Multiwaveband Variability of. Seyferts and LINERS
|
|
- Bernard Mitchell
- 5 years ago
- Views:
Transcription
1 Multiwaveband Variability of Seyferts and LINERS Relationship to X-rays Ian M c Hardy University of 1
2 Outline X-ray / UV / Optical variability X-ray / Radio variability 2
3 X-ray / UV/ Optical Variability What causes UV/optical variability in Seyferts? Reprocessing of X-rays? - X-rays lead uv/optical by short (hour-days) light travel time. Expect Lag Wavelength 1.33 Intrinsic disc variability X-rays lag: two possibilities Long lag (months), viscous propagation timescale for perturbations to reach X-ray region from optical in disc Short lag (hour-day), light travel time of UV seed photons to corona 3
4 NGC 4051: optical X-ray 4
5 NGC
6 NGC4051 Optical lags by 1.5+/- 0.5 d (above 99% confidence) Breedt et al
7 MKN 79 (Breedt et al, 2009, MNRAS) Long timescales (years) uncorrelated behaviour. Intrinsic disc variations in optical? Short timescales (days-weeks) - well correlated. Hint that optical lags, but lag not well defined 7
8 Swift UV / optical interband lags Line is Lag Wavelength 1.33 NGC2617 Shappee et al 2014 Between data points per band Fit to UV-optical with fixed power law slope of 4/3 does not go through X-ray point 8
9 Swift Monitoring of NGC5548: (> 500 observations) Good correlation, but not perfect, eg large W2 rise after day 6480 McHardy et al, 2014, MNRAS, 444,
10 Lag of X-rays by UVW2 Mean-subtracted lightcurves Intensively sampled period Lag distribution (Javelin Zu et al 2011) 10
11 NGC 5548 All Swift Bands 11
12 Lags as function of wavelength Lag Wavelength 1.23 Expect 4/3 power for Shakura-Sunyaev disc. So good agreement. Fit goes through X-ray point Model lags (McHardy et al, 2014) BUT observed lags are longer than expected for the Mass and m Red line is time for HALF of reprocessed light to arrive. Microlensing obs (eg Morgan et al 2010) also require larger disc than SS model Hotter than expected disc (eg higher Inhomogeneous disc (Dexter and Agol 2011)? m, higher Lx)? Time associated with the reprocessing mechanism? Same result in extensive follow up observations (Edelson et al 2015, Fausnaugh et al 2015) 12
13 XMM and ground based lags for NGC4395 Mass 3.6x10 5, x100 lower than NGC5548, and x10 lower Does it also have longer lags than predicted? m UVW1 with OM Ground based g-band monitoring around globe (Peterson, Elvis, Uemura Chand, Netzer, Kaspi and others) (Connolly et al. in prep) 13
14 NGC4395: Swift X-ray / UVW2 Looking within individual Swift visits (TOO 12 ks) uvw2 lags X-rays by ~400s 14
15 XMM and ground based monitoring of NGC4395 X-ray XMM UVW1- XMM OM g-band ground December
16 NGC DCFs X-rays vs UVW1 X-rays vs g-band (Using Emmanouloupolos et al 2013 improved lightcurve simulation method for simulations) 16
17 NGC4395 Javelin lags UVW1 lags X-rays by 473 (+47, -98) s g-band lags X-rays by 788 (+44, -54) s 17
18 NGC4395 Lags vs Wavelength Lags very short. Intrinsic reprocessing time must be very short. Simple linear fit (red) is best fit (forced through zero). However powerlaw of index 4/3 (blue) is also acceptable So reprocessing dominates here also, but agreement with Shakura-Sunyaev models is closer than for NGC5548 does disc structure depend on M, mdot, Temp? 18
19 NGC Models observations model emission profiles Solid lines total disc energy release in band, including X-ray contribution Dashed lines gravitational energy release Observed lags correspond to peak emission radii (models from P. Lira) 19
20 Dependence of reprocessing on disc temperature: X-ray / UV Variability of NLS1s DCF Swift UVW2 X-rays Cameron et al, in prep Poor correlation 20
21 X-ray / optical correlation strength depends inversely on disc temperature From Cameron PhD thesis; also Breedt Phd thesis 21
22 LINERS M81
23 M81 NuSTAR NuSTAR 1000s bins 4d observation With Andy Young, Bristol 23
24 LINER M81 NuSTAR Spectrum Disc reflection very weak or absent So optical is NOT reprocessed X-rays Cut-off PL is good fit Γ=1.85 E_cut=230 kev Hot iron line 6.62 kev -ADAF? (Young, McHardy et al, in prep) 24
25 X-ray / UV Variability of M81 IF there is a UV/X-ray correlation, then - X-rays lagging UV: UV could be seed photons for X-rays, eg cyclo/synchrotron from corona - UV lagging X-rays: UV from synchrotron jet, downstream from X-ray corona 25
26 X-ray / UV Variability of M81 Swift UV X-rays Cameron 2014 Phd Thesis 26
27 X-ray / W1 Variability of M81 Some short timescale correspondence 27
28 X-ray / UV Variability of M81 W1 W Lag of X-ray by UVW2 (days) Weak correlations, close to zero lag, possibly small UV lag Suggests UV are not seed photons for X-rays but are from downstream jet Javelin result from Harvey-Taylor UG Could just be part of same emission component 28
29 X-ray / UV Variability of LINERS UVW1 UVW2 X-RAYS 29
30 X-Ray / mm / Radio Relationship in LINERS NGC7213, M81 (More luminous radio sources than Seyferts) Do the perturbations which drive the X-rays carry on into the jet? Are liners the equivalent of `hard state X-ray binaries?
