$\begin{figure} \par {\hspace*{2mm}\includegraphics[width=5.6cm,angle=0]{4883f003... ...4883f004.ps}\par\includegraphics[width=5.7cm,angle=270]{4883f005.ps}\end{figure}$

Figure 2: Sky obtained by ellipse fitting: upper panel: $r^{\prime }$ -band image of NGC 5300 exemplary overlayed by eight fixed ellipses at every 100 pixels in the range 300-700 pixels. The white rectangular regions are masked areas. Middle panel: mean isophotal intensity (in counts) of the fixed ellipses fitted every 10 pixels. The region between the vertical dashed lines is used to determine the sky value ( $1146.52 \pm 0.09$ ), which is indicated as a horizontal dashed line together with the two dotted lines at $\pm$ $1\sigma$ . Lower panel: final surface brightness profile (circles) overlayed by the four profiles obtained by either over- or undersubtracting the sky by $\pm$ $1\sigma$ (triangles) or by $\pm 3\sigma$ (squares). The horizontal dashed line gives the critical surface brightness ( $\mu _{\rm crit}$ ) up to where we trust the profile i.e. where the $\pm 1\sigma$ profiles deviate by more than 0.2 mag.

In the text

$\begin{figure} \par\includegraphics[width=7.0cm,angle=0]{4883f008.ps}\end{figure}$

Figure 4: Classification schema (following Erwin et al. 2006): The three main disk types according to break features in their surface brightness profiles are Type I (no break), Type II ( downbending break), and Type III ( upbending break). In case the galaxy is barred (SB/SX) the downbending breaks (Type II) are subdivided according to the position of the break in respect to the bar: Type II.i (inside) or Type II.o (outside). An additional level of subclassification is applied for this class trying to relate the observed break to a physical origin. These are Type II.o-AB, Type II.o-OLR, and Type II.o-CT (see text). For apparently unbarred galaxies (SA/S?) we use only Type II-CT or Type II-AB. The upbending breaks (Type III) are subdivided according to the possible nature of the outer region: (d)isk- or (s)pheroid-like. Some galaxies are better described with two breaks, each of which could be associated to one of the individual types. They are assigned a mixed classification (e.g. Type II-CT + III).

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In the text

$\begin{figure} \par\includegraphics[width=5.4cm,angle=270,clip]{4883f009.ps}\inc... ...883f015.ps}\includegraphics[width=5.4cm,angle=270,clip]{4883f016.ps}\end{figure}$

Figure 5: Prototypical examples for each class of profiles: Type I, Type II-CT, Type II.o-OLR, and Type III (top to bottom). Left panels: $r^{\prime }$ -band images (unrotated cut-outs from the SDSS fields) with the break radius marked with an ellipse. The ellipse for the first Type I galaxy corresponds to the noise limit at $\sim$ 140''. Right panels: azimuthally averaged, radial SDSS surface brightness profiles in the $g^{\prime }$ (triangles) and $r^{\prime }$ (circles) band overlayed by $r^{\prime }$ band exponential fits to the individual regions: single disk or inner and outer disk. In addition we show the critical surface brightness ( $\mu _{\rm crit}$ ) for each band (dotted and dashed horizontal lines), down to which the profile is reliable (see Appendix A for a detailed legend).

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In the text

$\begin{figure} \par\includegraphics[width=6.1cm,angle=270]{4883f025.ps}\par\includegraphics[width=6.1cm,angle=270]{4883f026.ps} \end{figure}$

Figure 6: Example of how to establish the break radius, the break region and the associated scalelengths: upper panel: azimuthally averaged, surface brightness profile, overlayed by the best fitting exponentials (with scalelengths $h_{\rm in}$ and $h_{\rm out}$ ) marking the position of the boundaries (b_1-4) and the break radius $R_{\rm br}$ . Lower panel: approximated derivative (crosses) of the profile providing a local scalelength ( $h_{\rm local}$ ) together with the rebinned and smoothed version (triangles). The horizontal dashed line marks our characteristic (or mean) value which is the median of the $1/\hbox{$h_{\rm local}$ }~$ distribution. The vertical dotted lines mark the inner and outer boundary of the break region.

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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,angle=270]{4883f027.ps}\end{figure}$

Figure 7: Break radius ( $R_{\rm br}$ ) in absolute units (kpc) versus dynamical mass ( $\mathcal{M}_{\rm dyn}\!=\!2.326\times10^5 \frac{D_{25}}{2} \hbox{$v_{\rm rot}$ }~\!^2$ ) and absolute magnitude ( $M_{\rm abs}$ ) in the B-band according to LEDA for the different break types: Type II-CT (upper row), Type III (middle row), and Type II.o-OLR (bottom row). Overplotted are robust linear fits (dashed lines) to guide the eye and in the lower right corner of each plot the Spearman rank correlation coefficient. The break radius correlates in all three cases with absolute magnitude. With the exception of the Type II-CT, the relation of the position of the break with the dynamical mass is less tight.

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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,angle=270]{4883f028.ps}\end{figure}$

Figure 8: Classical truncations (Type II-CT): break radius in units of inner scalelength versus absolute magnitude ( $M_{\rm abs}$ ) (left, upper panel), rotational velocity ( $v_{\rm rot}$ ) (left, middle panel), extinction corrected central surface brightness of the inner disk ( $\mu _{0,\rm in}$ ) (left, lower panel), break radius in linear unit ( $R_{\rm br}$ ) (right, upper panel), inner scalelength in linear unit ( $h_{\rm in}$ ) (right, middle panel), and Hubble type (T) (right, lower panel). Overplotted are robust linear fits (dashed lines) to guide the eye and in the lower right corner of each plot the Spearman rank correlation coefficient.

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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,angle=270]{4883f029.ps}\end{figure}$

Figure 9: Classical truncations (Type II-CT): extrapolated central surface brightness $\mu _0$ (open circles) and surface brightness at the break radius $\mu _{\rm br}$ (filled squares) in the $r^{\prime }$ band versus absolute magnitude ( $M_{\rm abs}$ ) in B according to LEDA. Overplotted are robust linear fits (dashed lines) to guide the eye and in the lower and upper right corner the Spearman rank correlation coefficient for each data set.

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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,angle=270]{4883f031.ps}\end{figure}$	Figure 11: Frequency of profile types Type I (open circles), Type II-CT (filled squares), Type III (open triangles), and Type II.o-OLR (open squares) in relation to the Hubble type. The galaxies are merged in three morphological bins (T between 2.5-4.4, 4.5-6.4, and 6.5-8.4). The associated points are connected with lines and slightly shifted in T to be able to separate them.
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In the text

$\begin{figure}\par\includegraphics[width=5.7cm,angle=270]{4883f032.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f033.ps} \par\end{figure}$ IC 1067: Type II.o-OLR (possible Type I)
J145305.2+031954 .SBS3. 3.0 -18.97 2.0 1665

Galaxy close to the border of the SDSS field but almost complete with a nearby, physical companion (IC 1066, v=1577 km s^-1 ) only $2.2\hbox {$^\prime $ }$ away, which slightly influences the background estimation (together with two nearby bright stars). The strong peak at $\sim$ $20\hbox {$^{\prime \prime }$ }$ in the final profile is related to the ring around the prominent bar and the dip at $\sim$ 35 $^{\prime \prime }$ to the inter-arm region of the two symmetric spiral arms peaking at $\sim$ 40 $^{\prime \prime }$ . Although possible to fit (at least for the $r^{\prime }$ band profile) with a single exponential (Type I), we classify the galaxy as Type II.o-OLR, with a break around twice the bar radius at $\sim$ $40\hbox {$^{\prime \prime }$ }$ , having an inner disk region too small to be detected with our automatic break searching routine. This is consistent with the classification and profile by Erwin et al. (2006). The region inside $\sim$ $40\hbox {$^{\prime \prime }$ }$ is excluded for the fit of the outer scalelength.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f034.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f035.ps} \par\end{figure}$ IC 1125: Type I
J153305.6-013742 .S..8* 7.7 -20.05 1.7 2868

According to the coordinates in NED the companion (KPG 467A) in Karachentsev's Isolated Pairs of Galaxies Catalogue Karachentsev (1972) corresponds only to a faint starlike object about $11\hbox {$^{\prime \prime }$ }$ away. The small bump in the radial profile at $\sim$ 40 $^{\prime \prime }$ corresponds to an outer spiral arms. Otherwise we see no obvious deviation from a single exponential and therefore the galaxy is classified as Type I.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f036.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f037.ps} \par\end{figure}$ IC 1158: Type II.o-CT
J160134.1+014228 .SXR5* 5.3 -19.36 2.2 2018

Galaxy shows clearly a truncated profile with an extended break region, starting approximately at the end of the spiral arms. The center looks like a secondary bar with a small ring embedded in larger bar of size roughly $\protect\la$ $22\hbox {$^{\prime \prime }$ }$ (without any noticeable feature in the final profile). So the break with downbending profile at $\sim$ $60\hbox {$^{\prime \prime }$ }$ is well beyond a typical Type II.o-OLR break.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f038.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f039.ps} \par\end{figure}$ NGC 0450: Type II.o-CT
J011530.8-005138 .SXS6* 6.0 -19.63 3.0 1712

A background galaxy (UGC 00807, 11587km s^-1 ) is superimposed. The mean ellipticity of the outer disk is difficult to determine. The inner disk looks fairly round whereas the outer disk looks rather elliptical. The size of the slightly more elliptical inner part, associated to be the bar (although without any noticeable feature in the final profile), is roughly $\sim$ 8 $^{\prime \prime }$ , so the break with the downbending profile at $\sim$ 84 $^{\prime \prime }$ is well beyond a typical Type II.o-OLR break and roughly outside the spiral arm region.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f040.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f041.ps} \end{figure}$ NGC 0701: Type II.i (possible Type I)
J015103.8-094209 .SBT5. 5.1 -19.74 2.5 1729

Galaxy is in a multiple system together with NGC 0681 and NGC 4594 (where PGC 006667 (see below) is also part of) with an additional small physical companion (IC 1738, v=1750 km s^-1 ) about $6\hbox {$^\prime $ }$ away. Galaxy close to our high axis ratio limit so the dust may have some influence. The inner region shows no nucleus, so the centering is done from the outer isophotes. The extend of the bar is unknown, but the visible bump at $45\hbox {$^{\prime \prime }$ }$ is probably not related to a bar. It is possible to construct a break at $45\hbox {$^{\prime \prime }$ }$ (which would be more pronounced in the $g^{\prime }$ band), but the inner drop could be also due to the higher inclination with dust and/or patchy star formation affecting the profile.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f042.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f043.ps} \end{figure}$ NGC 0853: Type III
J021141.5-091817 .S..9P 8.3 -18.42 1.5 1405

