AC Fabian, M. Cappi, J Sanders. Cosmic Feedback from AGN
|
|
- Lorin Hines
- 5 years ago
- Views:
Transcription
1 AC Fabian, M. Cappi, J Sanders Cosmic Feedback from AGN
2 AC Fabian, M Cappi, J Sanders, S Heinz, E Churazov, B McNamara, J Croston, D Worrall, F Humphrey, F Tombesi, J Reeves, M Giustini, P O Brien, T Reiprich P Nulsen, T Ponman, N Werner, W Forman, A Young, N Brandt, G Chartas
3 Possible effect of central black hole on host galaxy E BlackHole 30 E Galaxy Energy released by growth of Black Hole Gravitational Binding Energy of Host Galaxy 2 major modes for the interaction: Kinetic (radio/jet) and Radiative (quasar)
4 KEY QUESTIONS 1) Understanding the energy flow in cool cores of clusters, groups and ellipticals: (Velocity field, bulk motions, shocks, turbulence ) 2) Understanding the energy and mass flow of AGN outflows: (Mass and energy components, velocity structure, variability, ionization structure ) X-rays are most direct probe of crucial volume-filling component
5 Cool Cores in Clusters X-ray brightest region in Clusters and Groups, with size ~100 kpc Radius of XMS FOV ~ 130 kpc at z~0.1, which is well matched to cool cores Need to map flows (velocities and line widths), Line strengths, metallicities etc Athena XMS offers order of magnitude (or more) improvement over ASTRO-H on spatial resolution and counts, and 2 on spectral resolution.
6 Chandra 1.4 Ms
7
8
9 M84 Hydra A
10 Perseus Athena XMS simulation FoV ~ counts per pixel in brightest region in 50ks observation Most of the structures are resolved with 10 PSF and much better than XMM 5 PSF is desirable, but not required
11 Perseus - simulated spectrum From Fe-K only: 38 km/s broadening (34 km/s absolute) From Fe-L only: 24 km/s broadening (24 km/s absolute) Can use soft and hard bands independently
12
13 Perseus bubble scan 250 ks Cygnus A at FeK
14 Centaurus measuring radiative cooling & metals
15 Abell 1835 more distant cluster at z = 0.25 Abell 1835: luminous x erg/s Readout XMS FoV Athena PSF is much better than XMM for removing point sources Note: the Athena images are smoothed and rebinned Chandra images
16 Abell 1835 Sim-X simulation with background 50 ks SIM-X simulation with XMS showing ct/pixel Including finite exposure time and background ICM easily visible out to several hundred kpc
17 Abell 1835 broadening comparison XMM: 260 ks RGS observation of 30 arcsec strip Athena & ASTRO-H: 50 ks observations of 7 radius region (not resolved by ASTRO-H) Thermal broadening only assumed Almost 10x better than the larger XMM region in 1/5 of the exposure time 12 km/s absolute velocity accuracy (90% level)
18 Sanders+09 v turb <274 km/s
19 Abell 1835 limits on cooling To understand AGN feedback we need to measure the gas distribution as a function of temperature What fraction successfully cools, forming stars? RGS results from Sanders et al ks Athena 2 simulations Assumes 100 Msun/yr cooling below 2.7 kev and hot component from 7 arcsec radius region
20 Cool Core Summary Athena well matched for science Background unlikely to be an issue (note surface brightness independent of z for nearby objects) WFI will carry out general cluster study simultaneously Results should enable major advances to be made
21 Outflows from AGNs and their feedback impact on galaxies/groups/clusters: Most important is to: i) Do detailed modeling and probe the outflow dynamics in brightest AGNs (to constrain geometry and location, hence energetics); ii) Characterize the outflow properties (N w,, out ) in QSOs up to z=2. Where we stand now: Theory Proga and Kallman 2004
22 PDS456 z=0.184 Reeves+09 Suzaku Kinetic power ~ erg/s XMM 2001 in red
23 Chartas et al
24
25 Absorption spectroscopy with calorimeter resolution up to 8-10 kev will revolutionize the field First probes of absorption line profiles (P-Cygni?) Probe of flow dynamics on short time-scales F. Tombesi Important to probe the geometry and location of the outflow, and therefore the total mass outflow and the kinetic power associated to AGN feedback.
