A “MeerKAT-meets-LOFAR” study of the complex multi-component (mini-)halo in the extreme sloshing cluster Abell 2142

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Volume 686 (June 2024)

A&A, 686 (2024) A44

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Table 4.

Summary of our point-to-point correlation fit results for the large-scale halo in Abell 2142, performed using Linmix.

Image	Slope	Intrinsic	Spearman	Pearson
		scatter	coeff.	coeff.
	b	σ_int	r_S	r_P
1283 MHz (full)	$1 . 12_{- 0.05}^{+ 0.06}$ $1.12^{+0.06}_{-0.05}$	$0 . 021_{- 0.005}^{+ 0.007}$ $0.021^{+0.007}_{-0.005}$	0.91	0.91
143 MHz (full)	$0 . 76_{- 0.02}^{+ 0.02}$ $0.76^{+0.02}_{-0.02}$	$0 . 011_{- 0.002}^{+ 0.002}$ $0.011^{+0.002}_{-0.002}$	0.92	0.94

1283 MHz (matched)	$0 . 88_{- 0.05}^{+ 0.06}$ $0.88^{+0.06}_{-0.05}$	$0 . 017_{- 0.004}^{+ 0.005}$ $0.017^{+0.005}_{-0.004}$	0.91	0.91
143 MHz (matched)	$0 . 81_{- 0.05}^{+ 0.04}$ $0.81^{+0.04}_{-0.05}$	$0 . 011_{- 0.003}^{+ 0.003}$ $0.011^{+0.003}_{-0.003}$	0.94	0.93

α	$0 . 07_{- 0.03}^{+ 0.03}$ $0.07^{+0.03}_{-0.03}$	−	0.17	0.26

Notes. Relations were fitted between the X-ray surface brightness and either the radio surface brightness at the listed frequency or spectral index (each at 60 arcsec resolution) as indicated in the first column. Here b is the best-fit correlation slope, and r_S and r_P are the Spearman and Pearson correlation coefficients, respectively. The “full” fits were performed on the full region including upper limits, as presented in the upper row of Fig. 11; the “matched” fits were performed using only regions where both MeerKAT and LOFAR measure a surface brightness of at least 2σ, as described in the text.

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