3 Results

3.1 Mkn 1

Mkn 1 (NGC 449) is a highly inclined SB0a galaxy at redshift z = 0.0159, with 1'' corresponding to 460 pc projected distance in the sky. We show its B band image in Fig. 1. The [OIII] emission has radial extent $\sim$9'' (4 kpc) at PA = 83$^\circ$, elongated along the major axis of the nuclear continuum at PA = 87$^\circ$ (Mulchaey & Wilson 1995).

Although the profiles of optical emission lines of Mkn 1 show blue asymmetry (e.g. De Robertis & Shaw 1990), no asymmetry or evident broad wings are seen in the near-infrared (NIR; Veilleux et al. 1997). There is, therefore, no strong evidence for an obscured BLR in Mkn 1.

We show the B-I map of Mkn 1 in Fig. 2. There are several blue regions in the host galaxy to the E and SE of the nucleus, probably related to star forming activity, and an arclike red region situated S of the nucleus. Closer to the center, there is a blue elongated structure of $\sim$2.5'' (1.2 kpc extent across the nucleus at PA = 290$^\circ$). The nucleus is slightly closer to the E end of this elongation. Although not closely parallel to the axis of the [OIII] emission (PA = 83$^\circ$; Mulchaey & Wilson 1995), this blue elongation may be caused by scattered light from the nucleus. We shall discuss the origin of the detected structures in all the galaxies, in the context of the unified models, in Sect. 4. The colours of the blue elongation are given in Table 3.1. Note that in all the galaxies studied, these colours include a contribution from the red underlying stellar population in the nuclear region. Therefore, the real colours of the structures must be even bluer than those reported here.

  

Table 1: The colours of the blue maxima, their distance from the nuclei, and the relevant position angles

3.2 Mkn 533

Mkn 533 (NGC 7674, Arp 182) is an SBb spiral galaxy at z = 0.0289, with 1'' corresponding to 840 pc projected distance in sky. We show the B band image of Mkn 533 in Fig. 3. It has asymmetric arms and tidal connection to the nearby compact elliptical, NGC 7675. Mkn 533 has a nuclear double radio source, with diameter $\sim$0.75'' (630 pc) at PA = 117$^\circ$  (Kukula et al.1995). H$\alpha$ emission of Mkn 533 has polarised broad wings (Miller & Goodrich 1990; Tran 1995a; Young et al.1996). The nuclear polarisation rises steeply to the blue, the polarised flux spectrum is much bluer than the total flux spectrum, and the polarisation PA $\sim$ 31$^\circ$ is independent of wavelength, and perpendicular to the radio axis. All this indicates dust scattering as the main polarisation mechanism.

The forbidden optical emission lines (e.g. [OIII]) in Mkn 533 have strong blue wings (e.g. De Robertis & Shaw 1990; Veilleux 1991) and broad wings have been found in the NIR HeI, Pa$\beta$ and Br$\gamma$ lines (Ruiz et al. 1994; Veilleux et al.1997). Further evidence for an obscured central source in Mkn 533 comes from the hard X-ray spectrum, which shows a prominent Fe K line and a flat powerlaw continuum, well fitted by a steep intrinsic spectrum reflected by optically thick cold matter (Malaguti et al.1998). The intrinsic X-ray luminosity is at least one order of magnitude larger than what is observed.

We present the B-I maps of Mkn 533 in Fig. 4 (the whole galaxy) and Fig. 5 (nuclear region). The spiral structure, effects of dust reddening and star forming regions are clearly visible in the disk of Mkn 533 (Fig. 4). In the nuclear region (Fig. 5), there is a blue elongation from the nucleus to NW (PA = 310$^\circ$) of 3.2'' (2.7 kpc) total extent. This structure is aligned closely parallel to the radio axis and perpendicular to the polarisation orientation, and probably represents scattered light from the nucleus. Its colours are given in Table 3.1.

