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Chandra and XMM View of Mass, Entropy, and AGN Feedback in Galaxy Groups

This study analyzes the mass, entropy, and AGN feedback in galaxy groups using data from Chandra and XMM-Newton telescopes. It explores the c-M relation and gas fractions in X-ray groups, with a focus on two interesting groups: AWM4 and NGC 5044.

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Chandra and XMM View of Mass, Entropy, and AGN Feedback in Galaxy Groups

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  1. THE CHANDRA AND XMM VIEW OF MASS, ENTROPY AND AGN FEEDBACK IN GALAXY GROUPS FABIO GASTALDELLO IASF MILANO, UCI, OCCHIALINI FELLOW D. BUOTE, P. HUMPHREY,L. ZAPPACOSTA,J. BULLOCK, W. MATHEWS,F. BRIGHENTI, P. TEMI, S. ETTORI

  2. MASS RESULTS: c-M PLOT AND GAS FRACTIONS FOR X-RAY GROUPS • ENTROPY PROFILES • AGN FEEDBACK IN TWO INTERESTING GALAXY GROUPS: • AWM4: A CORONA IN A RELAXED OBJECT • NGC 5044: CAVITIES, FILAMENTS AND COLD FRONTS IN THE PERSEUS OF GROUPS OUTLINE

  3. THE COSMOLOGICAL MODEL Allen et al. 2004

  4. 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

  5. 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

  6. 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

  7. 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

  8. 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

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

  10. Assume spherical symmetry Fit spectra with coronal plasma models and obtain (deprojected) spectral quantities Fit parameterized functions to radial profiles of gas density and temperature Assume hydrostatic equilibrium Calculate the radial mass profile X-RAY MASS DETERMINATION

  11. “Parametric mass method” is the principal approach of the study: we assume parameterizations for the temperature and mass profiles to calculate the gas density assuming HE Gas density solution DATA ANALYSYS We considered also the temperature solution

  12. DATA ANALYSYS • Fit gas density and temperature simultaneously assuming only parameterizations for temperature and mass. • Advantages: • better constraints on M • easy to interpret goodness of fit

  13. HYDROSTATIC EQUILIBRIUM • MULTIPHASE GAS/PROJECTION EFFECTS IN CORES • DISCRETE SOURCES IN Es • BKG SUBTRACTION • DEPROJECTION AND FITTING PROCEDURES X-RAY SYSTEMATICS

  14. DATA ANALYSYS • Chandra inner regions • XMM outer regions NGC 533

  15. MULTI T UNRESOLVED POINT SOURCES 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

  16. 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,ZFe). • 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

  17. 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 BKG SUBTRACTION

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

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

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

  21. 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

  22. 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

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

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

  25. ENTROPY PROFILES

  26. ENTROPY PROFILES

  27. COMPARISON WITH MASSIVE CLUSTERS AND GRAVITATIONAL SIMULATIONS PRATT ET AL. 2006

  28. COMPARISON WITH MASSIVE CLUSTERS AND GRAVITATIONAL SIMULATIONS

  29. FUTURE WORK: SUZAKU ! Abell 262: SATO, MATSUSHITA & FG 09

  30. Fabian et al. 2003

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

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

  33. AWM4 AND AGN FEEDBACK Inspired by Donahue+05

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

  35. X-RAY CORONAE Abell 3627 Sun+09

  36. AWM4 AND AGN FEEDBACK

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

  38. AWM4 AND AGN FEEDBACK Sun+09 Gastaldello+08

  39. AWM4 AND AGN FEEDBACK Cavagnolo+08

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

  41. NGC 5044 Gastaldello+09

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

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

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

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

  46. COLD FRONTS IN CLUSTERS Ascasibar & Markevitch 06

  47. COLD FRONTS IN CLUSTERS Markevitch & Vikhlinin 07

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

  49. NGC 5044 Gastaldello+09

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