Microlensing Constraints on Quasar X-ray Emission Regions
|
|
- Hubert Baldwin Tucker
- 5 years ago
- Views:
Transcription
1 Microlensing Constraints on Quasar X-ray Emission Regions Xinyu Dai (Univ. of Oklahoma) Bin Chen (Univ. of Oklahoma) Chris Kochanek (Ohio State Univ.) George Chartas (College of Charleston) Chris Morgan (Naval Academy) Jeff Blackburne (Ohio State Univ.) Ana Mosquera (Ohio State Univ.) E. Baron (Univ. of Oklahoma) R. Kantowski (Univ. of Oklahoma) 2/21/2014 NAOC Colloquium, X. Dai 1
2 2/21/2014 NAOC Colloquium, X. Dai 2
3 Flux Density First Cosmological Lens Q Wavelength Discovered in /21/2014 NAOC Colloquium, X. Dai 3
4 Currently ~150 Quasar-Galaxy Lens 2/21/2014 NAOC Colloquium, X. Dai 4
5 Basic Observables Quasar image B Quasar image A Quasar image C Host galaxy Quasar image D Lens galaxy Hubble Image of Gravitational Lens RXJ (Morgan, Kochanek, Falco, and Dai 2006) 2/21/2014 NAOC Colloquium, X. Dai 5
6 Time Delay in PG Measured in X-rays T(A1-A2)=0.16 days Time Chartas, Dai, Garmire /21/2014 NAOC Colloquium, X. Dai 6 of 20
7 Schematic Plot of a Gravitational Lens D os Image D ls D ol Source y x y = D os D ol x - D ls a Point Mass a = 4GM Lens c 2 x 2/21/2014 NAOC Colloquium, X. Dai 7
8 Caustics and Critical Curves Source Plane 2/21/2014 NAOC Colloquium, X. Dai 8
9 Microlensing the Quasar Structure A typical quasar has an angular size of 1e-9 arcsec. 1 degree = 60 arcmin 1 arcmin = 60 arcsec Hubble Space Telescope 0.1 arcsec Quasi-Stellar Object Very Long Baseline Interferometry (VLBI) 0.1 milli-arcsec (1e-4 arcsec) 2/21/2014 NAOC Colloquium, X. Dai 9
10 But the smarter ones They quarrel and argue among each other 2/21/2014 NAOC Colloquium, X. Dai 10
11 2/21/2014 NAOC Colloquium, X. Dai 11
12 Magnification Pattern Produced by Stars C B A D 4GM 2 c 2/21/2014 NAOC Colloquium, X. Dai 12
13 How to use microlensing to measure the source size? Qualitative Approach Larger sources smooth the magnification pattern and have smaller microlensing variability. 2/21/2014 NAOC Colloquium, X. Dai 13
14 Intrinsic Variability Time delays A B = 12.0, A C = 9.6, A D = 87 days Days 2/21/2014 NAOC Colloquium, X. Dai 14
15 Removing intrinsic variability Microlensing Variability We observe this in almost all the systems we monitor 2/21/2014 NAOC Colloquium, X. Dai 15
16 X-ray Microlensing Is More Dramatic April 2004 Nov 2006 June 2000 Nov 2006 RXJ1131 and HE1104 by Chandra (Chartas et al. 2009) 2/21/2014 NAOC Colloquium, X. Dai 16
17 Examples of Magnification Patterns in the Monte-Carlo Simulations Image A * / =1 * / =0.5 * / =0.25 * / =0.125 Image C 2/21/2014 NAOC Colloquium, X. Dai 17
18 2/21/2014 NAOC Colloquium, X. Dai 18
19 2/21/2014 NAOC Colloquium, X. Dai 19
20 Microlensing Model Setup A Monte-Carlo approach 10 step in stellar density 46X61 log grid for optical/x-ray size 5 steps in un-microlensed flux fraction 4 cases in treatment of global magnification offset 10^6 trials for each magnification pattern. 2/21/2014 NAOC Colloquium, X. Dai 20
21 A Solution in RXJ Dai et al. 2010, ApJ, 709, 278 2/21/2014 NAOC Colloquium, X. Dai 21
22 Probability Finally the Accretion Disk Size 100 AU 14 AU Size 2/21/2014 NAOC Colloquium, X. Dai 22
23 Challenge Optical Emission Models The classic AGN Model (Shakura & Sunyaev 1973) predicts Yielding 3-4 times smaller size than microlensing measurements Solutions: T µr -3/ 4 Flatter Temperature Profiles Inhomogeneous Disk 2/21/2014 NAOC Colloquium, X. Dai 23
24 Current Program Regular monitoring ~20 lenses in optical (B, V, R, I) bands. Sparse Hubble monitoring 1131 and 2237 in rest-frame ultra-violet in Sparse Chandra X-ray monitoring 7 lenses in (including a 680 ks large program in and a 800 ks large program in ). 2/21/2014 NAOC Colloquium, X. Dai 24
25 Chandra Monitoring of Gravitational Lenses 2/21/2014 NAOC Colloquium, X. Dai 25
26 X-ray and Optical Microlensing Variability Q2237, Chen et al. (2011, 2012); Mosquera et al. (2013) Time RXJ1131, Chartas et al. (2012) 2/21/2014 NAOC Colloquium, X. Dai 26
27 X-ray Microlensing Light Curves (Chen et al. 2012) 2/21/2014 NAOC Colloquium, X. Dai 27
28 Probability X-ray and Optical Emission Sizes QJ0158, Morgan et al. (2012) HE0435, Blackburne et al. (2011) HE1104, Blackburne et al. (2013) Size Q2237, Mosquera et al. (2013) 2/21/2014 NAOC Colloquium, X. Dai 28
