EZOA J1856-03 There is a possible galaxy faintly visible in deep NIR EZOA J1856-03 images at (RA,Dec) =(18:56:00.5,-03:12:21) at a distance of 2.2' from the EZOA J1856-03 EZOA position. Its large and diffuse appearance matches the profile EZOA J1856-03 well. The NRT observation of this position shows an improved profile with EZOA J1856-03 even peaks and a high flux ratio of 1.2, which seems to confirm this EZOA J1856-03 candidate. EZOA J1921+14 The possible cross-match candidate has been confirmed. EZOA J2001+26 There are three galaxies in the field, one of which (2MASX EZOA J2001+26 J20010969+2655338) was observed by Kraan-Korteweg et al. 2018 = EZOA J2001+26 2018MNRAS.481.1262K with the NRT but not detected. We observed now the EZOA J2001+26 other two and can confirm the one closer to the EZOA position (pointing A) EZOA J2001+26 as the cross-match. EZOA J2102+46 The possible cross-match candidate has been confirmed. EZOA J2125+48 There is no cross-match for this marginal (SNR=5.2) EZOA EZOA J2125+48 detection. We observed it with four pointings. We have possible detections EZOA J2125+48 at RA = 21:25:36.9 (pointing A) and RA = 21:25:16.0 (pointing D), albeit EZOA J2125+48 with less than the expected flux and showing only the lower velocity EZOA J2125+48 horn. However, the baseline of all observations is affected by GPS EZOA J2125+48 residuals, the rms is high (between 4 and 7) and the SNR is low (around EZOA J2125+48 3). Ideally we need more observations to improve the SNRs, but for the time EZOA J2125+48 being we assume that the detection is only a possible one and might not be EZOA J2125+48 real. EZOA J2131+43 We observed the most likely cross-match (pointing A) and EZOA J2131+43 obtained a clearly confused profile, about twice as wide as the EBHIS EZOA J2131+43 profile. To the south, at a distance of 3.1' from the EZOA position (and EZOA J2131+43 0.6b from our pointing A), is a tight group of galaxies (2MASX EZOA J2131+43 J21312321+4336182) that was observed by Paturel et al. 2003 = EZOA J2131+43 2003A%26A...412...57P, listed in our table as pointing B (footnote: It was EZOA J2131+43 also observed by Masters et al. 2014 = 2014MNRAS.443.1044M, but we prefer a EZOA J2131+43 direct comparison of two NRT detections because of the NRT's unusual beam EZOA J2131+43 form.). The flux at pointing A is marginally higher than at pointing B, and EZOA J2131+43 also pointing A's peak flux is about 10 mJy higher. We conclude that EZOA J2131+43 most of the EZOA detection comes from our cross-match at (RA,Dec) = EZOA J2131+43 (21:31:17.9,+43:39:03). 2MASX J21312321+4336182 likely contributes, and its EZOA J2131+43 low-velocity part is, in fact, visible in the EBHIS spectrum, though it is EZOA J2131+43 strongly affected by baseline variations. EZOA J2216+50 We observed both the cross-match position (pointing A) and EZOA J2216+50 the EZOA position (pointing B). Both are affected by RFI. We could confirm EZOA J2216+50 the cross-match, but the measured flux is unreliable due to insufficient EZOA J2216+50 RFI subtraction. Pointing B was also observed with the WIBAR receiver to EZOA J2216+50 test the RFI mitigation software, resulting in a clearer profile EZOA J2216+50 (Sect. 5.3). However, the pointing is 1.0b from the cross-match position, EZOA J2216+50 resulting in a flux ratio of 0.4 as compared to the uncertain flux ratio of EZOA J2216+50 0.7 found for pointing A. EZOA J2230+51 This possible EZOA detection was not detected in the EZOA J2230+51 pointings towards two possible cross-match candidates. However, we