HD 3431 In an M31 target field on ASTRO-2. delta Cet =HD 16582: Korhonen and Reiz (1986A&AS...64..487K) give .081+/-.021% delta Cet and 155.0+/-7.3deg for polarization at B, similar to our values delta Cet given in Table 3. HD 21588 In the field of GK Per. HR 1099 =V711 Tau: Active chromosphere, RS CVn type variable. The low value HR 1099 of polarization in Table 1, consistent with zero, is the sum of HR 1099 observations made 01/08/90 and 10/02/90 which do not differ HR 1099 significantly. This is consistent with Koch and Pfeiffer HR 1099 (1977IBVS.1260....1K) and Weiler et al. 1978ApJ...225..919W) who HR 1099 find no polarization and no variability at levels of a few HR 1099 hundredths percent. A spectrum, but no polarimetry, was obtained HR 1099 during ASTRO-1. HD 23594 =HR 1161: The value of P we obtain at V is somewhat lower than that HD 23594 of the Coyne et al. (1979AJ.....84..356C) value at G=.71%+/-.02%, HD 23594 and similar to Appenzeller's (1968ApJ...151..907A) .63%. HD 23985 =HR 1188: Pleiades ISM probe HD 24368 Pleiades ISM probe HD 27360 In the field of TW Cam. BD+26 730 BY Dra type. This data is a combination of observations on BD+26 730 02/23/89 and 10/08/89, which are not significantly different. Saar BD+26 730 et al. (1994A&A...286..194S) report quiescent polarization in U and BD+26 730 B of about .4% and .1%, respectively; our data for U and B in BD+26 730 Table 3 is consistent with this level of polarization. HD 29647 Our calculated lambda_{max}_ is greater than the longest wavelength HD 29647 in the observational data, so it has a relatively large HD 29647 uncertainty. Our values differ somewhat from the 2.30%, 7300{AA} HD 29647 P_{max}_, lambda_{max}_ of Whittet et al. (1992ApJ...386..562W), HD 29647 whose values should be more reliable since they had polarimetry for HD 29647 longer wavelengths. Our data show rotation of position angle about HD 29647 64deg to 73deg in the range 3200-7600{AA}, similar to theirs. HD 37356 =HR 1923: The sum of observations made on 03/25/92 and 01/11/93. HD 37356 CGS's 1.56+/-.10% at 5200+/-100{AA} differ by over 1sigma from our HD 37356 values of P_{max}_ and lambda_{max}_. Appenzeller HD 37356 (1968ApJ...151..907A) gives P at V of 1.46%, the same as ours. HPOL HD 37356 data show a position angle rotation from 70deg at the shortest HD 37356 wavelengths to 66deg at the longest. HD 38087 The sum of observations made 12/28/92, 01/31/93, and 02/15/93. HD 38087 SMF's average values of 2.93% at 6400{AA} P_{max}_ and HD 38087 lambda_{max}_ are both significantly greater than ours. Appenzeller HD 38087 (1968ApJ...151..907A) gives P at V of 2.54%, not significantly HD 38087 differing from ours. HD 251204 This star is given as an HST polarization standard In Turnshek et HD 251204 al. (1990AJ.....99.1243T); their P at V of 4.04% at 147deg is HD 251204 significantly lower than ours. Hiltner (1951ApJ...114..241H) gives HD 251204 4.7% at 155deg, the same as ours. HD 45629 ISM probe for HD 45677 HD 46064 =HR 2373: ISM probe for HD 45677; the polarization is small, so HD 46064 lambda_{max}_ has a relatively large uncertainty. NGC 2264 67 =Walker 67: Wilking et al. (1980ApJ...235..905W) give 5.31+/-.06% NGC 2264 67 and 8100 +/- 200{AA} for P_{max}_ and lambda_{max}_. Our values are NGC 2264 67 consistent with these; theirs must be considered more reliable NGC 2264 67 because the star is too faint to observe well at PBO, and NGC 2264 67 lambda_{max}_ is longward of our longest wavelength observed. HD 50562 Schulte-Ladbeck et al. (1992ApJ...391L..37S) used this star as a HD 50562 way of estimating the ISM polarization to EZ CMa. Their HD 50562 polarization values are superseded by the those given here, which HD 50562 are derived from a combination of their observation plus three HD 50562 later observations (01/08/91, 12/28/92, 02/01/94 and 12/10/94) with HD 50562 the same instrument. The star is relatively faint with low HD 50562 polarization, resulting in relatively large uncertainty for HD 50562 lambda_{max}_. HD 50646 In the field of EZ CMa; the sum of observations made 03/05 HD 50646 and 03/23/94. delta CMa =HD 54605: F supergiant; sum of observations made 01/06/90 and delta CMa 03/13/90. Serkowski (1970ApJ...160.1083S) gives P at V of .14% at delta CMa 26deg and Behr (1959, Veroff. Gottingen, No 126) gives .15% at delta CMa 34deg, both of which are consistent with our low polarization. HD 56126 Post-AGB star; any possible circumstellar matter is not evident HD 56126 in the polarimetry. HD 60325 HPOL observations were made 01/14/90 and 03/25/90. SMF give average HD 60325 values of 5300{AA} and 1.23% for P_{max}_ and lambda_{max}_ with HD 60325 uncertainties about 200{AA} and .03%. Our values are consistent HD 60325 with these, but have lower uncertainty. HD 61931 =HR 2969: Rapid rotator. The data is the sum of four observations HD 61931 made over 11 days (01/05, 01/08, 01/13 and 01/16/90), with no HD 61931 variation; the polarization follows a typical ISM pattern. phi Leo =HD 98058: Rapid rotator; shell star. This data is the sum of two phi Leo observations (04/25/90 and 05/01/90) which do not differ phi Leo significantly from zero in any filter; values for U, B and R are in phi Leo Table 3. Bhatt (1996A&AS..120..451B) gives P at V .43+/-.09% at phi Leo 49+/-6deg; Clayton and Marlborough (1980ApJ...242..165C) find phi Leo polarization not significantly greater than zero, and Coyne phi Leo (1974AJ.....79..565C) gives polarization values from .18% in the phi Leo ultraviolet decreasing to .03% in G. HD 109055 For this suggested low polarization standard Clemens and Tapia HD 109055 (1990PASP..102..179C) give .015+/-.031%. Berdyugin et al. HD 109055 (1995A&A...294..568B) give P at V .12+/-.05% at 95+/-12deg; their HD 109055 position angle differs from ours but by only 1-2sigma, reasonable HD 109055 given the small polarization. HD 117567 Field of FK Comae. Korhonen and Reiz (1986A&AS...64..487K) give HD 117567 P at B .037+/-.027% at 110.6+/-18.5deg, consistent with our value HD 117567 given in Table 3. 109 Vir =HD 130109: MF give polarization .05% and Behr (1959, Veroff. 109 Vir Gottingen, No 126) gives .15%; both of these are consistent with 109 Vir our low polarization. xi Boo A =HD 131156: Combination of five observations made over about four xi Boo A weeks (04/08, 04/13, 04/17, 04/27 and 05/08/90); there is no xi Boo A polarization at V significantly greater than zero; this is xi Boo A consistent with Leroy's 1993 .008+/-.008%. xi Boo A Houvelin et al. (1988ApJ...329..882H) report variations in U of xi Boo A 0-.3%; the largest U polarization we observe is .13+/-.04%. Our xi Boo A average values for U, B and R are in Table 3; no significant xi Boo A variation was observed. HD 142863 Clemens and Tapia (1990PASP..102..179C) give 1.891+/-.063% at HD 142863 83.7+/-.1deg at V for this proposed standard, somewhat higher than HD 142863 our values. MF give 1.72% at 84.7deg at B; similar to ours in HD 142863 Table 3. nu Sco =HD 145502: The sum of three observations over about four weeks nu Sco (05/06, 05/11, and 06/04/92).WLR give 7000+/-100{AA} and nu Sco 1.55+/-.04% and CGS give 7000{AA} and 1.21% for P_{max}_ and nu Sco lambda_{max}_. Our K is somewhat larger than expected from the WLR nu Sco relation, but our values are within about 1sigma of theirs; nu Sco however, the quality of our observation is below average longward nu Sco of about 6500{AA}. sigma Sco =HD 147165: SMF give 5600+/-100{AA} and 1.55+/-.07% for P_{max}_ sigma Sco and lambda_{max}_. Our values are consistent with these and have sigma Sco lower quoted errors. The position angle rotates from 4deg to sigma Sco 174deg in the in the range 3200-7600{AA}; rotation is also sigma Sco marginally evident in the data in Gehrels and Silvester sigma Sco (1965AJ.....70..579G) and Coyne and Gehrels (1966AJ.....71..355C); sigma Sco their uncertainties are much greater than ours. Kemp and sigma Sco Wolstencroft (1972ApJ...176L.115K) find evidence of circular sigma Sco polarization, which is zero at about 5800{AA} (reading from their sigma Sco graph), about our lambda_{max}_. (Martin and Angel sigma Sco (1976ApJ...207..126M) noted that this is about the same as SMF's sigma Sco lambda_{max}_.) zeta Her =HD 150680: The sum of observations on 04/25 and 05/02/90. Leroy zeta Her 1993 gives P as .00010+/-.00015%, consistent with our low value. delta Her =HD 156164: Rapid rotator. Behr (1959, Veroff. Gottingen, No 126) delta Her gives polarization value indistinguishable from zero, consistent delta Her with our value. 