Identifying compact symmetric objects with high-precision VLBI and Gaia astrometry

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Table A.2.

CSO parameters used in Fig. 2 in the main paper.

Name	Radio power P_1, 4	Projected size	H–H velocity	Kinematic age	Spectral index	Ref
	log(W Hz⁻¹)	(pc)	(c)	(year)
J0038+2302	25.03	31.3	0.25	410	0.62	2
J0111+3906	28.10	39.0	0.34	380	0.62	2
J0119+3210	25.44	98.0	≤0.64	≥500	0.67	2
J0713+4349	27.38	146.0	0.51	930	0.48	2
J0832+1832	25.74	21.2	0.06	1200	0.74	1
J1035+5628	27.36	181.8	0.96	620	0.81	2
J1110+4817	27.31	162.9	≤0.64	≥830	1.34	1
J1111+1955	26.79	75.7	≤0.18	≥1360	1.02	1,2
J1158+2450	25.92	28.9	≤0.16	≥1160	0.29	1
J1234+4753	26.20	49.9	0.10	1680	0.46	1
J1244+4048	27.21	220.4	≤2.00	≥130	0.63	1
J1247+6723	25.06	13.9	0.26	160	0.65	1,2
J1324+4048	27.06	32.7	0.12	870	0.94	2
J1326+3154	27.32	278.1	0.88	1030	0.66	1,2
J1335+5844	27.07	84.2	0.16	1800	0.04	2
J1358+4737	26.12	24.3	0.31	250	0.66	1
J1407+2827	25.85	11.1	0.13	160	0.36	1,2
J1414+4554	25.69	86.7	≤0.16	≥1740	0.78	2
J1415+1320	27.04	30.2	0.91	100	−1.11	2
J1511+0518	25.31	7.3	0.08	480	−0.51	1,2
J1602+2418	27.86	63.4	2.54	80	0.78	1
J1609+2641	27.71	290.0	0.63	1500	1.05	2
J1723+6500	24.48	2.8	≤0.10	≥90	0.4	2
J1734+0926	27.58	100.5	0.25	1300	0.75	2
J1815+6127	27.48	73.6	≤1.21	≥200	1.57	1
J1845+3541	27.55	31.0	0.55	180	0.62	2
J1939−6342	27.63	128.0	0.30	1400	1.62	2
J1944+5448	26.67	165.0	0.50	1080	0.78	2
J1945+7055	25.46	57.0	≤0.19	≥1000	0.54	1,2
J2022+6136	27.09	24.5	0.18	440	−0.23	2
J2203+1007	27.86	81.8	0.53	500	0.53	2
J2355+4950	26.81	179.2	0.31	1900	0.81	1,2

Notes. Column (1): source name; Column (2): radio power at 1.4 GHz; Column (3): projected linear size in pc; Column (4): hotspot separation velocity in c; Column (5): kinematic age; Column (6): spectral index calculated from 2−8 GHz from this paper or 5−8 GHz from An & Baan (2012); Column (7): references: 1 – this paper, 2 – An & Baan (2012); Note: Five sources in the Gaia+VLBI CSO sample are also included in An & Baan (2012), and for these sources, the data from An & Baan (2012) is used. : For sources with conflicting kinematic measurements (particularly J1111+1955), we adopt the more reliable values from previous studies with longer monitoring baselines as indicated in the reference column.

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