have a EZOA J2230+51 serendipitous detection at v = 5806 km/s , which is like due to the EZOA J2230+51 targeted cross-match candidate (pointing A). EZOA J2237+53 The cross-match is a galaxy pair (2MASX J22370662+5357049 is EZOA J2237+53 nearly edge on, while 2MASX J22370933+5358339 is fairly inclined), both of EZOA J2237+53 which contribute to the HI detection. We observed the former, while the EZOA J2237+53 latter (at 0.25b) was observed previously both with the NRT (Paturel et EZOA J2237+53 al. 2003 = 2003A%26A...412...57P) and the Green Bank 300-foot telescope EZOA J2237+53 (GBT; Courtois et al. 2009 = 2009AJ....138.1938C); we have added them to EZOA J2237+53 our table for comparison. Our NRT observation shows a clear peak at v < EZOA J2237+53 5100 km/s, which is not obvious in the EBHIS profile. Comparing the two EZOA J2237+53 NRT profiles we can tell by the relative peak heights that the profile at EZOA J2237+53 5100 < v < 5400 km/s comes from J22370662+5357049, while J22370933+5358339 EZOA J2237+53 covers 5200 < v < 5550 km/s. Thus the EZOA detection comes mainly from EZOA J2237+53 J22370933+5358339. Note that Paturel et al. 2003 = 2003A%26A...412...57P EZOA J2237+53 only measure the profile from v > 5200 km/s (same as the EBHIS profile), EZOA J2237+53 while Courtois et al. 2009 = 2009AJ....138.1938C give parameters for the EZOA J2237+53 full profile. EZOA J2329+61 There is no obvious cross-match for this detection. We EZOA J2329+61 observed the EZOA position (pointing A) as well as positions about 1b EZOA J2329+61 (~1.8') to the west (pointing B) and east (pointing C), respectively, to EZOA J2329+61 cover the EBHIS positional uncertainty area. Only pointing A at the EZOA EZOA J2329+61 position shows a marginal detection, confirming the EZOA detection, but EZOA J2329+61 with a much lower flux (note, though, that the EBHIS profile has a low SNR EZOA J2329+61 of 4.8). The cross-match is likely found north or south of the EZOA EZOA J2329+61 position at a larger distance. EZOA J0041+57 The NRT spectrum looks like a bona fide detection at v = EZOA J0041+57 9547 km/s, but it lies within a velocity range where RFI occurs frequently. EZOA J0041+57 Simultaneous observation with the WIBAR receiver and subsequent RFI EZOA J0041+57 mitigation shows that the apparent profile is entirely due to RFI (see EZOA J0041+57 Sect. 5.3). EZOA J0112+63 We observed this marginal EZOA detection, which that has no EZOA J0112+63 cross-match, with three pointings, covering the EBHIS positional EZOA J0112+63 uncertainty area. The profile is marginal at pointing A and stronger at EZOA J0112+63 pointing B though the flux is still lower than the EBHIS value (~50%). The EZOA J0112+63 profile shape appears less lopsided than in the EBHIS detection, which EZOA J0112+63 agrees with the cross-match lying closer to position B. We decided to EZOA J0112+63 re-investigate NIR images of this area and found that at (RA,Dec) = EZOA J0112+63 (01:12:12.0,+63:57:14) the DSS2-I and 2MASS-K band images show a diffuse EZOA J0112+63 patch which could be a low surface brightness galaxy (this agrees with the EZOA J0112+63 high extinction of AK = 0.6). Pan-STARRS1 images confirm this to be a EZOA J0112+63 galaxy. It is 0.8b west of pointing B, which agrees with the measured flux EZOA J0112+63 ratio of 0.5. EZOA J0112+63 Pointing A also shows a serendipitous detection at v = 7503 km/s, for which EZOA J0112+63 no cross-match is visible either. EZOA J0125+64 There is no cross-match for this detection. Our detection EZOA J0125+64 at the EZOA position