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

Size: px
Start display at page:

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

Transcription

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

2 Overview Introduction to AGN Evidence for unified model Structure Radiative transfer models for dusty torus

3 Active Galactic Nuclei Emission-line spectrum demonstrating wider range of ionization than HII regions and grater range of velocities Emission line profile showing greater range of velocities than in starburst galaxies blue featureless continuum probably emitted by accretion disk around a supermassive black hole and/or synchrotron emission

4 Radio-quiet galaxies Seyfert 1 galaxies Exhibit narrow and broad line emission HI, He I, He II emission line FWHM ~ 5,000-10,000 km/s Strong kev X-ray emission Seyfert 2 galaxies Narrow line region in flux spectra Line FWHM are < 1000 km/s No strong kev emission

5 Radio galaxies Broad-line radio galaxies (BLRGs) Analogous to Seyfert 1s Bright, starlike nucleus surrounded by a very faint, hazy envelope Narrow-line radio galaxies (NLRGs) Analogous to Seyfert 2s Giant or supergiant elliptical galaxies (cd, D, E) May display extended radio lobes, or a core and halo

6 Cygnus A (Perley, Dreher, and Cowan, NRAO/AUI)

7 Quasars and QSOs Quasars - Strong radio sources distant enough that the nucleus appears starlike Quasi-stellar objects (QSOs) - radio quiet high-luminosity starlike objects Both quasars and QSOs distinguished by large redshift, nebular lines

8 Centaurus A

9 Sources of energy Accretion Magnetic field anchored to accretion disk Induces electric field, emitting synchrotron radiation that contributes to continuum Most energetic AGN must accrete 1-10 M sun yr -1 Blandford-Znajek mechanism For 10 8 M sun black hole, R s = 3 x cm, B = 10 4 G, P ~ B 2 R S2 c = 2.7 x erg s -1

10 A unified model? Evolutionary relationship between different AGN types Quasars and blazars -> radio galaxies -> normal elliptical galaxies QSOs -> Seyferts -> normal spiral galaxies Role of observing angle in classification

11 Constraints on unified model Torus must be opaque Only hard x-rays observed in Seyfert 2 galaxies Continuum in Seyfert 2s weaker than Seyfert 1s Broad-line region is close to center and clumpy Broad-line region responds quickly (1-4 weeks) to changes in continuum Narrow-line region is farther away, but still near nucleus (and also clumpy) n e ~ 10 4 cm -3 T ~ 10 4 K

12 C. M. Urry and P. Padovani

13 Evidence for a unified model Antonucci and Miller (1985) observed NGC 1068 (Seyfert 2) in polarized light and found a Seyfert 1 spectrum with broad emission lines Seyfert 1 nucleus hidden from direct view by optically thick material

14 Evidence for a unified model H emission lines appear to be produced by continuum radiation and subsequent recombination common origin for emission lines for Seyfert 1 and 2 galaxies, broad- and narrow-line radio galaxies, quasars, and QSOs from Shuder (1981)

15 Unified model Powered by a supermassive black hole M sun and its accretion disk, extending to ~ 1 pc Surrounded by a dusty toroidal structure, extending to > 100 pc

16 Structure of unified model Broad lines (H α and H β ) vary on short time scales (~0.1 year), but narrow lines vary little Seyfert 2 galaxies found to have Seyfert 1 nuclei (Antonucci and Miller, 1985) Indicates that broad and narrow lines in spectra originate under different regions under different circumstances

17 Broad line region Broad-line region is close to center and clumpy Responds to changes in continuum (1-4 weeks for Seyfert galaxies, longer for QSOs) T ~ 10 4 K n e ~ cm -3 Clumpy; flat distribution of optically thick clouds

18 AGN in the infrared Obscuring dusty torus should reradiate absorbed nuclear radiation in IR Seyfert 2 galaxies exhibit 10µm silicate absorption feature However, Seyfert 1s and quasars do not exhibit the 10µm silicate feature in emission One solution: clumps of dust in torus

19 Modeling a clumpy medium (Nenkova et al. 2002) calculated IR emission from clumps in obscuring torus Included emission from externally illuminated clumps and cloud shadowing Model reproduces important IR features broad IR bump extending to ~ 100 µm 10mm feature apparent in equatorial viewing, but smeared out in axial viewing because of cloud shadowing Optical depth of clouds constrained to τ V > 60 additional clouds in the outer torus of lower optical depth would not significantly affect the SED

20 From Nenkova et al. (2002)

21 Summary Differences between Seyfert and radio galaxies, QSOs, and quasars appears to be due to orientation (and possibly age) Unified model of AGN is supported and refined by observations in all wavelengths IR observations particularly important for testing models for dust distribution in outer torus

22 References Antonucci and Miller, ApJ 297, 621, 1985 Antonucci, ARA&A, 31, 473, 1993 Carroll and Ostlie. An Introduction to Modern Astrophysics Nenkova et al., ApJ, 570L, 9, 2002 Osterbrock and Ferland. Astrophysics of Gaseous Nebulae and Active Galactic Nuclei (second edition) Shuder, ApJ, 244, 12, 1981.

