CLUSTERS OF GALAXIES IN X-RAYS FABIO GASTALDELLO INAF IASF-MILANO Silvano Molendi INAF IASF-Milano Silvano Molendi INAF IASF-Milano Pasquale Mazzotta Univ Roma Tor Vergata Pasquale Mazzotta Univ Roma Tor Vergata Paolo Tozzi INAF OA Trieste Paolo Tozzi INAF OA Trieste Stefano Ettori INAF OA Bologna Stefano Ettori INAF OA Bologna

RESEARCH UNITS INAF IASF-MILANO: 6 members, 862 ks (XMM+Chandra) + 1 Ms (Integral) INAF OA BOLOGNA + UNIVERSITA’ BOLOGNA: 14 members, 1 Ms (XMM+Chandra) UNIVERSITA’ ROMA TOR VERGATA + IASF-ROMA: 8 members, 1.5 Ms (XMM+Chandra) INAF OA TRIESTE + UNIVERSITA’ TRIESTE: 5 members, 489 ks (XMM+Chandra)

THE LARGEST VIRIALIZED STRUCTURES TODAY AND “FAIR ARCHIVES OF THE UNIVERSE” Coma cluster in the optical Coma cluster in X-rays CLUSTERS IN A NUTSHELL

Coma cluster in the opticalComa cluster in X-rays Galaxies (5%) Intra-cluster medium (ICM) Thermal plasma X-rays (10-30%) Dark Matter Gravitational potential 1E THE BULLET CLUSTER Relativistic particles Radio

CLUSTERS IN A NUTSHELL RELAXED or COOL CORE Peaked SB and spherical symmetry T drop at the center Low central cooling time (t cool <t Hubble ) Steep entropy profiles Metal abundance peak Presence of a BCG NON COOL CORE No clear SB peak and distorsions in morphology Flat T profiles High central cooling time Flat entropy profiles Flat metal abundance profiles THE CLUSTER POPULATION IS USUALLY DIVIDED INTO TWO CLASSES, LIKELY LINKED TO THE DYNAMICAL STATE AND MERGERS

CLUSTERS IN A NUTSHELL COOL CORE VS. NON-COOL CORE

CLUSTERS IN A NUTSHELL COOL CORE VS. NON-COOL CORE

CLUSTERS IN A NUTSHELL COOL CORE VS. NON-COOL CORE

CLUSTERS IN A NUTSHELL COOL CORE VS. NON-COOL CORE Cavagnolo et al. (2009)

CLUSTERS IN A NUTSHELL COOL CORE VS. NON-COOL CORE ●CC oNCC De Grandi & Molendi (2001)

CLUSTERS IN A NUTSHELL MAJOR MERGERS CAN CAUSE THE LARGE SCALE DISTURBANCES IN SB E T AND THE INCREASE OF ENTROPY WE SEE IN NCC ●CC oNCC Ricker & Sarazin (2001) Markevitch 2011

CLUSTERS IN A NUTSHELL CLUSTER MERGERS AND RADIO EMISSION CONNECTION (Mpc SCALE IN RADIO HALOS AND RELICS) TURBULENT REACCELERATION SCENARIO (e.g. Brunetti et al. 2009) Markevitch 2011 A 520 A 754

CLUSTERS IN A NUTSHELL AGN FEEDBACK IN COOL CORES NECESSARY TO STOP COOLING: HEATING DUE TO CAVITIES IN THE ICM AND WEAK SHOCKS CAUSED BY RADIO JETS PERSEUS Fabian et al MS0735 McNamara et al. 2006

CLUSTERS IN A NUTSHELL CLUSTERS ARE BOTH ASTROPHYSICAL LABORATORIES AND COSMOLOGICAL TOOLS Vikhlinin+09

CLUSTERS IN A NUTSHELL YOU NEED TO UNDERSTAND PHYSICS TO USE HYDROSTATIC EQUILIBRIUM TO OBTAIN MASS AS IN THE FGAS TEST Allen+08

CLUSTERS IN A NUTSHELL YOU NEED TO UNDERSTAND PHYSICS TO USE SCALING RELATIONS TO OBTAIN MASS IN THE MASS FUNCTION TEST Vikhlinin+09

CLUSTERS IN A NUTSHELL CLUSTERS ALLOW MULTIPLE INDIPENDENT PROBES OF THEIR MASS (LENSING, X-RAYS, GALAXY DYNAMICS,SZ …) Anderson+10 Hoekstra+07

RESEARCH UNITS: TOPICS TWO MAIN LINES OF RESEARCH: DETAILED STUDY OF THE PHYSICS OF THE ICM IN NEARBY CLUSTERS (MI, BO, RM, TS) STUDY OF AVERAGE CLUSTER PROPERTIES AND THEIR EVOLUTION WITH REDSHIFT, CLUSTER SCALING RELATIONS AND MASS COMPARISON WITH OTHER TECNIQUES (MI, BO, RM, TS) A LOT OF COLLABORATION BETWEEN THE RUs, MANY PAPERS AND PROJECTS IN COMMON

X-RAY – LENSING MASS COMPARISON IN POOR CLLUSTERS OGURI 2006 GALAXY GROUPS – POOR CLUSTERS WITH IMAGE SEPARATION IN THE RANGE 6”-16” HAVE BEEN SCARCELY REPORTED