has about half the EBHIS flux (~50%). We conclude that EZOA J0125+64 the cross-match lies either east or west near the edge of the NRT beam. EZOA J0141+63 Without a possible cross-match we observed the EZOA position EZOA J0141+63 for this possible EBHIS detection. We detect a marginal profile, albeit EZOA J0141+63 with a ~30% lower flux. We also tried to observe a galaxy visible with WISE EZOA J0141+63 (pointing B) but the observation failed. Due to the low NRT flux (though EZOA J0141+63 both detections have a low SNR), we expect that the cross-match is likely EZOA J0141+63 nearer the edges of the NRT and EBHIS beams (more likely in the east-west EZOA J0141+63 direction). EZOA J0147+63 There is no obvious cross-match for this detection. We EZOA J0147+63 observed the EZOA position (pointing A) as well as a position at RA = EZOA J0147+63 01:47:33 about 1.4b to the east (pointing B). Further southeast, 5.1' (or EZOA J0147+63 2.4b) away, lies 2MASX J01474890+6305128, which was previously observed and EZOA J0147+63 detected by us (see Kraan-Korteweg et al. 2018 = 2018MNRAS.481.1262K) and EZOA J0147+63 is listed as pointing C in Table B.1 for convenience. All three EZOA J0147+63 observations show a detection, albeit with varying profile shapes. We EZOA J0147+63 conclude that the EBHIS detection is likely a confused profile with an EZOA J0147+63 invisible galaxy close to the EZOA position as the main contributor and EZOA J0147+63 2MASX J01474890+6305128 as the confusing partner (contributing mainly at EZOA J0147+63 the high velocity end of the profile). EZOA J0147+63 We also found a serendipitous detection at v = 7515 km/s in pointing A, but EZOA J0147+63 no candidate for it. EZOA J0213+66 Schroeder et al. 2019 = 2019MNRAS.489.2907S reported two EZOA J0213+66 galaxies in the field without being able to tell which could be the EZOA J0213+66 cross-match. We observed both and find that the galaxy at (RA,Dec) EZOA J0213+66 =(02:13:11.5,+66:12:28) (pointing B) is the cross-match. We have also EZOA J0213+66 detected the other galaxy at (RA,Dec) =(02:13:33.4,+66:10:39) as a weak, EZOA J0213+66 low-velocity shoulder at v >~ 4020 km/s, which is not visible in the EBHIS EZOA J0213+66 spectrum. This indicates that the two galaxies could form a pair. EZOA J0233+58 We confirm the cross-match with 2MASX J02333595+5836438 but EZOA J0233+58 also report emission at the high-velocity end of the profile, v <~ 4720 EZOA J0233+58 km/s, which is not visible in the EBHIS spectrum. It may come from a EZOA J0233+58 companion galaxy, 2MASX J02334017+5836388. EZOA J0252+62 As the cross-match 2MASX J02520392+6235505 lies at a large EZOA J0252+62 distance from the EZOA position (4.0' north), it is likely that another EZOA J0252+62 galaxy contributes to the profile. We observed both the cross-match and a EZOA J0252+62 galaxy about 0.9b to the South of it (and 4.4' south of the EZOA position), EZOA J0252+62 visible on DSS and WISE images. For comparison, we also observed the EZOA EZOA J0252+62 position (pointing C). We find that at both galaxy positions the flux is EZOA J0252+62 slightly higher than at the EZOA position. We conclude that both EZOA J0252+62 cross-matches contribute to the EBHIS detection. EZOA J0253+55 The NRT/EBHIS flux ratio at the probable cross-match EZOA J0253+55 candidate position (pointing A) is low at 0.5, though it should be noted EZOA J0253+55 that the EBHIS profile is noisy with an rms of 14 mJy. When we observed the EZOA J0253+55 EZOA position (pointing B), we found an even lower flux ratio of 0.3. This EZOA