Radio Galaxies. D.Maino. Radio Astronomy II. Physics Dept., University of Milano. D.Maino Radio Galaxies 1/47

Save this PDF as:
 WORD  PNG  TXT  JPG

Size: px
Start display at page:

Download "Radio Galaxies. D.Maino. Radio Astronomy II. Physics Dept., University of Milano. D.Maino Radio Galaxies 1/47"

Transcription

1 Radio Galaxies D.Maino Physics Dept., University of Milano Radio Astronomy II D.Maino Radio Galaxies 1/47

2 Active Galactic Nuclei AGN: nuclei of galaxies with energetic phenomena that can not clearly and directly attributed to stars D.Maino Radio Galaxies 2/47

3 Active Galactic Nuclei Luminous UV emission from compact region in the center Doppler-broad emission lines High variability of days,months time scales Non-thermal emission Compact Radio Core Extenced linear radio structures (jets+hotspots) X-ray, γ-ray and (also) TeV emission CR production D.Maino Radio Galaxies 3/47

4 History of AGN Two main classes of AGN: Seyfert galaxies: often spiral with L L gal Quasars: often elliptical with L > 100 L gal D.Maino Radio Galaxies 4/47

5 History of AGN 1908: Fath& Slipher detect strong emission lines similar to PN with width of few 100km/s in NGC 1068 D.Maino Radio Galaxies 5/47

6 History of AGN: Seyfert galaxies Galaxy centers show broad lines High-excitation emission lines What is the source of broad lines? D.Maino Radio Galaxies 6/47

7 History of AGN: First detection of Optical jets 1923: Curtis detected jets in M87 D.Maino Radio Galaxies 7/47

8 History of AGN: Hubble discovery 1926: Hubble discovers the expansion of the universe nebulae are indeed extra-galactic objects 1943: Seyfert finds multiple galaxies similar to NGC1068 (hence their name) 1955: Detector of radio emission from NGC : First insight on Seyfert galaxies (Woltjer): unresolved nuclei (< 100pc) nuclear emission last for > 10 8 yr (1/100 of spirals are Seyfert and universe is yr old) nuclear mass is high if broadening is caused by bounded material (M v 2 r/g 10 9 M ) D.Maino Radio Galaxies 8/47

9 History of AGN: first Radio Surveys Early radio surveys played a crucial role in discovering quasars 3C: third cambridge catalogue (1959) at 159MHz (> 9Jy) basis for extra-galactic radio astronomy, cosmology and quasars! PKS: Parkes (> 4Jy) (> 1Jy) 4C: fourth cambridge (now 8): deeper/smaller AO: Aricibo Occulation survey Mostly normal galaxies (i.e. thermal emission of spirals) Stars with strange broad emission lines D.Maino Radio Galaxies 9/47

10 Radio Galaxy Emission Typical ( normal ) radio emission from a galaxy is due to: synchrotron radiation: e and other c-rays moving in the galactic magnetic field - S ν 0.7/ 0.9 free-free emission from Hii regions - S ν 0.15 thermal emission from dust heated by stellar radiation - S B(T )ν 1.5 D.Maino Radio Galaxies 10/47

11 History of AGN: Discovery of Quasars 3C273: the 273 source in the 3C catalogue Compact radio sources, star like but for a wisp of light D.Maino Radio Galaxies 11/47

12 Radio Properties of Quasars Although quasars discovered with radio they always are quite faint at radio wavelenghts Two main components: Compact: < 1 with flat spectrum, optically thick and also have clear optical source Extended: usually double lobes with steep spectra and optically thin D.Maino Radio Galaxies 12/47

13 Classes of (extended) Radio-Galaxies Large radio-galaxies with lobes can be divided into two types from Fanaroff-Riley (1974) FRI: weaker radio sources, bright at the center and fainter toward the edges FRII: collimated jets with hotspots L 1.4GHz = ergs/s/hz D.Maino Radio Galaxies 13/47

14 Classes of (extended) Radio-Galaxies D.Maino Radio Galaxies 14/47

15 The Zoo of AGN Diagnostic via BPT (Baldwin, Phillips & Telervich) diags. Why these lines? In general lines are sensitive to different parameters affecting the ISM (T, ρ, ionizing field, etc.) [OIII]/[OII]: is sensitive to ionization parameter (i.e. how the gas is ionized) [OI]/H α : is sensitive to hardness (energy) of radiation field D.Maino Radio Galaxies 15/47