29 X-ray and Optical Emission Sizes Excluded Excluded Excluded 2/21/2014 NAOC Colloquium, X. Dai 29
30 Energy Dependent X-Ray Microlensing Q2237 Chen et al. 2011, ApJL, 740, 34 Larger microlensing variability in hard band. Smaller hard source Temperature gradient in corona 2/21/2014 NAOC Colloquium, X. Dai 30
31 Energy Dependent X-ray Microlensing QJ0158, Morgan et al. (2012) Q2237, Mosquera et al. (2013) Hard X-ray Smaller in 2 cases (QJ0158, Q2237). Consistent in 2 cases (could due to S/N) Hard X-ray larger in one case (RXJ1131). 2/21/2014 NAOC Colloquium, X. Dai 31
32 Microlensing of Iron Lines (Chen et al. 2012a) Fe Lines are observed in almost all case. Sometime we see split of the line. 2/21/2014 NAOC Colloquium, X. Dai 32
33 Microlensing of Iron Lines Chen et al. (2012a) Iron line EWs in lensed quasars are larger than those of normal AGN of same luminosities. Iron line size is even smaller than X-ray continuum. 2/21/2014 NAOC Colloquium, X. Dai 33
34 Model of AGN Accretion Disk Hard X-ray Soft X-ray Iron line Accretion Disk Black Hole Cycle 14/ ks program. Corona Calibrating all data from Cycle 1 to 15. 2/21/2014 NAOC Colloquium, X. Dai 34
35 X-ray Emission Under Strong Gravity Chen et al. 2013, ApJ, 762, /21/2014 NAOC Colloquium, X. Dai 35
36 Testing Unification Models Predicted aox distribution between BALs and non-bals 2/21/2014 NAOC Colloquium, X. Dai 36
37 Compare with Observations BALQSOs, Morabito et al Type I (red) and II (blue) AGN, Winter et al /21/2014 NAOC Colloquium, X. Dai 37
38 Polarization of the X-ray, EUV Continua In 0435, the EUV size is similar to the X- ray size 2/21/2014 NAOC Colloquium, X. Dai 38
39 Combining Kerr-Lensing and Microlensing 2/21/2014 NAOC Colloquium, X. Dai 39
40 D m m m Potential New Spin Measurement Technique 5 (A) spin a = 0 red : Kerr+Micro solid : 75 degree blue : Micro only dotted : 15 degree (B) spin a = (B) (A) [a = VS a = 0] (75 deg) (15 deg) Time (in pixel) 2/21/2014 NAOC Colloquium, X. Dai 40
41 Potential New Spin Measurement Technique 2/21/2014 NAOC Colloquium, X. Dai 41
42 Future Perspectives on Strong Lensing Data from Pan-Starrs, DES, Large Synoptic Survey Telescope (LSST) will be available in the next 6-7 years. E.g. LSST 20,000 square degrees Six bands Well-sampled light-curves E.g. LSST will detect 4,000 gravitational strong lenses: increase the current sample by 40 times. 2/21/2014 NAOC Colloquium, X. Dai 42
43 Microlensing Microlensing will still lead the angular resolution at least in the next 20 years in AGN studies. Increase the measurements from ~20 to 4,000. Dependence with mass, accretion rate, radio emission, and many other parameters. 2/21/2014 NAOC Colloquium, X. Dai 43
44 Lens Galaxy Light curves also provide time delay measurements. Image positions and time delays matter distribution Dark Gravitational lensing provides a unique tool to study the inter-stellar medium in the lens galaxy (Dai et al. 2003; Dai & Kochanek 2005; Dai et al. 2006; Dai & Kochanek 2009). ISM properties of 4,000 galaxies. 2/21/2014 NAOC Colloquium, X. Dai 44
45 X-ray Microlensing after Chandra Era Athena+: m 2 effective area at 1 kev, 5--3 angular resolution 10,000 Quasar-Galaxy lenses detected by DES, LSST, WFIRST We will apply the technique to the large separation lens like SDSS /21/2014 NAOC Colloquium, X. Dai 45
Using Microlensing to Probe Strong Gravity Near Supermassive Black Holes
Using Microlensing to Probe Strong Gravity Near Supermassive Black Holes Interstellar: Kip Thorne and Double Negative visual-effects team Presented by: George Chartas Chris Kochanek (OSU) Henric Krawczynski
More informationarxiv: v1 [astro-ph.ga] 31 Jan 2018
Draft version February 2, 2018 Typeset using L A TEX preprint style in AASTeX61 PROBING PLANETS IN EXTRAGALACTIC GALAXIES USING QUASAR MICROLENSING Xinyu Dai 1 and Eduardo Guerras 1 arxiv:1802.00049v1
More informationModeling Quasar Microlensing
WDS'5 Proceedings of Contributed Papers Physics, 2 26, 25. ISBN 978-8-7378-3-2 MATFYZPRESS Modeling Quasar Microlensing L. Ledvina and D. Heyrovský Institute of Theoretical Physics, Faculty of Mathematics
More informationGravitational Lensing: Strong, Weak and Micro
P. Schneider C. Kochanek J. Wambsganss Gravitational Lensing: Strong, Weak and Micro Saas-Fee Advanced Course 33 Swiss Society for Astrophysics and Astronomy Edited by G. Meylan, P. Jetzer and P. North
