Parsec-scale HI outflows in powerful radio galaxies

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Volume 647 (March 2021)

A&A, 647 (2021) A63

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Table 1.

Properties of observations.

Source	z	Array ^(a)	Code ^(b)	Date	ν_obs^(c)	T_obs^(d)	Pol. ^(e)	Correlator pass	IFs	BW ^(f)	N_ch^(g)	Δν^(h)
				[GHz]	[min]				[MHz]		[kHz]
3C 293	0.045	EVN+VLBA+Ar	GN002A	2015-03-02	1.36	500	Dual	Continuum	4	16	32	500
								Spectral-line	1	16	512	31.25
4C 52.37	0.106	EVN+VLBA+Ar	GN002C	2015-10-15	1.28	500	Dual	Continuum	4	16	32	500
								Spectral-line	1	16	512	31.25

Notes.

^(a)

Array used for observation. EVN: Effelsberg (Germany), phased-up Westerbork (Five stations, Netherlands), Jodrell-Bank (United Kingdom), Onsala (Sweden); VLBA (USA): Los Alamos (NM), Kitt Peak (AZ), St. Croix (VI), Mauna Kea (HI), Hancock (NH), Brewster (WA), Fort Davis (TX), North Liberty (IA), Pie Town (NM), Owens Valley (CA); Ar: Arecibo (Puerto Rico).

^(b)

Experiment code.

^(c)

Observing frequency.

^(d)

Observing time. For the VLBI experiment, this represents the total on-source time of the whole array.

^(e)

Polarization: dual denotes that two polarization were used (LL and RR).

^(f)

Bandwidth (of each IF).

^(g)

Number of channels in a single band or IF.

^(h)

Channel width in frequency.

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