127 TT CRATERIS (UG) Range: 12.7-15.8V Position: 11 34 47.20 -11 45 30.0 (J2000, from .dat file) Magnitude: V=15.843 B-V=0.627 (Henden, single night) ID RA (2000) DEC X Y N V ERR B-V ERR a) Comparison star sequence 1 11 34 25.6 -11 47 30 -317 -120 3 10.643 0.016 1.023 0.010 2 11 34 41.6 -11 48 10 -83 -160 3 12.570 0.015 0.753 0.003 3 11 34 46.7 -11 46 12 -8 -42 3 13.171 0.020 0.636 0.010 4 11 34 27.0 -11 41 24 -296 246 3 13.478 0.013 0.648 0.009 5 11 34 34.9 -11 41 10 -180 260 3 14.150 0.014 0.519 0.014 6 11 34 26.4 -11 45 03 -305 27 3 14.399 0.010 1.029 0.014 7 11 34 50.0 -11 44 12 40 78 3 14.662 0.016 0.743 0.013 8 11 34 43.9 -11 48 42 -49 -192 3 15.248 0.019 0.916 0.015 9 11 34 30.4 -11 49 00 -246 -210 3 15.640 0.011 1.204 0.028 10 11 34 48.7 -11 48 54 22 -204 3 15.963 0.026 0.659 0.016 11 11 35 01.4 -11 44 28 208 62 3 16.400 0.036 0.967 0.025 12 11 34 34.5 -11 45 16 -187 14 3 16.803 0.013 0.681 0.030 13 11 34 37.3 -11 46 55 -146 -85 3 17.404 0.040 0.407 0.054 b) Wide-colour extension for CCD calibration 11 34 27.7 -11 40 25 -286 305 3 17.957 0.032 0.475 0.073 11 34 52.1 -11 42 13 71 197 3 16.744 0.040 1.435 0.070 11 34 42.0 -11 43 01 -76 149 3 16.430 0.020 1.505 0.106 Notes: 1 There is a photoelectric sequence for this variable derived by Pam Kilmartin (Kilmartin, Publ. VSS RASNZ, No. 16, 1991). Misselt (PASP, 108,1996) measured the same three stars as Kilmartin. In addition VSS RASNZ chart 909 has the same sequence letters as allocated by the discoverer of this variable, Richard Fleet. And the AAVSO preliminary chart dated 03/1991 has visual estimates, which are up to one magnitude too bright at the faint end of the sequence. ID Henden Kilmartin Misselt RASNZ/ AAVSO V B-V V B-V V B-V Fleet 2 12.570 0.753 12.64 0.7 12.617 0.786 A 12.3 3 13.171 0.636 13.21 0.5 13.196 0.667 B 12.7 7 14.662 0.743 14.4 0.7 14.681 0.783 E 12.7 8 15.248 0.916 F 14.2 10 15.963 0.659 G 15.0 2 Kilmartin also measured two additional Fleet comparison stars, namely C and D. These two stars do not form part of the current sequence, and are not necessary to form a complete sequence. However they are included here for completeness sake: RA (2000) DEC X Y Kilmartin RASNZ/ AAVSO V B-V Fleet 11 35 21.1 -11 54 05 497 -515 13.09 0.5 C 13.1 11 34 14.6 -11 47 27 -479 -117 14.2 1.3 D 13.5 3. This variable becomes redder as it fades to its quiescent magnitude, as shown by the colour of B=V=0.627 given above from a single measure when the variable was at minimum. Compare this to another single night measurement, when near maximum the variable was measued at V=13.422 and B-V=0.084, the blue colour being typical of a dwarf nova. Bruce Sumner Revised 7 June 1999