen, Joseph, Pani, Paolo, Santangelo, Andrea, Shu, XinWen, Wang, JunFeng, Wang, Jian-Min, Xue, YongQuan, Xu, YuPeng, Yuan, WeiMin, Yuan, YeFei, Zhang, Shuang-Nan, Zhang, Shu, Agudo, Ivan, Amati, Lorenzo, Andersson, Nil, Baglio, Cristina, Bakala, Pavel, Baykal, Altan, Bhattacharyya, Sudip, Bombaci, Ignazio, Bucciantini, Niccoló, Capitanio, Fiamma, Ciolfi, Riccardo, Cui, Wei K., D’Ammando, Filippo, Dauser, Thoma, Del Santo, Melania, De Marco, Barbara, Di Salvo, Tiziana, Done, Chri, Dovčiak, Michal, Fabian, Andrew C., Falanga, Maurizio, Gambino, Angelo Francesco, Gendre, Bruce, Grinberg, Victoria, Heger, Alexander, Homan, Jeroen, Iaria, Rosario, Jiang, JiaChen, Jin, ChiChuan, Koerding, Elmar, Linares, Manu, Liu, Zhu, Maccarone, Thomas J., Malzac, Julien, Manousakis, Antonio, Marin, Frédéric, Marinucci, Andrea, Mehdipour, Missagh, Méndez, Mariano, Migliari, Simone, Miller, Cole, Miniutti, Giovanni, Nardini, Emanuele, O’Brien, Paul T., Osborne, Julian P., Petrucci, Pierre Olivier, Possenti, Andrea, Riggio, Alessandro, Rodriguez, Jerome, Sanna, Andrea, Shao, LiJing, Sobolewska, Malgosia, Sramkova, Eva, Stevens, Abigail L., Stiele, Holger, Stratta, Giulia, Stuchlik, Zdenek, Svoboda, Jiri, Tamburini, Fabrizio, Tauris, Thomas M., Tombesi, Francesco, Torok, Gabriel, Urbanec, Martin, Vincent, Frederic, Wu, QingWen, Yuan, Feng, in’ t Zand, Jean J. M., Zdziarski, Andrzej A., Zhou, XinLin, ITA, USA, GBR, FRA, DEU, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Chinese Academy of Sciences (CAS), National Science Centre, Poland (NCN), High Energy Astrophys. & Astropart. Phys (API, FNWI), Rosa, Alessandra De, Gou, Lijun, Lu, Fangjun, Shu, Xinwen, Wang, Junfeng, Xue, Yongquan, Xu, Yupeng, Yuan, Weimin, Yuan, Yefei, Jiang, Jiachen, Jin, Chichuan, Shao, Lijing, Wu, Qingwen, and Zhou, Xinlin

Subjects
ACTIVE GALACTIC NUCLEI, Accretion, accretion, black holes physics, X-ray, Physics and Astronomy (all), black holes physic, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Black holes physics, Polarimetry, FOS: Physical sciences, BLACK-HOLE SPIN, General Physics and Astronomy, Strong field, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, ELECTROMAGNETIC EMISSION, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), XMM-NEWTON, Physics, LENS-THIRRING PRECESSION, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], QUASI-PERIODIC OSCILLATIONS, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], IRON K, Accretion (astrophysics), X ray, [SDU]Sciences of the Universe [physics], ULTRA-FAST OUTFLOWS, Astrophysics::Earth and Planetary Astrophysics, SPECTRAL FEATURES, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], X-RAY BINARIES
Abstract

In this paper we describe the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to accretion flows in the strong field gravity regime around both stellar-mass and supermassive black-holes. eXTP has the unique capability of using advanced 'spectral-timing-polarimetry' techniques to analyze the rapid variations with three orthogonal diagnostics of the flow and its geometry, yielding unprecedented insight into the inner accreting regions, the effects of strong field gravity on the material within them and the powerful outflows which are driven by the accretion process., Accepted for publication on Sci. China Phys. Mech. Astron. (2019)

