J0631-01  The distance between the HI position and the counterpart is rather large (d_sep=6.1'), but the HI detection is located near the corner of the cube (l,b=212.2{deg},-5.1{deg}), where the sensitivity is lower. On the other hand, the HIPASS position is much closer to the counterpart (d_sep_=2.3')
J0647-00A There is a possible galaxy visible in the NIR next to a group of stars at (R.A.,decl.)=(06:47:06.0,-00:35:27), with a distance of 1.2' to the HI position
J0653-03A J0653-03A, J0653-03B, and J0653-04 The spectra of all three detections show emission from the other galaxies as well
J0653-03B J0653-03A, J0653-03B, and J0653-04 The spectra of all three detections show emission from the other galaxies as well
J0653-04  J0653-03A, J0653-03B, and J0653-04 The spectra of all three detections show emission from the other galaxies as well
J0657-05A J0657-05A and J0657-05B Both spectra show emission of the other galaxy as well
J0657-05B J0657-05A and J0657-05B Both spectra show emission of the other galaxy as well
J0700-04  Begum et al. (2005MNRAS.359L..53B) observed this galaxy with the VLA and found that the HI emission comes from two dwarf galaxies. Both are faintly visible on the deep NIR images
J0704-13  Underneath the narrow HI profile there appears to be a broader profile (under the detection threshold) at a more northern decl., as can be made out in the data cube. The obvious cross-match for the narrow profile is the nearly face-on galaxy 2MASXJ07042532-1346257, while farther north (at about equal distance from the fitted HI position) lies a galaxy pair, 2MASXJ07041909-1338217 and an unpublished galaxy at (R.A.,decl.)=(07:04:18.7,-13:37:47), which is likely the counterpart of the broader profile
J0709-03  This galaxy is not in NED but was found in SIMBAD
J0717-22B J0717-22B and J0717-22A These two detections are close together, and the images show a close galaxy pair that is likely interacting (it is bright in IRAS as well as WISE). There is a (single) optical velocity for the IRAS source (2750+/-70km/s; Visvanathan & Yamada 1996 (cat. J/ApJS/107/521)) that agrees well with the main HI detection (J0717-22A). There are also three smaller galaxies in the area, two of which are likely background, but one (2MASXJ07174038-2224406) is a possible candidate, too. The HI detection J0717-22A comes most likely either from the more edge-on component of the galaxy pair (CGMW 2-0730) or from both (the profile is lopsided). The narrow profile J0717-22B could come from the less inclined component of the galaxy pair (CGMW 2-0731), or it could come from a hidden late-type galaxy (A_B_=3.8^m^). It is less likely coming from 2MASXJ07174038-2224406, which seems nearly edge-on (though at these extinction levels faint outer spiral arms could be invisible)
J0717-22A J0717-22B and J0717-22A These two detections are close together, and the images show a close galaxy pair that is likely interacting (it is bright in IRAS as well as WISE). There is a (single) optical velocity for the IRAS source (2750+/-70km/s; Visvanathan & Yamada 1996 (cat. J/ApJS/107/521)) that agrees well with the main HI detection (J0717-22A). There are also three smaller galaxies in the area, two of which are likely background, but one (2MASXJ07174038-2224406) is a possible candidate, too. The HI detection J0717-22A comes most likely either from the more edge-on component of the galaxy pair (CGMW 2-0730) or from both (the profile is lopsided). The narrow profile J0717-22B could come from the less inclined component of the galaxy pair (CGMW 2-0731), or it could come from a hidden late-type galaxy (A_B_=3.8^m^). It is less likely coming from 2MASXJ07174038-2224406, which seems nearly edge-on (though at these extinction levels faint outer spiral arms could be invisible)
J0718-09  There are two low surface brightness (LSB) galaxies in the field; the closer and more extended one is given as the cross-match. It is possible, though, that the other galaxy at (R.A.,decl.)=(07:18:14.5,-09:03:03) may contribute to the signal (see J0700-04)
J0725-24A The profile shows a high-velocity shoulder. A close inspection of the data cube indicates a fainter HI emission at smaller R.A. with the obvious candidate 2MASXJ07245535-2430057
J0732-16  This seems to be a star-forming region with an HII region and star cluster. There is a 2MASS detection nearby (2MASXJ07315300-1658237) that looks like a small, nearly edge-on galaxy. However, the extinction in this area is large and spatially highly variable, which means that the galaxy could be also be a nearly face-on barred spiral. Owing to the large spatial variation of the extinction, a hidden galaxy is also possible
