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

Size: px
Start display at page:

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

Transcription

1 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

2

3 Components of Galaxies: Black Holes Possible Evidence that Black Holes are the central engines of Quasars/QSOs Average QSO produces L sun from its nucleus alone.

4 Evidence 2: Light variations in nuclear light are consistent With source sizes of ~ 0.1 pc Black Hole Narrow Line Region (NLR) (Lower velocity gas farther from black hole) Broad Line Region (BLR) (High velocity gas near black hole) Accretion Disk (feeds black hole)

5 Reverberation Technique Estimating sizes of BLR Ionized gas from BLR Continuum Emission Active galaxies vary in energy output

6 Reverberation (cont ) Time lag, t, between a change in the continuum emission (black hole + accretion disk) & BLR is used to estimate size, L, of the BLR.

7 Evidence 3: Powerful relativistic radio jets are seen emanating from either side of the nuclear region The highly collimated nature of the emission favors a single source of emission

8 Black Holes as Central Engines Lots of energy Emanating from a small space Model: Material from an accretion disk falling into a supermassive nuclear black hole. Energy: Gravitational energy of sources near dense massive object converted to radiative energy.

9 Counterpoint: Supernovae & not BH? Quasar SN Difficulty: Sustaining the SN Rate Needed to Power QSOs for ~ yrs

10 Calculation of Black Hole Mass from the Eddingtion Luminosity Accretion Disk Black Hole (gravitational force) (radiative force)

11 Condition for accretion: F grav > F rad Solving for black hole mass yields, Where L edd is the Eddington Luminosity i.e., the Luminosity a source would have if the gravitational Force exactly balanced the radiative force. If 10% of the total mass/energy of the accreting material is converted to radiative energy, the mass accretion rate is,

12 Black Hole Mass: Size & Velocity Dispersion of the BLR Size of BLR: r ~ 0.1 pc = 3x10 15 m FWHM of gas in BLR Mass is thus,

13 Black Hole Mass: Quasar Co-moving Volume Density QSO density was higher in the past QSO density presently low FWHM is ~ QSO lifetime Maximum lifetime of QSO: M sun yr -1 accretion rate:

14 Dormant Black Holes in Nearby Normal Galaxies Qu: Given that the density of QSOs was higher in the past, & that QSOs built up black holes with masses on the order of M sun, where are these dead QSOs? An: Perhaps these dormant QSOs are in the nuclear regions of nearby normal galaxies. The implication of this is that almost every massive galaxy has gone through an active galactic phase. Qu: Why aren t present day, nearly normal galaxies active? An: Because they re not being fed. [Quasars] can live forever, but they must fed.

15 Evidence for Mass of Central Black Holes in Nearby Galaxies If dead quasars are in the nuclear regions of nearby normal galaxies, how might we infer their presence? By their gravitational effect on stars & gas in the nuclear regions of galaxies

16 From Gas Kinematics Active Galaxy M87 M BH ~ 3x10 9 M sun

17 Evidence for Massive/Compact Central Energy from Maser Rotation Curve (Miyoshi et al. 1995, Nature 373, 127) V(r) = (832 ± 2) [r / (0.25)] -½ Mass interior to 0.18 pc is M = 4.1x10 7 M sun pc

18 Gas Dynamics (cont )

19 Qu: Is a Nuclear Cusp Evidence of a BH? (Shu, pg 330)

20 (Kormendy & Richstone 1995 ARAA, 33, 581) Answer: No.

21 From Stellar Kinematics: The Galaxy HST NICMOS Imaging of GC (Rieke et al., in prep) Change in stellar position Velocity Mass Keck Imaging of GC (Ghez et al. 1998, ApJ, 509, 678)

22 The Galactic Center M ~ 2.6x10 6 M sun Advantage: GC is close I.e., mass interior to stars being traced by velocity dispersion is likely dominated by black hole, not stars. Possible Problem: some stars may not be in the GC (Ghez et al. 1998, ApJ, 509, 678)

23 From M / L(r) How can a large sample of galaxies be searched for black holes? The method should involve stellar kinematics gas motion is subject to non-gravitational forces Method: M / L (r) of central regions of galaxies

