1 VCC 1226 (M49, NGC 4472). A thin, boomerang-shaped dust lane crosses
  1  the galaxy's center at a position angle of roughly -45{deg}, extending
  1  ~1.5" on either side. Faint dust patches are seen within 3.5" of the
  1  center. There is no indication of a nucleus from the dust-corrected
  1  images. The isophotes show no significant deviations from ellipses.
  2 VCC 1316 (M87, NGC 4486). The inner 0.25" of the g-band image is
  2  saturated. The optical synchrotron jet emanating from the unresolved,
  2  nonthermal nucleus is clearly visible and was masked prior to the
  2  isophotal analysis. Dust filaments radiate from the center outward,
  2  extending out to 13" from the nucleus. There are two very red objects
  2  close to the galaxy center: one directly south of the nucleus, at a
  2  distance of ~6", the other southeast of the nucleus at a distance of
  2  11.5". The former appears to be a globular cluster, and the latter a
  2  faint background galaxy. The isophotes appear very regular.
  3 VCC 1978 (M60, NGC 4649). This galaxy shows very regular isophotes,
  3  with no evidence of a morphologically distinct nuclear component.
  4 VCC 881 (M86, NGC 4406). NGC 4406 is a well-known example of a galaxy
  4  moving through a cluster at supersonic velocity (e.g., White et al.
  4  1991ApJ...379...52W; Rangarajan et al. 1995MNRAS.277.1047R; Stickel et
  4  al. 2003A...397..503S; Elmegreen et al. 2000AJ....120..733E); on-going
  4  dust stripping is believed to be taking place as a consequence. The
  4  ACSVCS residual images indeed show several dust filaments radiating
  4  from the center, mainly in the southeast quadrant, all the way to the
  4  edge of the chip. The isophotes are regular, a fact reflected in the
  4  constancy of the ellipticity, position angle and higher order
  4  coefficients, all of which are consistent with zero. However, in the
  4  inner 0.4", the surface brightness profile decreases inward, a fact
  4  first noticed by Carollo et al. (1997ApJ...481..710C). At first sight,
  4  this behavior is consistent with what is expected from a small dust
  4  disk, however, the color image shows no color difference between this
  4  region and the surrounding areas. The other explanation is that the
  4  stellar density actually decreases within this region. However, the
  4  "depleted" area appears, in projection, quite round, rounder than the
  4  galaxy isophotes, and might even be slightly miscentered (extending
  4  more to the southeast).
  5 VCC 798 (M85, NGC 4382). The isophotes are very boxy within 1"; the
  5  boxiness persists all the way to the center, where there almost seems
  5  to be a "butterfly" pattern, extending about 0.3" on either side and
  5 aligned with the major axis of the galaxy. The isophotes become
  5 distorted beyond 50". The residual image shows the possible presence
  5 of two small dust patches about 4" southwest of the center. There is
  5 no evidence of a nucleus.
  6 VCC 763 (M84, NGC 4374). Like M87 (=3C 374), M84 (=3C 272.1) is a
  6  well-known radio source. Two parallel dust lanes, one crossing (but
  6  not centered on) the galaxy's center, the other just north of the
  6  first, run in the east-west direction. The larger (northern) dust lane
  6  extends for approximately 14", while the lane crossing the center
  6  extends for about 5". Both lanes are surrounded by fainter dust wisps
  6  and filaments. The isophotes are very regular.
  7 VCC 731 (NGC 4365). The galaxy is a member of the W-cloud, at a
  7  distance of 23 Mpc (S. Mei et al. 2007ApJ...655..144M). A resolved,
  7  slightly elongated nucleus is clearly visible in the color image, as
  7  well as in the individual frames. The nucleus is bluer than the
  7  surrounding galaxy and clearly affects the surface brightness
  7  profiles, in particular in the g band. The isophotes appear quite
  7  regular.
  8 VCC 1535 (NGC 4526). This galaxy hosts a large dust disk, very
  8  reminiscent of the one seen, at lower inclination, in VCC 1154. The
  8  disk extends 15.6" on either side of the galaxy's center and is
  8  aligned with the major axis of the galaxy (in the east-southeast
  8  direction). The plane of the disk makes an angle of approximately
  8  15{deg}. to the line of sight, the northern side being the closest.
  8  There are several blue knots within the disk, probably indicative of
  8  star formation. Because the underlying stellar population within the
  8  disk is likely different from that characterizing the main body of the
  8  galaxy, the dust correction for this galaxy fails, and the isophotes
  8  can only be recovered outside a semimajor axis of 7". At a radius of
  8  approximately 10" the isophotes become visibly boxy; the boxiness is
  8  rather extreme at a radius of 20". Beyond, the isophotes assume a
  8  diamond shape appearance (as a consequence the A4 coefficient becomes
  8  nonzero), and finally become disky at a radius of approximately 70".