Published
2019
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8. The XMM-SERVS Survey: XMM-Newton Point-source Catalogs for the W-CDF-S and ELAIS-S1 Fields

Author

Ni, Qingling, Brandt, W. N., Chen, Chien-Ting, Luo, Bin, Nyland, Kristina, Yang, Guang, Zou, Fan, Aird, James, Alexander, David M., Bauer, Franz Erik, Lacy, Mark, Lehmer, Bret D., Mallick, Labani, Salvato, Mara, Schneider, Donald P., Tozzi, Paolo, Traulsen, Iris, Vaccari, Mattia, Vignali, Cristian, Vito, Fabio, Xue, Yongquan, Banerji, Manda, Chow, Kate, Comastri, Andrea, Del Moro, Agnese, Gilli, Roberto, Mullaney, James, Paolillo, Maurizio, Schwope, Axel, Shemmer, Ohad, Sun, Mouyuan, Timlin, John D., III, Trump, Jonathan R., Ni Q., Brandt W.N., Chen C.-T., Luo B., Nyland K., Yang G., Zou F., Aird J., Alexander D.M., Bauer F.E., Lacy M., Lehmer B.D., Mallick L., Salvato M., Schneider D.P., Tozzi P., Traulsen I., Vaccari M., Vignali C., Vito F., Xue Y., Banerji M., Chow K., Comastri A., Del Moro A., Gilli R., Mullaney J., Paolillo M., Schwope A., Shemmer O., Sun M., Timlin Iii J.D., Trump J.R., Ni, Qingling, Brandt, W. N., Chen, Chien-Ting, Luo, Bin, Nyland, Kristina, Yang, Guang, Zou, Fan, Aird, Jame, Alexander, David M., Bauer, Franz Erik, Lacy, Mark, Lehmer, Bret D., Mallick, Labani, Salvato, Mara, Schneider, Donald P., Tozzi, Paolo, Traulsen, Iri, Vaccari, Mattia, Vignali, Cristian, Vito, Fabio, Xue, Yongquan, Banerji, Manda, Chow, Kate, Comastri, Andrea, Del Moro, Agnese, Gilli, Roberto, Mullaney, Jame, Paolillo, Maurizio, Schwope, Axel, Shemmer, Ohad, Sun, Mouyuan, Timlin, John, D., Iii, and Trump, Jonathan R.

Subjects
Physics, Active galactic nuclei, Active galactic nucleus, X-ray active galactic nuclei, Point source, astro-ph.GA, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Active galaxie, X-ray surveys, Catalogs, Surveys, Active galactic nuclei, Active galaxies, X-ray active galactic nuclei, X-ray point sources, X-ray quasars, X-ray surveys, 205, 1671, 16, 17, 2035, 1270, 1821, 1824, Astrophysics - Astrophysics of Galaxies, Catalog, X-ray quasar, Survey, X-ray point sources)
Abstract

We present the X-ray point-source catalogs in two of the XMM-Spitzer Extragalactic Representative Volume Survey (XMM-SERVS) fields, W-CDF-S (4.6 deg$^2$) and ELAIS-S1 (3.2 deg$^2$), aiming to fill the gap between deep pencil-beam X-ray surveys and shallow X-ray surveys over large areas. The W-CDF-S and ELAIS-S1 regions were targeted with 2.3 Ms and 1.0 Ms of XMM-Newton observations, respectively; 1.8 Ms and 0.9 Ms exposures remain after flare filtering. The survey in W-CDF-S has a flux limit of 1.0 $\times$ 10$^{-14}$ erg cm$^{-2}$ s$^{-1}$ over 90% of its area in the 0.5-10 keV band; 4053 sources are detected in total. The survey in ELAIS-S1 has a flux limit of 1.3 $\times$ 10$^{-14}$ erg cm$^{-2}$ s$^{-1}$ over 90% of its area in the 0.5-10 keV band; 2630 sources are detected in total. Reliable optical-to-IR multiwavelength counterpart candidates are identified for $\approx$ 89% of the sources in W-CDF-S and $\approx$ 87% of the sources in ELAIS-S1. 3186 sources in W-CDF-S and 1985 sources in ELAIS-S1 are classified as AGNs. We also provide photometric redshifts for X-ray sources; $\approx$ 84% of the 3319/2001 sources in W-CDF-S/ELAIS-S1 with optical-to-NIR forced photometry available have either spectroscopic redshifts or high-quality photometric redshifts. The completion of the XMM-Newton observations in the W-CDF-S and ELAIS-S1 fields marks the end of the XMM-SERVS survey data gathering. The $\approx$ 12,000 point-like X-ray sources detected in the whole $\approx$ 13 deg$^2$ XMM-SERVS survey will benefit future large-sample AGN studies., 40 pages, 35 figures. Accepted for publication in ApJS. Data products available at: https://personal.psu.edu/wnb3/xmmservs/xmmservs.html