The inner region shows no clear nucleus but many ${\rm H}$ II regions, so the centering is done from the outer isophotes. The inner disk is slightly asymmetric with an additional light patch in the western part, therefore mean ellipticity and PA difficult to fix. Almost continuously upbending profile beyond the peak at 15 $^{\prime \prime }$ , which includes all ${\rm H}$ II regions, getting flat at $\sim$ 42 $^{\prime \prime }$ . The inner profile is rather curved and not well approximated with a single exponential. The apparent outer break at $\sim$ 100 $^{\prime \prime }$ is only due to the improper fixed ellipse fit in the outer parts.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f044.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f045.ps} \end{figure}$ NGC 0941: Type II-CT
J022827.9-010906 .SXT5. 5.4 -19.02 2.5 1535

Galaxy shows only a very small, point-like nucleus and is in a small group of galaxies (including NGC 936 and NGC 955). The small dip at $\sim$ 40 $^{\prime \prime }$ is associated with the inner spiral arm region. Although classified as SAB no real bar visible on image or in the profile thus the downbending break is classified as Type II-CT.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f046.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f047.ps} \end{figure}$ NGC 1042: Type II-AB
J024023.9-082558 .SXT6. 6.1 -19.83 4.4 1264

A large scale gradient (from top to bottom) in the background of the $r^{\prime }$ and $g^{\prime }$ band image is removed with a linear fit. Only partly fitted since $\protect\la$ 1/3 of galaxy is beyond SDSS field. Galaxy shows an asymmetric (frayed) extension towards the south-east and a sharper edge towards the north-west, which makes it not really lopsided but looking rather like being affected by moving in a dense IGM. The extended (frayed) spiral arms build the outer disk, so ellipticity and PA very difficult to fix. The inner bump in the profile at $\sim$ 90 $^{\prime \prime }$ is due to spiral arms. The inner profile is below the inward extrapolation of the outer disk, but due to the asymmetric shape of the disk we call this galaxy only Type II-AB.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f048.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f049.ps} \end{figure}$ NGC 1068 $\equiv$ M 77: Type II.o-OLR
J024240.8-000048 RSAT3. 3.0 -21.69 7.6 1068

Only partly fitted since $\protect\la$ 1/3 of galaxy is beyond the SDSS field. Galaxy appears to have an inner disk, elongated into a bar-like structure sitting in an outer disk with clearly different PA and with indication for an additional outer ring at $\sim$ 200 $^{\prime \prime }$ . According to Erwin (2004) it is a double-barred galaxy with an inner bar of size $\sim$ 15-20 $^{\prime \prime }$ and an outer bar which is very oval (not very strong) and very large (extending out to < $\sim~$ 100 $^{\prime \prime }$ ; as seen by e.g. Schinnerer et al. 2000). The galaxy looks in this sense similar to NGC 5248 (Jogee et al. 2002). This peculiar shape makes its very difficult to decide on a mean ellipticity and PA of the outer disk from the photometry. The position of the outer ring corresponds to the downbending break at $\sim$ 190 $^{\prime \prime }$ and is therefore roughly twice the bar radius. This suggests the Type II.o-OLR classification, although the profile looks at first glance more like a Type III with a break at $\sim$ 100 $^{\prime \prime }$ .

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f050.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f051.ps} \end{figure}$ NGC 1084: Type III
J024559.7-073437 .SAS5. 5.1 -20.20 3.2 1299

A large scale gradient (from top to bottom) in the background of the $r^{\prime }$ band image is removed with a linear fit. Slightly inclined galaxy sitting clearly in a more roundish outer envelope, beyond which some stream-like remnants of a possible recent interaction are visible. Small edge-on galaxy along the stream path is confirmed to be only a background galaxy. According to SDSS spectroscopy there is another object inside the disk (RA: 02 46 00.3, Dec -07 34 17) with similar velocity and associated to a visible light concentration. The peculiar shape of the outer disk region makes it very difficult to decide on a mean ellipticity and PA from the photometry. The resulting profile inside the break at $\sim$ 90 $^{\prime \prime }$ is rather curved towards the center with additional kinks ( $\sim$ 25 $^{\prime \prime }$ and $\sim$ 50 $^{\prime \prime }$ ), so it is not clear what the galaxy might be inside the Type III envelope.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f052.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f053.ps} \end{figure}$ NGC 1087: Type III
J024625.2-002955 .SXT5. 5.3 -20.46 3.7 1443

An apparent faint low surface brightness (center-less) structure towards the North is only scattered light from a nearby star. The galaxy center is not well defined, it shows only a small bar-like structure with a double nucleus, so we used the slightly lopsided (but symmetric) outer disk for centering, which accounts for the central drop inside $\sim$ 50 $^{\prime \prime }$ in the final profile. There is no spiral structure visible in the outer disk. The transition seems to be rather sharp, but the inner profile is almost curved, so it is not clear what its break type is inside the Type III envelope.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f054.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f055.ps} \end{figure}$ NGC 1299: Type III
J032009.4-061550 .SBT3? 3.2 -19.25 1.2 2197

Galaxy is small and close to our high axis ratio limit. The background exhibits a gradient but the galaxy is small enough to avoid fitting it. SDSS spectroscopy detects an object 0.2 $^\prime$ away from center with similar velocity. The rather symmetric outer disk shows no spiral structure but has slightly different ellipticity and PA compared to the inner part. The shoulder in the profile at $\sim$ 15 $^{\prime \prime }$ is related to the inner (bar-like) region with changing PA.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f056.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f057.ps} \end{figure}$ NGC 2541: Type II-CT
J081440.1+490341 .SAS6. 6.2 -18.50 5.8 734

Galaxy with low surface brightness disk, having many patchy SF knots and an asymmetric (not well described with an ellipse), lopsided outer disk, which makes the chosen ellipticity and PA of the disk uncertain. The central peak is off by $\sim$ $8\hbox {$^{\prime \prime }$ }$ compared to the outer disk where the centering is done, which causes the dip in the final profile close to the center. The downbending break at $\sim$ 140 $^{\prime \prime }$ is still inside the nearly symmetric part of the disk, thus classified as Type II-CT but this should be taken with some caution. This galaxy was classified as SB in our original LEDA catalogue but has been recently reclassified being now SAB. However, NED lists this galaxy as SA, using the RC3 classification, which is consistent with no bar being visible on the image or in the profile, so the downbending break is not a Type II.o-OLR break.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f058.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f059.ps} \end{figure}$ NGC 2543: Type II.i
J081258.0+361516 .SBS3. 3.1 -20.66 2.5 2590

According to NED there is a dwarf elliptical galaxy (KUG 0809+363) at a similar distance. On the SDSS image (confirmed with DSS) there is an additional, low surface brightness structure visible at RA 08 13 08.5 and DEC +36 16 35, which is possibly another dwarf companion with an unknown distance. The galaxy is clearly double barred with a $R\sim 9\hbox {$^{\prime \prime }$ }$ long secondary bar. Two bright, s-shaped spiral arms dominate the inner disk. The extended spiral arm towards the north-east is responsible for a slightly asymmetric outer disk. This structure makes the photometric measurement of the inclination (ellipticity) and PA very difficult. The bar and pseudo-ring build by the inner spiral arms are responsible for the prominent bump at $\sim$ 35 $^{\prime \prime }$ in the profile, followed by a dip inside, which leads to the Type II.i classification.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f060.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f061.ps} \end{figure}$ NGC 2684: Type II-CT
J085454.1+490937 .S?... 7.8 -19.76 1.0 3043

The rich cluster in background, with significantly redder colour, forces a large background mask covering a small part of the galaxy. Slightly asymmetric disk with bright center and no coherent spiral arms makes ellipticity and PA uncertain. Bump at $\sim$ 12 $^{\prime \prime }$ in profile is due to an inner ring-like structure, without an associated obvious bar structure. The break at $\sim$ 25 $^{\prime \prime }$ is not related to a morphological feature in the disk and, although at about twice the ring radius, classified as Type II-CT. The upbending profile starting at $\sim$ 42 $^{\prime \prime }$ is most probably due to an improper sky subtraction caused by extended light from the background cluster.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f062.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f063.ps} \end{figure}$ NGC 2701: Type II-AB + III
J085905.9+534616 .SXT5* 5.1 -20.36 2.1 2528

According to NED there is a small companion (with similar velocity) superimposed on the galaxy disk towards the South at the end of a spiral arm which is masked here in addition to the bright star on the disk towards the West. The galaxy has a lopsided disk with the bar being offcenterd compared to the outer isophotes, where the centering is done. This is responsible for the dip in the center an possibly for the break at $\sim$ 42 $^{\prime \prime }$ , which is therefore called Type II-AB. The region beyond the second break at $\sim$ 70 $^{\prime \prime }$ corresponds to some faint, almost symmetric light around the galaxy with some large extension towards north-east, adding the classification Type III. This is possibly triggered by interaction with the dwarf companion at the other side.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f064.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f065.ps} \end{figure}$ NGC 2776: Type I
J091214.3+445717 .SXT5. 5.1 -21.04 2.9 2796

The galaxy is classified as SAB but a bar is not obvious on the image. The background estimate is uncertain due to a nearby (off-field), extremely bright star. For the final profile we used a round ellipticity instead of the usual value at $1\sigma$ (cf. Sect. 3.5) which gives an almost prototypical Type I profile with some minor wiggles, a bump at $\sim$ $25\hbox {$^{\prime \prime }$ }$ due to the inner spiral arms, and some outer bumps due to some very weak spiral arm structures in the outer disk.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f066.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f067.ps} \end{figure}$ NGC 2967: Type III-d
J094203.3+002011 .SAS5. 4.8 -20.26 2.6 1858

The galaxy is close to the edge of the SDSS field in an area with an increased background which is masked. Very faint, extended, but symmetric spiral arms inside the outer disk at $\sim 100\hbox {$^{\prime \prime }$ }$ are visible, which do not continue inwards but start beyond the bump in the transition region at $\sim$ 75 $^{\prime \prime }$ . The exact break radius is therefore uncertain.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f068.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f069.ps} \end{figure}$ NGC 3055: Type II.o-CT
J095517.9+041611 .SXS5. 5.0 -19.90 2.1 1816

Galaxy is classified as SAB and shows a narrow, thin bar, with the spiral arm structure wrapped around, which is responsible for the bump in the final profile at $\sim$ 18 $^{\prime \prime }$ . The break with a downbending profile at $\sim$ 55 $^{\prime \prime }$ is well beyond a typical Type II.o-OLR break.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f070.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f071.ps} \end{figure}$ NGC 3246: Type II-AB
J102641.8+035143 .SX.8. 8.0 -18.91 2.2 2138

