Galaxies with radio and optical jets Françoise Combes
|
|
- Basil Dalton
- 6 years ago
- Views:
Transcription
1 Chaire Galaxies et Cosmologie Galaxies with radio and optical jets Françoise Combes
2 The jet: component of the standard model Less than 10% of galaxies have an active nucleus. 10% of AGN have Radio jets («Radio-Loud») Every galaxy has a black hole but the activity time-scale is short, ~ million yrs According to the angle of the line of sight: the jet is seen, or relativistic motions, broad lines exist, or are hidden by the molecular torus (type 2, scattering, polarisation) 2
3 jet Distinction between jet and wind wind The wind comes from the heated disk, which can evaporate Or the magnetic pressure is too strong star BH disk Turbulence in the disk MRI instability magnetic lines 3
4 Activity cycles Separation of lobes ~ 100 kpc, V ~ 1000 km/s age t ~ 10 8 yrs Several cycles? Other way to estimate the duration of the activity cycles of AGN t ~ (galaxy life)(% active time) ~ (10 10 yrs)(1% of galaxies active with jets) ~ 10 8 yrs 4
5 Two types of morphologies for the radio jets High luminosity 3C 219 FR II (left) &FR I (right) 3C C 31 Low luminosity 3C 296 3C 47 Hot spots at the end 3C 465 Hot spots in the center 5
6 3C133 Image VLA Why only one jet? Faraday depolarisation~ 2 3C133 Polarisation Polarisation The visible jet is always towards the observer Laing, 1988 Eliminated hypothesis --The jet is alternatively on one side or the other --Absorbing medium 6
7 Relativistic aberration, Doppler boost Reference frame of the fluid Isotropic emission Reference frame of observer Lorentz transformation Already aberration at small speed (ex. rain) -- For AGN ~5 Flux multiplied by D 2 7
8 Total relativistic Doppler effect Doppler factor ~5 v/c ~ 0.98, D ~ 9.9 Aberration, Flux multiplied by D 2 Effect of time dilatation, Flux multiplied by D Time 1 Time 2 Time 3 Time 1 Time 2 Time 3 Source at rest Source in motion Doppler effect on frequencies, Flux in (synchrotron = 1) Flux multiplied by D 3+ ~D 4 ~ 9600 Some up to 100, D~200, and D 4 ~ !! S 8
9 Optical jets, various wavelengths Martel et al 2003
10 Superposition with Radio Jet radio: contours // optical jet (HST) 67kpc long HST+Merlin 10
11 HST Chandra Merlin 3C273, the most nearby quasar Jet detected at all wavelengths Superposition of optical jet (HST) in X-rays (Chandra) and in radio cm (Merlin) 11
12 12
13 Jets can be super-luminal P at velocity v, with respect to O y = r sin t = r/v J et radio dans 3C C279 Light coming from P reaches us in less time than light coming from O. Time observed for the object to go from O to P t app = t - x/c t app = (r/v) - (r/c) cos t app = (r/v) (1 - cos ) V apparent on the sky v app = y/t app v app = (v sin )/(1 - cos ) For v<<c c, =v/c ~0 v app =vsin For v ~ c, v app >> v and even larger than c To observer
14 Relativistic jets: a large range of scales High resolution Space Telescope + radio jet (VLA) 14
15 Black hole in rotation: origin of Radio jets? If the black hole is rotating, energy can be extracted from it, by the Penrose process 15
16 Penrose process E2 > E1 E<0 up to 29% E1 Jean-Pierre Luminet 16
17 Mechanism of Blandford-Znajek The goal is to extract energy and angular momentum from the black hole in rotation. The electromagnetic field around the hole is perturbed by magneto-spherical currents, which produce a torque Slow down the black hole Pair creation e+ - e- Poloidal B field, and B same sense Described by the potential vector A H Horizon Particules in T can only fall in the hole disk The positrons are quickly absorbed by the hole, The atmosphere is of negative charge 17
18 Blandford-Znajek (following) disk Poynting vector S= E x B / 18
19 Electromagnetic extraction of rotational energy S horizon Plasma dominated by magnetic energy ergosphere S S B B Flux of Poynting vector S Blandford and Znajek 1977 B Equatorial plane 19
20 Extraction MHD and not only MD Plasma dominated by magnetic energy S horizon v ergosphere Flux of vector of Poynting B S v v v S B Region dominated by particules Negative flux of particules Punsly & Coroniti 1990 S B Equatorial plane 20
