Shuang-Nan Zhang, Yuan Liu, Jin Zhang Institute of High Energy Physics

Slides:



Advertisements
Similar presentations
Tom Esposito Astr Feb 09. Seyfert 1, Seyfert 2, QSO, QSO2, LINER, FR I, FR II, Quasars, Blazars, NLXG, BALQ…
Advertisements

Disk corona in AGN: what do we expect? Bifang Liu Yunnan Observatory, CAS The disk corona evaporation model The model for X-ray binaries Similarities between.
The W i d e s p r e a d Influence of Supermassive Black Holes Christopher Onken Herzberg Institute of Astrophysics Christopher Onken Herzberg Institute.
Supermassive Black Holes in Radio-loud AGNs
Weighing black holes in radio-loud AGNs
What can we learn on the BLR from the smallest AGN? Or, how do the BLR properties change with luminosity, and what is it telling us? Specifically The BLR.
On the geometry of broad emission region in quasars Roberto Decarli Turin - May, 20 th, 2008 Università degli Studi dell’Insubria Dipartimento di Fisica.
“Do I have your attention…?”
Active Galactic Nuclei Very small angular size: point like High luminosity: compared to host galaxies Broad-band continuum emission: radio to TeV Strong.
Quasars, Active Galactic Nuclei (AGN), and Black Holes What is an “active galaxy” or “quasar”? How is it different from a “normal” galaxy? 1. Much, much.
The Dusty Torus of NGC1068 Literature Study for the Bachelor Research Project: Bas Nefs Maarten Zwetsloot.
COSPAR Workshop, Udaipur 2003 Active Galactic Nuclei : I Keith Arnaud NASA Goddard University of Maryland.
The nature of the dust and gas in the nucleus of NGC 1068.
Galaxies with Active Nuclei Chapter 17. You can imagine galaxies rotating slowly and quietly making new stars as the eons pass, but the nuclei of some.
Intrinsic Absorption in Quasars: BALs & NALs Jonathan Trump February 11, 2007.
Chapter 25: Quasars and active galaxies Features of quasars Quasars and distant galaxies Seyfert and radio galaxies Active galactic nuclei Supermassive.
Active Galaxies PHYS390 Astrophysics Professor Lee Carkner Lecture 22.
Numerical Modeling of Electromagnetic Radiation from AGN Jets Based on  -ray emission and spectral evolution of pair plasmas in AGN jets Bottcher et al.
Galaxies and the Foundation of Modern Cosmology III.
Active Galactic Nuclei Thomas Schlenker University of Washington Department of Physics PHYS 496 -What is an AGN? -What kinds of AGN’s are out there? -Unified.
Active Galactic Nuclei Ay 16, April 8, AGN DEFINITION PROPERTIES GRAVITATIONAL LENSES BLACK HOLES MODELS.
Quasars and Other Active Galaxies
Luminous Hot Accretion Flows extending ADAF beyond its critical accretion rate Feng Yuan Shanghai Astronomical Observatory, Chinese Academy of Science.
An Accretion Disc Model for Quasar Optical Variability An Accretion Disc Model for Quasar Optical Variability Li Shuang-Liang Li Shuang-Liang Shanghai.
Most of the power of galaxies come from the stars Almost all nearby galaxies Some galaxies have very bright sources right at the center Can be as bright.
 Galaxies with extremely violent energy release in their nuclei  Active Galactic Nuclei (AGN)  Up to many thousand times more luminous than the entire.
Low covering factor of the BLR in weak emission-line quasars Marek Nikołajuk Faculty of Physics Univ. of Białystok, Poland 3rd NCAC Symposium: „Accretion.
AGN (Continued): Radio properties of AGN I) Basic features of radio morphology II) Observed phenomena Superluminal motion III) Unification schemes.
The Evolution of Quasars and Massive Black Holes “Quasar Hosts and the Black Hole-Spheroid Connection”: Dunlop 2004 “The Evolution of Quasars”: Osmer 2004.
Cosmology and extragalactic astronomy Mat Page Mullard Space Science Lab, UCL 7. Quasars.
Modern Quasar SEDs Zhaohui Shang ( Tianjin Normal University ) Kunming, Feb
