1. THE CHANDRA AND XMM VIEW OF MASS, SLOSHING AND AGN FEEDBACK IN GALAXY GROUPS FABIO GASTALDELLO IASF MILANO, UCI F. BRIGHENTI, D. BUOTE, J. BULLOCK, S. DE GRANDI, D. ECKERT, S. ETTORI, L. DI GESU, S. GHIZZARDI, S. GIACINTUCCI, P. HUMPHREY, W.MATHEWS, S. MOLENDI, E. ROEDIGER, M. ROSSETTI, P. TEMI M. LIMOUSIN, T. VERDUGO, G. FOEX, R. MUNOZ, V. MOTTA, R. CABANAC AND THE SL2S TEAM

2. OUTLINE 1.MASS RESULTS: MASS PROFILE, c-M PLOT AND GAS FRACTIONS FOR X-RAY GROUPS 2.AGN FEEDBACK AND SLOSHING COLD FRONTS IN THE PERSEUS OF GROUPS, NGC 5044 3.LENSING GROUPS AND THE “BULLET” GROUP

3. DM DENSITY PROFILE Navarro et al. 2004 The concentration parameter c do not depend strongly on the innermost data points, r < 0.05 r vir (Bullock et al. 2001, B01; Dolag et al. 2004, D04).

4. c-M RELATION Bullock et al. 2001 c slowly declines as M increases (slope of -0.1) Constant scatter (σ logc ≈ 0.14) the normalization depends sensitively on the cosmological parameters, in particular σ 8 and w (D04,Kuhlen et al. 2005).

5. c-M RELATION Macciò et al. 2008

6. X-RAY MASS DETERMINATION Spectra averaged within circular annuli Normalization / shape of spectrum gives gas density / temperature

7. X-RAY MASS DETERMINATION A) Deproject with no need to assume parametrized quantities for gas quantities but smoothing required to obtain a physical mass profile (smoothed inversion) fit gas density and temperature simultaneously assuming only parameterizations for density (or T or entropy) and mass B) Forward-fitting: fit gas density and temperature simultaneously assuming only parameterizations for density (or T or entropy) and mass Buote & Humphrey 11

8. A SPECIAL ERA IN X-RAY ASTRONOMY ChandraXMM-Newton 1 arcsec resolutionHigh sensitivity due to high effective area, i.e. more photons SUZAKU Low and stable background

9. NFW a good fit to the mass profile c-M relation is consistent with no variation in c and with the gentle decline with increasing M expected from CDM ( α = - 0.04  0.03, P05). Vikhlinin et al. 2006 Pointecouteau et al. 2005 Clusters X-ray results

10. THE PROJECT Improve significantly the constraints on mass profiles and c-M relation by analyzing a wider mass range with many more systems, in particular obtaining accurate mass constraints on relaxed systems with 10 12 ≤ M ≤ 10 14 M sun There were very few constraints on groups scale (10 13 ≤ M ≤ 10 14 M sun ) In Gastaldello et al. 2007 we selected a sample of 16 objects in the 1-3 keV range from the XMM and Chandra archives with the best available data

12. RESULTS After accounting for the mass of the hot gas, NFW + stars is the best fit model MKW 4 NGC 533 STARS GAS DM

13. RESULTS No detection of stellar mass due to poor sampling in the inner 20 kpc or localized AGN disturbance A 2717

14. RESULTS No detection of stellar mass due to poor sampling in the inner 20 kpc or localized AGN disturbance NGC 5044 Buote et al. 2002

15. RESULTS NFW + stars best fit model Not all the objects require stellar mass, due to poor sampling in the inner 20 kpc or localized AGN disturbance. Stellar M/L in K band for the objects with best available data is 0.57  0.21, in reasonable agreement with SP synthesis models (≈ 1) Adopting more complicated models, like introducing AC or N04 did not improve the fits. AC produces too low stellar mass-to- light ratios

16. c-M relation for groups We obtain a slope α=-0.226  0.076, c decreases with M at the 3σ level

17. THE LOCAL X-RAY c-M RELATION Buote, Gastaldello et al. 2007: c-M relation for 39 systems ranging in mass from ellipticals to the most massive galaxy clusters (0.06- 20) x 10 14 M sun. A power law fit requires at high significance (6.6σ) that c decreases with increasing M (slope -0.172 ± 0.026) Normalization and scatter consistent with relaxed objects