J0733-28  The profile shows a high-velocity shoulder that seems to be caused by the inclined galaxy at (R.A.,decl.)=(07:33:23.2,-28:44:01)
0738-26   A galaxy pair is the obvious match for the HI detection. Both galaxies seem to be of similar (late) type, with CGMW 2-1056 being more edge-on and CGMW 2-1059 being less inclined. It is likely that both have HI and possibly contribute to the HI detection
J0742-20A There are at least five galaxies of similar size visible that could form a group of galaxies. The counterpart is a large spiral that is the most prominent in the B band. It is also the reddest on WISE images
J0743-32  There are two 2MASS galaxies in the area, but both are of earlier morphological type than the cross-match and hence less likely candidates. Nevertheless, they cannot be fully excluded as candidates
J0744-26  J0744-26 and J0744-25 These two HI detections are only 2.5' apart. There are five galaxies visible, two of which are possible candidates. 2MASXJ07442148-2602486 is the larger candidate and a late-type spiral. It agrees well with the profile of J0744-26, while the other galaxy, 2MASXJ07442386-2600016, seems to be an early-type spiral with a smaller diameter, which agrees better with J0744-25. Paturel et al. 2003 (cat. VII/237) observed 2MASXJ07442386-2600016 and found a detection at v=4686km/s though with a very low S/N of 2.7
J0744-25  J0744-26 and J0744-25 These two HI detections are only 2.5' apart. There are five galaxies visible, two of which are possible candidates. 2MASXJ07442148-2602486 is the larger candidate and a late-type spiral. It agrees well with the profile of J0744-26, while the other galaxy, 2MASXJ07442386-2600016, seems to be an early-type spiral with a smaller diameter, which agrees better with J0744-25. Paturel et al. 2003 (cat. VII/237) observed 2MASXJ07442386-2600016 and found a detection at v=4686km/s though with a very low S/N of 2.7
J0745-18  J0745-18 and J0746-18 Both spectra show emission of the other galaxy as well
J0746-18  J0745-18 and J0746-18 Both spectra show emission of the other galaxy as well
J0747-21  2MASXJ07471872-2138080 is confirmed through an optical velocity of v=6988+/-40km/s (Visvanathan & Yamada 1996 (cat. J/ApJS/107/521)). A nearby early spiral could be a companion
J0748-25A J0748-25A and J0748-25B These two HI detections are 4.1' apart (and at different velocities). There are six possible candidates in the area. 2MASXJ07483666-2510211 was detected by Paturel et al. 2003 (cat. VII/237) at v=6809km/s, while Kraan-Korteweg et al. (2015, in preparation) have observed 2MASXJ07483252-2516431 at v=6804km/s. Both used the Nancay Radio Telescope (NRT) and have measured a similar flux (~4.5Jykm/s and ~5.1Jykm/s, respectively), while our detection has a higher flux. We therefore conclude that 2MASXJ07483452-2513191, which is closer to our HI position, is the counterpart of J0748-25B. Owing to the two NRT observations, we can exclude four of the six galaxies as the candidate for J0748-25A. 2MASXJ07480561-2513459 has an optical velocity of v=7980km/s (Acker et al. 1991A&AS...87..499A) and is an IRAS galaxy. It is the most likely candidate for J0748-25A
J0748-25B J0748-25A and J0748-25B These two HI detections are 4.1' apart (and at different velocities). There are six possible candidates in the area. 2MASXJ07483666-2510211 was detected by Paturel et al. 2003 (cat. VII/237) at v=6809km/s, while Kraan-Korteweg et al. (2015, in preparation) have observed 2MASXJ07483252-2516431 at v=6804km/s. Both used the Nancay Radio Telescope (NRT) and have measured a similar flux (~4.5Jykm/s and ~5.1Jykm/s, respectively), while our detection has a higher flux. We therefore conclude that 2MASXJ07483452-2513191, which is closer to our HI position, is the counterpart of J0748-25B. Owing to the two NRT observations, we can exclude four of the six galaxies as the candidate for J0748-25A. 2MASXJ07480561-2513459 has an optical velocity of v=7980km/s (Acker et al. 1991A&AS...87..499A) and is an IRAS galaxy. It is the most likely candidate for J0748-25A
