HD24479 has several HPOL observations, as a Be star; the one given here is HD24479 from Dec 30, 1998. The polarization pattern is interstellar in HD24479 B, V, R, I, and matches the values given in HD24479 Appenzeller 1968ApJ...151..907A. HD24992 = ADS 2924 AB: Anderson et al. (1996AJ....112.2726A) give the HD24992 summed data in 100{AA} bins from two observations in 1995. The HD24992 data here include an observation made in 2001. K is higher than HD24992 the maximum .94 from W92's formula. DH give 2.3% at 145, HD24992 significantly different than in Table 2. HD25090 The Reticon 11/16/94 and CCD 09/12/96 observations are of similar HD25090 quality, the Reticon having somewhat greater uncertainty. The HD25090 Reticon data is given in 100{AA} bins in Table 2a of Anderson et HD25090 al. (1996AJ....112.2726A); the filter data are given here to HD25090 compare the UBVR data and to show the relative quality of the HD25090 observations. B, V, and R polarizations match, and PA matches to HD25090 within expected PA calibration; U polarizations differ somewhat. HD25090 P_max_ is the same in the two observations and {lambda}_max_ HD25090 differs by only about 50{AA}. The difference in K and the larger HD25090 uncertainty from the Reticon data is probably due to the somewhat HD25090 worse UX Reticon observation, and its lesser long wavelength HD25090 coverage. These two observations illustrate the reproducibility of HD25090 P_max_ and {lambda}_max_ results from high quality HPOL HD25090 observations. CGS give 5400+/-200{AA}, 5.57+/-.42% for HD25090 {lambda}_max_ and P_max_; {lambda}_max_ is a bit higher than, HD25090 and P_max_ is consistent with, values in Table 3. K from both HD25090 observations is higher than the maximum .93 from W92's formula. HD25290 DH give 1.1% polarization, much higher than in Table 2. HD25443 The Reticon polarization data is the sum of six observations taken HD25443 in 1991 and 1992; it is given in 100{AA} bins in Table 2a of HD25443 Anderson et al. (1996AJ....112.2726A), and is given here in the HD25443 filter bands to allow comparison with other observers. K is higher HD25443 than the maximum .94 from W92's formula. The values for HD25443 {lambda}_max_ and P_max_ in Table 3 are consistent with the values HD25443 given in SMF. Bastien et al. (1988AJ.....95..900B) report that the HD25443 star varied by about .3% over a period of days, in a 1800{AA} wide HD25443 band centered at 4700{AA}. The six HPOL observations differed from HD25443 the average by no more than .05% in V, and .1% in B. HD25497 DH give 1.7%, 149 photographic polarimetry, somewhat higher than HD25497 in Table 2. HD25498 has a composite spectrum (evident on Case Burrell Schmidt objective HD25498 prism plates as seen by author AJW); Balz (1956, Pubs. of the HD25498 Leander McCormick Obs., 13, Part 1) gives K3+A2; we use here HD25498 Harris's (1976ApJS...30..451H) K3III+A3V:: (:: indicates larger HD25498 uncertainty than usual about the spectral type) (also in her HD25498 "Remarks" section, Harris seems to be considering that the HD25498 composite spectrum star has the double HD number 25497/8; the HD HD25498 catalog notes state that HD25497 is the separate star about an HD25498 arc minute away from HD25498). SB data appear in Mermilliod et HD25498 al. (2007, Cat. ). Its absolute magnitude and HD25498 colors, and so, its spectroscopic parallax are more uncertain HD25498 than other stars in Table 1 (and estimates in the literature of HD25498 its spectral type solely from photometry are unreliable). The HD25498 polarization being larger than HD25497 suggests that it is HD25498 actually farther away. BD+61 677 K is higher than the maximum .95 from W92's formula, though this is BD+61 677 not as well determined as for the brighter stars given in Table 3. BD+62 649 DH give 2.2%, 146 photographic polarimetry, lower than in Table 2. BD+62 657 DH give 3.4%, 151 photographic polarimetry, lower than in Table 2. LS I +61 325 = GSC 4063/203. This identification is not noted on SIMBAD. This LS I +61 325 observation was done with HPOL on the WIYN telescope. The two LS I +61 325 different wavelength range observations were taken several months LS I +61 325 apart: PA for V differs by 2' from R and I; this is probably LS I +61 325 a calibration problem associated with the preliminary WIYN LS I +61 325 calibration currently available. NGC1502 01 = HR1260. With NGC 1502 02, these were observed the same night NGC1502 01 (95/11/15 = MJD 50036.8), so the observed difference in NGC1502 01 polarization has greater statistical significance than if they NGC1502 01 were observed on different nights. The data for HR1260 is given in NGC1502 01 100{AA} bins in Table 2a of Anderson et al. (1996AJ....112.2726A); NGC1502 01 the filter data is given here for comparison to the other cluster NGC1502 01 stars. K is larger than the maximum .90 from W92's formula. NGC1502 02 = SZ Cam We have used here the designations on SIMBAD (noting that NGC1502 02 there has been inconsistency in the literature on this); i.e., NGC1502 02 SZ Cam is the slightly northernmost of the two brightest stars in NGC1502 02 the cluster. NGC1502 02 These were observed the same night (95/11/15 = MJD 50036.8), so NGC1502 02 the observed difference in polarization has greater statistical NGC1502 02 significance than if they were observed on different nights. NGC1502 02 Since one component of the multiple system SZ Cam has Beta Lyrae NGC1502 02 characteristics, and HR 1260 also is a binary (Lorenz et al. NGC1502 02 1998A&A...332..909L) any difference may be partly intrinsic NGC1502 02 rather than in ISM polarization. NGC1502 02 K is larger than the maximum .90 from W92's formula. NGC1502 26 = BD+61 675: DH give 6.3%, 144, similar to Table 2. NGC1502 37 This observation was made with HPOL on the WIYN telescope during NGC1502 37 one night: Feb 10, 1996 = MJD 50123.64. K is higher than the NGC1502 37 maximum .91 from W92's formula.