18. THE LOCAL X-RAY c-M RELATION WMAP 1 yr Spergel et al. 2003

19. THE LOCAL X-RAY c-M RELATION WMAP 3yr Spergel et al. 2006

20. GAS FRACTIONS GASTALDELLO ET AL. 2007 (see also Sun+09) CLUSTERS GROUPS

21. THE PERSEUS CLUSTER Fabian+11

22. THE PERSEUS CLUSTER Fabian+11

23. THE PERSEUS CLUSTER Fabian+11

24. Fabian et al. 2003

25. NGC 5044 Gastaldello+09 (using J. Sanders’ binning code) See also results from longer Chandra observation (David+09)

26. NGC 5044 Gastaldello+09

27. NGC 5044 CAON ET AL. 2000 Gastaldello+09

28. DUST IN NGC 5044 TEMI, BRIGHENTI & MATHEWS 2007 8-4.5 µm PAH

29. NGC 5044 Gastaldello+09 BLACK : X-ray FILAMENT box #2 RED: X-ray FILAMENT box #7

30. COLD FRONTS IN CLUSTERS IN MERGING CLUSTERSIN RELAXED CLUSTERS Markevitch & Vikhlinin 07

31. COLD FRONTS IN CLUSTERS Ascasibar & Markevitch 06

32. SLOSHING CFs IN CLUSTERS Ascasibar & Markevitch 06

33. COLD FRONTS IN CLUSTERS Markevitch & Vikhlinin 07

34. HOW ABOUT GROUPS ? EXAMPLES IN MERGING SYSTEMS, e.g. NGC 1404 IN FORNAX (Machacek+05)

35. SLOSHING CFs IN NGC 5044 Gastaldello+09 z=0.009 kT=1.2 keV

36. SLOSHING CFs IN NGC 5044 Gastaldello+09 z=0.009 kT=1.2 keV

37. SLOSHING CFs IN NGC 5044 Gastaldello+09

38. SLOSHING CFs IN NGC 5044 Gastaldello+09 z=0.009 kT=1.2 keV

39. COMPARISON W/ SIMULATIONS

40. SLOSHING IN PERSEUS Simionescu+12

41. EXCESS IN NGC 5044

44. SLOSHING CFs IN IC 1860 Gastaldello+13 arXiv:1304.5478 z=0.022 kT=1.4 keV

45. SLOSHING CFs IN IC 1860 z=0.022 kT=1.4 keV Gastaldello+13 arXiv:1304.5478

46. SLOSHING CFs IN IC 1860

50. PECULIAR VELOCITIES AND PERTURBERS AM 06

51. MENDEL+08 STUDY OF 111 MEMBERS: PECULIAR VELOCITY OF 156 km/s WRT THE MEAN VELOCITY Z-score: 4.8σ PECULIAR VELOCITIES AND PERTURBERS: NGC 5044

52. DETECTION OF A SUBSTRUCTURE (99.9 %) AT 1.4 Mpc MENDEL+08. OR NGC 5054 (DAVID+09). PECULIAR VELOCITIES AND PERTURBERS: NGC 5044

53. cz = 2733 km/s cz = 1658 km/s

54. PECULIAR VELOCITIES AND PERTURBERS: NGC 5044 cz = 2733 km/s cz = 1658 km/s

55. PECULIAR VELOCITIES AND PERTURBERS: NGC 5044 BUZZONI+12

56. PECULIAR VELOCITIES AND PERTURBERS: IC1860 STUDY OF 81 MEMBERS AVAILABLE IN NED: PECULIAR VELOCITY OF 113±50 km/s (Z-score significant at the 2.3σ level) WRT THE MEAN VELOCITY

57. PECULIAR VELOCITIES AND PERTURBERS: IC1860 PRESENCE OF SUBSTRUCTURES AT A MARGINAL LEVEL 96%

58. PECULIAR VELOCITIES AND PERTURBERS: IC1860

60. V PEC OF BCGs COZIOL+09: “A large fractions of BCGs have significant peculiar velocity. This has one immediate consequence, which is that most clusters harboring a dominant galaxy are not dynamically relaxed” VAN DEN BOSCH+05: “The brightest galaxy in a dark matter halo is expected to reside at rest at the centre of the halo. In this paper, we test this `Central Galaxy Paradigm' (CGP) using group catalogues extracted from the Two-Degree Field Galaxy Redshift Survey (2dFGRS) and the Sloan Digital Sky Survey (SDSS). We show that the CGP is only consistent with the data in haloes with M < 10 13 M sun, while in more massive haloes the data indicate a non-zero offset between the brightest galaxy and the satellites. This indicates that either central galaxies reside at the minimum of the dark matter potential, but that the halo itself is not yet fully relaxed, or, that the halo is relaxed, but that the central galaxy oscillates in its potential well.