More informationObservational Cosmology
Astr 102: Introduction to Astronomy Fall Quarter 2009, University of Washington, Željko Ivezić Lecture 15: Observational Cosmology 1 Outline Observational Cosmology: observations that allow us to test
More informationQuasars ASTR 2120 Sarazin. Quintuple Gravitational Lens Quasar
Quasars ASTR 2120 Sarazin Quintuple Gravitational Lens Quasar Quasars Quasar = Quasi-stellar (radio) source Optical: faint, blue, star-like objects Radio: point radio sources, faint blue star-like optical
More informationBlack Hole and Host Galaxy Mass Estimates
Black Holes Black Hole and Host Galaxy Mass Estimates 1. Constraining the mass of a BH in a spectroscopic binary. 2. Constraining the mass of a supermassive BH from reverberation mapping and emission line
More informationAn Introduction to Radio Astronomy
An Introduction to Radio Astronomy Bernard F. Burke Massachusetts Institute of Technology and Francis Graham-Smith Jodrell Bank, University of Manchester CAMBRIDGE UNIVERSITY PRESS Contents Preface Acknowledgements
More informationGravitational Lensing. A Brief History, Theory, and Applications
Gravitational Lensing A Brief History, Theory, and Applications A Brief History Einstein (1915): light deflection by point mass M due to bending of space-time = 2x Newtonian light tangentially grazing
More informationExtragalactic DM Halos and QSO Properties Through Microlensing
Extragalactic DM Halos and QSO Properties Through Micro Eduardo Guerras (student) - Evencio Mediavilla (supervisor) Instituto de Astrofísica de Canarias Photon deflection by gravitating mass α = 4GM 2
More informationBroadband X-ray emission from radio-quiet Active Galactic Nuclei
29 th ASI Meeting ASI Conference Series, 2011, Vol. 3, pp 19 23 Edited by Pushpa Khare & C. H. Ishwara-Chandra Broadband X-ray emission from radio-quiet Active Galactic Nuclei G. C. Dewangan Inter-University
More informationThe Black Hole in the Galactic Center. Eliot Quataert (UC Berkeley)
The Black Hole in the Galactic Center Eliot Quataert (UC Berkeley) Why focus on the Galactic Center? The Best Evidence for a BH: M 3.6 10 6 M (M = mass of sun) It s s close! only ~ 10 55 Planck Lengths
More informationWe investigate the flux ratio anomalies between
arxiv:1711.07919v1 [astro-ph.co] 21 Nov 2017 A Quadruply Lensed SN Ia: Gaining a Time-Delay...Losing a Standard Candle Daniel A. Yahalomi 1, Paul L. Schechter 1,2, and Joachim Wambsganss 3 1 MIT Department
More informationarxiv:astro-ph/ v1 23 Dec 2005
3D spectroscopy as a tool for investigation of the BLR of lensed QSOs Luka Č. Popović Astronomical Observatory, Volgina 7, 11160 Belgrade, Serbia lpopovic@aob.bg.ac.yu arxiv:astro-ph/0512594v1 23 Dec 2005
More informationExtragalactic Microlensing: Quasars, Caustics & Dark Matter
Extragalactic Microlensing: Quasars, Caustics & Dark Matter Joachim Wambsganss Universität Heidelberg April 22, 2009 JENAM / NAM University of Hertfordshire Extragalactic Microlensing: Quasars, Caustics
More informationRESOLVING HIGH ENERGY UNIVERSE USING STRONG GRAVITATIONAL LENSING. Anna Barnacka Einstein Fellow at Harvard
Berenice Abbott RESOLVING HIGH ENERGY UNIVERSE USING STRONG GRAVITATIONAL LENSING Anna Barnacka Einstein Fellow at Harvard EXTRAGALACTIC JETS - M87 Increased X-ray emission by a factor of 50 from the HST-1
More informationStrong gravitational lenses in the 2020s
Strong gravitational lenses in the 2020s Masamune Oguri University of Tokyo 2014/7/18 TMT science forum @ Tucson Strong gravitational lenses are rare wide-field surveys find strong gravitational lenses
More informationPart two of a year-long introduction to astrophysics:
ASTR 3830 Astrophysics 2 - Galactic and Extragalactic Phil Armitage office: JILA tower A909 email: pja@jilau1.colorado.edu Spitzer Space telescope image of M81 Part two of a year-long introduction to astrophysics:
More informationX-raying High-Redshift AGNs and the First Black Holes: From Chandra to Lynx
X-raying High-Redshift AGNs and the First Black Holes: From Chandra to Lynx Niel Brandt, Fabio Vito, the Chandra Deep Fields Team, and the Lynx First Accretion Light Working Group Some Relevant Results
More informationGravitation. Isaac Newton ( ) Johannes Kepler ( )
Schwarze Löcher History I Gravitation Isaac Newton (1643-1727) Johannes Kepler (1571-1630) Isaac Newton (1643-1727) Escape Velocity V = 2GM R 1/2 Earth: 11.2 km/s (40 320 km/h) Moon: 2.3 km/s (8 300 km/h)
