B2 radio galaxies info on  archival images

Table 2 summarizes some optical properties determined from the HST observations: In columns 1 and 2 we give the radio and optical names of the object, in column 3 the redshift, in column 4 the presence or absence of dust features in the nucleus (d means disklike structure, l stands for a dust lane and p means irregular dust patches), in column 5 the position angle of the dust feature, and in columns 6 and 7 the presence of an optical core and an optical jet, respectively. Below the table more detailed information on the sources is given.

• 0034+25: There is a prominent dust band in the center of this galaxy, likely a highly inclined dusty disk. . At larger radii, isophotes are very cuspy and oriented at the same position angle as the inner disk, which indicates the presence of a stellar disk coplanar with the inner one. The galaxy belongs to the Zw cluster 0034.4+2532.
• 0055+26 (NGC 326): This is a system of two galaxies, also referred to as a dumbbell galaxy. Only the galaxy hosting the radio source is shown. The two galaxies do not show any peculiarities. There is a third much fainter object in the field. The galaxy belongs to a group with extended X-ray emission (Worrall et al. 1995)
• 0055+30 (NGC 315): A highly inclined, very regular nuclear disk, is seen in absorption in this galaxy. It is oriented at P.A. ca. 160 degrees and extends to 40 pc. At its center there is an unresolved nuclear source. Irregular dust patches are also present on the South side of the galaxy. See also Verdoes Kleijn et al. (1999).
• 0104+32 (NGC 383, 3C 31): An extended nuclear dusty disk is seen at low inclination, with an unresolved nuclear component at its center. The disk diameter is r=350 arcsec (2.5 kpc) along the major axis (P.A. 160 degrees). The galaxy belongs to a chain of which it is the brightest member. See also Martel et al. (1999) and Verdoes Kleijn et al. (1999).
• 0116+31: An S-shaped dust lane bisects its nuclear region. Its inner P.A. is about 7 degrees. Conway (1996) detected a disk of HI in absorption which fully occults one of the minilobes and partially covers the other.
• 0120+33 (NGC 507): Brightest galaxy of the Zw cluster 0107+3212. The galaxy appears very regular and smooth.
• 0149+35 (NGC 708): A low brightness galaxy whose nuclear regions are crossed by an irregular dust lane and dust patches. It is the brightest galaxy of the cluster Abell 262.
• 0648+27: A galaxy with an irregular morphology, enhanced by the presence of dusty features. On its northern side there is a chain of knots, probably regions of star formation, parallel to the dusty filaments.
• 0708+32: The host galaxy does not exhibit any obvious peculiarities.
• 0722+30: The only source of the B2 sample associated with a spiral galaxy. It is a highly inclined galaxy which fills the PC field of view. Strong absorption is associated with its disk and a bulge-like component is also clearly visible. The radio emission originates from two symmetric jet-like features at an angle of 25 degrees to the disk.
• 0755+37 (NGC 2484): The galaxy is characterized by a central unresolved nuclear source. After subtraction of a galaxy elliptical model the presence of a one-sided optical jet is revealed, cospatial with the SE brighter radio jet.
• 0908+37: This galaxy shows a point-like nucleus at the center of a highly elongated absorption feature, possibly an edge-on disk (P.A. = 160 degrees). A fainter companion galaxy (outside the image shown) is located 3.7 arcsec to the SW.
• 0915+32: A disk-like dust band surrounds its nuclear region.
• 0924+30: The host galaxy does not exhibit any obvious peculiarities.
• 1003+26: A very regular low brightness elliptical galaxy with no outstanding morphological features. The galaxy belongs to the cluster Abell 923.
• 1003+35 (3C 236): An off-centered dust lane crosses the galaxy to the SW, with 45 arcsec (2.5 kpc) extension. See also Martel et al. (1999).
• 1005+28: A diffuse and quite regular galaxy with no evident morphological peculiarities. A dust patch is visible.
