Active Galactic Nuclei SEDs as a function of type and luminosity
|
|
- Molly Grant
- 5 years ago
- Views:
Transcription
1 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 (SAO), R. Kilgard (Wesleyan University) 1
2 Key questions Q: What is the range of AGN SEDs? Well sampled multi-λ SEDs of AGNs (e.g. Elvis et al. 1994) Q: What physical components and processes are at the origin of AGN SEDs? Model both the host and the AGN (e.g. Silva et al. 2004) Q: Do AGN SEDs behave as predicted by current models (evolutionary model, receding torus, unification model)? Investigate dependency of main parameters (e.g. Maiolino et al. 2007) Q: Do we have the data, and the techniques to do all of the above? 2
3 AGN emitting components Torus Obscuration Accretion disk + BLR+NLR Infrared Optical Type 1 Unobscured Type 2 Obscured Host galaxy Elliptical (Hönig et al. 2006) Illustration: CXC/Weiss Spiral Starburst ULIRG X 3
4 Do AGN properties depend on their evolutionary stage? AGN: Obscured AGN Obscured QSO Unobscured AGN Merger of large galaxies Host: Star-forming galaxy Starburst Elliptical AGN luminosity and absorption evolution (Hopkins et al. 2005) AGN feedback Fuel exhaustion Halt of star-formation Starburst Bulge & SMBH growth (Di Matteo et al. 2005)
5 X-ray selected AGN sample XMM-Newton Medium Deep Survey (Chiappetti et al. 2005; Polletta et al. 2007) 02h 30m, -5 (SWIRE/XMM-LSS) F(2-10 kev)>10-14 erg cm -2 s sources 71 spectroscopic z photo-z Chandra/SWIRE Survey (Polletta et al. 2006; Trouille et al. 2008) 10h 46m, +59 (SWIRE/Lockman Hole) F(0.3-8 kev)>3x10-15 erg cm -2 s sources 309 spectroscopic z Multi-λ data: Ugriz J(H)K Spitzer ( μm) VLA (20cm) XMDS Chandra/SWIRE 5
6 Spectral Energy Distribution Classification Galaxy & AGN template Library Spirals & Ellipticals Starbursts & Seyferts Stars Dust Stars Dust Acc. + Disk Disk QSOs Dust (Polletta et al. 2007; Silva et al. 1998; Berta et al. 2003; 2005; Hatziminaoglou et al. 2005) 6
7 X-ray selected AGN SEDs Star-forming like AGN SEY1.8 & AGN2 AGN1 Elliptical (2%) Sey1.8 (10%) AGN1 (26%) Star-forming galaxy (33%) AGN2 (29%) (Polletta et al. 2007) 7
8 Optical-IR SEDs vs X-ray properties Median XOI SEDs of X-ray selected AGNs Type 1 QSO template (Elvis et al. 1994) AGN1 Sey1.8 AGN2 Star-forming like AGN ELL Dominant energy source vs λ Class Optical Infrared X-ray AGN1 AGN AGN Unabsorbed Sey1.8 Host galaxy AGN Unabsorbed 543 X-ray selected AGNs from the XMDS & Chandra/SWIRE surveys (Chiappetti et al. 2005; Polletta et al. 2006) AGN2 Host galaxy AGN Absorbed SFG Host galaxy Host galaxy Very absorbed ELL Host galaxy Host galaxy Unabs. & Weak 8
9 Gas absorption vs Type Overall the SED classification correlates with the absorption in the X-rays (N H ) N H from X-ray spectral fitting or Hardness Ratio AGN1 Sey1.8 AGN2 Star-forming like AGN 9
10 Median X-ray-Optical-Infrared SEDs vs X-ray Luminosity AGN1 Sey1.8 L(X) vs L(MIR) Bluer? Log(L X )< <Log(L X )<44.89 Log(L X )>44.89 Log(L X )< <Log(L X )<44.21 Log(L X )>44.21 AGN2 Redder? Star-forming like AGN Host type Log(L X )< <Log(L X )<44.48 Log(L X )>44.48 Log(L X )< <Log(L X )<44.35 Log(L X )>