24 Search criteria for black hole survey of nearby galaxies The galaxy should be edge-on to minimize (v sin i) effects The galaxy must be relatively nearby, so that the best possible resolution can be obtained The galaxy must have no recent history of star formation (old stellar populations do not vary much in M / L with r) The galaxies should rotate to minimize the effects of anisotropy (Note: Giant elliptical galaxies don t rotate) The galaxies must have no evidence of nuclear dust (dust absorbs optical light, which gives an erroneous values of M / L V )

25 Case Study: NGC 3115 Edge-on Disk Galaxy HST: rotating Nuclear region

26 Kinematic Evidence of Edge-on Disk (Kormendy & Richstone 1992, ApJ, 393, 559) No Minor Axis Rotation

27 Imaging Brightness Profiles Seeing is important! Surface Brightness (mag arcsec -2 ) radius as a function of radius

28 Brightness Profiles Data + Models Measure Projected Brightness Distribution Determine Unprojected/seeing corrected I(r). (K&R 1992)

29 Spectroscopy: Velocity Profiles Velocity Radius of 0 Spatial

30 Sometimes, AGN contribution to Galaxy Continuum must be Accounted for Sombrero Galaxy AGN Line emission Low Luminosity AGN Stellar Absorption Lines (Kormendy et al. 1996, ApJ 473, L91)

31 Fitting Velocity Profiles to Data Exponential Disk Keplerian V(r) = constant Same Process as for I(r) (K&R 1992)

32 M / L(r) vs. Radius M = 1x10 9 Msun (K&R 1992)

33

34 Another Example: M31 (Andromeda Galaxy) M ~ 3x10 7 M sun (Kormendy & Richstone 1995)

35 And Another: The Sombrero Galaxy M ~ 1x10 9 M sun (e.g., Kormendy et al. 1996, 473, 91)

36 A Less Convincing Example: NGC 3377 M / L V (r 0) not as Extreme M ~ 2x10 8 M sun (Kormendy, Bender, Evans & Richstone 1998, AJ, 115, 1823)

37 Alternatives Explanations 1) Anisotropies can cause errors in the estimation of nuclear black hole masses Line of Sight

38 2) Dust in the core of the galaxy can cause artificially high values of M / L. Check: Unsharp Masking Patchiness in focussed / unfocussed (or model) images is a likely sign of dust Due to disk in nucleus of Galaxy Due to disky isophotes (Kormendy & Richstone 1992, ApJ, )

39 3) Metallicities: metal-rich galaxies have high M/L V because of line blanketing M/L V ~ 1-10 for Old Stellar Populations M/L Spread in Elliptical Galaxies 1) Metallicities 2) Anisotropies M / L = 9σ 2 / 2πGΣ 0 r c M/L of Globular Clusters 1) Metallicity (Kormendy, in High Energy Neutrino Astrophysics)

40 4) Dense Star Clusters & Not Black Hole? Probably Not. σ c & r c of Galaxies with Supermassive Nuclear Black Holes are same as Other Elliptical Galaxies and Bulges. I.e., IMFs must be similar. (Kormendy, in Structure & Dynamics of Elliptical Galaxies, 17)

41 Log M vs. M B,Bulge (Kormendy et al. 1998, AJ, 115, 1823)

42 The Magorrian Relation log (Υ fit / Υ sun ) = -1.11± (0.18±0.03) log (L / L sun ) log (M,fit / M sun ) = -1.79± (0.96±0.12) log (M bulge / M sun ) (Magorrian et al. 1998, AJ, 115, 2285)

43 M - σ r e/8 Relation Best data: M ~ σ 4.8±0.5 (Ferrarese & Merritt 2000, ApJ, 539, L9)

44 A Check: M - v rms Relation σ c (r e / 8) v rms (r e / 4) M ~ (σ rms ) 4.6±0.8 Note: v rms = [(s 2 + v r / sin 2 i) re/4 ] ½ v r = mean line-of-sight velocity

45 M - σ e Relation M = 1.2(±0.2) x10 8 M sun (σ e / 200 km/s) 3.75±0.3 (Gebhardt et al. 2000, ApJ, 539, L13)

46 M - σ Relation Appears to Hold for Active Galaxies Also Stellar + AGN components to spectrum complicate matters (Ferrarese et al. 2001, ApJ, 555, 79)