61. V PEC OF BCGs Van den Bosch+05

62. RADIO EMISSION: NGC 5044 GMRT RADIO DATA AT 610 MHz David+09

63. RADIO EMISSION: NGC 5044 GMRT RADIO DATA AT 235 MHz David+09

64. RADIO EMISSION: NGC 5044 GMRT RADIO DATA AT 235 MHz David+09

65. RADIO EMISSION: IC 1860 ABSENCE OF EXTENDED 1.4 GHz EMISSION (DUNN+10)

66. RADIO EMISSION: IC 1860 GMRT RADIO DATA AT 325 MHz. EMISSION AT THESE SCALES INDICATES VERY STEEP SPECTRUM.

67. RADIO EMISSION ZuHone+13

68. IMAGE SEPARATION DISTRIBUTION OF SL OGURI 2006 GALAXY GROUPS – POOR CLUSTERS WITH IMAGE SEPARATION IN THE RANGE 6”-16” HAVE BEEN SCARCELY REPORTED

69. IMAGE SEPARATION DISTRIBUTION OF SL OGURI 2006 NO 6”-15” IMAGE SEPARATION LENSES IN THE CLASS SURVEY (PHILLIPS+01, McKEAN10)

70. SL2S GROUPS INITIAL SAMPLE OF 13 OBJECTS, 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

71. SL2S GROUPS

72. 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 R E = 2.5“) XMM SNAPSHOTS OF 5-10 ks TO SECURE FLUXES FOR DEEPER CHANDRA OBSERVATION. ENOUGH PHOTONS FOR MORPHOLOGY AND POSSIBLY TEMPERATURE

73. SL2SJ09013-0158 z = 0.30 (PHOT) STRAIGHT ARC BETWEEN THE TWO GALAXIES SL R E = 6.8“

74. 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

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

76. SL2SJ22214-0053 z = 0.334 STRAIGHT ARC BETWEEN THE TWO GALAXIES SL R E = 6.83±0.15“

77. SL2SJ22214-0053 JUST A POINT SOURCE DETECTED, HOWEVER VERY SHALLOW XMM EXPOSURE (5 KS)

78. SL2SJ09413-1100 z = 0.385 EXTENDED STELLAR HALO FOR CENTRAL GALAXY SL R E = 7.50±0.81“

79. SL2SJ09413-1100 RATHER REGULAR X-RAY EMISSION TEMPERATURE OF KT=3.6±0.4

80. SL2SJ09413-1100 CLEARLY EXTENDED SOURCE

81. SL2SJ02140-0532 z = 0.444 MULTIPLE IMAGES (SOUTHERN ARC MAYBE NOT ASSOCIATED) SL R E = 7.3“ ± 0.5”

82. SL+WL+GALAXY DYNAMICS (VERDUGO+11) UNIMODAL NFW W/ c_200 = 6.0±0.6 AND M_200 ≈ 1.0 x 10 14 REPRODUCES WELL ALL THE CONSTRAINTS

83. SL2SJ02140-0535 EVIDENCE FOR A SINGLE HALO: FIT A SINGLE HALO IN SL, NO OPTICAL SUBSTRUCTURE (MUNOZ+11, IN PREP) X-RAY EXTENDED BUT NOT ENOUGH COUNTS FOR SPECTRAL INFORMATION

84. SL2SJ08544-0053 z = 0.351 BIMODAL LUMINOSITY DISTRIBUTION (TWO DISTRINCT SUBGROUPS FROM SPECTROSCOPY WITH A VELOCITY DIFFERENCE OF 1200 km/s, MUNOZ+13). PERTURBED LENSING CONFIGURATION WHICH REQUIRES EXTERNAL MASS (LIMOUSIN+10) SL R E = 5.5“ ± 0.1”