Published
2021

9. Mapping the Inner Structure of Quasars with Time-Domain Spectroscopy

Author

Shen, Yue, Anderson, Scott, Berger, Edo, Brandt, W. N., De Rosa, Gisella, Fan, Xiaohui, Ferrarese, Laura, Gezari, Suvi, Graham, Matthew, Greene, Jenny, Grier, Catherine J., Grindlay, Josh, Haggard, Daryl, Hall, Patrick B., Ho, Luis, Medel, Hector Ibarra, Ilic, Dragana, Ivezic, Zeljko, Jencson, Jacob, Jiang, Linhua, Juneau, St��phanie, Kasliwal, Mansi, Kollmeier, Juna, Kutyrev, Alexander, Li, Jennifer I-Hsiu, Liu, Guilin, Liu, Xin, MacLeod, Chelsea, Melnick, Gary, Metzger, Brian, Myers, Adam D., O'Dea, Christopher, Petric, Andreea, Popovi��, Luka ��., Prakash, Abhishek, Purcell, Bill, Richards, Gordon T., Rieke, George, Tanvir, Nial, Trakhtenbrot, Benny, Wood-Vasey, Michael, Xue, Yongquan, and Yang, Qian

Subjects
Astrophysics of Galaxies (astro-ph.GA), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

The ubiquitous variability of quasars across a wide range of wavelengths and timescales encodes critical information about the structure and dynamics of the circumnuclear emitting regions that are too small to be directly resolved, as well as detailed underlying physics of accretion and feedback processes in these active supermassive black holes. We emphasize the importance of studying quasar variability with time-domain spectroscopy, focusing on two science cases: (1) reverberation mapping (RM) to measure the broad-line region sizes and black hole masses in distant quasars; (2) spectroscopic follow-up of extreme variability quasars that dramatically change their continuum and broad-line flux within several years. We highlight the need for dedicated optical-infrared spectroscopic survey facilities in the coming decades to accompany wide-area time-domain imaging surveys, including: (1) the next phase of the Sloan Digital Sky Survey (SDSS-V; ~2020-2025), an all-sky, time-domain multi-object spectroscopic survey with 2.5m-class telescopes; (2) the planned Maunakea Spectroscopic Explorer, a dedicated 10m-class spectroscopic survey telescope with a 1.5 sq. deg field-of-view and multiplex of thousands of fibers in both optical and near-IR (J+H) to begin operations in 2029; (3) the Time-domain Spectroscopic Observatory (TSO), a proposed Probe-class ~1.3m telescope at L2, with imaging and spectroscopy (R=200, 1800) in 4 bands (0.3 - 5 micron) and rapid slew capability to 90% of sky, which will extend the coverage of Hbeta to z=8., Science White Paper for the US Astro 2020 Decadal Survey

Published
2019

10. High Redshift Obscured Quasars and the Need for Optical to NIR, Massively Multiplexed, Spectroscopic Facilities

Author

Petric, Andreea, Lacy, Mark, Juneau, Stéphanie, Shen, Yue, Fan, Xiaohui, Flagey, Nicolas, Gordon, Yjan, Haggard, Daryl, Hall, Patrick B., Hathi, Nimish, Ilic, Dragana, Lagos, Claudia D. P., Liu, Xin, O'Dea, Christopher, Popović, Luka, Sheinis, Andy, Wang, Yiping, and Xue, Yongquan