More informationRELATIVISTIC SPECTROSCOPY OF BLACK HOLES
RELATIVISTIC SPECTROSCOPY OF BLACK HOLES Michael Parker ESAC science seminar 24/5/18 BLACK HOLES 101 For an object to just escape a massive body, it needs the sum: Kinetic energy + gravitational binding
More informationLecture 11: SDSS Sources at Other Wavelengths: From X rays to radio. Astr 598: Astronomy with SDSS
Astr 598: Astronomy with SDSS Spring Quarter 4, University of Washington, Željko Ivezić Lecture : SDSS Sources at Other Wavelengths: From X rays to radio Large Surveys at Many Wavelengths SDSS: UV-IR five-band
More informationHigh Redshift Universe
High Redshift Universe Finding high z galaxies Lyman break galaxies (LBGs) Photometric redshifts Deep fields Starburst galaxies Extremely red objects (EROs) Sub-mm galaxies Lyman α systems Finding high
More informationThe phenomenon of gravitational lenses
The phenomenon of gravitational lenses The phenomenon of gravitational lenses If we look carefully at the image taken with the Hubble Space Telescope, of the Galaxy Cluster Abell 2218 in the constellation
More informationAn Introduction to Radio Astronomy
An Introduction to Radio Astronomy Second edition Bernard F. Burke and Francis Graham-Smith CAMBRIDGE UNIVERSITY PRESS Contents Preface to the second edition page x 1 Introduction 1 1.1 The role of radio
More informationMulti-wavelength Astronomy
astronomy Multi-wavelength Astronomy Content What do we measure Multi-wavelength approach Data Data Mining Virtual Observatory Hands on session Larmor's formula Maxwell's equations imply that all classical
More informationX-ray data analysis. Andrea Marinucci. Università degli Studi Roma Tre
X-ray data analysis Andrea Marinucci Università degli Studi Roma Tre marinucci@fis.uniroma3.it Goal of these lectures X-ray data analysis why? what? how? Why? Active Galactic Nuclei (AGN) Physics in a
More informationarxiv: v1 [astro-ph.ga] 8 Nov 2018
DRAFT VERSION NOVEMBER 9, 2018 Typeset using L A TEX twocolumn style in AASTeX61 ESTIMATE OF THE ACCRETION DISK SIZE IN THE GRAVITATIONALLY LENSED QUASAR HE 0435-1223 USING MICROLENSING MAGNIFICATION STATISTICS
More informationActive Galactic Nuclei
Active Galactic Nuclei How were they discovered? How common are they? How do we know they are giant black holes? What are their distinctive properties? Active Galactic Nuclei for most galaxies the luminosity
More informationCloudy Workshop Participants
Cloudy Workshop Participants 2016 June Shandong University, Weihai DENNIS ALP KTH Royal Institute of Technology the ultra-soft X-ray excess in RLNLS1s Madhurjya P Bora Gauhati University, India magnetospheric
More informationTesting the nature of astrophysical black hole candidates. Cosimo Bambi (Fudan University, Shanghai)
Testing the nature of astrophysical black hole candidates Cosimo Bambi (Fudan University, Shanghai) 8 June 2013, Annual Meeting of the Physics Department Fudan University, Shanghai Tests of General Relativity
More informationActive Galactic Nuclei
Active Galactic Nuclei Optical spectra, distance, line width Varieties of AGN and unified scheme Variability and lifetime Black hole mass and growth Geometry: disk, BLR, NLR Reverberation mapping Jets
More informationarxiv:astro-ph/ v1 17 Dec 2001
Spectral properties of the Narrow-Line Seyfert 1 Quasar PG1211+143 arxiv:astro-ph/0112387v1 17 Dec 2001 A. Janiuk 1, B. Czerny 1, G.M. Madejski 2 1) N. Copernicus Astronomical Centre, Bartycka 18, 00-716,
More informationarxiv:astro-ph/ v1 26 Apr 2003
Gravitational lensing: a unique tool for cosmology ASP Conference Series, Vol. xxx, 2003 D. Valls Gabaud and J. P. Kneib (eds.) Flux Ratio Anomalies: Micro- and Milli-lensing arxiv:astro-ph/0304480v1 26
More informationREU Final Presentation
July 28, 2009 Outline 1 History Historical Background Outline 1 History Historical Background 2 to the project Theory: Deflection angle, lensing diagram, and equations Outline 1 History Historical Background
More informationProbing the Cosmos with light and gravity: multimessenger astronomy in the gravitational wave era
Utah State University DigitalCommons@USU Colloquia and Seminars Astrophysics 9-7-2011 Probing the Cosmos with light and gravity: multimessenger astronomy in the gravitational wave era Shane L. Larson Utah