31 NGC7213 X-RAY/RADIO MJD S ~ ν + α (Bell et al, 2011) 31
32 NGC7213 X-RAY/RADIO 8 GHz lags X-rays by ~24 days 5 GHz lags X-rays by ~40 days 32
33 M81 sub-mas structure Sub-mas bending jet similar to blazars Here from Ros, McH et al; See also Marti-Vidal et al
34 M81 radio-mm variability: strong correlation Radio lags by approx 3d - consistent with standard synchrotron jet 34
35 SMA 1.3mm vs AMI 15GHz radio Radio lags mm by a few days ie definite synchrotron jet 35
36 M81 Swift X-ray and AMI 15 GHz Radio Guy Pooley 36
37 M81 X-ray vs Radio AMI 15GHz from Pooley; OVRO from Richards, Readhead and Pearson 37
38 M81 X-ray / Radio ICCF / DCF ICCF DCF Good overall correlation. Perturbations (from disc?) which drive X-rays may propagate down the jet to drive radio variations. Lag of X-ray by Radio (days) Centroid of lag, using Peterson lagerror8 prog simulations 21 +/- 3d Peak of lag 44 +/- 3d (Thanks to Brad Peterson) Scaling to binaries is unclear: X-ray / optical binary lag of 0.1s (Gandhi et al 10) is consistent (assuming also linear lag scaling with wavelength) But X-ray/radio lag of 7 minutes (Wilms et al 2007) is too long. 38
39 M81 X-ray and Radio scaled When scaled for mass, M81 data fits on Fundamental Plane for jet dominated sources very well observed Merloni et al 2003, Falcke et al 2004, Koerding et al
40 LINER M81 Lags Radio lags X-ray by approx Radio lags mm by UV lags X-rays by ~ 21d - a messy correlation, OK on long timescales ~ 3d - well defined correlation ~ 0.5d - weak correlation but lag, well defined. Long X-ray / radio lag with shorter mm / radio lag could mean synchrotron emitting part of jet starting some way from BH and X-ray emitting corona. Then UV has to be part of the X-ray emission component. Or maybe X-ray / radio lag is actually shorter, then jet could start near BH 40
41 Another Coronal / Jet Connection : QSO 3C273 RXTE X-ray Gamma-ray Only occasional simultaneous flares, but perhaps the Gamma-ray emission, overall, is greatest when the average X-ray level is highest?
42 X-ray / Gamma-ray correlation : 3C273 So there may be a small amount of co-spatial X- and Gamma-ray emission, but most comes from separate emission regions.
43 X-ray / Radio Variability of Radio Quiet Seyferts 43
44 X-ray bright Seyfert: NGC4151 Mundell et al 2003 Radio jets commonly seen in nearby Seyferts but rarely (never?) luminous or compact enough to expect significant Synchrotron Self-Compton X-rays. So is there a radio / X-ray relationship? If so, why?
45 Radio variability from Seyferts, ie high accretion rate, Soft State, AGN NGC5548 Wrobel radio variability over months but no parallel X-ray observations See also Mundel et al 2009 Seyferts are thought to be the equivalent of soft state X-ray binaries. No detectable radio emission from soft state binaries Russel et al
46 NGC Seyfert Looks just like a classical radio galaxy except much smaller and of much lower luminosity. (Jones et al, in prep) Component separation is ~50 light years (Girolleti and Panessa 2009)
47 NGC4051 VLA A array observations Radio Default beam Fixed beam Smoothed X-ray X-ray At best, only a very weak hint of X-ray/radio correlation Jones et al
48 NGC4051 Radio vs. X-ray - all arrays No strong evidence for large amplitude radio variability (Jones et al, 2011) 48
49 NGC4051 on radio `fundamental plane for jet-dominated sources (Merloni et al 2003, Falcke et al 2004, Koerding et al 2006 Here plotting just hard state objects from Koerding etal NGC4051 is ~1 decade radio quiet Jet orientation? 49
50 NGC4051 as a coronal radio source? L R /L x ~10-5 If so, X-ray is integral of radio emission (Neupert effect seen in stellar coronae) Too faint to search for that effect here. From Laor and Behar
51 NGC5548 AMI 15GHz Compact core (Guy Pooley) Other source is unrelated 51
52 NGC5548 X-ray / Radio Variability AMI 15GHz - Guy Pooley Swift RXTE 52
53 NGC5548: X-ray / Radio Lag Radio lags X-ray by 42 +/- 17d Too long for radio to be seed photons in corona Accretion rate fluctuations from disc, perturbing X-ray corona, could propagate down jet to radio emission 53
54 CONCLUSIONS SEYFERTS: Short timescale UV/optical variability is X-ray reprocessing but implied disc size in NGC5548 is ~3x too big for Shakura Sunyaev model. Are all AGN discs bigger than theoretically expected? If so, why? LINERS: Short timescale UV variability in M81 correlates weakly with the X-rays with very short lag. No disc, so j et emission? M81 radio lags X-rays by ~20d. Radio lags mm by ~3d. Possibly perturbations which drive X-rays also go down the jet. Seyferts: weak correlation of X-ray and radio with radio lagging by about 40d. Some similarities to liner M81.