J0253+55 indicates that the cross-match is either the observed candidate or an EZOA J0253+55 invisible galaxy close to it. EZOA J0253+55 Furthermore, a galaxy pair at ~4.4' from the EZOA position had been EZOA J0253+55 observed previously by us with the NRT (Kraan-Korteweg et al. 2018 = EZOA J0253+55 2018MNRAS.481.1262K): 2MASX J02531475+5528143 and 2MASX J02531969+5529140 EZOA J0253+55 are also listed in the table as pointing C and D, respectively. The pair EZOA J0253+55 was detected at v = 4462 km/s and 4337 km/s, respectively, with fluxes too EZOA J0253+55 low for detection in the EBHIS survey (though the former is also visible in EZOA J0253+55 our spectrum of pointing A). However, both observations also show the EZOA EZOA J0253+55 detection at v = 3809 km/s albeit at a lower flux. Kraan-Korteweg et EZOA J0253+55 al. 2018 = 2018MNRAS.481.1262K also observed a third, uncatalogued galaxy EZOA J0253+55 further north (pointing E). The separations between the EZOA cross-match EZOA J0253+55 candidate and these three galaxies are 1.0b, 1.4b and 1.1b, respectively, EZOA J0253+55 and all three show only the higher velocity peak at v ~ 3820 km/s, while EZOA J0253+55 our observation of the candidate shows a narrow double horn with a second EZOA J0253+55 (slightly higher) peak at v ~ 3700 km/s, which, in turn, is the main peak EZOA J0253+55 in pointing B. EZOA J0253+55 We conclude that the cross-match has a large (resolved) HI disc, whose EZOA J0253+55 lower-velocity end lies close to the EZOA position while the high-velocity EZOA J0253+55 end points towards the galaxy pair. This would also explain the overall EZOA J0253+55 lower fluxes measured at the NRT. EZOA J0308+64 This EZOA detection is of a local dwarf galaxy (at a EZOA J0308+64 distance of 9.8 Mpc; Schroeder et al. 2019 = 2019MNRAS.489.2907S) without a EZOA J0308+64 stellar counterpart listed. We observed the EZOA position and detected a EZOA J0308+64 strong signal at a slightly lower flux (70%). The fact that the NRT profile EZOA J0308+64 shows two peaks of equal height indicates that the galaxy must lie well EZOA J0308+64 within the telescope beam. We subsequently searched Pan-STARRS1 images and EZOA J0308+64 found a diffuse galaxy only 0.25' from the EZOA position, which, indeed, is EZOA J0308+64 also visible (though not recognisable as a galaxy) on DSS2-R, at (RA,Dec) = EZOA J0308+64 (03:08:27.3,+64:59:37). EZOA J0314+64 Since the EZOA detection is located at the edge of the EBHIS EZOA J0314+64 cube, its profile is noisy and its position and HI parameters are EZOA J0314+64 uncertain. Our observation of the cross-match 2MASX J03151297+6452348 shows EZOA J0314+64 a profile which is ~80 km/s wider than could be estimated from the noisy EZOA J0314+64 EBHIS profile. EZOA J0324+60 The search for a cross-match revealed a diffuse patch on the EZOA J0324+60 DSS2-R image that could be a late-type dwarf galaxy but was too uncertain EZOA J0324+60 to be listed as cross-match in Schroeder et al. 2019 = EZOA J0324+60 2019MNRAS.489.2907S. We observed this position with a flux ratio of EZOA J0324+60 0.7. Though the flux is slightly lower than expected, we can confirm the EZOA J0324+60 cross-match since we also noted an elongated, diffuse LSB galaxy on EZOA J0324+60 Pan-STARRS1 images. At a distance of 18.3 Mpc we can assume that the HI EZOA J0324+60 disc is resolved by the NRT beam, which explains the lower flux. EZOA J0328+53 and EZOA J0328+53B: EZOA J0328+53 (v = 8538 km/s) is a noisy EZOA J0328+53 EBHIS detection with a double horned profile, and EZOA