More informationChandra discovery of the intracluster medium around UM425 at redshift 1.47
Chandra discovery of the intracluster medium around UM425 at redshift 1.47 Smita Mathur and Rik J. Williams Astronomy Department, The Ohio State University, 140 West 18th Avenue, Columbus OH 43220 ABSTRACT
More informationAGN Feedback In an Isolated Elliptical Galaxy
AGN Feedback In an Isolated Elliptical Galaxy Feng Yuan Shanghai Astronomical Observatory, CAS Collaborators: Zhaoming Gan (SHAO) Jerry Ostriker (Princeton) Luca Ciotti (Bologna) Greg Novak (Paris) 2014.9.10;
More informationAGN Selec)on Techniques. Kris)n Kulas Astro 278 Winter 2012
AGN Selec)on Techniques Kris)n Kulas Astro 278 Winter 2012 Selec)on Techniques Op)cal X- ray Radio Infrared Variability X- ray and Radio Physical Processes Detec)on of Sources Benefit of Wavelength Regime
More informationBlack Hole Accretion and Wind
Black Hole Accretion and Wind Feng Yuan Shanghai Astronomical Observatory, Chinese Academy of Sciences Accretion Regimes Hyper-accretion, slim disk, ADAF (Abramowicz et al. 1988) TDEs, ULXs, SS433 Thin
More informationStudying microquasars with X-ray polarimetry
Studying microquasars with X-ray polarimetry XIPE extp IXPE Andrea Marinucci From quiescence to ouburst: when microquasars go wild! Ile de Porquerolles 25 September 2017 Outline - Introduction - Polarimetry
More informationAC Fabian, M. Cappi, J Sanders. Cosmic Feedback from AGN
AC Fabian, M. Cappi, J Sanders Cosmic Feedback from AGN AC Fabian, M Cappi, J Sanders, S Heinz, E Churazov, B McNamara, J Croston, D Worrall, F Humphrey, F Tombesi, J Reeves, M Giustini, P O Brien, T Reiprich
More informationQuasars as dark energy probes
Quasars as dark energy probes Bożena Czerny Center for Theoretical Physics & Copernicus Astronomical Center, Warsaw, Poland In collaboration with J. Średzińska, M. Bilicki, M. Chodorowski, K. Hryniewicz,
More informationActive galaxies. Some History Classification scheme Building blocks Some important results
Active galaxies Some History Classification scheme Building blocks Some important results p. 1 Litirature: Peter Schneider, Extragalactic astronomy and cosmology: an introduction p. 175-176, 5.1.1, 5.1.2,
More informationAGILE and Blazars: the Unexpected, the Unprecedented, and the Uncut
AGILE and Blazars: the Unexpected, the Unprecedented, and the Uncut Rome, AGILE γ-ray Symposium 2017.12.12 Stefano Vercellone (INAF-OAB) 1 Rationale A review of the whole set of AGILE results on extra-galactic
More informationActive galactic nuclei (AGN)
Active galactic nuclei (AGN) General characteristics and types Supermassive blackholes (SMBHs) Accretion disks around SMBHs X-ray emission processes Jets and their interaction with ambient medium Radio
More informationMoment of beginning of space-time about 13.7 billion years ago. The time at which all the material and energy in the expanding Universe was coincident
Big Bang Moment of beginning of space-time about 13.7 billion years ago The time at which all the material and energy in the expanding Universe was coincident Only moment in the history of the Universe
More informationCOSMOGRAIL: present and future
COSMOGRAIL: present and future F. Courbin, G. Meylan, V. Bonvin, M Tewes, D. Sluse, D. Paraficz... For the COSMOGRAIL collaboration Laboratoire d astrophysique http://lastro.epfl.ch Quasar Time Delay Meeting
More informationTransient iron fluorescence: new clues on the AGN disk/corona?
Transient iron fluorescence: new clues on the AGN disk/corona? Emanuele Nardini Horizon 2020 INAF/Arcetri AstroFIt2/MSCA in collaboration with: D. Porquet (CNRS/Strasbourg), J. Reeves (Keele+UMBC), V.
More informationBlack Holes and Active Galactic Nuclei
Black Holes and Active Galactic Nuclei A black hole is a region of spacetime from which gravity prevents anything, including light, from escaping. The theory of general relativity predicts that a sufficiently
More informationCosine of emission angle: Energy (kev)
EFFECTS OF STRONG GRAVITY ON THE X-RAY SPECTRA OF AGN AND BHCs A. MARTOCCHIA 1, V. KARAS 2 and G. MATT 3 (1) SISSA-ISAS Via Beirut 2/4, I-34014 Trieste (Italy) (2) Astronomical Institute, Charles University
More informationHubble Space Telescope ultraviolet spectroscopy of blazars: emission lines properties and black hole masses. E. Pian, R. Falomo, A.