  9 VCC 1903 (M59, NGC 4621). The g-band images are saturated within the
  9  inner 0.25". Based on the z-band image only, there does not appear to
  9  be a morphologically distinct nucleus; however, there is a clear,
  9  edge-on, thin, faint stellar disk, extending at least 10" from the
  9  center. The presence of the disk is reflected in the B4 coefficient.
 10 VCC 1632 (M89, NGC 4552). Two thin dust filaments radiate from the
 10  center in the west-northwest direction, out to a distance of about 6".
 10  Small dust patches are visible within 11". A small dust patch, less
 10  than 1" across, surrounds (but it is not centered on) the center of
 10  the galaxy. There is a very red object to the southwest of the center,
 10  at a distance of about 10". The isophotes are very regular; there is
 10  no indication of a nucleus.
 11 VCC 1231 (NGC 4473). Rather elongated system; the color image shows
 11  no evidence of dust, however, there is a small (less than 1") thin
 11  rectangular feature crossing the center of the galaxy. This feature is
 11  aligned with the major axis and bluer than the surrounding regions; it
 11  is probably responsible for the negative B4 coefficient in the very
 11  innermost region. Further out, the galaxy becomes disky, and remains
 11  so out to about 10". There does not appear to be a morphologically
 11  distinct nucleus.
 12 VCC 2095 (NGC 4762). This galaxy has a very thin, edge-on disk,
 12  extending all the way to the edge of the CCDs. Within the inner 15" on
 12  either side of the nucleus, the disk appears to become thinner and
 12  fainter as the radius decreases; it reaches maximum surface brightness
 12  between 15" and 40" from the center, and it is bluer than the
 12  surrounding galaxy.
 13 VCC 1154 (NGC 4459). This galaxy harbors a spectacular dust disk,
 13  similar to the one seen, at higher inclination, in VCC 1535. The disk
 13  is about 17" across, and its plane is inclined by 45{deg}. to the line
 13  of sight. There are several blue clumps in the disk, probably
 13  indicative of star formation. Several wisps and filaments extend
 13  beyond the edge of the disk. As for the case of VCC 1535, the
 13  correction for dust fails, and the profile can only be recovered
 13  beyond 7."5 from the center. Unlike the case of VCC 1535, the
 13  isophotes look regular.
 14 VCC 1062 (NGC 4442). This galaxy appears quite regular within the
 14  inner 15". Beyond, the isophotes become boxy, and a faint elongated
 14  outer envelope dominates the galaxy's appearance. This is slightly
 14  tilted (toward south) relative to the inner regions, causing the
 14  isophotes to twist slightly. The images show no strong evidence of a
 14  morphologically distinct nucleus.
 15 VCC 2092 (NGC 4754). This galaxy has two morphologically distinct
 15  components: the main body, which appears quite regular, and a
 15  misaligned (by about 45{deg}) bar, extending out to 25" from the
 15  center. A faint nucleus is likely present.
 16 VCC 369 (NGC 4267). This galaxy is quite round in the innermost
 16  6"; beyond it becomes more elongated, with perhaps a slight twist in
 16  the major axis position angle, to revert to round again beyond 50". It
 16  is possible that the change in the isophotal shape is due to a stellar
 16  bar similar (but much fainter) to the one seen in VCC 2092. A faint
 16  nucleus is likely present.
 17 VCC 759 (NGC 4371). This galaxy has a small dust disk at the center,
 17  only about 1."6 across. The disk is inclined by about 26i{deg}. to the
 17  line of sight, and its major axis seems to coincide with the major
 17  axis of the galaxy (which is aligned in the east-west direction). The
 17  structure beyond is not easily interpretable. There seems to be a thin
 17  (less than 1" across) blue nuclear stellar ring centered on the
 17  galaxy's center, with a radius just below 11". The inclination and
 17  orientation of the stellar ring are the same as those of the nuclear
 17  dust disk. Within this ring, there seems to be at least one additional
 17  blue arc. Just beyond the stellar ring, there seems to be a second,
 17  this time redder, stellar ring, about 6" across. Farther out, at a
 17  distance of about 34", a ring rests at the end of a kpc-scale bar. The
 17  presence of the rings makes the A4 and B4 coefficients nonzero. The
 17  position angle, ellipticity and the surface brightness profile are
 17  also irregular. There does not appear to be a stellar nucleus,
 17  although the presence of the dust makes this statement hard to
 17  quantify.
 18 VCC 1692 (NGC 4570). This galaxy shows a thin, circumnuclear stellar
 18  ring, centered on the nucleus (which appears resolved), extending just
 18  less than 2" on either side and aligned with the main body of the
 18  galaxy. Although almost edge-on, the structure indeed appears to be a
 18  ring rather than a disk; an inner gap is apparent from the images. The
 18  ring is bluer than the surrounding galaxy. The galaxy is very
 18  elongated, with a thin, edge-on disk that appears to become slightly
 18  thicker toward the center, where it joins the main bulge.