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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 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

ASCA Observations of Radio-Loud AGNs

ASCA 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 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

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

Astrophysics of Gaseous Nebulae and Active Galactic Nuclei

Astrophysics of Gaseous Nebulae and Active Galactic Nuclei SECOND EDITION Astrophysics of Gaseous Nebulae and Active Galactic Nuclei Donald E. Osterbrock Lick Observatory, University of California, Santa Cruz Gary J. Ferland Department of Physics and Astronomy,

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

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

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

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

Part two of a year-long introduction to astrophysics:

Part 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

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

Debate on the toroidal structures around hidden- vs non hidden-blr of AGNs

Debate on the toroidal structures around hidden- vs non hidden-blr of AGNs IoA Journal Club Debate on the toroidal structures around hidden- vs non hidden-blr of AGNs 2016/07/08 Reported by T. Izumi Unification scheme of AGNs All AGNs are fundamentally the same (Antonucci 1993)

More information

Chapter 15 2/19/2014. Lecture Outline Hubble s Galaxy Classification. Normal and Active Galaxies Hubble s Galaxy Classification

Chapter 15 2/19/2014. Lecture Outline Hubble s Galaxy Classification. Normal and Active Galaxies Hubble s Galaxy Classification Lecture Outline Chapter 15 Normal and Active Galaxies Spiral galaxies are classified according to the size of their central bulge. Chapter 15 Normal and Active Galaxies Type Sa has the largest central

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

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

Optical polarization from AGN

Optical polarization from AGN Optical polarization from AGN Damien Hutsemékers (University of Liège, Belgium) Polarization & AGN II, 11-12 May 2015, Strasbourg, France 1 Outline Polarization properties of radio-quiet AGN including

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

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

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

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

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

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 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

Quasars: Back to the Infant Universe

Quasars: 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 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

Dusty AGN torii. Ionization cones: toroidal obscuration

Dusty AGN torii. Ionization cones: toroidal obscuration Dusty AGN torii Ionization cones: toroidal obscuration hst cone hst cone 1 A hidden seyfert I inside a Seyfet II Seyfert I/II statistics as a measure of H/R 2 Conclusion so far: unification model requires

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

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

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

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

Active Galaxies. Lecture Topics. Lecture 24. Active Galaxies. Potential exam topics. What powers these things? Lec. 24: Active Galaxies

Active 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 information

Thus Far. Intro / Some Definitions Hubble Classification Components of Galaxies. Specific Galaxy Types Star Formation Clusters of Galaxies

Thus Far. Intro / Some Definitions Hubble Classification Components of Galaxies. Specific Galaxy Types Star Formation Clusters of Galaxies Thus Far Intro / Some Definitions Hubble Classification Components of Galaxies Stars Gas Dust Black Holes Dark Matter Specific Galaxy Types Star Formation Clusters of Galaxies Components of Galaxies:

More information

Spotting the misaligned outflows in NGC 1068 using X ray polarimetry

Spotting the misaligned outflows in NGC 1068 using X ray polarimetry Spotting the misaligned outflows in NGC 1068 using X ray polarimetry René W. Goosmann Observatoire astronomique de Strasbourg, France in collaboration with Giorgio Matt, Frédéric Marin, and Martin Gaskell

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

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

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

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

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

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

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

Orianne ROOS CEA-Saclay Collaborators : F. Bournaud, J. Gabor, S. Juneau

Orianne ROOS CEA-Saclay Collaborators : F. Bournaud, J. Gabor, S. Juneau Orianne ROOS CEA-Saclay Collaborators : F. Bournaud, J. Gabor, S. Juneau Bachelor of Physics, Master of Astrophysics Université de Strasbourg PhD, Université Paris-Diderot Observatoire de Strasbourg Les

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

Star systems like our Milky Way. Galaxies

Star systems like our Milky Way. Galaxies Galaxies Star systems like our Milky Way Galaxies Contain a few thousand to tens of billions of stars,as well as varying amounts of gas and dust Large variety of shapes and sizes Gas and Dust in

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

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

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

A. Thermal radiation from a massive star cluster. B. Emission lines from hot gas C. 21 cm from hydrogen D. Synchrotron radiation from a black hole