Hubble Space Telescope ultraviolet spectroscopy of blazars: emission lines properties and black hole masses E. Pian, R. Falomo, A. Treves 1 Outline Extra Background Introduction Sample Selection Data Analysis
More informationBROAD SPECTRAL LINE AND CONTINUUM VARIABILITIES IN QSO SPECTRA INDUCED BY MICROLENSING:METHODS OF COMPUTATION
Proceedings of the IX Bulgarian-Serbian Astronomical Conference: Astroinformatics (IX BSACA) Sofia, Bulgaria, July -,, Editors: M. K. Tsvetkov, M. S. Dimitrijević, O. Kounchev, D. Jevremović andk. Tsvetkova
More informationReverberation Mapping in the Era of MOS and Time-Domain Surveys: from SDSS to MSE
Reverberation Mapping in the Era of MOS and Time-Domain Surveys: from SDSS to MSE Yue Shen Carnegie Obs -> University of Illinois at Urbana-Champaign MSE Science Team Meeting, July 29-31 2015, Big Island
More informationSimultaneous X-ray and Radio Observations of Seyferts, and Disk-Jet Connections
Simultaneous X-ray and Radio Observations of Seyferts, and Disk-Jet Connections Ashley Lianne King, University of Michigan Advisor: Jon M. Miller Collaborators: John Raymond, Michael Rupen, Kayhan Gültekin,
More informationASTRON 449: Stellar (Galactic) Dynamics. Fall 2014
ASTRON 449: Stellar (Galactic) Dynamics Fall 2014 In this course, we will cover the basic phenomenology of galaxies (including dark matter halos, stars clusters, nuclear black holes) theoretical tools
More informationIntroduction to AGN. General Characteristics History Components of AGN The AGN Zoo
Introduction to AGN General Characteristics History Components of AGN The AGN Zoo 1 AGN What are they? Active galactic nucleus compact object in the gravitational center of a galaxy that shows evidence
More informationBlack Holes in Hibernation
Black Holes in Hibernation Black Holes in Hibernation Only about 1 in 100 galaxies contains an active nucleus. This however does not mean that most galaxies do no have SMBHs since activity also requires
More informationStudying microquasars with X-ray polarimetry
Studying microquasars with X-ray polarimetry extp Andrea Marinucci IXPE Congresso Nazionale Oggetti Compatti X Padova 14 September 2017 Outline - Introduction - Polarimetry and microquasars: Coronal geometry
More informationTesting the nature of astrophysical black hole candidates. Cosimo Bambi Fudan University
Testing the nature of astrophysical black hole candidates Cosimo Bambi Fudan University http://www.physics.fudan.edu.cn/tps/people/bambi/ 26 September 2013, National Astronomical Observatories, Beijing
More informationThe quest for early Black Holes
The quest for early Black Holes Andrea Comastri (INAF-Bologna) Roberto Gilli (INAF-Bologna) Cristian Vignali (Bologna University) Marcella Brusa (MPE) and many others Outline High redshift (z > 3) AGN
More information2. Active Galaxies. 2.1 Taxonomy 2.2 The mass of the central engine 2.3 Models of AGNs 2.4 Quasars as cosmological probes.
2. Active Galaxies 2.1 Taxonomy 2.2 The mass of the central engine 2.3 Models of AGNs 2.4 Quasars as cosmological probes Read JL chapter 3 Active galaxies: interface with JL All of JL chapter 3 is examinable,
More informationGamma Ray Bursts. Progress & Prospects. Resmi Lekshmi. Indian Institute of Space Science & Technology Trivandrum
Gamma Ray Bursts Progress & Prospects Resmi Lekshmi Indian Institute of Space Science & Technology Trivandrum Why study GRBs? to study GRBs end stages of massive star evolution jet launching, collimation
More informationIn a dense region all roads lead to a black Hole (Rees 1984 ARAA) Deriving the Mass of SuperMassive Black Holes
In a dense region all roads lead to a black Hole (Rees 1984 ARAA) Deriving the Mass of SuperMassive Black Holes Stellar velocity fields MW Distant galaxies Gas motions gas disks around nearby black holes
More informationHI Galaxy Science with SKA1. Erwin de Blok (ASTRON, NL) on behalf of The HI Science Working Group
HI Galaxy Science with SKA1 Erwin de Blok (ASTRON, NL) on behalf of The HI Science Working Group SKA1 HI Science Priorities Resolved HI kinematics and morphology of ~10 10 M mass galaxies out to z~0.8
More informationLearning Objectives: Chapter 13, Part 1: Lower Main Sequence Stars. AST 2010: Chapter 13. AST 2010 Descriptive Astronomy
Chapter 13, Part 1: Lower Main Sequence Stars Define red dwarf, and describe the internal dynamics and later evolution of these low-mass stars. Appreciate the time scale of late-stage stellar evolution
More informationTesting Accretion Disc Theory in AGN: X-ray/Optical Inter-band Lags in NGC Sam Connolly
New Results in X-Ray Astronomy 2015 Testing Accretion Disc Theory in AGN: X-ray/Optical Inter-band Lags in NGC 4395 Sam Connolly With Ian McHardy (University of Southampton) Brad Peterson, Curtis McCully
More informationThe Next 2-3 Weeks. Important to read through Chapter 17 (Relativity) before I start lecturing on it.
