Table 1: GPS sources. Columns 1 through 13 provide source name, optical identification (G: galaxy, Q: quasar, EF: empty field), optical magnitude ("V'',"R'' are the bands in the optical, "r'' band-defined by Stanghellini et al. 1993), redshift (those with * are a photometric estimate by Heckman et al. 1994), linear scale factor pc/mas [ $H_{0}=100~ h~ \rm km~s^{-1}~ Mpc^{-1}$ and q₀=0.5 have been assumed], maximum VLBI angular size fromPapers I, II or this observation, maximum VLBI linear size, 5 GHz total flux density measured at Effelsberg, low frequency spectral index, high frequency spectral index, turnover frequency, peak flux density and references for the spectral information (Refs. 1, de Vries et al. 1997; 2, Stanghellini et al. 1998; 3, Dallacasa et al. 2000; 4, O'Dea et al. 1996; 5, Spoelstra et al. 1985).

1
2 3 4 5 6 7 8 9 10 11 12 13

Source
id mag z pc/mas $\theta$ L $S_{\rm {Ef}}$ $\alpha_{\rm l}$ $\alpha_{\rm h}$ $\nu_{\rm m}$ $S_{\rm m}$ Refs.

[mas] [pc] [Jy] [GHz] [Jy]

0554-026
G 18.5V 0.235 2.37 h^-1 30 71 h^-1 -1.07 0.63 1.0 0.8 1

0914+114
G 20.0r 0.178 1.95 h^-1 150 293 h^-1 0.11 -0.1 1.6 0.3 2.3 2

1133+432
EF 40 0.45 -0.60 0.6 1.0 1.4 1

1333+589
EF 20 0.67 -0.84 0.52 4.9 0.73 3

1433-040
G 22.3r 20 4, 5

1509+054
G 16.2V 0.084 1.06 h^-1 17 18 h^-1 -1.72 0.46 11 0.77 3

1518+046
Q 22.2R 1.296 4.3 h^-1 160 688 h^-1 1.06 -0.6 1.3 0.9 4.58 2

1751+278
G 21.7R 0.86* 4.2 h^-1 50 210 h^-1 -0.27 0.57 1.4 0.6 1

1824+271
G? 22.9R 45 -0.39 0.75 1.0 0.4 1

2121-014
G 23.3R 1.158 4.3 h^-1 88 378 h^-1 -0.56 0.75 0.5 1.8 1

2322-040
G 23.5R 65 -0.42 0.75 1.4 1.3 1

2323+790
G 19.5V 32 0.43 -0.3 0.75 1.4 1.2 1

DA193
Q 18.0V 2.365 4.0 h^-1 4 16 h^-1 -1.6 0.6 9.5 7.8 2

OQ208
G 14.6r 0.077 1.0 h^-1 10 10 h^-1 -1.5 1.6 4.9 2.76 2

**Table 1:** GPS sources. Columns 1 through 13 provide source name, optical identification (G: galaxy, Q: quasar, EF: empty field), optical magnitude ("V'',"R'' are the bands in the optical, "r'' band-defined by Stanghellini et al. 1993), redshift (those with * are a photometric estimate by Heckman et al. 1994), linear scale factor pc/mas [ $H_{0}=100~ h~ \rm km~s^{-1}~ Mpc^{-1}$ and q₀=0.5 have been assumed], maximum VLBI angular size fromPapers I, II or this observation, maximum VLBI linear size, 5 GHz total flux density measured at Effelsberg, low frequency spectral index, high frequency spectral index, turnover frequency, peak flux density and references for the spectral information (Refs. 1, de Vries et al. 1997; 2, Stanghellini et al. 1998; 3, Dallacasa et al. 2000; 4, O'Dea et al. 1996; 5, Spoelstra et al. 1985).
1	2	3	4	5	6	7	8	9	10	11	12	13
Source	id	mag	z	pc/mas	$\theta$	L	$S_{\rm {Ef}}$	$\alpha_{\rm l}$	$\alpha_{\rm h}$	$\nu_{\rm m}$	$S_{\rm m}$	Refs.
					[mas]	[pc]	[Jy]			[GHz]	[Jy]
0554-026	G	18.5V	0.235	2.37 h^-1	30	71 h^-1		-1.07	0.63	1.0	0.8	1
0914+114	G	20.0r	0.178	1.95 h^-1	150	293 h^-1	0.11	-0.1	1.6	0.3	2.3	2
1133+432	EF				40		0.45	-0.60	0.6	1.0	1.4	1
1333+589	EF				20		0.67	-0.84	0.52	4.9	0.73	3
1433-040	G	22.3r			20							4, 5
1509+054	G	16.2V	0.084	1.06 h^-1	17	18 h^-1		-1.72	0.46	11	0.77	3
1518+046	Q	22.2R	1.296	4.3 h^-1	160	688 h^-1	1.06	-0.6	1.3	0.9	4.58	2
1751+278	G	21.7R	0.86*	4.2 h^-1	50	210 h^-1		-0.27	0.57	1.4	0.6	1
1824+271	G?	22.9R			45			-0.39	0.75	1.0	0.4	1
2121-014	G	23.3R	1.158	4.3 h^-1	88	378 h^-1		-0.56	0.75	0.5	1.8	1
2322-040	G	23.5R			65			-0.42	0.75	1.4	1.3	1
2323+790	G	19.5V			32		0.43	-0.3	0.75	1.4	1.2	1
DA193	Q	18.0V	2.365	4.0 h^-1	4	16 h^-1		-1.6	0.6	9.5	7.8	2
OQ208	G	14.6r	0.077	1.0 h^-1	10	10 h^-1		-1.5	1.6	4.9	2.76	2

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