16 The Zoo of AGN: Seyfert Seyfert type depends on the width of the optical lines Sy2: narrow emission lines FWHM few 100km/s Sy1: broad permitted lines (Hα,HeII,..) of δv < 10 4 km/s from high density n e > 10 9 cm 3 and narrow forbidden lines ([OIII],[NII]) from low density n e cm 3 Sy1.x(1.9,1.8,..): increase with width of Hα and Hβ lines NL Sy1: subclass of Sy2 with X-ray excess and optical FeII emission D.Maino Radio Galaxies 16/47

17 The Zoo of AGN: Quasars and QSO Quasars: Quasi Stellar Radio sources QSO: Quasi Stellar Object Scaled version of Seyfert where nucleus is very luminous M b < 21.5 Often star-like Spectra similar to Sy 1 but with weaker NL Either Radio-Loud QSOs or Radio-Quiet QSOs with transition at P 5GHz W/Hz/sr. RL QSOs are only 5-10% of total QSOs D.Maino Radio Galaxies 17/47

18 The Zoo of AGN: BL Lac BL Lac: is the protorype of its class. Star like with very weak emission lines and variable, intense and polarized continuum. Lines appear during quiescent phases Blazars: Encompass BL Lacs and optically violent-variable (OVV) QSOs. Strong relativistically beamed jet along the los D.Maino Radio Galaxies 18/47

19 Unification Scheme? Postulate a standard model for the structure of AGN Radio galaxies, quasars, QSOs, Seyfert, BL Lacs are indeed the same type of object what s the origin of the difference? The angle is everything: viewing angle makes the differnce Centre of a galaxy is a Black Hole surrounded by an accretion disk, together with clouds of gas and a dusty torus Energy output comes from accretion of material onto the BH D.Maino Radio Galaxies 19/47

20 Unification Scheme! D.Maino Radio Galaxies 20/47

21 Standard Model of AGN Accretion disk: r 10 3 pc, n cm 3 and v 0.3c Broad Line Region: r pc, n cm 3 and v few 10 3 km/s Torus: r 1 100pc, n cm 3 Narrow Line Region: r pc, n cm 3 and v few 100km/s D.Maino Radio Galaxies 21/47

22 Unification of AGNs D.Maino Radio Galaxies 22/47

23 Support to Unification BLR near nucleus is obscured by torus in Sy2. Hot scattered e from BLR can arrive to observer Sy2 is like Sy1 in polarised light Ionization cones: UV emission comes from the accretion disk and light up a cone of gas away from the torus that absorbs part of it All Seyfert galaxies have a NLR with very similar properties Size of Sy 1 continuum emitting regions are smaller than those of Sy 2 Direct image of torus D.Maino Radio Galaxies 23/47

24 Image of Torus D.Maino Radio Galaxies 24/47

25 FIR/Radio Correlation Van der Kruit (1971) discovered a correlation in a Seyfert (AGN) galaxy between luminosity at 10µm and at 1415 MHz Extended and verified for normal galaxies thanks to the IRAS satellite from which ( ) ( ) FIR 2.58 Wm 2 = S60µm + S 100µm Jy total flux 40µm < λ < 120µm Define ( q log FIR Wm 2 ) ( log S ν Wm 2 Hz 1 q log version of ratio: σ q 0.2 and q = 2.3 at 1.4 GHz ) D.Maino Radio Galaxies 25/47

26 FIR/Radio Correlation D.Maino Radio Galaxies 26/47

27 Radio Galaxies Cyngnus A from 2cm D.Maino Radio Galaxies 27/47

28 Why Study Radio-Loud AGN? Comparison between radio-load AGN and optical AGN samples origin of radio-loudness Some radio and soft X-ray AGN show little or no line emission include AGN missed from emission-line selection Radio activity is an efficient mean of feeding AGN energy directly back into environment (e.g. sound waves) role of AGN feedback on environment Radio galaxies and Radio-loud quasars are the most powerfull radio sources but radio is a small fraction of the total amount of energy 10 4 of optical output D.Maino Radio Galaxies 28/47