J0748-26  J0748-26, J0749-26A, and J0749-26B These three HI detections are close together, and the profiles are confused. While J0748-26 and J0749-26B have obvious candidates, MIRIAD failed to fit the position of J0749-26A, and the distance to the cross-match could be larger. There are two candidates, ESO 493-G017 and 2MASXJ07490476-2611061. ESO 493-G017 is an Sab galaxy and was observed with the NRT by Chamaraux et al. 1999 (cat. J/MNRAS/307/236), who find a lower peak flux (~60mJy). 2MASXJ07490476-2611061 is therefore the more likely counterpart
J0749-26A J0748-26, J0749-26A, and J0749-26B These three HI detections are close together, and the profiles are confused. While J0748-26 and J0749-26B have obvious candidates, MIRIAD failed to fit the position of J0749-26A, and the distance to the cross-match could be larger. There are two candidates, ESO 493-G017 and 2MASXJ07490476-2611061. ESO 493-G017 is an Sab galaxy and was observed with the NRT by Chamaraux et al. 1999 (cat. J/MNRAS/307/236), who find a lower peak flux (~60mJy). 2MASXJ07490476-2611061 is therefore the more likely counterpart
J0749-26B J0748-26, J0749-26A, and J0749-26B These three HI detections are close together, and the profiles are confused. While J0748-26 and J0749-26B have obvious candidates, MIRIAD failed to fit the position of J0749-26A, and the distance to the cross-match could be larger. There are two candidates, ESO 493-G017 and 2MASXJ07490476-2611061. ESO 493-G017 is an Sab galaxy and was observed with the NRT by Chamaraux et al. 1999 (cat. J/MNRAS/307/236), who find a lower peak flux (~60mJy). 2MASXJ07490476-2611061 is therefore the more likely counterpart
J0751-26  A possible candidate looks small and seems to be a more distant galaxy. However, an LSB halo cannot be excluded (WISE images show considerable [foreground] emission in the W3 and W4 bands and are therefore not conclusive)
J0753-22  The candidate is a galaxy triple (IRAS source), and if they are companions, the HI signal could come from more than one of them. Note that the HI detection in the literature is associated with CGMW 2-1471, which is the smallest galaxy in the triplet. There are more galaxies in the area that may indicate a galaxy group
J0755-23  At least five candidates are visible in the area. The largest and brightest, 2MASXJ07551159-2304175, is an inclined early spiral and a likely candidate for this HI mass (logM_HI_=9.8). Two other galaxies, CGMW 2-1571 and a new galaxy at (R.A.,decl.)=(07:55:34.1,-23:04:33), are also large but bluer and of later morphological type. This is possibly a group of galaxies
J0756-26  The profile is confused. The HIPASS profile, with a position d_sep_=5' farther south, extends only to v~6700km/s, while our profile extends to v~6800km/s. Using the HIPASS webpage, the position of our candidate gives a more similar profile to ours. The HIZOA cube shows a peak at (R.A.,decl.)~(07:56:47,-26:16:27), which was not identified as a separate detection during the search. We conclude that the confusing partner is 2MASXJ07563846-2615018 far in the south. Huchtmeier et al. 2001 (cat. J/A+A/377/801) observed this galaxy with the Effelsberg Radio Telescope at an HI velocity of 241km/s. The HIZOA data cube does not show anything at this velocity and with a peak flux of 67mJy and a width of W_50_=26km/s
J0756-31  There are two equally sized galaxies close together, possibly a pair. One seems edge-on; the other has a small inclination. The profile is more consistent with the less inclined galaxy
J0802-22  The counterpart, ESO 494-G013, was also observed with the Effelsberg Radio Telescope by Kraan-Korteweg & Huchtmeier (1992A&A...266..150K) and detected at v=1983km/s. We could not confirm this detection at the given peak flux of ~0.15Jy
J0805-27  J0805-27 and J0806-27 These two HI detections are close together, and the profiles cannot be fully separated, that is, some of the HI parameters are uncertain
J0806-27  J0805-27 and J0806-27 These two HI detections are close together, and the profiles cannot be fully separated, that is, some of the HI parameters are uncertain
J0807-25  Kraan-Korteweg & Huchtmeier (1992A&A...266..150K) detected this galaxy with the Effelsberg Radio Telescope at v=1019km/s, while our detection is at v=7679km/s. The HIPASS archive (http://www.atnf.csiro.au/research/multibeam/release/) does not show any (bright) detection at this position and velocity
J0808-35  There are two candidates of similar size: 2MASXJ08083663-3558328 is of a later spiral type and more inclined than 2MASXJ08080066-3558243. The HI detection lies between these two galaxies, and from a closer inspection of the data cube it is likely that both galaxies contribute to the signal. C. Kraan-Korteweg et al. (2016, in preparation), using the NRT, detected 2MASXJ08080066-3558243 without the broader base of our detection (which is therefore likely due to 2MASXJ08083663-3558328)
