135 PR HERCULIS (UG) Range: 14.0-21.0V Position: 18 08 04.44 +38 46 17.3 (J2000, A. Henden) Magnitude: V=20.96 B-V=-0.07 (Henden) ID RA (2000) DEC X Y N V ERR B-V ERR a) Comparison star sequence 1 18 08 08.4 +38 44 47 47 -90 3 11.117 0.381 0.998 0.173 2 18 08 05.6 +38 44 13 14 -124 3 11.542 0.273 0.928 0.171 3 18 08 25.0 +38 47 15 241 58 3 11.865 0.169 0.660 0.076 4 18 07 40.0 +38 52 20 -285 363 3 11.979 0.118 0.473 0.036 5 18 07 52.6 +38 43 17 -138 -180 3 12.342 0.037 1.086 0.043 6 18 08 20.5 +38 44 12 188 -125 4 12.776 0.000 1.258 0.005 7 18 08 11.8 +38 49 41 87 204 4 12.989 0.011 0.674 0.009 8 18 08 03.3 +38 45 28 -13 -49 4 13.811 0.008 0.961 0.004 9 18 08 12.2 +38 47 14 91 56 4 13.924 0.009 0.680 0.003 10 18 08 18.3 +38 45 38 163 -39 4 14.483 0.005 0.787 0.009 11 18 08 00.8 +38 46 10 -42 -7 3 14.929 0.008 0.780 0.003 12 18 08 00.2 +38 46 18 -49 1 3 15.270 0.000 0.731 0.010 13 18 08 00.9 +38 47 24 -40 67 3 15.582 0.000 0.834 0.002 14 18 08 03.6 +38 46 09 -9 -8 3 15.738 0.000 1.015 0.007 15 18 08 01.7 +38 45 57 -32 -20 3 16.617 0.016 0.636 0.012 16 18 07 59.6 +38 46 34 -56 17 3 17.382 0.013 0.695 0.021 17 18 08 04.2 +38 47 01 -3 44 3 18.383 0.006 0.589 0.003 18 18 08 07.6 +38 46 25 38 8 3 18.965 0.077 0.832 0.094 19 18 08 06.4 +38 45 55 23 -22 2 20.155 0.014 0.472 0.170 b) Wide-colour extension for CCD calibration 18 07 46.1 +38 42 55 -214 -202 3 17.633 0.166 0.426 0.038 18 08 06.6 +38 48 33 26 136 3 16.574 0.006 0.454 0.012 18 08 25.0 +38 45 24 241 -53 3 16.870 0.006 1.471 0.034 18 08 22.9 +38 48 05 216 108 3 17.776 0.013 1.514 0.063 Notes: 1. Stars 1,2,3,and 4 are saturated, are have large errors. Star #1 has a reliable Tycho-2 magnitude of 10.63 +/-0.06. Another bright star in the south of the field, due south of star #1, has a reliable Tycho-2 magnitude of V=9.62 +/-0.02. 2. Stars 18 and 19 are very faint and therfore also have large errors. They should be used of guidance only. 3. The position and magnitude for PR Her, shown in the title block, were derived from deep CCD frames obtained at Flagstaff Station during May 1999. The minimum magnitude of V=20.6 was determined from a single deep image. 4. This is an extremely faint dwarf nova at minimum, and the identification chart in Downes and Shara (1993) does not show the variable as it is too faint. Bruce Sumner posted 020119