 19 VCC 1030 (NGC 4435). There is a small dust disk, about 8" across,
 19  centered on the galaxy's center. The disk is inclined 16{deg}. to the
 19  line of sight. Although similar, this disk is smaller and less
 19  structured than those in VCC 1154 and VCC 1532. Several regions within
 19  the disk are quite blue, probably due to star formation. This prevents
 19  an accurate dust correction, and the isophotes are not recovered
 19  within the inner 2". Because of the dust, it is also impossible to
 19  assess the presence of a nucleus. The isophotes are visibly boxy in
 19  the inner 10", switching to disky further out.
 20 VCC 2000 (NGC 4660). The center is saturated in the g-band image.
 20  The galaxy is very elongated but becomes boxy at a distance of about
 20  6" (along the major axis) from the center. At the corresponding
 20  distance along the minor axis (4.5"), to the south, there is a small,
 20  faint, very blue structure, resembling a nucleus with two spiral arms.
 20  The "arm" facing the nucleus of VCC 2000 is more extended and looser
 20  than the arm facing away. The entire structure is about 2."5 across.
 21 VCC 685 (NGC 4350). This is a very elongated system, with a large-scale
 21  edge-on stellar disk typical of S0 galaxies. The presence of the disk
 21  affects the B4 coefficient, which becomes positive beyond a few
 21  arcsec. There is a nuclear, nearly edge-on dust disk, about 4" in
 21  diameter. The dust disk is surrounded by a blue stellar disk,
 21  extending perhaps 1.5" beyond the edge of the dust disk. Dust,
 21  stellar, and outer disks are all aligned. In correcting for dust
 21  absorption, the color of the region underlying the dust disk has been
 21  assumed equal to the color of the surrounding stellar disk, although
 21  the correction is still not entirely successful. There is no obvious
 21  evidence for the presence of a nucleus from the color images or the
 21  surface brightness profiles (although this is not a secure conclusion,
 21  because of the presence of the dust). The vast majority of globular
 21  clusters are found in the equatorial plane of the galaxy and are
 21  therefore likely associated with the large-scale disk.
 22 VCC 1664 (NGC 4564). There appears to be a faint nucleus in the color
 22  image, although its presence is not obvious in the individual images.
 22  The galaxy becomes quite disky beyond 10".
 23 VCC 654 (NGC 4340). The galaxy is quite round within the inner 1."7,
 23  beyond which it becomes stretched in the northeast-southwest direction,
 23  due to the presence of an inner bar surrounded by a nuclear stellar
 23  ring. Beyond 6", the galaxy is elongated in the east-west direction.
 23  The very innermost region (within 0.5") is also elongated, in the same
 23  direction as the outer parts. From the color image, the innermost
 23  structure appears bluer than the main body of the galaxy. An outer
 23  stellar ring with semimajor axis of about 56" bounds an outer bar; a
 23  small irregular galaxy lies along this ring about 40" to the northeast
 23  of the center.
 24 VCC 944 (NGC 4417). This galaxy has a thin edge-on blue stellar disk,
 24  aligned with the main body. There appears to be a faint nucleus, both
 24  from the color image and from the g-band surface brightness profile.
 25 VCC 1938 (NGC 4638). The galaxy is visibly disky beyond a few arcsec.
 25  A thin, edge-on stellar disk seems to be embedded in the outer, thick
 25  disk of the galaxy. The latter does not extend all the way in,
 25  stopping at a distance of about 4.5" from the center. There is a faint
 25  indication of two tightly wound dust spiral arms extending from the
 25  disk, at a distance of 13" from the center, although there is no
 25  feature associated with these structures in the color image. The
 25  latter do show, however, an inner, red disk about 12" in radius. There
 25  is no obvious dust absorption associated with this disk in the
 25  individual images, and therefore this is probably a stellar feature.
 25  The color images also indicate the presence of a compact nucleus. In
 25  the isophotal analysis, the center seems to wander and was therefore
 25  held fixed. A fainter galaxy (possibly a nucleated dwarf elliptical)
 25  is seen about 100" to the east, while a very red object is present
 25  about 17" east of the nucleus.
 26 VCC 1279 (NGC 4478). This galaxy is generally well behaved on large
 26  scales. There is no hint of the existence of a large-scale disk, but
 26  the isophotes become more elongated in the very innermost region. The
 26  color image betrays the existence of a small (less than 1" in radius)
 26  blue stellar disk, which is seen almost edge-on and oriented along the
 26  major axis of the galaxy. The presence of a disk is also reflected in
 26  the B4 coefficient. From the surface brightness profile, it is
 26  possible that a compact nucleus exists, affecting the profile within
 26  the inner 1" or so, although the feature seen could also be
 26  attributable to the disk.