11 SED Modeling (separating AGN and Host) Input : rest-frame SED [4-13 points] QSO template (Elvis et al. 1994) Model: - Host (26 templates: ell, spirals, starbursts) - type 1 AGN (3 templates) (Polletta et al. 2007, Silva et al. 1998, da Cunha et al. 2008) Model parameters [5]: L(Host), Host type, L(AGN), AGN type, AGN extinction (A V ) 11
12 AGN SED type vs Luminosity & Redshift AGN1 AGN dominates at all wavelengths and it is unobscured. Host consistent with early-type spiral. L Host galaxy scales with L AGN All Log(L X )< <Log(L X )<44.89 Log(L X )>
13 AGN SED type vs Luminosity & Redshift SEY18 AGN dominates atλ>2μm, Host dominates at optical & near-ir λ, similar contributions in the UV Host consistent with late-type spiral. L AGN /L Host increases with LX All Log(L X )< <Log(L X )<44.21 Log(L X )>
14 AGN SED type vs Luminosity & Redshift AGN2 AGN dominates atλ>2μm, Host dominates at λ<2μm if AGN is moderately - luminous. AGN might dominate at all wavelengths if highly luminous. AGN is heavily obscured. Host consistent with late-type spiral. L AGN /L Host increases with LX All Log(L X )< <Log(L X )<44.48 Log(L X )>
15 AGN SED type vs Luminosity & Redshift Star-forming like AGN AGN dominates atλ>3-5μm. AGN is characterized by a wide range of obscuration. Host consistent with star-forming galaxy. L AGN /L Host increases with LX All Log(L X )< <Log(L X )<44.35 Log(L X )>
16 Summary: AGN SED type vs Luminosity & Redshift 1) L(AGN)/L(Host) increases with L X in all types, but at different rates AGN1 Sey1.8 AGN2 SFG 16
17 Summary: AGN SED type vs Luminosity & Redshift 1) L(AGN)/L(Host) increases with L X in all types, but at different rates 2) No or little obscuration in AGN1 and Sey1.8, high obscuration in AGNs, wide range of obscuration in SFGs A V applied to AGN template in SED modeling AGN1 Sey1.8 AGN2 Star-forming like AGN 17
18 Summary: AGN SED type vs Luminosity & Redshift 1) L(AGN)/L(Host) increases with L X in all types, but at different rates 2) No or little obscuration in AGN1 and Sey1.8, high obscuration in AGNs, wide range of obscuration in SFGs 3) Host galaxy: AGN1 Sey1.8 & AGN2 SFG early spiral late spiral star-forming 4) AGN vs Host AGN1: AGN > host SEY1.8: AGN>Host atλ>2 μm and AGN Host in the UV AGN2: AGN>Host atλ>2 μm at low L(AGN), at all λ at high L(AGN) SFG: AGN>Host atλ>3-5 μm 18
19 From large sample studies to specific cases (small sub-samples with a bit more data) Mid-infrared spectra warm dust (torus) properties Study case: 21 Spitzer-selected AGN2 at high luminosity Far-infrared data cool/cold dust (starburst, cirrus) component Study case: 10 Spitzer-selected AGN2 at high luminosity detected at 70μm, 160μm or 1.2mm 19
20 Mid-infrared SEDs and spectra of obscured QSOs Model: Clumpy Torus (Hönig et al. 2006) Elliptical (host) (Silva et al. 1998) Total (host+torus) (Polletta et al. 2008a) 20
21 Mid-infrared SEDs and spectra of obscured QSOs Model: Clumpy Torus (Hönig et al. 2006) Elliptical (host) (Silva et al. 1998) Total (host+torus) (Polletta et al. 2008a) 21
22 Modeling failures and solution Torus+Host+ COLD Torus ABSORBER Host Torus Host External obscuration already proposed by Keel 1980; Lawrence & Elvis 1982; see also Rigby et al. 2006; Brand et al. 2007, Urrutia et al. 2007; Sajina et al Cold Absorber: Galactic center extinction curve (Chiar & Tielens 2006) SED Fitting 23 Workshop 22