Galaxy is selected from the NGC catalogue Tully (1988) by (Pisano & Wilcots 1999) as being isolated. Their ${\rm H}$ I measurements show a lopsided disk which resembles the one on the present SDSS image. The central bar region is clearly offcenterd compared to the outer isophote, which is used for the centering. The downbending break in the final profile and the downbending at the very center is therefore most probably only an apparent break due to the fixed ellipse fitting. Thus the galaxy is classified as Type II-AB. The background is rather disturbed by a bright star, but the galaxy is small enough not to be significantly influenced.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f072.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f073.ps} \end{figure}$ NGC 3259: Type III-d
J103234.8+650228 .SXT4* 4.0 -19.84 2.1 1929

The background is rather disturbed by a bright star, but the galaxy is small enough not to be significantly influenced. Galaxy is isolated according to Prada et al. (2003), but has one SDSS-detected dwarf companion ( $\sim$ 18.0 $g^{\prime }$ -mag) about 10 $^\prime$ away with similar velocity (v=1744 km s^-1 ) and another possible, dwarf companion (or large ${\rm H}$ II region) projected on the south part of the disk (no counterpart in NED), which is partly covered by a foreground star, but also clearly present on the DSS image. The break region of the upbending profile at $\sim$ $55\hbox {$^{\prime \prime }$ }$ is fairly extended and curved. The inner profile shows wiggles at $\sim$ 15 $^{\prime \prime }$ and $\sim$ 30 $^{\prime \prime }$ , but the resolution is too low to identify a bar or ring. The spiral structure apparently extends into the outer disk well beyond the break, with two, thin symmetric spiral arms (plus more fluffy ones) starting at the defined break radius. However, it is not clear if they are really the continuation of the inner arms. The upbending characteristic is confirmed by a profile shown in Courteau (1996) (see UGC 05717).

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f074.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f075.ps} \end{figure}$ NGC 3310: Type III
J103845.8+533012 .SXR4P 4.0 -20.25 2.8 1208

The galaxy is clearly disturbed with a shell-like structure in the outer disk, which is probably the result of a recent merger with a smaller galaxy (cf. Conselice et al. 2000). The inner region is also slightly asymmetric, but still used for centering. The inner region, corresponding to a high surface brightness, tightly wound spiral, inside the break at $\sim$ 50 $^{\prime \prime }$ , is curved starting at $\sim$ 20 $^{\prime \prime }$ . The wiggles in the outer disk are due to the shells. An additional upbending beyond $\sim$ 150 $^{\prime \prime }$ is due to a prominent outer shell. The very outer parts are in addition influenced by an inhomogeneous sky and a large mask.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f076.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f077.ps} \end{figure}$ NGC 3359: Type II-AB
J104636.3+631328 .SBT5. 5.0 -20.42 7.2 1262

The inner disk shows an extended bar (roughly $R\sim\!45$ $^{\prime \prime }$ ), which is not visible in the final profile, and two bright spiral arms. The broad extension of this arms build the outer disk, so there is no clear elliptical outer structure visible which makes the photometric inclination (ellipticity) and PA measurements highly uncertain. The outer slope is influenced by a rather uncertain sky estimate in both bands, but the apparent downbending break at $\sim$ 200 $^{\prime \prime }$ is not due to a sky error, but coincides with the region where the two outer arms dominate. Thus the galaxy is classified as Type II-AB.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f078.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f079.ps} \end{figure}$ NGC 3423: Type II-CT
J105114.3+055024 .SAS6. 6.0 -19.54 3.9 1032

Bulge-like inner region ( $\protect\la$ 30 $^{\prime \prime }$ ) coincides with inner high surface brightness disk with spiral structure. Final profile is clearly downbending but the exact break radius is difficult to place due to an extended feature around $\sim$ 70 $^{\prime \prime }$ corresponding to an aligned spiral arm (with a possible straight structural element towards the north-east, called (Chernin 1999) spiral-arm row).

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f080.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f081.ps} \end{figure}$ NGC 3488: Type II.o-CT
J110123.6+574039 .SBS5* 5.1 -18.80 1.6 3226

Galaxy is isolated according to Prada et al. (2003). A bright star covering part of the outer disk needs an extended mask. A small bar of roughly $R\sim\!6\hbox{$^{\prime\prime}$ }$ size is visible as an elongated isophote on the image. The final profile is clearly downbending, but the exact break radius is difficult to place. The extended break region resembles in this case again a straight line, thus one could also define two break radii at $\sim$ 32 $^{\prime \prime }$ and $\sim$ 58 $^{\prime \prime }$ . This could be caused by the extended mask, whereas the spiral structure extending to $\sim$ 40 $^{\prime \prime }$ seems not to be responsible for this behaviour. The bar is to small for its OLR to be associated with the first break, thus the galaxy is classified Type II.o-CT. The light beyond $\sim$ 58 $^{\prime \prime }$ is still symmetric and not affected by sky errors. The peak at $\sim$ 20 $^{\prime \prime }$ corresponds to the inner two arms.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f082.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f083.ps} \end{figure}$ NGC 3583: Type III-d
J111411.0+481906 .SBS3. 3.2 -19.57 2.3 2347

The apparent companion, a spiral galaxy (NGC 3577) towards the south-west is non-physical with v=5336 km s^-1 . The galaxy shows a stream-like arm extending towards the north-west outside of the galaxy connected to a small superimposed E0 satellite at $0.9\hbox {$^\prime $ }$ north (not in NED). Due to this structure the outer disk seems to have a slightly different ellipticity and PA. The bump at $\sim$ 30 $^{\prime \prime }$ in the final profile is due to the end of the bar and beginning of spiral arms. The inner profile with an extended wiggle at $\sim$ 55 $^{\prime \prime }$ (corresponding to the spiral arms) makes it difficult to characterise the break region (starting at $\sim$ 85 $^{\prime \prime }$ with an upbending profile) as being curved or sharp.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f084.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f085.ps} \end{figure}$ NGC 3589: Type II-CT
J111513.2+604201 .S..7* 7.0 -18.49 1.5 2217

Due to the higher inclination and extended elongated structure the size of the bar is not well defined. The center is also not well defined, but centering on the outer isophote coincides roughly with the brightest pixel. The sky estimate is rather uncertain due to the bright star in the FOV. The final profile shows a downbending break at $\sim$ 40 $^{\prime \prime }$ , classified as Type II-CT but also consistent with being Type II.o-OLR allowing the bar to be of size $\sim$ 20 $^{\prime \prime }$ which is consistent with the image. The small bump $\sim$ 22 $^{\prime \prime }$ in the profile just corresponds to some aligned ${\rm H}$ II regions.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f086.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f087.ps} \end{figure}$ NGC 3631: Type I
J112102.4+531008 .SAS5. 5.1 -20.62 4.9 1388

The galaxy forms a nearby group together with NGC 3178, NGC 3898, NGC 3953 and NGC 3992 (also part of our sample) in the Ursa Major cluster and shows plenty of substructure. It has two prominent spiral arms with different pitch angles, one of them turns nearly straight, classified by Arp (1966) as a spiral galaxy with one heavy arm. In addition, it has a faint extended spiral arm (or maybe stream-like structure) in the far outer disk towards North, therefore the outer disk is slightly asymmetric and the mean ellipticity and PA are difficult to fix. There is an extended light patch on the image visible towards south-west. Although there is no bright star nearby which could create such an artefact it is unlikely a dwarf companion, since it is not visible on the DSS. The final radial light profile is quite unusual and cumbersome to classify, since it exhibits an extended bump between $\sim$ 50-140 $^{\prime \prime }$ , which corresponds to the begin of the two spirals to the end of the inner (undisturbed) disk. Beyond $\sim$ 140 $^{\prime \prime }$ the extended, slightly offcenterd outer disk with the spiral arm structure (or stream) starts. If we do not exclude the bump from the fit, one can argue for a downbending break at $\sim$ 75 $^{\prime \prime }$ , or a Type I profile with an extreme wiggle (this would be a Type II.i if the galaxy would be barred). We decided to exclude the bump and the inner region from the fit ( $R \protect~\rlap{\lower -0.5ex\hbox{$>$ }}{\lower 0.5ex\hbox{$\sim~$ }}140$ $^{\prime \prime }$ ) which gives also a Type I profile where the region around $\sim$ 35 $^{\prime \prime }$ is also roughly fitted. Due to this problems the classification should be taken with caution.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f088.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f089.ps} \end{figure}$ NGC 3642: Type III-d
J112218.0+590427 .SAR4* 4.0 -20.60 5.5 1831

The background is slightly inhomogeneous and the galaxy is rather extended. From the nearly round inner disk a single, star forming, spiral arm starts towards the outer disk with slightly more than one revolution, forming the strongly asymmetric, lopsided outer disk. Therefore the ellipticity and PA is determined further inside. The final profile looks fairly curved and with extended wiggles in the outer disk at $\sim$ 100 $^{\prime \prime }$ and $\sim$ 155 $^{\prime \prime }$ due to the outer spiral arm passing the ellipse. There is a steeper inner exponential part visible between $\sim$ 25-75 $^{\prime \prime }$ followed outwards by an upbending profile, which is roughly at the position where the extended spiral arm starts to unwrap, which leads to the Type III classification. Inwards of $\sim$ 25 $^{\prime \prime }$ there is again another steeper exponential part visible together with a possible bulge component.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f090.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f091.ps} \end{figure}$ NGC 3756: Type II.o-CT
J113648.3+541737 .SXT4. 4.3 -19.89 3.8 1525

Only partly fitted since $\protect\la$ 1/4 of galaxy is beyond field. Known three armed spiral galaxy which shows one wide spiral arm starting at $\sim$ 60 $^{\prime \prime }$ extending roughly towards the downbending break at $\sim$ 100 $^{\prime \prime }$ . The extended bump $\sim$ 45 $^{\prime \prime }$ is due to the three inner tightly wound spiral arms and makes it, similar to NGC 3631, difficult to fit the inner region. However, since the bump is less strong we decided to include it. The galaxy is classified as SAB (RC3) but the bar is not obvious on the image and its maximum size would be $R \protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}25\hbox{$^{\prime\prime}$ }$ thus the break is well outside the range for typical Type II.o-OLR breaks and is classified as Type II.o-CT.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f092.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f093.ps} \end{figure}$ NGC 3888: Type I
J114734.7+555800 .SXT5. 5.3 -20.43 1.8 2648

The background on the image shows a large gradient due to a bright star off the field, but the galaxy is small enough to be not affected. The galaxy has one "malformed'' (kinked) spiral arm across the disk. There is a possible dwarf, irregular companion visible towards the south-west, but without any distance information. The final profile exhibits an extended wiggle (with an unusual integral sign shape) at $\sim$ 33 $^{\prime \prime }$ , looking like two shifted exponential regions, but there is no point in placing a break there. The peak at $\sim$ 22 $^{\prime \prime }$ is related to an aligned spiral arm, whereas the peak at $\sim$ 12 $^{\prime \prime }$ could be due to the end of a possible bar or inner ring (no obvious on the image). Therefore the galaxy is classified as Type I and not as Type II.i, although the dip in the profile is clearly visible. It could be explained by dust lanes close to the center, which also explains the dip being more prominent in the $g^{\prime }$ band.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f094.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f095.ps}\par \end{figure}$ NGC 3893: Type III-d
J114838.4+484234 .SXT5* 4.8 -20.33 4.1 1193