 27 VCC 1720 (NGC 4578). Well-behaved elliptical, with regular isophotes.
 27  Both the color image and the surface brightness profiles show evidence
 27  of a stellar nucleus.
 28 VCC 355 (NGC 4262). Two dust filaments radiate away from the center in
 28  a spiral pattern, reaching out to a distance of about 4". Other than
 28  that, the galaxy appears regular within this region. Beyond, the
 28  isophotes twist (from a position angle of about -30{deg} to
 28  approximately +20{deg}) and become quite disky. Inspection of the
 28  images reveals the presence of a bar, aligned at a position angle of
 28  +10{deg} and extending about 27" from side to side. The bar appears
 28  slightly misaligned with respect to the main body of the galaxy at the
 28  same radius. The end of the bar has a "flattened" appearance,
 28  resembling a hammer, although there is no obvious indication of a ring
 28  or spiral arms protruding from it. There is no obvious color feature
 28  associated with the bar. There might be a hint of a compact stellar
 28  nucleus from the surface brightness profiles.
 29 VCC 1619 (NGC 4550). This galaxy is intermediate, as far as dust
 29  morphology is concerned, between the "dust filaments" types (e.g., M87
 29  and NGC 4472) and the" large-scale dust disk" types (e.g., VCC 1154).
 29  Dust filaments radiate outward from the center, but they have larger
 29  optical depth compared to the ones seen in M87 or VCC 355, for
 29  instance. Although the filaments form a disk structure, this is not
 29  quite as organized as the disks seen in VCC 1154 or VCC 1532. The main
 29  dust filaments/lanes are confined within a 10" from the center, but
 29  dust patches can be seen further out, up to a distance of 25". The
 29  dust correction performs well, indicating that the galaxy's color
 29  within the dust region is similar to that of the neighboring areas.
 29  The surface brightness profile indicates the presence of a large
 29  nucleus.
 30 VCC 1883 (NGC 4612). This galaxy resembles VCC 355, in that it shows
 30  a dramatic isophotal twist. In this case, however, there is no
 30  evidence of dust. The presence of a bar is not quite as obvious as it
 30  is in the case of VCC 355, but the galaxy isophotes become "stretched"
 30  at a distance of about 17" from the center, as would be expected if a
 30  boxy, elongated component were superimposed to the main body of the
 30  galaxy. The "ends" of the bar are visible, albeit barely, in the
 30  individual images. The bar is misaligned with the main body of the
 30  galaxy, producing a 40{deg} change in the position angle of the major
 30  axis. A stellar nucleus causes an inflection in the innermost 0.2" of
 30  the surface brightness profile.
 31 VCC 1242 (NGC 4474). This galaxy resembles VCC 685 but for the presence
 31  of dust. Very elongated system, with a large-scale edge-on stellar
 31  disk typical of S0 galaxies. The presence of the disk affects the B4
 31  coefficient, which becomes positive beyond a few arcsec, and the
 31  galaxy appears bluer in the equatorial plane. A nucleus is visible in
 31  both of the individual images and is reflected in the shape of the
 31  surface brightness profiles in the inner 0.3". The galaxy has a
 31  significantly larger GC system compared to galaxies in the same
 31  magnitude range.
 32 VCC 784 (NGC 4379). The isophotes become slightly disky at a distance
 32  of approximately 10" from the center, as shown by the B4 coefficient
 32  and ellipticity change between 10" and 20". Unlike the case of VCC 1883
 32  and VCC 355, there is no convincing evidence that a bar might be
 32  present, although the fact that the position angle changes (just as it
 32  does for VCC 1883 and VCC 355 where the bar sets in) is suggestive.
 32  The images and surface brightness profile are clearly affected by the
 32  presence of a nucleus in the inner 0.2".
 33 VCC 1537 (NGC 4528). This galaxy is in the same class as VCC 1883 and
 33  VCC 355 (and perhaps VCC 784 and VCC 778) but shows even more extreme
 33  properties. The bar is very prominent and is misaligned relative to
 33  the major axis of the main body of the galaxy by about of 60{deg}, with
 33  the bar almost aligned in the east-west direction. Ellipticity,
 33  position angle, and A4 and B4 coefficients change abruptly where the
 33  bar sets in. The surface brightness in the main body of the galaxy
 33  changes abruptly at the radius corresponding to the edge of the bar;
 33  being fainter within the region swept by the bar than outside. There
 33  is no clear evidence for a nucleus, although the surface brightness
 33  profile is quite steep.