26 What s s next? POPULATION STUDIES Minimum 2-10 kev flux to constrain (N W, ) within (20%, 10%) in a 100 ks observation QUANTIFY AGN FEEDBACK UP TO z~2 Margherita Margherita Giustini - Ph.D. Giustini Thesis defense, 16/05/2011 Bologna 15/04/2011
27 What s s next? INDIVIDUAL DETAILED STUDIES The ATHENA view of a mini-bal QSO PN 5 ks XMS 5 ks UNVEIL THE DYNAMICS OF THE INNER ACCRETION/EJECTION FLOW Margherita Margherita Giustini - Ph.D. Giustini, Thesis defense, 16/05/2011 Bologna 15/04/2011
28 Superwinds
29
30 M82
31
32
33 20% of massive star formation at low z in starbursts Starburst/superwind galaxies account for most star formation at 2<z<4 ULIRGS have BALS and Superwind (Mdot~1000 Msun/yr, v~1000km/s) eg Mkn 231
34 Summary Athena will give crucial information on gas velocity, metallicity, ionization and emission measure for all forms of galaxy feedback X-rays are the only probe of volume-filling component
35
36
37 Strawman for Feedback science case vs A1/2/3 Nearby cool cores Sources <F 2-10keV > # <Exp.> (ks) Tot. Exp. (Ms) Doable? A1, A2, A3? clusters few 1e A1, A2, A3 Nearby groups groups few 1e A1, A2, A3 Bad Med Best Distant (z<0.3) cool cores clusters few 1e A1, A2, A3 Outflows (dynamics) Outflows (feedback) Sey/PGs/ RGs >1e A1, A2, A3 PGs/QSOs >1e A1, A2, A3 Total N.B: Already makes use of targets and observations needed for Strong Gravity Strawman
38 Where we stand now (after Chandra and XMM-Newton): ~20 well-studied sources t=4 years t=6 months t=3 days t=10 ks Strong spectral variability, complex and variable ionized absorbers
39 The FOM for AGN feedback is the absorption line sensitivity (EW=50 ev, 100 ks, 5sigma) XMS Athena3 is preferred for outflows dynamics Athena1 is preferred for cosmological feedback
40 A2 XMS A3 XMS XMM pn Astro-H
41 Centaurus - detailed soft spectra Astro-H limits are 0.55, 0.76 and 2 Msun/yr in 50 ks
42 Absorption spectroscopy with calorimeter resolution between 2-7 kev will allow to constrain absorbers in a sample of QSOs up to z=2 Flux limits to measure (N w, ) within (10%, 5%) in 100 ks obs. Important to probe AGN feedback up to z~2
Studying AGN winds and feedback with Athena. Massimo Cappi. INAF/IASF-Bologna. 4. Future
Studying AGN winds and feedback with Athena Massimo Cappi INAF/IASF-Bologna Outline 1. Athena in Cosmic Vision 2. Athena general Science Goals 3. Athena s possible contribution(s) to studies of AGN winds
More informationRELATIVISTIC SPECTROSCOPY OF BLACK HOLES
RELATIVISTIC SPECTROSCOPY OF BLACK HOLES Michael Parker ESAC science seminar 24/5/18 BLACK HOLES 101 For an object to just escape a massive body, it needs the sum: Kinetic energy + gravitational binding
More informationAGN feedback from accretion disk winds
AGN feedback from accretion disk winds Francesco Tombesi NASA Goddard Space Flight Center University of Maryland, College Park Collaborators: J. Reeves, M. Cappi, C. Reynolds, R. Mushotzky, S. Veilleux,
More informationFrancesco Tombesi. University of Rome, Tor Vergata NASA - Goddard Space Flight Center University of Maryland, College Park
Francesco Tombesi University of Rome, Tor Vergata NASA - Goddard Space Flight Center University of Maryland, College Park (credit JAXA s press release) Warm Absorbers (WAs) (Photo) ionized Mrk 509 v~300-800
More informationVariable X-ray absorption in the mini-bal QSO PG
Variable X-ray absorption in the mini-bal QSO PG 1126-041 Margherita Giustini Massimo Cappi, George Chartas, Mauro Dadina, Mike Eracleous, Gabriele Ponti, Daniel Proga, Francesco Tombesi, Cristian Vignali,
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 informationAstrophysics of feedback in local AGN and starbursts
Astrophysics of feedback in local AGN and starbursts A personal view Gabriele Ponti co-chair of swg 2.3 Max Planck Institute for Extraterrestrial Physics (Garching) Outline 1) Why is feedback required?