47 M via Reverberation Mapping & Ionization Models also appear to work (Kormendy & Gebhardt 2001, in Relativistic Astrophysics)

48 Nearby Galaxy with no Black Hole: M 33 Disk Galaxy Negligible Bulge (e.g., Merritt, Ferrarese, & Joseph 2001, Science, 293, 1116)

49 Why is there a Relationship? A First Guess Stellar mass and Black Hole Mass are related And σ traces stellar mass better than, e.g., blue light does For early-type galaxies, M ~ L 5/4 Faber Jackson relation L ~ σ 4 Thus, M ~ σ 5 Universal fraction of baryonic mass is converted into Black Holes (Ferrarese & Merritt 2000)

50 Details to Come Detailed Discussion of Active Galactic Nuclei Profile Fits to Galaxies Elliptical/Bulge Core Parameterization

In a dense region all roads lead to a black Hole (Rees 1984 ARAA) Deriving the Mass of SuperMassive Black Holes

In a dense region all roads lead to a black Hole (Rees 1984 ARAA) Deriving the Mass of SuperMassive Black Holes In a dense region all roads lead to a black Hole (Rees 1984 ARAA) Deriving the Mass of SuperMassive Black Holes Stellar velocity fields MW Distant galaxies Gas motions gas disks around nearby black holes

More information

A Supermassive Black Hole in the Dwarf Starburst Galaxy Henize Amy Reines Einstein Fellow National Radio Astronomy Observatory

A Supermassive Black Hole in the Dwarf Starburst Galaxy Henize Amy Reines Einstein Fellow National Radio Astronomy Observatory A Supermassive Black Hole in the Dwarf Starburst Galaxy Henize 2-10 Amy Reines Einstein Fellow National Radio Astronomy Observatory Supermassive black holes and galaxy evolution Supermassive black holes

More information

ASTRON 449: Stellar (Galactic) Dynamics. Fall 2014

ASTRON 449: Stellar (Galactic) Dynamics. Fall 2014 ASTRON 449: Stellar (Galactic) Dynamics Fall 2014 In this course, we will cover the basic phenomenology of galaxies (including dark matter halos, stars clusters, nuclear black holes) theoretical tools

More information

FORMATION OF SUPERMASSIVE BLACK HOLES Nestor M. Lasso Cabrera

FORMATION OF SUPERMASSIVE BLACK HOLES Nestor M. Lasso Cabrera FORMATION OF SUPERMASSIVE BLACK HOLES Nestor M. Lasso Cabrera In this presentation the different theories that can explain the formation of Supermassive Black Holes (SMBH) are presented. Before focus on

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

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

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

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

Astro2010 Science White Paper: Tracing the Mass Buildup of Supermassive Black Holes and their Host Galaxies

Astro2010 Science White Paper: Tracing the Mass Buildup of Supermassive Black Holes and their Host Galaxies Astro2010 Science White Paper: Tracing the Mass Buildup of Supermassive Black Holes and their Host Galaxies Anton M. Koekemoer (STScI) Dan Batcheldor (RIT) Marc Postman (STScI) Rachel Somerville (STScI)

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

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

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

Observing the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics

Observing the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics Observing the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics with: Tim Heckman (JHU) GALEX Science Team (PI: Chris Martin), Lee Armus,

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

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 - 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

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

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

Supermassive Black Holes: Galaxy Monsters

Supermassive Black Holes: Galaxy Monsters # 18 Supermassive Black Holes: Galaxy Monsters Dr. John Kormendy April 19, 2002 Produced by and for Hot Science - Cool Talks by the Environmental Science Institute. We request that the use of these materials

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

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

ACTIVE GALACTIC NUCLEI: optical spectroscopy. From AGN classification to Black Hole mass estimation

ACTIVE GALACTIC NUCLEI: optical spectroscopy. From AGN classification to Black Hole mass estimation ACTIVE GALACTIC NUCLEI: optical spectroscopy From AGN classification to Black Hole mass estimation Second Lecture Reverberation Mapping experiments & virial BH masses estimations Estimating AGN black hole