 34 VCC 778 (NGC 4377). There are three small spiral galaxies at
 34  approximately 17", 19" and 31" from the center of VCC 788; the largest
 34  galaxy is approximately 11" across. The three galaxies are aligned
 34  approximately in the east-west direction; there is no obvious
 34  isophotal disturbance in VCC 778 at the radius where these galaxies
 34  are, and therefore the three spirals are probably part of a background
 34  group. All three galaxies were masked in fitting the isophotal
 34  parameters. This galaxy shows the same features seen in VCC 784: at
 34  radii between approximately 3."5 and 8", the isophotes twist, the
 34  ellipticity, the B4 and, especially, the A4 coefficients jump, as due
 34  to the presence of a misaligned bar (the misalignment here is about
 34  20{deg}), producing "diamond" shaped isophotes. The bar is not directly
 34  visible in the individual frames but produces a discontinuity in the
 34  surface brightness profile.
 35 VCC 1321 (NGC 4489). This galaxy shows a dramatic (almost 90{deg})
 35  isophotal twist that takes place abruptly at approximately 5" from the
 35  center. However, unlike the case of VCC 1537, the twist is not
 35  accompanied by a change in the higher order coefficients, in fact the
 35  isophotes remain very regular all the way out. There is therefore no
 35  evidence that this twist is due to a bar.
 36 VCC 828 (NGC 4387). The galaxy is visibly boxy beyond 1", but otherwise
 36  it does not show evidence of structure. A nucleus is clearly visible
 36  from the individual frames and the surface brightness profiles.
 37 VCC 1250 (NGC 4476). This galaxy harbors a nuclear, clumpy, dust disk,
 37  about 11" in radius. The clumps are clearly organized in a spiral
 37  structure. The plane of the disk is inclined by about 20{deg} to the
 37  line of sight; the north-west side of the disk is the closest. This
 37  disk is similar but clumpier and smaller than the ones seen VCC 1154
 37  or VCC 1532. The correction for dust performs better than in the case
 37  of VCC 1154 or VCC 1532, indicating that the change in the stellar
 37  population embedded in the disk (relative to the one surrounding it),
 37  is not as extreme as in those galaxies. Several blue clumps, organized
 37  in an almost complete arc structure, are however clearly visible
 37  within the disk, and the isophotal parameter within the inner 10"
 37  should be interpreted with caution. There is clear indication of the
 37  presence of a nucleus from both the individual and the color image,
 37  and from the surface brightness profiles. The color of the nucleus
 37  cannot be assessed because of the presence of dust. The nucleus
 37  appears to be offset by just over 1" in the north direction relative
 37  to the center of the dust disk (the disk's major axis is aligned in
 37  the north-northeast direction). The isophotal center is not very
 37  stable even in the outer regions, varying by as much as 0."1 between
 37  subsequent isophotes; but it does seem to be consistent with the
 37  location of the nucleus. The isophotes seem quite regular, at least in
 37  the outer region.
 38 VCC 1630 (NGC 4551). From the individual images, in the very innermost
 38  region, it is barely possible to make out the presence of a faint
 38  stellar disk, possibly flaring out at the edges. This is reflected in
 38  the abrupt change of the A4 and B4 coefficients in the inner 0.1".
 38  There is a clear resolved nucleus.
 39 VCC 1146 (NGC 4458). The innermost isophotes appear quite disky, as
 39  reflected in the negative B4 coefficient in the inner 0.2". The
 39  ellipticity increases steadily toward the center. The galaxy hosts a
 39  large, bright nucleus.
 40 VCC 1025 (NGC 4434). This galaxy is quite round, although it
 40  becomes visibly more elongated in a narrow radial range around 8".
 40  There are no features seen in the color image. There is a hint of the
 40  presence of a large nucleus from a "break" in the surface brightness
 40  profiles around 1".
 41 VCC 1303 (NGC 4483). This galaxy appears to have two smooth spiral
 41  arms, first noticeable extending from the central bulge at a distance
 41  of approximately 7" from the galaxy's center. The arms extend in the
 41  east-west direction at first (the major axis of the galaxy is at a
 41  position angle of 60{deg}), then bend toward north in a clockwise
 41  fashion. The position angle and B4 and A4 coefficients all change
 41  outward of 10" because of the arms. There are no features visible in
 41  the color image.
 42 VCC 1913 (NGC 4623). This galaxy is somewhat similar to VCC 1630 in
 42  that it shows (more clearly in this case) the presence of a thick,
 42  edge-on nuclear stellar disk, about 1" in radius. From the color
 42  image, the disk appears slightly bluer than the host galaxy. A nucleus
 42  is quite apparent in the individual images, and seems to affect the
 42  surface brightness profile in the inner 0.3". At larger scales, the
 42  galaxy appears to have a "structure within the structure" morphology:
 42  within the inner 7", the light is dominated by a boxy bulge. Beyond,
 42  there appears to be a disky (or at least highly elongated) "halo" or
 42  disk. The transition between the two structures is quite abrupt and
 42  can be seen as a discontinuity in the surface brightness profile in
 42  the individual images. All of the structures share the same major
 42  axis.