23 Fitting the far-infrared emission of obscured QSOs AGNs detected at 70 or 160μm evidence for starburst component M 82 Torus Elliptical Total Log(νLν) (erg s -1 ) Log(νLν) (erg s -1 ) Rest-frame Log(λ) (μm) Rest-frame Log(λ) (μm) Rest-frame Log(λ) (μm) Rest-frame Log(λ) (μm) Starburst with L(FIR) L SFR M /yr (Polletta et al., 2008a) 23
24 Far-infrared/mm emission of obscured QSOs High-z obscured QSOs detected at mm wavelengths BUT Need far-ir data to constrain the FIR emission? z= mm? z= mm (Polletta et al. 2008b) L(AGN) ~ L & L(SB) ~ L 24
25 Summary X-ray-Optical-Infrared SEDs of 536 X-ray selected AGNs from the XMDS and SWIRE/ Chandra surveys SED classification based on fitting the SEDs with templates Median XOI SEDs built for each type and as a function of L X Optical-IR SEDs modeled with 2 components: host galaxy + AGN and 5 parameters (host type and luminosity, AGN type, extinction, and luminosity) SEDs cover a broad range of types (AGN1, SEY18, AGN2, SFG, ELL) mostly due to a combination of L(Host)/L(AGN), and AGN obscuration (not to the host type) Optical-Infrared SED types correlate with the X-ray spectrum (absorption) and dust extinction The SEDs change with the X-ray luminosity because of changes in the AGN/Host ratio (not observed in AGN1) Detailed modeling of AGN dust components is becoming possible. Study cases presented on hot/warm dust and cool/cold dust. Good perspectives to constrain torus models and AGN dust properties with mid-ir spectroscopy (IRS) and far-ir/sub-mm/mm sensitive observations (Herschel, SCUBA2) 25
Active Galactic Nuclei in the infrared: identification, energetic and properties of the obscuring material
Active Galactic Nuclei in the infrared: identification, energetic and properties of the obscuring material Mari Polletta (Institut d Astrophysique de Paris) Collaborators: D. Weedman (Cornell U.), S. Hoenig
More informationWhat s the fuss about AGN?
What s the fuss about AGN? Mari Polletta (IASF-INAF Milan, Italy) 1 Outline What is an Active Galactic Nucleus (AGN)? AGN role and importance AGN evolutionary models and feedback Star-formation and AGN
More informationRadio Properties Of X-Ray Selected AGN
Radio Properties Of X-Ray Selected AGN Manuela Molina In collaboration with: M. Polletta, L. Chiappetti, L. Paioro (INAF/IASF-Mi), G.Trinchieri (OA Brera), F. Owen (NRAO) and Chandra/SWIRE Team. Astrosiesta,
More informationMULTI-WAVELENGTH OBSERVATIONS OF X-RAY SELECTED AGN: WHAT WE NEED AND WHY
1 MULTI-WAVELENGTH OBSERVATIONS OF X-RAY SELECTED AGN: WHAT WE NEED AND WHY M. Polletta 1,2 and D. M. Alexander 3 1 INAF - IASF Milan, via E. Bassini 15, 20133 Milan, Italy 2 Institut d Astrophysique de
More informationChien-Ting Chen! Dartmouth College
AGN vs SF 2014 Durham University Obscuration and Star formation in Luminous Quasars Chien-Ting Chen! Dartmouth College In collaboration with: Ryan C. Hickox, Stacey Alberts, David M. Alexander, Roberto
More informationThe bolometric output of AGN in the XMM-COSMOS survey
The bolometric output of AGN in the XMM-COSMOS survey Elisabeta Lusso Dipartimento di Astronomia Università di Bologna-INAF/OABO A. Comastri, C. Vignali, G. Zamorani, M. Brusa, E. Treister, R. Gilli, M.