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

12.1 Elliptical Galaxies

12.1 Elliptical Galaxies 12.1 Elliptical Galaxies Elliptical Galaxies Old view: ellipticals are boring, simple systems Ellipticals contain no gas & dust Ellipticals are composed of old stars Ellipticals formed in a monolithic

More information

The Classification of Galaxies

The Classification of Galaxies Admin. 11/9/17 1. Class website http://www.astro.ufl.edu/~jt/teaching/ast1002/ 2. Optional Discussion sections: Tue. ~11.30am (period 5), Bryant 3; Thur. ~12.30pm (end of period 5 and period 6), start

More information

Measuring Black Hole Masses in Nearby Galaxies with Laser Guide Star Adaptive Optics

Measuring Black Hole Masses in Nearby Galaxies with Laser Guide Star Adaptive Optics Measuring Black Hole Masses in Nearby Galaxies with Laser Guide Star Adaptive Optics Claire Max Anne Medling Mark Ammons UC Santa Cruz Ric Davies Hauke Engel MPE-Garching Image of NGC 6240: Bush et al.

More information

Molecular Gas and the Host Galaxies of Infrared-Excess Quasi-Stellar Objects

Molecular Gas and the Host Galaxies of Infrared-Excess Quasi-Stellar Objects Molecular Gas and the Host Galaxies of Infrared-Excess Quasi-Stellar Objects A. S. Evans (Stony Brook) J. A. Surace & D. T. Frayer (Caltech) D. B. Sanders (Hawaii) Luminous Infrared Galaxies Properties

More information

AS1001:Extra-Galactic Astronomy

AS1001:Extra-Galactic Astronomy AS1001:Extra-Galactic Astronomy Lecture 5: Dark Matter Simon Driver Theatre B spd3@st-andrews.ac.uk http://www-star.st-and.ac.uk/~spd3 Stars and Gas in Galaxies Stars form from gas in galaxy In the high-density

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

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

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

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

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

The central engine: energetics and demographics

The central engine: energetics and demographics The central engine: energetics and demographics Overview Global properties Total energy output Efficiency Mass Energy and black-hole mass densities Formation scenarios Determining BH masses from observations

More information

Frequency of Seyfert Type Transitions in a Sample of 102 Local Active Galactic Nuclei

Frequency of Seyfert Type Transitions in a Sample of 102 Local Active Galactic Nuclei Frequency of Seyfert Type Transitions in a Sample of 102 Local Active Galactic Nuclei Jordan Runco A Thesis presented for the degree of Physics Department of Physics California Polytechnic State University

More information

The Black Hole in the Galactic Center. Eliot Quataert (UC Berkeley)

The 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 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

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

AST Cosmology and extragalactic astronomy. Lecture 20. Black Holes Part II

AST Cosmology and extragalactic astronomy. Lecture 20. Black Holes Part II AST4320 - Cosmology and extragalactic astronomy Lecture 20 Black Holes Part II 1 AST4320 - Cosmology and extragalactic astronomy Outline: Black Holes Part II Gas accretion disks around black holes, and

More 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

Inconvenient Tales of Dinosaurs

Inconvenient Tales of Dinosaurs Inconvenient Tales of Dinosaurs D. Richstone Univ of Michigan Thanks to key collaborators: Tod Lauer, Sandy Faber, Karl Gebhardt, Kayhan Gultekin, John Kormendy, Scott Tremaine And thanks to NASA Black

More information

Chapter 15 The Milky Way Galaxy. The Milky Way

Chapter 15 The Milky Way Galaxy. The Milky Way Chapter 15 The Milky Way Galaxy The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band of light across the sky From the outside, our

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

Coevolution (Or Not) of Supermassive Black Holes and Galaxies

Coevolution (Or Not) of Supermassive Black Holes and Galaxies Coevolution (Or Not) of Supermassive Black Holes and Galaxies Luis C. Ho ( 何子山 ) The Observatories of the Carnegie Institution for Science Ho 2008, ARA&A Nuclear Activity in Nearby Galaxies Kormendy &