 43 VCC 1327 (NGC 4486A). Small, faint galaxy with a bright foreground
 43  star nearby. An edge-on dust disk is clearly visible. The galaxy
 43  projects 7.5" from M87.
 44 VCC 1125 (NGC 4452). This galaxy is an edge-on S0. There seem to be
 44  four separate components: a resolved nucleus, an inner, thin stellar
 44  disk, confined within 2" from the center, a "middle" thicker, stellar
 44  disk, extending out to distances of about 17" from the center, and an
 44  outer, thinner stellar disk, which is highly flattened. An inner bulge
 44  seems to be almost an extension of the middle disk. The smaller inner
 44  disk is bluer in color than the outer disks; there is no appreciable
 44  color difference between the middle and the outer disk and the bulge
 44  of the galaxy. The presence of the nucleus is very clear from the
 44  surface brightness profile.
 45 VCC 1475 (NGC 4515). The galaxy shows a nucleus, surrounded by an
 45  edge-on blue disk, which flares out slightly at the end. The disk
 45  extends for a total of about 4". The nucleus is visible in the surface
 45  brightness profile as well.
 46 VCC 1178 (NGC 4464). A compact nucleus is clearly visible in the
 46  color image, but barely discernible in the surface brightness
 46  profiles. The isophotes appear regular.
 47 VCC 1283 (NGC 4479). A clear nucleus is visible from the color
 47  image and the surface brightness profile. The isophotes appear quite
 47  regular, although there seems to be a faint bar extending out to about
 47  30".
 48 VCC 1261 (NGC 4482). This galaxy hosts a resolved nucleus. The
 48  isophotes appear regular. Several faint background galaxies are seen
 48  within 50".
 49 VCC 698 (NGC 4352). The galaxy is quite disky within 1", becoming
 49  boxy further out, and then disky again outside 10". The inner disk
 49  (which is blue) and a resolved nucleus are visible in the color image;
 49  the nucleus is noticeable in the surface brightness profile as well.
 50 VCC 1422. This galaxy has a bright, resolved nucleus, clearly
 50  dominating the surface brightness profile. The isophotes appear
 50  regular. The color image shows possible evidence of a large
 50  filamentary dust structure about 26" southwest of the nucleus,
 50  distributed azimuthally within a 90{deg} radius.
 51 VCC 2048. This galaxy has a bright nucleus, dominating the surface
 51  brightness profile and clearly visible in the color image. The nucleus
 51  is surrounded by a thin edge-on stellar disk, as a consequence of
 51  which the isophotes are very disky.
 52 VCC 1871. Unlike other galaxies in the same magnitude range, this
 52  is quite round, perhaps because of inclination effects. The isophotes
 52  are regular. A bright resolved nucleus is clearly visible in the
 52  surface brightness profiles and color image.
 53 VCC 9. This galaxy has fainter surface brightness than galaxies in
 53  the same magnitude range, and a flat core. There are two bright
 53  clusters within 2" from the center, but nothing at the center of the
 53  isophotes.
 54 VCC 575 (NGC 4318). This galaxy shows a clear structure in the stellar
 54  population. At a distance of about 4" from the center, a stellar disk
 54  or wide ring sets in; the ring is brighter than the region within it,
 54  causing a kink in the surface brightness profile. It is possible that
 54  the ring is actually the result of a spiral structure, although the
 54  spiral "arms" do not appear to extend all the way to the center of the
 54  galaxy. The ring might be similar to the structure seen edge-on in
 54  other galaxies, for instance VCC 1938, where an outer "disk" is
 54  present but does not extend all the way to the center. Although there
 54  is no structure associated with the ring/truncated disk in the color
 54  image, this does show a thin, edge-on red disk extending approximately
 54  2.5" across the nucleus.
 55 VCC 1910. The surface brightness profile is dominated by the stellar
 55  nucleus, which is brighter than any globular cluster within the field.
 55  The isophotes are regular. There is a very red globular cluster just
 55  over 2" west of the nucleus.
 56 VCC 1049. From the brightness profile there does not seem to be
 56  evidence of a separate nuclear component, although the profile is
 56  quite steep and the galaxy becomes significantly bluer toward the
 56  center. The isophotes are fairly regular. There are two small, faint
 56  irregular/spiral galaxies, one 20" to the southeast, the other 19" to
 56  the north, probably both in the background.
 57 VCC 856. This galaxy shows a clear face-on spiral pattern. The arms
 57  are quite wide, smooth and regular. The center of the galaxy has a
 57  bright, resolved nucleus. There is no evidence of a bulge component.
 57  This galaxy would be better classified as a dwarf spiral.
 58 VCC 140. A nucleus is clearly visible both in the color image and in
 58  the surface brightness profiles. The isophotes are regular. Several
 58  faint background galaxies are seen within the field.