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

Most bulge-dominated galaxies host black holes with masses that tightly correlate with the masses of their bulges. This may indicate that the black holes may regulate galaxy growth or vice versa, or that they may grow in lock-step. The quest to understand how, when, and where those black-holes formed motivates much of extragalactic astronomy. Here we focus on a population of galaxies with active black holes in their nuclei (active galactic nuclei or AGN), that are fully or partially hidden by dust and gas: the emission from the broad line region is either completely or partially obscured with a visual extinction of 1 or above. This limit, though not yet precise, appears to be the point at which the populations of AGN may evolve differently. We highlight the importance of finding and studying those dusty AGN at redshifts between 1 and 3, the epoch when the universe may have gone through its most dramatic changes. We emphasize the need for future large multiplexed spectroscopic instruments that can perform dedicated surveys in the optical and NIR to pin down the demographics of such objects and study their reddening properties, star-formation histories, and excitation conditions. These key studies will shed light on the role of black holes in galaxy evolution during the epoch of peak growth activity., Comment: Science White Paper for the US Astro 2020 Decadal Survey, 5 pages, 2 figures

Published
2019
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11. A new, faint population of X-ray transients

Author

Junxian Wang, Steve Schulze, Franz E. Bauer, Maurizio Paolillo, Cristian Vignali, Piero Ranalli, Ohad Shemmer, David M. Alexander, Keiichi Maeda, Kevin Schawinski, F. Forster, David Alexander Kann, Paolo Tozzi, Ken'ichi Nomoto, Ezequiel Treister, Donald P. Schneider, Roberto Gilli, Alexey Tolstov, W. N. Brandt, Nozomu Tominaga, Bin Luo, Guang Yang, Andrea Comastri, Masaomi Tanaka, Yongquan Xue, Bauer, Franz E., Treister, Ezequiel, Schawinski, Kevin, Schulze, Steve, Luo, Bin, Alexander, David M., Brandt, William N., Comastri, Andrea, Forster, Francisco, Gilli, Roberto, Kann, David Alexander, Maeda, Keiichi, Nomoto, Ken'Ichi, Paolillo, Maurizio, Ranalli, Piero, Schneider, Donald P., Shemmer, Ohad, Tanaka, Masaomi, Tolstov, Alexey, Tominaga, Nozomu, Tozzi, Paolo, Vignali, Cristian, Wang, Junxian, Xue, Yongquan, and Yang, Guang

Subjects
Active galactic nucleus, gamma-ray burst: general, galaxies: active, X-rays: bursts, X-rays: general, Astrophysics::High Energy Astrophysical Phenomena, Population, gamma-ray burst: general, galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, X-rays: general, 01 natural sciences, Tidal disruption event, 0103 physical sciences, education, X-rays: bursts, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, 010308 nuclear & particles physics, Astronomy, White dwarf, Astronomy and Astrophysics, Light curve, Redshift, Afterglow, Space and Planetary Science, general, X-rays: general [gamma-ray burst], Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, X-rays: burst
Abstract