The background around the galaxy is affected by a nearby, bright star and a close (3.7 $^\prime$ away, with similar velocity v=905 km s^-1 , SB0/a:pec), smaller, companion galaxy (NGC 3896), both members of the Ursa Major Cluster. Galaxy exhibits a wide, extended spiral arm like structure towards the east, which could also be a stream or tidal feature. Due to this structure it is not possible to derive the ellipticity and PA from the outer disk, so their values are more uncertain. The final profile clearly shows an Type III upbending profile starting at $\sim$ 150 $^{\prime \prime }$ corresponding to the beginning of the extended structure to one side and some more symmetric faint light on the other side. The inner disk shows a prominent wiggle $\sim$ 90 $^{\prime \prime }$ which is associated to a pseudoring of wrapped spiral arms.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f096.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f097.ps} \end{figure}$ NGC 3982: Type III
J115628.3+550729 .SXR3* 3.2 -19.54 2.3 1351

Close to Ursa Major Cluster but membership questionable (Tully et al. 1996). Galaxy exhibits a detached, narrow, starforming spiral arm embedded into the very outer, symmetric disk towards south-west. The final profile beyond the central part is smooth and straight down to $\sim$ 55 $^{\prime \prime }$ where it clearly starts upbending, classified as Type III, which is consistent with the profile by (Tully et al. 1996). The break corresponds to the end of the inner disk, excluding the faint outer arm, which produces the bump at $\sim$ 75 $^{\prime \prime }$ (more pronounced in the $g^{\prime }$ band). The transition zone is rather sharp. Dip-peak structure between $\sim$ 5-12 $^{\prime \prime }$ corresponds to the inner bar/ring region. The exact size of the bar is not well determined on the SDSS image. Erwin (2005), using HST images, gives 5 $^{\prime \prime }$ and classifies the galaxy therefore as Type II.o-OLR + III (with an "extreme'' OLR break). We exclude the inner $R\protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}13\hbox{$^{\prime\prime}$ }$ from our fit and leave it with a Type III classification.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f098.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f099.ps} \end{figure}$ NGC 3992 $\equiv$ M 109: Type II.o-OLR
J115735.9+532235 .SBT4. 3.8 -20.98 6.9 1286

Large galaxy with a small part off the SDSS field. Member of Ursa Major Cluster (Tully et al. 1996). Embedded in the large bar of size roughly $R\sim 70\hbox {$^{\prime \prime }$ }$ (as measured on the image) is possibly a secondary bar half the size. Unusual very faint extension visible in both bands (more pronounced in $g^{\prime }$ band) towards north-east, which is possibly but unlikely stray-light from a nearby bright, red star. The one-sigma ellipse is therefore not representative so the mean ellipticity and PA are determined further inside. Final profile shows a clear downbending break at $\sim$ 140 $^{\prime \prime }$ at about twice the bar radius corresponding roughly to a pseudoring of the spiral arms, therefore classified as Type II.o-OLR. Bump at $\sim$ 200 $^{\prime \prime }$ does not coincide with a spiral arm.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f100.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f101.ps} \end{figure}$ NGC 4030: Type III
J120023.4-010603 .SAS4. 4.1 -20.27 3.9 1476

Two superimposed bright stars are masked. According to Zaritsky et al. (1993) it is an isolated galaxy with a satellite system (largest UGC 06970, SB(s)m, with $\hbox{$M_{\rm abs}$ }~=-17.7$ ). The galaxy shows two prominent spiral arms beyond a more flocculent center starting at $\sim$ 30 $^{\prime \prime }$ , followed by a single arm extending slightly further out towards south-west. Final profile shows a Type III break at $\sim$ 150 $^{\prime \prime }$ where the transition zone is rather sharp, followed by a fairly symmetric outer region without spiral structure. The bump at $\sim$ 80 $^{\prime \prime }$ corresponds to the end of inner spiral arms.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f102.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f103.ps} \end{figure}$ NGC 4041: Type III-d
J120212.2+620814 .SAT4* 4.3 -19.92 2.7 1486

According to Sandage & Bedke (1994) this galaxy forms a kinematic triplet with NGC 4036 and UGC 7009 and is probably member of the Ursa Major Cluster. However, Tully et al. (1996) does not list any of these as members. Galaxy shows a detached, extended, star-forming spiral arm structure in the outer, asymmetric disk, similar to NGC 2967, but smaller and only one-sided, which makes the photometric inclination (ellipticity) and PA uncertain. In the final profile the disk inside the Type III break at $\sim$ 75 $^{\prime \prime }$ corresponds roughly to the region with the spiral arms, which are also responsible for the extended bump between $\sim$ 30-75 $^{\prime \prime }$ (more pronounced in $g^{\prime }$ band). The very inner region looks bar-like, but is probably only the spiral structure continuing into the center.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f104.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f105.ps} \end{figure}$ NGC 4102: Type II.o-OLR + III
J120623.1+524239 .SXS3$ 3.0 -19.38 3.1 1082

Galaxy belongs to the Ursa Major Cluster Tully et al. (1996). On the image an elongated inner bar region inside a starforming ring is visible which is responsible for the dip and bump structure between $\sim$ 25-35 $^{\prime \prime }$ in the final profile. Erwin (2005) measures the size of the bar to $\sim$ 15 $^{\prime \prime }$ and the outer ring to $\sim$ 35 $^{\prime \prime }$ , so the apparent break at $\protect~\rlap{\lower -0.5ex\hbox{$>$ }}{\lower 0.5ex\hbox{$\sim~$ }}40\hbox{$^{\prime\prime}$ }$ (although measured from outside, it starts only at $\sim$ 58 $^{\prime \prime }$ ) is classified as a Type II.o-OLR. The apparent upbending at $\sim$ 120 $^{\prime \prime }$ is unlikely a sky error, visible around the whole galaxy and confirmed by the profile in Courteau (1996) (see UGC 07096) and also visible in Erwin et al. (2006). This adds the Type III classification.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f106.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f107.ps} \end{figure}$ NGC 4108: Type II-AB
J120644.0+670944 PSA.5* 5.0 -20.13 1.7 2828

Galaxy in a triple system with NGC 4108A (v=2256 km s^-1 ) and NGC 4108B (v=2673 km s^-1 ), the latter is also part of the present sample. According to Nordgren et al. (1997) NGC 4108 and NGC 4108B appear to be possibly joined by an ${\rm H}$ I bridge. Very inner center $\protect\la$ $5\hbox {$^{\prime \prime }$ }$ looks like small bar, or the spiral structure starts from the very center. The outer disk is asymmetric with one side rather sharp and the other more shallow with indication for a single spiral arm. The disk is lopsided, so the outer contour is used for centering (center $\sim$ 4 $^{\prime \prime }$ off the brightest pixel, causing the central dip in the profile), which implies that the photometric inclination (ellipticity) and PA are not well defined. The apparent break at $\sim$ 44 $^{\prime \prime }$ is related to the transition between the symmetric outer disk going inwards to the offcenterd inner disk and therefore most probably not intrinsic but a Type II-AB break.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f108.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f109.ps} \end{figure}$ NGC 4108B: Type I
J120711.3+671410 .SXS7P 7.0 -18.46 1.3 2840

Companion to NGC 4108 (see above). Galaxy exhibits an offcentered bar ( $\sim$ 5 $^{\prime \prime }$ off compared to the center derived from the outer isophote). Very outer disk slightly asymmetric towards north-east (outer spiral arm?). In the final profile the central dip and inner wiggle are due to the the offcentered bar, the peak at $\sim$ 22 $^{\prime \prime }$ corresponds to an aligned spiral arm-like region. Although a downbending break at $\sim$ 32 $^{\prime \prime }$ with low scalelength contrast is possible, Type II-AB, the galaxy is consistent and classified as Type I due to the wiggles in the center.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f110.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f111.ps} \end{figure}$ NGC 4123: Type I
J120811.1+025242 .SBR5. 4.8 -19.55 4.1 1364

Galaxy with extended bar ( $R\sim\!55$ $^{\prime \prime }$ ) studied in detail by Weiner et al. (2001) using a surface brightness profile which is consistent with the SDSS one. The outer disk is slightly asymmetric, more rectangular than elliptical, with an extended starforming spiral arm structure towards south-west, which makes the photometric inclination (ellipticity) and PA uncertain. The final profile exhibits extended wiggles. The bar and associated spiral arms are visible between $\sim$ 30-110 $^{\prime \prime }$ and the bump at $\sim$ 170 $^{\prime \prime }$ corresponds to a starforming outer spiral arm. Although being far from a prototypical Type I we used this classification, since the profile shows too many changes to reasonably argue for any other type.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f112.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f113.ps} \end{figure}$ NGC 4210: Type II.o-OLR + II.o-CT
J121515.9+655908 .SBR3. 3.0 -19.89 2.0 3000

Companion galaxy (CGCG 315-030, m=15.5) 13 $^\prime$ away with similar velocity (v=2679 km s^-1 ). Gradient in the background due to a very bright star (off field), but galaxy small enough to be not significantly influenced. The final profile shows an inner bump at $\sim$ 15 $^{\prime \prime }$ corresponding to a pseudoring of wrapped spiral arms (slightly further out than the bar). The apparent dip $\sim$ 8 $^{\prime \prime }$ is due to the bar orientation being perpendicular to the major axis of the galaxy. Similar to NGC 3488 the profile shows a clear downbending. However, the break radius is uncertain due to the extended break region, which resembles in this case again a straight line. Thus one could also define two break radii at $\sim$ 33 $^{\prime \prime }$ , corresponding roughly to end of inner spiral arm structure, and $\sim$ 55 $^{\prime \prime }$ , not related to sky errors and symmetric around the disk. In contrast to NGC 3488 the bar is here large enough to argue for a combination of a Type II.o-OLR and a Type II.o-CT break, this should be confirmed with a more detailed study on the bar size of NGC 4210.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f114.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f115.ps} \end{figure}$ NGC 4273: Type II-AB + III
J121956.2+052036 .SBS5. 5.1 -20.41 2.1 2435

Galaxy in south-western corner of the Virgo Cluster with three similar sized neighbours, NGC 4268, NGC 4281, and closest and slightly overlapping at the very outer disk NGC 4277. The disk is lopsided with one side sharp edged and the other side with a wide spiral arm feature towards south-east (embedded in the outer disk), similar to NGC 4108. Centering on the outer disk causes the dip at $\sim$ 10 $^{\prime \prime }$ and hides the very bright nucleus sitting in a bar-like structure which is offcentered by $\sim$ 16 $^{\prime \prime }$ . The break at $\sim$ 45 $^{\prime \prime }$ in the final profile is clearly related to the lopsided disk and therefore classified as Type II-AB. In addition, there is an Type III break with an upbending profile visible beyond $\sim$ 80 $^{\prime \prime }$ due to the influence of the companion (possibly intrinsic and not just projected).