J0328+53B (v = 11952 EZOA J0328+53 km/s) is a possible single-peak detection. The two detections are separated EZOA J0328+53 by ~1.9'. There is one possible cross-match candidate visible to the south EZOA J0328+53 (at 1.1b and 0.5b from the two EZOA source positions, respectively), which EZOA J0328+53 we observed (both pointings A) along with the EZOA J0328+53 position EZOA J0328+53 (pointings B). Pointing A is affected by RFI in the velocity range 8500 - EZOA J0328+53 9500 km/s and is therefore inconclusive regarding the EZOA J0328+53 EZOA J0328+53 detection, while EZOA J0328+53B is clearly not detected. Pointing B shows EZOA J0328+53 baseline variations in the range 8000 - 9000 km/s and no recognisable HI EZOA J0328+53 profile, nor does it show a detection for EZOA J0328+53B. EZOA J0328+53B and EZOA J0328+53: EZOA J0328+53 (v = 8538 km/s) is a noisy EZOA J0328+53B EBHIS detection with a double horned profile, and EZOA J0328+53B (v = 11952 EZOA J0328+53B km/s) is a possible single-peak detection. The two detections are separated EZOA J0328+53B by ~1.9'. There is one possible cross-match candidate visible to the south EZOA J0328+53B (at 1.1b and 0.5b from the two EZOA source positions, respectively), which EZOA J0328+53B we observed (both pointings A) along with the EZOA J0328+53 position EZOA J0328+53B (pointings B). Pointing A is affected by RFI in the velocity range 8500 - EZOA J0328+53B 9500 km/s and is therefore inconclusive regarding the EZOA J0328+53 EZOA J0328+53B detection, while EZOA J0328+53B is clearly not detected. Pointing B shows EZOA J0328+53B baseline variations in the range 8000 - 9000 km/s and no recognisable HI EZOA J0328+53B profile, nor does it show a detection for EZOA J0328+53B. EZOA J0332+58 Schroeder et al. 2019 = 2019MNRAS.489.2907S mention a EZOA J0332+58 possible galaxy at (RA,Dec) = (03:32:48.4,+58:14:55), which could be the EZOA J0332+58 cross-match. Our observation of this position (pointing A) shows a EZOA J0332+58 detection, but with too low a flux (60%). We also observed the EZOA EZOA J0332+58 position (pointing B), which shows a much stronger profile. The NRT/EBHIS EZOA J0332+58 flux ratio at pointing B is 0.9, indicating that the actual cross-match is EZOA J0332+58 very close to the B position. We thus give a new positional uncertainty for EZOA J0332+58 the EZOA detection with 0.2' in RA and 1.4' in Dec (referring to the inner EZOA J0332+58 ten percent of the NRT beam). EZOA J0349+53 This marginal, single-peak EZOA detection is confirmed EZOA J0349+53 (pointing A) with an NRT/EBHIS flux ratio of 0.5, which implies that the EZOA J0349+53 cross-match lies near the edge of the NRT beam in the east-west direction. EZOA J0358+47 The NRT profile at the position of the cross-match ZOAG EZOA J0358+47 G152.52-04.48 shows a sloped high-velocity shoulder (at v <~ 5700 km/s). To EZOA J0358+47 check if this could be due to confusion, we also observed a galaxy at 0.4b. EZOA J0358+47 This profile, though, shows both a lower shoulder and a lower total flux, EZOA J0358+47 and we therefore exclude confusion. EZOA J0431+45 Though this was considered a firm, although weak and noisy, EZOA J0431+45 detection by Schroeder et al. 2019 = 2019MNRAS.489.2907S, we could not EZOA J0431+45 confirm it with three pointings covering the EBHIS positional uncertainty EZOA J0431+45 area. EZOA J0433+39 We observed the cross-match of this possible EZOA source, EZOA J0433+39 3.0' from the EZOA position. We detect a strong double horn profile with EZOA J0433+39 equal peaks but with a lower flux (60%). The