55
56 Material I won t show is below
57 Infrared Optical Lags: NGC3783 Green is V-band, for comparison. J-band similar lightcurve to V-band, but K-band lags. V and J mostly reprocesing from disc, K includes some torus contribution Lira et al, submitted also Saganuma et al
58 XMM and ground based monitoring of NGC s bins December
59 X-ray / UV Variability of NLS1s DCF Swift UVW2 X-rays Cameron et al, in prep 59
60 NGC4051 X-ray Spectra and radio 60
61 X-ray / Gamma-ray variability : 3C273 Gamma-ray X-ray Gamma-ray Much more high-frequency variability in Gamma-rays
62 X-ray / Gamma-ray correlation : 3C273
The origin of UV / Optical Variability of AGN: Relationship to X-ray Variability. Ian M c Hardy. University of Southampton 1
The origin of UV / Optical Variability of AGN: Relationship to X-ray Variability Ian M c Hardy University of 1 Main Questions What drives UV/optical variability in AGN? How is the X-ray band related to
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 informationarxiv: v1 [astro-ph.he] 23 Jul 2014
Mon. Not. R. Astron. Soc. 000, 000 000 (2014) Printed 11 July 2018 (MN LATEX style file v2.2) Swift monitoring of NGC5548: X-ray reprocessing and short term UV/optical variability arxiv:1407.6361v1 [astro-ph.he]
More informationOsservatorio Astronomico di Bologna, 27 Ottobre 2011
Osservatorio Astronomico di Bologna, 27 Ottobre 2011 BASIC PARADIGM: Copious energy output from AGN (10 9-10 13 L Θ ) from accretion of material onto a Supermassive Black Hole SMBH ( 10 6-10 9 M Θ ). AGN
More informationMAXI and AGN X-ray Variability
MAXI and AGN X-ray Variability Ian M c Hardy 1 1 School of Physics and Astronomy, University of Southampton, University Road, Southampton SO17 1BJ, UK E-mail(IM): imh@astro.soton.ac.uk Abstract The X-ray
More informationSwift monitoring of NGC 5548: X-ray reprocessing and short-term UV/optical variability
doi:10.1093/mnras/stu1636 Swift monitoring of NGC 5548: X-ray reprocessing and short-term UV/optical variability I. M. McHardy, 1 D. T. Cameron, 1 T. Dwelly, 1,2 S. Connolly, 1 P. Lira, 3 D. Emmanoulopoulos,
More informationX-ray variability of AGN
X-ray variability of AGN Magnus Axelsson October 20, 2006 Abstract X-ray variability has proven to be an effective diagnostic both for Galactic black-hole binaries and active galactic nuclei (AGN). This
More informationLong-Term X-ray Spectral Variability of AGN
Long-Term X-ray Spectral Variability of AGN Sam Connolly Ian McHardy, Chris Skipper, Dimitrios Emmanoulopoulos, Tom Dwelly University of Southampton Jet Triggering Mechanisms in Black Hole Sources TIFR,
More informationThe Accretion Geometry of NGC 5548
The Accretion Geometry of NGC 5548 Emma Gardner & Chris Done Durham University Reverberation as a Tool for Investigating Accretion Geometries UV Disc Illuminates Clouds Clouds Re-emit Flux as Lines Czerny
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 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 informationX-rays from AGN in a multiwavelength context. Chris Done, University of Durham Martin Ward, Chichuan Jin, Kouchi Hagino
X-rays from AGN in a multiwavelength context Chris Done, University of Durham Martin Ward, Chichuan Jin, Kouchi Hagino Plan! What can we learn about AGN variability from BHB? What can we learn about tidal
More informationLeMMINGs the emerlin radio legacy survey of nearby galaxies Ranieri D. Baldi
LeMMINGs the emerlin radio legacy survey of nearby galaxies Ranieri D. Baldi in collaboration with I. McHardy, D. Williams, R. Beswick and many others The radio-loud / radio-quiet dichotomy Among the many
More informationThe nature of X-ray spectral variability in Seyfert galaxies
Mon. Not. R. Astron. Soc. 342, L31 L35 (2003) The nature of X-ray spectral variability in Seyfert galaxies Richard D. Taylor, Philip Uttley and Ian M. M c Hardy Department of Physics and Astronomy, University
More informationASTRO-H Studies of Accretion Flow onto Supermassive Black Hole
ASTRO-H Studies of Accretion Flow onto Supermassive Black Hole 2015 October 21 The Institute of Physical and Chemical Research (RIKEN) Nishina center Hirofumi Noda 1. Contents I. Introduction II. Geometry
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 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 informationRadio and X-rays from GRS Close correlations of the third kind
Mem. S.A.It. Vol. 82, 41 c SAIt 211 Memorie della Radio and -rays from GRS 1915+15 - Close correlations of the third kind Ralph Spencer 1 and Anthony Rushton 1,2,3 1 Jodrell Bank Centre for Astrophysics
More informationThe Phenomenon of Active Galactic Nuclei: an Introduction
The Phenomenon of Active Galactic Nuclei: an Introduction Outline Active Galactic Nuclei (AGN): > Why are they special? > The power source > Sources of Continuum Emission > Emission & absorption lines
