Chandra observation of the sample galaxy clusters

Slides:

Advertisements

Similar presentations

Dark Matter in Dwarf Galaxies

Advertisements

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),

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

Cosmological constraints from estimates of M gas -M tot -c in X-ray luminous clusters S. Ettori (INAF/OA Bologna) with F. Gastaldello, M. Meneghetti, I.

The Sharpest Spatial View of a Black Hole Accretion Flow from the Chandra X-ray Visionary Project Observation of the NGC 3115 Bondi Region Jimmy Irwin.

CLASH: Cluster Lensing And Supernova survey with Hubble ACS Parallels WFC3 Parallels 6 arcmin. = 2.2 z=0.5 Footprints of HST Cameras: ACS FOV in.

Luigina Feretti Istituto di Radioastronomia CNR Bologna, Italy Radio observations of cluster mergers X-Ray and Radio Connections, Santa Fe, NM February.

Numerical issues in SPH simulations of disk galaxy formation Tobias Kaufmann, Lucio Mayer, Ben Moore, Joachim Stadel University of Zürich Institute for.

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

First X-Ray Results from the Optically Selected Red Sequence Cluster Survey (RCS) at Z ~ 1 Amalia K. Hicks, Erica Ellingson, Howard Yee, Tesla Jeltema,

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.

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

A Different Dark Matter Potential for Modeling Cluster Atmospheres Andisheh Mahdavi University of Hawai’i.

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

On the Distribution of Dark Matter in Clusters of Galaxies David J Sand Chandra Fellows Symposium 2005.

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

Particle Astrophysics & Cosmology SS Chapter 8 Structure Formation.

Annalisa Bonafede PhD student at IRA Radio Astronomy Institute Bologna (Italy) With: L. Feretti, G. Giovannini, M. Murgia, F. Govoni, G. B.Taylor, H. Ebeling,

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

Astrophysics & Cosmology Sabine Schindler Institute for Astrophysics University of Innsbruck.

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

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

X-Ray Observations of RCS Clusters at High Redshift

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

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

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

Observational Constraints on Galaxy Clusters and DM Dynamics Doron Lemze Tel-Aviv University / Johns Hopkins University Collaborators : Tom Broadhurst,

A multi-colour survey of NGC253 with XMM-Newton Robin Barnard, Lindsey Shaw Greening & Ulrich Kolb The Open University.

The clustering of galaxies detected by neutral hydrogen emission Sean Passmoor Prof. Catherine Cress Image courtesy of NRAO/AUI and Fabian Walter, Max.

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.

Background treatment in spectral analysis of low surface brightness sources Alberto Leccardi & Silvano Molendi Garching, 2 nd May 2006 EPIC background.

MASS AND ENTROPY PROFILES OF X-RAY BRIGHT RELAXED GROUPS FABIO GASTALDELLO UC IRVINE & BOLOGNA D. BUOTE P. HUMPHREY L. ZAPPACOSTA J. BULLOCK W. MATHEWS.

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

SUNYAEV-ZELDOVICH EFFECT. OUTLINE  What is SZE  What Can we learn from SZE  SZE Cluster Surveys  Experimental Issues  SZ Surveys are coming: What.

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.

Diffuse Intergalactic Light in Intermediate Redshift Cluster: RX J I. Toledo (PUC) J. Melnick (ESO) E. Giraud (LPTA) F. Selman (ESO) H. Quintana.

Discovery of a Dark Matter Ring in CL Myungkook James Jee Johns Hopkins University, Baltimore, USA July 3, 2007 IAP Myungkook James Jee Johns Hopkins.

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.

Initial Results from the Chandra Shallow X-ray Survey in the NDWFS in Boötes S. Murray, C. Jones, W. Forman, A. Kenter, A. Vikhlinin, P. Green, D. Fabricant,

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

Correlations of Mass Distributions between Dark Matter and Visible Matter Yuriy Mishchenko and Chueng-Ryong Ji NC State University Raleigh, NC KIAS-APCTP-DMRC.

中国科学院高能物理研究所 INSTITUTE OF HIGH ENERGY PHYSICS Constraints on the cross-section of dark matter annihilation from Fermi observation of M31 Zhengwei Li Payload.

On the evolution of Cool Core Clusters Joana Santos (INAF-Trieste) Piero Rosati (ESO), Paolo Tozzi (INAF-Trieste), Hans Boehringer (MPE), Stefano Ettori.

DETERMINATION OF THE HUBBLE CONSTANT FROM X-RAY AND SUNYAEV-ZELDOVICH EFFECT OBSERVATIONS OF HIGH-REDSHIFT GALAXY CLUSTERS MAX BONAMENTE – UNIVERSITY OF.

Major dry-merger rate and extremely massive major dry-mergers of BCGs Deng Zugan June 31st Taiwan.