A. Thermal radiation from a massive star cluster. B. Emission lines from hot gas C. 21 cm from hydrogen D. Synchrotron radiation from a black hole ASTR 1040 Accel Astro: Stars & Galaxies Prof. Juri Toomre TA: Nicholas Nelson Lecture 26 Thur 14 Apr 2011 zeus.colorado.edu/astr1040-toomre toomre HST Abell 2218 Reading clicker what makes the light? What

More information

Powering the Universe with Supermassive Black Holes. Steve Ehlert and Paul Simeon

Powering the Universe with Supermassive Black Holes. Steve Ehlert and Paul Simeon Powering the Universe with Supermassive Black Holes Steve Ehlert and Paul Simeon Overview Introduction to Galactic Nuclei Galactic Nuclear Activity Input and output energies. The aftermath of AGN flares.

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

Ultra Luminous Infared Galaxies. Yanling Wu Feb 22 nd,2005

Ultra Luminous Infared Galaxies. Yanling Wu Feb 22 nd,2005 Ultra Luminous Infared Galaxies Yanling Wu Feb 22 nd,2005 The Biggest and the brightest Biggest and the best & best and the brightest Definition: LIRG: L8-1000umL

More information

The Milky Way Galaxy

The Milky Way Galaxy 1/5/011 The Milky Way Galaxy Distribution of Globular Clusters around a Point in Sagittarius About 00 globular clusters are distributed in random directions around the center of our galaxy. 1 1/5/011 Structure

More information

Luminous radio-loud AGN: triggering and (positive?) feedback

Luminous radio-loud AGN: triggering and (positive?) feedback Luminous radio-loud AGN: triggering and (positive?) feedback Clive Tadhunter University of Sheffield ASA, ESA, NRAO Collaborators: C. Ramos Almeida, D. Dicken," R. Morganti,T. Oosterloo, " R. Oonk, M.

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

Interferometry and AGN

Interferometry and AGN Interferometry and AGN Michelson Summer Workshop 2006 Mark R. Swain Acknowledgements to: Walter Jaffe, Klaus Meisenheimer, Konrad Tristram, & Markus Wittkowski 2 August 2006 1 Overview Themes Origin of

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

IR Instrumentation & AGN: Revealing Inner Secrets. Chris Packham University of Florida 7 th October, 2011

IR Instrumentation & AGN: Revealing Inner Secrets. Chris Packham University of Florida 7 th October, 2011 IR Instrumentation & AGN: Revealing Inner Secrets Chris Packham University of Florida 7 th October, 2011 Presentation Outline T λ" i m e! Instrumentation past, present, and near future INGRID MMT-POL T-ReCS,

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

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

Active Galactic Nuclei SEDs as a function of type and luminosity

Active Galactic Nuclei SEDs as a function of type and luminosity Active Galactic Nuclei SEDs as a function of type and luminosity Mari Polletta (IASF-INAF Milan) Collaborators: L. Chiappetti (IASF-INAF), L. Maraschi, M. Giorgetti, G. Trinchieri (Brera-INAF), B. Wilkes

More information

Supernovae. Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization

Supernovae. Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization Supernovae Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization 1 Supernova Basics Supernova (SN) explosions in our Galaxy and others

More information

AGN Central Engines. Supermassive Black Holes (SMBHs) Masses and Accretion Rates SMBH Mass Determinations Accretion Disks

AGN Central Engines. Supermassive Black Holes (SMBHs) Masses and Accretion Rates SMBH Mass Determinations Accretion Disks AGN Central Engines Supermassive Black Holes (SMBHs) Masses and Accretion Rates SMBH Mass Determinations Accretion Disks 1 Supermassive Black Holes Need to generate L > 10 43 ergs/sec inside radius < 10

More information

Today. Practicalities

Today. Practicalities Today Broad and narrow emission line regions Unification AGN and galaxy formation AGN-10: HR 2007 p. 1 Practicalities Exam Dates (?) Example of exam questions Mini-symposium Dec 13. 13:45 Power points

More information

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

Radio Galaxies. D.Maino. Radio Astronomy II. Physics Dept., University of Milano. D.Maino Radio Galaxies 1/47 Radio Galaxies D.Maino Physics Dept., University of Milano Radio Astronomy II D.Maino Radio Galaxies 1/47 Active Galactic Nuclei AGN: nuclei of galaxies with energetic phenomena that can not clearly and

More information

Energy Source for Active Galactic Nuclei

Energy Source for Active Galactic Nuclei Quasars Quasars are small, extremely luminous, extremely distant galactic nuclei Bright radio sources Name comes from Quasi-Stellar Radio Source, as they appeared to be stars! Can have clouds of gas near