We report on the detection of a remarkable new fast high-energy transient found in the Chandra Deep Field-South, robustly associated with a faint (mR = 27.5 mag, zph ∼ 2.2) host in the CANDELS survey. The X-ray event is comprised of 115(+12)(−11) net 0.3–7.0 keV counts, with a light curve characterized by an ≈100 s rise time, a peak 0.3–10 keV flux of ≈5 × 10(−12) erg s(−1) cm(−2) and a power-law decay time slope of −1.53 ± 0.27. The average spectral slope is Γ=1.43(+0.23)(−0.13), with no clear spectral variations. The X-ray and multiwavelength properties effectively rule out the vast majority of previously observed high-energy transients. A few theoretical possibilities remain: an ‘orphan’ X-ray afterglow from an off-axis short-duration gamma-ray burst (GRB) with weak optical emission, a low-luminosity GRB at high redshift with no prompt emission below ∼20 keV rest frame, or a highly beamed tidal disruption event (TDE) involving an intermediate-mass black hole and a white dwarf with little variability. However, none of the above scenarios can completely explain all observed properties. Although large uncertainties exist, the implied rate of such events is comparable to those of orphan and low-luminosity GRBs as well as rare TDEs, implying the discovery of an untapped regime for a known transient class, or a new type of variable phenomena whose nature remains to be determined., Monthly Notices of the Royal Astronomical Society, 467 (4), ISSN:0035-8711, ISSN:1365-2966, ISSN:1365-8711

Published
2017

12. X-Ray Spectral Analyses of AGNs from the 7Ms Chandra Deep Field-South Survey: The Distribution, Variability, and Evolutions of AGN Obscuration

Author

Maurizio Paolillo, Jun Xian Wang, W. N. Brandt, Franz E. Bauer, Zhiyuan Ji, Paolo Tozzi, Ohad Shemmer, Andrea Comastri, Teng Liu, Guang Yang, Anton M. Koekemoer, Guido Risaliti, Yongquan Xue, Roberto Gilli, Donald P. Schneider, Bin Luo, Vincenzo Mainieri, David M. Alexander, Q. Daniel Wang, Mauro Giavalisco, Cristian Vignali, Liu, Teng, Tozzi, Paolo, Wang, Jun-Xian, Brandt, William N., Vignali, Cristian, Xue, Yongquan, Schneider, Donald P., Comastri, Andrea, Yang, Guang, Bauer, Franz E., Paolillo, Maurizio, Luo, Bin, Gilli, Roberto, Wang, Q. Daniel, Giavalisco, Mauro, Ji, Zhiyuan, Alexander, David M, Mainieri, Vincenzo, Shemmer, Ohad, Koekemoer, Anton, Risaliti, Guido, Zhiyuan, Ji, ITA, and USA

Subjects
catalog, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Population, galaxies: active, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 0103 physical sciences, Spectral analysis, survey, education, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, 010308 nuclear & particles physics, X-ray, Astronomy and Astrophysics, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Redshift, X-rays: galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Chandra Deep Field South, Astrophysics - High Energy Astrophysical Phenomena, galaxies: evolution, X-rays: galaxie
Abstract

We present a detailed spectral analysis of the brightest Active Galactic Nuclei (AGN) identified in the 7Ms Chandra Deep Field South (CDF-S) survey over a time span of 16 years. Using a model of an intrinsically absorbed power-law plus reflection, with possible soft excess and narrow Fe K$\alpha$ line, we perform a systematic X-ray spectral analysis, both on the total 7Ms exposure and in four different periods with lengths of 2-21 months. With this approach, we not only present the power-law slopes, column densities $N_H$, observed fluxes, and absorption-corrected 2-10~keV luminosities $L_X$ for our sample of AGNs, but also identify significant spectral variabilities among them on time scales of years. We find that the $N_H$ variabilities can be ascribed to two different types of mechanisms, either flux-driven or flux-independent. We also find that the correlation between the narrow Fe line EW and $N_H$ can be well explained by the continuum suppression with increasing $N_H$. Accounting for the sample incompleteness and bias, we measure the intrinsic distribution of $N_H$ for the CDF-S AGN population and present re-selected subsamples which are complete with respect to $N_H$. The $N_H$-complete subsamples enable us to decouple the dependences of $N_H$ on $L_X$ and on redshift. Combining our data with that from C-COSMOS, we confirm the anti-correlation between the average $N_H$ and $L_X$ of AGN, and find a significant increase of the AGN obscured fraction with redshift at any luminosity. The obscured fraction can be described as $f_{obscured}\thickapprox 0.42\ (1+z)^{0.60}$., Comment: 35 figures, ApJS accepted

Published
2017

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