More informationarxiv:astro-ph/ v1 6 May 2004
XMM-NEWTON OBSERVATIONS OF THREE HIGH REDSHIFT RADIO GALAXIES arxiv:astro-ph/0405116 v1 6 May 2004 Abstract E. Belsole, D.M. Worrall, M. J. Hardcastle Department of Physics - University of Bristol Tyndall
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 Powerful Black Hole Wind in the Luminous Quasar PDS 456
The Powerful Black Hole Wind in the Luminous Quasar PDS 456 James Reeves Astrophysics Group, Keele University & UMBC in collaboration with: E. Nardini (Keele), J. Gofford (Keele/UMBC) - M. Costa, G. Matzeu
More informationv Characteristics v Possible Interpretations L X = erg s -1
Ultra Luminous X-ray sources v Characteristics L X = 39-41 erg s -1 >> M black hole(bh) L Edd = 39 erg s -1. Usually seen in star forming regions. On arms of spiral galaxies (right). In starburst or irregular
More informationMassive molecular gas flows and AGN feedback in galaxy clusters
Massive molecular gas flows and AGN feedback in galaxy clusters CO(3-2) Helen Russell (Cambridge) Brian McNamara (Waterloo), Andy Fabian (Cambridge), Paul Nulsen (CfA), Michael McDonald (MIT), Alastair
More informationX- ray surface brightness fluctuations and turbulence in galaxy clusters. Jeremy Sanders. Andy Fabian. Sanders & Fabian 2011, MNRAS, submitted
X- ray surface brightness fluctuations and turbulence in galaxy clusters Jeremy Sanders Andy Fabian Sanders & Fabian 2011, MNRAS, submitted Simulations predict that in galaxy clusters turbulent energy
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 informationDriving hot and cold gas flows with AGN feedback in galaxy clusters Credit: ESO
Driving hot and cold gas flows with AGN feedback in galaxy clusters Credit: ESO Helen Russell (Cambridge) Brian McNamara (Waterloo), Andy Fabian (Cambridge), Paul Nulsen (CfA), Michael McDonald (MIT),
More informationNew generation X-ray telescope
New generation X-ray telescope Your image Agata Różańska CAMK PAN, Warsaw 38 Zjazd PTA, Kraków, Atmosphere is not transparent to X-rays Kraków, 38 Zjazd PTA, Zielona Góra ATHENA L2 mission of ESA Cosmic
More informationClusters of galaxies and the large scale structure of the universe. Gastão B. Lima Neto IAG/USP
Clusters of galaxies and the large scale structure of the universe Gastão B. Lima Neto IAG/USP IWARA, Maresias 10/2009 Our story begins... William Herschel recognizes the clustering of nebulae and their
More informationNuclear X-ray Emission and Mass Outflow From Broad Lined Radio Galaxies (Lorentz Center, Leiden 2009)
Nuclear X-ray Emission and Mass Outflow From Broad Lined Radio Galaxies (Lorentz Center, Leiden 2009) James Reeves (Keele Univ, UK) Collaborators:- Rita Sambruna (NASA/GSFC), Francesco Tombesi (NASA/GSFC
More informationThe Jet/ISM Interaction in Three Nearby Radio Galaxies as seen with Chandra
The Jet/ISM Interaction in Three Nearby Radio Galaxies as seen with Chandra R. P. Kraft, W. R. Forman, E. Churazov, J. Eilek, M. J. Hardcastle, S. Heinz, C. Jones, M. Markevitch, S. S. Murray, P. A. J.
