2017A&A...603A.122G


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.18CET00:37:18

2017A&A...603A.122G - Astronomy and Astrophysics, volume 603A, 122-122 (2017/7-1)

Sardinia Radio Telescope observations of Abell 194. The intra-cluster magnetic field power spectrum.

GOVONI F., MURGIA M., VACCA V., LOI F., GIRARDI M., GASTALDELLO F., GIOVANNINI G., FERETTI L., PALADINO R., CARRETTI E., CONCU R., MELIS A., POPPI S., VALENTE G., BERNARDI G., BONAFEDE A., BOSCHIN W., BRIENZA M., CLARKE T.E., COLAFRANCESCO S., DE GASPERIN F., ECKERT D., ENSSLIN T.A., FERRARI C., GREGORINI L., JOHNSTON-HOLLITT M., JUNKLEWITZ H., ORRU E., PARMA P., PERLEY R., ROSSETTI M., TAYLOR G.B. and VAZZA F.

Abstract (from CDS):

Aims. We study the intra-cluster magnetic field in the poor galaxy cluster Abell 194 by complementing radio data, at different frequencies, with data in the optical and X-ray bands.
Methods. We analyzed new total intensity and polarization observations of Abell 194 obtained with the Sardinia Radio Telescope (SRT). We used the SRT data in combination with archival Very Large Array observations to derive both the spectral aging and rotation measure (RM) images of the radio galaxies 3C 40A and 3C 40B embedded in Abell 194. To obtain new additional insights into the cluster structure, we investigated the redshifts of 1893 galaxies, resulting in a sample of 143 fiducial cluster members. We analyzed the available ROSAT and Chandra observations to measure the electron density profile of the galaxy cluster.
Results. The optical analysis indicates that Abell 194 does not show a major and recent cluster merger, but rather agrees with a scenario of accretion of small groups, mainly along the NE-SW direction. Under the minimum energy assumption, the lifetimes of synchrotron electrons in 3C 40 B measured from the spectral break are found to be 157±11Myr. The break frequency image and the electron density profile inferred from the X-ray emission are used in combination with the RM data to constrain the intra-cluster magnetic field power spectrum. By assuming a Kolmogorov power-law power spectrum with a minimum scale of fluctuations of Λmin=1kpc, we find that the RM data in Abell 194 are well described by a magnetic field with a maximum scale of fluctuations of Λmax=(64±24)kpc. We find a central magnetic field strength of <B0≥(1.5±0.2)µG, which is the lowest ever measured so far in galaxy clusters based on Faraday rotation analysis. Further out, the field decreases with the radius following the gas density to the power of η=1.1±0.2. Comparing Abell 194 with a small sample of galaxy clusters, there is a hint of a trend between central electron densities and magnetic field strengths.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: clusters: general - galaxies: clusters: individual: Abell 194 - magnetic fields - large-scale structure of Universe - large-scale structure of Universe

Simbad objects: 41

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Number of rows : 41

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 ACO 119 ClG 00 56 16.8 -01 15 00           ~ 509 2
2 LBQS 0056-0009 Sy1 00 59 05.5145931113 +00 06 51.619894852   18.07 17.89 16.9   ~ 235 1
3 NGC 383 rG 01 07 24.95870 +32 24 45.2140   13.6 12.14     ~ 706 3
4 4C 01.02 QSO 01 08 38.7712667820 +01 35 00.318317679   18.54 18.39 19.05   ~ 457 1
5 NVSS J012401-013706 Rad 01 24 01.15 -01 37 06.5           ~ 1 0
6 NVSS J012406-005638 Rad 01 24 06.08 -00 56 38.4           ~ 1 0
7 NVSS J012410-013357 Rad 01 24 10.06 -01 33 57.3           ~ 1 0
8 NVSS J012426-005827 Rad 01 24 26.51 -00 58 27.6           ~ 1 0
9 NVSS J012431-010459 Rad 01 24 31.84 -01 04 59.8           ~ 1 0
10 NVSS J012438-011232 Rad 01 24 38.50 -01 12 32.4           ~ 1 0
11 NVSS J012450-012208 Rad 01 24 50.32 -01 22 08.0           ~ 1 0
12 XMMU J012513.0-012802 X 01 25 13.0 -01 28 02           ~ 3 0
13 QSO J0125-0005 QSO 01 25 28.8436590768 -00 05 55.930666802   16.92 16.64 16.30   ~ 249 1
14 NVSS J012538-011139 Rad 01 25 38.67 -01 11 39.2           ~ 1 0
15 NVSS J012542-005302 Rad 01 25 42.83 -00 53 02.1           ~ 1 0
16 NGC 541 IG 01 25 44.305 -01 22 46.19 13.42 13.03 12.08     ~ 187 2
17 NAME Minkowski's Object GiC 01 25 47.038 -01 22 18.48   16       ~ 58 1
18 NVSS J012557-005442 Rad 01 25 57.96 -00 54 42.4           ~ 1 0
19 NGC 545 BiC 01 25 59.21 -01 20 25.4   13.21 13.34     ~ 125 2
20 NGC 547 GiP 01 26 00.577 -01 20 42.43   13.16 13.34     ~ 312 3
21 ACO 194 ClG 01 26 01.3 -01 22 02           ~ 325 2
22 NVSS J012622-013756 Rad 01 26 22.50 -01 37 56.6           ~ 1 0
23 NVSS J012624-005101 Rad 01 26 24.50 -00 51 00.0           ~ 1 0
24 NVSS J012628-010418 Rad 01 26 28.40 -01 04 18.4           ~ 1 0
25 NVSS J012746-013446 Rad 01 27 46.46 -01 34 46.7           ~ 1 0
26 NVSS J012748-014134 Rad 01 27 48.18 -01 41 34.2           ~ 1 0
27 3C 48 QSO 01 37 41.2995845985 +33 09 35.079126038   16.62 16.20     ~ 2431 2
28 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3464 3
29 3C 129 rG 04 49 09.064 +45 00 39.40   19       ~ 242 2
30 ACO 523 ClG 04 59 01 +08 46.5           ~ 39 0
31 ICRF J052109.8+163822 Sy1 05 21 09.88592749 +16 38 22.0517668   19.37 18.84 18.480   ~ 726 1
32 ClG J0717+3745 ClG 07 17 36.50 +37 45 23.0           ~ 332 0
33 NAME Hya A LIN 09 18 05.651 -12 05 43.99   14.38 14.8     ~ 880 1
34 NAME Hydra I Cluster ClG 10 36 36.0 -27 31 04           ~ 764 1
35 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4108 2
36 3C 286 Sy1 13 31 08.2885060664 +30 30 32.960825108   17.51 17.25     ~ 3618 1
37 ACO 2199 ClG 16 28 37.0 +39 31 28           ~ 1084 1
38 NGC 6251 Sy2 16 32 31.96990024 +82 32 16.3999540 15.24 14.66 12.89 7.62   ~ 643 0
39 ACO 2255 ClG 17 12 50.04 +64 03 10.6           ~ 493 0
40 ACO 2382 ClG 21 51 57.2984 -15 36 48.067           ~ 108 0
41 UGC 12064 AGN 22 31 20.625 +39 21 29.81   14.6       ~ 415 1

    Equat.    Gal    SGal    Ecl

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2019.11.18-00:37:18

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