Active Galaxies Definition – –Amount of Energy –Type of Energy Non-thermal Polarized Other characteristics –Emission spectra Hydrogen – Balmer series &
THE HST VIEW OF LINERS AND OTHER LOCAL AGN MARCO CHIABERGE CNR - Istituto di Radioastronomia - Bologna Alessandro Capetti (INAF-OATo) Duccio Macchetto.
Variability of radio-quiet AGN across the spectrum: facts and ideas B. Czerny Copernicus Astronomical Center, Warsaw, Poland.
The Evolution of AGN Obscuration
Investigating the relation of corona and disk from a blue AGN sample Liu, Jieying Yunnan Astronomical Observatory, CAS 第三届黑洞天体物理前沿问题年度研讨会 (2008),SHAO ,
Spins of supermassive black holes in quasars and galaxies Jian-Min Wang ( 王建民 ) Institute of High Energy Physics Chinese Academy of Sciences, Beijing Dec.
AGN9: Black Holes & Revelations 25 May 2010 Eleonora Sani Enhanced star formation in Narrow Line Seyfert 1 AGN Co-Is: D. Lutz, G. Risaliti, L. H. Gallo,
The Differences in the SEDs of Type 1 and Type 2 AGNs: Contributions from starbursts Xue-Bing Wu Collaborator: Ran Wang (Astronomy Department, Peking University)
Black holes and accretion flows Chris Done University of Durham.
On the X-ray origin in Quiescent Black Hole X-ray Binaries Hui Zhang ( 张惠 ) Shanghai Astronomical Observatory, Chinese Academy of Sciences Collaborators:
Galaxies with Active Nuclei Chapter 14:. Active Galaxies Galaxies with extremely violent energy release in their nuclei (pl. of nucleus).  “active galactic.
Quasars and Active Galactic Nuclei
Active Galactic Nuclei Chapter 25 Revised Active Galactic Nuclei Come in several varieties; Starburst Nuclei – Nearby normal galaxies with unusually.
Active Galaxies and Supermassive Black Holes Chapter 17.
Astrophysics from Space Lecture 6: Supermassive black holes Prof. Dr. M. Baes (UGent) Prof. Dr. C. Waelkens (KUL) Academic year
Quasars and Other Active Galaxies
Quasars, Active Galaxies, and Gamma-Ray Bursters Chapter Twenty-Seven.
AGN / Starbursts in the very dusty systems in Bootes Kate Brand + the Bootes team NOAO Lijiang, August 2005.
Variability and Flares From Accretion onto Sgr A* Eliot Quataert (UC Berkeley) Collaborators: Josh Goldston, Ramesh Narayan, Feng Yuan, Igor Igumenshchev.
Most of the power of ordinary galaxies come from the stars Some galaxies have very bright sources right at the center Can be as bright as a galaxy, or.
Active Galaxies Galaxies with extremely violent energy release in their nuclei (pl. of nucleus). → “Active Galactic Nuclei” (= AGN) Up to many thousand.
X-RAY PROPERTIES OF FR II/NLRG X-RAY PROPERTIES OF FR II/NLRG E. Trussoni 1, A. Capetti 1, B. Balmaverde 2 1 INAF – Osservatorio Astronomico di Torino,
Universe Tenth Edition Chapter 24 Quasars and Active Galaxies Roger Freedman Robert Geller William Kaufmann III.
A Search for Blazars among the Unidentified EGRET Gamma-Ray Sources.
The black hole fundamental plane: revisit with a larger sample of radio and X-ray emitting broad line AGNs Zhao-Yu Li Astronomy Department, Peking University.
Quasars, Active Galaxies, and super-massive black holes
Announcements Observing Monday-Thursday of this week counts on the third exam. Fourth exam is Wednesday, November 17 Review will be Monday, November 15.
The origin nuclear X-ray emission in the nuclei of radio galaxy-FR Is
Shuang-Nan Zhang, Yuan Liu, Jin Zhang Institute of High Energy Physics
Cygnus X-1 is a Black Hole Binary
ACTIVE GALAXIES and GALAXY EVOLUTION
Active Versus Normal Galaxies
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide.
Galaxies With Active Nuclei
Group Nov. 01, USTC 4/18/2019 Group Nov. 01, USTC AGN-dominated SFG-dominated.
Galaxies With Active Nuclei
Balmer Lines as a Probe of Physical Processes in the Broad Line Region
Variability Study of Fermi Blazars
Presentation transcript:

Dusty Torus Formation by Anisotropic Radiative Feedback of Active Galactic Nuclei Shuang-Nan Zhang, Yuan Liu, Jin Zhang Institute of High Energy Physics and National Astronomical Observatories of China Chinese Academy of Sciences Liu,Y. & Zhang, S.N., 2011, ApJL, 728, L44

The unified model of AGN Formation? Dusty torus Evolution?

AGN feedback The distribution of the dust is anisotropic The normal of the accretion disk The distribution of the dust is anisotropic The UV/optical radiation from the accretion disk is also anisotropic The effect of radiation pressure is significant due to the presence of dust observer A~500

The evolution of AGNs A B C Momentum effect of radiation

Evaporation radius The inner radius of dust Energy effect of radiation

The profile of a dusty torus

NH-L/LEdd plane Raimundo, Fabian, Bauer et al. 2010

The fraction of type 2 AGNs Hasinger 2008

The inner radius of dusty torus Suganuma et al. 2006

The evolution of dusty torus Luminous, with torus, but without bright BLR

Weak line quasars Shemmer et al. 2009; EW<5 A; continuum similar to normal quasars

Radio quiet BL Lac No obvious emission lines Plotkin et al. 2009

Are WLQs and Radio Quiet BL Lac the Objects Predicted by Our Model? Predictions Luminous accretion disk emission Existence of Dusty Torus Tests Low polarization  disk not jet Low variability  disk not jet Hot dust emission  torus illuminated by luminous disk

Polarization Test: radio quiet BL Lac Very low polarization in continuum spectra: only two of 25 candidates are observed with weak polarization (Heidt & Nilsson 2011); non detection for all others The continuum spectrum is consistent with disk origin

Long Term Variability Test So far observations are quite limited Weaker than radio loud BL Lac? Need more observations Plotkin et al. 2010

Long Term Variability Test SDSS Stripe 82(12 radio quiet BL Lac,4 WLQ,27 radio loud BL Lac) Radio quiet Radio loud

Lightcurve amplitudes Radio loud Radio quiet

Four SDSS Radio Quiet BL Lac Observed with Lijiang 2 Four SDSS Radio Quiet BL Lac Observed with Lijiang 2.4 m at V, I and R bands SDSS 094533.99+100950.1 SDSS 094533.99+100950.1 081250.80+522530.8 085025.60+342750.9 085025.60+342750.9 090107.64+384658.8

Very weak short timescale variability! Short Term Variability Test m(BL Lac)-m(Star) Time (Hour) Very weak short timescale variability!

Hot Dust Test in weak line quasars Black body from hot dust Diamond-Stanic et al. 2009 Evidence of hot dust in WLQ

Conclusions The distribution of dusty gas should also be anisotropic due to the influence of the anisotropic disk radiation. Our model can explain the presence of some obscured AGNs with high Eddington ratios and can also reproduce the observed decreasing fraction of type 2 AGNs with increasing luminosity. Our model predicts the existence of luminous AGNs with dusty tori, but without luminous broad line regions. Weak line quasars and radio quiet BL Lac? Weak polarization, low variability and hot dust feature confirm our model predictions. Liu,Y. & Zhang, S.N., 2011, ApJL, 728, L44