0859+0330 This detection does not seem to have an optical counterpart and 
0859+0330  is not in the vicinity of another galaxy. The velocity width is about
0859+0330  90km/s, and the highest measured column density at this resolution
0859+0330  is N_HI_~4.7x10^-17^cm^-2^.
0921+0200 detection with no visible optical counterpart in the DSS image, and 
0921+0200  no known galaxy within four degrees. This object has a narrow line 
0921+0200  width of only 55km/s and an integrated column density of 
0921+0200  N_HI_~3.5x10^-17^cm^-2^, assuming the emission fills the beam.
0956+0845 HI detection in the immediate neighbourhood of NGC 3049 at a projected
0956+0845  distance of only ~0.7 degrees, although the central velocity is 
0956+0845  offset by about 150km/s. This detection has a relatively weak, but 
0956+0845  very broad profile of ~200km/s, it could be related to NGC 3049. The
0956+0845  total flux of this detection is 11Jy.km/s, corresponding to a column 
0956+0845  density of N_HI_~1.4x10^18^cm^-2^, integrated over the full line 
0956+0845  width.
1035+0045 Isolated HI detection with no nearby galaxy at a similar radial 
1035+0045  velocity. At angular distances of two and four degrees, there are 
1035+0045  strong indications for other HI detections with a similar profile at 
1035+0045  exactly the same radial velocity. These detections did not pass the 
1035+0045  8{sigma} detection limit and therefore are not listed in the table of
1035+0045  detections. WVFS 1035+0045 could be the brightness component of a 
1035+0045  much more extended underlying filament, the velocity width is 65km/s,
1035+0045  with an integrated column density of N_HI_~4.1x10^-17^cm^-2^.
1055+0415 A relatively strong HI detection in the direct vicinity of NGC 3521, 
1055+0415  at an offset of 2.5 degrees. The radial velocity is comparable, 
1055+0415  although 100km/s offset from the systematic velocity of NGC 3521. 
1055+0415  Note, however, the more than 500km/s linewidth of this galaxy. When 
1055+0415  assuming a distance to this galaxy of 7.7Mpc, the projected 
1055+0415  separation of WVFS 1055+0415 is ~350 kpc. It has a 110km/s line 
1055+0415  width and an integrated column density of N_HI_~5.4x10^-17^cm^-2^.
1140+0115 There seems to be a bridge connecting this source with UGC 6578, which
1140+0115  is a relatively small galaxy. The angular offset to UGC 6578 is about
1140+0115  1.1 degree, which corresponds to 300kpc at a distance of 15.3Mpc. 
1140+0115  WVFS 1140+0115 has a line width of 85km/s and a column density of 
1140+0115  N_HI_~3.8x10^-17^cm^-2^.
1152+0145 This detection is about 3.5 degrees separated from two massive 
1152+0145  galaxies, NGC 4116 and NGC 4123. These two galaxies are confused in 
1152+0145  our data cubes and appear as one source. The radial velocity of 
1152+0145  WVFS 1152+0145 is similar to the two galaxies, and when using a 
1152+0145  distance of 25.4Mpc to NGC 4116, the projected separation of the 
1152+0145  filament is 1.5Mpc. An interesting fact is that the spectral profile
1152+0145  of NGC 4116/4123 shows an enhancement at exactly the velocity of 
1152+0145  WVFS 1152+0145, indicating that there is extra HI at this velocity. 
1152+0145  WVFS 1152+0145 has a line width of 70km/s and an integrated column 
1152+0145  density of N_HI_~3.3x10^-17^cm^-2^. 
1200+0145 An HI detection at exactly the same radial velocity as UGC 7332 at a 
1200+0145  separation of 4.4 degrees. UGC 7332 has a likely distance of seven 
1200+0145  Mpc, which means that the projected distance between the galaxy and 
1200+0145  WVFS 1200+0145 is about 500kpc. We note that there are several other
1200+0145  galaxies at a very similar radial velocity, but slightly more 
1200+0145  separated from WVFS 1200+0145. This new HI detection has a line width
1200+0145  of only 50km/s and a column density of N_HI_~4.4x10^-17^cm^-2^.