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 informationHard X-ray AGN and the Cosmic X-ray Background
Hard X-ray AGN and the Cosmic X-ray Background Sergey Sazonov Space Research Institute, Moscow, Russia 1 Rome, Oct. 17, 2013 Plan Cosmic X-ray background: measurements, modeling and implications for heavily
More informationarxiv:astro-ph/ v1 12 Mar 2007
Spectral Energy Distributions of Hard X-ray selected AGNs in the XMDS Survey arxiv:astro-ph/0703255v1 12 Mar 2007 M. Polletta 1, M. Tajer 2,3, L. Maraschi 2, G. Trinchieri 2, C.J. Lonsdale 1, L. Chiappetti
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 informationOBSCURATION IN EXTREMELY LUMINOUS QUASARS
The Astrophysical Journal, 675:960Y984, 2008 March 10 # 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A. A OBSCURATION IN EXTREMELY LUMINOUS QUASARS M. Polletta, 1,2 D. Weedman,
More informationIRS Spectroscopy of z~2 Galaxies
IRS Spectroscopy of z~2 Galaxies Houck et al., ApJ, 2005 Weedman et al., ApJ, 2005 Lutz et al., ApJ, 2005 Astronomy 671 Jason Marshall Opening the IR Wavelength Regime for Discovery One of the primary
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 informationUltra 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 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 informationObserving 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 mid and far-ir view of the star formation activity in galaxy systems and their surroundings
A mid and far-ir view of the star formation activity in galaxy systems and their surroundings Andrea Biviano Andrea Biviano INAF/Osservatorio Astronomico di Trieste Outline: mid-ir & multiwavelength observations
More informationDusty star-forming galaxies at high redshift (part 5)
Dusty star-forming galaxies at high redshift (part 5) Flow of story 4.1 4.2 4.3 Acquiring Spectroscopic or Photometric Redshifts Infrared SED Fitting for DSFGs Estimating L IR, T dust and M dust from an
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 informationMulti-wavelength ISM diagnostics in high redshift galaxies
Multi-wavelength ISM diagnostics in high redshift galaxies Alexandra Pope (UMass Amherst) Transformational Science in the ALMA Era: Multi-Wavelength Studies of Galaxy Evolution Conference Charlottesville,
More informationMulti-wavelength analysis of Hickson Compact Groups of Galaxies.
Multi-wavelength analysis of Hickson Compact Groups of Galaxies. Thodoris Bitsakis Department of Physics, University of Crete Paper: Bitsakis T., Charmandaris V., da Cunha E., Diaz-Santos T., Le Floc h
More informationLecture 11: SDSS Sources at Other Wavelengths: From X rays to radio. Astr 598: Astronomy with SDSS
Astr 598: Astronomy with SDSS Spring Quarter 4, University of Washington, Željko Ivezić Lecture : SDSS Sources at Other Wavelengths: From X rays to radio Large Surveys at Many Wavelengths SDSS: UV-IR five-band
More informationTHE XMM-NEWTON AND SPITZER VIEW OF GALAXY/AGN FORMATION AT. F.J. Carrera, J. Ebrero 1, M.J. Page 2, and J.A. Stevens 3
1 THE XMM-NEWTON AND SPITZER VIEW OF GALAXY/AGN FORMATION AT F.J. Carrera, J. Ebrero 1, M.J. Page 2, and J.A. Stevens 3 1 Instituto de Física de Cantabria, Avenida de los Castros, 39005 Santander, Spain
More informationFeeding the Beast. Chris Impey (University of Arizona)
Feeding the Beast Chris Impey (University of Arizona) Note: the box is growing due to cosmic expansion but this is factored out. Heirarchical Structure Active Galactic Nuclei (AGN) Nuclear activity in
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 informationConnection between AGN and Star Formation activities, or not?