More information

The Galaxy. (The Milky Way Galaxy)

The Galaxy. (The Milky Way Galaxy) The Galaxy (The Milky Way Galaxy) Which is a picture of the Milky Way? A A is what we see from Earth inside the Milky Way while B is what the Milky Way might look like if we were far away looking back

More information

Fundamental Planes and Galaxy Formation

Fundamental Planes and Galaxy Formation Fundamental Planes and Galaxy Formation Philip Hopkins, NoviCosmo 2007 Fundamental Planes = Scaling Laws Obeyed by Galaxies vs Origin of scaling laws: Ideally, we d understand every galaxy as an individual:

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 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

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

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

Demographics of radio galaxies nearby and at z~0.55. Are radio galaxies signposts to black-hole mergers?

Demographics of radio galaxies nearby and at z~0.55. Are radio galaxies signposts to black-hole mergers? Elaine M. Sadler Black holes in massive galaxies Demographics of radio galaxies nearby and at z~0.55 Are radio galaxies signposts to black-hole mergers? Work done with Russell Cannon, Scott Croom, Helen

More 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

Survey of Astrophysics A110

Survey of Astrophysics A110 Goals: Galaxies To determine the types and distributions of galaxies? How do we measure the mass of galaxies and what comprises this mass? How do we measure distances to galaxies and what does this tell

More information

Roman Shcherbakov (University of Maryland, Hubble Fellow),

Roman Shcherbakov (University of Maryland, Hubble Fellow), NGC3115, credit: NASA Sgr A*, credit: NASA Roman Shcherbakov (University of Maryland, Hubble Fellow), Ka-Wah Wong, Jimmy Irwin (University of Alabama), Chris Reynolds (UMD), Fred Baganoff (MIT), Daniel

More information

Lecture 19: Galaxies. Astronomy 111

Lecture 19: Galaxies. Astronomy 111 Lecture 19: Galaxies Astronomy 111 Galaxies What is a galaxy? Large assembly of stars, gas and dust, held together by gravity Sizes: Largest: ~1 Trillion stars (or more) Smallest: ~10 Million stars Milky

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

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

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

Nuclear Star Formation, The Torus, & Gas Inflow in Seyfert Galaxies

Nuclear Star Formation, The Torus, & Gas Inflow in Seyfert Galaxies Nuclear Star Formation, The Torus, & Gas Inflow in Seyfert Galaxies Richard Davies 1, H. Engel 1, M. Schartmann 1, G. Orban de Xivry 1, E. Sani 2, E. Hicks 3, A. Sternberg 4, R. Genzel 1, L. Tacconi 1,

More information

High-Energy Astrophysics Lecture 6: Black holes in galaxies and the fundamentals of accretion. Overview

High-Energy Astrophysics Lecture 6: Black holes in galaxies and the fundamentals of accretion. Overview High-Energy Astrophysics Lecture 6: Black holes in galaxies and the fundamentals of accretion Robert Laing Overview Evidence for black holes in galaxies and techniques for estimating their mass Simple

More information

Our Galaxy. We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky.

Our Galaxy. We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky. Our Galaxy Our Galaxy We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky. Early attempts to locate our solar system produced erroneous results.

More information

Black Hole and Host Galaxy Mass Estimates

Black Hole and Host Galaxy Mass Estimates Black Holes Black Hole and Host Galaxy Mass Estimates 1. Constraining the mass of a BH in a spectroscopic binary. 2. Constraining the mass of a supermassive BH from reverberation mapping and emission line

More information

Ay162, Spring 2006 Week 8 p. 1 of 15

Ay162, Spring 2006 Week 8 p. 1 of 15 Astronomy 162, Week 8 Milky Way Galaxy, continued Patrick S. Osmer Spring, 2006 Rotation of Galaxy How do we know the galaxy is rotating, and how do we measure its rotation? Measure radial velocities of

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

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

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

The cosmic distance scale

The cosmic distance scale The cosmic distance scale Distance information is often crucial to understand the physics of astrophysical objects. This requires knowing the basic properties of such an object, like its size, its environment,