29 Derive SED from radio surveys There are several mechanism acting to contribute to the SED: relativistic e can loose energy by adiabatic expansion, synch. inverse Compton, etc We already know that N(E) varies with time both for adiabatic expansion (decrease in L but spectrum unchanged) and by radiation E = B 2 t 1/2 ν break B 3 t 2 yr For ν < ν break spectra index is unchanged For ν > ν break α = α 0 1/2 D.Maino Radio Galaxies 29/47

30 Derive SED from radio surveys Energy lost affects mainly large scale structures (e.g. lobes) Typical α = 0.7 for radio lobes ( ) B 3/2 ( ν ) 1/2 t 1/2 = Myr µg GHz D.Maino Radio Galaxies 30/47

31 Self-absorption in the relativistic e gas Optically thick case: consider internal absorption of e T b is close to the kinetics temperature of e Opacity larger at lower ν plasma opaque at low-ν and transparent at high τ 1 S(ν) ν 5/2 B 1/2 dω Mainly in the central compact region or very small radio sources Higher turnover frequency smaller size of emitting region D.Maino Radio Galaxies 31/47

32 Self-absorption in the relativistic e gas D.Maino Radio Galaxies 32/47

33 Polarization Synchrotron emission is highly polarized For an uniform B, the polarization of an ensemble of e is linear, normal to B and with fraction p = 3α + 3 3α + 7 Expected aroung 70-80% with 2 < α < 4 but observed up to 20% tangled B D.Maino Radio Galaxies 33/47

34 Different types of Radio Galaxies Morphology of radio galaxies could be different for several reasons: radio power propably related to AGN power orientaton of the radio emisson instrinsic differences in the (nuclear regions of ) host galaxy environment D.Maino Radio Galaxies 34/47

35 Different types of Radio Galaxies D.Maino Radio Galaxies 35/47

36 Different types of Radio Galaxies Morphology does not depend on size D.Maino Radio Galaxies 36/47

37 Different type of Radio Galaxies Interaction with environment D.Maino Radio Galaxies 37/47

38 Fanaroff-Riley Type I and II FRII: high radio power with very bright edges (hot-spots) collimated jets, B to jets, high Mach number (supersonic jet) backflow steep spectral index from hot-spot to nucleus FRI: low radio power large opening angle jet, B to jets, low Mach number fain lobes spectral index steep away from nucleus D.Maino Radio Galaxies 38/47

39 Fanaroff-Riley Type I and II Reasons for differences are not totally clear; likely related to nuclear region Different seen also in other wavebands Possible impact from environment: low-power radio galaxies are usually in clusters Not only morphological but also physical: strong separation in M b F 1400 plane D.Maino Radio Galaxies 39/47

40 Source of AGN power Main source is accretion onto the central BH Before entering matter is heated by friction to high temperatures (X-ray emission) BH radius is R S = 2GM BH c 2 = few light hours Energy available for a mass m at distance R S? E max = GM BHm R S = 1 2 mc2 Half the rest energy of the infalling mass is converted into kinetic energy If mass is decelerated by friction KE into thermal energy with efficiency η < 0.5 (usually η = 0.1) D.Maino Radio Galaxies 40/47

41 Source of AGN power Since L is de/dt for an AGN we have L = η dm dt c2 The MW has a luminosity of 1000L dm/dt 10 9 M /yr If with η = 0.1 we assume 1M per year we will have L = η dm dt c2 = ( ) 2 = L 100 times brighter than the entire MW D.Maino Radio Galaxies 41/47

42 The Eddington limit This is the maximum L for a given BH mass Two forces in balance: outward flow of photons gravitational force from infall material du dt = p ρ Φ = 0 If pressure is dominated by radiation with flux F p ρ = k c F where k = σ T /m p is the opacity (for hydrogen) If opacity is constant, with Gauss Theorem and Poisson eq. L = c Φ ds = c 2 ΦdV = 4πGc ρdv = 4πGMc k s k V k v k D.Maino Radio Galaxies 42/47

43 The Eddington limit Subs. the expression for k we obtain L Edd = 4πGMm ( ) pc M = L σ T M Evidence of SMBH found in most galaxies Relation between BH M and M b and σ e D.Maino Radio Galaxies 43/47

