J/A+A/672/A42 LoTSS-DR2 ICM dynamics (Zhang+, 2023)
The Planck clusters in the LOFAR sky. III.
LoTSS-DR2: Dynamic states and density fluctuations of the intracluster medium.
Zhang X., Simionescu A., Gastaldello F., Eckert D., Camillini L.,
Natale R., Rossetti M., Brunetti G., Akamatsu H., Botteon A., Cassano R.,
Cuciti V., Bruno L., Shimwell T. W., Jones A., Kaastra J. S., Ettori S.,
Brueggen M., de Gasperin F., Drabent A., R. van Weeren J.,
Roettgering H.J.A.
<Astron. Astrophys. 672, A42 (2023)>
=2023A&A...672A..42Z 2023A&A...672A..42Z (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; X-ray sources
Keywords: X-rays: galaxies: clusters - galaxies: clusters: general -
galaxies: clusters: intracluster medium - turbulence
Abstract:
The footprint of the recent second data release of the LOFAR Two-metre
Sky Survey (LoTSS-DR2) covers 309 Planck Sunyaev-Zeldovich (SZ)
selected galaxy clusters, 83 of which host a radio halo and 26 host a
radio relic(s). It provides an excellent opportunity to statistically
study the properties of extended cluster radio sources, especially
their connection with merging activities.
We quantify cluster dynamic states to investigate their relation with
the occurrence of extended radio sources. We also search for
connections between intracluster medium (ICM) turbulence and
nonthermal characteristics of radio halos in the LoTSS-DR2.
We analyzed XMM-Newton and Chandra archival X-ray data of all Planck
SZ clusters in the footprint of LoTSS-DR2. We computed concentration
parameters and centroid shifts that indicate the dynamic states of the
clusters. We also performed a power spectral analysis of the X-ray
surface brightness fluctuations to investigate large-scale density
perturbations and estimate the turbulent velocity dispersion.
Furthermore, we searched for the relation between radio halo power and
the turbulent dissipation flux channeled to particle acceleration.
The concentration parameters measured by the two telescopes agree
well, but the centroid shift has a larger scatter. The surface
brightness power spectral analysis results in a large scatter of the
surface brightness and density fluctuation amplitudes. We therefore
only found a marginal anticorrelation between density fluctuations and
cluster relaxation state, and we did not find a correlation between
density fluctuations and radio halo power. Nevertheless, the injected
power for particle acceleration calculated from turbulent dissipation
is correlated with the radio halo power, where the best-fit unity
slope supports the turbulent (re)acceleration scenario. Two different
acceleration models, transit-time damping and adiabatic stochastic
acceleration, cannot be distinguished due to the large scatter of the
estimated turbulent Mach number. We introduced a new quantity [k_T
YX]rRH, which is proportional to the turbulent acceleration power
assuming a constant Mach number. This quantity is strongly correlated
with radio halo power, where the slope is also unity.
Description:
This is an X-ray focused work of the paper series "The Planck clusters
in the LOFAR sky". We use archival XMM-Newton and Chandra data to
compute two morphological parameters, which are the concentration
parameter and the centroid shift for 150 (sub)clusters in the sample
of the this series.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 110 150 Full morphological parameters measured by
XMM-Newton and Chandra
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See also:
J/A+A/660/A78 : LoTSS-DR2 sample overview release (Botteon+, 2022)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Name PSZ2 cluster name (PSZ2 GLLL.ll+BB.bb)
21- 22 A2 --- Subcluster Position of the subcluster if there are
more than one X-ray detection (1)
25- 33 E9.4 --- cC ?=- Chandra concentration parameter
36- 44 E9.4 --- e_cC ?=- Chandra concentration parameter error
47- 55 E9.4 --- wC ?=- Chandra centroid shift
58- 66 E9.4 --- e_wC ?=- Chandra centroid shift error
69- 77 E9.4 --- cX ?=- XMM-Newton concentration parameter
80- 88 E9.4 --- e_cX ?=- XMM-Newton concentration parameter error
91- 99 E9.4 --- wX ?=- XMM-Newton centroid shift
102-110 E9.4 --- e_wX ?=- XMM-Newton centroid shift error
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Note (1): Positions as E, E1, E2, EN, ES, N, S, W, W1 or W2.
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Acknowledgements:
Xiaoyuan Zhang, xzhang(at)mpe.mpg.de
Refences:
Botteon et al., Paper I 2022A&A...660A..78B 2022A&A...660A..78B, Cat. J/A+A/660/A78
Bruno et al., Paper II 2023A&A...672A..41B 2023A&A...672A..41B
Cassano et al., Paper IV 2023A&A...672A..43C 2023A&A...672A..43C
(End) Patricia Vannier [CDS] 14-Oct-2022