More informationThe high-energy view of Seyfert galaxies through broad-band monitoring campaigns
The high-energy view of Seyfert galaxies through broad-band monitoring campaigns Francesco Ursini INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna In collaboration with: P.-O. Petrucci,
More informationarxiv:astro-ph/ v1 30 Dec 2006
AGN Variability from X-rays to Radio Waves ASP Conference Series, Vol. 390, 2006 C.M. Gaskell, I.M. M c Hardy, B.M. Peterson, and S.G. Sergeev (eds) Optical and X-ray Variability of AGNs arxiv:astro-ph/0701008v1
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 informationMultiwavelength rapid timing of X-ray binaries
Multiwavelength rapid timing of X-ray binaries Poshak Gandhi JAXA International Top Young Fellow Martin Durant Andy Fabian Piergiorgio Casella Vik Dhillon Jon Miller Elena Mason Kazuo Makishima Julien
More informationConnections between Radio and High Energy Emission in AGN
Connections between Radio and High Energy Emission in AGN Geoff Bicknell Research School of Astronomy & Astrophysics Australian National University 1 Collaborators: Loredana Bassani, INAF, Bologna Nadine
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 informationLecture 9. Quasars, Active Galaxies and AGN
Lecture 9 Quasars, Active Galaxies and AGN Quasars look like stars but have huge redshifts. object with a spectrum much like a dim star highly red-shifted enormous recessional velocity huge distance (Hubble
More informationEavesdropping on accretion disks:
disks: Broad-band variability properties of cataclysmic variables and their connections to XRBs/AGN E. Körding, P. Uttley, C. Knigge, P.J. Groot, C. Aerts, P. Jonker, M. Still Overview Why look at CVs?
More informationNuSTAR spectral analysis of the two bright Seyfert 1 galaxies: MCG and NGC Alessia Tortosa Università Roma Tre
NuSTAR spectral analysis of the two bright Seyfert 1 galaxies: MCG 8-11-11 and NGC 6814 Alessia Tortosa Università Roma Tre From the Dolomites to the event horizon: sledging down the black hole potential
More informationNot only typical flaring blazars in the Fermi gamma-ray sky. The strange cases of SBS and PKS
Not only typical flaring blazars in the Fermi gamma-ray sky. The strange cases of SBS 0846+513 and PKS 0521-36 Filippo D Ammando (University of Perugia and INFN) and M. Orienti (Univ. of Bologna and INAF-IRA)
More informationRelativistic jets from evolving accretion discs
Relativistic jets from evolving accretion discs Rob Fender (Southampton / Amsterdam) Thanks to: Elena Gallo, Simone Migliari, Tom Maccarone (Amsterdam) Tomaso Belloni (Brera), Stephane Corbel (Saclay),
More informationRob Fender University of Southampton. Jets from X-ray binaries and their connection to accretion flows, black hole spin, mass and environment
Rob Fender University of Southampton Jets from X-ray binaries and their connection to accretion flows, black hole spin, mass and environment When jets are formed I: Connection to spectra of accretion flow
More informationPiecing Together the X-ray Background: The Bolometric Output of AGN. Ranjan Vasudevan Supervisor: Prof. A. C. Fabian
Piecing Together the X-ray Background: The Bolometric Output of AGN Supervisor: Prof. A. C. Fabian Active Galactic Nuclei: Geometry of Emitting Regions X-rays UV Martin Krause (2007) Active Galactic Nuclei:
More informationHard X-ray selected sample of AGN: population studies
Hard X-ray selected sample of AGN: population studies Angela Malizia INCREASE OF AGN POPULATION IN THE INTEGRAL SURVEYS most of the unidentified objects have been subsequently classified as AGN Many more
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 informationCoronal geometry at low mass- accretion rates from XMM and NuSTAR spectra. Felix Fürst Caltech for the NuSTAR AGN physics and binaries teams
Coronal geometry at low mass- accretion rates from XMM and NuSTAR spectra Felix Fürst for the NuSTAR AGN physics and binaries teams Accreting black holes Supermassive black hole: Cen A Central engine of
More informationPoS(SWIFT 10)142. The Swift-XRT observations of HBL Source 1ES
The Swift-XRT observations of HBL Source 1ES 199+ ab, Patrizia Romano b, Stefano Vercellone b, Sergo Kapanadze a, Grigol Kharshiladze c a E. Kharadze Abastumani Astrophysical Observatory, Ilia State University,
More informationLong term multi-wavelength variability studies of the blazar PKS
52nd Rencontres de Moriond 2017 Very High Energy Phenomena in the Universe Long term multi-wavelength variability studies of the blazar PKS 2155-304 Jill Chevalier D. Sanchez, P. Serpico, J-P. Lenain,
More informationWhat can we learn from the AGN radio quiet continuum with SIMBOL-X?