Connection between AGN and Star Formation activities, or not? Y.Sophia Dai ( 戴昱 ) National Astronomical Observatories of China (NAOC) daysophia@gmail.com Close Correlations between SMBH and hosts M SMBH
More informationAstr 2320 Thurs. April 27, 2017 Today s Topics. Chapter 21: Active Galaxies and Quasars
Astr 2320 Thurs. April 27, 2017 Today s Topics Chapter 21: Active Galaxies and Quasars Emission Mechanisms Synchrotron Radiation Starburst Galaxies Active Galactic Nuclei Seyfert Galaxies BL Lac Galaxies
More informationACTIVE GALACTIC NUCLEI I. AN INTRODUCTION Sebastian F. Hoenig Lecturer & Marie Curie Fellow Outline and learning goals I. Phenomenology What are AGN? How are they identified? II. Energy output Where is
More informationHunting for Monsters. Selecting and Characterizing Obscured Quasars with WISE Kevin Hainline Hidden Monsters Dartmouth College August 2016
Hunting for Monsters Selecting and Characterizing Obscured Quasars with WISE Kevin Hainline Hidden Monsters Dartmouth College August 2016 Ryan Hickox Dartmouth College Mike DiPompeo Christopher Carroll
More informationThe 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 informationSOFIA/HAWC+ Detection of a Gravitationally Lensed Starburst Galaxy at z = 1.03
SOFIA/HAWC+ Detection of a Gravitationally Lensed Starburst Galaxy at z = 1.03 Jingzhe Ma University of California, Irvine Collaborators: Asantha Cooray, Arianna Brown, Hooshang Nayyeri, Hugo Messias,
More informationSPECTRAL ENERGY DISTRIBUTIONS OF HARD X-RAY SELECTED ACTIVE GALACTIC NUCLEI IN THE XMM-NEWTON MEDIUM DEEP SURVEY
The Astrophysical Journal, 663:81Y102, 2007 July 1 # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. A SPECTRAL ENERGY DISTRIBUTIONS OF HARD X-RAY SELECTED ACTIVE GALACTIC
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 informationOrianne 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 informationHigh-redshift galaxies
High-redshift galaxies Houjun Mo May 4, 2004 Galaxies can now be observed to z 6 Normal galaxies with 0.2 < z < 1 The Lyman-break population at z 3 The sub-mm sources at z 3 Between 1 2, spectroscopy desert,
More informationSUPPLEMENTARY INFORMATION
doi:10.1038/nature11096 Spectroscopic redshifts of CDF-N X-ray sources We have taken a recent compilation 13 as our main source of spectroscopic redshifts. These redshifts are given to two decimal places,
More informationSurvey of dusty AGNs based on the mid-infrared all-sky survey catalog. Shinki Oyabu (Nagoya University) & MSAGN team
Survey of dusty AGNs based on the mid-infrared all-sky survey catalog Shinki Oyabu (Nagoya University) & MSAGN team Search for Active Galactic Nuclei Purpose 1 The MIR selection can minimize wavelength-dependent
More informationResults from the Chandra Deep Field North
Results from the Chandra Deep Field North Brandt, Alexander, Bauer, Garmire, Hornschemeier, Immler, Lehmer, Schneider, Vignali, Wu, Barger, Cowie, Bautz, Nousek, Sargent, Townsley Chandra Deep Field North
More informationRadio Quiet AGN: Black Hole & Host Galaxy Proper;es
Radio Quiet AGN: Black Hole & Host Galaxy Proper;es (ESO) Collaborators: V. Mainieri, P. Padovani, P. Rosa6, N. Miller, K. I. Kellermann, P. Tozzi, S. Va>akunnel, A. Bongiorno, + PEP Collaboration Credit:
More informationMolecular 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 informationHard X-ray selected sample of AGN: population studies
Hard X-ray selected sample of AGN: population studies Angela Malizia INCREASE OF AGN POPULATION IN THE INTEGRAL SURVEYS most of the unidentified objects have been subsequently classified as AGN Many more
More informationThe Far-Infrared Radio Correlation in Galaxies at High Redshifts
The Far-Infrared Radio Correlation in Galaxies at High Redshifts Plan A My own work aims and methodology My results so far Implications of my results What I plan to do next brief summary of the FIR-Radio
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 informationThe Herschel Multi-tiered Extragalactic Survey (HerMES) The Evolution of the FIR/SMM Luminosity Function and of the Cosmic SFRD
The Herschel Multi-tiered Extragalactic Survey (HerMES) The Evolution of the FIR/SMM Luminosity Function and of the Cosmic SFRD Lucia Marchetti University of Padova - Open University Mattia Vaccari - University