J0816-27B A diffuse emission visible in the B band at (R.A.,decl.)=(08:17:07.0,-27:45:15) at a distance of 3.0' to the HI position is the likely counterpart if confirmed as a galaxy
J0817-27  The HI profile seems to be either disturbed or confused. The counterpart is NGC 2559, which appears also disturbed in the optical (Corwin et al., 1985sgcc.book.....C). There is an LSB dwarf close by, at (R.A.,decl.)=(08:17:24.4,-27:28:04), which may be a companion. At about 18' north and south are two other HI detections (J0816-27A and J0816-27B) with similar velocities
J0817-29A This cross-match is listed in SIMBAD but not in NED
J0822-36  There is a possible galaxy visible in the NIR at (R.A.,decl.)=(08:22:50.4,-36:36:41), with a distance of 0.5' to the HI position, which, if real, is a likely counterpart
J0824-41  There are two similar-looking galaxies, possibly a galaxy pair. 2MASXJ08240445-4144221 is more inclined, while 2MASXJ08235945-4143111 seems to show a bar and the start of a spiral arm; both match the profile well enough. The profile has a low S/N of 5, and it is not possible to tell whether one or both galaxies contribute to the signal
J0827-35  Paturel et al. 2003 (cat. VII/237) have observed IRAS 08254-3512, which is 5.4' north of our detection. Their detection is similar to ours with a slightly lower peak flux. Nothing is visible at the IRAS position, and the counterpart is more likely an invisible LSB between these two positions (which would agree with the narrow single-peak profile and low HI mass (logM_HI_=8.0)
J0827-36  There are two galaxies close together, probably a galaxy pair. 2MASXJ08271103-3629389 is edge-on and seems to match the profile better; it also has an optical velocity of 9512+/-40km/s (Visvanathan & Yamada 1996 (cat. J/ApJS/107/521)). The pair was detected by IRAS as well
J0834-37  The cross-match is a nearly face-on spiral galaxy. There is a diffuse LSB galaxy visible in the B band close by, at (R.A.,decl.)=(08:34:16.9,-37:32:36), which may contribute to the signal
J0851-44  There are two possible counterparts visible in the NIR, one edge-on and one a little inclined. The profile seems to match the galaxy with less inclination better
J0857-39  J0857-39 and J0858-39 Both spectra show emission of the other galaxy as well
J0858-39  J0857-39 and J0858-39 Both spectra show emission of the other galaxy as well
J0858-45A There are two possible counterparts visible in the NIR, possibly a galaxy pair. 2MASXJ08580941-4548126 shows spiral arms, either disturbed or with a companion close by, while 2MASXJ08581399-4550547 is a very inclined early-type spiral. The profile matches the former slightly better, and a possible contribution from both galaxies cannot be excluded
J0902-53  There is a small edge-on galaxy in the field. Even taking the extinction into account (A_B_=2.7^m^, the galaxy seems too small for this distance (v=7122km/s) and HI mass (logM_HI_=9.8) but cannot be fully excluded
J0916-54A J0916-54A and J0916-54B Both spectra show emission of the other galaxy as well
J0916-54B J0916-54A and J0916-54B Both spectra show emission of the other galaxy as well
J0927-48  The high-velocity shoulder in the profile is likely caused by J0929-48
J0932-51  The cross-match is an interacting galaxy pair (IRAS source). Both are spirals, and it is not possible to decide where the HI comes from
J0939-56  There is a possible galaxy visible in the NIR at (R.A.,decl.)=(09:39:36.3,-56:53:05) with a distance of 0.8' to the HI position, which, if real, matches the profile well
J0949-47A The cross-match (ESO 213-G002) is a peculiar S0 galaxy that seems to have either a companion or a jet to the south. Farther south (d_sep_=3.6) is RKK 1666, which is likely to contribute: the data cube shows a faint, narrower profile at (R.A.,decl.)~(09:49:24,-47:59:48)
J0949-56  The distance between the HI position and the position of the cross-match, d_sep_=11.8', is for an S/N of 77 rather large. A closer inspection of the data cube revealed a fainter HI detection close by (d_sep_=1.6') with an approximate position of (R.A.,decl.)~(09:48:18.6,-56:29:49) and v~1641km/s, which appears as a low-velocity shoulder in the profile of J0949-56. The obvious candidate here is 2MASXJ09482319-5627370