21 Torque slowing down the black hole: Jx B Meridian plane Punsly & Coroniti 1990 Angular momentum L 21
22 Numerical simulations: MD & MHD Monopole field (Komissarov 2001, McKinney 2005) Z H Le flux of Poynting corresponds to model of Blandford-Znajek stationnary state a=0.5 a=0.1 a=0.9 t=120 Lorentz factor 0 Z R The energy is extracted from BH, the introduction of particules MHD does not change the phenomenon MD R MHD very similar to MD model a=0.9 from 0 to 14 22
23 Ergosphere and B field in simulations Simulations MD, uniform field (Komissarov 2004) B 2 D 2 h All field lines entering the Ergosphere are in rotation up to 0.5 times of hole horizon ergosphere The dissipative layer in the equatorial plane is the source of energy Dissipative layer The energie is extracted from the region between The energie is extracted from the region between horizon and ergosphere (=processus of Penrose) 23
24 Jets are confined by magnetic fields Collimation over 8 orders of magnitude in scales 24
25 MHD and jet confinement The differential rotation twists the field lines which slows down rotation and allows more accretion Magnetic pressure and thermal pressure accelerate the jet Magnetic tension collimates Uchida et al
26 Ejection mechanisms A black hole in rotation (a~1) accretes ionized and magnetized gas The gas falls in the hole, and some Electromagnetic energy is ejected along the rotation axis This energy flux (Poynting) will be charged with particules, to form a relativistic jet Similarity with the processus of Blandford-Znajek The reaction of the magnetic field is to accelerate the plasma in counter-rotation rotation of the hole Magnetic field lines Ergosphere Black hole Arrival of L < 0 Koide et al
27 The radio galaxies are in general Ellipticals, may b b M M be because M BH ~M bulbe NGC 7052 NGC 4261
28 Galaxies host Cen A of FR-Is and FR-IIs The radio galaxies FR I and FR II are Giant ellipticals with dust lanes The FRI are often cd galaxies at the center of rich clusters M87 28
29 The majority of quasars are observed in galaxy mergers Violent gas shocks fueling of the black hole
30 Ejection of plasma: radio lobes in ellipticals, results of merers Cygnus A Image radio, VLA Optical mage, HST 30
31 A double quasar, just merging: 3C75, z=0.023 Image radio, VLA Optical limage HST 25,000 ly 31
32 Radio lobes, galaxies in motion 3C129 Galaxies move at a velocity up to 1000km/s in galaxy clusters 3C465 32
33 How two radio lobes can merge in a signle one NGC 1265, Perseus cluster 33
34 Weaker radio sources: more diffuse lobes Radio, VLA NGC 1316 in Fornax HST
35 Origin of radio mission : Power-law spectrum decreasing with frequency (slope 0 at nucleus, then -1) linearly polarised emission (at least 30%, which is a lot) Synchrotron radiation emitted by electrons in relativistic motion in a magnetic field For an electron of energy 2 2 v E m e c avec γ 1 1 γ 2 The characteristic frequency of emission is 6 2 c ~ γ B Hz With B in Gauss c 35
36 Emission gamma (TeV) from a blazar Very high energy photons are emitted by radio AGN, when their jet is oriented towards the observer blazar & «Flat Spectrum Radio Quasar» (FSRQ) Doppler factors of 20-50! 36 Marscher 2005
37 Jets in Gamma: high variability Radiation mechanisms: synchrotron, SSC (synchrotron (y self-compton) & EIC (external inverse Compton) At low power: SSC At high power: EIC Variability on time scales down to minutes 37
38 The blazar sequence The highest luminosity blazars have the softest spectra Electrons of high energy In low power objects injection between min = to At high L, min is smaller 38
39 Mechanisms of photons in culture B-field 2. Pair production 3. Compton scattering 3. Compton scattering 1. Seed high- 5. Compton 4. Pair energy photon scattering production Multiplication of high energy rays, as soon as (1) high energy photons are injected (2) there exists a B field transverse or chaotic (3) () an isotropic radiation field (BLR at cm) (4) the Lorentz factor of the jet ~4-10 Stern & Poutanen (2006, 2008) 39
