2013A&A...550A..92C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST22:09:52

2013A&A...550A..92C - Astronomy and Astrophysics, volume 550A, 92-92 (2013/2-1)

A multi-frequency study of the SZE in giant radio galaxies.

COLAFRANCESCO S., MARCHEGIANI P., DE BERNARDIS P. and MASI S.

Abstract (from CDS):

Radio galaxy (RG) lobes contain relativistic electrons embedded in a tangled magnetic field that produce, in addition to low-frequency synchrotron radio emission, inverse-Compton scattering (ICS) of the cosmic microwave background (CMB) photons. This produces a relativistic, non-thermal Sunyaev-Zel'dovich effect (SZE). We study the spectral and spatial properties of the non-thermal SZE in a sample of radio galaxies and make predictions for their detectability in both the negative and the positive part of the SZE, with space experiments like Planck, OLIMPO, and Herschel-SPIRE. These cover a wide range of frequencies, from radio to sub-mm. We model the SZE in a general formalism that is equivalent to the relativistic covariant one and describe the electron population contained in the lobes of the radio galaxies with parameters derived from their radio observations, namely, flux, spectral index, and spatial extension. We further constrain the electron spectrum and the magnetic field of the RG lobes using X-ray, gamma-ray, and microwave archival observations. We determine the main spectral features of the SZE in RG lobes, namely, the minimum, the crossover, and the maximum of the SZE. We show that these typical spectral features fall in the frequency ranges probed by the available space experiments. We provide the most reliable predictions for the amplitude and spectral shape of the SZE in a sample of selected RGs with extended lobes. In three of these objects, we also derive an estimate of the magnetic field in the lobe at the ~µG level by combining radio (synchrotron) observations and X-ray (ICS) observations. These data, together with the WMAP upper limits, set constraints on the minimum momentum of the electrons residing in the RG lobes and allow realistic predictions for the visibility of their SZE to be derived with Planck, OLIMPO, and Herschel-SPIRE. We show that the SZE from several RG lobes can be observed with mm and sub-mm experiments like Planck, OLIMPO, and Herschel-SPIRE, as well as with ground-based telescopes that have ≲ mJy sensitivity and sub-arcmin spatial resolution. These measurements will be crucial to disentangle the relativistic electron distribution from that of the magnetic field in RG lobes and to constrain the properties of their ICS emission, which is also visible at very high X-ray and gamma-ray energies.

Abstract Copyright:

Journal keyword(s): cosmology: theory - cosmic background radiation - galaxies: active

Simbad objects: 28

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Number of rows : 28

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 QSO B0205+350 BLL 02 08 38.1632218391 +35 23 12.802507619     19.24 18.8   ~ 88 0
2 3C 191 QSO 08 04 47.9666563347 +10 15 23.744155270   18.65 18.40     ~ 261 2
3 7C 093653.10+360601.00 Sy2 09 39 52.7593482853 +35 53 58.921088539   19.51 18.60     ~ 255 1
4 ICRF J114722.1+350107 Sy2 11 47 22.13056 +35 01 07.5226   17.89 16.83 10.26   ~ 149 1
5 B2 1158+35 Rad 12 00 49.1 +34 51 23           ~ 2 0
6 NGC 4261 LIN 12 19 23.2160630 +05 49 29.700024   13.92 12.87     ~ 1114 0
7 87GB 121815.5+635745 Rad 12 20 37 +63 41.1           ~ 1 0
8 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6207 3
9 3C 274.1 rG 12 35 31.00 +21 20 51.3   20       ~ 135 1
10 2MASX J13110466+2728070 Sy2 13 11 04.670 +27 28 07.24   18.93 18.00     ~ 187 1
11 4C 69.15 rG 13 13 58.854 +69 37 18.00           ~ 28 0
12 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 3995 3
13 4C 64.19 rG 13 50 42.04 +64 29 30.0   20.7 20.7 21.1   ~ 76 1
14 2MASS J14004343+3019185 BiC 14 00 43.436 +30 19 18.50           ~ 34 1
15 NVSS J140046+302106 Rad 14 00 46.00 +30 21 06.6           ~ 34 1
16 3C 294 rG 14 06 44.00 +34 11 25.0           ~ 216 1
17 ICRF J151640.2+001501 Sy1 15 16 40.21905831 +00 15 01.9089633   17.28 16.64 10.53   ~ 162 1
18 4C 51.31B Rad 15 21 14.55648 +51 05 00.8808   21.3       ~ 13 0
19 3C 326 Rad 15 52 26.60 +20 06 00.0   17.87 17.08     ~ 208 3
20 7C 1602+3739 Rad 16 04 23.4 +37 31 49           ~ 7 0
21 Mrk 1498 Sy1 16 28 04.0562531526 +51 46 31.483240761   17.0       ~ 82 0
22 B3 1636+418 Rad 16 37 53.4 +41 46 01           ~ 6 0
23 NAME Hercules A BiC 16 51 08.024 +04 59 34.91     18.25     ~ 432 1
24 NVSS J170301+421804 Rad 17 03 01.20 +42 18 04.7           ~ 3 1
25 ICRF J172320.7+341757 Sy1 17 23 20.7958592865 +34 17 57.966961854   15.58 15.46     ~ 281 1
26 8C 1834+620 Sy2 18 35 10.9 +62 04 08           ~ 43 2
27 2MAXI J2042+751 Sy1 20 42 37.3081453418 +75 08 02.444858560     14.46 13.80   ~ 210 0
28 3C 432.0 QSO 21 22 46.3256803670 +17 04 37.908511525   18.18 17.96     ~ 203 2

    Equat.    Gal    SGal    Ecl

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2020.07.03-22:09:52

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