More informationSupernova Remnant Science with AXIS. Brian Williams & Hiroya Yamaguchi
Supernova Remnant Science with AXIS Brian Williams & Hiroya Yamaguchi Big Picture Questions - How do supernovae dictate the life cycle of elements in the ISM? - What are the progenitors of the various
More informationBroad X-ray Absorption lines from the Wind in PDS 456
Broad X-ray Absorption lines from the Wind in PDS 456 James Reeves (UMBC & Keele), Emanuele Nardini, Valentina Braito (Brera & UMBC), Francesco Tombesi (GSFC), Paul O Brien (Leicester), Jane Turner (UMBC),
More informationRadio AGN feedback on galaxy scales: What can Athena show us?
Radio AGN feedback on galaxy scales: What can Athena show us? Beatriz Mingo 1st Athena Scientific Conference ESAC, 2015 University of Leicester Collaborators: Mike Watson (Leicester) Martin Hardcastle
More informationSnowballs in hell! X-ray galactic coronae in galaxy! clusters and the need for sub-arcsecond resolution! Simona Giacintucci (NRL)!
Snowballs in hell X-ray galactic coronae in galaxy clusters and the need for sub-arcsecond resolution Simona Giacintucci (NRL) M. Markevitch (GSFC), T. Clarke (NRL), E. Richards (NRC-NRL) X-ray Skies with
More informationA new fast wind in a star forming galaxy
A new fast wind in a star forming galaxy V. Braito J. Reeves, G. Matzeu, E. Nardini, M. Costa, A. Lobban, F. Tombesi L. Ballo, R. Della Ceca, P. Severgnini, J. Turner PDS456: the prototype of the UFOs
More informationNuStar has similar area kev, Astro-H better at E> 80 Kev
NuStar has similar area 20-80 kev, Astro-H better at E> 80 Kev 10 3 1 HXI Effective Area [cm 2 ] 10 2 10 1 5 10 30 80 Energy [kev] NuStar and Astro-H HXI should have similar FOV HXI becomes background
More informationFuture X-rayX Spectroscopy Missions. Jan-Willem den Herder
Future X-rayX Spectroscopy Missions Jan-Willem den Herder contents Plasma diagnostics in the 0.1 to 10 kev band with resolution > 100 X-ray spectrometers: instrumental promises Future missions (a dream)
More informationProbing variable iron emission and absorption lines in AGNs with XEUS. Massimo Cappi. IASF-Bologna
Probing variable iron emission and absorption lines in AGNs with XEUS Massimo Cappi INAF/IASF-Bologna IASF-Bologna Outline 1. Evidence for (redshifted) relativistic Fe emission lines 2. Evidence for VARIABLE
More informationAGN Feedback in the Hot Halo of NGC 4649
AGN Feedback in the Hot Halo of NGC 4649 A. Paggi1 G. Fabbiano1, D.-W. Kim1, S. Pellegrini2, F. Civano3, J. Strader4 and B. Luo5 Harvard-Smithsonian Center for Astrophysics; 2Department of Astronomy, University
More informationarxiv: v1 [astro-ph] 18 Dec 2007
Mem. S.A.It. Vol. 75, 282 c SAIt 2004 Memorie della ÇÙØ ÓÛ Ò Û Ò Ò Æ ÓÖ Ë Ñ Óй M. Cappi 1, F. Tombesi 1,2, and M. Giustini 1,2 arxiv:0712.2977v1 [astro-ph] 18 Dec 2007 1 INAF-IASF, Bologna, Via Gobetti
More informationSurveys for high-redshift (z>6) AGN with AXIS (cf. Athena) James Aird. University of Cambridge (-> University of Leicester)
Surveys for high-redshift (z>6) AGN with AXIS (cf. Athena) James Aird University of Cambridge (-> University of Leicester) SMBH seed formation mechanisms Pop III star remnants MBH ~ 100 M z~20-30 Direct
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 informationSoft X-ray Emission Lines in Active Galactic Nuclei. Mat Page
Soft X-ray Emission Lines in Active Galactic Nuclei Mat Page MSSL-UCL Observations of soft X-ray line emission allow us to investigate highly ionized plasmas in galaxies and AGN. I ll start with the most
More informationarxiv: v1 [astro-ph.co] 16 Dec 2011
**Volume Title** ASP Conference Series, Vol. **Volume Number** **Author** c **Copyright Year** Astronomical Society of the Pacific arxiv:1112.3750v1 [astro-ph.co] 16 Dec 2011 Variable X-ray absorption
More informationFeedback from growth of supermassive black holes