44 Superluminal motion Some radio-galaxies, BL Lac and Quasars show evindence of jets (or part of them) apparently moving faster than light Observed in 1970 and was used to move Quasar from cosmological distance: optical illusions plausible within SR They are indeed optical illusions but Quasars are at cosmological distances! D.Maino Radio Galaxies 44/47

45 Superluminal motion What is important here is the angle between jet and line-of-sight The jet is moving with v c along AB. At time t 1 a ray from the jet starts in A while at t 2 another ray starts at B. Observing times are t 1 and t 2 Elasped time is δt so AB = vδt and we can find AC and BC t 2 = t 2 + D L /c, t 1 = t 1 + D L /c + vδtcosθ/c δt = δt + vδtcosθ/c = δt (1 βcosθ) D.Maino Radio Galaxies 45/47

46 Superluminal motion The apparent jet motion is BC = D L sinφ D L φ But D L φ = vδtsinθ and the apparent transverse velocity v T along BC is v T = φd L δt = vsinθ 1 βcosθ β T = v T c = βsinθ 1 βcosθ D.Maino Radio Galaxies 46/47

47 Superluminal motion Find angle θ for maximum β T β T θ = 0 cosθ max = β sinθ max = 1 β 2 = 1 γ βmax T = βγ Therefore for γ 1 - the jet is moving with v c - even if β < 1 one can get βt max > 1 and hence superluminal motion since v T is the only velocity we can measure. D.Maino Radio Galaxies 47/47

Active Galactic Nuclei

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 information

Introduction to AGN. General Characteristics History Components of AGN The AGN Zoo

Introduction 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 information

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.

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. 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 information

Astr 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 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 information

Active galactic nuclei (AGN)

Active 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 information

A zoo of transient sources. (c)2017 van Putten 1

A 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 information

Active galaxies. Some History Classification scheme Building blocks Some important results

Active 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 information

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.

BH Astrophys Ch1~2.2. hp://www.astro.princeton.edu/~burrows/classes/250/distant_galaxies.html hp://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 information

Vera Genten. AGN (Active Galactic Nuclei)

Vera 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 information

Active Galaxies & Emission Line Diagnostics

Active 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 information

Schwarzchild 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. 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 information

An introduction to Active Galactic Nuclei. 1.

An 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 information

X-ray data analysis. Andrea Marinucci. Università degli Studi Roma Tre

X-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 information

Active Galactic Nuclei - Zoology

Active 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 information

Extragalactic Radio Sources. Joanne M. Attridge MIT Haystack Observatory

Extragalactic 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 information

A Unified Model for AGN. Ryan Yamada Astro 671 March 27, 2006

A 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 information

Accretion Disks. 1. Accretion Efficiency. 2. Eddington Luminosity. 3. Bondi-Hoyle Accretion. 4. Temperature profile and spectrum of accretion disk

Accretion 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 information

Lecture 9. Quasars, Active Galaxies and AGN

Lecture 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 information

Quasars and AGN. What are quasars and how do they differ from galaxies? What powers AGN s. Jets and outflows from QSOs and AGNs

Quasars 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 information

Set 4: Active Galaxies

Set 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 information

Chapter 17. Active Galaxies and Supermassive Black Holes

Chapter 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 information

Radio Loud Black Holes. An observational perspective

Radio 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 information

TEMA 6. Continuum Emission

TEMA 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 information

High-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. 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 information

Black Holes and Active Galactic Nuclei

Black 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 information

Galaxies 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 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 information

Hubble 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. 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 information

Active Galaxies & Quasars

Active 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 information

Active Galactic Nuclei OIII

Active 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 information

Lecture 7 Active Galactic Nuclei - I

Lecture 7 Active Galactic Nuclei - I Lecture 7 Active Galactic Nuclei - I i) Brief History emission-line galaxies Radio-astronomy radio sources discovery of quasars theoretical interpretations going through the details ii) General properties

More information

Active Galactic Alexander David M Nuclei

Active 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 information

The X-Ray Universe. The X-Ray Universe

The 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 information

Starbursts, AGN, and Interacting Galaxies 1 ST READER: ROBERT GLEISINGER 2 ND READER: WOLFGANG KLASSEN