61 Oph =HR 6609 = HD 161270 = ADS 10750 A; and HD 161289 = HR 6610 = 61 Oph ADS 10750 B, 21" separation. This translates to a separation of 61 Oph about 3300 AU at estimated distance modulus of There are no 61 Oph spectral peculiarities indicated in any references in the 61 Oph literature. The polarization difference of .12% at V is marginally 61 Oph statistically significant since both observations were obtained the 61 Oph same night, and so may be a case of two components of a wide double 61 Oph differing in ISM polarization. In Table 3 the polarizations at B 61 Oph are indistinguishable, and at R are different with a significance 61 Oph somewhat less than at V. 3 Sgr =HD 161592: SMF give 5800+/-100{AA} and 1.53+/-.01% for P_{max}_ 3 Sgr and lambda_{max}_, consistent with our values which have lower 3 Sgr quoted errors. 68 Oph =HD 164577: The polarization in Table 1 is the sum of observations 68 Oph on 07/20/93 and 03/04/94; the polarization pattern is what would be 68 Oph expected for ISM polarization with lambda_{max}_ in the V spectral 68 Oph range, but the uncertainties are so large relative to the 68 Oph polarization that the WLR parameters are not given, but the 68 Oph polarizations at B and R are given in Table 3. Leroy 68 Oph (1993A&A...274..203L) gives P at V .180+/-.013% at 41deg; 68 Oph MF give P at B .13+/-.03% at 45.0deg; Both are almost identical to 68 Oph our values. Vidal-Madjar et al. (1993IAUC.5795....1V) reported 68 Oph a possible circumstellar disk; however, Vidal-Madjar et al. 68 Oph (Ap&SS.223..198V) question their own initial interpretation. Our 68 Oph polarimetry shows no evidence of circumstellar effects. HD 168625 A combination of four observations made 08/20, 09/30, 10/02 and HD 168625 10/06/92. All four show Halpha emission. Our lambda_{max}_ is HD 168625 similar to CGS's 5200{AA}, but differs from WLR's 4500{AA}. Our HD 168625 P_{max}_ is considerably larger than WLR's 4.13% and CGS'S 4.20%. HD 168625 This star being relatively faint and heavily reddened, our HD 168625 observation is not good enough at short wavelengths to determine if HD 168625 there is a polarization decrease in the Balmer continuum, as for HD 168625 nu Cep (See below), or whether there is a polarization effect at HD 168625 the Halpha emission line. As an emission line supergiant, and so HD 168625 having possible intrinsic variable polarization due to HD 168625 circumstellar matter, this star would not seem to be a good choice HD 168625 for future general ISM studies. HD 168701 In the field of HD 168625. HD 192182 In the field of WR star HD 192163. Krautter (1980A&AS...39..167K) HD 192182 gives P at about B .08+/-.03% at 77.3+/-10.4deg, consistent with HD 192182 our value in Table 3. 21 Vul = HD 192518: Rapid rotator. Clayton HD 192182 and Marlborough (1980ApJ...242..165C) found average polarization at HD 192182 4093{AA} about .18% at about 55deg, similar to our value at B in HD 192182 Table 3. A spectrum, but no polarimetry, was obtained during HD 192182 ASTRO-1. HD 235255 ,and HD 196177: Field of V1974 Cyg = Nova Cyg 1992 HD 196177 ,and HD 235255: Field of V1974 Cyg = Nova Cyg 1992 HD 196421 ,HD 198378, HD 198679, HD 198793, and HD 199136: In the region of HD 196421 HD 197770, which WUPPE observed on both missions. HD 199308 In the region of HD 197770. Hiltner (1951ApJ...114..241H) gives HD 199308 1.9% at 162deg, consistent with ours. ER Vul =HD 200391: RS CVn star, rapid rotator, active chromospheres. No ER Vul evidence of circumstellar matter in the polarimetry. HD 198378 See HD 196421 HD 198679 See HD 196421 HD 198793 See HD 196421 HD 199136 See HD 196421 nu Cep =HD 207260: The data in table 1 and the parameters in Table 2 were nu Cep calculated from a combination of eleven separate observations made nu Cep during the period 08/20/91 to 10/06/92, and allowing K to vary from nu Cep the standard WLR formula. nu Cep Our computed value of K is considerably larger than that given by nu Cep the WLR formula, about .75. Since it is evident in Fig. 1 that the nu Cep polarization decreases