Research Collection Other Conference Item Feedback from growth of supermassive black holes Author(s): Begelman, Mitchell C.; Ruszkowksi, Mateusz Publication Date: 2003 Permanent Link: https://doi.org/10.3929/ethz-a-004585094
More informationMolecular gas & AGN feedback in brightest cluster galaxies
Molecular gas & AGN feedback in brightest cluster galaxies Helen Russell Brian McNamara Alastair Edge Robert Main Adrian Vantyghem Francoise Combes Andy Fabian Philippe Salomé Outline Introduction Radiative
More informationEnrico Fermi School Varenna Cool Cores and Mergers in Clusters Lecture 3
Enrico Fermi School Varenna Cool Cores and Mergers in Clusters Lecture 3 Craig Sarazin Dept. of Astronomy University of Virginia A85 Chandra (X-ray) Cluster Merger Simulation Cool Cores in Clusters Central
More informationGalaxy groups: X-ray scaling relations, cool cores and radio AGN
Galaxy groups: X-ray scaling relations, cool cores and radio AGN Ming Sun (UVA) (M. Voit, W. Forman, P. Nulsen, M. Donahue, C. Jones, A. Vikhlinin, C. Sarazin ) Outline: 1) Scaling relations and baryon
More informationNew Suzaku Results on Active Galaxies. or Reflections on AGN. James Reeves (Keele) and Suzaku team (given by Lance Miller)
New Suzaku Results on Active Galaxies or Reflections on AGN James Reeves (Keele) and Suzaku team (given by Lance Miller) Overview Overview of Suzaku and instrument performance. Why Suzaku is important
More informationFeedback in Galaxy Clusters
Feedback in Galaxy Clusters Brian Morsony University of Maryland 1 Not talking about Galaxy-scale feedback Local accretion disk feedback 2 Outline Galaxy cluster properties Cooling flows the need for feedback
More informationEmbedded Spiral Patterns in the massive galaxy cluster Abell 1835
2017/06/08 X-ray Universe @ Rome Embedded Spiral Patterns in the massive galaxy cluster Abell 1835 Shutaro Ueda (ISAS/JAXA), Tetsu Kitayama (Toho University), Tadayasu Dotani (ISAS/JAXA, SOKENDAI) This
More informationX-ray spectroscopy of nearby galactic nuclear regions
X-ray spectroscopy of nearby galactic nuclear regions 1. How intermittent are AGNs? 2. What about the silent majority of the SMBHs? 3. How do SMBHs interplay with their environments? Q. Daniel Wang University
More informationA Shock Model for the the Outburst from the Supermassive Black Hole in M87 Bill Forman - SAO/CfA
M87 A Shock Model for the the Outburst from the Supermassive Black Hole in M87 Bill Forman - SAO/CfA interactions galore; stripping at work, M87 outburst Low Eddington ratio accretion (like other normal
More informationTurbulent Heating in the X-ray Brightest Galaxy Clusters
Turbulent Heating in the X-ray Brightest Galaxy Clusters Irina Zhuravleva KIPAC, Stanford University E. Churazov, A. Schekochihin, S. Allen, P. Arevalo, A. Fabian, W. Forman, M. Gaspari, E. Lau, D. Nagai,
More informationDan Evans (Harvard), Julia Lee (Harvard), Jane Turner (UMBC/GSFC), Kim Weaver (GSFC), Herman Marshall (MIT) NGC 2110 Spectroscopy
Dan Evans (Harvard), Julia Lee (Harvard), Jane Turner (UMBC/GSFC), Kim Weaver (GSFC), Herman Marshall (MIT) Fe Kα Lines and Reflection: AGN Geometry The Fe Kα line complex in general consists of a narrow
More informationWhere are the missing baryons? Craig Hogan SLAC Summer Institute 2007
Where are the missing baryons? Craig Hogan SLAC Summer Institute 2007 Reasons to care Concordance of many measures of baryon number (BBN, CMB,.) Evolution of our personal baryons (galaxies, stars, planets,
More informationThe perspective of X-ray galaxy clusters with the XIFU/Athena instrument
The perspective of X-ray galaxy clusters with the XIFU/Athena instrument Nicolas Clerc IRAP Toulouse, France AtomDB workshop 17, Athens, GA November 3rd 17 Clusters of galaxies ; large-scale structure
