93   AW SAGITTAE   (UGSU)   Range: 13.8-19.32 
     Position:   19 58 37.08  +16 41 28.5 (Henden, June 1999)
     Magnitude:  V=19.221  B-V=0.024      (Henden, June 1999)

ID     RA (2000)    DEC       X    Y   N    V      ERR     B-V    ERR     

a) Comparison star sequence

1    19 58 20.6  +16 43 59  -236  151  3  11.050  0.137   0.546  0.022   
2    19 58 38.8  +16 41 42    25   14  3  11.977  0.017   0.288  0.003   
3    19 58 35.0  +16 44 11   -30  163  3  12.196  0.029   1.001  0.016   
4    19 58 36.1  +16 42 43   -14   75  4  13.223  0.019   0.526  0.023   
5    19 58 48.3  +16 41 26   160   -2  3  13.770  0.023   0.838  0.020   
6    19 58 35.7  +16 40 49   -21  -39  3  13.952  0.027   1.384  0.033   
7    19 58 39.8  +16 43 37    39  129  3  14.228  0.026   1.297  0.035   
8    19 58 27.4  +16 41 40  -139   12  3  14.692  0.022   1.221  0.034   
9    19 58 46.7  +16 39 42   138 -106  3  15.011  0.016   0.673  0.065   
10   19 58 40.5  +16 40 54    49  -34  3  15.348  0.031   0.758  0.031   
11   19 58 31.5  +16 40 59   -80  -29  3  15.639  0.031   0.819  0.028   
12   19 58 40.3  +16 41 06    46  -22  3  16.040  0.020   1.105  0.048   
13   19 58 35.4  +16 41 12   -25  -16  3  16.438  0.034   0.781  0.021   
14   19 58 33.4  +16 41 12   -54  -16  3  17.279  0.087   0.883  0.015   
15   19 58 34.8  +16 41 24   -33   -4  3  17.770  0.045   1.251  0.411   

 
b) Wide-colour set for CCD calibration

     19 58 45.1  +16 40 28   115  -60  3  14.804  0.026   0.422  0.034   
     19 58 52.6  +16 47 25   223  357  3  12.820  0.028   0.450  0.016   
     19 58 18.5  +16 39 51  -268  -97  3  13.715  0.015   1.720  0.032   
     19 58 50.0  +16 37 59   185 -209  3  14.056  0.039   1.801  0.021   


Notes:

1. Star #1 is saturated and should be used with care. It is probably 
about 0.2 magnitude too bright. 

2. The coordinates and magnitude of AW Sge were determined from 
co-added photometry obtained by Henden in June 1999.

3. There are two bright stars just outside the field of this photometry.
They both have accurate Tycho-2 photometry. One is in the southwest 
corner and has a magnitude of V=9.41, and the other on the western 
edge has a magnitude of V=9.64.

4. Superhumps were detected for the first time in July 2000 (Masi 2000, 
vsnet-chat 5111), verifying this as another SU UMa-type dwarf nova. 
The identification chart in Downes and Shara (1993) of this extremely 
crowded field makes positive identification of the variable difficult. 

5. Minimum of V=19.2 found from a single image.


Bruce Sumner
27 June 1999
Revised 7 December 2000