PKS 1502+106: A high-redshift Fermi blazar at extreme angular resolution - Structural dynamics with VLBI imaging up to 86 GHz

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Table 2

Summary of the six observing epochs of PKS 1502 + 106 at 86 GHz observed with the GMVA.

Obs. Date	Array elements	S _peak ¹	rms²	S _total ³	b _maj ⁴	b _min ⁵	PA⁶
		(Jy beam^-1)	(mJy beam^-1)	(Jy)	(mas)	(mas)	(°)

2009-05-07^I	VLBA₈ + Pb + Pv + On + Ef	2.230	0.61	2.853	0.27	0.06	−3.9
2009-10-13^II	VLBA₈ + Pv + Pb + On + Ef	0.878	0.91	1.101	0.20	0.05	−5.2
2010-05-06^III	VLBA₇ (−Nl) + Pv + Pb + On + Mh + Ef	0.487	0.36	0.614	0.32	0.08	−10.4
2011-05-07^IV	VLBA₈ + Pv + Pb + On + Mh + Ef	0.762	0.53	0.875	0.29	0.07	−4.8
2011-10-09^V	VLBA₈ + Ys + Pv + On + Ef	0.571	1.67	0.652	0.20	0.07	−4.2
2012-05-17^VI	VLBA₇ (−Fd) + Ef + On + Pv + Ys	0.535	1.18	0.616	0.24	0.06	−5.8

Notes. Station designations: VLBA₈ is same as above; Ef – Effelsberg; Mh – Metsähovi; On – Onsala; Pb – Plateau de Bure (phased array); Pv – Pico Veleta; Ys – Yebes; and and Parameters listed above correspond to the final, uniformly weighted, untapered image. Labels I–VI correspond to the quasi-simultaneous data forming the spectra in Fig. 8 (see Sect. 3.4).

⁽¹⁾

peak flux density,

⁽²⁾

off-source rms noise,

⁽³⁾

total flux density of the MODELFIT image.

⁽⁴⁾

Major

⁽⁵⁾

minor axes along with the

⁽⁶⁾

position angle of the restoring beam.

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