Jet formation studies in AGN: A search for new targets

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Table 1.

Sources in the sample and their main properties.

IAU name	Other	z	pc/mas	Log (M_BH)	Accr. mode	Radio morph.	Log (P_t)
0055+30	NGC 315	0.0165	0.33	9.32⁽¹⁾	LEG⁽¹²⁾	FRI	24.24
0104+32	3C 31	0.0170	0.34	9.62⁽²⁾	LEG⁽¹³⁾	FRI	24.80
0106+13	3C 33	0.0597	1.14	8.83⁽³⁾	HEG⁽¹³⁾	FRII	26.42
0220+43	3C 66B	0.0213	0.43	9.32⁽⁴⁾	LEG⁽¹³⁾	FRI	25.30
0222+36	B2 0222+36	0.0333	0.66	8.75⁽⁵⁾	LEG⁽¹⁴⁾	C	23.93
0313+41	IC 310	0.0188	0.38	8.48⁽⁶⁾	LEG⁽¹⁵⁾	FRI	23.73
0331+39	4C 39.12	0.0206	0.41	8.86⁽⁷⁾	LEG⁽¹⁶⁾	FRI	24.20
0844+31	IC 2402	0.0673	1.27	8.99⁽⁸⁾	LEG⁽¹⁴⁾	FRII	25.53
1142+20	3C 264	0.0216	0.43	8.67⁽⁴⁾	LEG⁽¹³⁾	FRI	25.17
1217+29	NGC 4278	0.0021	0.04	8.53⁽⁹⁾	LEG⁽¹⁴⁾	C	21.75
1626+39	3C 338	0.0304	0.60	8.89⁽⁴⁾	LEG⁽¹³⁾	FRI	25.57
1658+30	4C 30.31	0.0344	0.68	8.93⁽¹⁰⁾	LEG⁽¹²⁾	FRI	24.63
1833+32	3C 382	0.0579	1.11	8.98⁽¹¹⁾	HEG⁽¹³⁾	FRII	26.04
1842+45	3C 388	0.0917	1.69	9.18⁽⁵⁾	LEG⁽¹³⁾	FRII	26.47
2243+39	3C 452	0.0811	1.51	8.89⁽³⁾	HEG⁽¹³⁾	FRII	26.64
2335+26	3C 465	0.0302	0.60	9.14⁽⁴⁾	LEG⁽¹³⁾	FRI	25.61

Notes. Col. 1: IAU name. Col. 2: Other name. Col. 3: Redshift. Col. 4: Parsecs per milli-arcsecond. Col. 5: Black hole mass in solar masses. Col. 6: Accretion mode. Col. 7: Radio morphology. ‘C’ indicates a compact structure on kpc scales. Col. 8: 408 MHz radio power in W/Hz.

References: Col. 5: [1] Boizelle et al. (2021), [2] North et al. (2019), [3] Koss et al. (2022), [4] Balmaverde et al. (2008), [5] Woo & Urry (2002), [6] Aleksić et al. (2014b), [7] derived from the relation by Tremaine et al. (2002) based on the stellar velocity dispersion from van den Bosch et al. (2015), [8] Sikora et al. (2013), [9] Ly et al. (2004), [10] derived from the relation by Tremaine et al. (2002) based on the stellar velocity dispersion from Bettoni et al. (2009), [11] Fausnaugh et al. (2017). Col. 6: [12] Gonçalves & Serote Roos (2004), [13] Buttiglione et al. (2010), [14] Liuzzo et al. (2013), [15] Owen et al. (1996). [16] based on the Eddington ratio estimated in X-rays by Bi et al. (2020). Col. 7: see Liuzzo et al. (2009). Originally classified as compact, 4C 39.12 was re-classified as FRI by Liuzzo et al. (2013). Col. 8: see Liuzzo et al. (2009). For IC 310 only, we estimated the power from the 365 MHz flux density (Douglas et al. 1996), assuming α = −0.7.

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