Orianne ROOS CEA-Saclay Collaborators : F. Bournaud, J. Gabor, S. Juneau
|
|
- Oliver Hampton
- 5 years ago
- Views:
Transcription
1 Orianne ROOS CEA-Saclay Collaborators : F. Bournaud, J. Gabor, S. Juneau
2 Bachelor of Physics, Master of Astrophysics Université de Strasbourg PhD, Université Paris-Diderot Observatoire de Strasbourg Les Grands Moulins How did I end up here? M2 internship in SAp, then PhD
3 «Modeling the link between AGN and star formation in primeval galaxies» Primeval/high-redshift galaxies AGN, AGN feedback Link with star formation HPC, simulations Stellar feedback
4 Some galaxies suddenly stop forming stars (they get quenched and then they die ) : why? Ideal culprit : central supermassive black hole SMBH mass related to bulge mass -> co-evolution? Energy generated by SMBHs in active phases (AGNs) theoretically able to blow away all gas of the host AGNs needed to reproduce observed number of stars in simulations => Link between AGN feedback and SF quenching?
5 Halo (gas and globular clusters) To turn the Earth into a black hole, you would need to squeeze it into a 9 mm radius sphere!! Bulge (stars) Disk (gas, stars, dust, ) Supermassive black hole 10^9 solar masses Radius : 3 x 10^9 km
6 Halo (gas and globular clusters) Bulge (stars) Disk (gas, stars, dust, ) Supermassive black hole 10^9 solar masses Radius : 3 x 10^9 km
7 8
8 Local disk galaxies look like spirals Clumpy, gas-rich high-redshift disk-galaxies Gabor & Bournaud, 2013
9 z band H band z - H z band H band z - H Typical star-forming galaxies at z ~ 2. (Guo et al 2012) 10
10 Primeval/high-redshift galaxies AGN AGN feedback Link with star formation HPC To kill or not to kill? Stellar feedback
11 From Urry & Padovani 1995, modified (Schematic) Structure of an AGN : Active Galactic Nucleus Unified AGN Model : BLR (< 3 ly) NLR (> 300 ly) Radio jets (>>3 kly) Emission cone
12 Ground-based Optical/Radio image AGN HST image Artist view Reynolds et al 2014
13 Primeval/high-redshift galaxies AGN AGN feedback Link with star formation HPC To kill or not to kill? Stellar feedback
14 A clump of gas falls onto the AGN Thermal feedback : HEATING in the simulation AGN absorbs energy due to accretion and re-emits fraction of it, heating central region Creation of a hot and diffuse outflow of gas Radiative feedback : IONIZATION added a posteriori Energy of photons emitted by AGN is so high that encountered gas is ionized
15 From Urry & Padovani 1995, modified Structure of an AGN : Active Galactic Nucleus Unified AGN Model : BLR (< 3 ly) NLR (> 300 ly) Radio jets (>>3 kly) Emission cone
16 Primeval/high-redshift galaxies AGN AGN feedback Link with star formation HPC To kill or not to kill? Stellar feedback
17 AGN feedback vs star formation : Stars form into cold and dense clumps of gas WHEREAS AGN feedback dilutes and heats gas Is there an impact on star formation?
18 Primeval/high-redshift galaxies AGN AGN feedback Link with star formation HPC To kill or not to kill? Stellar feedback
19 High Performance Computing More than 5000 computation nodes 5 PB of disks ( 100 GB/s of bandwith) 10 PB of bands 1 PB of cache
20 Primeval/high-redshift galaxies AGN AGN feedback Link with star formation HPC To kill or not to kill? Stellar feedback
21 Do AGN (outflows) quench SF? Gas temperature Max. resolution : 6 pc GMCs are resolved. High-velocity AGN-driven outflows Mass outflow rates : ~ % of SFR (~ 30 M_sun/yr). 1 snapshot = 1 moment in the simulation Gabor & Bournaud 2014
22 Simulation Do AGN (outflows) of a high-redshift quench SF disk-galaxy? Gas temperature AGN outflows do Max. resolution : 6 pc GMCs not quench are resolved. star formation. High-velocity AGN-driven outflows but : Do AGNs Mass outflow rates : ~ quench % SF of SFR? (~ 30 M_sun/yr). AGN photoionization 1 snapshot = 1 moment in the simulation Gabor & Bournaud 2014
23 Does AGN radiation quench SF? Gas density map of the disk seen edge-on What happens in the disk?? RT with Cloudy (Ferland et al 2013) (cannot probe positive feedback) 3000 lines cast isotropically from location of BH Galactic disk edge-on Zoom in Simulation with standard thermal AGN feedback (Gabor & Bournaud 2013) + RT post-processing (Roos et al ApJ )