very noisy EBHIS profile is EZOA J0433+39 about twice as wide as the NRT profile but seems to include a noise peak, EZOA J0433+39 which would explain the lower flux in our NRT detection. EZOA J0437+43 Schroeder et al. 2019 = 2019MNRAS.489.2907S give a galaxy EZOA J0437+43 pair as cross-match. We observed the northern component (2MASX EZOA J0437+43 J04370228+4356359; pointing A) but were not able to observe the eastern one EZOA J0437+43 (2MASX J04370607+4355349, a more inclined, earlier type spiral). The two EZOA J0437+43 galaxies are only 0.4b apart. The NRT profile looks clearly confused and EZOA J0437+43 wider than the EBHIS profile, which is quite noisy and, basically, shows EZOA J0437+43 only the two highest peaks. The galaxy was also observed by Springob et EZOA J0437+43 al. 2005 = 2005ApJS..160..149S with the GBT. Their profile is heavily EZOA J0437+43 smoothed and shows few features, but it is obvious that is shows emission EZOA J0437+43 at higher velocities than our NRT profile (at v <~ 4100 km/s). Since the EZOA J0437+43 east-west GBT HPBW is larger than the NRT's by a factor of about three, we EZOA J0437+43 assume that they have detected more flux from the companion galaxy, whose EZOA J0437+43 disc is oriented in an east-west direction, and that the NRT beam therefore EZOA J0437+43 would not see all of it. We conclude that both galaxies are detected, with EZOA J0437+43 the emission at the higher velocity end of the profile coming from 2MASX EZOA J0437+43 J04370607+4355349. EZOA J0437+54 We observed a pair of galaxies: 2MASX J04373506+5414339 EZOA J0437+54 (pointing A) is fairly face-on, at v(opt) = 5369 km/s (Huchra et al. 2012 = EZOA J0437+54 2012ApJS..199...26H) and is considered the probable EZOA cross-match, while EZOA J0437+54 2MASX J04374087+5415389 (pointing B) is almost edge-on, at v(opt) = 5653 EZOA J0437+54 km/s (Huchra et al. 2012 = 2012ApJS..199...26H). Our NRT observations show EZOA J0437+54 an overall stronger profile for the former, while the profile of pointing B EZOA J0437+54 is weaker and seems to have a high-velocity shoulder. We conclude that both EZOA J0437+54 galaxies are detected but only 2MASX J04373506+5414339 contributes to the EZOA J0437+54 noisy EBHIS profile. EZOA J0438+44 Schroeder et al. 2019 = 2019MNRAS.489.2907S noted the EZOA J0438+44 close-by galaxy UGC 3108 at d = 4.4' from the EZOA position but excluded EZOA J0438+44 its contribution to the signal. We observed the adopted cross-match 2MASX EZOA J0438+44 J04381402+4407596 (1.5b from UGC 3108) and confirm the EZOA detection. UGC EZOA J0438+44 3108 was observed by Springob et al. 2005 = 2005ApJS..160..149S with the EZOA J0438+44 GBT, where it shows a wider profile starting at v < 3800 km/s (listed in EZOA J0438+44 our table as pointing B). The GBT profile shows our detection as a EZOA J0438+44 pronounced high velocity horn at v = 4000 - 4100 km/s. Although we cannot EZOA J0438+44 exclude that the EBHIS and NRT observations both see part of the HI disc of EZOA J0438+44 UGC 3108, the contribution from our cross-match is clearly dominating. EZOA J0446+44 We observed the EZOA position since there is no EZOA J0446+44 cross-match. The detected signal shows an NRT/EZOA flux ratio of 1.1 and EZOA J0446+44 the profile shows symmetric peaks. We conclude that the cross-match is well EZOA J0446+44 within the NRT beam, that is, very close to the EZOA position. We thus give EZOA J0446+44 a new positional uncertainty for the EZOA detection with 0.2' in RA and EZOA J0446+44 1.3' in Dec (referring to the inner ten percent