J0950-49  There are two different optical velocities for this galaxy: v=12391+/-500km/s (Kraan-Korteweg et al. 1995, cat. J/A+A/297/617) is uncertain and seems high for a galaxy of this appearance; v=4043+/-82km/s (Saunders et al. 2000, cat. VII/221) is about 3{sigma}  from our HI velocity and agrees better with the optical appearance of the galaxy
J0950-52  A possible candidate visible at all wavelengths is close to a star, which makes it difficult to determine its appearance, but it seems too small for this velocity (v=2244km/s). The star and the extinction (A_B_=4.3^m^) could hide a larger halo, but a hidden LSB galaxy is a more likely cross-match. The galaxy is a possible IRAS source (IRAS 09482-5209; though it could be also the bright star to the north)
J0952-61  No galaxy is visible at the position of RKK 1733. It is only d_sep_=0.8' from the 2MASS position, which is not listed by Kraan-Korteweg 2000 (cat. J/A+AS/141/123), though it is clearly visible in the B band. It seems possible that both IDs indicate the same galaxy
J0952-55A The profile is highly lopsided. The cross-match is large and diffuse with a small bulge in the NIR. It is not possible to distinguish whether it may be disturbed or may have a small companion
J0953-49  There is a large LSB galaxy visible in the B band, as well as a smaller inclined galaxy (RKK 1732). The LSB galaxy matches the profile better
J1000-58A J1000-58A and J1000-58B The two counterparts are only 1.5' apart, and the two profiles cannot be fully separated
J1000-58B J1000-58A and J1000-58B The two counterparts are only 1.5' apart, and the two profiles cannot be fully separated
J1004-58  The profile shows a prominent horn that, according to the data cube, could be caused by two close-by double-horn profiles separated in both R.A. and decl. (10:04:34,-58:31:10 and 10:04:04,-58:39:15, respectively). There are two NIR-bright candidates in these positions, which are likely counterparts. This is supported by that fact that the distances between HI position and the two counterparts (d_sep_=4.8' and d_sep_=4.2') are large for an S/N of 36; see also Figure 4
J1024-52  The candidate seems to be a galaxy pair (possibly interacting since it is an IRAS source). 2MASXJ10240866-5159040 is slightly rounder and of earlier type than RKK 2457, and it is not quite clear whether only one of them or both contribute to the signal
J1058-66  This is a confused profile. the HIPASS detection J1059-66 lies farther south and shows a broad double-horn profile clearly caused by ESO 093-G003 with an optical measurement of v=1470+/-270km/s (Fairall 1980MNRAS.192..389F). Our HI detection could not be separated from this because the ESO galaxy lies beyond the edge of the cube and was therefore not properly detected
J1149-64  There is a large spiral with a smaller companion visible in the NIR. It is likely that the companion contributes to the profile
J1214-58  There are two galaxies in the field, possibly companions. WKK 0788 is edge-on and seems to match the profile slightly better than the later type WKK 0782. There is no indication of confusion
J1222-57  Schroder et al. 2009 (cat. J/A+A/505/1049) have detected this galaxy in the OFF beam and associated it with WKK 0969 (which lies d_sep_=10.2'2 to the southeast of our detection) as the only known galaxy in the area, while at d_sep_=6.2' we find a galaxy that is not listed in the literature as the more likely counterpart
J1234-61  There are two galaxies visible, possibly a galaxy pair. They have similar appearance except that the galaxy at (R.A.,decl.)=(12:33:47.8,-61:29:57) appears more face-on. The profile appears to be confused, and it is likely that both galaxies are detected
J1304-58  The distance of 5.6' to the cross-match is large, but the HI detection is near the edge of the cube and the S/N is low. The galaxy is well visible in the B band. The other candidates in the field do not agree as well with the profile
J1310-57  There are two bright galaxies (E and S) in the field and several smaller ones, possibly a group of galaxies
J1314-58  This is a strong signal with a lopsided double horn. There are two galaxies in the field: WKK 2020 is more edge-on and a later spiral than 2MASXJ13150989-5856116, which has an optical velocity of v=2355+/-50km/s (Fairall 1998lssu.conf.....F). They are likely to form a pair with both contributing to the signal. This is supported by the fact that the distance to each of the galaxies (d_sep_=2.5' and d_sep_=3.0', respectively) is unusually high for the S/N of 96 of the HI detection: the median S/N of cross-matches with distances between 2.0 and 3.0 is 9.8 with a sigma of 7.2; hence, this is a 12{sigma} deviation. In addition, the HI position lies just between these two galaxies