24 log Initial r SFR [M O yr -1 kpc -3 ] log Final r SFR [M O yr -1 kpc -3 ] log log Initial Initial r temperature [K] SFR [M O yr -1 kpc -3 ] log Rel. temperature change log Final r SFR [M O yr -1 kpc -3 ] log log Initial Gas temperature density [cm -3 [K] ] log Rel. temperature change log Fraction of neutral H log Gas dens log Fraction of n Before RT -6 L_AGN 10 L_AGN 100 L_AGN Before RT rho_sfr f_ion L AGN 10 x L AGN 100 x L AGN Even at a QSO -10 luminosity, the galactic disk remains completely neutral! Edge-on view -12 super-powerful -14 AGN L_AGN = 10^44.5 erg/s -18
25 Is the impact of AGN feedback luminosity-dependent? With a higher AGN luminosity : - Regions ionized by AGN enlarged - Most heated gas is in the gaseous halo - Galactic disk remains neutral even for QSO luminosity Let s focus on the central region : 600 x 600 pc (face-on view)
26 log Initial r SFR [M O yr -1 kpc -3 ] log Final r SFR [M O yr -1 kpc -3 ] log log Initial r temperature [K] SFR [M O yr -1 kpc -3 ] log Rel. temperature change log Final r SFR [M O yr -1 kpc -3 ] log log Initial Gas density temperature [cm -3 ] [K] log Rel. temperature change log Fraction of neutral H log Gas dens log Fraction o n Before RT -6 L_AGN 10 L_AGN 100 L_AGN Before RT rho_sfr f_ion L AGN 10 x L AGN 100 x L AGN Even at a QSO luminosity, the bulk of the star forming clumps is not affected! super-powerful -14 AGN -16 Face-on view zoom in L_AGN = 10^44.5 erg/s -18
27 log Initial r SFR [M O yr -1 kpc -3 ] log Final r [M yr -1 kpc -3 ] log Initial temperature [K] log Final temperature [K] log Gas density [cm log Fraction of neutr 2 Does AGN radiation 0 quench SF? Diffuse star-forming 8 regions are prevented from forming stars 8 - The stronger the AGN, the more efficiently gas is heated/ionized But pc dense star-forming clumps shield themselves > Major contributors to the total SFR are not affected. Roos et al ApJ
28 SFR [M ] O yr -1 ] (> 10 cm -3 ) ) Instantaneous reduction of the total SFR due to AGN photo-ionization SFR reduction is not significant Density of affected gas is small No feedback Thermal FB Initial FB + RT : 1 x L AGN 10 x L AGN 100 x L AGN Time [Myrs]
29 Primeval/high-redshift galaxies AGN AGN feedback Link with star formation HPC To kill or not to kill? Stellar feedback
30 Physical Origins of Galactic Outflows Do AGN+stellar outflows quench star formation? in z~2 star-forming galaxies Work in progress! 11 Mh of computation time, very high resolution (1.5 pc), AGN feedback + stellar feedback, suite of 7 simulations
31 Stars-driven outflows : High mass outflow rate Limited velocity ( km/s) Multiple SNe and young stars per galaxy Bournaud et al. 2014, AGN-driven outflows : Low outflow density High velocity ( km/s) 1 AGN in the center of the galaxy (usually) Gabor & Bournaud 2014,
32 Example : 10 kpc M*=3.5x10 10 Outflows generated by : - Supernovae (kin. energy) - Young stars (rad. pressure) - Both (no AGN)
33 Three runs with different feedback processes, all evolved for 80 Myr. Supernovae OB stars SNe + OB stars 10 kpc M*=3.5x10 10 Outflow rates Outflows from SNe + OB stars >> Outflows from SNe + Outflows from OB stars See also Hopkins+14 Gas density of simulated disk seen edge-on
34 Three runs with different feedback processes, all evolved for 80 Myr. Supernovae OB stars SNe + OB stars 10 kpc M*=3.5x10 10 Accurate modeling of stellar feedback is crucial for the outflow parameters!! Outflow rates Outflows from SNe + OB stars >> Outflows from SNe + Outflows from OB stars See also Hopkins+14 Gas density of simulated disk seen edge-on
35 Thermal energy injection from AGN Ionization from AGN Thermal energy injection from SNe Kinetic energy injection from SNe Radiative pressure from OB stars High space and mass resolution : probe GMCs and avoid numerical coupling + half resolution : check convergence
36 Supernovae OB stars SNe + OB stars 10 kpc M*=3.5x10 10 Thermal AGN feedback 10 kpc Outflow rates First time ever. Let s POGO! (a) + RT postprocessing ~30 Gabor & Bournaud 2013 (b) Combined effect of all feedback models may lead to very powerful and fast winds with high mass loading. M1 : Mgas = 15 1E9 Msun M2 : Mgas = 49 1E9 Msun M3 : Mgas = 115 1E9 Msun M3 : AGN + stellar FB M1, M2 : AGN ; stellar FB ; AGN + stellar FB
37 Beginning Stellar outflows AGN + stellar outflows AGN outflows t1 < t2 < t3
38 Beginning Stellar outflows AGN + stellar outflows t1 < t2 < t3 With M1 and M2 : Study outflow characteristics as a function of time Identify outflow pattern for AGN FB only and stellar FB only Study outflow pattern for AGN + stellar FB : - = sum? - > sum? - < sum? Nature of expelled gas : impact on SF?