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

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

RGS observations of cool gas in cluster cores Jeremy Sanders Institute of Astronomy University of Cambridge A.C. Fabian, J. Peterson, S.W. Allen, R.G.

(1) Laboratoire d’Astrophysique de Marseille [F] - (2) Université de Montréal [Ca] - (3) Observatoire de Paris [F] Asymmetries within Optical Discs of.

Metal abundance evolution in distant galaxy clusters observed by XMM-Newton Alessandro Baldi Astronomy Dept. - University of Bologna INAF - OABO In collaboration.

Evolution of clusters M. Arnaud CEA - service d’astrophysique Saclay Assuming favored cosmology  =0.3  =0.7.

TWO SAMPLES OF X-RAY GROUPS FABIO GASTALDELLO UC IRVINE & BOLOGNA D. BUOTE P. HUMPHREY L. ZAPPACOSTA J. BULLOCK W. MATHEWS UCSC F. BRIGHENTI BOLOGNA.

The XMM Distant Cluster Project: Survey limits and Pilot Survey Georg Lamer A. Schwope, V. Hambaryan, M. Godolt (AIP) H. Böhringer, R. Fassbender, P. Schücker,

Combine Observations of Galaxy Clusters to Constrain Cosmological Parameters Heng Yu ( 余恒 ) & Zong-Hong Zhu Beijing Normal University

Ni ABUNDANCE IN THE CORE OF THE PERSEUS CLUSTER: AN ANSWER TO THE SIGNIFICANCE OF RESONANT SCATTERING AND SNIa ENRICHMENT Fabio Gastaldello (CNR-IASF,

The Dynamical State of Massive Galaxy Clusters Conclusions  Lensing to dynamical mass discrepancy do seems to probe the dynamical state of galaxy clusters.

Composite profile of the Fe Kα spectral line emitted from a binary system of supermassive black holes Predrag Jovanović1, Vesna Borka Jovanović2 and Duško.

Jesper Rasmussen (Univ. of Birmingham)

Advisors: Tom Broadhurst, Yoel Rephaeli

The Search for Gamma-Rays From Galaxy Clusters

Investigating the Faint X-ray Sources in

Analysis of Off-Nuclear X-Ray Sources in Galaxy NGC 4945

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

Subaru Weak Lensing Study of Seven Merging Clusters of Galaxies

Surface Brightness Profile - NGC 3379 (giant elliptical)

XMM v Chandra - Cluster Analysis

The X-ray Morphology and Spectra of Galactic Disks

THE X-RAY C-M RELATION FABIO GASTALDELLO INAF-IASF MILANO, UCI

Presentation transcript:

Chandra observation of the sample galaxy clusters Babyk Iu., Melnyk O., Elyiv A. National Taras Shevchenko University of Kyiv, Ukraine Institut d'Astrophysique et de Géophysique, Liège , Belgique

Cluster of galaxies Name ObsID z Ex. Time (ksec) Instr. A223 4967 0.21 45.6 ACIS-I A521 430 0.25 39.6 ACIS-S A611 3194 0.28 36.6 A697 4217 19.7 A907 3205 0.15 47.7 A1204 2205 0.17 23.9 A1413 537 0.14 9.34 A2744 2212 0.31 25.14 CL0024+17 929 0.39 40.34 RXJ 1347.5-1145 2222 0.45 93.9

The spectrum of one ring and fit his by WABS*MEKAL model. Data reduction v 1. For data reduction we used CIAO 4.2 soft. Detection and removal of point sources. Splitting of image on concentric rings. We used Xspec 12.6 for fitting our spectrums in each ring. We selected MEKAL model for fitting (Mewe, Kaastra & Leidahl). 5. We obtained T and Norm – parameter. The spectrum of one ring and fit his by WABS*MEKAL model.

Radial temperature profiles Name T, keV T, (10^7)K A223 5,01 5.81 A521 10.21 12.65 A611 6.24 7.23 A697 10.22 12.09 A907 6.38 A1204 4.84 5.61 A1413 8.07 9.37 A2744 9.82 11.41 CL0024+17 4.30 4.99 RXJ 1347.5+1145 11.81 13.41

Method

The results of modeling Abell 223 Abell 1204 Abell 1413 Abell 2744 CL 0024+17 Observational (black points) and simulated (red solid lines) surface brightness. The distribution our errors. (90% probability)

The density and mass profiles for dark matter and intracluster gas (ICM) Abell 223 Abell 1204 Abell 1413 Abell 2744 CL 0024+17 The density profiles for dark matter (upper curves) and gas (lower curves). The mass profiles for dark matter (upper curves) and gas (lower curves).

The integrated total mass profiles

Short conclusions We determined the total mass galaxy of clusters and build the mass profiles for dark matter and gas. We found the fraction dark matter and intracluster gas in the total mass of clusters. Also, we presented radial temperature profiles for each cluster and density profiles for dark matter and intracluster gas.