12514+1027 There are two redshifts for this object in the literature: 12514+1027 0.30 (Wilman et al., 1998MNRAS.300L...7W) and 0.3189 (PSCz, 12514+1027 Cat. ). We have coverage of both redshifts and find no clear 12514+1027 OH emission, but there are regions in the bandpass between the two 12514+1027 frequencies that are unobservable because of RFI. We use the PSCz 12514+1027 redshift as the fiducial for computing luminosities and limits on 12514+1027 the OH emission of this object. 13451+1232 We attempted to make a reobservation of this tentative OH detection 13451+1232 by Dickey et al. (1990AJ....100.1457D), but the strong radio 13451+1232 continuum (5.4Jy) produced standing waves in the spectrum and 13451+1232 frustrated detection of any OH lines. The host of this probable OHM 13451+1232 is classified a Seyfert 2 by Kim, Veilleux, & Sanders 13451+1232 (1998ApJ...508..627K) and a Seyfert 1.5 by Baan, Salzer & LeWinter 13451+1232 (1998ApJ...509..633B) (the latter indicate that two nuclei were 13451+1232 observed, but only one classification is listed for this object). 13451+1232 Veilleux, Sanders, & Kim (1997ApJ...484...92V) have detected broad 13451+1232 Pa{alpha} emission from this merger, indicating that it contains a 13451+1232 buried quasar. In fact, many groups refer to this object as an 13451+1232 "IR quasar." This is a double nucleus system, with nuclear 13451+1232 separation of 3" (7.1kpc) and ample molecular gas: logM(H_2_)=10.78 13451+1232 (Scoville et al., 2000AJ....119..991S). 01562+2528 This OHM shows broad, blended lines, which are easily identified, 01562+2528 despite the highly uncertain optical redshift. Although the ACF 01562+2528 shows no second peak, the 1665MHz line is quite prominent. Galactic 01562+2528 H I has been masked at 52200km/s. The DSS image of the host of this 01562+2528 OHM shows a multicomponent object with possible extended emission. 01562+2528 Observations at the Palomar 5m telescope confirm this with the 01562+2528 detection of two nuclei (Paper V, Condon et al., 2002, in prep.). 01562+2528 We classify the northeast nucleus of this OHM host a starburst. The 01562+2528 southwest nucleus lacked sufficient signal for optical 01562+2528 classification, but a redshift was measured (see Paper V). The 01562+2528 velocity of the northeastern nucleus is consistent with the OH 01562+2528 redshift but that of the southwestern nucleus is not. 02524+2046 This OHM has the most unusual spectrum of the survey sample. The 02524+2046 peak flux density is 40mJy; RFI and receiver considerations aside, 02524+2046 such an OHM would be detectable beyond z=1 at Arecibo in a short 02524+2046 integration time. The emission lines are strong and narrow and show 02524+2046 extremely good correspondence between 1667 and 1665 lines, including 02524+2046 a blue tail on each complex. The correspondence is so good that we 02524+2046 can measure the hyperfine ratio for each component of the line 02524+2046 profile. From high velocity to low, we find RH=1.40, 5.63, and 1.88 02524+2046 (Table 6 lists the hyperfine ratio of the combined emission: 02524+2046 RH=3.2). Galactic H I has been masked in the spectrum and is 02524+2046 accompanied by a dip in the weights spectrum. There is also an 02524+2046 interesting feature at 51800km/s, which is likely to be H I in the 02524+2046 off-source position (5m later than the on-source position) with a 02524+2046 heliocentric velocity of about -300km/s. This is probably associated 02524+2046 with the Magellanic stream. We classify the host of this OHM as a 02524+2046 starburst (Paper V, Condon et al., 2002, in prep.). 03521+0028 The optical redshift perfectly matches the 1667MHz line, as well as 03521+0028 the marginally significant 1665MHz line. The feature identified as 03521+0028 the 1665MHz line by the ACF and the position of the 1667MHz line is 03521+0028 a 3.4{sigma} detection and is quite narrow. The host of this OHM is 03521+0028 classified in the mid-IR as starburst by Lutz, Veilleux, & Genzel 03521+0028 (1999ApJ...517L..13L) and in the optical as a LINER by Veilleux, 03521+0028 Kim, & Sanders (1999ApJ...522..113V) and us (Paper V, Condon et al., 03521+0028 2002, in prep.). K-band imaging by Murphy et al. 03521+0028 (1996AJ....111.1025M) gives a nuclear separation of 1.6" or 3.6kpc. 03521+0028 Solomon et al. (1997ApJ...478..144S) measure a CO(10) line width of 03521+0028 150km/s, estimate a H_2_ mass of 4.3x10^10^M_{sun}_, and derive a 03521+0028 blackbody radius of 319pc. 03566+1647 There is no obvious 1665 MHz line in this OHM spectrum, and the ACF 03566+1647 shows no secondary peak. We compute an upper limit on the 1665MHz 03566+1647 line flux, assuming a 1{sigma} line of width equal to the 1667MHz 03566+1647 line to obtain a lower limit on the hyperfine ratio: RH>~9.6. The 03566+1647 optical redshift does not correspond to the peak OH emission. We 03566+1647 classify the host of this OHM as a Seyfert 2 (Paper V, Condon et 03566+1647 al., 2002, in prep.). 10035+2740 This OHM has a number of sharp lines, and it is unclear whether the 10035+2740 1665MHz line is present (there is a narrow 4{sigma} ine somewhat 10035+2740 above the expected position that is included in the estimate of RH). 