of the NRT beam). EZOA J0455+34 The possible cross-match candidate has been confirmed. EZOA J0457+39 The NRT observation at the position of this possible EZOA EZOA J0457+39 detection shows a 3 sigma detection with only 10% of the EBHIS flux EZOA J0457+39 recovered. The two pointings east and west of the EZOA position show no EZOA J0457+39 detection at all. It is possible that the cross-match lies further north or EZOA J0457+39 south (note, though, that the north-south NRT HPBW of 22' is twice that of EZOA J0457+39 EBHIS), or the detection may be spurious. More observations are needed to EZOA J0457+39 confirm this weak signal. EZOA J0546+31 Apart from the cross-match 2MASX J05462224+3155264, there EZOA J0546+31 are several smaller, uncatalogued, galaxies visible on the images, possibly EZOA J0546+31 forming a galaxy group. We observed the three most prominent ones and can EZOA J0546+31 confirm that 2MASX J05462224+3155264 (pointing A) is indeed the EZOA J0546+31 cross-match. We also detect at least one of the smaller ones (pointing C, EZOA J0546+31 with a prominent peak at v = 7600 km/s), and cannot exclude low level EZOA J0546+31 contamination of the NRT detections by one or more of the others. The EBHIS EZOA J0546+31 parameters are likely unaffected due to the lower sensitivity. EZOA J0548+19 The cross-match is a close galaxy pair, 2MASX EZOA J0548+19 J05485392+1911467. We observed the main component (pointing A, an inclined EZOA J0548+19 large spiral), which shows a clearly confused profile, possibly due to the EZOA J0548+19 smaller companion, an earlier type spiral at d = 0.25'. The EBHIS detection EZOA J0548+19 does not show confusion, but it is very weak, and the sloped low-velocity EZOA J0548+19 shoulder (v <~ 5700 km/s) seen with the NRT is likely lost in the EZOA J0548+19 noise. There is also a large galaxy far to the south-east (2MASX EZOA J0548+19 J05490625+1904314; at 1.6b), which we observed (pointing B) to exclude the EZOA J0548+19 possibility that the elongated NRT beam might have picked up emission from EZOA J0548+19 it. Although this spectrum shows a detection, it is too weak to account for EZOA J0548+19 the strong low-velocity shoulder visible in pointing A. Instead, this is EZOA J0548+19 likely an off-beam detection of our galaxy pair. EZOA J0636+00 Deep NIR images reveal the cross-match to be a galaxy EZOA J0636+00 triplet: pointing A targets 2MASX J06362668+0055433, which consists of an EZOA J0636+00 inclined spiral galaxy and a peculiar-looking companion (fragmented, or EZOA J0636+00 possibly a tight group of small -- or distant -- galaxies), while pointing EZOA J0636+00 B (0.8' to the west) 2MASX J06362361+0055513 appears more face-on. The EZOA J0636+00 observed HI fluxes are about the same. Since the two pointings are EZOA J0636+00 separated by 0.4b, we would expect a notable difference between the two EZOA J0636+00 fluxes if only one source were detected. We therefore conclude that both EZOA J0636+00 (or all three) galaxies are detected by both the NRT and EBHIS. EZOA J0649+09 The most likely cross-match is 2MASX J06493148+0939437 at a EZOA J0649+09 rather large distance of d 3.3' from the EZOA position. We observed this EZOA J0649+09 galaxy (pointing A), but the detection is dominated by a strong EZOA J0649+09 OFF-position detection (from about 20' east). Near that position lies UGC EZOA J0649+09 3565, which was detected by Springob et al. 2005 = 2005ApJS..160..149S with EZOA J0649+09 the Arecibo telescope in the velocity range ~7250 - 7600 km/s. This implies EZOA J0649+09 