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f116.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f117.ps} \end{figure}$ NGC 4480: Type II.o-CT
J123026.8+041447 .SXS5. 5.1 -20.14 2.1 2494

The galaxy is small, rather inclined, and classified as SAB with bar size of roughly $R\sim\!10\hbox{$^{\prime\prime}$ }$ (measured from the image). The final profile shows a clear downbending break at $\sim$ 55 $^{\prime \prime }$ , significantly further out compared to a typical Type II.o-OLR break thus classified as Type II.o-CT, corresponding roughly to the end of the spiral arms. The inner profile exhibits an extended bump at $\sim$ 35 $^{\prime \prime }$ (more pronounced in the $g^{\prime }$ and less in the $i^{\prime }$ band) most probably related to the star formation in the spiral arms and not to a possible Type II.o-OLR + II.o-CT as for NGC 4210, which shows the same structure in both bands.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f118.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f119.ps} \end{figure}$ NGC 4517A: Type II.o-CT + II.o-AB
J123228.1+002325 .SBT8* 7.9 -19.18 3.8 1562

This low surface brightness galaxy has an elongated, barred center, of size $R\sim\!30$ $^{\prime \prime }$ , with a foreground star very close and a slightly asymmetric, lopsided outer disk. The final profile exhibits a sharp break at $\sim$ 150 $^{\prime \prime }$ due to the asymmetric outer disk, which is not well described with the mean ellipticity and PA used, thus classified as Type II-AB. There is an additional feature (bump or break) visible around $\sim$ 80 $^{\prime \prime }$ , which is not obviously related to an aligned spiral arm and could be explained by a weak downbending break. Since the bar appears to be only weak and the break at more than twice the bar radius it is classified as Type II.o-CT, which should be taken with caution.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f120.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f121.ps} \end{figure}$ NGC 4545: Type II.o-CT
J123434.2+633130 .SBS6* 5.9 -20.49 2.5 3000

Small galaxy with an s-shaped inner region of size $\sim$ 12 $^{\prime \prime }$ (associated to be the bar) leading to two (or three) tightly wrapped, spiral arms. Final profile exhibits a break at $\sim$ 58 $^{\prime \prime }$ , being too far out for a typical Type II.o-OLR thus classified as Type II.o-CT. The dip at $\sim$ 8 $^{\prime \prime }$ corresponds to the region where the spiral arms start from the bar-structure which is nearly perpendicular to the ellipse major axis.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f122.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f123.ps} \end{figure}$ NGC 4653: Type II-AB
J124350.9-003341 .SXT6. 6.1 -20.37 3.0 2658

Paired galaxy with NGC 4642 (v=2471 km s^-1 , $\sim$ 10 $^\prime$ away) while apparent dwarf companion on the image towards south-east is a confirmed background galaxy (v=7843 km s^-1 ). Extended mask used to avoid straylight by bright stars. Mean ellipticity and PA difficult to determine, since it is different for the inner disk (used for centering) with two, very regular spiral arms inside $\protect\la$ 30 $^{\prime \prime }$ , compared to the outer disk with more frayed spiral fragments, starting to be asymmetric on larger scales at $\protect\la$ $80\hbox {$^{\prime \prime }$ }$ (mainly towards south-west). This asymmetry causes also the apparent break at $\sim$ 105 $^{\prime \prime }$ thus the galaxy is classified as Type II-AB.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f124.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f125.ps} \end{figure}$ NGC 4668: Type III
J124532.0-003209 .SBS7* 7.1 -18.88 1.5 1654

Small galaxy close to our high axis ratio limit, which forms a close pair with NGC 4666 (v=1474 km s^-1 ) about $7\hbox {$^\prime $ }$ away and also has a wider association with NGC 4632 (v=1557 km s^-1 ) according to Sandage & Bedke (1994). The final profile exhibits a break at $\sim$ 70 $^{\prime \prime }$ followed by an upbending profile corresponding to a slightly asymmetric, faint outer disk and although close to, most probably not related to a sky error, thus classified as Type III. The full extend of the bar is uncertain, although the bump around $\sim$ 20 $^{\prime \prime }$ is certainly related to the bar and a possible spiral arm. The whole inner region is included in the inner disk fit.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f126.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f127.ps} \end{figure}$ NGC 4904: Type II.o-OLR + III
J130058.6-000138 .SBS6. 5.7 -18.69 2.1 1213

Only partly fitted since $\protect\la$ 1/5 of galaxy is beyond field. The galaxy has a dominating, thick bar of size $R\protect~\rlap{\lower -0.5ex\hbox{$>$ }}{\lower 0.5ex\hbox{$\sim~$ }}20$ $^{\prime \prime }$ whereas the center along the bar is not well defined (centering on brightest pixel). It has an unusual spiral arm structure with one extending nearly straight towards south-west forming more droplet shaped isophotes. The image shows indication for an additional, extremely faint, extended patch of light outside the disk towards south-west. Final profile shows a clear downbending break at $\sim$ 40 $^{\prime \prime }$ , associated on one side with a ring-like structure which is about twice the bar radius, thus classified as Type II.o-OLR. The apparent upbending at $\sim$ 90 $^{\prime \prime }$ is almost certainly produced by the additional patch of light unrelated to any artificial source, thus adding the Type III classification.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f128.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f129.ps} \end{figure}$ NGC 5147: Type II.o-OLR + III
J132619.2+020604 .SBS8. 7.9 -18.77 1.8 1154

The medium-sized star superimposed on the galaxy close to its center is masked. The bar size is uncertain but could be associated to an elliptical region of size $R\protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}15\hbox{$^{\prime\prime}$ }$ on the image not reflected in the final profile. The extended bump between $\sim$ 25-45 $^{\prime \prime }$ is associated to the inner disk containing the spiral arms with some ring-like, distributed SF regions. Excluding the full region allows for a crude Type I classification. However, using a break at $\sim$ 30 $^{\prime \prime }$ (about twice the bar radius thus classified as Type II.o-OLR) followed by a downbending profile with another break at $\sim$ 75 $^{\prime \prime }$ leading to an upbending profile (therefore classified as Type III) seems more reasonable, even so the upbending is very close to our detection limit. The disk beyond the ring-like structure is slightly asymmetric with a single, wide, and faint spiral arm-like structure towards north-east just inside the outer break. The outermost isophote is again nearly round and symmetric.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f130.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f131.ps} \end{figure}$ NGC 5300: Type II.o-CT
J134816.1+035703 .SXR5. 5.0 -18.93 3.5 1246

Galaxy close to border of SDSS field but almost complete. The size of the weak bar is about $R\sim\!12\hbox{$^{\prime\prime}$ }$ (measured from the image). The final profile shows the prototypical Type II.o-CT behaviour. A sharp break at $\sim$ 85 $^{\prime \prime }$ followed by a downbending profile. The break is way to far out for a normal Type II.o-OLR break given the small bar size, and corresponds roughly to the end of the visible spiral arm structure.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f132.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f133.ps} \end{figure}$ NGC 5334: Type II.o-CT
J135254.4-010651 .SBT5* 5.0 -19.22 3.9 1433

Galaxy has a bar with a visible dust lane of size $R \protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}20$ $^{\prime \prime }$ as measured from the image. The final profile is clearly downbending, but the exact position of the break is difficult to place. The extended break region resembles in this case again a straight line, so that one could also define two break radii at $\sim$ 85 $^{\prime \prime }$ and $\sim$ 125 $^{\prime \prime }$ . However, since the first one is not even close to twice the bar radius and no other particular feature is responsible for the second break, the galaxy is classified Type II.o-CT with a single break at $\protect~\rlap{\lower -0.5ex\hbox{$>$ }}{\lower 0.5ex\hbox{$\sim~$ }}90$ $^{\prime \prime }$ .

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f134.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f135.ps} \end{figure}$ NGC 5376: Type II.o-OLR
J135516.1+593024 .SXR3$ 3.0 -20.00 2.1 2293

Galaxy close to the border of the SDSS field but almost complete. It has a known, similar-sized companion (UGC 08859, v=1610 km s^-1 ) about $7.4\hbox {$^\prime $ }$ away and there is another possible, much fainter dwarf companion ( $3.5\hbox {$^\prime $ }$ away towards north-west) visible on the image. The final profile shows a weak break at $\sim$ 35 $^{\prime \prime }$ coinciding with the end of some very faint spiral arms. The dip at $\sim$ 14 $^{\prime \prime }$ and the peak at $\sim$ $18 \hbox {$^{\prime \prime }$ }$ are related to a pseudoring structure (mentioned also in RC1) around a possible bar. Although the exact size of the bar is difficult to fix, assuming it is there, the break is close to twice the inner ring radius and therefore classified as Type II.o-OLR.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f136.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f137.ps} \end{figure}$ NGC 5430: Type II.o-OLR
J140045.8+591943 .SBS3. 3.1 -20.86 2.2 3238

Galaxy is isolated according to Prada et al. (2003). The center is dominated by a strong bar with dustlanes of size $R\sim\!35$ $^{\prime \prime }$ , followed by two wrapped spiral arms. The very center is slightly elongated, looking twofold (effect of dust lane?), thus the centering is uncertain. The extended bump at $\sim$ 45 $^{\prime \prime }$ in the final profile is associated with the wrapped spiral arms. We have included the bump and bar for fitting the inner scalelength, because it does not change the result much. It is in principle possible to fit the full profile with a single exponential (Type I), allowing for this extended bump. However, we chose to fit a break at $\sim$ 70 $^{\prime \prime }$ . This reduces the deviation from the model and since it is about twice the bar radius the galaxy is classified as Type II.o-OLR.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f138.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f139.ps} \end{figure}$ NGC 5480: Type III-d
J140621.5+504332 .SAS5* 5.0 -19.72 1.7 2119

A large scale gradient (from top to bottom) in the background of the $r^{\prime }$ band image is removed with a linear fit. Galaxy forms a close pair with NGC 5481 (v=2143 km s^-1 ) only $3.1\hbox {$^\prime $ }$ away with the very outer isophotes starting to overlap. Galaxy appears to consist of two regions. An inner disk with the bright center and the spiral arms of size $R\sim\!40$ $^{\prime \prime }$ with a common ellipticity and PA, sitting in a more diffuse outer disk having a different ellipticity and a nearly orthogonal PA. The systems looks like an extended bar in an underlying disk, similar to NGC 1068 and the photometric inclination (ellipticity) and PA is difficult to determine and therefore uncertain. The final profile exhibits a break with an upbending profile at $R\sim\!75$ $^{\prime \prime }$ , thus classified as Type III, which is consistent with the profile shown by Courteau (1996) (cf. UGC 09026). Between the inner disk and the break there is indication for two symmetric, thick spiral arms emerging from the inner bar-like disk.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f140.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f141.ps} \end{figure}$ NGC 5584: Type II.o-CT
J142223.8-002315 .SXT6. 6.1 -19.80 3.2 1702

Bright foreground star nearby but the influence is small. Two additional brighter stars in the outer disk force extended masking. The inner disk is dominated by two prominent spiral arms plus some more asymmetric ones with many starforming patches. The galaxy is classified as SAB, but the bar size ( $R\sim\!10$ $^{\prime \prime }$ ) is difficult to determine, since the spiral arms seem to continue towards the center. Similar to NGC 3488 the profile shows a clear downbending, however, with uncertain break radius due to the extended break region which resembles in this case again a nearly straight line, so that one could also define two break radii at $\sim$ 60 $^{\prime \prime }$ and $\sim$ 110 $^{\prime \prime }$ . Since the bar is too small to be responsible for the inner break we use a single break at $\sim$ 90 $^{\prime \prime }$ enclosing roughly the inner spiral structure followed by a slightly asymmetric outer disk (one side with a clearly more diffuse appearance).