More informationSHAPING GALAXIES WITH BLACK HOLE FEEDBACK
MARTIN BOURNE DEBORA SIJACKI, MIKE CURTIS, SERGEI NAYAKSHIN, ALEX HOBBS & KASTYTIS ZUBOVAS SHAPING GALAXIES WITH BLACK HOLE FEEDBACK CONSTRAINING FEEDBACK MODELS SCALING RELATIONS LARGE SCALE OUTFLOWS
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 informationPhysics of the hot evolving Universe
Physics of the hot evolving Universe Science themes for a New-Generation X-ray Telescope Günther Hasinger Max-Planck-Institut für extraterrestrische Physik Garching ESA Cosmic Vision 2015-2025 Workshop,
More informationChandra discovery of the intracluster medium around UM425 at redshift 1.47
Chandra discovery of the intracluster medium around UM425 at redshift 1.47 Smita Mathur and Rik J. Williams Astronomy Department, The Ohio State University, 140 West 18th Avenue, Columbus OH 43220 ABSTRACT
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 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 informationGalaxy Clusters: Cosmic High-Energy Laboratories to Study the Structure of Our Universe
Galaxy Clusters: Cosmic High-Energy Laboratories to Study the Structure of Our Universe Hans Böhringer Max-Planck-Institut für Extraterrestrische Physik, D-85748 Garching, Germany Abstract. This contribution
More informationPart 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 informationA Multi-wavelength View of the Archetypal CSS Radio Galaxy 3C303.1: Evidence for Shocks and Induced Star Formation
A Multi-wavelength View of the Archetypal CSS Radio Galaxy 3C303.1: Evidence for Shocks and Induced Star Formation Chris O Dea (Rochester Institute of Technology) HST Spectroscopy: Alvaro Labiano, Wim
More informationTHE INVERSE-COMPTON X-RAY SIGNATURE OF AGN FEEDBACK
THE INVERSE-COMPTON X-RAY SIGNATURE OF AGN FEEDBACK MARTIN BOURNE IN COLLABORATION WITH: SERGEI NAYAKSHIN WITH THANKS TO: ANDREW KING, KEN POUNDS, SERGEY SAZONOV AND KASTYTIS ZUBOVAS Black hole (g)astronomy
More informationSOFT X-RAY LAGS AND THE CORRELATION WITH BH MASS IN RADIO QUIET AGN
SOFT X-RAY LAGS AND THE CORRELATION WITH BH MASS IN RADIO QUIET AGN flux time Barbara De Marco (Centro de Astrobiología, CSIC-INTA) Collaborators: G. Ponti, P. Uttley, M. Cappi, G. Miniutti, M. Dadina,
More informationThe Hot and Energetic Universe
The Hot and Energetic Universe An Athena+ supporting paper Astrophysics of feedback in local AGN Authors and contributors M. Cappi, C. Done, E. Behar, S. Bianchi, V. Braito, E. Costantini, M. Dadina, C.
More informationScientific cases for Simbol-X of interest of the Italian community
Scientific cases for Simbol-X of interest of the Italian community Based on the High Energy Astrophysics study: Fields of interest and perspective for the national community ASI 2003-2004 Fabrizio Fiore
More informationResolving the Space-Time Around Black Holes
Resolving the Space-Time Around Black Holes Kendrah Murphy & Tahir Yaqoob Johns Hopkins University Image from Dovciak et al. (2004) Introduction Black holes are defined by their mass, charge, and angular
More informationProbing the Outskirts of Strongly Merging Double Clusters
Probing the Outskirts of Strongly Merging Double Clusters S. W. Randall - CfA E. Bulbul, R. Paterno-Mahler, C. Jones, W. Forman, E. Miller, S. Murray, C. Sarazin, E. Blanton Probing the Outskirts of Strongly
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 informationGalaxy Clusters with XEUS. Silvano Molendi Stefano Borgani Stefano Ettori
Galaxy Clusters with XEUS Silvano Molendi Stefano Borgani Stefano Ettori Cosmic Vision Under the Cosmic Vision theme "The Universe taking shape" Investigation of galaxy clusters is declared to be amongst
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 informationTransient iron fluorescence: new clues on the AGN disk/corona?
