AGN in Clusters of Galaxies Paul Martini The Ohio State University J.S. Mulchaey, D.D. Kelson (OCIW) E. Kim (CfA), A. Athey (OCIW)

Slides:

Advertisements

Similar presentations

Star formation histories and environment Bianca M. Poggianti INAF – Osservatorio Astronomico di Padova WE ARE ALL AFTER THE BIG PICTURE: 1)To what extent,

Advertisements

Migration of Nearby Spirals Tom Hughes AGN feedback or Environmental effects? Supervisors: Luca Cortese, Jonathan Davies astro-ph:

Low-frequency radio maps for the REXCESS cluster sample S.R. Heidenreich, University of Southampton In collaboration with J.H. Croston, University of Southampton;

Luminous Infrared Galaxies with the Submillimeter Array: Probing the Extremes of Star Formation Chris Wilson (McMaster), Glen Petitpas, Alison Peck, Melanie.

Observations of the evolution of HI in galaxies across different environments. D.J. Pisano (West Virginia University)

Unresolved X-Ray Sources in Intermediate Redshift Cluster Fields Unresolved X-Ray Sources in Intermediate Redshift Cluster Fields S. Fawcett, A. Hicks,

Kelley Liebst AST 591 School of Earth and Space Exploration Arizona State University.

HI Gas as Function of Environment When and where do galaxies stop accreting cool gas? How do they loose the cool gas? When do they stop forming stars?

Chania, Crete, August 2004 “The environment of galaxies” Pierre-Alain Duc Recycling in the galaxy environment F. Bournaud J. Braine U. Lisenfeld P. Amram.

24-28 October 2005 Elena Belsole University of Bristol Distant clusters of Galaxies Ringberg Workshop X-ray constraints on cluster-scale emission around.

Life Before the Fall: Group Galaxy Evolution Prior to Cluster Assembly Anthony Gonzalez (Florida) Kim-Vy Tran (CfA) Michelle Conbere (Florida) Dennis Zaritsky.

Ben Maughan (CfA)Chandra Fellows Symposium 2006 The cluster scaling relations observed by Chandra C. Jones, W. Forman, L. Van Speybroeck.

Studying the mass assembly and luminosity gap in fossil groups of galaxies from the Millennium Simulation Ali Dariush, University of Birmingham Studying.

Lensing of supernovae by galaxies and galaxy clusters Edvard Mörtsell, Stockholm Jakob Jönsson, Oxford Ariel Goobar; Teresa Riehm, Stockholm.

Galaxy Groups in HICAT Jamie Stevens. Outline Introduction Group-finding in HICAT HIPASS group properties Star formation properties Summary.

Dark Halos of Fossil Groups and Clusters Observations and Simulations Ali Dariush, Trevor Ponman Graham Smith University of Birmingham, UK Frazer Pearce.

The Regulation of Star Formation by AGN Feedback D AVID R AFFERTY (Penn State / Ohio U.) Collaborators: Brian McNamara (Waterloo) and Paul Nulsen (CfA)

Evolution of Luminous Galaxy Pairs out to z=1.2 in the HST/ACS COSMOS Field Jeyhan Kartaltepe, IfA, Hawaii Dave Sanders, IfA, Hawaii Nick Scoville, Caltech.

The Origins and Ionization Mechanisms of Warm Filaments in Cool Core Clusters Michael McDonald Postdoctoral Associate - MIT Kavli Institute In collaboration.

Weak-Lensing selected, X-ray confirmed Clusters and the AGN closest to them Dara Norman NOAO/CTIO 2006 November 6-8 Boston Collaborators: Deep Lens Survey.

AGN and Quasar Clustering at z= : Results from the DEEP2 + AEGIS Surveys Alison Coil Hubble Fellow University of Arizona Chandra Science Workshop.

The Distribution of Baryons in Galaxy Clusters and Groups Anthony Gonzalez University of Florida Dennis Zaritsky, Ann Zabludoff University of Arizona Ohio.

The spatial clustering of X-ray selected AGN R. Gilli Istituto Nazionale di Astrofisica (INAF) Osservatorio Astronomico di Bologna On behalf of the CDFS.

Magnetic Jets and Lobes in Cosmological MHD Hui Li Los Alamos National Laboratory NSF/DOE Center for Magnetic Self-Organization (CMSO) Collaborators: H.

A Primer on SZ Surveys Gil Holder Institute for Advanced Study.

Extended Radio Sources in Clusters of Galaxies Elizabeth Blanton University of Virginia.