 59 VCC 1355. The galaxy has a bright, resolved nucleus. The isophotes
 59  are quite round and regular. 60. VCC 1087. The nucleus is marginally
 59  resolved, and the isophotes appear regular.
 61 VCC 1297 (NGC 4486B). Lauer et al., 1996ApJ...471L..79L, identified a
 61 double nucleus, separated by 12 pc (0.15"), based on deconvolved WFPC2
 61 images of this galaxy. The two nuclei are not immediately apparent in the
 61 ACS images, although the galaxy is quite disky within the inner 100 pc,
 61 with this trend persisting all the way to the center, and the profile is
 61 slightly asymmetric in the inner 40 pc. Beyond about 10", the surface
 61 brightness profile is clearly truncated by interaction with M87, which
 61 projects only 7.3" away.
 62 VCC 1861. Like other galaxies in this magnitude range (with the
 62  exception of VCC 1297) this galaxy has a bright, resolved nucleus
 62  superimposed to a flat core. The isophotes are quite round and
 62  regular.
 63 VCC 543. A resolved nucleus dominates the surface brightness profile.
 63  This galaxy is quite elongated, but the isophotes are regular.
 64 VCC 1431. Round galaxy with a resolved nucleus. There are three red,
 64  faint irregular galaxies between 9" and 12" to the northeast; probably
 64  background. The isophotes are regular.
 65 VCC 1528. This galaxy has a bright, nucleus. The isophotes are
 65  regular.
 66 VCC 1695. This galaxy has a bright, nucleus. The isophotes are regular,
 66  there is no evidence of dust, although the residual images show
 66  evidence of a large-scale spiral structure. In the color image, there
 66  seems to be an elongated, large, red, faint feature about 20" to the
 66  east, although this is not visible in the single images.
 67 VCC 1833. Unlike galaxies in a similar magnitude range, this galaxy
 67 does not appear to have a distinct nucleus. The isophotes are regular.
 68 VCC 437. This galaxy has a bright, resolved nucleus. The isophotes
 68  are regular. A background galaxy cluster is visible in the frame.
 69 VCC 2019. This galaxy has a bright nucleus, and low surface brightness.
 69  Several bright clusters are seen, and a small but resolved object is
 69  detected about 12" to the north.
 70 VCC 33. This galaxy has a bright nucleus dominating the surface
 70  brightness profile. The globular cluster population is small. An
 70  extremely red object (not obviously extended) is seen about 4" east of
 70  the nucleus.
 71 VCC 200. This galaxy has a bright nucleus dominating the surface
 71  brightness profile.
 72 VCC 571. The center of this galaxy is crossed by a dust lane running
 72  in the northwest direction (approximately along the major axis of the
 72  galaxy). The dust lane extends out to about 8" (becoming wider and
 72  more diffuse with increasing distance from the center) in the
 72  southeast direction, and just over 1" in the northwest direction. More
 72  wisps are seem further out, especially on the northwest side. The
 72  correction for dust performs well. Several blue star clusters are seen
 72  near the center (although not along the dust lane itself), probably
 72  indicative of recent star formation.
 73 VCC 21. Elongated system, may be better classified as a dwarf
 73  irregular/dwarf elliptical transition object. There are several bright
 73  clusters near, but none exactly at, the center.
 74 VCC 1488. Elongated system. There is a small spiral galaxy, about 6"
 74  across, 8" to the south; this galaxy has been masked in fitting the
 74  isophotes. An unconstrained fit to the isophotes runs into problems
 74  because of the low gradient in the surface brightness profile, but
 74  between 0.5" and 5" the isophotes are centered very accurately on the
 74  nucleus. ELLIPSE was therefore run over a more extended radial range
 74  by fixing the position of the center to that of the nucleus.
 75 VCC 1779. This galaxy might be best classified as a dIrr/dE
 75  transition object. Dust filaments are seen radiating from the center
 75  outward within the inner 6". From a visual inspection of the image,
 75  there appear to be very few objects that could be identified as GCs;
 75  three of these are near the center, although none is at the nuclear
 75  position. A small spiral galaxy is seen about 17" to the southwest .
 76 VCC 1895. Highly elongated, faint elliptical. The nucleus is clearly
 76  visible and may be slightly elongated in the same direction as the
 76  major axis of the galaxy.
 77 VCC 1499. This galaxy should be classified as a dIrr/dE. There are
 77  several bright clusters and blue associations close to the center,
 77  although there does not appear to be a proper nucleus, and there is no
 77  convincing evidence of dust. The center of the isophotes drifts to the
 77  east as the radius is increased.
 78 VCC 1545. This galaxy has a bright, resolved nucleus. The galaxy is
 78  fairly round, the isophotes are regular. The galaxy has a fairly
 78  substantial population of bright globular clusters.