The Next 2-3 Weeks [27.1] The Extragalactic Distance Scale. [27.2] The Expansion of the Universe. [29.1] Newtonian Cosmology [29.2] The Cosmic Microwave Background [17] General Relativity & Black Holes
More informationTMT and Space-Based Survey Missions
TMT and Space-Based Survey Missions Daniel Stern Jet Propulsion Laboratory/ California Institute of Technology 2014 California Institute of Technology TMT Science Forum 2014 July 17 Outline Summary of
More informationTesting astrophysical black holes. Cosimo Bambi Fudan University
Testing astrophysical black holes Cosimo Bambi Fudan University http://www.physics.fudan.edu.cn/tps/people/bambi/ 29 October 2015 Interdisciplinary Center for Theoretical Studies (USTC, Hefei) Plan of
More informationChapter 19 Galaxies. Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past. halo
Chapter 19 Galaxies Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past halo disk bulge Barred Spiral Galaxy: Has a bar of stars across the bulge Spiral Galaxy 1
More informationActive Galaxies & Quasars
Active Galaxies & Quasars Normal Galaxy Active Galaxy Galactic Nuclei Bright Active Galaxy NGC 5548 Galaxy Nucleus: Exact center of a galaxy and its immediate surroundings. If a spiral galaxy, it is the
More informationAccretion Disks. 1. Accretion Efficiency. 2. Eddington Luminosity. 3. Bondi-Hoyle Accretion. 4. Temperature profile and spectrum of accretion disk
Accretion Disks Accretion Disks 1. Accretion Efficiency 2. Eddington Luminosity 3. Bondi-Hoyle Accretion 4. Temperature profile and spectrum of accretion disk 5. Spectra of AGN 5.1 Continuum 5.2 Line Emission
More informationOptical variability of quasars: damped random walk Željko Ivezić, University of Washington with Chelsea MacLeod, U.S.
Optical variability of quasars: damped random walk Željko Ivezić, University of Washington with Chelsea MacLeod, U.S. Naval Academy IAU Symposium 304, Yerevan, Armenia, October 7-12, 2013 OUTLINE Practically
More informationHomework 9 due Nov. 26 (after Thanksgiving)
Homework 9 due Nov. 26 (after Thanksgiving) [CO 17.6 parts (a), (b)] [16.6 1 st ed., parts (a), (b)] Derive the deflection of the light ray passing a massive object. Note that your answer will come out
More informationActive Galactic Nuclei OIII
Active Galactic Nuclei In 1908, Edward Fath (1880-1959) observed NGC 1068 with his spectroscope, which displayed odd (and very strong) emission lines. In 1926 Hubble recorded emission lines of this and
More informationStellar Binary Systems and CTA. Guillaume Dubus Laboratoire d Astrophysique de Grenoble
Stellar Binary Systems and CTA Guillaume Dubus Laboratoire d Astrophysique de Grenoble Barcelona Cherenkov Telescope Array Meeting, 24-25 January 2008 X-ray binaries picture by H. Spruit relativistic outflow
More informationTEMA 6. Continuum Emission
TEMA 6. Continuum Emission AGN Dr. Juan Pablo Torres-Papaqui Departamento de Astronomía Universidad de Guanajuato DA-UG (México) papaqui@astro.ugto.mx División de Ciencias Naturales y Exactas, Campus Guanajuato,
More informationQuasars in the SDSS. Rich Kron NGC June 2006 START CI-Team: Variable Quasars Research Workshop Yerkes Observatory
Quasars in the SDSS Rich Kron 28 June 2006 START CI-Team: Variable Quasars Research Workshop Yerkes Observatory NGC 1068 About 10% of all of the spectra in the SDSS database are of quasars (as opposed
More informationNew Suzaku Results on Active Galaxies. or Reflections on AGN. James Reeves (Keele) and Suzaku team (given by Lance Miller)
New Suzaku Results on Active Galaxies or Reflections on AGN James Reeves (Keele) and Suzaku team (given by Lance Miller) Overview Overview of Suzaku and instrument performance. Why Suzaku is important
More informationActive Galactic Nuclei - Zoology
Active Galactic Nuclei - Zoology Normal galaxy Radio galaxy Seyfert galaxy Quasar Blazar Example Milky Way M87, Cygnus A NGC 4151 3C273 BL Lac, 3C279 Galaxy Type spiral elliptical, lenticular spiral irregular
More informationSource plane reconstruction of the giant gravitational arc in Abell 2667: a condidate Wolf-Rayet galaxy at z 1
Source plane reconstruction of the giant gravitational arc in Abell 2667: a condidate Wolf-Rayet galaxy at z 1 Speaker: Shuo Cao Department of Astronomy Beijing Normal University Collaborators: Giovanni
More informationAST Cosmology and extragalactic astronomy. Lecture 20. Black Holes Part II
AST4320 - Cosmology and extragalactic astronomy Lecture 20 Black Holes Part II 1 AST4320 - Cosmology and extragalactic astronomy Outline: Black Holes Part II Gas accretion disks around black holes, and
More informationBrief update (3 mins/2 slides) on astrophysics behind final project
