X-RAY GROUPS WITH CHANDRA AND XMM: MASS, ENTROPY AND AGN HEATING

X-RAY GROUPS WITH X-RAY GROUPS WITH CHANDRA AND XMM: MASS, CHANDRA AND XMM: MASS, ENTROPY AND AGN HEATINGENTROPY AND AGN HEATING

FABIO GASTALDELLO

UC IRVINE & BOLOGNAD. BUOTE UCI

P. HUMPHREY UCI

L. ZAPPACOSTA UCI & TRIESTE

J. BULLOCK UCI

W. MATHEWS UCSC

F. BRIGHENTI UCSC & BOLOGNA

S. ETTORI BOLOGNA

1. MASS PROFILES FOR A SAMPLE OF X-RAY BRIGHT AND RELAXED GROUPS

2. ENTROPY PROFILES FOR THE SAME SAMPLE. RELEVANT SCALE FOR BREAKDOWN OF SELF-SIMILARITY

3. AGN FEEDBACK IN AN INTERESTING OBJECTS

4. PRELIMINARY RESULTS ON A FLUX-LIMITED SAMPLE

OUTLINE / MOTIVATIONOUTLINE / MOTIVATION

• 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 = -0.040.03, P05).

Vikhlinin et al. 2006Pointecouteau et al. 2005

Clusters X-ray resultsClusters X-ray results

THE PROJECTTHE 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 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

RESULTSRESULTS•After accounting for the mass of the hot gas, NFW + stars is the best fit model

MKW 4

NGC 533

STARS

GAS

DM

RESULTSRESULTS•No detection of stellar mass due to poor sampling in the inner 20 kpc or localized AGN disturbance

NGC 5044

Buote et al. 2002

c-M relation for groupsc-M relation for groups

We obtain a slope α=-0.2260.076, c decreases with M at the 3σ level

GAS FRACTIONSGAS FRACTIONS

GASTALDELLO ET AL. 2007

CLUSTERS

GROUPS

ENTROPY PROFILESENTROPY PROFILES

COMPARISON WITH MASSIVE CLUSTERS AND COMPARISON WITH MASSIVE CLUSTERS AND GRAVITATIONAL SIMULATIONSGRAVITATIONAL SIMULATIONS

PRATT ET AL. 2006

COMPARISON WITH MASSIVE CLUSTERS AND COMPARISON WITH MASSIVE CLUSTERS AND GRAVITATIONAL SIMULATIONSGRAVITATIONAL SIMULATIONS

AGN FEEDBACK IN GROUPSAGN FEEDBACK IN GROUPS

“UNFORTUNATELY, AGN HEATING IS NOT AS WELL STUDIED IN GROUPS AS IN CLUSTERS” (McNAMARA & NULSEN, ARAA).

NGC 5044 IS BRIGHT AND NEARBY (z=0.009). IDEAL TARGET TO STUDY AGN FEEDBACK.

NGC 5044 AGAIN …NGC 5044 AGAIN …

NGC 5044 AGAIN …NGC 5044 AGAIN …

CAON ET AL. 2000

DUST IN NGC 5044 DUST IN NGC 5044

TEMI, BRIGHENTI & MATHEWS 2007

NOGS (NORAS GROUP SAMPLE)NOGS (NORAS GROUP SAMPLE)

• Purely X-ray selected flux limited samples have been very effective in cluster studies (e.g.,Gioia+90,Edge+90,Rosati+95,Scharf+97,Vikhlinin+98,Romer+00,Bohringer+00) and they have follow-up studies with XMM or Chandra (REXCESS,400d2)

• Groups have been historically selected in the optical band, only one pioneering study of 8 groups from the ROSAT NEP survey (Henry+95)

• We used the NORAS catalogue:

1. 10h20m-14h region due to superior re-analysis

2. fx > 3x10-12 erg cm-2 s-1, completeness to better than 82%

3. Lx < 5x1043 erg s-1

• 15 objects, 5 in the archive, 10 observed with a Chandra LP (400ks, PI Buote)


A 1275

A 1142A 1185

A 1377


A 1314

NGC 4104

NGC 5129

RXJ 022


A 1177

RGH 80

SUMMARYSUMMARY

• DETAILED MASS PROFILES FOR A SAMPLE OF X-RAY BRIGHT GROUPS ARE WELL FITTED BY NFW+STARS. GAS FRACTIONS ARE LOWER AND WITH MORE SCATTER COMPARED TO CLUSTERS.

•BROKEN POWER LAW BEHAVIOR OF ENTROPY PROFILES POINTS TO MORE IMPORTANT LOCAL MODIFICATIONS (AGN).

•IT’S TIME TO STUDY AGN FEEDBACK IN GROUPS WITH MULTI-LAMBDA DATA. NGC 5044 CAN BE THE PERSEUS OF GROUPS.

•RESULTS FOR A COMPLETE X-RAY SELECTED, FLUX LIMITED SAMPLE COMING SOON. IT’S IMPORTANT TO HAVE ALSO XMM DATA TO GO TO LARGE RADII.

X-RAY GROUPS WITH CHANDRA AND XMM: MASS, ENTROPY AND AGN HEATING

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