Transient iron fluorescence: new clues on the AGN disk/corona? Emanuele Nardini Horizon 2020 INAF/Arcetri AstroFIt2/MSCA in collaboration with: D. Porquet (CNRS/Strasbourg), J. Reeves (Keele+UMBC), V.
More informationUltra-fast disk wind from a high accretion rate black hole 1H
Ultra-fast disk wind from a high accretion rate black hole 1H 0707-495 Kouichi Hagino (ISAS/JAXA) H. Odaka, C. Done, R. Tomaru, S. Watanabe, T. Takahashi K. Hagino et al. 2016, MNRAS, 461, 3954 BREAKING
More informationX-Ray observability of WHIM and our new mission concept DIOS Intergalactic. Oxygen. Surveyor ) Noriko Yamasaki ISAS/JAXA
X-Ray observability of WHIM and our new mission concept DIOS (Diffuse Intergalactic Oxygen Surveyor ) Noriko Yamasaki ISAS/JAXA 1 Cosmic Baryon Budget requires missing baryon The observed baryons are only
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 informationDark Energy: Measuring the Invisible with X-Ray Telescopes
Black holes, Galactic Dark Center Matter and Galactic Center Dark Energy: Measuring the Invisible with X-Ray Telescopes Christine Jones Before 1930 -- only optical observations of the sky Intro Before
More informationX-ray Jets with AXIS
X-ray Jets with AXIS AGN jets may contribute to feedback in massive systems from z>6 to z=0, but we do not know How jets are formed What jets are made of Where jets deposit their energy When jets are active
More informationClusters of Galaxies " High Energy Objects - most of the baryons are in a hot (kt~ k) gas." The x-ray luminosity is ergs/sec"
Clusters of Galaxies! Ch 4 Longair Clusters of galaxies are the largest gravitationally bound systems in the Universe. At optical wavelengths they appear as over-densities of galaxies with respect to the
More informationProbing the Detailed Physics of Hot Baryons with Lynx: Predictions from Mock Observations. John ZuHone
Probing the Detailed Physics of Hot Baryons with Lynx: Predictions from Mock Observations Chandra John ZuHone Lynx Probing the Physics of Hot Baryons We need all three of Lynx s killer features for this
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 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 informationWhere are oxygen synthesized in stars?
The oxygen abundance from X-rays : methods and prospects K. Matsushita Where are oxygen synthesized in stars? Hot intracluster medium (ICM) Warm-hot intergalactic medium? Hot interstellar medium in early-type
More informationAGN Selec)on Techniques. Kris)n Kulas Astro 278 Winter 2012
AGN Selec)on Techniques Kris)n Kulas Astro 278 Winter 2012 Selec)on Techniques Op)cal X- ray Radio Infrared Variability X- ray and Radio Physical Processes Detec)on of Sources Benefit of Wavelength Regime
More informationGasflows in Galaxy Clusters
Gasflows in Galaxy Clusters Brian McNamara University of Waterloo Perimeter Ins7tute for Theore7cal Physics, Canada H. Russell, C.J. Ma, A. Vantyghem, C. Kirkpatrick, R. Main P. Nulsen, A. Edge, A., Fabian,
More informationAstro2020 Science White Paper A Unification of the Micro and Macro Physics in the Intracluster Medium of Nearby Clusters
Astro2020 Science White Paper A Unification of the Micro and Macro Physics in the Intracluster Medium of Nearby Clusters arxiv:1904.06739v1 [astro-ph.he] 14 Apr 2019 Thematic Areas: Planetary Systems Star
More informationAnalysis of Off-Nuclear X-Ray Sources in Galaxy NGC Sarah M. Harrison
SLAC-TN-6-19 August 26 Analysis of Off-Nuclear X-Ray Sources in Galaxy NGC 4945 Sarah M. Harrison Office of Science, Science Undergraduate Laboratory Internship (SULI) Massachusetts Institute of Technology
More informationX-raying High-Redshift AGNs and the First Black Holes: From Chandra to Lynx
X-raying High-Redshift AGNs and the First Black Holes: From Chandra to Lynx Niel Brandt, Fabio Vito, the Chandra Deep Fields Team, and the Lynx First Accretion Light Working Group Some Relevant Results