3.3 Mkn 607

Mkn 607 (NGC 1320) is a nearly edge-on S0a galaxy at redshift z = 0.0090, with 1'' corresponding to 260 pc projected distance in the sky. We show a B band image of Mkn 607 in Fig. 6. The [OIII] emission is extended along the major axis of the host galaxy (PA = 137$^\circ$) with $\sim$12'' (3.1 kpc) radius (Mulchaey et al. 1996b). The PA of the innermost [OIII] emission and that of the nuclear continuum emission is 132$^\circ$ (Mulchaey & Wilson 1995; Mulchaey et al.1996b).

We show the B-I maps of Mkn 607 in Fig. 7 (the whole galaxy) and Fig. 8 (nuclear region). A red narrow dust lane at closest distance of 5.1'' (1.3 kpc) is visible along the whole SW side of the host galaxy (already seen in the B band image; Fig. 6). Several blue star forming regions can be detected in the host galaxy (Fig. 7). In the central region (Fig. 8), a red extended region is visible on the SW side of the nucleus (at 1.2''; 310 pc), probably related to the larger scale SW dust lane. In addition, there is a faint blue elongated structure emanating from the nucleus toward NW (PA = 320$^\circ$) up to 0.9'' (230 pc) distance. Its orientation agrees perfectly with the axis of the [OIII] emission, and possibly represents scattered light from the nucleus. Its colours are given in Table 3.1.

3.4 Mkn 1066

Mkn 1066 (UGC 2456) is an inclined SB(s)0 galaxy at redshift z = 0.0121, with 1'' corresponding to 350 pc projected distance on the sky. We show its B band image in Fig. 9. The nuclear continuum is aligned at PA = 137$^\circ$ (Mulchaey et al.1996b). The radial extent of the [OIII] emission is 6.5'' (2.3 kpc) at PA = 134$^\circ$, with a double structure across the nucleus separated by $\sim$3.3'' (1.2 kpc) at PA = 131$^\circ$  (Mulchaey et al.1996b). The innermost [OIII] gas is concentrated into a narrow jet-like feature extending 1.4'' (490 pc) NW of the nucleus at PA $\sim 310$$^\circ$, with much fainter emission up to 0.8'' (280 pc) SE at PA $\sim$ 130$^\circ$ (Bower et al.1995). The [OIII] emission is thus parallel to the axis of the linear triple radio source extending 2.8'' (1.0 kpc) with bipolar jetlike morphology along PA = 134$^\circ$  (Ulvestad & Wilson 1989). No polarised or NIR broad lines have been detected in Mkn 1066 (Miller & Goodrich 1990; Kay 1994; Veilleux et al.1997), and the UV continuum polarisation is parallel to the radio axis, unlike in the Seyfert 2s with evidence for scattered nuclear light.

We show the B-I map of Mkn 1066 in Fig. 10. Note that the I band nucleus is saturated, so the structure in the central few pixels is not real. The star forming regions in the host galaxy are clearly visible in Fig. 10. There is a very red region SW of the nucleus at 2.6'' (910 pc). Finally, there is a blue elongated structure NW of the nucleus (PA = 325$^\circ$) with total extent 4.2'' (1.5 kpc). This structure agrees well with the axis of the [OIII] and radio emission, and possibly represents scattered light from the nucleus. Its colours are given in Table 3.1.

3.5 NGC 788

NGC 788 is an S0a galaxy at redshift z = 0.0136, with 1'' corresponding to 390 pc projected distance in the sky. We show its B band image of in Fig. 11. It shows faint spiral arms at $\sim$30'' (12 kpc) radius from the nucleus. The [OIII] emission extends to 4.3'' (1.7 kpc) from the nucleus at PA = 105$^\circ$, while the major axis of the nuclear continuum is at PA = 112$^\circ$ (Mulchaey et al.1996b).