What can we learn from the AGN radio quiet continuum with SIMBOL-X? Pierre-Olivier Petrucci LAOG, Grenoble, France Generalities about the RQ AGN X-ray emission - continuum - reflection component Expected
More informationPredicting Jets in Cygnus X-2
Predicting Jets in Cygnus X-2 Monika Balucinska-Church X-ray Binaries Group, School of Physics and Astronomy, University of Birmingham, U.K. The X-ray Universe 2014 June 16-19, Trinity College, Dublin
More informationThe X-Ray Universe. The X-Ray Universe
The X-Ray Universe The X-Ray Universe Potsdam University Dr. Lidia Oskinova Sommersemester 2017 lida@astro.physik.uni-potsdam.de astro.physik.uni-potsdam.de ~lida/vorlesungxrayso17.html Chandra X-ray,
More informationBlack Holes in the local Universe
Outline 1. AGN evolution and the history of accretion 2. From AGN SED to AGN physics Accretion discs and X-ray coronae in AGN 3. Do AGN reveal accretion mode changes? The fundamental plane of BH activity
More informationMWL. A Brief Advertisement Before Your Regularly Scheduled Program
MWL A Brief Advertisement Before Your Regularly Scheduled Program PKS 1441+25 PKS 1441+25 z=0.939! VHE detection over more than a single day! PKS 1441+25 37.7% polarization! PKS 1441+25 Continues optical
More informationDemographics of radio galaxies nearby and at z~0.55. Are radio galaxies signposts to black-hole mergers?
Elaine M. Sadler Black holes in massive galaxies Demographics of radio galaxies nearby and at z~0.55 Are radio galaxies signposts to black-hole mergers? Work done with Russell Cannon, Scott Croom, Helen
More informationLecture 20 High-Energy Astronomy. HEA intro X-ray astrophysics a very brief run through. Swift & GRBs 6.4 kev Fe line and the Kerr metric
Lecture 20 High-Energy Astronomy HEA intro X-ray astrophysics a very brief run through. Swift & GRBs 6.4 kev Fe line and the Kerr metric Tut 5 remarks Generally much better. However: Beam area. T inst
More informationAstr 2320 Thurs. April 27, 2017 Today s Topics. Chapter 21: Active Galaxies and Quasars
Astr 2320 Thurs. April 27, 2017 Today s Topics Chapter 21: Active Galaxies and Quasars Emission Mechanisms Synchrotron Radiation Starburst Galaxies Active Galactic Nuclei Seyfert Galaxies BL Lac Galaxies
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 onto the Massive Black Hole in the Galactic Center. Eliot Quataert (UC Berkeley)
Accretion onto the Massive Black Hole in the Galactic Center Eliot Quataert (UC Berkeley) Why focus on the Galactic Center? GR! Best evidence for a BH (stellar orbits) M 4x10 6 M Largest BH on the sky
More informationGRB history. Discovered 1967 Vela satellites. classified! Published 1973! Ruderman 1974 Texas: More theories than bursts!
Discovered 1967 Vela satellites classified! Published 1973! GRB history Ruderman 1974 Texas: More theories than bursts! Burst diversity E peak ~ 300 kev Non-thermal spectrum In some thermal contrib. Short
More informationKey issues in black hole accretion - Science by ASTRO-H - Shin Mineshige (Kyoto Univ.)
