The Atacama Cosmology Telescope: Observations of supermassive black hole binary candidates - Strong sinusoidal variations at 95, 147, and 225 GHz in PKS 2131–021 and PKS J0805–0111

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Table 5.

Power-law fits to the frequency–phase relation (Eq. (4)) at select ranges of radio and mm frequencies.

AGN	Data Sets	Span	b	a	χ²/d.o.f.	PTE
		(GHz)		(cycles GHz⁻¹)
PKS 2131–021	Haystack, OVRO, ALMA, ACT	3–345	$- 0 . 3_{- 0.1}^{+ 0.1}$ $-0.3^{+0.1}_{-0.1}$	$0 . 396_{- 0.001}^{+ 0.09}$ $0.396^{+0.09}_{-0.001}$	13.3/7	0.07
PKS 2131–021	Haystack, OVRO, ALMA, ACT	3–225	$- 0 . 46_{- 0.09}^{+ 0.1}$ $-0.46^{+0.1}_{-0.09}$	$0 . 44_{- 0.04}^{+ 0.06}$ $0.44^{+0.06}_{-0.04}$	1.01/6	0.99
PKS 2131–021	OVRO, ACT	15–225	$- 0 . 8_{- 0.6}^{+ 0.1}$ $-0.8^{+0.1}_{-0.6}$	$0 . 8_{- 0.2}^{+ 2}$ $0.8^{+2}_{-0.2}$	0.21/1	0.65
PKS J0805–0111	OVRO, ACT	15–225	$- 0 . 7_{- 0.4}^{+ 0.2}$ $-0.7^{+0.2}_{-0.4}$	$1 . 2_{- 0.3}^{+ 2}$ $1.2^{+2}_{-0.3}$	0.22/1	0.64

Notes. Uncertainties are 68% credible intervals.

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