40 Why some AGN have radio jets and not others? Frequency and circumstances: Most AGN have no jet, 90% are «Radio-Quiet» 10% of «Radio-Loud»: a true dichotomie Are these different phases of an universal evolution? R=Radio/Optical Centaurus A Blue: X-rays Red: Radio Kellerman
41 Two sequences in the plane L B L R 41
42 Same sequences in (L B /L Edd )-(L R /L Edd ) This time normalised to L Edd (M BH /M ) erg/s 42
43 R~ L R /L B, accretion rate ~ L acc /L Edd 43
44 Criteria for radio jets 1) The parameter R increases when the accretion rate L acc /L Edd decreases 2) This is verified for both sequences «radio-loud» and «radio-quiet» 3) A saturation of the parameter R occurs at low accretion rate λ <
45 Dependence of R on the mass of the BH For powerful radio jets, M BH must be > 10 8 M 45
46 The micro-quasars in our Galaxy: nearby, variable at human time-scale SS433: micro-quasar Objects of stellar masses The end of life for massive stars Rotation of the BH 1000 times 46 per second
47 Microquasars & Quasars 47
48 Micro-quasar GRS 1915 superluminal velocity Scale: one month X-Rays: red Gamma-rays: grenn Radio : blue Ejection cycles of about one hour A dizain per day 48
49 Radio versus X for micro-quasars S radio S X S X For low accretion rates, the radio luminosity increases with the accretion rate (L X ) like L R L 0.7 X (Gallo et al. 2003) But for higher accretion rates 001Edd 0.01, the jet production becomes intermittent (Fender et al., 2004) 49
50 The accretion phases vary for example Cyg X-1 Accretion High (H) (small truncation radius) Accretion low (L) (higher truncation radius) Transitions Energy emitted in photons Compton H L 50
51 Fender ? 0.1? The different phases Instable Intermittent Micro-quasars & AGN The hard X are correlated with the radio emission In the high luminosity phase, the disk radiates efficiently, and electrons are not emitted Disque mince In the low phase, ADAF Pas de jet ni Truncation of the disk, formation de couronne of a corona where photons are comptonized (hard X-rays) Disque tronqué Couronne et jet continu The corona is the jet base51
52 Several phases for the Seyfert Seyferts 1 in general accrete at the Eddington limit this corresponds to a high accretion rate, unstable -- oscillation time-scale of ~ 2 yr (M/10 6 M ) Some Seyfert galaxies have no longer broad lines Narrow Line S1 example NLS1 PKS M = M ; could become a classical S 1 in < 10 yr A brighter AGN, broader lines 52
53 Criteria for radio jets For AGNs as for micro-quasars, L R and L acc are related for the low accretion rates, and for high accretion rates, the production of jets become intermittent (e.g., Merloni et al., 2003, Nipoti et al., 2005) But the relations are verified separately for spirals and ellipticals, as for two parallel relations there exists an other parameter, related to the formation of these galaxies, and of their central black hole The spin of the black hole? 53
54 The role of the black hole spin If jets are produced by the extraction of the rotational energy of black holes and if elliptical galaxies have more luminous radio jets -- does this mean that ellipticals have not enough gas to stop the jets? -- or ellipticals have higher spin parameters (a)? Ellipticals are formed by mergers of smaller galaxies, but more frequently by major mergers Alargenumber of minor mergers could arrive in the same final mass state, but the spin would be cancelled statistically 54
55 Minor & major mergers The final angular momentum coming from several BH of random orientation cancels out Aresidual spin is expected for the black hole resulting from amajormerger merger 55
56 Simulations of jet formation Brinkmann & Brinkmann Camenzind 2004 & Camenzind LSW
57 Esin et al A. Müller (2004) 57
58 Unstable: Oscillations sity Luminos Fender & Belloni 2004 ARAA Frequency 58