in the Balmer continuum, similar to the nu Cep pattern for Be stars, the parameters were calculated using only nu Cep wavelengths longward of 3700{AA}. This is a supergiant, so nu Cep circumstellar matter would not be unexpected; our spectra do not nu Cep show obvious nu Cep emission at Halpha, though it may be partially filled in; Gray and nu Cep Garrison (1987ApJS...65..581G) report emission in the wings of nu Cep Hbeta and classify it as A2Iae, and Rosendhal (1973ApJ...186..909R) nu Cep and Frandsen (1975A&A....43..267F) find emisssion inside the Halpha nu Cep absorption line; and there is evidence of a stellar wind in the UV nu Cep (Lamers et al., 1995ApJ...455..269) and radio nu Cep (Talavera and Gomez de Castro, 1987A&A...181..300T). The low nu Cep level of polarization at the shortest wavelengths relative to the nu Cep Serkowski curve also seems to be present in the data of Gehrels nu Cep and Silvester (1965AJ.....70..579G) and nu Cep Coyne and Gehrels (1966AJ.....71..355C). This suggests that at nu Cep least some of the polarization is intrinsic to the star, which nu Cep might explain comparatively short lambda_{max}_ found by us and WLR nu Cep and the deviation from the WLR formula for K; this implies that nu Cep this star should not be used in the future for general ISM nu Cep polarization studies, though WLR did use it with filter nu Cep polarimetry. Avery et al. (1975AJ.....80.1026A) consider it to be nu Cep circularly polarized; however, since lambda_{max}_ is probably nu Cep affectd by intrinsic polarization, it is probably not worthwhile to nu Cep compare it to the wavelength where circular polarization is zero. HD 210072 Hiltner (1951ApJ...114..241H) gives .7% at 47deg, consistent with HD 210072 our values. HD 216783 In the field of EW Lac. HD 217035 Hiltner (1951ApJ...114..241H) gives 1.7% at 91deg, consistent with HD 217035 our values. HD 217312 Hiltner (1951ApJ...114..241H) gives 1.3% at 80deg, consistent with HD 217312 our values. HD 217476 G supergiant. SMF give mean values of 2.77+/-.07% and 4900+/-100{AA} HD 217476 for P_{max}_ and lambda_{max}_. Our lambda_{max}_ differs HD 217476 significantly from this, but since this is a supergiant with Halpha HD 217476 emission (present in our spectrum), it may very well have some HD 217476 variable intrinsic polarization due to circumstellar matter, though HD 217476 since the WLR formula fits the data well, most of the observed HD 217476 polarization may be interstellar. HD 218323 CGS give 1.95+/-.14% and 5200+/-200{AA} for P_{max}_ and HD 218323 lambda_{max}_. Our lambda_{max}_ differs from this, and our values HD 218323 have lower quoted uncertainty. HD 218342 CGS give 2.23+/-.20% and 5400+/-200{AA} for P_{max}_ and HD 218342 lambda_{max}_. Our values are similar to these, with lower quoted HD 218342 uncertainties. lambda And: Active Chromosphere; RS CVn type HD 218342 variable. Barbour and Kemp (1981ApJ...246..203B) indicate that this HD 218342 star is unpolarized at the .1% level of sensitivity, but variable at HD 218342 the .01% level; Piirola (1977A&AS...30..213P) gives .006% HD 218342 polarization, and this value is quoted by Tinbergen HD 218342 (1979A&AS...35..325T) (in a list of zero-polarization standards) and HD 218342 by Leroy (1993A&AS..101..551L) (in a list of stars near the Sun); HD 218342 our value, from a single observation, is consistent with this. 6 Cas G supergiant. Hiltner (1951ApJ...114..241H) gives 1.2% at 57deg, 6 Cas consistent with our values. Avery et al. (1975AJ.....80.1026A) 6 Cas find that it is very probably circularly polarized. The circular 6 Cas polarization probably passes through zero between the the V and R 6 Cas band centers, or in the R band itself, consistent with the 6 Cas wavelength of lambda_{max}_. There is possible position angle 6 Cas rotation from 54deg at the shortest HPOL wavelengths to over 56deg 6 Cas at the longest; polarization values for U, B, and R are given in 6 Cas Table 3. Since there is Halpha emission present in our spectrum, it 6 Cas may very well have some intrinsic polarization due to circumstellar 6 Cas matter, though since the WLR fit is very good most of the 6 Cas polarization may be intersterstellar.