54 DH AQUILAE (UGSU) Range: 11.9-18.2V Position: 19 26 10.83 -10 15 29.8 (J2000, from .dat file) Magnitude: V=18.244 B-V=0.249 (Henden, single night) ID RA (2000) DEC X Y N V ERR B-V ERR a) Comparison star sequence 1 19 26 04.1 -10 17 34 -98 -124 3 11.159 0.199 0.318 0.065 2 19 26 03.4 -10 14 34 -109 56 3 11.670 0.081 0.495 0.053 3 19 26 21.1 -10 14 53 152 37 3 12.364 0.010 1.385 0.007 4 19 26 12.3 -10 15 24 22 6 3 12.717 0.009 0.546 0.017 5 19 26 08.0 -10 12 33 -41 177 3 13.220 0.013 0.640 0.018 6 19 26 17.3 -10 16 16 96 -46 3 13.395 0.013 1.329 0.008 7 19 26 14.9 -10 12 48 61 162 3 13.821 0.005 0.719 0.011 8 19 26 08.6 -10 16 33 -32 -63 3 14.298 0.011 1.415 0.007 9 19 26 07.3 -10 14 41 -52 50 3 14.831 0.008 1.085 0.012 10 19 26 06.0 -10 15 29 -70 1 3 15.294 0.011 0.775 0.012 11 19 26 06.6 -10 16 07 -63 -37 4 15.859 0.023 1.208 0.024 12 19 26 07.7 -10 15 25 -46 5 3 16.050 0.011 1.282 0.010 13 19 26 10.1 -10 15 07 -10 23 3 16.678 0.019 1.136 0.019 14 19 26 10.0 -10 15 26 -12 4 3 18.312 0.066 0.859 0.037 b) Wide-colour extension for CCD calibration 19 26 13.0 -10 13 02 32 148 3 12.841 0.006 0.175 0.018 19 25 57.2 -10 16 07 -200 -37 3 12.866 0.010 0.487 0.013 19 26 24.8 -10 12 04 207 206 3 14.750 0.013 1.739 0.009 19 25 51.3 -10 15 16 -288 14 3 14.910 0.014 1.781 0.005 Notes: 1. Stars #1 and #2 are saturated and their magnitudes are approximate. The accurate magnitudes by Vogt (see table below) should be used for these two stars. 2. There is a photoelectric V sequence published on the AAVSO 'f' chart dated 12/1991. In addition Vogt measured three stars in this field (Publ. No. 8,VSS RASNZ, 1980). ID Henden AAVSO Vogt V V V 1 11.159 10.7 10.82 2 11.670 11.5 11.57 4 12.717 12.6 12.67 9 14.831 14.9 10 15.294 16.2 See note 3. 15.484 15.5 14 16.050 See note 3. 3. The AAVSO star 162 has been misplotted on the AAVSO chart. At this position there is a brighter star, star 10. The real position of 162 is at the location of star 14, some 25 arcsec to the east. 4. There is a bright Tycho-2 star south of this field at 19h 25m 58.4s -10d 21" 42" with a reliable magnitude of V=10.13+/-0.04. 5. The first ever detection of superhumps, with a period of 0.0805d, was made during the September 1991 superoutburst, proving the SU UMa-type nature of this dwarf nova (Nogami, et al. 1995, IBVS 4227) Thr variable isinvisible on the Downes and Shara (1993) identification chart. 6. Appears to be constant at minimum with a magnitude of V=18.2. Bruce Sumner Revised 29 July 1999