We show B-I maps of NGC 788 in Fig. 12 (the whole galaxy) and Fig. 13 (nuclear region). The blue inclined ring of emission with $\sim$30'' (12 kpc) radius around the nucleus, tracing the faint spiral structure is clearly visible in Fig. 12. The nucleus is situated between two blue regions (Fig. 13), the less extended at 0.4'' (160 pc) S (PA = 170$^\circ$) and the more extended at 1.1'' (430 pc) NW (PA = 315$^\circ$). There is also a red extended region at 1.3'' (510 pc) S-SW of the nucleus. Although the axis of the blue double structure (PA $\sim$ 150$^\circ$) does not correspond well with the axis of the [OIII] emission (PA = 105$^\circ$), the blue maxima may represent localized peaks in the scattered light from the nucleus. Their colours are given in Table 3.1.

3.6 NGC 5347

NGC 5347 is an SBab galaxy at redshift z = 0.00778, with 1'' corresponding to 230 pc projected distance in the sky. Its B band image is presented in Fig. 14. It shows a bar enclosed by a ring structure at $\sim$25'' (5.8 kpc) radius, and faint spiral arms emerging from the ring at the ends of the bar (see also Gonzalez-Delgado & Perez 1996). The bar is oriented roughly parallel to the major axis of the galaxy. The [OIII] emission of NGC 5347 has a double nuclear structure perpendicular to the bar (Pogge 1989). An H$\alpha$ emission knot is located at 2.7'' (620 pc) NE at PA = 25$^\circ$ from the nucleus, perpendicular to the bar (Gonzalez-Delgado & Perez 1996). The knot has high excitation spectrum and a large Ca triplet EW, suggesting the presence of red supergiants associated with an old burst of star formation. The emission line ratios of the knot, however, indicate photoionisation by a hard AGN continuum (Gonzalez-Delgado & Perez 1996). The nuclear continuum emission is probably emitted anisotropically, as supported by photon deficit arguments (Gonzalez-Delgado & Perez 1996).

We show the B-I map of NGC 5347 in Fig. 15. The blue star forming regions, the ring structure and the spiral arms in the host galaxy are clearly visible. There is also a red dust lane running S of the nucleus roughly E to W at a closest distance of 3.3'' (760 pc), delineating the bar. In the central region, the emission knot at 2.7'' (620 pc) at PA = 25$^\circ$ NE of the nucleus is clearly seen. Even closer to the nucleus, there is a blue elongated structure with total extent $\sim$1.3'' (300 pc) toward N of the nucleus (PA = 10$^\circ$). These structures probably represent the brightest localized peaks in the scattered light from the nucleus. Their colours are given in Table 3.1.

3.7 NGC 5929

NGC 5929 is an Sab pec galaxy interacting with the starburst galaxy NGC 5930, together forming the galaxy pair Arp 90. The redshift of NGC 5929 is z = 0.00854, with 1'' corresponding to 250 pc projected distance in the sky. The B band image of the system is shown in Fig. 16. NGC 5929 has a faint hard X-ray spectrum, implying heavy absorption (Rush & Malkan 1996). It has triple radio structure extended along PA = 61$^\circ$, with total diameter 1.3'' (320 pc; Su et al.1996). The SW lobe is at 0.7'' (170 pc) distance from the nucleus and is slightly stronger than the NE lobe at 0.6'' (150 pc) distance. The [OIII] emission resembles closely the radio morphology, with two peaks straddling the nucleus at PA $\sim$ 60$^\circ$ (Bower et al. 1994). However, the [OIII] peaks are closer to the nucleus (1.1'' = 280 pc separation). Also, the NE [OIII] component is bisected by a dust lane. The [OIII] emission does not define a clear biconical morphology as in many other Seyfert 2s. Also, there is no evidence for obscuration in the direct images, except the dust lane, nor do energy balance considerations suggest anisotropy of the nuclear radiation (Bower et al.1994).