Key issues in black hole accretion - Science by ASTRO-H - Shin Mineshige (Kyoto Univ.) Beyond Beyond the standard disk model Standard-type disk (standard disk or SS disk) Efficient machine to convert gravitational
More informationOptical and infrared emission of X-ray novae S.A.Grebenev, A.V.Prosvetov, R.A.Burenin
Optical and infrared emission of X-ray novae S.A.Grebenev, A.V.Prosvetov, R.A.Burenin Space Research Institute (IKI), Moscow INTEGRAL 15 YEARS (Venice, Oct. 18, 2017) Sergei Grebenev Why X-ray novae? LMXB
More informationActive Galactic Nuclei
Active Galactic Nuclei Prof. Jeff Kenney Class 18 June 20, 2018 the first quasar discovered 3C273 (1963) very bright point source (the quasar ) jet the first quasar discovered 3C273 (1963) very bright
More informationBLACK HOLES (AND NEUTRON STARS) IN X-RAY BINARIES: Evolution and Accretion states TEO MUÑOZ DARIAS MARIE CURIE FELLOW. Oxford Astrophysics
BLACK HOLES (AND NEUTRON STARS) IN X-RAY BINARIES: Evolution and Accretion states TEO MUÑOZ DARIAS MARIE CURIE FELLOW Oxford Astrophysics ESAC 2014 Low Mass X-ray Binaries (LMXBs) Normal (
More informationRevealing the coronal properties of Seyfert galaxies with NuSTAR
Revealing the coronal properties of Seyfert galaxies with NuSTAR Andrea Marinucci (Roma Tre) on behalf of the NuSTAR AGN Physics WG Dublin The X-ray Universe 2014 June 19, 2014 Overview Brief introduction
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 information1932: KARL JANSKY. 1935: noise is identified as coming from inner regions of Milky Way
1932: KARL JANSKY Is assigned the task of identifying the noise that plagued telephone calls to Europe 1935: noise is identified as coming from inner regions of Milky Way MANY YEARS GO BY. 1960: a strong
More informationObservational Evidence of Black Holes Kolkata (India), Feb 2008
Observational Evidence of Black Holes Kolkata (India), Feb 2008 S Chakrabarti L Titarchuk R Kerr F Mirabel T Belloni S Zhang E Koerding T Alexander G Bisnovatyi-Kogan M DellaValle Z Paragi T Alexander
More informationThe NuSTAR view of Radio-quiet AGN
The NuSTAR view of Radio-quiet AGN (Università degli Studi Roma Tre) on behalf of the NuSTAR AGN Physics WG Active Galactic Nuclei 11 Where Black Holes and Galaxies meet Trieste, 23-26 September 2014 Outline
More informationarxiv: v3 [astro-ph.he] 3 Oct 2017
Mon. Not. R. Astron. Soc. 000, 1 16 () Printed 4 October 2017 (MN LATEX style file v2.2) The origin of the UV/optical lags in NGC 5548 Emma Gardner and Chris Done Centre for Extragalactic Astronomy, Department
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 informationarxiv: v1 [astro-ph.he] 6 Feb 2012
Mon. Not. R. Astron. Soc., () Printed 7th February 22 (MN LATEX style file v2.2) Correlated X-ray/Ultraviolet/Optical variability in the very low mass AGN NGC 4395 arxiv:22.84v [astro-ph.he] 6 Feb 22 D.
More informationSoft X-ray Emission Lines in Active Galactic Nuclei. Mat Page
Soft X-ray Emission Lines in Active Galactic Nuclei Mat Page MSSL-UCL Observations of soft X-ray line emission allow us to investigate highly ionized plasmas in galaxies and AGN. I ll start with the most
More informationCHARACTERIZATION OF AGN VARIABILITY IN THE OPTICAL AND NEAR INFRARED REGIMES
Paulina Lira - Konrad Tristram - Patricia Arévalo - Julián Mejía-Restrepo - Luis Ho - Regis Cartier - Paolo Coppi - Minjin Kim - + CHARACTERIZATION OF AGN VARIABILITY IN THE OPTICAL AND NEAR INFRARED REGIMES
More informationMulti-wavelength Surveys for AGN & AGN Variability. Vicki Sarajedini University of Florida
Multi-wavelength Surveys for AGN & AGN Variability Vicki Sarajedini University of Florida What are Active Galactic Nuclei (AGN)? Galaxies with a source of non-stellar emission arising in the nucleus (excessive
More informationAlan Marscher Boston University
The Relationship between Radio and Higher Frequency Emission in AGNs Alan Marscher Boston University Research Web Page: www.bu.edu/blazars Sketch of an AGN 10 6 to > 10 9 M sun black hole + accretion disk
More informationOVERVIEW OF A 3C279 s FLARE and SIMULATION OF AGNs
Gamma-ray Large Area Space Telescope OVERVIEW OF A 3C279 s FLARE and SIMULATION OF AGNs Alessandro Buzzatti Università degli Studi di Torino / SLAC Alessandro Buzzatti 1 Outline Overview of 3C279 flare
More informationSIMILARITY AND DIVERSITY OF BLACK HOLE SYSTEMS View from the Very High Energies
