Cosmic dance in the Shapley Concentration Core - II. The uGMRT-MeerKAT view of filaments in the brightest cluster galaxies and tailed radio galaxies in the A3528 cluster complex

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Volume 694 (February 2025)

A&A, 694 (2025) A28

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Table 5.

Halo-FDCA elliptical fitting results, as well as the ‘manual’ flux densities.

Frequency	Central brightness	Major e-folding radius	Minor e-folding radius	Goodness fit	Fitted flux density	Image flux density	Fitted radio power	Image radio power
ν [MHz]	I₀ [μJy arcsec⁻²]	r_e, 1 [kpc]	r_e, 2 [kpc]	χ²/dof	S_{< 3re} [mJy]	S_img [mJy]	P_{< 3re} [W Hz⁻¹]	P_img [W Hz⁻¹]
410	6.2 ± 0.4	$83 . 9_{- 4.8}^{+ 5.1}$ $83.9^{+5.1}_{-4.8}$	$57 . 6_{- 3.2}^{+ 3.4}$ $57.6^{+3.4}_{-3.2}$	922.13/891	158.9 ± 7.8	185.7 ± 15.1	(9.5 ± 0.5)×10²³	(1.1 ± 0.1)×10²⁴
700	3.4 ± 0.2	$127 . 6_{- 8.9}^{+ 9.6}$ $127.6^{+9.6}_{-8.9}$	48.6 ± 4.0	742.65/683	111.9 ± 8.2	66.1 ± 3.6	(6.7 ± 0.5)×10²³	(4.1 ± 0.2)×10²³
1284	N/A	N/A	N/A	N/A	76.3 ± 15.0 ^( † )	8.4 ± 1.0	(4.1 ± 0.2)×10²³	(5.2 ± 0.6)×10²²

Notes. ^( † )Flux density extrapolated from the flux densities at 410 MHz and 700 MHz. The image flux density was calculated subtracting the flux density within the white solid lines in Fig. 14 from a region surrounding the candidate mini halo (dashed line in Fig. 14). Uncertainties were estimated summing in quadrature the uncertainties of each flux desnity (i.e. ‘total’ and ‘masked’) following Eq. (1).

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