39 Study 3 galaxy masses : < Outflow rate > Very high? *-dominated? AGN-dominated? High Mstar M1 M2 M3 Mass loading compatible with observed IGM density?
40 If such dense UFOs are produced : Evolve until steady state is reached Study mass loading, expelled gas, Impact on star formation? Impact on IGM? UFO = ultra-fast outflow
41 If such dense UFOs are NOT produced : What other wind sources could produce UFOs? What kills them? What other non-linear effects are we missing?
42 Primeval/high-redshift galaxies AGN AGN feedback Link with star formation HPC To kill or not to kill? Stellar feedback
43 SUMMARY : For further details, see Roos et al ApJ AGNs, through ionization and outflows, affect the gas of the galaxy, but mostly the non star-forming phase (halo : ionization cone). - Total instantaneous SFR is marginally reduced by thermal and radiative AGN feedback, even at QSO luminosities (< 4 %) AGNs do not kill galaxies - In association with outflows : + Gabor & Bournaud 2014 Frequent AGNs in high-z SFGs seem to be a promising mechanism to regulate/remove the mass of galaxies, without impacting star formation (up to 100 Myr-scale), i.e. preserving the steady-state evolution with relatively constant SFHs. Would this conclusion change with accurate modeling of stellar and AGN winds? Stay tuned for the POGO project!
44 Thank you for your attention.
45 log Initial temperature log Gas [K] density log [cm Gas -3 ] log Initial r log Initial density [cm -3 ] log Initial r SFR [M O yr -1 temperature kpc -3 [K] SFR [M O yr -1 kpc -3 ] ] Orianne Roos, with S. Juneau, F. Bournaud and J. Gabor see Roos et al log Final r log Final log Final r log Final temperature [K] SFR [M O yr -1 temperature kpc -3 [K] SFR [M O yr -1 kpc -3 ] ] log Fraction of neutral log Fraction H of neutral 4-2 hermal and radiative 2 AGN feedback in high-z galaxies -4 n Before RT mainly affect diffuse 4 gas ρ_sfr L AGN -12 and have very little impact on the star-forming phase of the ISM Reduction of SFR < 4% -18 f_ion 10 x L AGN 100 x L AGN L_AGN = 10^44.5 erg/s Edge-on view -16 suppressed, but major contributors to the SFR are left unaffecte Face-on view zoom in Diffuse and extended star-forming regions around the AGN are
46 n Before RT L_AGN 10 L_AGN 100 L_AGN f_ion T rho_sfr Edge-on view L_AGN = 10^44.5
47 Simulation of a high-redshift disk galaxy Typical density profile of a LOP in the disk
48 Large-scale spectral synthesis code : Ferland et al, 2013 Computes radiative transfer and molecular chemistry along 1D lines Divides each line into thin zones Balances recombination and ionization processes Input : ionization source and density profile Output : ionization fraction, temperature, line emission
49 AGN SEDs X-rays UV optical FIR X-rays UV optical FIR
50 Seyfert- and QSO-matched SEDs
51 Emission cone : From STScI, modified by G. Rieke Mean half-opening angle : ~ 30 at low-z (Müller-Sanchez+2011)
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 informationA Unified Model for AGN. Ryan Yamada Astro 671 March 27, 2006
A Unified Model for AGN Ryan Yamada Astro 671 March 27, 2006 Overview Introduction to AGN Evidence for unified model Structure Radiative transfer models for dusty torus Active Galactic Nuclei Emission-line
More informationFeedback from Radiation Pressure during Galaxy Formation
Feedback from Radiation Pressure during Galaxy Formation Eliot Quataert (UC Berkeley) w/ Norm Murray, Jackson Debuhr, Phil Hopkins... Spitzer s view of Carina Outline Feedback: What is it good for? Absolutely
More informationALMA Synergy with ATHENA
ALMA Synergy with ATHENA Françoise Combes Observatoire de Paris 9 September 2015 ALMA & Athena: common issues Galaxy formation and evolution, clustering Surveys of galaxies at high and intermediate redshifts
More informationAGN Feedback In an Isolated Elliptical Galaxy
AGN Feedback In an Isolated Elliptical Galaxy Feng Yuan Shanghai Astronomical Observatory, CAS Collaborators: Zhaoming Gan (SHAO) Jerry Ostriker (Princeton) Luca Ciotti (Bologna) Greg Novak (Paris) 2014.9.10;
More informationActive Galactic Nuclei
Active Galactic Nuclei How were they discovered? How common are they? How do we know they are giant black holes? What are their distinctive properties? Active Galactic Nuclei for most galaxies the luminosity
More informationActive Galaxies. Lecture Topics. Lecture 24. Active Galaxies. Potential exam topics. What powers these things? Lec. 24: Active Galaxies