59 Conclusions Properties of jets -- relativistic boost, disymmetry y -- superluminal jets -- analogy with micro-quasars -- The radio power is 3 orders of magnitude larger in ellipticals relative to spirals How are jets formed? -- Extraction of the rotational energy of the BH (Blandford-Znajek) (processus of Penrose + B field) -- the radio power increases when the accretion rate decreases Ellipticals have black holes with a larger spin ( a~1) Could be due to their formation in major mergers 59
Active 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 informationChapter 17. Active Galaxies and Supermassive Black Holes
Chapter 17 Active Galaxies and Supermassive Black Holes Guidepost In the last few chapters, you have explored our own and other galaxies, and you are ready to stretch your scientific imagination and study
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 informationVera Genten. AGN (Active Galactic Nuclei)
Vera Genten AGN (Active Galactic Nuclei) Topics 1)General properties 2)Model 3)Different AGN-types I. Quasars II.Seyfert-galaxies III.Radio galaxies IV.young radio-loud AGN (GPS, CSS and CFS) V.Blazars
More informationA zoo of transient sources. (c)2017 van Putten 1
A zoo of transient sources (c)2017 van Putten 1 First transient @ first light UDFj-39546284, z~10.3 Bouwens, R.J., et al., Nature, 469, 504 Cuchiara, A. et al., 2011, ApJ, 736, 7 z=9.4: GRB 090429B, z~9.4
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 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 informationMagnetic Fields in Blazar Jets
Magnetic Fields in Blazar Jets Bidzina Z. Kapanadze Ilia State University, Tbilisi, Georgia MFPO 2010- Cracow, May 17-21 Blazars are defined as a AGN class with following features: featureless spectra;
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 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 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 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 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 informationOutflows & Jets: Theory & Observations
Outflows & Jets: Theory & Observations Lecture winter term 008/009 Henrik Beuther & Christian Fendt 10.10 17.10 4.10 31.10 07.11 14.11 1.11 8.11 05.1 1.1 19.1 6.1 09.01 16.01 3.01 30.01 Introduction &
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 informationA Unified Model for AGN. Ryan Yamada Astro 671 March 27, 2006
A Unified Model for AGN Ryan Yamada Astro 671 March 27, 2006 Overview Introduction to AGN Evidence for unified model Structure Radiative transfer models for dusty torus Active Galactic Nuclei Emission-line
More informationExtragalactic Radio Sources. Joanne M. Attridge MIT Haystack Observatory
Extragalactic Radio Sources Joanne M. Attridge MIT Haystack Observatory It all began in the 1940s... Galaxies=condensations of gas, dust and stars held together by their own gravitational potential M 87
More informationActive Galactic Alexander David M Nuclei
d.m.alexander@durham.ac.uk Durham University David M Alexander Active Galactic Nuclei The Power Source QuickTime and a YUV420 codec decompressor are needed to see this picture. Black hole is one billionth
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 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 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 informationTheoretical aspects of microquasars
Theoretical aspects of microquasars Bingxiao Xu Department of Physics & Astronomy, GSU ABSTRACT: Microquasars (black hole X-ray binaries with relativistic jets) are first found by means of multiwavelengths
More informationACTIVE GALACTIC NUCLEI: FROM THE CENTRAL BLACK HOLE TO THE GALACTIC ENVIRONMENT
Julian H. Krolik ACTIVE GALACTIC NUCLEI: FROM THE CENTRAL BLACK HOLE TO THE GALACTIC ENVIRONMENT PRINCETON UNIVERSITY PRESS Princeton, New Jersey Preface Guide for Readers xv xix 1. What Are Active Galactic
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 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 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 informationAn introduction to Active Galactic Nuclei. 1.