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f142.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f143.ps} \end{figure}$ NGC 5624: Type III
J142635.3+513503 .S?... 5.0 -18.69 1.1 2186

Large scale gradient (from top to bottom) in the background of the $r^{\prime }$ band image is removed with a linear fit. Very small galaxy which is most probably of noticeably later type than classified (Sc). Inner region dominated by an offcenterd (compared to the outer isophote used for centering) narrow bar, or rim-like structure of size $\sim$ 10 $^{\prime \prime }$ which is responsible for the central dip in the profile. The PA of the outermost region is twisted compared to the inner, bar-like structure. The final profile exhibits a straight line starting from $\sim$ 20 $^{\prime \prime }$ (enclosing the central region including the bar having the same PA) down to a break at $\sim$ 45 followed by an upbending profile (classified as Type III) into the more symmetric, diffuse outer disk without visible substructure.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f144.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f145.ps} \end{figure}$ NGC 5660: Type II-CT
J142949.8+493722 .SXT5. 5.1 -20.62 2.8 2585

Galaxy close to the edge of the SDSS field but almost complete sitting in a strip with higher background. According to Sandage & Bedke (1994) it has a small companion nearby ("a likely dwarf Im companion of unknown redshift"), however this could be associated with UGC 09325 (v=3730 km s^-1 ) being clearly a background galaxy. Galaxy shows two, slightly asymmetric inner spiral arms plus an additional one extending towards the outer disk. Although classified as SAB there is no bar-like structure visible except for a possible ring-like structure of size $R\sim\!5$ $^{\prime \prime }$ . The final profile is not well described with a single exponential (Type I), already excluding the region beyond $R\sim\!90\hbox{$^{\prime\prime}$ }$ which is most probably affected by an incorrect sky subtraction. Unaffected of this it is better described as having a break at $\sim$ 70 $^{\prime \prime }$ , corresponding to the end of the single extended spiral arm, with a following downbending profile, which is too far out to be related to the possible bar and therefore classified as Type II-CT. The bump at $\sim$ 40 $^{\prime \prime }$ is related to the end of the inner spiral arms and beginning of the outer extended one. NIR imaging of the underlying old disk population should give clarification to the classification.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f146.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f147.ps} \end{figure}$ NGC 5667: Type II.i + III
J143022.9+592811 .S..6* 5.8 -19.69 1.7 2222

Galaxy small and close to the edge of the SDSS field but almost complete with an untypical appearance. The inner region ( $R \protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}30$ $^{\prime \prime }$ ) looks like an extended bar with dustlanes and a possible additional, tilted, secondary inner bar of size $R \protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}7$ $^{\prime \prime }$ . Outside this region there are two asymmetric narrow spiral arms visible towards north-west followed by an outer, slightly asymmetric, envelope, which makes the photometric inclination (ellipticity) and PA uncertain. The final profile shows a downbending break at $\sim$ 25 $^{\prime \prime }$ , related to (and inside) the extended bar structure, therefore classified as Type II.i, followed by an exponential down to another break at $\sim$ 65 $^{\prime \prime }$ where an additional upbending starts adding the Type III classification. The outer profile is uncertain due to a higher error in the sky. A still justifiable sky value could create a continuous outer slope, but this is unlikely, since it will not create the asymmetric shape of the outer isophotes.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f148.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f149.ps} \end{figure}$ NGC 5668: Type I
J143324.4+042702 .SAS7. 6.7 -19.65 2.8 1672

Galaxy close to the edge of the SDSS field but almost complete. Although classified as SA there is a weak bar or oval inner structure of size $R\sim\!12\hbox{$^{\prime\prime}$ }$ visible on the image, reflected by a small shoulder in the final profile. The outer disk (beyond $R\sim\!100$ $^{\prime \prime }$ ) is slightly asymmetric and more extended towards the North. The bump at $\sim$ 70 $^{\prime \prime }$ in the final profile is related to brighter spiral arms in this region. There is a possible upbending break visible at $\sim$ 100 $^{\prime \prime }$ (associated to the asymmetric outer disk) or $\sim$ 140 $^{\prime \prime }$ but the scalelength contrast is too low and it is too close to the sky error to argue for a Type III classification.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f150.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f151.ps} \end{figure}$ NGC 5693: Type II-AB
J143611.2+483504 .SBT7. 6.8 -18.64 1.9 2537

Small galaxy with unusual appearance, showing an inner extended bar-like structure of size $R\sim\!15$ $^{\prime \prime }$ , apparently with two central peaks, probably caused by a superimposed foreground star. The brightest pixel in the bar structure does not correspond to the center obtained from the outer isophotes and is off by $\sim$ $7\hbox {$^{\prime \prime }$ }$ causing the inner dip in the final profile. The bar-like structure is followed by a single spiral arm extending towards the outer (quite roundish and symmetric) disk, which is used to obtain the ellipticity and PA. The final profile cannot be well fitted with a single exponential (Type I) but rather shows a downbending behaviour albeit with an uncertain break radius due to the extended break region which resembles again a nearly straight line, so that one could also define two break radii at $\sim$ 30 $^{\prime \prime }$ and $\sim$ 50 $^{\prime \prime }$ . Although the first break is at twice the bar radius, we classify this galaxy as Type II-AB since this whole region is clearly lopsided with an significantly offcentered bar.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f152.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f153.ps} \end{figure}$ NGC 5713: Type III
J144011.4-001725 .SXT4P 4.1 -20.50 2.8 1958

According to Sandage & Bedke (1994) in a group of late-type spirals with four members in a region smaller than the Local Group. No bright nucleus in the bar-like structure so the centering is done from the outer isophotes. In addition to a more chaotic inner region with spiral structure (producing the bump between $R\sim\!10{-}35\hbox{$^{\prime\prime}$ }$ in the final profile) there is clear substructure in the outer disk visible. Towards the South ( $1.5\hbox {$^\prime $ }$ from the center) we see a very diffuse additional patch of light (size $R \protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}20$ $^{\prime \prime }$ and masked), in addition to a more elongated feature ( $\approx$ $1\hbox {$^\prime $ }$ from the center, unmasked) towards north-east. The profile shows a break at $\sim$ 115 $^{\prime \prime }$ with an upbending profile associated with a rather symmetric featureless outer part. The break is not caused by a possible sky error thus classified as Type III.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f154.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f155.ps} \end{figure}$ NGC 5768: Type I
J145207.9-023147 .SAT5* 5.0 -19.24 1.6 2018

Bright star superimposed so using an extended mask. Photometric inclination (ellipticity) at $1\sigma$ in the free ellipse fit does not match the outer parts well, therefore we used the outermost ellipse which leaves the ellipticity and PA uncertain. Similar to NGC 3888 the final profile exhibits an extended wiggle (with an unusual integral sign shape) at $\sim$ 50 $^{\prime \prime }$ (without being a break) corresponding to a set of spiral arms in the outer disk which do not start at the center. The inner break at $\sim$ 18 $^{\prime \prime }$ is associated with the inner spiral arms and the bar-like center. Although showing extended wiggles the galaxy is classified as Type I since there is no better fitting alternative.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f156.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f157.ps} \end{figure}$ NGC 5774: Type II.o-OLR + III
J145342.6+033500 .SXT7. 6.9 -19.09 2.8 1655

Galaxy has a close physical, edge-on, companion (NGC 5775, SBc?, v=1681 km s^-1 ) and exhibits an outer, extended spiral arm pointing towards NGC 5775 (similar to the M 51/NGC 5159 system but having a more similar sized mass) producing an asymmetric outer disk where the very outer isophotes already overlap. The center is obtained from outer ellipse fits (different from brightest pixel) since the inner elongated, narrow, bar-like region $R\sim\!10\hbox{$^{\prime\prime}$ }$ is without an obvious nucleus. The shoulder in the final profile at $\protect~\rlap{\lower -0.5ex\hbox{$>$ }}{\lower 0.5ex\hbox{$\sim~$ }}35\hbox{$^{\prime\prime}$ }$ corresponds to the end of the more extended bar-like structure enclosing the inner bar having a different PA. The break at $\sim$ 80 $^{\prime \prime }$ with the downbending profile being at about twice the extended bar radius is therefore classified Type II.o-OLR. The upbending profile (classified as Type III) beyond a break at $\sim$ 120 $^{\prime \prime }$ is due to the asymmetric outer disk with extended spiral arms. Fitting the profile with a single exponential (Type I) leaves three extended wiggles which are better explained by a Type II.o-OLR + III break combination.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f158.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f159.ps} \end{figure}$ NGC 5806: Type III
J150000.4+015329 .SXS3. 3.3 -19.74 3.0 1440

Galaxy close to our high axis ratio limit (dust lane visible?) and close to the edge of the SDSS field but almost complete. From the inner disk there is an additional patch of diffuse light visible towards the south-east (not masked) extending into the asymmetric outer disk, which makes the photometric inclination (ellipticity) and PA uncertain since obtained further in. The final profile shows a shoulder at $\sim$ 40 $^{\prime \prime }$ related to the inner bar-like center with the beginning of the spiral arms and a break at $\sim$ 120 $^{\prime \prime }$ . The break is close to the position of the extra patch of light followed by an upbending profile (classified as Type III) extending into the outer asymmetric disk without spiral structure. Our classification agrees well with Erwin et al. (2006) and the Type III profile is also visible in Courteau (1996) (cf. UGC 09645).