Active Galaxies Lecture 24 APOD: M82 (The Cigar Galaxy) 1 Lecture Topics Active Galaxies What powers these things? Potential exam topics 2 24-1 Active Galaxies Galaxies Luminosity (L MW *) Normal < 10
More informationAstrophysical 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 informationBlack Holes and Active Galactic Nuclei
Black Holes and Active Galactic Nuclei A black hole is a region of spacetime from which gravity prevents anything, including light, from escaping. The theory of general relativity predicts that a sufficiently
More informationThe 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 informationHigh Redshift Universe
High Redshift Universe Finding high z galaxies Lyman break galaxies (LBGs) Photometric redshifts Deep fields Starburst galaxies Extremely red objects (EROs) Sub-mm galaxies Lyman α systems Finding high
More informationThe Monster Roars: AGN Feedback & Co-Evolution with Galaxies
The Monster Roars: AGN Feedback & Co-Evolution with Galaxies Philip Hopkins Ø (Nearly?) Every massive galaxy hosts a supermassive black hole Ø Mass accreted in ~couple bright quasar phase(s) (Soltan, Salucci+,
More informationMotivation Q: WHY IS STAR FORMATION SO INEFFICIENT? Ṁ M gas / dyn. Log SFR. Kennicutt Log. gas / dyn
Motivation Q: WHY IS STAR FORMATION SO INEFFICIENT? Ṁ 0.017 M gas / dyn Log SFR Kennicutt 1998 Log gas / dyn Motivation Q: WHY IS STAR FORMATION SO INEFFICIENT? Moster 2009 No Feedback 10% of baryons Log(
More informationEmpirical Evidence for AGN Feedback
Empirical Evidence for AGN Feedback Christy Tremonti MPIA (Heidelberg) / U. Wisconsin-Madison Aleks Diamond-Stanic (U. Arizona), John Moustakas (NYU) Much observational and theoretical evidence supports
More informationActive galactic nuclei (AGN)
Active galactic nuclei (AGN) General characteristics and types Supermassive blackholes (SMBHs) Accretion disks around SMBHs X-ray emission processes Jets and their interaction with ambient medium Radio
More informationActive Galaxies & Emission Line Diagnostics
Active Galaxies & Emission Line Diagnostics Review of Properties Discussed: 1) Powered by accretion unto a supermassive nuclear black hole 2) They are the possible precursors to luminous massive galaxies
More informationSTAR 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 informationAGN/Galaxy Co-Evolution. Fabio Fontanot (HITS)
AGN/Galaxy Co-Evolution Fabio Fontanot (HITS) 21/11/2012 AGN activity in theoretical models of galaxy formation Represents a viable solution for a number of long-standing theoretical problems Properties
More informationIntroduction to AGN. General Characteristics History Components of AGN The AGN Zoo
Introduction to AGN General Characteristics History Components of AGN The AGN Zoo 1 AGN What are they? Active galactic nucleus compact object in the gravitational center of a galaxy that shows evidence
More informationSuperbubble Feedback in Galaxy Formation
Superbubble Feedback in Galaxy Formation Ben Keller (McMaster University) James Wadsley, Samantha Benincasa, Hugh Couchman Paper: astro-ph/1405.2625 (Accepted MNRAS) Keller, Wadsley, Benincasa & Couchman
More informationAstro2010 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 informationThe 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 informationAstr 2320 Thurs. April 27, 2017 Today s Topics. Chapter 21: Active Galaxies and Quasars
Astr 2320 Thurs. April 27, 2017 Today s Topics Chapter 21: Active Galaxies and Quasars Emission Mechanisms Synchrotron Radiation Starburst Galaxies Active Galactic Nuclei Seyfert Galaxies BL Lac Galaxies
More informationPowering Active Galaxies
Powering Active Galaxies Relativity and Astrophysics ecture 35 Terry Herter Bonus lecture Outline Active Galaxies uminosities & Numbers Descriptions Seyfert Radio Quasars Powering AGN with Black Holes
More informationThus 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 informationBlack Holes in the Early Universe Accretion and Feedback
1 1 Black Holes in the Early Universe Accretion and Feedback 1 1 Black Holes in the Early Universe Accretion and Feedback Geoff Bicknell & Alex Wagner Australian National University 1 1 High redshift radio
More informationIn 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 informationActive Galactic Nuclei - Zoology
Active Galactic Nuclei - Zoology Normal galaxy Radio galaxy Seyfert galaxy Quasar Blazar Example Milky Way M87, Cygnus A NGC 4151 3C273 BL Lac, 3C279 Galaxy Type spiral elliptical, lenticular spiral irregular
More informationThe Phenomenon of Active Galactic Nuclei: an Introduction