SIMILARITY AND DIVERSITY OF BLACK HOLE SYSTEMS View from the Very High Energies 1 Symp. 324, 12-16 September, 2016 Classical view Spinning black hole Accretion disk Collimated jets of particles 2 Looking
More informationQuasars and AGN. What are quasars and how do they differ from galaxies? What powers AGN s. Jets and outflows from QSOs and AGNs
Goals: Quasars and AGN What are quasars and how do they differ from galaxies? What powers AGN s. Jets and outflows from QSOs and AGNs Discovery of Quasars Radio Observations of the Sky Reber (an amateur
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 informationGalaxies with Active Nuclei. Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes
Galaxies with Active Nuclei Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes Active Galactic Nuclei About 20 25% of galaxies do not fit well into Hubble categories
More informationModelling the Variability of Blazar Jets
Modelling the Variability of Blazar Jets A Selfconsistent SSC Model Matthias Weidinger Institut für Theoretische Physik und Astrophysik, Universität Würzburg GRK Tage: 24. Juli 2009 M. Weidinger (Uni Wü)
More informationUvA-DARE (Digital Academic Repository)
UvA-DARE (Digital Academic Repository) Long-term monitoring of the archetype Seyfert galaxy MCG-6-30-15: X-ray, optical and near-ir variability of the corona, disc and torus Lira, P.; Arévalo, P.; Uttley,
More informationRoberto Soria (UCAS) Jets and outflows from super-eddington sources
Jets and outflows from super-eddington sources Roberto Soria (UCAS) Also thanks to: Ryan Urquhart (ICRAR PhD student) James Miller-Jones (ICRAR-Curtin) Manfred Pakull (Strasbourg Observatory) Christian
More informationACCRETION JET CONNECTION τ α MBH
Radio Observations ACCRETION JET CONNECTION τ α MBH 1 hr in GRS 1915+105 = 30 yr in SgrA* Mirabel et al. 1998 THE TRIGGERS OF JETS ARE INSTABILITIES IN THE ACCRETION DISK (TRANSITION LOW HARD TO HIGH THE
More informationThe BAT AGN Survey - Progress Report J. Tueller, C. Markwardt, L. Winter and R. Mushotzky Goddard Space Flight Center
The BAT AGN Survey - Progress Report J. Tueller, C. Markwardt, L. Winter and R. Mushotzky Goddard Space Flight Center The Swift BAT (Burst and Transient Telescope) has been observing the whole sky in the
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 informationX-ray time lags and reverberation from accreting black holes
X-ray time lags and reverberation from accreting black holes Phil Uttley University of Amsterdam Thanks to: Ed Cackett, Erin Kara, Andy Fabian, Dan Wilkins (Review paper: arxiv:1405.6575) 1. Background
More informationSchwarzchild Radius. Black Hole Event Horizon 30 km 9 km. Mass (solar) Object Star. Star. Rs = 3 x M (Rs in km; M in solar masses)
Schwarzchild Radius The radius where escape speed = the speed of light. Rs = 2 GM/c2 Rs = 3 x M (Rs in km; M in solar masses) A sphere of radius Rs around the black hole is called the event horizon. Object
More informationThe Extragalactic Gamma-Ray View of AGILE and Fermi
INAF, Osservatorio Astronomico di Capodimonte 22 February 2012 The Extragalactic Gamma-Ray View of AGILE and Fermi Elena Pian INAF, Trieste Astronomical Observatory & Scuola Normale Superiore di Pisa UNIFIED
More informationQuasars and Active Galactic Nuclei (AGN)
Quasars and Active Galactic Nuclei (AGN) Astronomy Summer School in Mongolia National University of Mongolia, Ulaanbaatar July 21-26, 2008 Kaz Sekiguchi Hubble Classification M94-Sa M81-Sb M101-Sc M87-E0
More informationAn explanation for the soft X-ray excess in AGN. Jamie Crummy collaborators: Andy Fabian, Luigi Gallo, Randy Ross Suzaku Team
An explanation for the soft X-ray excess in AGN Jamie Crummy collaborators: Andy Fabian, Luigi Gallo, Randy Ross Suzaku Team Soft excess The soft excess is at a constant temperature over a large range
More informationObservations of Active Galactic Nuclei at very high energies with H.E.S.S.
Observations of Active Galactic Nuclei at very high energies with H.E.S.S. Robert Wagner for the H.E.S.S. Collaboration http://www.mpi-hd.mpg.de/hess/ @hesstelescopes 1 H.E.S.S. High Energy Stereoscopic
More informationGuiding Questions. Active Galaxies. Quasars look like stars but have huge redshifts
Guiding Questions Active Galaxies 1. Why are quasars unusual? How did astronomers discover that they are extraordinarily distant and luminous? 2. What evidence showed a link between quasars and galaxies?