J1329-61  There is a possible galaxy visible in the NIR at (R.A.,decl.)=(13:30:01.0,-61:51:44) with a distance of 1.2' to the HI position, which matches the profile well
J1337-58B There are three spiral galaxies in the field, two of which are of similar size and possibly form a pair. 2MASXJ13372458-5852216 is fairly edge-on and of earlier morphological type than 2MASXJ13373282-5854136, which has an optical velocity of v=3709+/-70km/s (Visvanathan & Yamada 1996 (cat. J/ApJS/107/521)). It seems likely that both galaxies contribute to the profile (see, for example, the profile given in Schroder et al. 2009 (cat. J/A+A/505/1049) for WKK 2390 = 2MASXJ13372458-5852216)
J1344-65  The counterpart, WKK 2503, was also observed and detected by Schroder et al. 2009 (cat. J/A+A/505/1049). Their profile, with a higher velocity resolution, is clearly confused, that is, the peak at 2750-2950km/s seems to belong to a second galaxy that is visible neither in the optical nor in the NIR
J1353-58  This HI detection seems to be a companion of the Circinus galaxy (J1413-65). We have adopted the same distance to calculate the HI mass
J1405-65  There are two LSB galaxies in the field. The fainter and rounder seems to fit the profile better. The cube shows a possible faint HI detection under the detection limit at v~3400km/s and with a larger line width, which could be the other, more edge-on, galaxy in the field (WKK 2924). WKK 2924 was also observed by Schroder et al. 2009 (cat. J/A+A/505/1049), where both detections were noted. While the detection at 3410km/s was attributed to WKK 2924 (as we do), the detection at 2864km/s was attributed to WKK 2938, which lies to the south at d_sep_=7.2'. However, the position and flux of our HI detection rule out WKK 2938 as a counterpart
J1406-57  There is a galaxy pair in the field. Their morphological types seem to be similar, and 2MASXJ14061018-5752098 is edge-on while 2MASXJ14062739- 5751425 is less inclined. It is likely that both contribute to the profile (the data cube seems to support a separation in R.A.)
J1413-65  This is the well-known Circinus galaxy. It is resolved with respect to the Parkes beam
J1416-58  This galaxy has the largest line width: W_50_=699+/-12km/s (and W_20_=730+/-18km/s). The NIR images show a perfect edge-on galaxy with a clear bulge
J1424-60  There is a possible galaxy visible in the NIR at (R.A.,decl.)=(14:25:10.3,-60:05:49) with a distance of 2.5' to the HI position, which matches the profile well. However, owing to the high extinction and faintness of the object, we cannot say for certain that this is a galaxy
J1435-61  There are several galaxies visible on the VISTA image. Owing to the high extinction (A_B_=26.6^m^), only the bulges are clearly visible, and it is not possible to compare sizes and morphological types. We have chosen the largest as the most likely counterpart, which is also red on WISE
J1448-54  The HI detection is a nearby dwarf galaxy (D=11.5Mpc). The candidate appears very small, but with an extinction of A_B_=3.3^m^ a large LSB halo is possible
J1452-56  The cross-match is a very edge-on late-type spiral galaxy. It seems to have a companion to the north that is less inclined but of similar morphological type. According to the data cube, it is likely that both contribute to the profile
J1501-57  There is a galaxy pair in the field, both very similar-looking inclined medium-type spirals. The profile, however, implies a galaxy with little inclination. A closer inspection of the data cube reveals a broader profile under the detection limit, similar to J1004-58. On the other hand, the extinction in this region is fairly high (A_B_=10.5^m^) and varies across the field (which is most prominent in the I band). Therefore, either the cross-match is an invisible face-on/late-type galaxy, or we have detected a lopsided horn of one of the galaxies in the pair (note that the baseline is very variable here)
J1504-55  There is a possible galaxy visible in the NIR at (R.A.,decl.)=(15:04:24.3,-55:29:09) with a distance of 1.2' to the HI position. It lies between stars, and this cannot be unambiguously identified as a galaxy
J1509-52  This HI detection is resolved with respect to the Parkes beam
