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CLUSTERS OF GALAXIES IN X-RAYS

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

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CLUSTERS OF GALAXIES IN X-RAYS

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

  2. 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)

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

  4. Intra-cluster medium (ICM) Thermal plasma X-rays (10-30%) CLUSTERS IN A NUTSHELL Relativistic particles Radio Galaxies (5%) Dark Matter Gravitational potential Coma cluster in the optical Coma cluster inX-rays 1E 0657-156 THE BULLET CLUSTER

  5. CLUSTERS IN A NUTSHELL • 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 • RELAXED or COOL CORE • Peaked SB and spherical symmetry • T drop at the center • Low central cooling time (tcool<tHubble) • Steep entropy profiles • Metal abundance peak • Presence of a BCG • THE CLUSTER POPULATION IS USUALLY DIVIDED INTO TWO CLASSES, LIKELY LINKED TO THE DYNAMICAL STATE AND MERGERS

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

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

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

  9. CLUSTERS IN A NUTSHELL Cavagnoloet al. (2009) • COOL CORE VS. NON-COOL CORE

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

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

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

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

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

  15. 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

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

  17. 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 = 0.3-0.8) • LUMINOSITY MAPS BASED ON LIGHT DISTRIBUTION OF ELLIPTICALS HAVE FOR SOME OBJECTS COMPLICATED SHAPE. WEAK LENSING SIGNAL DETECTED FOR 6 GROUPS

  18. SL2S GROUPS

  19. SL2S GROUPS SL2SJ08544-0053 z = 0.351 BIMODAL LUMINOSITY DISTRIBUTION (TWO DISTRINCT SUBGROUPS FROM SPECTROSCOPY, MUNOZ+11, IN PREP.). PERTURBED LENSING CONFIGURATION WHICH REQUIRES EXTERNAL MASS (LIMOUSIN+10) SL RE = 5.5“ ± 0.1”

  20. SL2S GROUPS SL2SJ02140-0532 z = 0.444 MULTIPLE IMAGES (SOUTHERN ARC MAYBE NOT ASSOCIATED) SL RE = 7.3“ ± 0.5”

  21. 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 B2108+213 WITH RE = 2.5“) • XMM SNAPSHOTS OF 5-10 ksTO SECURE FLUXES FOR DEEPER CHANDRA OBSERVATION. ENOUGH PHOTONS FOR MORPHOLOGY AND POSSIBLY TEMPERATURE

  22. SL2S GROUPS X-RAY FOLLOW-UP

  23. SL2S GROUPS X-RAY FOLLOW-UP Gastaldelloet al., in prep. 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 1014 SOLAR MASSES

  24. SL2SJ09013-0158 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

  25. SL2SJ09013-0158 CLEARLY EXTENDED SOURCE (rc = 150 ± 60 kpc, 34” ± 13”, ß = 0.58 ± 0.12)

  26. 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 ?

  27. A 2028

  28. A 2028 GREAT DEAL OF STRUCTURE IN THE TEMPERATURE MAP PRESENCE OF A CORONA (1 KeV GAS ASSOCIATED WITH THE BCG IN SUBCLUSTER A)

  29. A 2028 Imagecredit: D. Horner A2028 AS SEEN BY ASCA

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

  31. XMM FOLLOW-UP OF PLANCK CLUSTERS

  32. XMM FOLLOW-UP OF PLANCK CLUSTERS SZ DETECTED CLUSTER @ Z = 1

  33. XMM FOLLOW-UP OF PLANCK CLUSTERS

  34. AN EVOLVED CC AT Z=1 230 ks Chandra Santos, Tozzi et al. in prep. 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.

  35. AN EVOLVED CC AT Z=1 The Fe peakisusedto put significantconstraints on the enrichmenttimeof the ICM, and the temperature map and the surfacebrightness are investigated in searchofsignaturesof the ongoing feedback processdrivenby the radio AGN, imagedwith VLA archival data. (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”.

  36. 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

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