The Phenomenon of Active Galactic Nuclei: an Introduction Outline Active Galactic Nuclei (AGN): > Why are they special? > The power source > Sources of Continuum Emission > Emission & absorption lines
More informationThe Hot Gaseous Halos of Spiral Galaxies. Joel Bregman, Matthew Miller, Edmund Hodges Kluck, Michael Anderson, XinyuDai
The Hot Gaseous Halos of Spiral Galaxies Joel Bregman, Matthew Miller, Edmund Hodges Kluck, Michael Anderson, XinyuDai Hot Galaxy Halos and Missing Baryons Dai et al. (2010) Rich clusters have nearly all
More informationThree Major Components
The Milky Way Three Major Components Bulge young and old stars Disk young stars located in spiral arms Halo oldest stars and globular clusters Components are chemically, kinematically, and spatially distinct
More informationLecture 9. Quasars, Active Galaxies and AGN
Lecture 9 Quasars, Active Galaxies and AGN Quasars look like stars but have huge redshifts. object with a spectrum much like a dim star highly red-shifted enormous recessional velocity huge distance (Hubble
More informationAGN feedback and the connection to triggering
AGN feedback and the connection to triggering Ryan C. Hickox Dartmouth College The Triggering Mechanisms for Active Galactic Nuclei Lorentz Center, Leiden 26 July 2013 Illustration courtesy NASA Outline
More informationSimultaneous X-ray and Radio Observations of Seyferts, and Disk-Jet Connections
Simultaneous X-ray and Radio Observations of Seyferts, and Disk-Jet Connections Ashley Lianne King, University of Michigan Advisor: Jon M. Miller Collaborators: John Raymond, Michael Rupen, Kayhan Gültekin,
More informationThe Physics, Observational Signatures, and Consequences of AGN-Driven Galactic Winds
The Physics, Observational Signatures, and Consequences of AGN-Driven Galactic Winds ESA artist's conception Claude-André Faucher-Giguère Northwestern University CIERA With Eliot Quataert, Alex Richings,
More informationActive Galactic Nuclei-I. The paradigm
Active Galactic Nuclei-I The paradigm An accretion disk around a supermassive black hole M. Almudena Prieto, July 2007, Unv. Nacional de Bogota Centers of galaxies Centers of galaxies are the most powerful
More informationActive Galactic Nuclei
Active Galactic Nuclei Optical spectra, distance, line width Varieties of AGN and unified scheme Variability and lifetime Black hole mass and growth Geometry: disk, BLR, NLR Reverberation mapping Jets
More informationBlack Holes in Hibernation
Black Holes in Hibernation Black Holes in Hibernation Only about 1 in 100 galaxies contains an active nucleus. This however does not mean that most galaxies do no have SMBHs since activity also requires
More informationAGN 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 informationFormation of z~6 Quasars from Hierarchical Galaxy Mergers
Formation of z~6 Quasars from Hierarchical Galaxy Mergers Yuexing Li et al Presentation by: William Gray Definitions and Jargon QUASAR stands for QUASI-stellAR radio source Extremely bright and active
More informationThe Contribution of Active Galactic Nuclei to the Excess Cosmic Radio Background at 1.4 GHz
The Contribution of Active Galactic Nuclei to the Excess Cosmic Radio Background at 1.4 GHz David R. Ballantyne Center for Relativistic Astrophysics, School of Physics, Georgia Tech The Cosmic Backgrounds
More informationMulti-wavelength Surveys for AGN & AGN Variability. Vicki Sarajedini University of Florida
Multi-wavelength Surveys for AGN & AGN Variability Vicki Sarajedini University of Florida What are Active Galactic Nuclei (AGN)? Galaxies with a source of non-stellar emission arising in the nucleus (excessive
More informationTHE CONNECTION BETWEEN STAR FORMATION AND DARK MATTER HALOS AS SEEN IN THE INFRARED
ESLAB 2013 04/04/2013 Noordwijk THE CONNECTION BETWEEN STAR FORMATION AND DARK MATTER HALOS AS SEEN IN THE INFRARED Material at http://irfu.cea.fr/sap/phocea/page/index.php?id=537 Matthieu Béthermin In
More informationOur goals for learning: 2014 Pearson Education, Inc. We see our galaxy edge-on. Primary features: disk, bulge, halo, globular clusters All-Sky View
Our Galaxy Chapter 19 Lecture The Cosmic Perspective 19.1 The Milky Way Revealed What does our galaxy look like? What does our galaxy look like? How do stars orbit in our galaxy? Seventh Edition Our Galaxy
More informationActive 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 informationStar Formation Indicators
Star Formation Indicators Calzetti 2007 astro-ph/0707.0467 Brinchmann et al. 2004 MNRAS 351, 1151 SFR indicators in general! SFR indicators are defined from the X ray to the radio! All probe the MASSIVE