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 informationAthena Athena+ Towards a European Large X-ray Observatory. Mike Watson University of Leicester. Athena+
Athena Towards a European Large X-ray Observatory Mike Watson University of Leicester Topics Brief history and context New ESA approach to L-class selection The concept Credits: Athena & teams The road
More informationAdvanced Telescope for High Energy Astrophysics
Advanced Telescope for High Energy Astrophysics Etienne Pointecouteau IRAP (Toulouse, France) Member of the Athena Collaboration and of the X-IFU Science Team Why does the observable universe look the
More informationMASS PROFILES OF X-RAY BRIGHT RELAXED GROUPS: METHODS AND SYSTEMATICS
MASS PROFILES OF X-RAY BRIGHT RELAXED GROUPS: METHODS AND SYSTEMATICS FABIO GASTALDELLO IASF-INAF MILANO & UC IRVINE D. BUOTE UCI P. HUMPHREY UCI L. ZAPPACOSTA TRIESTE J. BULLOCK UCI W. MATHEWS UCSC F.
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 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 informationTrends in Intracluster Metallicity
Trends in Intracluster Metallicity The Right Answer ICM metallicity is ~0.3 solar with a negative gradient within ~0.15 R180, as measured from Fe K lines M Fe M gas 4 10 4 Leccardi & Molendi (2008) (For
More informationA Suzaku, NuSTAR, and XMM-Newton view on variable absorption and relativistic reflection in NGC 4151
A Suzaku, NuSTAR, and XMM-Newton view on variable absorption and relativistic reflection in NGC 411 T. Beuchert, A.G. Markowitz, T. Dauser, J.A. García, M.L. Keck, J. Wilms, M. Kadler, L.W. Brenneman,
More informationATHENA Mission Design and ESA Status. David Lumb ESA Study Scientist MPE Jan 13 th 2012
ATHENA Mission Design and ESA Status David Lumb ESA Study Scientist MPE Jan 13 th 2012 Topics covered ESA L class mission reformulation Current status & programmatics Athena Mission Design Spacecraft Optics
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 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 informationActive 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 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 informationBlack Hole Accretion and Wind
Black Hole Accretion and Wind Feng Yuan Shanghai Astronomical Observatory, Chinese Academy of Sciences Accretion Regimes Hyper-accretion, slim disk, ADAF (Abramowicz et al. 1988) TDEs, ULXs, SS433 Thin
More informationThe Hot and Energetic Universe
The Hot and Energetic Universe An Athena+ supporting paper Understanding the build-up of supermassive black holes and galaxies at the heyday of the Universe Authors and contributors A. Georgakakis, F.
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 informationNew Forms of Convection in Galaxy Cluster Plasmas (i.e., how do galaxy clusters boil?)
New Forms of Convection in Galaxy Cluster Plasmas (i.e., how do galaxy clusters boil?) Eliot Quataert (UC Berkeley) Hydra A w/ Chandra in collaboration with Ian Parrish Prateek Sharma Overview Hot Plasma
More informationThe quest for Type 2 quasars: What are the X-ray observations of optically selected QSOs2 telling us?
The quest for Type 2 quasars: What are the X-ray observations of optically selected QSOs2 telling us? Cristian Vignali Dipartimento di Astronomia, Universita`degli Studi di Bologna In collaboration with
More informationarxiv:astro-ph/ v1 5 Dec 1996
To appear in Proceedings of the Workshop on High Throughput X-ray Spectroscopy, ed. by P. Sullivan & H. Tananbaum (Cambridge: Smithsonian Astrophysical Observatory), in press. High Resolution X-ray Spectra
More informationThe Radio/X-ray Interaction in Abell 2029
The Radio/X-ray Interaction in Abell 2029 Tracy Clarke (Univ. of Virginia) Collaborators: Craig Sarazin (UVa), Elizabeth Blanton (UVa) Abell 2029: Background z = 0.0767, D=320 Mpc, scale = 1.44 kpc/ typically
More information