More informationMulti-wavelength behaviour of III Zw2
Multi-wavelength behaviour of III Zw2 Nikita Salvi, Mat J. Page, Jason A. Stevens, Keith O. Mason and Kinwah Wu arxiv:astro-ph/0201545v1 31 Jan 2002 Mullard Space Science Laboratory, University College
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 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 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 informationOrigin of X-rays in blazars
Origin of X-rays in blazars Greg Madejski, Stanford / KIPAC With much of the work presented here done by Amy Furniss, Masaaki Hayashida, Krzysztof Nalewajko, Marek Sikora, Jim Chiang, David Paneque, Mislav
More informationAGN Feedback at the Parsec Scale
AGN Feedback at the Parsec Scale Feng Yuan Shanghai Astronomical Observatory, CAS with: F. G. Xie (SHAO) J. P. Ostriker (Princeton University) M. Li (SHAO) OUTLINE Intermittent activity of compact radio
More informationHard X-ray Properties of Water Maser Galaxies
Hard X-ray Properties of Water Maser Galaxies Eugenia Litzinger University of Würzburg & Dr. Karl Remeis-Observatory Bamberg/ECAP J. Walther, M. Kadler, M. Langejahn, W.H. Baumgartner, N. Gehrels, C.B.
More informationHard X-ray AGN and the Cosmic X-ray Background
Hard X-ray AGN and the Cosmic X-ray Background Sergey Sazonov Space Research Institute, Moscow, Russia 1 Rome, Oct. 17, 2013 Plan Cosmic X-ray background: measurements, modeling and implications for heavily
More informationRestarting activity. in the nucleus of PBC J Lorena Hernández García
Restarting activity in the nucleus of PBC J2333.9-2343 Lorena Hernández García Collaborators: Francesca Panessa Marcello Giroletti Gabriele Ghisellini Loredana Bassani Nicola Masetti Mirjana Povic Angela
More informationNEAR-INFRARED PHOTOMETRY OF BLAZARS
NEAR-INFRARED PHOTOMETRY OF BLAZARS C. Chapuis 1,2,S.Corbel 1, P. Durouchoux 1,T.N.Gautier 3, and W. Mahoney 3 1) Service d Astrophysique DAPNIA, CEA Saclay F-91191 Gif sur Yvette cedex 2) Département
More informationFrom X-ray Binaries to AGN: the Disk/Jet Connection
From X-ray Binaries to AGN: the Disk/Jet Connection Rich Plotkin University of Amsterdam ( Michigan) with Sera Markoff (Amsterdam), Scott Anderson (Washington), Niel Brandt (PSU), Brandon Kelly (UCSB),
More informationThe physical state of radio-mode, low- luminosity AGN
The physical state of radio-mode, low- luminosity AGN Andrea Merloni Max-Planck Institut für Extraterrestrische Physik 5GHz, VLA image of Cyg A by R. Perley PhiGN start-up workshop, 14/12/2007 Parallel
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 informationASCA Observations of Radio-Loud AGNs
ASCA Observations of Radio-Loud AGNs Rita M. Sambruna & Michael Eracleous Department of Astronomy & Astrophysics, The Pennsylvania State University 525 Davey Lab, University Park, PA 16802 and arxiv:astro-ph/9811017v1
More informationActive Galaxies. Lecture Topics. Lecture 24. Active Galaxies. Potential exam topics. What powers these things? Lec. 24: Active Galaxies
Active Galaxies Lecture 24 APOD: M82 (The Cigar Galaxy) 1 Lecture Topics Active Galaxies What powers these things? Potential exam topics 2 24-1 Active Galaxies Galaxies Luminosity (L MW *) Normal < 10
More informationX-ray to UV variability correlation in MCG
A&A 430, 435 442 (2005) DOI: 10.1051/0004-6361:20041801 c ESO 2005 Astronomy & Astrophysics X-ray to UV variability correlation in MCG 6-30-15 P. Arévalo 1, I. Papadakis 2, B. Kuhlbrodt 3,4, and W. Brinkmann
More informationarxiv: v1 [astro-ph.he] 19 Jul 2013
Accepted to ApJ Letters on 18 July 2013 Preprint typeset using L A TEX style emulateapj v. 5/2/11 A DISTINCTIVE DISK-JET COUPLING IN THE LOWEST-MASS SEYFERT, NGC 4395 Ashley L. King 1, Jon M. Miller 1,
More informationDark Matter ASTR 2120 Sarazin. Bullet Cluster of Galaxies - Dark Matter Lab
Dark Matter ASTR 2120 Sarazin Bullet Cluster of Galaxies - Dark Matter Lab Mergers: Test of Dark Matter vs. Modified Gravity Gas behind DM Galaxies DM = location of gravity Gas = location of most baryons
More information