86. SL2SJ08544-0053 ELONGATED X-RAY EMISSION TEMPERATURE OF KT=2.7±0.4

87. SL2SJ08544-0053 CLEARLY EXTENDED SOURCE (r c = 128 ± 56 kpc, 26” ± 11”, ß = 0.52 ± 0.07)

88. SL2SJ08544-0053: THE BULLET GROUP SEPARATION BETWEEN X-RAY GAS AND GALAXIES

89. THE BULLET GROUP SEPARATION BETWEEN THE X-RAY PEAK AND THE GALAXY ASSOCIATED WITH THE LENS OF 22” (109 Kpc)

90. WHY LOOKING FOR BULLETS ?

91. Galaxies (5%) Intra-cluster medium (ICM) Thermal plasma X-rays (10-30%) Dark Matter Gravitational potential 1E 0657-156 THE BULLET CLUSTER MARKEVITCH+04

92. CONSTRAINTS ON DM SELF- INTERACTION CROSS SECTION RANDALL+08

93. BABY BULLET (MACS J0025) BRADAČ+08

94. SHAN+10 SL2S J08544

95. BULLETTICITY MASSEY+11

96. BULLETTICITY Measurement of a statistical signal using lensing (Euclid) and X-ray surveys (EROSITA)

97. BULLETTICITY MASSEY+11

98. BULLETTICITY FORERO-ROMERO+11

99. CONCLUSIONS Mass constraints for X-ray bright groups derived from good quality Chandra and XMM data can be of the same quality as obtained for hot, massive clusters. This crucial mass regime has provided the crucial evidence of the decrease of c with increasing M. Gas fraction reveal a more dramatic effect of feedback on these low mass scale The group environment is a nice environment to study the effect of sloshing Lensing groups will play an increasing role in the future with large area surveys

100. Concentrations for relaxed halos are larger by 10% compared to the whole population (Jing 2000, Wechsler 2002, Maccio’ 2006). They show also smaller scatter (σ logc ≈ 0.10) Wechsler et al. 2002 Selection Effects

101. AWM4 AND AGN FEEDBACK Gastaldello+08, see also O’Sullivan+05, Giacintucci+08

102. AWM4 AND AGN FEEDBACK Gastaldello+08 It’s also a fossil system (Zibetti+08)

103. AWM4 AND AGN FEEDBACK Inspired by Donahue+05

104. AWM4 AND AGN FEEDBACK Bauer+05 CC NCC CC NCC De Grandi & Molendi 01

105. EVERY RADIO BCG HAS A COOL CORE (?) Sun+09

106. X-RAY CORONAE Sun+09Abell 3627

107. AWM4 AND AGN FEEDBACK

108. Gastaldello+08 Sun+09

109. AWM4 AND AGN FEEDBACK Cavagnolo+08

110. X-RAY SYSTEMATICS 1.HYDROSTATIC EQUILIBRIUM 2.MULTIPHASE GAS/PROJECTION EFFECTS IN CORES 3.DISCRETE SOURCES IN Es 4.BKG SUBTRACTION 5.DEPROJECTION AND FITTING PROCEDURES

111. Chandra inner regions XMM outer regions NGC 533 DATA ANALYSYS

112. DATA ANALYSIS Chandra is crucial in the inner region where a steep temperature gradient is present When data are available, we use Chandra in the core and XMM in the outer regions MULTI T UNRESOLVED POINT SOURCES

113. BKG SUBTRACTION Bkg subtraction always crucial of course because of low surface brightness but different respect to clusters: particle background is not so crucial, important are the galactic components (and SWCX, we should routinely check for it, e.g. Carter & Sembay 08) We completely model the various bkg components (e.g. Lumb et al. 2002), exploiting the fact that the source component, mainly characterized by the Fe-L shell, is clearly spectrally separated from the other bkg components

114. BKG MODELLING NGC 5044 offset Buote et al. 2004

115. DATA ANALYSIS NGC 1550 Projection of the 3D ρ and T thus obtained to the results from spectral analysis, including the radial variation of the plasma emissivity  (T,Z Fe ). Using an onion peeling deprojection (e.g., Fabian et al. 1981) gives consistent results with the above method Spectroscopic like T problem (e.g., Mazzotta et al. 2004). Folding through responses : no systematic effects