J1513-54  This is a close galaxy pair, possibly interacting (IRAS source). The larger component is listed here
J1514-52  This HI detection is resolved with respect to the Parkes beam
J1530-54  There is a possible galaxy visible in the NIR at (R.A.,decl.)=(15:31:00.5,-54:03:37) with a distance of 0.2 to the HI position, which matches the profile well
J1530-59  The cross-match is a close galaxy pair, possibly interacting (IRAS source). It is not possible to tell whether one or both contribute to the profile
J1532-56  This galaxy is extended and has been observed with the Australia Telescope Compact Array by Staveley-Smith et al. (1998AJ....116.2717S) with a positional accuracy of 15'' (NED). At an extinction of A_B_=57^m^ nothing is visible at this position
J1549-60  There are three galaxies in the field. The counterpart seems slightly larger in the B band, as well as with WISE, than WKK 5337 and the third galaxy at (R.A.,decl.)=(15:49:39.6,-60:15:24)
J1550-58  Schroder et al. 2009 (cat. J/A+A/505/1049) observed WKK 5366 (at d_sep_=4.9) with almost the same flux. We have excluded WKK 5366 as a counterpart since it has an optical velocity of 4822+/-82km/s (Woudt et al. 2004, cat. J/A+A/415/9), and the distance is fairly large for such a bright detection
J1553-50  Despite the high extinction (A_B_=9.2^m^), several small galaxies of similar appearance can be seen, possibly forming a group. We have chosen the largest with obvious bulge and disk as the probable counterpart
J1553-49  J1553-49 and J1554-50 This is an area of complex emission that cannot easily be disentangled. The data cube shows also some fainter emission below our detection limit. While the cross-match for J1554-50 is a nearly edge-on galaxy with no other galaxy visible within a 5' radius, for J1553-49 there are four galaxies visible in the NIR (two of which are unknown). The largest, 2MASXJ15534458-5000182, seems to be an early-type galaxy and is an unlikely candidate. The galaxy at (R.A.,decl.)=(15:54:01.1,-49:54:06) shows a diffuse halo and a small bulge and seems to be the most likely candidate. It is also bright in the WISE bands W3 and W4. A candidate for possible confusion could be 2MASXJ15534427-5002132 at 4.8 from the HI position
J1554-50  J1553-49 and J1554-50 This is an area of complex emission that cannot easily be disentangled. The data cube shows also some fainter emission below our detection limit. While the cross-match for J1554-50 is a nearly edge-on galaxy with no other galaxy visible within a 5' radius, for J1553-49 there are four galaxies visible in the NIR (two of which are unknown). The largest, 2MASXJ15534458-5000182, seems to be an early-type galaxy and is an unlikely candidate. The galaxy at (R.A.,decl.)=(15:54:01.1,-49:54:06) shows a diffuse halo and a small bulge and seems to be the most likely candidate. It is also bright in the WISE bands W3 and W4. A candidate for possible confusion could be 2MASXJ15534427-5002132 at 4.8 from the HI position
J1553-61  Schroder et al. 2009 (cat. J/A+A/505/1049) observed WKK 5430, which is 5.3' to the north of our position. Their detection is lopsided and has less flux than ours, which rules out WKK 5430 as the counterpart. In addition, the HIPASS position (R.A.,decl.)=(15:53:43.5,-61:13:34) favors WKK 5447
J1557-50A J1557-50A and J1557-50B These two HI detections are 6.5 apart, and the two profiles are slightly confused. The extinction is fairly high (A_B_~17^m^), and a hidden galaxy cannot be excluded
J1557-50B J1557-50A and J1557-50B These two HI detections are 6.5 apart, and the two profiles are slightly confused. The extinction is fairly high (A_B_~17^m^), and a hidden galaxy cannot be excluded
J1603-49  There are two candidates, both nearly edge-on. They are of similar size, possibly a galaxy pair. The candidate at (R.A.,decl.)=(16:03:34.6,-49:51:16) is slightly larger with a larger bulge (it is also brighter on WISE)
J1612-56  The detection of WKK 6219 by Schroder et al. 2009 (cat. J/A+A/505/1049) seems to be the low-velocity horn of J1612-56
J1616-48A J1616-48A and J1616-48B These two HI detections are 2.0' apart, and the profiles are confused
J1616-48B J1616-48A and J1616-48B These two HI detections are 2.0' apart, and the profiles are confused