that half of our profile is affected by it, and only the NRT peak at v ~ EZOA J0649+09 7620 km/s lies just outside the profile of UGC 3565. We also observed four EZOA J0649+09 other galaxies in the area (see Fig. A.1). EZOA J0649+09 The peak at v ~ 7620 km/s is fainter for pointing C and appears of similar EZOA J0649+09 strength in pointings A and D (2MASX J06492673+0937525) though both are EZOA J0649+09 likely diminished (in different proportions) by the OFF-position EZOA J0649+09 profile. On the other hand, the two easterly pointings, B and E, are EZOA J0649+09 unaffected by the OFF-detection. They show detections in the range v = 7300 EZOA J0649+09 - 7600 km/s where the profile at v = 7500 - 7600 km/s is slightly stronger EZOA J0649+09 in pointing E and the emission at v = 7300 - 7500 km/s is likely due to the EZOA J0649+09 target of pointing B. EZOA J0649+09 We conclude that the galaxies at pointing B and E are both detected in the EZOA J0649+09 velocity range v = 7300 - 7600 km/s. Based on the spectra, we cannot EZOA J0649+09 distinguish whether one or both of the 2MASX galaxies has emission at v <~ EZOA J0649+09 7620 km/s. However, 2MASX J06493148+0939437 at pointing A is more likely to EZOA J0649+09 be a strong HI detection since it is closer to both the EZOA position and EZOA J0649+09 the nearby HIZOA detection (Donley et al. 2005 = 2005AJ....129..220D). The EZOA J0649+09 latter shows a likely confused profile with a peak at v ~ 7550 km/s, which EZOA J0649+09 we do not see in any of the NRT profiles due to the OFF-position detection. EZOA J0649+09 The galaxy at pointing C does not seem to have any emission in the velocity EZOA J0649+09 range. As to the EBHIS detection, it does not appear confused but the EZOA J0649+09 profile is noisy and its SNR of 5.4 is low. The EBHIS profile starts at v = EZOA J0649+09 7350 km/s, which means the galaxy at pointing B contributes only little, EZOA J0649+09 and most of the emission seems to come from 2MASX J06493148+0939437. EZOA J0652-03 This marginal EZOA detection could not be confirmed. The EZOA J0652-03 ATNF HIZOA data archive (https://www.atnf.csiro.au/research/multibeam/release) EZOA J0652-03 shows a similar peak, which contributed to its inclusion into the EZOA EZOA J0652-03 catalogue. However, none of the three NRT pointings show any indication of EZOA J0652-03 a detection (the peak flux density should be around 100 mJy): pointing A is EZOA J0652-03 the most likely cross-match, pointing B is the EZOA position, and pointing EZOA J0652-03 C was set at a search position between these two to form a continuous EZOA J0652-03 coverage of this area with the NRT beams. EZOA J0702-03 This detection was also found by Staveley-Smith et al. 2016 EZOA J0702-03 = 2016AJ....151...52S as HIZOA J0702-03B at (RA,Dec) = EZOA J0702-03 (07:02:34.5,-03:18:30), about 1.9' north of the EZOA position. There are EZOA J0702-03 two small cross-match candidates about 0.6b to the west. We observed the EZOA J0702-03 northern, more likely one (pointing A) as well as the EZOA position EZOA J0702-03 (pointing B). The flux ratio at pointing A is 0.9, as opposed to 0.6 at the EZOA J0702-03 EZOA position. We can thus confirm that the cross-match lies close to EZOA J0702-03 pointing A, though both candidates appear too small for a galaxy at a EZOA J0702-03 radial distance of ~32 Mpc and an HI mass of log(M(HI))/M(sun)) = 9.1. To EZOA J0702-03 note, there is a bright star close by, which could prevent us from seeing a EZOA J0702-03 possible LSB disk or from finding the cross-match.