Appendix B: Notes to Table 2

FGC 242 Our lower-velocity detection is likely due to a confusion with IC 200, $5\hbox{$.\mkern-4mu^\prime$ }1$ away at $V_{\rm h}=3846$ km s^-1 (RC3); our weak higher-velocity detection may be due to interference.

FGC 245 Our detection is likely a spurious feature due to recurrent bandpass structure (see Sect. 3.1.1).

FGC 284 Our apparent detection is likely due to a confusion with CGCG 462-006, at $V_{\rm h}=4100$ km s^-1 (Giovanelli & Haynes 1993) and with a projected distance of $10\hbox{$.\mkern-4mu^\prime$ }7$ from FGC 284.

FGC 511 Our detection may result from confusion with the Sb spiral NGC 1681, located $8\hbox{$.\mkern-4mu^\prime$ }7$ away, with $V_{\rm h}=2751$ km s^-1 (Huchra et al. 1993), although that galaxy has no published H I detection. In observations obtained with a higher-velocity search range, a second marginal detection is present at the edge of the bandpass, near $V_{\rm h}\sim10095$ km s^-1, with $W_{20}~\rlap{$>$ }{\lower 1.0ex\hbox{$\sim$ }}\ 137$ km s^-1 and $S~\rlap{$>$ }{\lower 1.0ex\hbox{$\sim$ }}\ 0.60$ Jy km s^-1.

FGC 567 We see marginal features near $V_{\rm h}\sim5300$ km s^-1 in spectra obtained using two different autocorrelator configurations, but both features are quite weak.

FGC 598 The optical counterpart of FGC 598 appears extraordinarily diffuse and of low surface brightness on the DSS. The line we detect is likely a result of confusion with the Sa galaxy UGC 3679, $8\hbox{$.\mkern-4mu^\prime$ }5$ away at $V_{\rm h}=5831$ km s^-1 (RC3) and/or the Sb spiral CGC 205-017, $9\hbox{$.\mkern-4mu^\prime$ }2$ away, at $V_{\rm h}=5751$ km s^-1 (Marzke et al. 1996), although CGCG 205-017 has no previously reported H I detection. An additional marginal detection is present in our spectrum at $V_{\rm h}\sim7246$ km s^-1 with $W_{20}\sim180$ km s^-1 and $S\sim0.76$ Jy km s^-1.

FGC 613 Our possible detection of FGC 613 is not corroborated by Giovanelli et al. (1997), who report $V_{\rm h}=7310$ km s^-1 for FGC 613. One possibility is that their detection resulted from a confusion with the Sab spiral UGC 3774 ( $V_{\rm h}=7242$ km s^-1; RC3), $4\hbox{$.\mkern-4mu^\prime$ }6$ from FGC 613, as the peak flux they report for FGC 613 should have been well above our detection limit.

UGC 3716 Our detected line profile is peculiar, probably due to a blended detection. A number of galaxies with redshifts similar to our detected line are present in this region, and two of these galaxies would have overlapped in our beam: UGC 3718, with $V_{\rm h}=6208$ km s^-1, $1\hbox{$.\mkern-4mu^\prime$ }4$ away, and CGC 205-025 with $V_{\rm h}=6257$ km s^-1, $8\hbox{$.\mkern-4mu^\prime$ }1$ away. Their redshifts were determined optically (Marzke et al. 1996), but both have early-type morphologies and neither has previously been detected in H I, hence it is unknown whether we have detected one of these objects, or whether UGC 3716 is an H I-rich member of this group.

FGC 904 Our observations may be contaminated by the Sa spiral NGC 2907 lying $5\hbox{$.\mkern-4mu^\prime$ }6$ away with $V_{\rm h}=2090$ km s^-1, W₂₀=510 km s^-1, and S=6.1 Jy km s^-1 (Richter & Huchtmeier 1987).

UGC 5550 Our detected H I feature is quite weak, although its velocity is close to the optical redshift of $V_{\rm h}=4475$ km s^-1 reported by Makarov et al. (1999).

FGC 1248 The weak feature we observe does not correspond in velocity to the optical redshift of $V_{\rm h}=9897$ km s^-1 measured for FGC 1248 by Makarov et al. (1999); no H I line feature is apparent in our spectrum near the Makarov et al. velocity.

FGC 1359 Our marginal detection may be due to contamination from the E? galaxy MCG-01-31-003, $2\hbox{$.\mkern-4mu^\prime$ }4$ away, with $V_{\rm h}=5589$ km s^-1 (Da Costa et al. 1998), although MCG-01-31-003 has no previously reported detection in H I.

FGC 1563 A matching off-beam feature suggests the emission feature may be due to interference.

ESO 576-047 Our detection is very near the edge of the bandpass and may be spurious.

UGC 7553 Our line profile is likely blended or confused with the S0 galaxy CGCG014-041 $9\hbox{$.\mkern-4mu^\prime$ }8$ away at $V_{\rm h}=8800$ km s^-1 (Metcalfe et al. 1989), although CGCG 014-041 has no previously reported reported detection in H I. We also marginally detect an additional source at $V_{\rm h}\sim4905$ km s^-1 with $W_{20}\sim413$ km s^-1 and $S\sim1.3$ Jy km s^-1.

UGC 8538 A strong off-beam detection or interference overlaps with our observed line profile, hence our source flux and linewidth are lower limits, making the validity of our detection questionable. The off-beam source appears strong and narrow, and no optical catalogued galaxy appears at the location of the off-beam observations; however both the on- and off-beam sources were present in observations obtained on four different days over a one-month period.

FGC 1793 Our lower-velocity detection is likely due to confusion with the dwarf ESO 580-008, $9\hbox{$.\mkern-4mu^\prime$ }1$ from FGC 1793, with $V_{\rm h}=3437$ km s^-1 (Maia et al. 1993); the second source is likely a confusion with the SBc spiral NGC 5716, $9\hbox{$.\mkern-4mu^\prime$ }7$ away, with $V_{\rm h}=4119$ km s^-1 (RC3).

FGC 1903 Our detection appears to be due to a confusion with UGC 9855, an Im galaxy $4\hbox{$.\mkern-4mu^\prime$ }4$ from FGC 1903 with $V_{\rm h}=3480$ km s^-1 (Schneider et al. 1992).

FGCE 1446 Inspection of the DSS reveals a number of other galaxies present in our beam, including the Sb spiral ESO 596-010 at $V_{\rm h}=4732$ km s^-1, $8\hbox{$.\mkern-4mu^\prime$ }8$ away (Fisher et al. 1995). Our detection is likely due to a confusion with this galaxy, although ESO 596-010 has not been previously detected in H I.

ESO 342-044 This region contains a galaxy group, and numerous other galaxies were present in our beam, including ESO 342-045, a spiral with $V_{\rm h}=4960$ km s^-1 (RC3), $7\hbox{$.\mkern-4mu^\prime$ }0$ from ESO 342-044. Our H I detection is mostly likely due to a confusion waith this object.

FGC 2506 A marginal feature is seen at the edge of our bandpass; if real, it may correspond to either a detection of FGC 2506, or to UM165m, a galaxy $2\hbox{$.\mkern-4mu^\prime$ }2$ away with $V_{\rm h}=5096$ km s^-1 (Terlevich et al. 1991) but with no previously reported H I detection.