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f160.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f161.ps} \end{figure}$ NGC 5850: Type II.o-OLR
J150707.7+013240 .SBR3. 3.0 -21.43 4.3 2637

Bright star nearby needs extended mask. The $r^{\prime }$ band background is slightly inhomogeneous. Galaxy is dominated by an extended bar of size $R\sim\!55\hbox{$^{\prime\prime}$ }$ enclosed by an inner ring out to $R\sim\!75\hbox{$^{\prime\prime}$ }$ having a secondary, inner bar of size $R\sim\!7\hbox{$^{\prime\prime}$ }$ with clearly different ellipticity and PA. There is an additional, faint outer ring (or pseudo-ring, since looking similar to some wrapped spiral arms) visible on the image related to the break at $\sim$ 130 $^{\prime \prime }$ in the final profile, thus obviously classified as Type II.o-OLR. Since the outer ring is used to determine the photometric inclination (ellipticity) and PA they are rather uncertain.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f162.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f163.ps} \end{figure}$ NGC 5937: Type III
J153046.1-024946 PSXT3P 3.2 -20.90 1.9 2870

Bright stars nearby need extended mask without really covering the outer disk. There is a possible, small dwarf companion (not in NED) visible about $1.5\hbox {$^\prime $ }$ away towards the north-west. The outer disk is slightly asymmetric with continuously changing ellipticity and PA, so the values applied for the final profile are rather uncertain. The break at $\sim$ 70 $^{\prime \prime }$ with an upbending profile (classified as Type III) is most probably related to the changing ellipticity and should be taken with caution.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f164.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f165.ps} \end{figure}$ NGC 6070: Type II.o-CT
J160958.9+004234 .SAS6. 6.0 -21.04 3.4 2085

Galaxy close to our high axis ratio limit having a very bright star (with an extended halo) in the FOV which is still small enough to avoid significant influence. Only partly fitted since < $\sim~$ 1/5 of galaxy is beyond SDSS field. The outer isophotes are slightly asymmetric, with one sharp and one more fluffy side, so the ellipticity and PA are uncertain. The final profile exhibits a clear downbending with a more extended break region around $R\sim\!95\hbox{$^{\prime\prime}$ }$ corresponding to the end of the spiral arm structure and classified as Type II.o-CT. Although the galaxy is classified as SA there is an elliptical central bar-like structure of size $\protect\la$ $10\hbox {$^{\prime \prime }$ }$ visible which would be however too small to argue for a Type II.o-OLR break. The small dip at $\sim$ 30 $^{\prime \prime }$ is produced by spiral arm contrast.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f166.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f167.ps} \end{figure}$ NGC 6155: Type II-AB
J162608.3+482201 .S?... 7.8 -19.45 1.3 2684

Small galaxy with an extended mask reaching into the outer disk to cover a very bright star close by. Lopsided disk with centering done from the outer isophotes. The center is $\sim$ 3 $^{\prime \prime }$ off the brightest pixel associated to a small bar-like central structure of size $R\sim\!5\hbox{$^{\prime\prime}$ }$ followed by a thin, star-forming, blue spiral arm feature towards north-east. The final profile shows a downbending break at $\sim$ 35 $^{\prime \prime }$ corresponding to the inner lopsided disk thus classified as a Type II-AB break, although this is just at the radius of an outer ring (best visible in the colour image).

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f168.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f169.ps} \end{figure}$ NGC 7437: Type II-CT
J225810.0+141832 .SXT7. 7.1 -18.88 1.8 2190

Small galaxy close to the edge of the SDSS field but almost complete. Similar to NGC 5300 the final profile shows the prototypical Type II.o-CT behaviour. A sharp break at $\sim$ 40 $^{\prime \prime }$ , corresponding roughly to the end of the apparent flocculent spiral arm structure, followed by a downbending profile. Although classified as SAB there is no obvious structure visible which could be identified with a bar. Using the beginning spiral arms as an upper limit ( $R\protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}8$ $^{\prime \prime }$ ) the break is still too far out for a normal Type II.o-OLR break.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f170.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f171.ps} \end{figure}$ NGC 7606: Type II-CT
J231904.8-082906 .SAS3. 3.2 -21.38 4.3 2187

Galaxy with multiple thin spiral arms. The final profile exhibits clearly a break at $\sim$ 110 $^{\prime \prime }$ corresponding roughly to the end of the visible spiral arm structure, following part of the ring enclosing an apparent hole (enhanced dust extinction?) in the disk towards the north-west. Since the galaxy is classified as SA and no bar structure visible the break is a Type II-CT. The apparent upbending of the profile beyond $\sim$ 190 $^{\prime \prime }$ is not related to a sky error but due to a changing ellipticity in the very outer disk (maybe due to a warp?).

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f172.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f173.ps} \end{figure}$ PGC 006667 $\equiv$ UGCA 021: Type II-AB
J014910.2-100345 .SBS7. 7.1 -18.77 2.9 1887

A large scale gradient (from top to bottom) in the background of the $r^{\prime }$ band image is removed with linear fit. Galaxy in NGC 701 group (see above). Final profile shows a bump at $\sim$ 20 $^{\prime \prime }$ due to the spiral arms starting from the bar-like center. The clear downbending break at $\sim$ 75 $^{\prime \prime }$ corresponds to a transition from the inner more symmetric to an asymmetric, extended outer disk region and is therefore classified as Type II-AB.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f174.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f175.ps} \end{figure}$ UGC 02081: Type II-CT
J023600.9+002512 .SXS6. 5.8 -18.56 1.8 2549

Galaxy close to the edge of the SDSS field but almost complete. The final profile shows a downbending break starting around $\sim$ 55 $^{\prime \prime }$ (clearly at $\sim$ 70 $^{\prime \prime }$ ) with a very faint, but symmetric light distribution beyond. Although classified as SAB the bar is not obvious from the image but the spiral arms allow to estimate an upper limit of $R \protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}7$ $^{\prime \prime }$ . Therefore the break (which is not produced by a sky error) is classified Type II-CT. The profile published in de Jong & van der Kruit (1994) is not deep enough to confirm the downbending.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f176.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f177.ps} \end{figure}$ UGC 04393: Type I
J082604.3+455803 .SB?.. 5.5 -19.49 2.2 2290

Galaxy is classified as SB and the inner region is dominated by an elongated bar-like structure of size $R\sim\!30$ $^{\prime \prime }$ . Therefore this region is excluded from the fit. The extended bar, having a kind of double nucleus, is slightly offcenter (central dip in profile) compared to the center obtained from the outer isophotes and is followed by a single, narrow spiral arm like structure extending south-west. In the outer disk there is an additional, faint spiral arm visible towards the south-east. There is also a very faint shell or stream-like structure detected, detached from the galaxy about $2\hbox {$^\prime $ }$ away to the north-west. The inclination (ellipticity) and PA are rather uncertain since they are continuously changing towards the outer disk. The final profile, beyond the inner bar region, is classified as Type I, due to the uncertain ellipticity and the asymmetric outer disk with the spiral arm, although there are two possible breaks visible at $\sim$ 60 $^{\prime \prime }$ and $\sim$ 80 $^{\prime \prime }$ , of which the first could correspond to a Type II.o-OLR break and the latter to a Type III.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f178.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f179.ps} \end{figure}$ UGC 06309: Type II.i
J111746.4+512836 .SB?.. 5.0 -19.63 1.3 3097

There is a small BCG (MRK 1445) about $3.5\hbox {$^\prime $ }$ away at roughly the same distance (v=2863 km s^-1 ). Galaxy exhibits very unusual, disturbed shape. The inner disk is dominated by a narrow bar of size $R\protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}20\hbox{$^{\prime\prime}$ }$ followed by two asymmetric spiral arms (one highly wrapped, forming an inner ring, the other almost extending straight). The disk beyond the spiral arms is also highly asymmetric and more egg-shaped with a region of low emission (high extinction?) towards the south-east, which makes the bar appear to be offcentered. However, the center from the very outer isophotes coincides again with the nucleus inside the bar. The extended dip and peak structure around $15{-}20\hbox {$^{\prime \prime }$ }$ in the final profile corresponds to the inter-arm region, respectively the pseudoring build by the arms, so the break around this radius is classified as Type II.i. This should be used with caution, since alternatively one can argue for a break at $\sim$ 35 $^{\prime \prime }$ , at about twice the bar radius thus a Type II.o-OLR break, while excluding the region between 15-30 $^{\prime \prime }$ .

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f180.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f181.ps} \end{figure}$ UGC 06518: Type II.i
J113220.4+535417 ...... 4.3 -18.94 1.0 3044

Small galaxy where, although not classified as barred in NED or LEDA, there is clearly a bar of size $R\sim\!10\hbox{$^{\prime\prime}$ }$ visible, with indication for a ring-like structure around, already reported by Takase & Miyauchi-Isobe (1984). Despite the possibility to argue for a break at $\sim$ 15 $^{\prime \prime }$ in the final profile we classify the galaxy as Type II.i excluding the region inside $R=10\hbox {$^{\prime \prime }$ }$ from the fit.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f182.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f183.ps} \end{figure}$ UGC 06903: Type II.o-CT
J115536.9+011415 .SBS6. 5.8 -18.80 2.5 1916

Very bright star in FOV but galaxy not influenced. Final profile shows clearly a downbending break around $\sim$ 65 $^{\prime \prime }$ corresponding roughly to the end of the visible spiral arm structure and classified Type II.o-CT, since the size of the bar with $R\protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}17$ is too small. The extended bump between $R\sim\!20{-}40\hbox{$^{\prime\prime}$ }$ is related to the inner two, highly wrapped (pseudoring?) spiral arms. The downbending shape is consistent with the profile shown in Jansen et al. (2000) (cf. ID 99).