Radio Sources in High-Redshift Galaxy Clusters: An Initial Look Megan Roscioli University of Chicago In collaboration with Mike Gladders, U. Chicago RCS-1,2.

Galaxy Clusters Perseus Cluster in X-rays. Why study clusters? Clusters are the largest virialized objects in the Universe. Cosmology: tail of density.

Luminosity & color of galaxies in clusters sarah m. hansen university of chicago with erin s. sheldon (nyu) risa h. wechsler (stanford)

The Evolution of X-ray Luminous Groups Tesla Jeltema Carnegie Observatories J. Mulchaey, L. Lubin, C. Fassnacht, P. Rosati, and H. Böhringer.

MODELING INTRACLUSTER MEDIUM AND DARK MATTER IN GALAXY CLUSTERS Elena Rasia Dipartimento di Astronomia Università di Padova Padova, April 9th, 2002.

8th Sino-German Workshop Kunming, Feb 23-28, 2009 Milky Way vs. M31: a Tale of Two Disks Jinliang HOU In collaboration with : Ruixiang CHANG, Shiyin SHEN,

Galactic Metamorphoses: Role of Structure Christopher J. Conselice.

How to start an AGN: the role of host galaxy environment Rachel Gilmour (ESO Chile & IfA, Edinburgh) Philip Best (Edinburgh), Omar Almaini & Meghan Gray.

The Evolution of Quasars and Massive Black Holes “Quasar Hosts and the Black Hole-Spheroid Connection”: Dunlop 2004 “The Evolution of Quasars”: Osmer 2004.

Wide Field Imagers in Space and the Cluster Forbidden Zone Megan Donahue Space Telescope Science Institute Acknowledgements to: Greg Aldering (LBL) and.

Coevolution of black holes and galaxies at high redshift David M Alexander (Durham)

Unravelling the formation and evolutionary histories of the most massive galaxies Ilani Loubser (Univ. of the Western Cape)

The Environments of Galaxies: from Kiloparsecs to Megaparsecs August 2004 Cool Cores in Galaxy Groups Ewan O’Sullivan Harvard-Smithsonian Center for Astrophysics.

Accretion in Early-Type Galaxies Haiguang Xu Department of Physics Shanghai Jiao Tong University

Dwarf LSB galaxies in the Virgo cluster Jonathan Davies.

Search for new Luminous Blue Variables (1) (Kniazev: RSA_OTH RSA_OTH-014) Vasilii Gvaramadze (SAI MSU) & Alexei Kniazev.

ORELSE in the Radio : AGN and Starbursts in High-Redshift Structures The Observations of Redshift Evolution in Large Scale Environments Survey Lori Lubin.

Constraining cluster abundances using weak lensing Håkon Dahle Institute of Theoretical Astrophysics, University of Oslo.

Hot gas in galaxy pairs Olga Melnyk. It is known that the dark matter is concentrated in individual haloes of galaxies and is located in the volume of.

Galactic Astronomy 銀河物理学特論 I Lecture 1-5: Dependence of Galaxy Properties on Environment Seminar: Park et al. 2007, ApJ, 658, 898 Lecture: 2011/11/07.

Galaxy Growth: The role of environment Simone Weinmann (MPA Garching) Collaborators: Guinevere Kauffmann, Frank van den Bosch, Anna Pasquali, Dan McIntosh,

Galaxy Wakes – Theory & Observations Irini Sakelliou University of Birmingham D.M. Acreman, T.J. Ponman, I.R. Stevens University of Birmingham M.R. Merrifield.

The coordinated growth of stars, haloes and large-scale structure since z=1 Michael Balogh Department of Physics and Astronomy University of Waterloo.

The Evolution of AGN Obscuration

The Environmental Effect on the UV Color-Magnitude Relation of Early-type Galaxies Hwihyun Kim Journal Club 10/24/2008 Schawinski et al. 2007, ApJS 173,

MMT Science Symposium1 “false-color” keV X-ray image of the Bootes field Thousands of AGNs in the 9.3 square degree Bootes field * X-ray and infrared.

The effects of the complex mass distribution of clusters on weak lensing cluster surveys Zuhui Fan Dept. of Astronomy, Peking University.

Baryon content of galaxy groups Ming Sun (University of Virginia) ‏ M. Voit, M. Donahue (MSU) A. Vikhlinin, W. Forman, C. Jones (CfA) N. Sehgal (KIPAC)

AMUSE-Virgo AGN MUlti-wavelength Survey in Early type galaxies Black Hole Accretion in the Nearby Universe: Evidence for Down-Sizing Elena Gallo | MIT.