Starbursts, AGN, and Interacting Galaxies 1 ST READER: ROBERT GLEISINGER 2 ND READER: WOLFGANG KLASSEN Starbursts, AGN, and Interacting Galaxies 1 ST READER: ROBERT GLEISINGER 2 ND READER: WOLFGANG KLASSEN Galaxy Interactions Galaxy Interactions Major and Minor Major interactions are interactions in which

More information

Set 4: Active Galaxies

Set 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 information

Guiding Questions. Active Galaxies. Quasars look like stars but have huge redshifts

Guiding 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 information

Dark Matter ASTR 2120 Sarazin. Bullet Cluster of Galaxies - Dark Matter Lab

Dark 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

Powering Active Galaxies

Powering 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 information

(Astro)Physics 343 Lecture # 12: active galactic nuclei

(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 information

Active Galactic Nuclei

Active 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 information

The Phenomenon of Active Galactic Nuclei: an Introduction

The 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 information

Active Galaxies. Ishwara Chandra C.H NCRA-TIFR

Active Galaxies. Ishwara Chandra C.H NCRA-TIFR December 20, 2012 Radio Astronomy Winter School, Active Galaxies Ishwara Chandra C.H NCRA-TIFR Astronomy is the study of planets, stars, galaxies, and other astronomical objects using the light they emit

More information

Black Holes and Quasars

Black Holes and Quasars Black Holes and Quasars Black Holes Normal and Super- massive The Schwartzchild Radius (event horizon) Normal and Super Massive Black Holes (SMBHs) The GalacAc Centre (GC) The Black Hole in Andromeda AcAve

More information

Evidence for BH: Active Galaxies

Evidence 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 information

Quasars and Active Galactic Nuclei (AGN)

Quasars 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 information

Black holes as central engines

Black 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 information

Active Galactic Nuclei

Active 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 information

Osservatorio Astronomico di Bologna, 27 Ottobre 2011

Osservatorio 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 information

Quasars ASTR 2120 Sarazin. Quintuple Gravitational Lens Quasar

Quasars 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 information

GRB history. Discovered 1967 Vela satellites. classified! Published 1973! Ruderman 1974 Texas: More theories than bursts!

GRB 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

Today in Astronomy 142: supermassive black holes in active-galaxy nuclei

Today 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 information

Astrophysical Quantities

Astrophysical Quantities Astr 8300 Resources Web page: http://www.astro.gsu.edu/~crenshaw/astr8300.html Electronic papers: http://adsabs.harvard.edu/abstract_service.html (ApJ, AJ, MNRAS, A&A, PASP, ARAA, etc.) General astronomy-type

More information

Misaligned AGN with Fermi-Lat:

Misaligned AGN with Fermi-Lat: Misaligned AGN with Fermi-Lat: a different perspective on relativistic jets PAOLA GRANDI INAF/IASF BOLOGNA, ITALY on behalf of the FERMI LAT Collaboration Many thanks to : Torresi E., Migliori G., P. Malaguti,

More information

Active Galaxies and Quasars

Active Galaxies and Quasars Active Galaxies and Quasars Radio Astronomy Grote Reber, a radio engineer and ham radio enthusiast, built the first true radio telescope in 1936 in his backyard. By 1944 he had detected strong radio emissions

More information

Radiative Processes in Astrophysics

Radiative 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 information

Astr Resources

Astr 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 information

ACTIVE GALACTIC NUCLEI: FROM THE CENTRAL BLACK HOLE TO THE GALACTIC ENVIRONMENT

ACTIVE 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 information

Overview of Active Galactic Nuclei

Overview of Active Galactic Nuclei Overview of Active Galactic Nuclei Andrei Lobanov Max-Planck Planck-Institut für Radioastronomie Outline Brief account of AGN studies Specific properties of AGN Major constituents of AGN AGN gallery AGN

More information

AGN Physics of the Ionized Gas Physical conditions in the NLR Physical conditions in the BLR LINERs Emission-Line Diagnostics High-Energy Effects

AGN Physics of the Ionized Gas Physical conditions in the NLR Physical conditions in the BLR LINERs Emission-Line Diagnostics High-Energy Effects AGN Physics of the Ionized Gas Physical conditions in the NLR Physical conditions in the BLR LINERs Emission-Line Diagnostics High-Energy Effects 1 Evidence for Photoionization - continuum and Hβ luminosity