More informationGalaxies 626. Lecture 10 The history of star formation from far infrared and radio observations
Galaxies 626 Lecture 10 The history of star formation from far infrared and radio observations Cosmic Star Formation History Various probes of the global SF rate: ρ* (z) M yr 1 comoving Mpc 3 UV continuum
More informationSpectral Energy Distributions as probes of star formation in the distant Universe
MODULO meeting 2-3 December 2010 Spectral Energy Distributions as probes of star formation in the distant Universe Simona Bovinelli ISSI International Space Science Institute IRAS (1983), ISO (1995) and
More informationBroadband 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 informationA Monster at any other Epoch:
A Monster at any other Epoch: Are Intermediate Redshift ULIRGs the Progenitors of QSO Host Galaxies? Barry Rothberg Large Binocular Telescope Observatory/George Mason University Co-Is: J. Fischer (NRL),
More informationGALAXY 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 informationChapter 17. Active Galaxies and Supermassive Black Holes
Chapter 17 Active Galaxies and Supermassive Black Holes Guidepost In the last few chapters, you have explored our own and other galaxies, and you are ready to stretch your scientific imagination and study
More informationAstr 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 informationThe search for. COSMOS and CDFS. Marcella Brusa
The search for obscured AGN in COSMOS and CDFS Marcella Brusa MPE - High Energy Group XMM view of the COSMOS field Results obtained in the framework of the COSMOS & CDFS/MUSIC teams: Bongiorno, Brunner,
More informationX-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 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 informationA TALE OF TWO MONSTERS: EMBEDDED AGN IN NGC6418 AND IRAS
A TALE OF TWO MONSTERS: EMBEDDED AGN IN NGC6418 AND IRAS16399 0937 Photometry Aperture 2.2 2.0 1.8 Optical 3.6 µm E 4.5 µm N Normalized flux 1.6 1.4 0 100 200 300 Figure 3.1: NGC6418 false color image
More informationarxiv: v1 [astro-ph.co] 27 May 2009
**FULL TITLE** ASP Conference Series, Vol. **VOLUME**, **YEAR OF PUBLICATION** **NAMES OF EDITORS** The Pedigrees of DOGs (Dust-Obscured Galaxies) arxiv:0905.453v [astro-ph.co] 27 May 2009 Arjun Dey National
More informationTHE EMISSION AND DISTRIBUTION OF DUST OF THE TORUS OF NGC 1068
THE EMISSION AND DISTRIBUTION OF DUST OF THE TORUS OF NGC 1068 ENRIQUE LOPEZ RODRIGUEZ Instrument Scientist (HAWC+) Stratospheric Observatory For Infrared Astronomy (SOFIA) / NASA elopezrodriguez@nasa.gov
More informationPROBING THE AGN/GALAXY CO-EVOLUTION AT ITS EXTREME
THE MOST LUMINOUS QUASARS: PROBING THE AGN/GALAXY CO-EVOLUTION AT ITS EXTREME Enrico Piconcelli Osservatorio Astronomico di Roma - INAF! A. Bongiorno, F. Fiore, M. Bischetti, L. Zappacosta OA-Roma! C.
More informationOutflows in local ULIRGS: [CII] 158 Broad Components and OH outflows
Outflows in local ULIRGS: [CII] 158 Broad Components and OH outflows Natalie Christopher, University of Oxford Dr Verma and Professor Roche, University of Oxford And the SHINING team, Lead by E. Sturm,
More informationActive Galactic Alexander David M Nuclei
d.m.alexander@durham.ac.uk Durham University David M Alexander Active Galactic Nuclei The Power Source QuickTime and a YUV420 codec decompressor are needed to see this picture. Black hole is one billionth
More informationMeasuring star formation in galaxies and its evolution. Andrew Hopkins Australian Astronomical Observatory
Measuring star formation in galaxies and its evolution Andrew Hopkins Australian Astronomical Observatory Evolution of Star Formation Evolution of Star Formation Evolution of Star Formation Evolution of
More informationThe symbiotic nature of AGN and SF activities of AGNs probed by the PAH 3.3 micron emission feature
The symbiotic nature of AGN and SF activities of AGNs probed by the PAH 3.3 micron emission feature Ji Hoon Kim Subaru Telescope National Astronomical Observatory of Japan Along with Myungshin Im, Dohyeong
More informationA zoo of transient sources. (c)2017 van Putten 1
