Study of solar brightness profiles in the 18–26 GHz frequency range with INAF radio telescopes - II. Evidence of coronal emission

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This article has an erratum: [https://doi.org/10.1051/0004-6361/202450907e]

Table 3.

Values of the modelled secondary lobe A₂ of the hypothetical beam patterns needed to fit the observed tails in the range 18–26 GHz with Grueff and SRT radio telescopes, in the assumption of ECB/CCBH solar models.

Frequency	Instrument	Model	R_c	R_eq	R_pol	A₂	ΔA
(GHz)			(arcsec)	(arcsec)	(arcsec)	(dBi)	(dBi)
18.3	Grueff	ECB	–	$991 . 7_{- 2.9}^{+ 6.1}$ $991.7^{+6.1}_{-2.9}$	$987 . 6_{- 2.8}^{+ 3.1}$ $987.6^{+3.1}_{-2.8}$	$58 . 8_{- 0.8}^{+ 1.0}$ $58.8^{+1.0}_{-0.8}$	5.8
18.3	Grueff	CCBH	$982 . 7_{- 1.8}^{+ 2.0}$ $982.7^{+2.0}_{-1.8}$	–	–	$60 . 6_{- 0.6}^{+ 0.6}$ $60.6^{+0.6}_{-0.6}$	7.6

18.8	SRT	ECB	–	$980 . 3_{- 0.6}^{+ 2.7}$ $980.3^{+2.7}_{-0.6}$	$981 . 8_{- 0.6}^{+ 3.5}$ $981.8^{+3.5}_{-0.6}$	$65 . 5_{- 0.4}^{+ 0.2}$ $65.5^{+0.2}_{-0.4}$	4.1
18.8	SRT	CCBH	$979 . 3_{- 0.8}^{+ 0.7}$ $979.3^{+0.7}_{-0.8}$	–	–	$66 . 5_{- 0.3}^{+ 0.2}$ $66.5^{+0.2}_{-0.3}$	5.1

24.7	SRT	ECB	–	$978 . 7_{- 0.4}^{+ 0.5}$ $978.7^{+0.5}_{-0.4}$	$979 . 6_{- 1.8}^{+ 1.3}$ $979.6^{+1.3}_{-1.8}$	$67 . 0_{- 0.4}^{+ 0.3}$ $67.0^{+0.3}_{-0.4}$	6.2
24.7	SRT	CCBH	$977 . 6_{- 2.0}^{+ 1.4}$ $977.6^{+1.4}_{-2.0}$	–	–	$67 . 4_{- 0.3}^{+ 0.1}$ $67.4^{+0.1}_{-0.3}$	6.6

25.8	Grueff	ECB	–	$989 . 8_{- 2.9}^{+ 4.2}$ $989.8^{+4.2}_{-2.9}$	$987 . 4_{- 1.5}^{+ 1.3}$ $987.4^{+1.3}_{-1.5}$	$60 . 2_{- 1.0}^{+ 0.9}$ $60.2^{+0.9}_{-1.0}$	12.2
25.8	Grueff	CCBH	$977 . 1_{- 1.3}^{+ 1.5}$ $977.1^{+1.5}_{-1.3}$	–	–	$62 . 2_{- 0.4}^{+ 0.6}$ $62.2^{+0.6}_{-0.4}$	14.2

Notes. We report also the difference between the modelled and the real values ΔA = A₂ − a₂, and the values of the mean, equatorial, and polar radii of the Sun (R_c, R_eq, and R_pol).

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