2018A&A...617A..11G


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST08:16:49

2018A&A...617A..11G - Astronomy and Astrophysics, volume 617A, 11-11 (2018/9-1)

Radio-continuum surveys with SKA and LOFAR: a first look at the perspectives for radio mini-halos.

GITTI M., BRUNETTI G., CASSANO R. and ETTORI S.

Abstract (from CDS):


Context. Diffuse synchrotron radio emission has been observed in a number of cool-core clusters on scales comparable to that of the cooling region. These radio sources are called "mini-halos". In order to understand their origin, which is still unclear, joint radio and X-ray statistical studies of large cluster samples are necessary to investigate the radio mini-halo properties and their connection with the cluster thermodynamics.
Aims. We here extend our previous explorative study and investigate the perspectives offered by surveys in the radio continuum with the LOw Frequency ARray (LOFAR) and the Square Kilometre Array (SKA), in particular examining the effect of the intracluster magnetic field in the mini-halo region for the first time.
Methods. By considering the minimum flux detectable in radio surveys and exploiting the Pradio-LX correlation observed for known mini-halos, we estimate the detection limits achievable by future radio observational follow-up of X-ray cluster samples, such as HIFLUGCS and eROSITA. This allows us to estimate the maximum number of radio mini-halos that can potentially be discovered in future surveys as a function of redshift and magnetic field strength.
Results. Under the optimistic assumption that all cool-core systems host a mini-halo and that the radio versus X-ray scaling relation extends to systems with lower X-ray luminosity, we show that future radio surveys with LOFAR and SKA1 (at ∼140MHz and ∼1.4GHz) have the potential to discover ∼1000-10000 radio mini-halo candidates up to redshift z=1. This shows that these surveys may be able to produce a breakthrough in the study of these sources. We further note that future SKA1 radio surveys at redshift z>0.6 will allow us to distinguish between different magnetic fields in the mini-halo region, because higher magnetic fields are expected to produce more powerful mini-halos, thus implying a larger number of mini-halo candidates detected at high redshift. For example, the non-detection with SKA1 of mini-halos at z>0.6 will suggest a low magnetic field (B < few µG). The synergy of these radio surveys with future X-ray observations and theoretical studies is essential in establishing the radio mini-halo physical nature.

Abstract Copyright: © ESO 2018

Journal keyword(s): galaxies: clusters: general - radio continuum: galaxies - X-rays: galaxies: clusters

Simbad objects: 16

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Number of rows : 16

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 426 ClG 03 19 47.2 +41 30 47           ~ 1939 1
2 ZwCl 0335+0956 ClG 03 38 35.3 +09 57 54           ~ 343 1
3 ACO 478 ClG 04 13 20.7 +10 28 35           ~ 467 0
4 ClG J0947+7623 ClG 09 47 12.9 +76 23 13           ~ 129 1
5 ZwCl 1021+0426 ClG 10 23 39.0 +04 11 14   15.6       ~ 250 0
6 ClG J1347-1145 ClG 13 47 33.5 -11 45 42           ~ 469 0
7 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 621 1
8 ZwCl 1455+2232 ClG 14 57 15.2 +22 20 30     18.62     ~ 262 0
9 ClG J1504-0248 ClG 15 04 07.4 -02 48 15           ~ 150 0
10 ACO 2029 ClG 15 10 58.7 +05 45 42           ~ 852 0
11 LEDA 1900245 Bla 15 32 53.780 +30 20 59.41   19.1   15.7   ~ 128 0
12 ACO 2204 ClG 16 32 45.7 +05 34 43           ~ 398 0
13 NAME Oph Cluster ClG 17 12 24.7 -23 21 01           ~ 240 0
14 ClG J1720+2638 ClG 17 20 09.6 +26 37 35           ~ 205 0
15 ACO 2390 ClG 21 53 34.6 +17 40 11           ~ 625 2
16 NAME Phoenix Cluster ClG 23 44 40.9 -42 41 54           ~ 122 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-08:16:49

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