J/A+A/695/A215 MaDCoWS clusters richness (Di Gennaro+, 2025)
Limits and challenges of the detection of cluster-scale diffuse radio emission
at high redshift The Massive and Distant Clusters of WISE Survey (MaDCoWS)
in LoTSS-DR2.
Di Gennaro G., Bruggen M., Moravec E., Di Mascolo L., Van Weeren R.J.,
Brunetti G., Cassano R., Botteon A., Churazov E., Khabibullin I.,
Lyskova N., De Gasperin F., Hardcastle M.J., Rottgering H.J.A.,
Shimwell T., Sunyaev R., Stanford A.
<Astron. Astrophys. 695, A215 (2025)>
=2025A&A...695A.215D 2025A&A...695A.215D (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Radio sources ; Redshifts
Keywords: radiation mechanisms: non-thermal - galaxies: clusters: general -
galaxies: clusters: intracluster medium -
large-scale structure of Universe
Abstract:
Diffuse radio emission in galaxy clusters is a tracer of
ultra-relativistic particles and uG-level magnetic fields, and is
thought to be triggered by cluster merger events. In the distant
Universe (i.e. z>0.6), such sources have been observed only in a
handful of systems, and their study is important to understand the
evolution of large-scale magnetic fields over the cosmic time.
Previous studies of nine Planck clusters up to z∼0.9 suggest a
fast amplification of cluster-scale magnetic fields, at least up to
half of the current Universe's age, and steep spectrum cluster scale
emission, in line with particle re-acceleration due to turbulence. In
this paper, we investigate the presence of diffuse radio emission in a
larger sample of galaxy clusters reaching even higher redshifts (i.e.
z?∼1). We selected clusters from the Massive and Distant
Clusters of WISE Survey (MaDCoWS) with richness λ15>40 covering
the area of the second data release of the LOFAR Two-Meter Sky Survey
(LoTSS-DR2) at 144MHz. These selected clusters are in the redshift
range 0.78-1.53 (with a median value of 1.05). We detect the
possible presence of diffuse radio emission, with the largest linear
sizes of 350-500kpc, in five out of the 56 clusters in our
sample. If this diffuse radio emission is due to a radio halo, these
radio sources lie on or above the scatter of the PV-M500
radio halo correlations (at 150MHz and 1.4GHz) found at z<0.6,
depending on the mass assumed. We also find that these radio sources
are at the limit of the detection by LoTSS, and therefore deeper
observations are important for future studies.
Description:
Final sample spans a wide photometric redshift range, that is
0.78≤z≤1.53 (median (zLoTSS∼1.05), and richness, that is
40<λ15<74.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 94 64 List of MaDCoWS clusters (Gonzalez et al.,
2019ApJS..240...33G 2019ApJS..240...33G, Cat. J/ApJS/240/33) in
LOFAR-DR2 (Shimwell et al., 2022A&A...659A...1S 2022A&A...659A...1S,
Cat. J/A+A/659/A1) with richness λ15>40
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See also:
J/ApJS/240/33 : MaDCoWS. I. Catalog of z∼1 galaxy clusters (Gonzalez+, 2019)
J/A+A/659/A1 : LOFAR Two-metre Sky Survey (LoTSS) DR2 (Shimwell+, 2022)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Cluster Cluster name (MOO), JHHMM+DDMM (1)
12- 15 F4.2 --- z Redshift (1)
18- 22 F5.3 --- zsp ? Spectroscopic redshift
25- 33 F9.5 deg RAdeg Right ascension (J2000) (1)
35- 42 F8.5 deg DEdeg Declination (J2000) (1)
44- 45 I2 --- lambda15 Richness (1)
47 I1 --- e_lambda15 Richness error (1)
49- 51 F3.1 10+14Msun M500 Cluster mass (2)
52 A1 --- --- [+]
53- 55 F3.1 10+14Msun e_M500 Cluster mass error (lower value)
56 A1 --- n_M500 [*] *: masses obtained from CARMA
observations (Decker et al.,
2019ApJ...878...72D 2019ApJ...878...72D)
57 A1 --- --- [+]
58- 60 F3.1 10+14Msun e1_M500 ? Cluster mass error (lower value)
63 A1 --- --- [-]
64- 66 F3.1 10+14Msun E_M500 ? Cluster mass error (upper value)
68 A1 --- --- [-]
69- 71 F3.1 10+14Msun E1_M500 ? Cluster mass error (upper value)
74- 78 E5.3 uJy/beam Mnoisefull Map noise of the full-resolution
80- 85 E6.3 uJy/beam Mnoiselow Map noise of the low-resolution
87 A1 --- l_S144MHz Limit flag on S144MHz
88- 90 F3.1 mJy S144MHz ?=- Flux density at 144MHz
92- 94 F3.1 mJy e_S144MHz ? Flux density at 144MHz
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Note (1): as reported in Gonzalez et al. (2019ApJS..240...33G 2019ApJS..240...33G,
Cat. J/ApJS/240/33G), MOO JHHMM+DDMM in Simbad
Note (2): column: cluster masses retrieved using the mass-richness scaling
relation (M500 - λ15; see Orlowski-Scherer et al.,
2021A&A...653A.135O 2021A&A...653A.135O, Cat. J/A+A/653/A135)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 29-Jul-2025