Nov 1, 2017 Brief update (3 mins/2 slides) on astrophysics behind final project Evidence for Dark Matter Next Wed: Prelim #2, similar to last one (30 mins). Review especially lecture slides, PEs and non-project
More informationAstr Resources
Astr 8400 - Resources Course web page: http://www.astro.gsu.edu/~crenshaw/astr8400.html Electronic papers: http://adsabs.harvard.edu/abstract_service.html NASA Extragalactic Database: http://nedwww.ipac.caltech.edu
More informationAstrophysical Research
Astrophysical Research Elena Bannikova Institute of Radio Astronomy of National Academy of Science V.N.Kharazin Kharkiv National University Astrophysical Research in Kharkiv Theoretical investigations
More informationBackground Picture: Millennium Simulation (MPA); Spectrum-Roentgen-Gamma satellite (P. Predehl 2011)
By Collaborators Alex Kolodzig (MPA) Marat Gilfanov (MPA,IKI), Gert Hütsi (MPA), Rashid Sunyaev (MPA,IKI) Publications Kolodzig et al. 2013b, A&A, 558, 90 (ArXiv : 1305.0819) Hüsti et al. 2014, submitted
More informationInclination-Dependent AGN Flux Profiles From Strong Lensing of the Kerr Space-Time
Inclination-Dependent AGN Flux Profiles From Strong Lensing of the Kerr Space-Time Bin Chen 1, Xinyu Dai 1, E. Baron 1,2,3,4 arxiv:1211.2510v1 [astro-ph.he] 12 Nov 2012 ABSTRACT Recent quasar microlensing
More informationWFIRST and JWST synergies in the study of First Light. M. Stiavelli STScI, Baltimore
WFIRST and JWST synergies in the study of First Light M. Stiavelli STScI, Baltimore 1 WFIRST and JWST synergies in the study of First Light Plan: - Detecting the First Stars WFIRST-AFTA as an object finder
More informationSKA Continuum Deep Field Surveys
SKA Continuum Deep Field Surveys Amit Vishwas April 7, 2010 The Square Kilometer Array The Next Generation Radio Telescope Spread over a long baseline ~1000 kms Large Effective Area: but only a fraction
More informationAge-redshift relation. The time since the big bang depends on the cosmological parameters.
Age-redshift relation The time since the big bang depends on the cosmological parameters. Lyman Break Galaxies High redshift galaxies are red or absent in blue filters because of attenuation from the neutral
More informationA Supermassive Black Hole in the Dwarf Starburst Galaxy Henize Amy Reines Einstein Fellow National Radio Astronomy Observatory
A Supermassive Black Hole in the Dwarf Starburst Galaxy Henize 2-10 Amy Reines Einstein Fellow National Radio Astronomy Observatory Supermassive black holes and galaxy evolution Supermassive black holes
More informationHow can Mathematics Reveal Dark Matter?
How can Mathematics Reveal? Chuck Keeton Rutgers University April 2, 2010 Evidence for dark matter galaxy dynamics clusters of galaxies (dynamics, X-rays) large-scale structure cosmography gravitational
More informationClusters of Galaxies " High Energy Objects - most of the baryons are in a hot (kt~ k) gas." The x-ray luminosity is ergs/sec"
Clusters of Galaxies! Ch 4 Longair Clusters of galaxies are the largest gravitationally bound systems in the Universe. At optical wavelengths they appear as over-densities of galaxies with respect to the
More informationSUPPLEMENTARY INFORMATION
doi:10.1038/nature11096 Spectroscopic redshifts of CDF-N X-ray sources We have taken a recent compilation 13 as our main source of spectroscopic redshifts. These redshifts are given to two decimal places,
More informationOn the Effects of Extended-Source Morphology on Emission-Line Redshift Accuracy
WFIRST Technical Report Rev: A Date: October 27, 2016 On the Effects of Extended-Source Morphology on Emission-Line Redshift Accuracy R. E. Ryan Jr., S. Casertano, & N. Pirzkal Abstract We discuss the
More informationBinary systems with accretion onto compact object
Micro-quasars 1 Binary systems with accretion onto compact object Cataclysmic variables X binaries White dwarf Neutron star Black hole Classification based on the mass of the donor star: LOW-MASS X-RAY
More informationSuper Massive Black Hole Mass Determination and. Categorization of Narrow Absorption Line Quasars Outflows
1 H. James Super Massive Black Hole Mass Determination and Categorization of Narrow Absorption Line Quasars Outflows By Hodari-Sadiki James April 30 th 2012 Abstract We looked at high luminosity quasars
More informationClusters of Galaxies with Euclid
Clusters of Galaxies with Euclid Figure by L. Caridà A. Biviano (INAF-OATS) largely based on Sartoris, AB, Fedeli et al. 2016 Euclid: ESA medium class A&A mission, selected Oct 2011, to be launched in
More informationGravitational light bending prevents gamma-gamma absorption in gravitational lenses
Gravitational light bending prevents gamma-gamma absorption in gravitational lenses NWU, South Africa E-mail: 26559226@nwu.ac.za Markus Böttcher NWU, South Africa E-mail: Markus.Bottcher@nwu.ac.za The
More information