2003A&A...412..373V


Query : 2003A&A...412..373V

2003A&A...412..373V - Astronomy and Astrophysics, volume 412, 373-385 (2003/12-3)

Measuring the cluster magnetic field power spectra from Faraday rotation maps of Abell 400, Abell 2634 and Hydra A.

VOGT C. and ENSSLIN T.A.

Abstract (from CDS):

We apply a novel technique of Faraday Rotation measure (RM) map analysis to three galaxy clusters, Abell 400, Abell 2634 and Hydra A, in order to estimate cluster magnetic field strengths, length scales and power spectra. This analysis - essentially a correlation analysis - is based on the assumption that the magnetic fields are statistically isotropically distributed across the Faraday screen. We investigate the difficulties involved in the application of the analysis to observational data. We derive magnetic power spectra for three clusters, i.e. Abell 400, Abell 2634 and Hydra A, and discuss influences on their shapes caused by the observational nature of the data such as limited source size and resolution. We successfully apply various tests to validate our assumptions. We show that magnetic fluctuations are probed on length scales ranging over at least one order of magnitude. Using this range for the determination of magnetic field strength of the central cluster gas yields 3µG in Abell 2634, 6µG in Abell 400 and 12µG in Hydra A as conservative estimates. The magnetic field autocorrelation length λB was determined to be 4.9kpc for Abell 2634, 3.6kpc for Abell 400 and 0.9kpc for Hydra A. We show that the RM autocorrelation length λRM is larger than the magnetic field autocorrelation length λB - for the three clusters studied, we found λRM≃2...4λB - and thus, they are not equal as often assumed in the literature. Furthermore, we investigate in a response analysis if it is possible to determine spectral slopes of the power spectra. We find that integrated numbers can be reliably determined from this analysis but differential parameters such as spectral slopes have to be treated differently. However, our response analysis results in spectral slopes of the power spectra of spectral indices α=1.6 to 2.0 suggesting that Kolmogorov spectra (α=5/3) are possible but flatter spectral slopes than α=1.3 can be excluded.

Abstract Copyright:

Journal keyword(s): radiation mechanism: non-thermal - galaxies: active - interplanetary medium - galaxies: cluster: general - radio continuum: general

Simbad objects: 14

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Number of rows : 14
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 ACO 119 ClG 00 56 08.57 -01 12 00.8           ~ 555 2
2 ACO 400 ClG 02 57 37.4 +06 00 45           ~ 399 3
3 3C 75 PaG 02 57 41.64 +06 01 28.0           ~ 300 1
4 ACO 514 ClG 04 47 40.0 -20 25 44           ~ 141 0
5 RXC J0450.0+4501 ClG 04 50 03.5 +45 01 27           ~ 40 1
6 NAME Hya A LIN 09 18 05.66848602 -12 05 43.8060823   14.38 14.8     ~ 1014 1
7 ACO 780 ClG 09 18 30 -12 15.7           ~ 453 0
8 NAME Hydra I Cluster ClG 10 36 36.0 -27 31 04           ~ 841 1
9 ACO 1656 ClG 12 59 44.40 +27 54 44.9           ~ 4816 2
10 ACO 1795 ClG 13 48 50.48 +26 35 07.4           ~ 1268 0
11 ClG J1411+5211 ClG 14 11 24.4 +52 12 38     20.11     ~ 118 3
12 NAME Cyg A Cluster ClG 19 59 30.3 +40 44 11           ~ 137 0
13 ACO 2634 ClG 23 38 18.4 +27 01 37           ~ 503 2
14 NGC 7720 Sy1 23 38 29.38324020 +27 01 53.2580084   13.9 13.3     ~ 542 4

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