An introduction to Active Galactic Nuclei. 1. Paolo Padovani, ESO, Germany The beginning AGN main properties The AGN zoo: radio-quiet and loud AGN, Unified Schemes, and relativistic beaming AGN masses
More informationHigh-Energy Astrophysics
Oxford Physics: Part C Major Option Astrophysics High-Energy Astrophysics Garret Cotter garret@astro.ox.ac.uk Office 756 DWB Michaelmas 2011 Lecture 9 Today s lecture: Black Holes and jets Part I Evidence
More informationActive Galactic Nuclei (AGNs): A type of AGNs: Quasars. Whatever is powering these QSO s must be very small!!
Active Galactic Nuclei (AGNs): Galaxies with lots of activity AST 101 General Astronomy: Stars & Galaxies Some galaxies at high redshift (large lookback times) have extremely active centers More than 1000
More informationSpins of Supermassive Black Holes. Ruth A. Daly
Spins of Supermassive Black Holes Ruth A. Daly Three key quantities characterize a black hole: mass, spin, and charge. Astrophysical black holes are thought to have zero net charge, and thus are characterized
More informationObservations of jet dissipation. Robert Laing (ESO/Oxford)
Observations of jet dissipation Robert Laing (ESO/Oxford) Overview X-ray radio connections in radio galaxies and quasars: High-energy emission from non-thermal electrons. The interaction of radio galaxies
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 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 informationAGN in hierarchical galaxy formation models
AGN in hierarchical galaxy formation models Nikos Fanidakis and C.M. Baugh, R.G. Bower, S. Cole, C. Done, C. S. Frenk Physics of Galactic Nuclei, Ringberg Castle, June 18, 2009 Outline Brief introduction
More informationActive Galaxies & Emission Line Diagnostics
Active Galaxies & Emission Line Diagnostics Review of Properties Discussed: 1) Powered by accretion unto a supermassive nuclear black hole 2) They are the possible precursors to luminous massive galaxies
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 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 informationGalaxies and Cosmology
F. Combes P. Boisse A. Mazure A. Blanchard Galaxies and Cosmology Translated by M. Seymour With 192 Figures Springer Contents General Introduction 1 1 The Classification and Morphology of Galaxies 5 1.1
More informationGamma-ray emitting narrow-line Seyfert 1 galaxies and their place in the AGN zoo
Gamma-ray emitting narrow-line Seyfert 1 galaxies and their place in the AGN zoo Filippo D Ammando (DIFA and INAF-IRA Bologna) Monica Orienti, Justin Finke, Marcello Giroletti, Josefin Larsson on behalf
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 informationSet 4: Active Galaxies
Set 4: Active Galaxies Phenomenology History: Seyfert in the 1920;s reported that a small fraction (few tenths of a percent) of galaxies have bright nuclei with broad emission lines. 90% are in spiral
More informationThe AGN / host galaxy connection in nearby galaxies.