A zoo of transient sources (c)2017 van Putten 1 First transient @ first light UDFj-39546284, z~10.3 Bouwens, R.J., et al., Nature, 469, 504 Cuchiara, A. et al., 2011, ApJ, 736, 7 z=9.4: GRB 090429B, z~9.4
More informationX-ray emission from star-forming galaxies
X-ray emission from star-forming galaxies, Marat Gilfanov & Rashid Sunyaev (Max Planck Institute for Astrophysics) Ultra-Luminous X-ray sources and Middle Weight Black Holes Monday May 24th, 2010 - ESAC
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 informationThe Massive Hosts of Radio Galaxies Across Cosmic Time
The Massive Hosts of Radio Galaxies Across Cosmic Time Nick Seymour (Spitzer Science Center/JPL) Obscured AGN Across Cosmic Time Seeon, June 7 th 2007 Co-conspirators: Daniel Stern (JPL), Carlos De Breuck,
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 informationGas Masses and Gas Fractions: Applications of the Kennicutt- Schmidt Law at High Redshift
Gas Masses and Gas Fractions: Applications of the Kennicutt- Schmidt Law at High Redshift Dawn Erb (CfA) Kennicutt-Schmidt Workshop, UCSD December 19, 2006 Overview Properties of star-forming galaxies
More informationWarm Molecular Hydrogen at high redshift with JWST
Warm Molecular Hydrogen at high redshift with JWST Pierre Guillard Institut d Astrophysique de Paris Université Pierre et Marie Curie he Warm H 2 with JWST Outline and take-home messages 1. Observations
More informationSurvey of dusty AGNs based on the mid-infrared all-sky survey catalog
Survey of dusty AGNs based on the mid-infrared all-sky survey catalog Shinki Oyabu (Nagoya University) & MSAGN team 1. Introduction 2. MSAGN 3. Results 1. AKARI results 2. Other activity 4. Dusty AGNs
More informationThe Bright Side of the X-ray Sky The XMM-Newton Bright Survey. R. Della Ceca. INAF Osservatorio Astronomico di Brera,Milan
The Bright Side of the X-ray Sky The XMM-Newton Bright Survey T. Maccacaro A. Caccianiga P. Severgnini V. Braito R. Della Ceca INAF Osservatorio Astronomico di Brera,Milan On behalf of the XMM-Newton Survey
More informationLeMMINGs the emerlin radio legacy survey of nearby galaxies Ranieri D. Baldi
LeMMINGs the emerlin radio legacy survey of nearby galaxies Ranieri D. Baldi in collaboration with I. McHardy, D. Williams, R. Beswick and many others The radio-loud / radio-quiet dichotomy Among the many
More informationA LARGE POPULATION OF MID-INFRAREDYSELECTED, OBSCURED ACTIVE GALAXIES IN THE BOÖTES FIELD
The Astrophysical Journal, 671:1365Y1387, 2007 December 20 # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. A A LARGE POPULATION OF MID-INFRAREDYSELECTED, OBSCURED ACTIVE
More informationDebate 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 informationActive Galactic Nuclei: Making the Most of the Great Observatories
Active Galactic Nuclei: Making the Most of the Great Observatories Niel Brandt (Penn State) AGN Spectral Energy Distribution 3.6-160 µm 1150-25000 A 0.3-8 kev Host galaxy Richards et al. (2006) Active
More informationX ray Survey Results on AGN Physics and Evolution Niel Brandt
X ray Survey Results on AGN Physics and Evolution Niel Brandt Chandra XMM Newton Photon statistics Hard response ACIS Best positions Highest sens. < 6 kev 50 250 times sens. of previous missions Good positions
More informationX-raying galactic feedback in nearby disk galaxies. Q. Daniel Wang University of Massachusetts
X-raying galactic feedback in nearby disk galaxies Q. Daniel Wang University of Massachusetts Chandra survey of diffuse X-ray emission from 53 edge-on galaxies i > 60 o, D < 30 Mpc (Li, J.-T. & Wang, Q.D.
More informationDust. The four letter word in astrophysics. Interstellar Emission
Dust The four letter word in astrophysics Interstellar Emission Why Dust Dust attenuates and scatters UV/optical/NIR Amount of attenuation and spectral shape depends on dust properties (grain size/type)
More informationChallenges in Finding AGNs in the Low Luminosity Regime. Shobita Satyapal Nick Abel(UC), Nathan Secrest (NRL), Amrit Singh (GMU), Sara Ellison(UVIC)
Challenges in Finding AGNs in the Low Luminosity Regime Shobita Satyapal Nick Abel(UC), Nathan Secrest (NRL), Amrit Singh (GMU), Sara Ellison(UVIC) Motivation and Overview Why are low luminosity AGNs important?