We show the B-I maps of the whole system in Fig. 17 and of NGC 5929 in Fig. 18. There is a blue stellar tail from the N part of NGC 5929 toward NGC 5930 and a red bridge between the galaxies, probably stellar emission reddened by the disc of NGC 5930 (Fig. 17; see also Lewis & Bowen 1993). The nucleus of NGC 5929 (Fig. 18) is situated between two blue maxima at opposite sides of the nucleus, the closer and brighter at 0.8'' (200 pc) SW (PA = 225$^\circ$) and the more distant and fainter at 2.0'' NE (PA = 45$^\circ$). Since the orientation of this structure agrees well with the [OIII] and radio axes, and the peaks are only slightly further away from the nucleus than the respective [OIII] and radio peaks, they possibly represent extranuclear scattering mirrors of anisotropically escaping nuclear light. The colours of the blue maxima are given in Table 3.1. A very red region, probably due to dust emission, is located 3.4'' (850 pc) S of the nucleus (PA = 166$^\circ$).

3.8 NGC 5953

NGC 5953 is an S0/a pec spiral galaxy at redshift z = 0.00655, with 1'' corresponding to 190 pc projected distance in the sky. It interacts with the late-type spiral NGC 5954, and together they form the galaxy pair Arp 91 (VV 244). We show a B band image of the system in Fig. 19. While NGC 5954 has pronounced spiral arms, faint emission to N and W of its disk and a stellar bridge extending toward NGC 5953, the latter appears relatively smooth. HI maps (Chengalur et al. 1995) show a long plume of emission to NW of NGC 5953, corresponding to faint optical stellar emission (Fig. 19), and probably associated to the S stellar bridge of NGC 5954.

From long-slit spectroscopy, Yoshida et al.(1993) detected an inclined ring of giant star forming regions around the nucleus of NGC 5953, with ring diameter $\sim$15'' (2.9 kpc). More recently, the circumnuclear star forming properties of NGC 5953 were studied by [OIII] and H$\alpha$ imaging (Gonzalez-Delgado & Perez 1997) and by UV imaging (Colina et al.1997). The UV continuum is concentrated in several compact circumnuclear knots in a ring with similar morphology to H$\alpha$. Yoshida et al.(1993) detected also a high-ionisation region 4'' (760 pc) NE from the nucleus at PA $\sim50$$^\circ$. Its location agrees well with radio morphology (PA = 40$^\circ$; Jenkins 1984), and it is probably ionised by an anisotropic nuclear continuum. Yoshida et al.estimate that the flux seen by the ENLR is an order of magnitude higher than that directly observed. The lack of similar emission region on the opposite (SW) side of the nucleus is probably due to obscuration and/or the torus inclination.

We show the B-I maps of the whole system in Fig. 20 and of NGC 5953 in Fig. 21. The overall features already visible in the direct B band image (Fig. 19), such as the stellar bridge between the galaxies, and the long plume of emission to NW of NGC 5953, are even more clearly visible in the B-I map (Fig. 20). In NGC 5953, the B-I map (Fig. 21) clearly shows the inclined star forming ring oriented roughly N-S with diameter $\sim 13\times$8'' ($2.5\times 1.5$ kpc). There is a red arc around the nucleus E-N-W with two main peaks at 1.6'' (300 pc) at PA = 320$^\circ$, and at 1.8'' (340 pc) at PA = 60$^\circ$, inside the star forming ring. Finally, there is a faint narrow blue elongated structure of 0.5'' (100 pc) extent at PA = 220$^\circ$. This elongation is at similar orientation to the [OIII] and radio axes and probably represent scattered light from the nucleus. Its colours are given in Table 3.1.

