The morphology of clusters of galaxies: the cluster-galaxy connection Irini Sakelliou Birmingham : T. Ponman MPIA : S. Falter, V. Smolcic, E. Bell MPE.

Slides:

Advertisements

Similar presentations

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

Advertisements

Florent Rostagni 1.  Context  Sample  Algorithm for detection and classification  Star formation  X-ray – optical study  Perspectives - Conclusion.

Front X-ray Studies of Galaxies and Galaxy Systems Jesper Rasmussen Ph.D. Defence Astronomical Observatory, Univ. of Copenhagen 17th March 2004.

To study x-ray cavity statistically, we retrieved archival data from the Chandra archive. We obtained our initial sample from the Cluster of galaxies (1522),

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

X-Ray Measurements of the Mass of M87 D. Fabricant, M. Lecar, and P. Gorenstein Astrophysical Journal, 241: , 15 October 1980 Image:

Deep Chandra and XMM-Newton Observations of NGC 4472 R. P. Kraft, S. W. Randall, W. R. Forman, P. E. J. Nulsen, C. Jones, A. Bogdan, M. J. Hardcastle,

Clusters & Super Clusters Large Scale Structure Chapter 22.

Dark Energy Observations of distant supernovae and fluctuations in the cosmic microwave background indicate that the expansion of the universe is accelerating.

The Radio/X-ray Interaction in Abell 2029 Tracy Clarke (Univ. of Virginia) Collaborators: Craig Sarazin (UVa), Elizabeth Blanton (UVa)

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

X-ray and Radio AGN in Coma Cluster Progenitors Quyen Nguyen Hart University of Colorado at Boulder, Center for Astrophysics and Space Astronomy Collaborators.

HI in galaxies at intermediate redshifts Jayaram N Chengalur NCRA/TIFR Philip Lah (ANU) Frank Briggs (ANU) Matthew Colless (AAO) Roberto De Propris (CTIO)

Galaxies Cluster formation : Numerical Simulations and XMM Observations JL Sauvageot *, Elena Belsole *,R.Teyssier *, Herve Bourdin + Service d'Astrophysique.

Clusters, Galaxies and the COSMOS J Berian James (IfA Edinburgh), John Peacock, Alexis Finoguenov, Henry Joy McCracken & Gigi Guzzo for the COSMOS collaboration.

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

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

PX269 Galaxies Part 5: Spatial distribution of galaxies PX269 Galaxies.

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.

Growth of Structure Measurement from a Large Cluster Survey using Chandra and XMM-Newton John R. Peterson (Purdue), J. Garrett Jernigan (SSL, Berkeley),

Radio galaxies in the Chandra Era, Boston, July 2008 Shock heating in the group atmosphere of the radio galaxy B A Nazirah Jetha 1, Martin Hardcastle.

I. Balestra, P.T., S. Ettori, P. Rosati, S. Borgani, V. Mainieri, M. Viola, C. Norman Galaxies and Structures through Cosmic Times - Venice, March 2006.

3C 186 A Luminous Quasar in the Center of a Strong Cooling Core Cluster at z>1 Aneta Siemiginowska CfA Tom Aldcroft (CfA) Steve Allen (Stanford) Jill Bechtold.

1 XMM-Newton Extended Source Analysis Software Steve Snowden & Kip Kuntz  Publicly Released 5 April 2006  XMM-Newton Extended Source Analysis Software.

An XMM-ESAS Update Steve Snowden NASA/Goddard Space Flight Center EPIC Operations and Calibration Meeting - BGWG Palermo - 11 March 2007.

Discovery of Galaxy Clusters Around Redshift 1 Deborah Haarsma, Calvin GLCW, June 1, 2007.

The Structure Formation Cookbook 1. Initial Conditions: A Theory for the Origin of Density Perturbations in the Early Universe Primordial Inflation: initial.

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

Low frequency radio observations of galaxy groups With acknowledgements to: R. Athreya, P. Mazzotta, T. Clarke, W. Forman, C. Jones, T. Ponman S.Giacintucci.

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

PRESIDENCY UNIVERSITY

An X-ray Study of the Bright Supernova Remnant G with XMM-Newton SNRs and PWNe in the Chandra Era Boston, MA – July 8 th, 2009 Daniel Castro,

Evolution of Galaxy groups Michael Balogh Department of Physics University of Waterloo.

1 XMM-Newton Extended Source Analysis Software Steve Snowden & Kip Kuntz  Publicly Released 5 April 2006  XMM-Newton Extended Source Analysis Software.

Dynamical state and star formation properties of the merging galaxy cluster Abell 3921 C. Ferrari 1,2, C. Benoist 1, S. Maurogordato 1, A. Cappi 3, E.

Richard Mushotzky (NASA/GSFC) and Amalia K. Hicks (University of Colorado) An enduring enigma in X-ray astronomy is the "missing mass" in cooling flow.

SYSTEMATICS ON CHANDRA X-RAY MASS ESTIMATES Elena Rasia Dipartimento di Astronomia, Padova,Italy Lauro Moscardini Giuseppe Tormen Stefano.

Santiago Chile (5-9 Dec 2005) 1 “Groups of Galaxies in the nearby Universe” ESO 2005 workshop X-ray Properties of a Mass- Selected Group Catalog P. Mazzotta.

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

Cosmological studies with Weak Lensing Peak statistics Zuhui Fan Dept. of Astronomy, Peking University.

Dwarf LSB galaxies in the Virgo cluster Jonathan Davies.

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

The interaction between galaxies and their environment Trevor Ponman University of Birmingham Jesper Rasmussen Carnegie Observatories.

AY202a Galaxies & Dynamics Lecture 17: Galaxy Groups & Clusters continued.