More informationQuasars and AGN. What are quasars and how do they differ from galaxies? What powers AGN s. Jets and outflows from QSOs and AGNs
Goals: Quasars and AGN What are quasars and how do they differ from galaxies? What powers AGN s. Jets and outflows from QSOs and AGNs Discovery of Quasars Radio Observations of the Sky Reber (an amateur
More informationObservational Evidence of AGN Feedback
10 de maio de 2012 Sumário Introduction AGN winds Galaxy outflows From the peak to the late evolution of AGN and quasars Mergers or secular evolution? The AGN feedback The interaction process between the
More information(Astro)Physics 343 Lecture # 12: active galactic nuclei
(Astro)Physics 343 Lecture # 12: active galactic nuclei Schedule for this week Monday & Tuesday 4/21 22: ad hoc office hours for Lab # 5 (you can use the computer in my office if necessary; Sections A
More informationGas 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 informationPaul Sell. University of Wisconsin-Madison Advisor: Christy Tremonti
A SAMPLE OF EXTREME MERGER-DRIVEN STARBURST GALAXIES AS VIEWED BY THE CHANDRA AND HUBBLE SPACE TELESCOPES Paul Sell University of Wisconsin-Madison Advisor: Christy Tremonti Collaboration: Aleks Diamond-Stanic,
More informationJunfeng Wang, G. Fabbiano, G. Risaliti, M. Elvis, M. Karovska, A. Zezas (Harvard CfA/SAO), C. G. Mundell (Liverpool John Moores University, UK), G.
Junfeng Wang, G. Fabbiano, G. Risaliti, M. Elvis, M. Karovska, A. Zezas (Harvard CfA/SAO), C. G. Mundell (Liverpool John Moores University, UK), G. Dumas, E. Schinnerer (MPIA), J. M. Mazzarella, J. H.
More informationTheoretical ideas About Galaxy Wide Star Formation! Star Formation Efficiency!
Theoretical ideas About Galaxy Wide Star Formation Theoretical predictions are that galaxy formation is most efficient near a mass of 10 12 M based on analyses of supernova feedback and gas cooling times
More informationJoop Schaye (Leiden) (Yope Shea)
Overview of sub-grid models in cosmological simulations Joop Schaye (Leiden) (Yope Shea) Length Scales (cm) Subgrid models Cosmological simulations 8 0 2 11 18 20 22 24 28 interparticle distance in stars
More informationThe Merger-Driven Star Formation History of the Universe
The Merger-Driven Star Formation History of the Universe Lars Hernquist, TJ Cox, Dusan Keres, Volker Springel, Philip Hopkins 08/17/07 Rachel Somerville (MPIA), Gordon Richards (JHU), Kevin Bundy (Caltech),
More informationQuasars ASTR 2120 Sarazin. Quintuple Gravitational Lens Quasar
Quasars ASTR 2120 Sarazin Quintuple Gravitational Lens Quasar Quasars Quasar = Quasi-stellar (radio) source Optical: faint, blue, star-like objects Radio: point radio sources, faint blue star-like optical
More informationGALAXIES. Edmund Hodges-Kluck Andrew Ptak
GALAXIES Edmund Hodges-Kluck Andrew Ptak Galaxy Science with AXIS How does gas get into and out of galaxies? How important is hot accretion for L* or larger galaxies? How does star formation/black hole
More informationSupernova Feedback in Low and High Mass Galaxies: Luke Hovey 10 December 2009
Supernova Feedback in Low and High Mass Galaxies: Luke Hovey 10 December 2009 Galactic Winds: Mathews, W. et al. 1971 Effects of Supernovae on the Early Evolution of Galaxies: Larson, R. 1974 The origin
More informationStars, 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 informationDLAs Probing Quasar Host Galaxies. Hayley Finley P. Petitjean, P. Noterdaeme, I. Pâris + SDSS III BOSS Collaboration 2013 A&A
DLAs Probing Quasar Host Galaxies Hayley Finley P. Petitjean, P. Noterdaeme, I. Pâris + SDSS III BOSS Collaboration 2013 A&A 558 111 Outline Feedback mechanisms in QSO host galaxies Strong DLAs at zqso
More informationProbing the End of Dark Ages with High-redshift Quasars. Xiaohui Fan University of Arizona Dec 14, 2004
Probing the End of Dark Ages with High-redshift Quasars Xiaohui Fan University of Arizona Dec 14, 2004 High-redshift Quasars and the End of Cosmic Dark Ages Existence of SBHs at the end of Dark Ages BH
More informationPart 2. Hot gas halos and SMBHs in optically faint ellipticals. Part 3. After Chandra?
Hot gas and AGN Feedback in Nearby Groups and Galaxies Part 1. Cool cores and outbursts from supermassive black holes in clusters, groups and normal galaxies Part 2. Hot gas halos and SMBHs in optically
More informationThe visible constituents of the Universe: Non-relativistic particles ( baryons ): Relativistic particles: 1. radiation 2.