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f184.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f185.ps} \end{figure}$ UGC 07700: Type II.o-CT
J123232.8+635238 .SBS8. 7.8 -18.50 1.8 3239

There is a very bright star in the FOV but the galaxy is not influenced. On same image there is an edge-on companion (S0/a galaxy NGC 4512) at similar distance (v=2536 km s^-1 ) visible. Ellipticity obtained from the very outer isophotes and not by the usual $1\sigma$ criterion. The final profile shows clearly a downbending behaviour outside the bar region. The bar is about $R\sim\!17\hbox{$^{\prime\prime}$ }$ in size and slightly offcentered (by $\sim$ 5 $^{\prime \prime }$ ) compared to the center obtained from the outer, symmetric isophotes. This causes the dip at the center. The extended break region is not exponential but shows a curvature, but still one could define two break radii at $\sim$ 40 $^{\prime \prime }$ and $\sim$ 50 $^{\prime \prime }$ . The region in between corresponds to a single spiral arm extending towards the north-east. Although the first one would roughly classify as a Type II.o-OLR break we used a single break slightly further out and classified the galaxy as Type II.o-CT.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f186.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f187.ps} \end{figure}$ UGC 08041: Type II.o-CT
J125512.7+000700 .SBS7. 6.8 -18.62 3.2 1376

Galaxy close to our high axis ratio limit and not influenced by the very bright star in FOV. The inner disk with a bright nucleus in the bar and weak spiral arm structure extends to about $\sim$ 100 $^{\prime \prime }$ , followed by a rather asymmetric, lopsided outer disk extending to the south-west. Centering on the outer isophotes ( $R\protect~\rlap{\lower -0.5ex\hbox{$>$ }}{\lower 0.5ex\hbox{$\sim~$ }}100$ $^{\prime \prime }$ ) would be off by more than $\sim$ 10 $^{\prime \prime }$ . The final profile shows a downbending break at $\sim$ 75 $^{\prime \prime }$ roughly corresponding to the end of the spiral structure. Since the bar is only of size $R\protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}12\hbox{$^{\prime\prime}$ }$ the break, at significantly more than twice the bar radius, is classified as Type II.o-CT. The fixed ellipse leaves the inner symmetric disk at about $\sim$ 100 $^{\prime \prime }$ into the asymmetric outer part causing the apparent upbending in the profile, which probably increases the fitted outer scalelength.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f188.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f189.ps} \end{figure}$ UGC 08084: Type II.o-OLR
J125822.4+024733 .SBS8. 8.1 -18.61 1.3 2824

Small galaxy dominated by an inner offcentered, asymmetric bar of size $R\sim\!17$ $^{\prime \prime }$ , which appears to be z-shaped together with the two spiral arms. The center is obtained from outer isophotes ( $\sim\!50 \hbox{$^{\prime\prime}$ }$ ) and is about $\sim$ 12 $^{\prime \prime }$ away from the brightest pixel in bar, which is responsible for the flat inner profile. The final profile shows clearly a downbending break at $\sim$ 40 $^{\prime \prime }$ corresponding to the spiral arms forming a kind of pseudoring in the outer parts. Since the break is at about twice the bar size the galaxy is classified as Type II.o-OLR.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f190.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f191.ps} \end{figure}$ UGC 08237: Type II.o-OLR
J130854.5+621823 PSB.3* 3.2 -19.61 0.9 3120

Galaxy is isolated according to Prada et al. (2003). The similar sized companion, only $2.3\hbox {$^\prime $ }$ away, is a confirmed background galaxy (UGC 08234, v=8100 km s^-1 ). Background needs extended mask due to straylight from a very bright star off the field. UGC 08237 is a small galaxy dominated by a bright, thick bar of size $R\protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}12\hbox{$^{\prime\prime}$ }$ (producing the shoulder in the final profile) followed by two nearly symmetric, wrapped spiral arms forming a pseudoring peaking at $\sim$ 20 $^{\prime \prime }$ . Similar to NGC 5701 (an early-type SB0/a galaxy from Erwin et al. (2006)) one could define a break at $\sim$ 25 $^{\prime \prime }$ just outside of the pseudoring forming the region $R\sim\!12{-}25$ which is no longer well fitted by an exponential profile. Erwin et al. (2006) call these systems "extreme'' OLR breaks, so we also classify the galaxy as Type II.o-OLR and apply a crude fit to obtain an inner scalelength.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f192.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f193.ps} \end{figure}$ UGC 08658 $\equiv$ Holmberg V: Type II-CT
J134039.9+541959 .SXT5. 5.1 -19.91 2.6 2285

Galaxy close to the border of the SDSS field but almost complete. Although classified as SAB, the bar size is not obvious from the image, but could be restricted by the spiral arms to be maximal $R\protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}10$ $^{\prime \prime }$ . The shoulder in the final profile at $\sim$ 20 $^{\prime \prime }$ is due to the inner spiral arms being aligned with the ellipse. There is a weak break at $\sim$ 65 $^{\prime \prime }$ visible which roughly coincides with the end of the inner spiral arm structure, although there are maybe two faint extensions into the outer disk. Since being at significantly more than two bar radii we classify the break as Type II-CT.

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f194.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f195.ps} \end{figure}$ UGC 09741 $\equiv$ NGC 5875A: Type III
J150833.5+521746 .S?... 6.0 -18.54 0.9 2735

The patch of faint light on the image towards the north-west is caused by straylight from a very bright star off field, but the galaxy is not affected. Very small galaxy dominated by a long, narrow bar of size $R\sim\!9$ $^{\prime \prime }$ , enclosed by a ring like structure building the inner $R\protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}17\hbox{$^{\prime\prime}$ }$ disk. The photometric inclination (ellipticity) and PA is obtained from the outer disk at $\sim$ 45 $^{\prime \prime }$ and not from the $1\sigma$ ellipse. Although it is possible to fit the profile beyond $\sim$ 17 $^{\prime \prime }$ with a single exponential the offset inside would be too large to be assigned solely to a bulge component of a typical Sc galaxy. In addition, an extended bulge component is also not visible on the image inside the narrow bar. Thus we argue for a break, classified as Type III, at $\sim$ 25 $^{\prime \prime }$ followed by an upbending profile into the symmetric featureless outer disk. The shape of the profile is consistent with the one shown by Jansen et al. (2000) (cf. ID 166).

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f196.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f197.ps} \end{figure}$ UGC 09837: Type II-CT
J152351.7+580311 .SXS5. 5.1 -19.45 1.8 2938

Although classified as SAB, the bar size is not obvious from the image, but could be restricted to be maximal $R\protect~\rlap{\lower -0.5ex\hbox{$<$ }}{\lower 0.5ex\hbox{$\sim~$ }}9$ $^{\prime \prime }$ by the two symmetric spiral arms starting beyond the bulge/bar region out to $R\sim\!25$ $^{\prime \prime }$ . Further out, there is more asymmetric spiral arm structure visible, with one arm almost forming a ring-like section, which makes the photometric inclination (ellipticity) and PA determination impossible at the $1\sigma$ ellipse. Since the ring like section extends to the end of our free ellipse fit, we set the ellipticity to 0.05 (round). In the final profile there is a break visible at $\sim$ 50 $^{\prime \prime }$ just beyond the bump produced by the ring-like spiral arm. Since this break is at significantly more than two times the upper limit for the bar radius we classify the break as Type II-CT. The deep surface photometry from Pohlen et al. (2002) is consistent with the results here (cf. Fig. 3) aside from this bump produced by the outer spiral arm, which seems to be suppressed in their averaged profile. The downbending shape with a break at $\sim$ 50 $^{\prime \prime }$ is consistent with the profile shown by van der Kruit (1987).

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f198.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f199.ps} \end{figure}$ UGC 10721: Type III
J170825.6+253103 .S..6? 5.8 -19.68 1.2 3118

Small galaxy close to our high axis ratio limit so the dust may get important. Galaxy shows an inner apparently inclined disk with a nucleus and some thin spiral arms sitting in an almost round outer isophote most probably related to a vertical structure (halo or thick disk). Thus the photometric inclination (ellipticity) and PA are highly uncertain since continously changing with radius. The shoulder at $\sim$ 12 $^{\prime \prime }$ in the final profile corresponds to an aligned spiral arm. There is a clear break visible at $\sim$ 40 $^{\prime \prime }$ followed by an upbending profile which is classified as Type III, associated to the transition between inner and outer disk (vertical structure?), so to be taken with some caution. The sharp transition in the profile argues against a thick disk. The upbending behaviour is confirmed by the profile from Courteau (1996).

$\begin{figure}\includegraphics[width=5.7cm,angle=270]{4883f200.ps}\par\hspace*{-0.5cm}\includegraphics[width=6.1cm,angle=270]{4883f201.ps} \end{figure}$ UGC 12709: Type II-CT
J233724.0+002327 .SXS9. 8.3 -19.05 3.0 2672

This is a faint, low surface brightness galaxy without a well defined center, so the centering (obtained from the $\sim$ 80 $^{\prime \prime }$ ellipse) and the photometric inclination (ellipticity) and PA (obtained at $\sim$ 70 $^{\prime \prime }$ ) are uncertain. The offcentered outer disk is reflected by the central dip in the final profile, which shows a clear downbending break at $\sim$ 70 $^{\prime \prime }$ corresponding roughly to the end of the flocculent starforming patches. Although classified as SAB the central region ( $\sim$ 10 $^{\prime \prime }$ ) is too fuzzy to argue for or against a bar, but in both cases it is to small to be responsible for the break, which is therefore classified as Type II-CT.

Appendix B: Rejected galaxies

$\begin{figure}\par\includegraphics[width=5.7cm,angle=270]{4883f202.ps}\includegr... ...883f206.ps}\includegraphics[width=5.7cm,angle=270]{4883f207.ps}\par \end{figure}$

Figure B.1: Galaxies rejected from the original LEDA-SDSS(DR2) sample: SDSS colour plates of NGC 0428, NGC 0988, NGC 2712, NGC 3023, NGC 4116, and NGC 4496A (from left to right and top to bottom).

In the text

$\begin{figure}\par\includegraphics[width=5.7cm,angle=270]{4883f208.ps}\includegr... ...ludegraphics[width=5.7cm,angle=270]{4883f214.ps}\hspace*{4cm}} \par \end{figure}$ Figure B.1: continued. Galaxies rejected from the original LEDA-SDSS(DR2) sample SDSS colour plates of NGC 4900, NGC 5218, NGC 5364, PGC 032356, UGC 04684, UGC 06162, and UGC 09215 (from left to right and top to bottom).

In the text

$\begin{figure} \par\includegraphics[width=5.6cm,angle=270]{4883f001.ps}\hspace*{3mm} \includegraphics[width=5.6cm,angle=270]{4883f002.ps}\end{figure}$	Figure 1: Histogram showing the distribution of galaxies covering the morphological types (T) and absolute magnitude ( $M_{\rm abs}$ ) for the full LEDA sample (rising hashed lines) and the studied SDSS DR2 subsample (falling hashed lines).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=5.5cm,angle=270]{4883f017.ps}\includeg... ...]{4883f023.ps}\includegraphics[width=5.5cm,angle=270]{4883f024.ps} \end{figure}$	Figure 5: continued. The ellipse for the first Type II.i galaxy corresponds to the inner boundary at $\sim$ 20''. For the mixed classifications two ellipses are shown corresponding to the associated breaks.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=5.5cm,angle=270]{4883f030.ps} \end{figure}$	Figure 10: Histogram of the surface brightness (in the $r^{\prime }$ band) at the break radius for the galaxies of Type II-CT (solid line), Type III (dashed line), and Type II.o-OLR (dotted line).
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All Figures

Appendix B: Rejected galaxies