 79 VCC 1192 (NGC 4467). This galaxy is a close companion of M49, which
 79  lies 4.2" away, outside the WFC frame to the east; the outer surface
 79  brightness profile is tidally truncated, the ellipticity is also
 79  affected. The surface brightness profile in the center is brighter (by
 79  1 to 2 magnitudes) than that of galaxies in the same magnitude range.
 79  A resolved nucleus is clearly present in the color images, as well as
 79  in the surface brightness profiles. There is a small blue cluster
 79  within 0.1" from the nucleus, a second about 0.9" to the southeast.
 80 VCC 1857. Very low surface brightness, elongated system. There are
 80  several faint clusters in the frame, and a very bright one about 6"
 80  west of the center. The position of the center was determined by block
 80  averaging and then contouring the images and was held fixed in fitting
 80  the isophotes.
 81 VCC 1075. The isophotal center is consistent with the location of
 81  a bright cluster, which is therefore identified as the nucleus. The
 81  central position is held fixed at the nuclear location in fitting the
 81  isophotes.
 82 VCC 1948. Elongated system. Although there are some faint clusters
 82  around the center, none appears to be at the isophotal center.
 83 VCC 1627. This galaxy has brighter surface brightness than galaxies
 83  in the same magnitude range. As a consequence, the nucleus is not as
 83  prominent in the surface brightness profile, although it is clearly
 83  visible in the color image. The galaxy is quite round; there are no
 83  signs of disturbance in the isophotes. A very red cluster is seen
 83  about 6" west of the nucleus; otherwise the galaxy has a small GC
 83  system compared to galaxies in the same magnitude range.
 84 VCC 1440. This galaxy has brighter surface brightness than galaxies
 84  with comparable B_T_, and a large number of bright globular clusters
 84  for a galaxy of this magnitude. A bright, resolved nucleus is clearly
 84  present.
 85 VCC 230. This galaxy has a bright nucleus. The galaxy is quite
 85  round and has what appears to be a significant globular cluster
 85  population. The isophotes are regular.
 86 VCC 2050. Very elongated system with a central, faint nucleus. The
 86 galaxy appears regular. A very red cluster is seen just over 7" south
 86 of the nucleus.
 87 VCC 1993. The g- and z-band images show a faint nucleus, which does
 87  not affect significantly the surface brightness profile. From a visual
 87  inspection of the image, there are very few objects that could be
 87  identified as globular clusters.
 88 VCC 751. Fairly elongated galaxy with a bright nucleus. The isophotes
 88  appear regular. There is a very red background galaxy about 12" east
 88  of the nucleus.
 89 VCC 1828. The nucleus is quite prominent.
 90 VCC 538 (NGC 4309A). Round system, with a bright, resolved nucleus.
 90  There is a bright spiral galaxy about 90" to the south.
 91 VCC 1407. This galaxy has a bright nucleus and has regular isophotes.
 91  There seems to be a large population of globular clusters. A very blue
 91  and small (less than 0.2" across) elongated feature is seen about 1.5"
 91  east of the nucleus. i
 92 VCC 1886. The brightest cluster in the frame appears to be at the
 92  location of the isophotal center; a second, almost as bright cluster
 92  is 4.7" to the northeast.
 93 VCC 1199. The galaxy is a close companion of M49, which lies only 4.5"
 93  away, and is a prime candidate for galaxy harassment. Its surface
 93  brightness is brighter than galaxies in the same magnitude range and
 93  is tidally truncated in the outer regions. The nucleus looks elongated
 93  (along the major axis of the galaxy), furthermore, there seems to be,
 93  from the g- and z-band images, a very thin edge-on disk also aligned
 93  with the galaxy major axis, extending less than 1" on either side of
 93  the center. The residual images also show evidence of a large-scale
 93  spiral pattern.
 94 VCC 1743. Very low surface brightness elongated galaxy, with a very
 94  faint nucleus. The nucleus seems to have the same color as the
 94  surrounding galaxy.
 95 VCC 1539. This galaxy has a large number of bright globular clusters
 95  for a galaxy of this magnitude. The galaxy is very round, has a bright
 95  nucleus, and becomes increasingly bluer toward the center.
 96 VCC 1185. Small, round system, with a bright nucleus. The isophotes are
 96  regular.
 97 VCC 1826. This galaxy has a very sparse cluster system. The nucleus is
 97  quite prominent.
 98 VCC 1512. This is a dIrr/dE transition object. There is a loose
 98  association of blue stars at the center. It is not clear whether this
 98  galaxy has dust or whether the darker areas seen toward the center are
 98  simply an illusion created by the presence of the bright blue
 98  associations. There does not seem to be a proper nucleus.
 99 VCC 1489. The light is dominated by a bright, resolved nucleus.
100 VCC 1661. This galaxy has a bright, resolved nucleus. The galaxy appears
100  quite round. The isophotes are regular.