More information

Multi-wavelength Astronomy

Multi-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 information

LeMMINGs the emerlin radio legacy survey of nearby galaxies Ranieri D. Baldi

LeMMINGs 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 information

The Most Luminous Radio Galaxies

The Most Luminous Radio Galaxies The Most Luminous Radio Galaxies The physics of radio galaxies and quasars The origin of their strong cosmological evolution Where they fit into the scheme of galaxy formation and evolution How does it

More information

Galaxies. Galaxy Diversity. Galaxies, AGN and Quasars. Physics 113 Goderya

Galaxies. 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 information

Payne-Scott workshop on Hyper Compact HII regions Sydney, September 8, 2010

Payne-Scott workshop on Hyper Compact HII regions Sydney, September 8, 2010 Payne-Scott workshop on Hyper Compact HII regions Sydney, September 8, 2010 Aim Review the characteristics of regions of ionized gas within young massive star forming regions. Will focus the discussion

More information

Structure of nuclei of extragalactic radio sources and the link with GAIA

Structure 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 information

Lecture 11 Quiz 2. AGN and You. A Brief History of AGN. This week's topics

Lecture 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 information

Evidence for BH: Active Galaxies

Evidence 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 information

Multi-wavelength Surveys for AGN & AGN Variability. Vicki Sarajedini University of Florida

Multi-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 information

TEMA 3. Host Galaxies & Environment

TEMA 3. Host Galaxies & Environment TEMA 3. Host Galaxies & Environment 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,

More information

Quasars are supermassive black holes, found in the centers of galaxies Mass of quasar black holes = solar masses

Quasars are supermassive black holes, found in the centers of galaxies Mass of quasar black holes = solar masses Quasars Quasars are supermassive black holes, found in the centers of galaxies Mass of quasar black holes = 10 6 10 9 solar masses Stars and gas fall into the black hole and shine in an accrecon disk billion

More information

A100H Exploring the Universe: Quasars, Dark Matter, Dark Energy. Martin D. Weinberg UMass Astronomy

A100H Exploring the Universe: Quasars, Dark Matter, Dark Energy. Martin D. Weinberg UMass Astronomy A100H Exploring the :, Dark Matter, Dark Energy Martin D. Weinberg UMass Astronomy astron100h-mdw@courses.umass.edu April 19, 2016 Read: Chaps 20, 21 04/19/16 slide 1 BH in Final Exam: Friday 29 Apr at

More information

Chapter 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 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 information

Galaxies with radio and optical jets Françoise Combes

Galaxies with radio and optical jets Françoise Combes Chaire Galaxies et Cosmologie Galaxies with radio and optical jets Françoise Combes The jet: component of the standard model Less than 10% of galaxies have an active nucleus. 10% of AGN have Radio jets

More information

Galaxies and Cosmology

Galaxies 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 information

Outline. Supermassive Black Holes Jets Hot spots and the evolution of radio galaxies

Outline. Supermassive Black Holes Jets Hot spots and the evolution of radio galaxies Active Galaxies Outline 2 Normal (boring) galaxies Active (fun) galaxies The extragalactic zoo: Quasars, Blazars, Radio Galaxies, BL Lacs, Seyferts, Optically Violent Variables, GHz Peaked Spectrum, Compact

More information

The parsec scale of. ac-ve galac-c nuclei. Mar Mezcua. International Max Planck Research School for Astronomy and Astrophysics

The parsec scale of. ac-ve galac-c nuclei. Mar Mezcua. International Max Planck Research School for Astronomy and Astrophysics The parsec scale of ESO ac-ve galac-c nuclei International Max Planck Research School for Astronomy and Astrophysics COST Ac(on MP0905 - Black Holes in a Violent Universe In collaboration with A. Prieto,

More information

Gamma-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 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 information

Martin Ward (Durham University, UK) allenges in Modern Astrophysics Sofia, Bulgaria Oct. 2009

Martin Ward (Durham University, UK) allenges in Modern Astrophysics Sofia, Bulgaria Oct. 2009 Martin Ward (Durham University, UK) allenges in Modern Astrophysics Sofia, Bulgaria Oct. 2009 What Makes a Galaxy ACTIVE? What is a Normal Galaxy? What is an Normal Galaxy? A literary analogy, adapted