• 1101+38: This source is associated with the BL Lac object Mrk 421. Not surprisingly it is dominated by its bright unresolved nucleus which produces strong diffraction spikes. Nonetheless a smooth elliptical host galaxy is clearly visible.
• 1113+24: A round smooth elliptical galaxy with a faint companion about 6 arcsec to the north. The galaxy is the brightest of the Zw cluster 1113.0+2452.
• 1204+34: Dust patches produce a spiral structure, which is clearly visible in both bands. It extends out to at least 2 arcsec from a fully resolved nucleus. A secondary, again resolved, nucleus is found to the NE at a distance of 3 arcsec. Both nuclei are embedded in a common elliptical halo, centered on the brighter one.
• 1217+29 (NGC 4278): This source is associated with the nearby galaxy NGC 4278. It shows a regular structure only slightly modified by diffuse dust absorption to its NW side. The nucleus is unresolved. The radio source is very compact, 2 pc (see, e.g., Schilizzi et al. 1983). The galaxy is known to have strong nuclear emission lines (Osterbrock 1960). It contains a large amount of neutral hydrogen (Raimond et al. 1981) rotating around an axis at about 1 degree.
• 1251+27 (Coma A, 3C 277.3): In addition to a prominent unresolved nucleus, note also the filamentary structure located r=350 arcsec to the SW. This corresponds to the radio knot K1 in van Breugel et al. (1985), detected also in emission lines. See also Martel et al. (1999).
• 1256+28 (NGC 4869): This galaxy presents a highly elongated absorption feature, possibly an edge on disk. It belongs to the Coma Cluster (Abell 1656).
• 1257+28 (NGC 4874): A very regular low brightness elliptical galaxy. It is one of the two dominant members of the Coma Cluster (Abell 1656).
• 1321+31 (NGC 5127): A dark lane covers the nucleus of this galaxy and extends out to a radius of 1 arcsec, P.A. -45 degrees . The galaxy belongs to the Zwicky cluster 1319.6+3135. See also Verdoes Kleijn et al. (1999).
• 1322+36 (NGC 5141): There is a wide dust band in the center of this galaxy, at P.A. 45 degrees. See also Verdoes Kleijn et al. (1999).
• 1339+26: A small dark nuclear band (P.A. 85 degrees ) characterizes this otherwise very regular galaxy. The galaxy is the eastern of a double system and is the dominant member of the cluster Abell 1775.
• 1346+26: A low brightness galaxy with an unresolved nucleus and dust in the form of an irregular lane and patches (P.A. 85 degrees ). A sort of tail is seen to the SW towards a companion. It is the brightest galaxy (cD) of the cluster Abell 1795.
• 1347+28: A regular elliptical galaxy with irregular dusty features. It belongs to Abell 1800.
• 1350+31: A highly irregular galaxy, with two compact emission knots separated by a filamentary dust lane which extends to form a fan-like shape at larger radii. See also Martel et al. (1999). See Akujor et al. (1996) for a high resolution radio map showing a flat spectrum core with a two sided jet.
• 1357+28: A round elliptical galaxy with a small dust lane (P.A. = 0 degrees ) bisecting the nuclear region.
• 1422+26: The host galaxy is very smooth with no outstanding morphological features. The bright central core is fully resolved.
• 1430+25: This elliptical galaxy does not exhibit any obvious peculiarities. An elongated nucleus has its major axis at P.A. 95 degrees . The radio-structure is head-tail type, but no obvious cluster or group is visible.
• 1441+26: The target is a spiral galaxy. However, comparison of the radio and optical maps shows that this is not the host of the radio source. The correct identification is with a faint elliptical galaxy located at RA = 14:41:56.35, Dec = 26:14:05.0. As the magnitude of this galaxy is well below the optical selection threshold of the B2 sample, it must be considered a misidentification.
• 1447+27: Two off-center linear dust lanes run 0.6 and 1. arcsec2 respectively north-east of the nucleus (P.A. 155 degrees  ) of this otherwise very regular galaxy.