The visible constituents of the Universe: Non-relativistic particles ( baryons ): Galaxies / Clusters / Super-clusters Intergalactic Medium Relativistic particles: 1. radiation 2. neutrinos Dark sector
More informationLuminous 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 informationStar 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 informationQuasar Feedback in Galaxies
Quasar Feedback in Galaxies Philip Hopkins Lars Hernquist, Norm Murray, Eliot Quataert, Todd Thompson, Dusan Keres, Chris Hayward, Stijn Wuyts, Kevin Bundy, Desika Narayanan, Ryan Hickox, Rachel Somerville,
More informationActive Galactic Nuclei (AGNs): A type of AGNs: Quasars. Whatever is powering these QSO s must be very small!!
Active Galactic Nuclei (AGNs): Galaxies with lots of activity AST 101 General Astronomy: Stars & Galaxies Some galaxies at high redshift (large lookback times) have extremely active centers More than 1000
More informationGalaxies with Active Nuclei. Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes
Galaxies with Active Nuclei Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes Active Galactic Nuclei About 20 25% of galaxies do not fit well into Hubble categories
More informationSome 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 informationGalaxy Activity in Semi Analytical Models. Fabio Fontanot (INAF OATs) Ljubljana 05/04/11
Galaxy Activity in Semi Analytical Models Fabio Fontanot (INAF OATs) Ljubljana 05/04/11 Part I: Theoretical background 1. Baryonic gas falls in the gravitational potential of Dark Matter Halos 2. Baryonic
More informationFeedback and Galaxy Formation
Heating and Cooling in Galaxies and Clusters Garching August 2006 Feedback and Galaxy Formation Simon White Max Planck Institute for Astrophysics Cluster assembly in ΛCDM Gao et al 2004 'Concordance'
More informationAstronomy 1 Fall 2016
Astronomy 1 Fall 2016 Lecture11; November 1, 2016 Previously on Astro-1 Introduction to stars Measuring distances Inverse square law: luminosity vs brightness Colors and spectral types, the H-R diagram
More informationAGN Feedback. Andrew King. Dept of Physics & Astronomy, University of Leicester Astronomical Institute, University of Amsterdam. Heidelberg, July 2014
AGN Feedback Andrew King Dept of Physics & Astronomy, University of Leicester Astronomical Institute, University of Amsterdam Heidelberg, July 2014 galaxy knows about central SBH mass velocity dispersion
More informationFormation and growth of galaxies in the young Universe: progress & challenges
Obergurgl. April 2014 Formation and growth of galaxies in the young Universe: progress & challenges Simon White Max Planck Institute for Astrophysics Ly α forest spectra and small-scale initial structure
More informationThe Interstellar Medium
The Interstellar Medium Fall 2014 Lecturer: Dr. Paul van der Werf Oortgebouw 565, ext 5883 pvdwerf@strw.leidenuniv.nl Assistant: Kirstin Doney Huygenslaboratorium 528 doney@strw.leidenuniv.nl Class Schedule
More informationMultiwavelength observation campaign of Mrk 509: UV spectra of the X-ray Outflow!!!!Gerard Kriss!! STScI!!! (with N. Arav, J. Kaastra & the Mrk 509
Multiwavelength observation campaign of Mrk 509: UV spectra of the X-ray Outflow!!!!Gerard Kriss!! STScI!!! (with N. Arav, J. Kaastra & the Mrk 509 Team)!! The Influence of AGN Outflows! «They may affect
More informationThe Impact of Quasar Feedback on the Formation & Evolution of Red Galaxies
The Impact of Quasar Feedback on the Formation & Evolution of Red Galaxies Philip Hopkins 07/17/06 Lars Hernquist, Volker Springel, Gordon Richards, T. J. Cox, Brant Robertson, Tiziana Di Matteo, Yuexing
More informationSolving. Andrey Kravtsov The University of Chicago Department of Astronomy & Astrophysics Kavli Institute for Cosmological Physics
Solving Constraining galaxy formation with gaseous halos Andrey Kravtsov The University of Chicago Department of Astronomy & Astrophysics Kavli Institute for Cosmological Physics X-ray Vision workshop:
More informationChapter 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 informationHalo Gas Velocities Using Multi-slit Spectroscopy
Halo Gas Velocities Using Multi-slit Spectroscopy Cat Wu Thesis Proposal, Fall 2009 Astronomy Department New Mexico State University Outline Diffuse ionized gas; galaxy halos Origin of halo galactic fountain
More informationThe Superbubble Power Problem: Overview and Recent Developments. S. Oey
The Superbubble Power Problem: Overview and Recent Developments S. Oey It has been known for decades that superbubbles generated by massive star winds and supernovae are smaller than expected based on
More informationReminders! Observing Projects: Both due Monday. They will NOT be accepted late!!!