1212+0245 This detection is most likely related to PGC 135791, as both position 
1212+0245  and velocity of the HI detection agree very well. It is the first 
1212+0245  time that an HI component has been detected for this dwarf galaxy at 
1212+0245  a distance of 5.3Mpc. The HI detection is quite strong, with a total
1212+0245  estimated flux of 6.3Jy.km/s when integrating over the full line 
1212+0245  width of 100km/s, which corresponds to a column density of 
1212+0245  N_HI_~8.2x10^-17^cm^-2^.
1216+0415 This is a relatively bright new detection, with a total flux of 
1216+0415  5.6Jy.km/s integrated over the 90km/s line width, which corresponds 
1216+0415  to a column density of N_HI_~7.2x10^-17^cm^-2^. There are several 
1216+0415  galaxies in the projected vicinity of WVFS 1216+0415 for which the 
1216+0415  redshift and distance are unknown. Most apparent is 
1216+0415  SDSS J121643.27+041537.7, a diffuse dwarf galaxy, listed in the Sloan
1216+0415  Digital Sky Survey (SDSS) archive. Although the centroid in the WVFS 
1216+0415  data is imprecise due to the low resolution, SDSS J121643.27+041537.7
1216+0415  is within the 90% contour of the peak flux. Higher resolution HI data
1216+0415  could provide a better indication whether the detected HI is related 
1216+0415  to this object. Separated by 2.2 degrees (corresponding to 500 kpc at
1216+0415  assuming distance of 13.1Mpc) from WVFS 1216+0415 is PGC 040411. This
1216+0415  HI detection could be related to the spiral galaxy PGC 040411, 
1216+0415  because of the relatively small projected distance and the matched 
1216+0415  radial velocity.
1217+0115 This detection is in the vicinity of several galaxies, at different 
1217+0115  distances, therefore it is difficult to say whether there is a 
1217+0115  relation between WVFS 1217+0115 and any of these galaxies. The most 
1217+0115  nearby galaxy is UGC 7394, separated by 0.8 degrees, which 
1217+0115  corresponds to 370kpc, at a distance of 27Mpc. At a distance of 
1217+0115  13.1Mpc are three galaxies: M61, UGC 7612 and UGC 7642, all separated
1217+0115  by ~3 degrees from WVFS 1217+0115, or 700kpc. There is reasonable 
1217+0115  correspondence in velocity with all of the aforementioned galaxies. 
1217+0115  Because of the large over-density it is most likely that 
1217+0115  WVFS 1217+0115 belongs to the group containing M61. The line width of
1217+0115  this detection is 80km/s, with an integrated column density 
1217+0115  of N_HI_~3.5x10^-17^cm^-2^.
1234+0345 This object is the HI counterpart of UGC 7715, at the same position 
1234+0345  and velocity. This galaxy is not listed in the HIPASS catalogue, 
1234+0345  however, it is not a completely new detection as the LEDA database 
1234+0345  gives a flux of 1.7Jy.km/s. We detect an almost two times larger flux
1234+0345  of 3.9Jy.km/s and a line width of 80km/s, which corresponds to an 
1234+0345  HI column density of N_HI_~4.9x10^-17^cm^-2^.
1253+0145 The line width of this detection is only 50km/s, with an integrated 
1253+0145  column density of N_HI_~3.1x10^-17^cm^-2^. This HI detection is 
1253+0145  possibly the counterpart of SDSS J125249.40+014404.3, a dwarf 
1253+0145  Elliptical listed in the SDSS archive with a radial velocity of 
1253+0145  883km/s and a distance of 5.8Mpc. Another possibility is a relation
1253+0145  with NGC 4772, this galaxy is at a larger distance of 13.0Mpc. There
1253+0145  is a connecting bridge of only half a degree and the radial velocity 
1253+0145  matches the peak of this object. The peak of this companion is 
1253+0145  slightly brighter than the galaxy itself, which is a little bit 
1253+0145  suspicious.
1324+0700 This detection is very isolated, and there does not seem to be any 
1324+0700  relationship to a nearby galaxy out to a few degrees. WVFS 1324+0700 
1324+0700  has a line width of 70km/s and a column density of 
1324+0700  N_HI_~3.9x10^-17^cm^-2^.
