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THE CHANDRA AND XMM VIEW OF MASS, SLOSHING AND AGN FEEDBACK IN GALAXY GROUPS

THE CHANDRA AND XMM VIEW OF MASS, SLOSHING AND AGN FEEDBACK IN GALAXY GROUPS. FABIO GASTALDELLO IASF MILANO, UCI

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THE CHANDRA AND XMM VIEW OF MASS, SLOSHING AND AGN FEEDBACK IN GALAXY GROUPS

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

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

  4. c slowly declines as M increases (slope of -0.1) • Constant scatter (σlogc ≈ 0.14) • the normalization depends sensitively on the cosmological parameters, in particular σ8 and w (D04,Kuhlen et al. 2005). c-M RELATION Bullock et al. 2001

  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) 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 Chandra XMM-Newton SUZAKU • Low and stable background • 1 arcsec resolution • High sensitivity due to high effective area, i.e. more photons

  9. Vikhlinin et al. 2006 Pointecouteau et al. 2005 • 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). Clusters X-ray results

  10. 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 1012 ≤ M ≤ 1014 Msun • There were very few constraints on groups scale (1013 ≤ M ≤ 1014 Msun) • 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 THE PROJECT

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

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

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

  14. 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 RESULTS

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

  16. 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 1014 Msun. • 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

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

  18. THE PERSEUS CLUSTER Fabian+11

  19. THE PERSEUS CLUSTER Fabian+11

  20. THE PERSEUS CLUSTER Fabian+11

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

  22. NGC 5044 Gastaldello+09

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

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

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

  26. COLD FRONTS IN CLUSTERS IN MERGING CLUSTERS IN RELAXED CLUSTERS Markevitch & Vikhlinin 07

  27. COLD FRONTS IN CLUSTERS Ascasibar & Markevitch 06

  28. SLOSHING CFs IN CLUSTERS Ascasibar & Markevitch 06

  29. COLD FRONTS IN CLUSTERS Markevitch & Vikhlinin 07

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

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

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

  33. SLOSHING CFs IN NGC 5044 Gastaldello+09

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

  35. COMPARISON W/ SIMULATIONS

  36. SLOSHING IN PERSEUS Simionescu+12

  37. EXCESS IN NGC 5044

  38. EXCESS IN NGC 5044

  39. EXCESS IN NGC 5044

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

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

  42. SLOSHING CFs IN IC 1860

  43. SLOSHING CFs IN IC 1860

  44. SLOSHING CFs IN IC 1860

  45. SLOSHING CFs IN IC 1860

  46. PECULIAR VELOCITIES AND PERTURBERS AM 06

  47. 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

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

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

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