3 Temperature profiles The shape of the temperatures profiles (some examples are shown in Fig.2) resemble the one obtained for hotter, more massive clusters.

Galaxy Groups Duncan A. Forbes Centre for Astrophysics & Supercomputing, Swinburne University.

TEMPERATURE AND DARK MATTER PROFILES OF AN X-RAY GROUP SAMPLE FABIO GASTALDELLO UNIVERSITY OF CALIFORNIA IRVINE D. BUOTE P. HUMPHREY L. ZAPPACOSTA J. BULLOCK.

TEMPERATURE AND DARK MATTER PROFILES OF AN X-RAY GROUP SAMPLE FABIO GASTALDELLO UNIVERSITY OF CALIFORNIA IRVINE D. BUOTE P. HUMPHREY L. ZAPPACOSTA J. BULLOCK.

The Detection of an Unexplained Emission Line at 3.56 keV Esra Bulbul Harvard-Smithsonian Center for Astrophysics Maxim Markevitch (NASA/GSFC), Adam Foster.

PHY306 1 Modern cosmology 3: The Growth of Structure Growth of structure in an expanding universe The Jeans length Dark matter Large scale structure simulations.

The Structure Formation Cookbook 1. Initial Conditions: A Theory for the Origin of Density Perturbations in the Early Universe Primordial Inflation: initial.

3 Mass profiles We use the temperature and gas density values obtained by fits to the spectra extracted in concentric annuli to calculate the gravitating.

Structural and scaling properties of galaxy clusters Probing the physics of structure formation M.Arnaud, G.Pratt, E.Pointecouteau (CEA-Sap Saclay) Dark.

Wide-field Weak Lensing Mass Reconstructions of Merging Galaxy Clusters Brett Ragozzine, Douglas Clowe Ohio University, Department of Physics & Astronomy,

X-RAY FOLLOW-UP OF STRONG LENSING OBJECTS: SL2S GROUPS (AND A1703) FABIO GASTALDELLO (IASF-MILAN, UCI) M. LIMOUSIN & THE SL2S COLLABORATION.

Main-Cluster XIS0XIS1XIS3 Weighted mean Chandra Figure 2 : XIS spectra of the main-cluster XIS keV Main-Cluster Sub-Cluster Search for Bulk Motion.

X-ray Astronomy School 2002 Clusters of Galaxies (and some Cosmology) Scientific and Data Analysis Issues Keith Arnaud NASA/GSFC and UMCP.

Cosmos Survey PI Scoville HST 590 orbits I-band 2 deg. 2 !

Group Evolution Multi-wavelength Survey (GEMS) Duncan A. Forbes Centre for Astrophysics & Supercomputing, Swinburne University.

Investigating dark matter halos of galaxies from the COMBO-17 survey Martina Kleinheinrich (Max-Planck-Institut für Astronomie, Heidelberg) & Hans-Walter.

Semi-analytical model of galaxy formation Xi Kang Purple Mountain Observatory, CAS.

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

G.W. Pratt, Ringberg, 26/10/2005 Structure and scaling of nearby clusters of galaxies – in X-rays Gabriel W. Pratt, MPE Garching, Germany.

Challenging the merger/sloshing cold front paradigm: A2142 revisited by XMM Mariachiara Rossetti (Università degli Studi di Milano & IASF Milano) D. Eckert,

PX269 Galaxies Part 5: Spatial distribution of galaxies.

Apparent high metallicity in 3-4 keV clusters:

Chandra observation of the sample galaxy clusters

Search for Bulk Motion in A2256 with Suzaku and ASTRO-H

Presentation transcript:

The morphology of clusters of galaxies: the cluster-galaxy connection Irini Sakelliou Birmingham : T. Ponman MPIA : S. Falter, V. Smolcic, E. Bell MPE : A. Finoguenov Colorado: P. Motl

Ringberg 2005 How structure is formed The formation of a Coma- like cluster. Left panels : Dark matter Right panels : Hot gas

Ringberg 2005 Galaxy-Cluster interactions They should affect both : the cluster and its galaxies An infalling galaxy in A2125 (z~0.25) Chandra/HST/VLA/KPNO images NASA press release

Ringberg 2005 Temperature maps Contours= surface brightness How/when and at which stage of cluster formation a) the galaxies are affected/tranformed and b) the ICM is affected by the infalling material?

Ringberg 2005 Simple measures of the structure. That it can work with X-ray and optical and simulated images Centroid offset : Determination of the centre of the distribution in annuli of increasing radius. The annuli are not concentric. Ellipticity Position Angle

Ringberg 2005 Ellipticity & Position angle Accumulation of counts (cnt) along circular annuli (  ). If the 2D distribution is elliptical the cnt-  plot should have 2 peaks. The shape of the cnt-  plot depends on the ellipticity and the position angle.

Ringberg 2005 Abell 2255 XMM-Newton image in the ( ) keV energy range (~14ks MOS exposure) Abell 2255 is a ~7keV at z=0.08 SDSS cluster galaxies. Red circle = XMM FOV

Ringberg 2005 High-z cluster at z=0.22 from COSMOS (Smolcic et al. 2006) It is a poor cluster, in the process of merging with other groups. X-ray contours Red cluster galaxies Blue galaxies

Ringberg 2005 A2255: Centroid offset X-rays: ICM distributionOptical : galaxy distribution

Ringberg 2005 Ellipticity & Position angle

Ringberg 2005 A2255: position angle

Ringberg 2005 Summary, Concluding remarks, & future A simple method to determine the dynamical ‘age’ of clusters from X-ray and optical observations There are still problems to be solved (e.g., errors) We need simple methods for determining the structure of clusters if we want to go higher redshifts Use simulated X-ray images to set the baseline z= 0.25 Simulated X-ray images from Motl et al.2004 z= 0.00