1424+0200 This detection appears to be very isolated, without a recognisable 
1424+0200  connection to a galaxy. The DSS image shows an optical galaxy, this 
1424+0200  is UGC 9215 at a radial velocity of 1397km/s, this is about 850km/s 
1424+0200  different from WVFS 1424+0200, so any relation is very unlikely. The 
1424+0200  line width of WVFS 1424+0200 is 70km/s and it has an integrated 
1424+0200  column density of N_HI_~4.7x10^-17^cm^-2^. 
1500+0815 There are several massive galaxies with a systemic velocity within 
1500+0815  100km/s of the velocity of WVFS 1500+0815 (NGC 5964, NGC 5921, 
1500+0815  NGC 5701, NGC 5669 and NGC 5194). All these galaxies are at a 
1500+0815  distance of about 24Mpc. At this distance the projected separation to
1500+0815  WVFS 1500+0815 would be between 2.5 and 5Mpc. A direct connection to
1500+0815  any of the galaxies is not obvious, unless there is a very large 
1500+0815  diffuse envelope between them, which is perhaps not unreasonable, as 
1500+0815  the radial velocities of the galaxies are all very similar. The 
1500+0815  highest measured column density of WVFS 1500+0815 is 
1500+0815   ~4.1x10^-17^cm^-2^, when integrated over the full line width of 
1500+0815   105km/s. As for all the new detections, there are many optical 
1500+0815   detections in the projected vicinity of the H idetection, but 
1500+0815   without redshift information. Worth special mention is 
1500+0815   SDSS J150103.32+081936.5, a dwarf galaxy that based on visual 
1500+0815   assessment could be at the relevant distance.
1524+0430 There are no known galaxies with a comparable radial velocity in the 
1524+0430  vicinity or WVFS 1524+0430. In the DSS images we find two dwarf 
1524+0430  galaxies that could be related to the HI detection: 
1524+0430  SDSS J152444.50+043302.3 and SDSS J152445.97+043532.5. Higher 
1524+0430  resolution HI data would be needed to resolve the HI and provide more
1524+0430  information about the exact position. Based on visual inspection both
1524+0430  SDSS sources could be at a relevant distance, as the optical 
1524+0430  appearance is similar to dwarf galaxies with a known radial velocity.
1524+0430  The line width is only 55km/s and it has a column density 
1524+0430  of N_HI_~3.1x10^-17^cm^-2^.
1529+0045 This is also an isolated HI detection without a clear optical 
1529+0045  counterpart. With a line width of only 50km/s and an integrated flux 
1529+0045  of 3.5Jy.km/s it is a relatively narrow, but strong detection 
1529+0045  compared to the other isolated detections. The peak column density of
1529+0045  WVFS 1529+0045 is N_HI_~4.4x10^-17^cm^-2^.
1547+0645 Another isolated detection without any nearby known galaxy or optical 
1547+0645  counterpart. With a velocity width of 50km/s and a total flux of only
1547+0645  2.2Jy.km/s this is the weakest detection that passed the detection 
1547+0645  threshold. The column density of WVFS 1547+0645 is only 
1547+0645  N_HI_~2.9x10^-17^cm^-2^.
1637+0730 The last new detection in the survey, NGC 6106 is at an offset of 
1637+0730  4.75 degrees to WVFS 1637+0730, corresponding to a projected distance
1637+0730  of two Mpc, at an assumed distance of 23.8Mpc. The radial velocity of
1637+0730  this galaxy is 1448km/s which is about 100km/s offset from 
1637+0730  WVFS 1637+0730. Because of the relatively large projected distance 
1637+0730  and the significant offset in velocity, a direct relation between 
1637+0730  WVFS 1637+0730 and NGC 6106 is not very obvious, and WVFS 1637+0730 
1637+0730  is more likely another isolated detection. In the DSS image an 
1637+0730  optical galaxy can be identified, this is UGC 10475, a background 
1637+0730  galaxy with a radial velocity of 9585km/s. The velocity width of 
1637+0730  WVFS 1637+0730 is 60km/s and it has a column density 
1637+0730  of N_HI_~3.6x10^-17^cm^-2^.