3.9 NGC 7212

NGC 7212 is in a pair of interacting galaxies. Its redshift is z = 0.0266, with 1'' corresponding to $\sim$770 pc projected distance in the sky. We show the B band image of NGC 7212 in Fig. 22. Polarised spectra of NGC 7212 show broad components to H$\alpha$ and H$\beta$, and this polarisation is higher than that in the continuum (Tran et al. 1992; Tran 1995a), an indication of a hidden BLR. Most likely, the polarisation arises from scattering by dust (Tran 1995a), because the spectrum is very red, the continuum polarisation rises smoothly to the blue, and the polarised flux spectrum is bluer than total flux spectrum. The [OIII] emission of NGC 7212 shows a jet-like high-ionisation feature extending up to 10'' (7.7 kpc) from the nucleus at PA = 10$^\circ$ (Tran 1995a). This jet is exactly parallel to the axis of the small scale double radio source (0.7'' separation; Falcke et al. 1998), and roughly perpendicular to the optical polarisation (PA = 93$^\circ$), suggesting that the jet is collimated radiation from the hidden nucleus obscured by a torus. The line ratios of the jet indicate photoinisation by the nuclear continuum. There is a faint broad base to H$\alpha$, probably the BLR reflected from the obscured nucleus by an offnuclear scattering mirror. However, no obvious BLR component to NIR lines was found by Veilleux et al.(1997).

We show the B-I maps of NGC 7212 in Fig. 23 (the whole system) and Fig. 24 (NGC 7212). The nucleus of NGC 7212 is very blue and an extended fan-shaped blue emission region extends from the nucleus to S (PA = 165$^\circ$) with total extent 2.3'' (1.8 kpc). This blue region is bisected by a red dust lane. A much redder narrow dust lane is situated on the other side of the nucleus, at closest distance 3.7'' (2.8 kpc) at PA = 280$^\circ$. Although the orientation of the blue elongation does not correspond perfectly with the [OIII] emission, it may represent scattered light from the nucleus. Its colours are given in Table 3.1.

3.10 NGC 7319

NGC 7319 (Arp 319) is an SBb galaxy belonging to the Stephen's Quintet compact group of galaxies. Its redshift is z = 0.0225, with 1'' corresponding to 650 pc projected distance in the sky. We show the B band image of NGC 7319 in Fig. 25. In the radio (van der Hulst & Rots 1981), NGC  7319 shows a jet-like feature SW to the nucleus at PA = 207$^\circ$ extending $\sim$6'' (3.9 kpc). The X-ray emission from Stephan's Quintet consists of two components: the soft X-ray emission probably arises from hot intracluster gas (Sulentic et al. 1995), while the hard X-ray emission, peaked on NGC 7319, is consistent with an absorbed powerlaw, and exhibits a strong Fe K line, providing strong evidence for an obscured nucleus in NGC 7319 (Awaki et al.1997).

The [OIII] emission of NGC 7319 extends for $\sim$10'' (6.5 kpc) toward S-SW, possibly in the form of an ionisation cone (Aoki et al.1996). The [OIII] morphology and PA agree well with the radio, however, the [OIII] peak is closer to the nucleus than the radio peak. The kinematics of the extended [OIII] emission indicates a high velocity outflow up to $\sim$9'' (5.8 kpc) from the nucleus, mainly photoionised by the nuclear radiation (Aoki et al.1996). The number of ionising photons required to ionise the ENLR is over 10 times higher than the number of photons in our line of sight, strongly indicating an anisotropic nuclear radiation field (Aoki et al.1996).

We show the B-I map of NGC 7319 in Fig. 26. To the S of the nucleus (PA = 210$^\circ$) there is a very red region at 0.7'' (460 pc), continuing further S as a more extended red region. The bluest region is situated 1.1'' (720 pc) N of the nucleus (PA = 10$^\circ$). The orientation of the blue elongation agrees well with the [OIII] and radio axes, and probably represents scattered light from the nucleus. Its colours are given in Table 3.1.

