TANAMI blazars in the IceCube PeV-neutrino fields | Astronomy & Astrophysics (A&A)

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Volume 566 (June 2014)

A&A, 566 (2014) L7

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Table 2

Details of interferometric observations and image parameters.

Source	ν	S_peak^a	σ_rms^a	S_total^a	T_B	Beam^a

0235−618	8.4	0.32	0.08	0.38	1.6	0.51 × 2.28, 5.8
		(0.35)	(0.06)	(0.37)		(4.85 × 7.70, −54.9)
0302−623	8.4	0.83	0.29	1.38	1.9	1.05 × 1.47, −2.8
	22.3	0.45	0.12	0.69	1.2	1.59 × 2.28, 87.6
0308−611	8.4	0.68	0.09	0.77	2.0	1.20 × 1.64, 38.8
		(0.73)	(0.05)	(0.77)		(3.89 × 4.49, −80.9)
	22.3	0.50	0.13	0.54	0.3	1.53 × 1.82, −75.9
1653−329	8.4	0.28	0.26	0.34	0.1	3.38 × 4.33, 86.8
	22.3	–^b	–^b	0.17^b		–^b
1714−336	8.4	0.74	0.36	1.27	0.02^c	3.26 × 3.98, 87.8
1759−396	8.4	1.63	0.18	2.01	3.1	0.64 × 2.70, 12.2
	22.3	1.12	0.18	1.19	0.2	1.47 × 4.32, 78.4

Notes. Columns: (1) IAU B1950 source name; (2) observing frequency in GHz; (3) peak flux density in Jy / beam; (4) image noise level in mJy / beam; (5) total flux density in Jy (uncertainties are ≲10% and ≲20% at 8.4 GHz and 22.3 GHz); (6) minimum core brightness temperature in 10¹¹ K and (7) restoring beam (size, position angle) in mas² and degree. ^cz = 0 assumed, affected by interstellar scattering broadening.

^(a)

Values in brackets denote the application of a Gaussian taper to the visibility data of 10% at a baseline length of 100 Mλ.

^(b)

One baseline experiment, flux density only accurate to ~50%.

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