More informationDeep Surveys or How We Learn About the Early Universe When We Can t Measure All that Would Be Nice!
Deep Surveys or How We Learn About the Early Universe When We Can t Measure All that Would Be Nice! Presented at the AAS Seminar on Infrared Astronomy, AAS Meeting, Jan 7, 2003, Seattle Marcia Rieke mrieke@as.
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 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 informationGalaxies. Need a (physically) meaningful way of describing the relevant properties of a galaxy.
Galaxies Aim to understand the characteristics of galaxies, how they have evolved in time, and how they depend on environment (location in space), size, mass, etc. Need a (physically) meaningful way of
More informationAstronomy across the spectrum: telescopes and where we put them. Martha Haynes Discovering Dusty Galaxies July 7, 2016
Astronomy across the spectrum: telescopes and where we put them Martha Haynes Discovering Dusty Galaxies July 7, 2016 CCAT-prime: next generation telescope CCAT Site on C. Chajnantor Me, at 18,400 feet
More informationThe History of Active Galaxies A.Barger, P. Capak, L. Cowie, RFM, A. Steffen, and Y. Yang
The History of Active Galaxies A.Barger, P. Capak, L. Cowie, RFM, A. Steffen, and Y. Yang Active Galaxies (AKA quasars, Seyfert galaxies etc) are radiating massive black holes with L~10 8-10 14 L sun The
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 informationIntroduction and Motivation
1 Introduction and Motivation This last two days at this conference, we ve focused on two large questions regarding the role that AGNs play in galaxy evolution: My research focuses on exploring these questions
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 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 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 informationStarbursts, 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 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 informationObscured AGN. I. Georgantopoulos National Observatory of Athens
Obscured AGN I. Georgantopoulos National Observatory of Athens Talk Outline Rationale: Why obscured AGN are important (especially the Compton-thick AGN) Obscured AGN from X-ray surveys (Chandra, XMM, Swift/BAT,
More informationQuasars 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 informationGas Accretion & Outflows from Redshift z~1 Galaxies
Gas Accretion & Outflows from Redshift z~1 Galaxies David C. Koo Kate Rubin, Ben Weiner, Drew Phillips, Jason Prochaska, DEEP2, TKRS, & AEGIS Teams UCO/Lick Observatory, University of California, Santa
More informationStudying Merger Driven BH Growth with Observations of Dual AGN
Studying Merger Driven BH Growth with Observations of Dual AGN Mike Koss University of Hawaii Richard Mushotzky and Sylvain Veilleux (U Maryland), Dave Sanders and Vivan U (Hawaii), Ezequiel Treister (U
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 informationCO 近赤外線吸収から探る銀河中心 pc スケールでのガスの物理状態 : あかりと Spitzer による低分散分光観測
ALMAワークショップ AGN 銀河質量降着 @sub-kpc @ 国立天文台三鷹 21 Dec. 2015 1 CO 近赤外線吸収から探る銀河中心 pc スケールでのガスの物理状態 : あかりと Spitzer による低分散分光観測 馬場俊介 ( 東大,ISAS/JAXA) 中川貴雄, 磯部直樹 (ISAS/JAXA), 白旗麻衣 ( 国立天文台 ) ALMAワークショップ AGN 銀河質量降着
More informationLuminous Infrared Galaxies
Luminous Infrared Galaxies FIRSED April 3, 2013 The Great Observatories All-sky LIRG Survey (GOALS) IRAS-detected galaxies with f 60μm > 5.24 Jy & b > 5 o 201 galaxies with L IR 10 11.0 L HST, Chandra
More informationBenjamin Weiner Steward Observatory November 15, 2009 Research Interests
Benjamin Weiner Steward Observatory November 15, 2009 Research Interests My recent research projects study galaxy evolution with emphasis on star formation histories, gas accretion and outflow, and galaxy
More information