  

Figure 1: The B band image of Mkn 1. The size of the image is $26\times 26$'' ($12\times 12$ kpc). In this and other figures, north is up, east to the left, the nucleus of the Seyfert galaxy is marked as a cross and, unless otherwise indicated, the scale bar corresponds to 1 kpc projected distance in the sky

  

Figure 2: The B-I map of Mkn 1. The size of the image is $26\times 26$'' ($12\times 12$ kpc). In this and other colour maps, dark shades indicate blue and light shades red emission. The B-I colour coding is from 1.0 to 2.0. Note the blue elongation across the nucleus at PA = 290$^\circ$ of $\sim$2.5'' (1.2 kpc) extent

  

Figure 3: The B band image of Mkn 533. The size of the image is $79\times 79$'' ($67\times 67$ kpc). The scale bar corresponds to 5 kpc projected distance in the sky

  

Figure 4: The B-I map of Mkn 533. The size of the image is $79\times 79$'' ($67\times 67$ kpc). The B-I colour coding is from 1.2 to 2.4. The scale bar corresponds to 5 kpc projected distance in the sky. Spiral structure and star forming regions are clearly visible in the main body of the galaxy. There is a blue elongation with a total extent of 3.2'' (2.7 kpc) from the nucleus along PA = 310$^\circ$

  

Figure 5: The B-I map of the innermost $21\times 21$'' ($18\times 18$ kpc) of Mkn 533, showing more clearly the structures seen in Fig. 4. The B-I colour coding is from 0.7 to 2.4

  

Figure 6: The B band image of Mkn 607. The size of the image is $53\times 53$'' ($14\times 14$ kpc)

  

Figure 7: The B-I map of Mkn 607. The size of the image is $53\times 53$'' ($14\times 14$ kpc). The B-I colour coding is from 2.2 to 2.8. Note the red dust lane along the whole SW side of the galaxy. Star forming regions are visible in the main body of the galaxy

  

Figure 8: The B-I map of the innermost $18\times 18$'' ($4.7\times 4.7$ kpc) of Mkn 607. The B-I colour coding is from 2.2 to 2.8. Note the possible blue elongation emanating at PA = 320$^\circ$ up to 0.9'' (230 pc) distance from the nucleus. There is a red region on the SW side of the nucleus, probably related to the larger scale dust lane (Fig. 7)

  

Figure 9: The B band image of Mkn 1066. The size of the image is $53\times 53$'' ($19\times 19$ kpc)

  

Figure 10: The B-I map of Mkn 1066. The size of the image is $53\times 53$'' ($19\times 19$ kpc). The B-I colour coding is from 1.6 to 3.0. Note that the I band image is saturated in the nucleus, so the structure in the central few pixels is not real. There is a blue elongated region at PA = 326$^\circ$ from the nucleus with 2.6'' (910 pc) extent, and a very red region SW of the nucleus. Spiral arms and star forming regions are visible in the disk

  

Figure 11: The B band image of NGC 788. The size of the image is $70\times 70$'' ($27\times 27$ kpc)

  

Figure 12: The B-I map of NGC 788. The size of the image is $70\times 70$'' ($27\times 27$ kpc). The B-I colour coding is from 2.2 to 2.6. Note the blue inclined ring of emission at $\sim$30'' (12 kpc) radius from the nucleus (see also Fig. 11). The nucleus is situated between two blue regions, at 0.4'' (150 pc) along PA = 170$^\circ$ and at 1.1'' (430 pc) along PA = 316$^\circ$. There is also an extended red region SW of the nucleus

  

Figure 13: The B-I map of the innermost $8.8\times 8.8$'' ($3.4\times 3.4$ kpc) of NGC 788, showing more clearly the structures seen in Fig. 12. The B-I colour coding is from 2.2 to 2.6

  

Figure 14: The B band image of NGC 5347. The size of the image is $88\times 88$'' ($20\times 20$ kpc)

  

Figure 15: The B-I map of NGC 5347. The size of the image is $88\times 88$'' ($20\times 20$ kpc). The B-I colour coding is from 0.7 to 2.1. Note the red dust lane running S of the nucleus roughly from E to W, probably related to the bar, and a blue elongation of $\sim$2.6'' (600 pc) extent N of the nucleus at PA = 8$^\circ$

  