Reminders! Website: http://starsarestellar.blogspot.com/ Lectures 1-15 are available for download as study aids. Reading: You should have Chapters 1-14 read. Read Chapters 15-17 by the end of the week.
More informationGas in and around z > 2 galaxies
Gas in and around z > 2 galaxies Michele Fumagalli August 2010 Santa Cruz Xavier Prochaska Daniel Kasen Avishai Dekel In collaboration with: Daniel Ceverino Joel Primack Gas in galaxies from theory Gas
More informationThe X-Ray Universe. The X-Ray Universe
The X-Ray Universe The X-Ray Universe Potsdam University Dr. Lidia Oskinova Sommersemester 2017 lida@astro.physik.uni-potsdam.de astro.physik.uni-potsdam.de ~lida/vorlesungxrayso17.html Chandra X-ray,
More informationAstronomy 422! Lecture 7: The Milky Way Galaxy III!
Astronomy 422 Lecture 7: The Milky Way Galaxy III Key concepts: The supermassive black hole at the center of the Milky Way Radio and X-ray sources Announcements: Test next Tuesday, February 16 Chapters
More informationThe first black holes
The first black holes Marta Volonteri Institut d Astrophysique de Paris M. Habouzit, Y. Dubois, M. Latif (IAP) A. Reines (NOAO) M. Tremmel (University of Washington) F. Pacucci (SNS) High-redshift quasars
More informationThe Illustris simulation: a new look at galaxy black hole co-evolution. Debora Sijacki IoA & KICC Cambridge
The Illustris simulation: a new look at galaxy black hole co-evolution Debora Sijacki IoA & KICC Cambridge LSS conference July 23 2015 Cosmological simulations of galaxy and structure formation Hierarchical
More informationChapter 19: Our Galaxy
Chapter 19 Lecture Chapter 19: Our Galaxy Our Galaxy 19.1 The Milky Way Revealed Our goals for learning: What does our galaxy look like? How do stars orbit in our galaxy? What does our galaxy look like?
More informationWhat Doesn t Quench Galaxy Formation?
What Doesn t Quench Galaxy Formation? Phil Hopkins Dusan Keres, Claude Faucher-Giguere, Jose Onorbe, Freeke van de Voort, Sasha Muratov, Xiangcheng Ma, Lena Murchikova, Norm Murray, Eliot Quataert, James
More informationSURVEYS: THE MASS ASSEMBLY AND STAR FORMATION HISTORY
Lecture #4 SURVEYS: THE MASS ASSEMBLY AND STAR FORMATION HISTORY Observational facts Olivier Le Fèvre ON Rio de Janeiro School 2014 Putting it all together Clear survey strategies Instrumentation and observing
More informationProbing 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 informationAstr 5465 Feb. 5, 2018 Kinematics of Nearby Stars
Astr 5465 Feb. 5, 2018 Kinematics of Nearby Stars Properties of Nearby Stars Most in orbit with the Sun around Galactic Center Stellar Kinematics Reveal Groups of Stars with Common Space Motion (Moving
More informationMulti-Phase Outflows in ULIRGs
Multi-Phase Outflows in ULIRGs Sylvain Veilleux (U. Maryland, Joint Space-Science Institute) Powerful wide-angle outflow in Mrk 231, the nearest quasar Gemini Press Release (based on the results of Rupke
More informationQuasar Absorption Lines
Tracing the Cosmic Web with Diffuse Gas DARK MATTER GAS STARS NEUTRAL HYDROGEN Quasar Absorption Lines use quasars as bright beacons for probing intervening gaseous material can study both galaxies and
More informationEnergy 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 informationAGN and Radio Galaxy Studies with LOFAR and SKA
AGN and Radio Galaxy Studies with LOFAR and SKA Andrei Lobanov MPIfR, Bonn AGN/RG Science AGN/RG drivers for LOFAR and SKA: astrophysical masers, nuclear regions of AGN, physics of relativistic and mildly
More informationEnergy 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 informationthe self-regulated agn feedback loop: chaotic cold accretion
the self-regulated agn feedback loop: chaotic cold accretion Massimo Gaspari Max Planck Institute for Astrophysics the self-regulated agn feedback loop: raining onto black holes Massimo Gaspari Max Planck
More informationActive Galactic Nuclei
Active Galactic Nuclei Prof. Jeff Kenney Class 18 June 20, 2018 the first quasar discovered 3C273 (1963) very bright point source (the quasar ) jet the first quasar discovered 3C273 (1963) very bright
More informationGRB history. Discovered 1967 Vela satellites. classified! Published 1973! Ruderman 1974 Texas: More theories than bursts!
Discovered 1967 Vela satellites classified! Published 1973! GRB history Ruderman 1974 Texas: More theories than bursts! Burst diversity E peak ~ 300 kev Non-thermal spectrum In some thermal contrib. Short
More information