2004A&A...413..415K


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.18CEST06:57:13

2004A&A...413..415K - Astronomy and Astrophysics, volume 413, 415-439 (2004/1-2)

Spatially resolved X-ray spectroscopy of cooling clusters of galaxies.

KAASTRA J.S., TAMURA T., PETERSON J.R., BLEEKER J.A.M., FERRIGNO C., KAHN S.M., PAERELS F.B.S., PIFFARETTI R., BRANDUARDI-RAYMONT G. and BOEHRINGER H.

Abstract (from CDS):

We present spatially resolved X-ray spectra taken with the EPIC cameras of XMM-Newton of a sample of 17 cooling clusters and three non-cooling clusters for comparison. The deprojected spectra are analyzed with a multi-temperature model, independent of any a priori assumptions about the physics behind the cooling and heating mechanisms. All cooling clusters show a central decrement of the average temperature, most of them of a factor of ∼2. Three clusters (Sersic 159-3, MKW 3s and Hydra A) only show a weak temperature decrement, while two others (A 399 and A 2052) have a very strong temperature decrement. All cooling clusters show a weak pressure gradient in the core. More important, at each radius within the cooling region the gas is not isothermal. The differential emission measure distribution shows a strong peak near the maximum (ambient) temperature, with a steep decline towards lower temperatures, approximately proportional to T3, or alternatively a cut-off at about a quarter to half of the maximum temperature. In general, we find a poor correlation between radio flux of the central galaxy and the temperature decrement of the cooling flow. This is interpreted as evidence that except for a few cases (like the Hydra A cluster) heating by a central AGN is not the most common cause of weak cooling flows. We investigate the role of heat conduction by electrons and find that the theoretically predicted conductivity rates are not high enough to balance radiation losses. The differential emission measure distribution has remarkable similarities with the predictions from coronal magnetic loop models. Also the physical processes involved (radiative cooling, thermal conduction along the loops, gravity) are similar for clusters loops and coronal loops. If coronal loop models apply to clusters, we find that a few hundred loops per scale height should be present. The typical loop sizes deduced from the observed emission measure distribution are consistent with the characteristic magnetic field sizes deduced from Faraday rotation measurements.

Abstract Copyright:

Journal keyword(s): galaxies: clusters: general - cooling flows - X-rays: galaxies: clusters

CDS comments: Table 12 : A 1835-1 = [AEF92] ACO 1835 1.

Simbad objects: 40

goto Full paper

goto View the reference in ADS

Number of rows : 40

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NGC 533 GiG 01 25 31.432 +01 45 33.57   13.1 14.11     ~ 203 0
2 NGC 708 BiC 01 52 46.482 +36 09 06.53 14.85 14.27 13.29 12.67 12.09 ~ 206 3
3 ACO 262 ClG 01 52 50.4 +36 08 46           ~ 645 1
4 UGC 2438 BiC 02 57 53.087 +13 01 50.87   16.5       ~ 17 0
5 ACO 399 ClG 02 57 56.4 +13 00 59           ~ 335 0
6 ACO 3112 ClG 03 17 52.4 -44 14 35           ~ 283 1
7 ESO 248-6 QSO 03 17 57.6794446 -44 14 17.165338   14.85   13.16   ~ 60 3
8 ACO 426 ClG 03 19 47.2 +41 30 47           ~ 1882 1
9 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3460 3
10 ZwCl 0335+0956 ClG 03 38 35.3 +09 57 54           ~ 338 1
11 2MASX J03384056+0958119 LIN 03 38 40.568 +09 58 11.94   16.5       ~ 34 1
12 ACO 3266 ClG 04 31 11.9 -61 24 23           ~ 363 0
13 ESO 118-30 IG 04 31 12.8 -61 27 09           ~ 18 1
14 ACO 496 ClG 04 33 30.3838 -13 14 21.584           ~ 653 2
15 NAME A496cD BiC 04 33 37.841 -13 15 43.04   13.95 14.22     ~ 88 1
16 ACO 754 ClG 09 08 50.1 -09 38 12           ~ 628 1
17 2MASX J09091923-0941591 BiC 09 09 19.233 -09 41 59.13   14   14.05   ~ 24 0
18 NAME Hya A LIN 09 18 05.651 -12 05 43.99   14.38 14.8     ~ 878 1
19 NAME Hydra I Cluster ClG 10 36 36.0 -27 31 04           ~ 763 1
20 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5644 0
21 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6025 3
22 NGC 4874 LIN 12 59 35.709 +27 57 33.80 13.01 13.7 11.40 12.122 11.386 ~ 699 3
23 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4096 2
24 MCG+05-33-005 LIN 13 48 52.511 +26 35 34.84   14.0       ~ 217 2
25 ACO 1795 ClG 13 49 00.5 +26 35 07           ~ 1134 0
26 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 611 1
27 NAME SMM J14010+0252 Sy1 14 01 02.0854024806 +02 52 42.389426039   19.3       ~ 39 2
28 ACO 1837 ClG 14 01 36.2 -11 07 48           ~ 98 0
29 2MASX J14013635-1107431 BiC 14 01 36.350 -11 07 43.17   14.87   13.48   ~ 20 0
30 ACO 2029 ClG 15 10 58.7 +05 45 42           ~ 835 0
31 UGC 9799 Sy2 15 16 44.4894653562 +07 01 17.830884159   15.19 14.17     ~ 409 3
32 ACO 2052 ClG 15 16 45.5 +07 00 01           ~ 664 1
33 NAME NGC 5920 Group ClG 15 21 50.7 +07 42 18     15.13     ~ 281 0
34 NGC 5920 LIN 15 21 51.870 +07 42 31.97   15.5       ~ 110 1
35 BAX 233.1222+04.6817 ClG 15 32 29.3 +04 40 54     15.13     ~ 58 0
36 UGC 9886 GiG 15 32 32.014 +04 40 51.64   15.3       ~ 24 1
37 ACO S 1101 ClG 23 13 58.5 -42 43 39           ~ 228 1
38 ESO 291-9 BiC 23 13 58.630 -42 43 39.31   14.68 14.6 14.537   ~ 46 3
39 ACO 4059 ClG 23 56 40.7 -34 40 18           ~ 345 1
40 ESO 349-10 QSO 23 57 00.689 -34 45 33.18   13.89 13.26 12.19   ~ 117 2

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2004A&A...413..415K and select 'bookmark this link' or equivalent in the popup menu


2019.10.18-06:57:13

© Université de Strasbourg/CNRS

    • Contact