Figure 16: The B band image of NGC 5929/5930. The size of the image is $70\times 70$'' ($18\times 18$ kpc). NGC 5929 is situated in the SW and NGC 5930 in the NE part of the figure

  

Figure 17: The B-I map of NGC 5929/5930. The size of the image is $70\times 70$'' ($18\times 18$ kpc). The B-I colour coding is from 1.0 to 2.4. NGC 5929 is situated in the SW and NGC 5930 in the NE part of the figure. The blue stellar tail from the N part of NGC 5929 toward NGC 5930 and the red stellar bridge between the galaxies are clearly visible. The nuclear region of NGC  5929 has double blue peaks at opposite sides of the nucleus, at 0.8'' (200 pc) at PA = 227$^\circ$, and at 2.0'' (500 pc) at PA = 47$^\circ$). There is also a very red region S of the nucleus

  

Figure 18: The B-I map of the innermost $18\times 18$'' ($4.5\times 4.5$ kpc) of NGC 5929, showing more clearly the structures seen in Fig. 17. The B-I colour coding is from 1.0 to 2.3

  

Figure 19: The B band image of NGC 5953/5954. The size of the image is $106\times 106$'' ($20\times 20$ kpc). NGC 5953 is situated in the SW and NGC 5954 in the NE part of the figure

  

Figure 20: The B-I map of NGC 5953/5954. The size of the image is $106\times 106$'' ($20\times 20$ kpc). The B-I colour coding is from 0.2 to 2.2. NGC  5953 is situated in the SW and NGC 5954 in the NE part of the figure. Note the blue stellar bridge between the galaxies, and the long plume of blue emission NW of NGC 5953. There is a red arc around the nucleus of NGC 5953 E-N-W, and an inclined lopsided star forming ring roughly N-S with diameter $13\times 8$'' ($2.5\times 1.5$ kpc). Finally, there is possibly a blue elongated structure up to 0.5'' (100 pc) from the nucleus at PA = 221$^\circ$

  

Figure 21: The B-I map of the innermost $18\times 18$'' ($3.4\times 3.4$ kpc) of NGC 5953, showing more clearly the structures seen in Fig. 20. The B-I colour coding is from 0.7 to 2.2

  

Figure 22: The B band image of the field of NGC 7212. The size of the image is $44\times 44$'' ($34\times 34$ kpc). NGC 7212 is situated in the SW and the main companion galaxy in the NE part of the figure. The scale bar corresponds to 5 kpc projected distance in the sky

  

Figure 23: The B-I map of the field of NGC 7212. The size of the image is $44\times 44$'' ($34\times 34$ kpc). The B-I colour coding is from 1.4 to 3.1. NGC 7212 is situated in the SW and the main companion galaxy in the NE part of the figure. The scale bar corresponds to 5 kpc projected distance in the sky. The nuclear region of NGC 7212 is very blue and an extended fan-shaped blue region emanates from the nucleus along PA = 166$^\circ$, with total extent of 2.3'' (1.8 kpc). This blue region is bisected by a red dust lane. A red narrow dust lane is visible on the other side of the nucleus

  

Figure 24: The B-I map of the innermost $18\times 18$'' ($14\times 14$ kpc) of NGC 7212, showing more clearly the structures seen in Fig. 23. The B-I colour coding is from 1.4 to 3.1. The scale bar corresponds to 5 kpc projected distance in the sky

  

Figure 25: The B band image of NGC 7319. The size of the image is $35\times 35$'' ($23\times 23$ kpc). The scale bar corresponds to 5 kpc projected distance in the sky

  

Figure 26: The B-I map of NGC 7319. The size of the image is $35\times 35$'' ($23\times 23$ kpc). The B-I colour coding is from 2.4 to 3.0. The scale bar corresponds to 5 kpc projected distance in the sky. The bluest region lies at 1.1'' (720 pc) from the nucleus at PA = 10$^\circ$. To the S of the nucleus at 0.7'' (460 pc) there is a very red region, extending further S as a red region