J1616-55  There are ATCA observations on this HI detection (Staveley-Smith et al. 1998AJ....116.2717S), which shows that the HI is extended and has two bright components about 25' apart. There is no counterpart visible in the optical or NIR despite a moderate extinction (A_B_=2.7^m^) indicating that the counterpart is likely to have a low surface brightness. Owing to its extent, the coordinates given in previous publications, Henning et al. (2000AJ....119.2686H) and Juraszek et al. (2000AJ....119.1627J), are 11.2' and 10.3' east of our position, while the exact position given in Staveley-Smith et al. (1998AJ....116.2717S) is only 5.0' (west) from our position
J1622-44A There is a possible galaxy visible in the NIR at (R.A.,decl.)=(16:22:05.2,-44:22:36) with a distance of 1.5' to the HI position, which matches the profile well. It lies next to a bright star, which makes the identification uncertain
J1625-42  The spectrum also shows J1624-42 at the lower velocities. It appears that the profiles overlap and the line widths and flux measurement are uncertain
J1625-55  The cross-match is a galaxy pair: 2MASXJ16253644-5533498 is bright and nearly edge-on (wide profile), while WKK 6819 is a late-type spiral (narrow profile)
J1633-44  There are two similar-looking small galaxies visible in the NIR, possibly a galaxy pair. The HI detection is too faint to tell whether one or both galaxies contribute to the profile
J1648-49  The HI cross-match seems to be a galaxy pair of similar appearance where both are likely to contribute
J1651-40  There is a possible galaxy visible in the NIR at (R.A.,decl.)=(16:51:53.2,-40:48:03) with a distance of 1.1' to the HI position. WISE shows also a faint reddish patch, though there is a possibility that it is Galactic
J1653-44  This galaxy is only visible with WISE and could be also a background galaxy
J1653-48  There is a possible galaxy visible in the NIR at (R.A.,decl.)=(16:53:21.1,-48:01:53) with a distance of 2.5' to the HI position, which matches the profile well
J1705-40  WISE shows a bright red extended emission at (R.A.,decl.)=(17:05:04.8,-40:58:08) with a distance of 1.3' to the HI position. According to the WISE colors, it could be either a starburst galaxy or an HII region (Jarrett et al. 2011ApJ...735..112J)
J1716-42  The only visible candidate seems too small for this distance, though a larger LSB halo cannot be excluded
J1716-35  There are two galaxies visible in the NIR. The edge-on galaxy at (R.A.,decl.)=(17:16:35.5,-35:57:26) does not match the profile as well as the less inclined galaxy at (17:16:51.8,-35:55:48)
J1719-37  This galaxy is only visible with WISE and could also be a background galaxy
J1811-21  J1811-21 and J1812-21 Both spectra show emission of the other galaxy as well
J1812-21  J1811-21 and J1812-21 Both spectra show emission of the other galaxy as well
J1821-06  The only candidate appears too small for a velocity of v=1788km/s and logM_HI_=8.8 even taking the extinction of A_B_=6.1^m^ into account, but a very LSB halo cannot be excluded
J1824-20  This galaxy was found on WISE images and is faintly visible on the IRSF images
J1825-07  There are four galaxies visible in the NIR, two of which are NVSS sources and one is an AGN with an optical velocity of v=10887km/s (Burenin et al. 2009AstL...35...71B). We assume the cross-match to be the most inclined. It is possible that all galaxies belong to a group or cluster
J1846-07B J1846-07B and J1846-07A These two HI detections are only 2.2' apart but well separated in velocity. There are two candidates visible in the NIR: both are very inclined, and the larger is assumed to be the cross-match for J1846-07A, while the cross-match for J1846-07B is smaller and seems to be of later morphological type
J1846-07A J1846-07B and J1846-07A These two HI detections are only 2.2' apart but well separated in velocity. There are two candidates visible in the NIR: both are very inclined, and the larger is assumed to be the cross-match for J1846-07A, while the cross-match for J1846-07B is smaller and seems to be of later morphological type
J1847+04  This galaxy lies at a Galactic latitude of l=36.06{deg} and belongs technically to the northern extension of HIZOA (Donley et al. 2005, cat. J/AJ/129/220)
J1855-03B There is a possible galaxy faintly visible in the NIR at (R.A.,decl.)=(18:56:00.5,-03:12:21) with a distance of 0.3' to the HI position. It is large and diffuse and, if real, matches the profile well
J1858+00  The profile could be confused or come from a disturbed HI distribution. The extinction is high (A_B_=12.2^m^), and only one candidate could be found on the images. No halo is visible, and a hidden galaxy cannot be excluded