The AGN / host galaxy connection in nearby galaxies. A new view of the origin of the radio-quiet / radio-loud dichotomy? Alessandro Capetti & Barbara Balmaverde (Observatory of Torino Italy) The radio-quiet
More informationGlobal Simulations of Black Hole Accretion. John F. Hawley Department of Astronomy, University of Virginia
Global Simulations of Black Hole Accretion John F. Hawley Department of Astronomy, University of Virginia Collaborators and Acknowledgements Julian Krolik, Johns Hopkins University Scott Noble, JHU Jeremy
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 informationObservational Evidence of AGN Feedback
10 de maio de 2012 Sumário Introduction AGN winds Galaxy outflows From the peak to the late evolution of AGN and quasars Mergers or secular evolution? The AGN feedback The interaction process between the
More informationInstabilities of relativistic jets
Instabilities of relativistic jets G. Bodo INAF Osservatorio Astrofisico di Torino, Italy A. Mignone, P. Rossi, G. Mamatsashvili, S. Massaglia, A. Ferrari show f Universality of relativistic jet phenomenon
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 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 information(Astro)Physics 343 Lecture # 12: active galactic nuclei
(Astro)Physics 343 Lecture # 12: active galactic nuclei Schedule for this week Monday & Tuesday 4/21 22: ad hoc office hours for Lab # 5 (you can use the computer in my office if necessary; Sections A
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 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 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 informationRadio Loud Black Holes. An observational perspective
Radio Loud Black Holes An observational perspective Tiziana Venturi INAF, Istituto di Radioastronomia, Bologna Overview of the first lesson 1) Synchrotron emission and radio spectra of AGN 2) Classification
More informationLecture 11 Quiz 2. AGN and You. A Brief History of AGN. This week's topics
Lecture 11 Quiz 2 AGN and You March 25 2003 8:00 PM BPS 1420 1. What system of time do astronomers use rather than the standard day-month-year system? 2. In that system, how long would it be between noon
More informationGalaxies. Galaxy Diversity. Galaxies, AGN and Quasars. Physics 113 Goderya
Galaxies, AGN and Quasars Physics 113 Goderya Chapter(s): 16 and 17 Learning Outcomes: Galaxies Star systems like our Milky Way Contain a few thousand to tens of billions of stars. Large variety of shapes
More informationEvidence for BH: Active Galaxies
Evidence for BH: Active Galaxies This is the second lecture in which we ll talk about evidence for the existence of black holes in the universe. Here we focus on active galactic nuclei, or AGN. Black holes
More informationFocussing on X-ray binaries and microquasars
Focussing on X-ray binaries and microquasars Didier BARRET Centre d Etude Spatiale des Rayonnements Toulouse, France Thank you Peter and Dolorès and the organizing committee I will start with the conclusions
More informationBlack holes as central engines
Chapter 15 Black holes as central engines Black holes imply a fundamental modification of our understanding of space and time. But at a more mundane level they also are of great practical importance in
More informationStructure of nuclei of extragalactic radio sources and the link with GAIA
Structure of nuclei of extragalactic radio sources and the link with GAIA J Roland, IAP & S Lambert, SYRTE I General properties of extragalactic radio sources Radio galaxies : associated with elliptical
More informationToday in Astronomy 142: supermassive black holes in active-galaxy nuclei
Today in Astronomy 142: supermassive black holes in active-galaxy nuclei Active-galaxy nuclei (AGNs) Relativistic and superluminal motion in quasar jets Radio galaxies, quasars and blazars: the same objects
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 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 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 information* What are Jets? * How do Jets Shine? * Why do Jets Form? * When were Jets Made?
* What are Jets? * How do Jets Shine? * Why do Jets Form? * When were Jets Made? 1 * Galaxies contain massive black holes which power AGN * Gas accretes through a magnetized disk * Blazars are relativistically
More informationRadio Galaxies High resolution observations of radio galaxies often show highly extended emission. Best known case: Cygnus A. Jet.
Radio Galaxies High resolution observations of radio galaxies often show highly extended emission. Best known case: Cygnus A Lobe Jet Nucleus Hotspot Emission is synchrotron radiation Physical extent can
More informationHigh-Energy Astrophysics Lecture 1: introduction and overview; synchrotron radiation. Timetable. Reading. Overview. What is high-energy astrophysics?