SL2S GROUPS INITIAL SAMPLE OF 13 OBJECTS (Limousin+09), A SUBSAMPLE OF THE SL2S BASED ON MULTI-COLOUR CFHTLS, IDEAL TO DETECT SL FEATURES AND FOLLOW-UP HUBBLE IMAGING (z = ) LUMINOSITY MAPS BASED ON LIGHT DISTRIBUTION OF ELLIPTICALS HAVE FOR SOME OBJECTS COMPLICATED SHAPE. WEAK LENSING SIGNAL DETECTED FOR 6 GROUPS

SL2S GROUPS

SL2SJ z = BIMODAL LUMINOSITY DISTRIBUTION (TWO DISTRINCT SUBGROUPS FROM SPECTROSCOPY, MUNOZ+11, IN PREP.). PERTURBED LENSING CONFIGURATION WHICH REQUIRES EXTERNAL MASS (LIMOUSIN+10) SL R E = 5.5“ ± 0.1”

SL2S GROUPS SL2SJ z = MULTIPLE IMAGES (SOUTHERN ARC MAYBE NOT ASSOCIATED) SL R E = 7.3“ ± 0.5”

SL2S GROUPS X-RAY FOLLOW-UP CLEARLY DIFFICULT BECAUSE WE ARE TARGETING LOW FLUX OBJECTS, HOWEVER MORE MASSIVE OBJECTS THAN PREVIOUS STUDIES (E.G., LARGEST IMAGE SEPARATION IN FASSNACHT+08 IS CLASS B WITH R E = 2.5“) XMM SNAPSHOTS OF 5-10 ks TO SECURE FLUXES FOR DEEPER CHANDRA OBSERVATION. ENOUGH PHOTONS FOR MORPHOLOGY AND POSSIBLY TEMPERATURE

SL2S GROUPS X-RAY FOLLOW-UP

SL2S GROUPS X-RAY FOLLOW-UP SEPARATION BETWEEN X-RAY GAS AND GALAXIES (MATTER) IN A BULLET-LIKE CONFIIGURATION ONLY ALONG THE L.O.S. AND FOR AN OBJECT OF FEW SOLAR MASSES Gastaldello et al., in prep.

TWO GROUPS DETECTED, THE N-ONE CONSISTENT WITH THE ELONGATION IN LUMINOSITY CONTOURS. THE S-ONE ASSOCIATED WITH THE LENS HAS A TEMPERATURE CONSISTENT WITH A POOR CLUSTER kT = 3.4 ± 0.6 keV SL2SJ

SL2SJ CLEARLY EXTENDED SOURCE (r c = 150 ± 60 kpc, 34” ± 13”, ß = 0.58 ± 0.12)

HIGH ABUNDANCE IN 3-4 KeV CLUSTERS ? BAUMGARTNER+05 ASCA RESULTS ON AVERAGE METALLICITY ON 273 CLUSTERS CLUSTERS WITH 3-4 KeV HAS APPARENTLY HIIGH ABUNDANCE: PHYSICS OR BIAS IN THE MEASUREMENT ?

A 2028

GREAT DEAL OF STRUCTURE IN THE TEMPERATURE MAP PRESENCE OF A CORONA (1 KeV GAS ASSOCIATED WITH THE BCG IN SUBCLUSTER A)

A 2028 A2028 AS SEEN BY ASCA Image credit: D. Horner

A 2028 “INVERSE” IRON BIAS Gastaldello+10 Region 1, core of clump A

XMM FOLLOW-UP OF PLANCK CLUSTERS

XMM FOLLOW-UP OF PLANCK CLUSTERS SZ DETECTED Z = 1

XMM FOLLOW-UP OF PLANCK CLUSTERS

Subaru-Suprime BVR color image of WARPJ1415 covering an area with 20Å~20 ( 1 Å~ 1 Mpc), centered at RA=14:15:11.08, DEC=+36:12:03.1. North is up and East is to the left. X-ray contours are overlaid in yellow. The 1500Å~1500 inset shows the core with a zoom factor of 2. AN EVOLVED CC AT Z=1 230 ks Chandra Santos, Tozzi et al. in prep.

AN EVOLVED CC AT Z=1 (Left) Chandra full-band image. (Middle) Residual Chandra soft-band image after subtraction of the best-fit single -model, with VLA radio contours overlaid in green. A clear diagonal asymmetry in X-ray emission is visible (sector A). (Right) VLA image of the radio source coincident with the cluster core. A pronouced extended feature with an extent of 80 kpc is seen in the NW direction. All images have a size of 10Å~10. The Chandra images are shown in logarithmic scale with a Gaussian smoothing of 2”. The Fe peak is used to put significant constraints on the enrichment time of the ICM, and the temperature map and the surface brightness are investigated in search of signatures of the ongoing feedback process driven by the radio AGN, imaged with VLA archival data.

AND MUCH MORE... CHANDRA-VLA PROGRAM TO OBSERVE COOL CORE CLUSTERS BRIGHT IN Hα AND X-RAY: MOST PROMISING TARGETS TO INVESTIGATE AGN FEEDBACK MERGERS – RADIO HALOS AND RELICS CONNECTION