More information

Other Galaxy Types. Active Galaxies. A diagram of an active galaxy, showing the primary components. Active Galaxies

Other 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 information

Not 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 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 information

Black Holes in Hibernation

Black 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 information

High-Energy Astrophysics

High-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 information

Gas 1: Molecular clouds

Gas 1: Molecular clouds Gas 1: Molecular clouds > 4000 known with masses ~ 10 3 to 10 5 M T ~ 10 to 25 K (cold!); number density n > 10 9 gas particles m 3 Emission bands in IR, mm, radio regions from molecules comprising H,

More information

The extreme ends of the spectrum: the radio/gamma connection

The 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 information

Radio 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. 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 information

Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines!

Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines! Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines Idealized 21cm spectra Example observed 21cm spectra HI densities

More information

Active Galactic Nuclei-I. The paradigm

Active 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 information

ACCRETION JET CONNECTION τ α MBH

ACCRETION 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 information

Astronomy 102 Lecture 17

Astronomy 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 information

VLBI observations of AGNs

VLBI 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 information

Lecture Outlines. Chapter 24. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.

Lecture Outlines. Chapter 24. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc. Lecture Outlines Chapter 24 Astronomy Today 8th Edition Chaisson/McMillan Chapter 24 Galaxies Units of Chapter 24 24.1 Hubble s Galaxy Classification 24.2 The Distribution of Galaxies in Space 24.3 Hubble

More information

Introduction to High Energy Astrophysics

Introduction to High Energy Astrophysics Introduction to High Energy Astrophysics Books 2011 2006 - for the history of the subject 1 The Sky in Different Astronomical Wavebands The context for high energy astrophysics Optical Infrared Millimetre-submillimetre

More information

Broadband X-ray emission from radio-quiet Active Galactic Nuclei

Broadband 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 information

Non-Blazar Gamma-ray Active Galactic Nuclei seen by Fermi-LAT. C.C. Teddy Cheung Naval Research Lab/NRC on behalf of the Fermi-LAT Collaboration

Non-Blazar Gamma-ray Active Galactic Nuclei seen by Fermi-LAT. C.C. Teddy Cheung Naval Research Lab/NRC on behalf of the Fermi-LAT Collaboration Non-Blazar Gamma-ray Active Galactic Nuclei seen by Fermi-LAT C.C. Teddy Cheung Naval Research Lab/NRC on behalf of the Fermi-LAT Collaboration 1 st LAT AGN Catalog (1LAC) Summary FmJ 2010 Entire 1LAC:

More information

High-Energy Astrophysics

High-Energy Astrophysics Part C Major Option Astrophysics High-Energy Astrophysics Garret Cotter garret@astro.ox.ac.uk Office 756 DWB Michaelmas 2012 Lecture 6 Today s lecture Synchrotron emission Part III Synchrotron self-absorption

More information

This week at Astro 3303

This 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 information

Active Galactic Nuclei (AGNs): A type of AGNs: Quasars. Whatever is powering these QSO s must be very small!!

Active 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 information

An Introduction to Radio Astronomy

An 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 information

High-Energy Astrophysics

High-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 information

Nuclear X-ray Emission and Mass Outflow From Broad Lined Radio Galaxies (Lorentz Center, Leiden 2009)

Nuclear X-ray Emission and Mass Outflow From Broad Lined Radio Galaxies (Lorentz Center, Leiden 2009) Nuclear X-ray Emission and Mass Outflow From Broad Lined Radio Galaxies (Lorentz Center, Leiden 2009) James Reeves (Keele Univ, UK) Collaborators:- Rita Sambruna (NASA/GSFC), Francesco Tombesi (NASA/GSFC

More information

Constraints on Extragalactic Background Light from Cherenkov telescopes: status and perspectives for the next 5 years

Constraints on Extragalactic Background Light from Cherenkov telescopes: status and perspectives for the next 5 years Constraints on Extragalactic Background Light from Cherenkov telescopes: status and perspectives for the next 5 years Daniel Mazin 1 and Martin Raue 2 1: IFAE, Barcelona 2: MPIK, Heidelberg This research

More information