10035+2740 Galactic H I has been masked in the final spectrum. The spectrum is 10035+2740 somewhat noisy, and it is unclear whether the multiple peaks are OH 10035+2740 or noise; there are two broad lines and smaller spikes on the less 10035+2740 prominent line. The weights spectrum is very clean. 10378+1108 This OHM is a redetection and was discovered by Kazes & Baan 10378+1108 (1991A&A...248L..15K). The measured properties listed in Table 6 are 10378+1108 consistent with those measured by Kazes & Baan (1991A&A...248L..15K) 10378+1108 and the spectra are similar, but comparison is difficult because of 10378+1108 very different signal-to-noise ratio observations. The spectrum in 10378+1108 Figure 1 shows a strong line with broad red and blue wings with no 10378+1108 clear 1665MHz line. The ACF of this spectrum shows no second peak. 10378+1108 K-band imaging by Murphy et al. (1996AJ....111.1025M) obtains an 10378+1108 upper limit on the nuclear separation (if any) of this OHM host: 10378+1108 less than 0.5" or 1.1kpc. The host of this OHM is classified as a 10378+1108 LINER by Veilleux et al. (1999ApJ...522..113V) and by us (Paper V, 10378+1108 Condon et al., 2002, in prep.). 11180+1623 Note that this object is NOT in the PSCz sample. The emission profile 11180+1623 of this OHM has a sharp red falloff and a blue tail. The 1665MHz 11180+1623 line identified by the ACF and the 1667MHz line prediction has 11180+1623 2.8{sigma} significance but resembles other baseline features. The 11180+1623 hyperfine ratio measured from this line is thus treated as a lower 11180+1623 limit. Galactic H I has been masked in the spectrum presented in 11180+1623 Figure 1. 12005+0009 This OHM has at least three distinct emission components and a very 12005+0009 broad total spectrum (1081km/s in the rest frame at 10% of the peak 12005+0009 flux density). The ACF is broad and multiply peaked but seems to 12005+0009 indicate the secondary component as the 1665MHz line, in agreement 12005+0009 with the prediction from the center of the main 1667MHz line. All 12005+0009 components are included in the total OH measure, but we tentatively 12005+0009 identify the secondary component as the 1665 MHz line for a rough 12005+0009 measure of the hyperfine ratio that excludes the highest velocity 12005+0009 tertiary component: RH~2.0. The DSS image of the OHM host is 12005+0009 extended and irregular. 12018+1941 We redetect an OHM first observed by Martin et al. 12018+1941 (1988A&A...201L..13M). The spectra look similar and all the 12018+1941 measurements presented in Table 6 are consistent with those of 12018+1941 Martin et al. (1988A&A...201L..13M), but the uncertainties are high 12018+1941 in both detections because of low signal-to-noise ratio. Galactic 12018+1941 H I has been masked in the spectrum presented in Figure 1. The ACF 12018+1941 shows a minor second peak, although there is no significant spectral 12018+1941 feature where we expect a 1665MHz line. We compute a lower bound on 12018+1941 RH, assuming a 1{sigma} 1665MHz profile with width equal to the 12018+1941 1667MHz line: RH>=5.6. The host of this OHM is classified as a LINER 12018+1941 by Baan et al. (1998ApJ...509..633B) and by Veilleux et al. 12018+1941 (1999ApJ...522..113V), although the latter group notes that it could 12018+1941 be a Seyfert 2. 12162+1047 This OHM has no obvious 1665MHz line, and mild standing waves in 12162+1047 the baseline. We measure only the main line, since the smaller line 12162+1047 on the blue side is similar in size and shape to noise features in 12162+1047 the bandpass. The ACF has no significant second peak. Assuming a 12162+1047 1{sigma} profile with width equal to the 1667MHz line width, we 12162+1047 obtain a rough upper bound on the 1665MHz emission, which provides a 12162+1047 lower bound on the hyperfine ratio: RH>=11.1. The DSS image shows a 12162+1047 pair of overlapping galaxies with significant separation 12162+1047 (roughly 11" or 26kpc). 12549+2403 This OHM has a sharp, well-defined second peak in the ACF. The 12549+2403 1665MHz line is poorly defined in the spectrum and if present has 12549+2403 a 3.6{sigma} peak. There are mild standing waves in the bandpass 12549+2403 that could masquerade as the 1665MHz line. The 1667MHz line is 12549+2403 asymmetrical, with sharp red falloff and a blue tail. The DSS image 12549+2403 of this object is extended and elliptical in shape but more or less 12549+2403 regular (no clear signs of interaction). 13218+0552 The host of this OHM is classified as a quasi-stellar object (QSO) or 13218+0552 Seyfert 1 (Low et al., 1988ApJ...327L..41L) and is one of three 13218+0552 Seyfert 1 hosts of OH megamasers. The other two are Mrk 231 13218+0552 (IRAS 12540+5708; Baan et al., 1992AJ....103..728B; Baan et al., 13218+0552 1998ApJ...509..633B; Kim et al., 1998ApJS..119...41K) and UGC 545 13218+0552 (IRAS 00509+1225; Bottinelli et al. 1990IAUC.4977Q....B; Sanders et 13218+0552 al., 1988ApJ...328L..35S), and Tables 7 and 8 list the properties of 13218+0552 these OHMs.