More information

Our View of the Milky Way. 23. The Milky Way Galaxy

Our View of the Milky Way. 23. The Milky Way Galaxy 23. The Milky Way Galaxy The Sun s location in the Milky Way galaxy Nonvisible Milky Way galaxy observations The Milky Way has spiral arms Dark matter in the Milky Way galaxy Density waves produce spiral

More information

Exam 4 Review EXAM COVERS LECTURES 22-29

Exam 4 Review EXAM COVERS LECTURES 22-29 Exam 4 Review EXAM COVERS LECTURES 22-29 Theoretically is there a center of the universe? Is there an edge? Do we know where Earth is on this? There is no center to the Universe, What kind of light we

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

Energy Sources of the Far IR Emission of M33

Energy Sources of the Far IR Emission of M33 Energy Sources of the Far IR Emission of M33 Hinz, Reike et al., ApJ 154: S259 265 (2004). Presented by James Ledoux 24 µm 70 µm 160 µm Slide 1 M33 Properties Distance 840kpc = 2.7 Mlyr (1'' ~ 4 pc) Also

More information

Chapter 21 Galaxy Evolution. How do we observe the life histories of galaxies?

Chapter 21 Galaxy Evolution. How do we observe the life histories of galaxies? Chapter 21 Galaxy Evolution How do we observe the life histories of galaxies? Deep observations show us very distant galaxies as they were much earlier in time (old light from young galaxies). 1 Observing

More information

The 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 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 information

Lecture 30. The Galactic Center

Lecture 30. The Galactic Center Lecture 30 History of the Galaxy Populations and Enrichment Galactic Evolution Spiral Arms Galactic Types Apr 5, 2006 Astro 100 Lecture 30 1 The Galactic Center The nature of the center of the Galaxy is

More information

X-ray variability of AGN

X-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 information

NEW CONSTRAINTS ON THE BLACK HOLE SPIN IN RADIO LOUD QUASARS

NEW CONSTRAINTS ON THE BLACK HOLE SPIN IN RADIO LOUD QUASARS NEW CONSTRAINTS ON THE BLACK HOLE SPIN IN RADIO LOUD QUASARS Andreas Schulze (NAOJ, EACOA Fellow)) Chris Done, Youjun Lu, Fupeng Zhang, Yoshiyuki Inoue East Asian Young Astronomers Meeting, EAYAM 2017

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

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

Stars, Galaxies & the Universe Lecture Outline

Stars, Galaxies & the Universe Lecture Outline Stars, Galaxies & the Universe Lecture Outline A galaxy is a collection of 100 billion stars! Our Milky Way Galaxy (1)Components - HII regions, Dust Nebulae, Atomic Gas (2) Shape & Size (3) Rotation of

More information

STAR FORMATION RATES observational overview. Ulrike Kuchner

STAR FORMATION RATES observational overview. Ulrike Kuchner STAR FORMATION RATES observational overview Ulrike Kuchner Remember, remember.. Outline! measurements of SFRs: - techniques to see what the SF rate is - importance of massive stars and HII regions - the

More information

4/12/18. Our Schedule. Measuring big distances to galaxies. Hamilton on Hawking tonight. Brightness ~ Luminosity / (Distance) 2. Tully-Fisher Relation

4/12/18. Our Schedule. Measuring big distances to galaxies. Hamilton on Hawking tonight. Brightness ~ Luminosity / (Distance) 2. Tully-Fisher Relation ASTR 1040: Stars & Galaxies Stefan s Quintet Our Schedule Next class (Tues Apr17) meets in Fiske Planetarium Mid-Term Exam 3 in class next Thur Apr 19 Review Sheet #3 still available, with review next

More information

AGN in hierarchical galaxy formation models

AGN 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 information

GALAXY EVOLUTION STUDIES AND HIGH PERFORMANCE COMPUTING

GALAXY EVOLUTION STUDIES AND HIGH PERFORMANCE COMPUTING GALAXY EVOLUTION STUDIES AND HIGH PERFORMANCE COMPUTING Andreas Efstathiou European University Cyprus Astrophysics and HPC group ACTIVE AREAS OF ASTRONOMY OPPORTUNITIES FOR THEORETICAL, OBSERVATIONAL AND

More information

4/18/17. Our Schedule. Revisit Quasar 3C273. Dark Matter in the Universe. ASTR 1040: Stars & Galaxies

4/18/17. Our Schedule. Revisit Quasar 3C273. Dark Matter in the Universe. ASTR 1040: Stars & Galaxies ASTR 1040: Stars & Galaxies HST Abell 2218 Prof. Juri Toomre TAs: Piyush Agrawal, Connor Bice Lecture 25 Tues 18 Apr 2017 zeus.colorado.edu/astr1040-toomre Our Schedule Observatory Night #8 + #9 (proj

More information