MNRAS, submitted. Galaxy evolution Evolution in global properties reasonably well established What drives this evolution? How does it depend on environment?

The GEMS Project and Collapsed Groups Duncan Forbes Swinburne University.

ICM-ISM Stripping in Virgo Cluster Spiral Galaxies Jeff Kenney (Yale University) with: J. Van Gorkom B. Vollmer H. Crowl * A. Abramson A. Chung J. Cortes.

CLUSTERS OF GALAXIES The Physics of the IGM: Cooling Flows.

Recent Progress in Understanding X-ray Emission From Early-type Galaxies: The Hot Gas Component Jimmy A. Irwin University of Michigan X-rays From Nearby.

Robust identification of distant Compton-thick AGNs IR AGN Optical AGN Need for deep optical-mid-IR spectroscopy: multiple lines of evidence for intrinsic.

X-ray Scaling Relations of Early Type Galaxies Dong-Woo Kim Harvard-Smithsonian Center for Astrophysics (X-ray View of Galaxy Ecosystems Boston in July.

Probing the Dynamics of Galaxy-Gas Interactions in Groups and Clusters with Chandra and XMM-Newton Marie Machacek Smithsonian Astrophysical Observatory.

Interpreting the relationship between galaxy luminosity, color, and environment. Andreas Berlind (NYU, CCPP) SPH predictions: Michael Blanton (NYU) David.

The GOOD NICMOS Survey (GNS): Observing Massive Galaxies at z > 2 Christopher J. Conselice (University of Nottingham) with Asa Bluck, Ruth Gruethbacher,

The formation and dynamical state of the brightest cluster galaxies

Merging Galaxy Cluster Abell 2255 in Mid-Infrared

The X-ray Evolution of Young Post-Merger

The AGN Butcher-Oemler Effect

Rubén Sánchez-Janssen (IAC) J.Alfonso L. Aguerri Casiana Muñoz-Tuñón

Presentation transcript:

AGN in Clusters of Galaxies Paul Martini The Ohio State University J.S. Mulchaey, D.D. Kelson (OCIW) E. Kim (CfA), A. Athey (OCIW)

Why Survey Clusters for AGN? 1. Different environment to probe AGN fueling (mergers, interactions, role of ISM) 2. Catalysts for galaxy evolution (ram pressure stripping, starvation, etc.) 3. Feedback of AGN on galaxy ISM and cluster ICM 4. Source of systematic error for X-ray (and SZ) cluster cosmology surveys 5. Large population of optically-dull AGN, much higher surface density than blank fields Images from Sun et al. (2005); McNamara et al. (2006); Martini et al. (2002) Why is this a MISST?

AGN Identification 35 (of 40) X-ray sources are AGN (10x or more X-ray luminous than either LMXBs or hot, gaseous halos) All but 4/35 (filled circles) are optically dull The most luminous contribute ~10% of the cluster L X We have identified 35 AGN in 8 clusters LMXB relation from Kim & Fabbiano (2004) Hot Gas relation from O’Sullivan et al. (2003)

AGN Distribution Radial Distribution Cumulative AGN and inactive galaxy distributions for all 8 clusters vs. R/r 200 Kinematic Distribution Distributions vs. |v-v c |/  Substructure Distribution Distribution vs.  where  2 = (11/  2 ) [  local -  ) 2 + (  local -  ) 2 ] (Dressler & Shectman 1988) AGN and inactive galaxies have identical distributions

AGN Fraction in Clusters Cluster AGN Fraction: The fraction of galaxies brighter than M R = -20 mag with L X >10 41 erg/s AGN f A ~ 5% averaged over 8 clusters Galaxy population brighter than M R <-20 mag is the main uncertainty AC114 (z=0.31) M R = -20 Martini et al. (2006b)

Dependence on Cluster Properties There is good evidence for cluster to cluster variation There are at best ‘intriguing trends’ between AGN fraction and various cluster properties Martini et al. (2006b)

Summary Cluster AGN fraction is unexpectedly high: f A ~ 5% Most cluster AGN are optically dull Cluster AGN trace the cluster galaxy population (to ~0.5 r 200 ) The AGN fraction varies from cluster to cluster

Wish List for Future Cluster Surveys A larger sample to determine if substructure or velocity dispersion influences the AGN fraction in clusters A high-redshift sample (z>0.5) to determine if there is evolution Quantification of the impact on cluster cosmology studies A comparable field AGN fraction (The ANEWs of this MISST)