High-Energy Astrophysics Lecture 1: introduction and overview; synchrotron radiation Robert Laing Lectures: Week 1: M 10, T 9 Timetable Week 2: M 10, T 9, W 10 Week 3: M 10, T 9, W 10 Week 4: M 10, T 9,
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 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 informationBH Astrophys Ch1~2.2. h"p://www.astro.princeton.edu/~burrows/classes/250/distant_galaxies.html h"p://abyss.uoregon.edu/~js/ast123/lectures/lec12.
BH Astrophys Ch1~2.2 h"p://www.astro.princeton.edu/~burrows/classes/250/distant_galaxies.html h"p://abyss.uoregon.edu/~js/ast123/lectures/lec12.html Outline Ch1. 1. Why do we think they are Black Holes?(1.1-1.2)
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 informationGAMMA-RAYS FROM MASSIVE BINARIES
GAMMA-RAYS FROM MASSIVE BINARIES W lodek Bednarek Department of Experimental Physics, University of Lódź, Poland 1. Sources of TeV gamma-rays PSR 1259+63/SS2883 - (HESS) LS 5039 - (HESS) LSI 303 +61 o
More informationPart 2. Hot gas halos and SMBHs in optically faint ellipticals. Part 3. After Chandra?
Hot gas and AGN Feedback in Nearby Groups and Galaxies Part 1. Cool cores and outbursts from supermassive black holes in clusters, groups and normal galaxies Part 2. Hot gas halos and SMBHs in optically
More informationDiversity of Multi-wavelength Behavior of Relativistic Jet in 3C 279 Discovered During the Fermi Era
Diversity of Multi-wavelength Behavior of Relativistic Jet in 3C 279 Discovered During the Fermi Era Rapid Variability of Blazar 3C 279 during Flaring States in 2013-2014 with Joint Fermi-LAT, NuSTAR,
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 informationPowering Active Galaxies
Powering Active Galaxies Relativity and Astrophysics ecture 35 Terry Herter Bonus lecture Outline Active Galaxies uminosities & Numbers Descriptions Seyfert Radio Quasars Powering AGN with Black Holes
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 information3D GRMHD Jet Simulations [and other stuff] Jonathan McKinney Stanford/KIPAC
3D GRMHD Jet Simulations [and other stuff] Jonathan McKinney Stanford/KIPAC Issues Addressed Radio Loud/Quiet Dichotomy Caused by Environment, Spin, Galaxy Evolution? Magnetosphere near BH How different
More informationMicroquasars and The Power of Spin
Microquasars and The Power of Spin Ralph Spencer, Tony Rushton with thanks to Mr Tony Blair COST Valencia 2010 1 Overview What are Microquasars? A bit of history A gallery of objects The link to AGN A
More informationEvidence for BH: Active Galaxies
Evidence for BH: Active Galaxies This is the first of two lectures in which we ll talk about evidence for the existence of black holes in the universe. It is actually in the next lecture, where we ll talk
More informationOther Galaxy Types. Active Galaxies. A diagram of an active galaxy, showing the primary components. Active Galaxies
Other Galaxy Types Active Galaxies Active Galaxies Seyfert galaxies Radio galaxies Quasars Origin??? Different in appearance Produce huge amount of energy Similar mechanism a Galactic mass black hole at
More informationRadiative Processes in Astrophysics
Radiative Processes in Astrophysics 11. Synchrotron Radiation & Compton Scattering Eline Tolstoy http://www.astro.rug.nl/~etolstoy/astroa07/ Synchrotron Self-Absorption synchrotron emission is accompanied
More informationHigh-Energy Astrophysics
Part C Major Option Astrophysics High-Energy Astrophysics Garret Cotter garret@astro.ox.ac.uk Office 756 DWB Lecture 10 - rescheduled to HT 2013 Week 1 Today s lecture AGN luminosity functions and their
More informationVLBI observations of AGNs
VLBI observations of AGNs Gabriele Giovannini Dipartimento di Astronomia, Universita di Bologna Istituto di Radioastronomia - INAF OUTLINE Single sources: Mkn 501 1144+35 Sample: nearby BL-Lacs nearby
