A multi-frequency, multi-epoch radio continuum study of the Arches cluster with the Very Large Array

Open Access

Table 1

Spectral indices.

ID	$α_{X}^{04 / 10 / 16}$ $\[\alpha_{X}^{04 / 10 / 16}\]$	$α_{X}^{26 / 10 / 16}$ $\[\alpha_{X}^{26 / 10 / 16}\]$	$α_{X}^{11 / 04 / 18}$ $\[\alpha_{X}^{11 / 04 / 18}\]$	$α_{C}^{10 / 06 / 18}$ $\[\alpha_{C}^{10 / 06 / 18}\]$	α²⁰¹⁸	$α_{X}^{07 / 05 / 22}$ $\[\alpha_{X}^{07 / 05 / 22}\]$	$α_{C X}^{04 / 07 / 22}$ $\[\alpha_{C X}^{04 / 07 / 22}\]$	α²⁰²²
F6	0.01 ± 0.06	−0.02 ± 0.07	−0.09 ± 0.03	0.01 ± 0.04	−	−0.26 ± 0.05	−0.15 ± 0.02	−0.17 ± 0.12
F7	0.43 ± 0.04	0.48 ± 0.12	0.82 ± 0.08	0.79 ± 0.17	0.79 ± 0.24	1.08 ± 0.09	0.90 ± 0.04	0.92 ± 0.21
F19	−0.75 ± 0.27	−0.36 ± 0.17	−0.21 ± 0.19	−0.51 ± 0.12	−0.75 ± 0.14	−0.61 ± 0.15	−0.32 ± 0.06	−0.35 ± 0.15
F3	0.46 ± 0.17	0.83 ± 0.11	0.74 ± 0.17	0.54 ± 0.12	0.56 ± 0.17	0.40 ± 0.04	0.85 ± 0.10	0.84 ± 0.19
Dong19	0.56 ± 0.42	0.64 ± 0.10	0.88 ± 0.10	1.18 ± 0.05	0.68 ± 0.18	0.59 ± 0.10	0.80 ± 0.14	0.80 ± 0.18
F4	0.91 ± 0.21	0.60 ± 0.45	1.24 ± 0.13	−	1.02 ± 0.18	0.50 ± 0.16	0.66 ± 0.15	0.82 ± 0.19
F5	0.66 ± 0.06	0.54 ± 0.22	0.40 ± 0.08	0.82 ± 0.23	0.60 ± 0.17	0.89 ± 0.40	0.87 ± 0.12	0.85 ± 0.20
F8	0.25 ± 0.14	0.69 ± 0.32	0.96 ± 0.32	−	0.44 ± 0.41	0.48 ± 0.06	1.10 ± 0.08	0.67 ± 0.54
Dong96	0.98 ± 0.74	0.50 ± 0.21	0.87 ± 0.15	−	0.73 ± 0.21	1.51 ± 0.15	0.76 ± 0.14	0.79 ± 0.23
F1	0.58 ± 0.46	0.70 ± 0.61	−0.52 ± 0.50	0.62 ± 0.35	1.02 ± 0.33	0.71 ± 0.22	0.34 ± 0.14	0.93 ± 0.37
F18	−0.45 ± 0.32^(*)	−	0.04 ± 0.29	−0.02 ± 0.13	−	−0.39 ± 0.15	−	−0.32 ± 0.49
F26	−1.01 ± 0.14	0.07 ± 0.29	−0.20 ± 0.17	−	−	−0.22 ± 0.15	−	−
F2	0.34 ± 0.49	0.94 ± 0.19	0.71 ± 0.76	−	0.58 ± 0.23	−0.07 ± 0.32	0.49 ± 0.18	0.45 ± 0.34
F9	0.72 ± 0.41	0.95 ± 0.26	0.78 ± 0.36^(*)	−	1.17 ± 0.36	0.63 ± 0.34	0.81 ± 0.24	1.03 ± 0.42
F12	−0.27 ± 0.51	−	0.22 ± 0.38	−	0.59 ± 0.37	−	−	0.32 ± 0.38
B1	−	−	−	−	0.92 ± 0.49	−	−	0.70 ± 0.53
F14	−	−	−	−	−1.59 ± 0.47	−	−	0.70 ± 0.62
F55	−	−	−	−	−1.15 ± 0.90	−	−	−0.86 ± 0.81

Notes. ^(*)These values were obtained using the peak flux from each sub-image. Due to relatively high S/N, the Gaussian fits did not match the synthesised beam in some sub-images, which resulted in a flux overestimation while performing the least-squares fit.

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