• 1450+28: Elliptical galaxy with no outstanding features. In Abell 1984.
• 1455+28: The presence of hour-glass shaped dust absorption gives this galaxy a quite irregular appearance. The central knot is compact but completely resolved. Companion galaxy at 145 arcsec.
• 1457+29: A wide dust lane (P.A. 10 degrees) runs perpendicularly to the galaxy projected minor axis. The redshift of the galaxy has been measured recently by Gonzalez-Serrano & Carballo (2000); this value has been added in Table 2.
• 1502+26 (3C 310): A smooth elliptical galaxy with a central unresolved source. See Martel et al. (1999).
• 1511+26 (3C 315): This galaxy shows a very high nuclear ellipticity which contrasts with the typical roundness of the B2 host galaxies. The ellipticity decreases at larger radii but the central very elongated central structure clearly extends at larger radii, probably indicative of a edge-on stellar disk. The radio source has a very peculiar, two-banana shaped, radio-structure. See de Koff et al. (1996).
• 1512+30: The host galaxy does not show any outstanding morphological features, except for very faint elongated dust absorption at the center.
• 1521+28: A well defined unresolved nucleus is superposed on the smooth core of the galaxy.
• 1525+29: The double peaked nuclear structure is caused by dust absorption, which is extended in the direction P.A. 7 degrees . The galaxy is the fainter of a pair in the cluster Abell 2079.
• 1527+30: The faint absorption from a possibly disk-like dust band is visible on the west side of this galaxy, extending to a radius of 0.3 arcsec. Its central region is resolved. In Abell 2083.
• 1553+24: This galaxy exhibits a point-like nucleus and, after removal of an elliptical model for the galaxy emission, a faint one-sided optical jet, cospatial with the NW brighter radio jet.
• 1557+26: A smooth and regular elliptical galaxy.
• 1610+29 (NGC 6086): This galaxy does not exhibit any obvious peculiarities. It is the brightest galaxy of the cluster Abell 2162.
• 1613+27: Very faint absorption features are seen to the SW on this otherwise regular galaxy.
• 1615+32 (3C 332): The emission of this source is dominated by its bright unresolved nucleus. A companion is seen to SW.
• 1626+39 (NGC 6166, 3C 338): Brightest galaxy of the cluster Abell 2199. An unresolved nucleus is superposed on the flat core of the galaxy. An arc-like dust feature extends from to nucleus to the W for 30 arcsec. Two fainter elliptical companions are also present. (see Martel et al. 1999).
• 1658+30: Smooth galaxy with a central unresolved core. The subtraction of an elliptical galaxy model reveals the presence of a faint one-sided optical jet, cospatial with the radio jet.
• 1726+31 (3C 357): The central knot is well resolved. A dust lane is also present on its SW side.
• 1827+32: Round galaxy with a possible weak nucleus.
• 1833+32 (3C 382): This source is associated with the broad line radio galaxy 3C382. The nuclear emission dominates the optical emission but the underlying host galaxy is clearly seen in these images. See also Martel et al. (1999).
• 2116+26 (NGC 7052): A spectacular, highly inclined disk-like structure of dust (at P.A. 3 degrees) surrounds the central source of this galaxy. See also Verdoes Kleijn et al. (1999). From the kinematics of the gas disk van der Marel & van den Bosch (1998) deduced the presence of a central black hole with a mass of  3 times 10^8 solar masses .
• 2229+39 (3C 449): A wide band of absorption is located on the West side of this source, at P.A. 65 degrees . See also Martel et al. (1999]). Note also the prominent unresolved nuclear source.
• 2236+35: A faint nucleus, probably unresolved, is seen in this elliptical galaxy.
• 2335+26 (NGC 7720, 3C 465): It is the brightest galaxy in the cluster Abell 2634. An elliptical region of dust absorption is located around the bright unresolved nucleus of this galaxy. See also Martel et al. (1999).