More informationThe extreme ends of the spectrum: the radio/gamma connection
The extreme ends of the spectrum: the radio/gamma connection Monica Orienti INAF IRA Bologna Astronomy Department, Bologna University This research has made used of data from the MOJAVE database that is
More informationQuasars: Back to the Infant Universe
Quasars: Back to the Infant Universe Learning Objectives! What is a quasar? What spectral features tell us quasars are very redshifted (very distant)? What spectral features tell us they are composed of
More informationPolarization Studies of Extragalactic Relativistic Jets from Supermassive Black Holes. Iván Agudo
Polarization Studies of Extragalactic Relativistic Jets from Supermassive Black Holes Iván Agudo What is an active galactic nuclei (AGN)? Compact regions at the centre of galaxies with much higher than
More informationPERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY. Paolo Lipari Vulcano 27 may 2006
PERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY Paolo Lipari Vulcano 27 may 2006 High Energy Neutrino Astrophysics will CERTAINLY become an essential field in a New Multi-Messenger Astrophysics What is
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 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 informationActive Galactic Nuclei-I. The paradigm
Active Galactic Nuclei-I The paradigm An accretion disk around a supermassive black hole M. Almudena Prieto, July 2007, Unv. Nacional de Bogota Centers of galaxies Centers of galaxies are the most powerful
More informationRADIO OBSERVATIONS AND THEIR PHYSICAL INTERPRETATIONS
A project report on RADIO OBSERVATIONS AND THEIR PHYSICAL INTERPRETATIONS By: Shishir Sankhyayan MSc-II Department of Physics University of Pune-411007 Guided by: Dr. Joydeep Bagchi IUCAA, Pune 1 Abstract
More informationJet Physics: implications for feedback. Robert Laing (ESO)
Jet Physics: implications for feedback Robert Laing (ESO) Aims Quantify the physics of jets in low-power radio galaxies by fitting 3D models to very deep, high-resolution radio images. Geometry Velocity
More informationAstronomy 102 Lecture 17
Today in Astronomy 102: supermassive black holes in active galaxy nuclei (AGNs) q Active galaxies: quasars, radio galaxies and their relatives. q Why the observations imply that they have supermassive
More informationThis week at Astro 3303
This week at Astro 3303 Lecture 12, Oct 04, 2017 Pick up PE#12 Today: HW#4 discussion AGN & supermassive black holes Reading: Chapter 3.5 & 10.4-10.5 of textbook à HW#4 discussion NGC1068/M77 Components:
More informationSet 4: Active Galaxies
Set 4: Active Galaxies Phenomenology History: Seyfert in the 1920 s reported that a small fraction (few tenths of a percent) of galaxies have bright nuclei with broad emission lines. 90% are in spiral
More informationRyosuke Itoh. Tokyo Institute of technology.
Ryosuke Itoh Tokyo Institute of technology 2017-06-13 @Ierapetra Partial travel support to the conference was provided by RadioNet. RadioNet has received funding from the European Union s Horizon 2020
More informationStellar Jets. Tom Maccarone (University of Southampton)
Stellar Jets Tom Maccarone (University of Southampton) This presentation draws heavily on an article by myself and Elmar Koerding from the December 2006 edition of Astronomy & Geophysics. ING archive/nick
More informationMagnetically-dominated relativistic jets.
Magnetically-dominated relativistic jets. Serguei Komissarov University of Leeds UK N.Vlahakis, Y.Granot, A.Konigl, A.Spitkovsky, M.Barkov, J.McKinney, Y.Lyubarsky, M.Lyutikov, N.Bucciantini Plan 1. Astrophysical
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 information