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

Supermassive Black Holes

Supermassive Black Holes Supermassive Black Holes Richard McDonald, student number 2798107 Swinburne Astronomy Online HET-604 April 8, 2006 Introduction This paper discusses black holes as they relate to active galactic nuclei

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

Surface Photometry Quantitative description of galaxy morphology. Hubble Sequence Qualitative description of galaxy morphology

Surface Photometry Quantitative description of galaxy morphology. Hubble Sequence Qualitative description of galaxy morphology Hubble Sequence Qualitative description of galaxy morphology Surface Photometry Quantitative description of galaxy morphology Galaxy structure contains clues about galaxy formation and evolution Point

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

1932: KARL JANSKY. 1935: noise is identified as coming from inner regions of Milky Way

1932: KARL JANSKY. 1935: noise is identified as coming from inner regions of Milky Way 1932: KARL JANSKY Is assigned the task of identifying the noise that plagued telephone calls to Europe 1935: noise is identified as coming from inner regions of Milky Way MANY YEARS GO BY. 1960: a strong

More information

The Correlation Between Supermassive Black Hole Mass and the Structure of Ellipticals and Bulges

The Correlation Between Supermassive Black Hole Mass and the Structure of Ellipticals and Bulges 1 The Correlation Between Supermassive Black Hole Mass and the Structure of Ellipticals and Bulges Peter Erwin 1, Alister W. Graham 2, Nicola Caon 1 (1) Instituto de Astrofísica de Canarias, La Laguna,

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

Probing the Origin of Supermassive Black Hole Seeds with Nearby Dwarf Galaxies. Amy Reines Einstein Fellow NRAO Charlottesville

Probing the Origin of Supermassive Black Hole Seeds with Nearby Dwarf Galaxies. Amy Reines Einstein Fellow NRAO Charlottesville Probing the Origin of Supermassive Black Hole Seeds with Nearby Dwarf Galaxies Amy Reines Einstein Fellow NRAO Charlottesville Motivation: The origin of supermassive BH seeds Motivation: The origin of

More information

SPECTROSCOPIC EVIDENCE FOR A SUPERMASSIVE BLACK HOLE IN NGC 4486B

SPECTROSCOPIC EVIDENCE FOR A SUPERMASSIVE BLACK HOLE IN NGC 4486B THE ASTROPHYSICAL JOURNAL, 482 : L139 L142, 1997 June 20 1997. The American Astronomical Society. All rights reserved. Printed in U.S.A. SPECTROSCOPIC EVIDENCE FOR A SUPERMASSIVE BLACK HOLE IN NGC 4486B

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

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

COSMOLOGY PHYS 30392 OBSERVING THE UNIVERSE Part I Giampaolo Pisano - Jodrell Bank Centre for Astrophysics The University of Manchester - January 2013 http://www.jb.man.ac.uk/~gp/ giampaolo.pisano@manchester.ac.uk

More information

An Introduction to Galaxies and Cosmology. Jun 29, 2005 Chap.2.1~2.3

An Introduction to Galaxies and Cosmology. Jun 29, 2005 Chap.2.1~2.3 An Introduction to Galaxies and Cosmology Jun 29, 2005 Chap.2.1~2.3 2.1 Introduction external galaxies normal galaxies - majority active galaxies - 2% high luminosity (non-stellar origin) variability

More information

Relazioni di scala tra Buchi Neri e Galassie Ospiti. Lezione 7

Relazioni di scala tra Buchi Neri e Galassie Ospiti. Lezione 7 Relazioni di scala tra Buchi Neri e Galassie Ospiti Lezione 7 First hints of BH-galaxy relations Kormendy & Richstone (1995) suggest the existence of a correlation between the total blue magnitude of the

More information

The Universe o. Galaxies. The Universe of. Galaxies. Ajit Kembhavi IUCAA

The Universe o. Galaxies. The Universe of. Galaxies. Ajit Kembhavi IUCAA Hello! The Universe of Galaxies The Universe o Galaxies Ajit Kembhavi IUCAA Galaxies: Stars: ~10 11 Mass: ~10 11 M Sun Contain stars, gas and dust, possibly a supermassive black hole at the centre. Much

More information

Galaxies. Hubble's measurement of distance to M31 Normal versus other galaxies Classification of galaxies Ellipticals Spirals Scaling relations

Galaxies. Hubble's measurement of distance to M31 Normal versus other galaxies Classification of galaxies Ellipticals Spirals Scaling relations Galaxies Hubble's measurement of distance to M31 Normal versus other galaxies Classification of galaxies Ellipticals Spirals Scaling relations Cepheids in M31 Up to 1920s, the Milky Way was thought by

More information

Part 2. Hot gas halos and SMBHs in optically faint ellipticals. Part 3. After Chandra?

