Name Mag h m s o ' " # Remarks GJ 3031 16.4 00 19 15 +42 36 42 158 WD LP 349-25 17.0 00 27 55 +22 19 32 131 M8 dwarf Mu Cass 5.1 01 08 16 +54 55 13 108 Pop II binary Wolf 59 11.4 01 16 10 +60 09 13 140 Md, B-V~2.0 Ups And 4.1 01 36 49 +41 24 09 109 Planetary System HD 10697 6.3 01 44 56 +20 04 59 110 Planetary System LP 30-55 14.1 02 1 54 +73 32 32 128 Md, B-V=1.9 TZ Aries 12.3 02 00 13 +13 3 7 120 Perturbation study LP354-381 16.6 02 31 41 +27 09 51 159 WD GJ 3173 15.1 02 38 33 +06 37 36 160 WD SO 0253+1652 15.4 02 53 01 +16 52 58 111 M6.5 Pleiades #5 6.8 03 47 29 +24 17 18 112 Cluster parallax GJ 3288 17.1 04 26 20 +04 32 33 161 WD Hip 21276 7.8 04 33 54 +64 38 00 113 G8-52 11.2 04 42 23 +20 46 34 122 Md (M dwarf) P 15-315 14.6 05 08 18 +75 38 15 141 GJ 3339 15.9 05 14 04 +08 00 15 162 WD GJ 1082 14.8 05 36 20 +41 29 55 163 WD G100- 50 14.8 05 58 53 +21 21 01 123 LHS1822 16.0 06 07 16 +73 31 59 164 WD P 160-22 14.7 06 23 51 +45 40 5 142 Hip 33142 11.2 06 54 05 +60 52 13 119 G109-32 12.2 06 54 30 +21 15 06 176 WD LP 206-11 15.1 07 11 11 +43 29 59 129 NGC 2355 14.0 07 17 0 +13 45 0 153 Calibration field GJ 1098 16.4 07 33 31 +64 09 30 165 WD LP 423-31 16.3 07 52 23 +16 12 15 133 LHS 1988 13.7 08 12 27 +43 09 28 118 Md very red but K: spc Praesepe #4 6.6 08 39 43 +19 46 41 116 Cluster parallax LP 209-59 15.0 08 49 8 +39 36 27 143 LP 312-51 15.2 08 59 29 +29 18 18 144 LHS 2090 15.5 09 00 23 +21 50 05 132 GJ 3529 17.0 09 05 33 +73 14 56 166 WD LHS 269 15.8 09 29 11 +25 58 9 124 GJ 2074 14.9 09 42 02 +06 57 05 167 WD GJ 2077 15.4 10 01 49 +14 41 24 168 WD LHS 2243 17.4 10 16 34 +27 51 49 156 LP 430-46 16.4 10 36 8 +19 23 30 138 LHS 285 16.9 10 37 02 +71 10 56 175 WD LP213-67,68 16.3 10 47 12 +40 26 43 154 Wolf 359 13.5 10 56 28 +07 00 42 117 Perturbation study LP 431-50 12.3 11 3 8 +15 17 51 145 LP 214-42 15.2 11 8 49 +39 55 12 146 GJ 1149 16.4 11 45 45 +63 06 11 169 WD UCAC40691564 15.0 11 50 19 +25 17 58 157 WD LHS 318 14.8 11 56 55 +26 39 56 125 LP 59-34 14.3 12 41 28 +19 5 1 147 GJ 3750 15.6 12 48 19 +58 19 34 170 WD LP 218-8 17.5 12 53 12 +40 34 03 155 LP 172- 4 15.5 12 54 32 +44 59 35 149 LP 496-48 14.5 12 54 50 +11 59 15 148 LP161-93 12.4 12 59 18 +00 10 24 121 Md GJ 3768 16.0 13 08 37 +85 02 42 171 WD improve pi 55+/-9.3 LP 220-13 17.5 13 56 41 +43 42 58 139 LHS 370 15.3 14 20 53 +36 57 17 126 LHS 2919 16.2 14 28 4 +13 56 14 134 G179-55 13.1 15 47 27 +45 07 51 127 Md LP 22-420 14.5 15 49 55 +79 39 51 135 LHS 3154 16.4 16 06 33 +40 54 21 150 G 225-54 14.9 16 16 42 +58 39 43 151 LP 275-74 16.0 16 37 1 +35 35 45 152 LHS 3241 15.7 16 46 31 +34 34 55 136 LHS3250 17.1 16 53 59 +62 53 14 172 WD, 2 targets CPM 173 11.5 17 05 53 +26 05 44 174 CPM of above LP387-036 16.5 17 05 53 +26 05 44 173 WD, 2 targets Hip 85605 11.0 17 29 36 +24 39 15 102 Hip error LP 71-82 13.1 18 2 16 +64 15 44 130 LP 335-12 17.2 18 39 33 +29 52 16 137 Sigma Dra 4.7 19 32 22 +69 39 40 105 Perturbation study HD 195019 6.9 20 28 19 +18 46 10 103 Planetary system 61 Cygni AB 5.8 21 06 55 +38 44 45 106 Perturbation study IM Pegasi 5.9 22 53 02 +16 50 28 104 Gravity Probe B guide LFT 1767 5.6 23 13 18 +57 10 08 107 Perturbation study Hip 116132 10.1 23 31 52 +19 56 14 115 M6V, Perturbation Above is a list of the stars currently being observed by The Thaw/CCD parallax program. Most of these stars are suspected M dwarfs within 20 parsecs of the Sun. Target stars are being added at a rate of about 2 per week. The approach is to observer the star twice about 3 months apart to detect probable parallactic motion and to improve the photometry of the star and reference stars in B, V, and I. If little motion is detected the star is observed twice more to yield a preliminary parallax which will be published as an approximate value. If a large parallax is indicated the star will be observed on approximately 8 more occasions to establish an accurate parallax. Correction to absolute will be enhanced by the use of relatively faint reference stars for which we will have approximate B, V, and I magnitudes. For initial tests of the precision see the chart on this web page. Initial parallax results are also available. Bright stars are observed through ND filters of 2.5, 5.0, 7.5, and 10.0 magnitudes. A similar precision is obtained for ND filtered and non-ND filtered stars.