Part 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 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

LECTURE 1: Introduction to Galaxies. The Milky Way on a clear night

LECTURE 1: Introduction to Galaxies. The Milky Way on a clear night LECTURE 1: Introduction to Galaxies The Milky Way on a clear night VISIBLE COMPONENTS OF THE MILKY WAY Our Sun is located 28,000 light years (8.58 kiloparsecs from the center of our Galaxy) in the Orion

More information

Dust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio.

Dust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio. More abs. Dust [1.1] kev V Wavelength Optical Infra-red More abs. Wilms et al. 000, ApJ, 54, 914 No grains Grains from http://www.astro.princeton.edu/~draine/dust/dustmix.html See DraineH 003a, column

More information

3D Spectroscopy to Dissect Galaxies Down to Their Central Supermassive Black Holes. Kambiz Fathi. Stockholm University, Sweden

3D Spectroscopy to Dissect Galaxies Down to Their Central Supermassive Black Holes. Kambiz Fathi. Stockholm University, Sweden 3D Spectroscopy to Dissect Galaxies Down to Their Central Supermassive Black Holes Kambiz Fathi Stockholm University, Sweden Towards a better understanding of the Hubble Diagram Towards a better understanding

More information

Star Formation Near Supermassive Black Holes

Star Formation Near Supermassive Black Holes 1 Star Formation Near Supermassive Black Holes Jessica Lu California Institute of Technology June 8, 2009 Collaborators: Andrea Ghez, Keith Matthews, (all) Mark Morris, Seth Hornstein, Eric Becklin, Sylvana

More information

Galaxy Morphology. - a description of the structure of galaxies

Galaxy Morphology. - a description of the structure of galaxies Galaxy Morphology - a description of the structure of galaxies Galaxy Morphology - a description of the structure of galaxies Galaxy Morphology - a description of the structure of galaxies Clearly astronomical

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

Number of Stars: 100 billion (10 11 ) Mass : 5 x Solar masses. Size of Disk: 100,000 Light Years (30 kpc)

Number of Stars: 100 billion (10 11 ) Mass : 5 x Solar masses. Size of Disk: 100,000 Light Years (30 kpc) THE MILKY WAY GALAXY Type: Spiral galaxy composed of a highly flattened disk and a central elliptical bulge. The disk is about 100,000 light years (30kpc) in diameter. The term spiral arises from the external

More information

Lecture 2 Demographics of AGN & SMBHs

Lecture 2 Demographics of AGN & SMBHs Lecture 2 Demographics of AGN & SMBHs Basic concepts of the standard model of AGN Evidence for the presence of supermassive BHs in AGN Methods to weight a BH in an AGN Demographics of QSOs and BHs, fate

More information

WHAT IS THE ORIGIN OF THE BLACK HOLE -BULGE MASS CORRELATION? By Curtis McCully

WHAT IS THE ORIGIN OF THE BLACK HOLE -BULGE MASS CORRELATION? By Curtis McCully WHAT IS THE ORIGIN OF THE BLACK HOLE -BULGE MASS CORRELATION? By Curtis McCully OUTLINE What is the Black hole-bulge mass correlation Observations Possible Theoretical Explanations BH - BULGE MASS CORRELATION

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

Galaxy photometry. The surface brightness of a galaxy I(x) is the amount of light on the sky at a particular point x on the image.

Galaxy photometry. The surface brightness of a galaxy I(x) is the amount of light on the sky at a particular point x on the image. Galaxy photometry The surface brightness of a galaxy I(x) is the amount of light on the sky at a particular point x on the image. A small patch of side D in a galaxy located at a distance d, will subtend

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

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