39.  V844 HERCULIS   (UGSU)   Range: 12.1-17.8V
     Position:   16 25 01.77  +39 09 27.0 (J2000, from .dat file)
     Magnitude:  V=17.771  B-V=-0.155     (Henden, single night)

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

a) Comparison star sequence

1    16 25 21.1  +39 12 24   224  177  1  10.622  0.013   1.095  0.011  
2    16 24 51.3  +39 12 08  -122  161  3  12.334  0.012   0.662  0.004  
3    16 25 22.8  +39 14 40   244  313  5  12.515  0.015   1.071  0.019  
4    16 25 13.2  +39 08 50   132  -37  5  12.836  0.011   0.994  0.012   
5    16 24 53.9  +39 05 28   -92 -240  5  13.496  0.017   0.689  0.006   
6    16 25 17.4  +39 08 56   182  -31  5  13.611  0.009   1.003  0.008   
7    16 24 57.2  +39 09 56   -53   29  5  14.086  0.011   0.638  0.007   
8    16 25 01.1  +39 11 14    -8  107  4  14.995  0.010   0.687  0.007   
9    16 25 14.7  +39 10 10   150   43  4  15.288  0.008   1.535  0.012   
10   16 25 04.2  +39 13 34    27  247  4  15.640  0.012   0.469  0.008   
11   16 25 16.2  +39 07 53   167  -94  4  15.702  0.011   0.732  0.009   
12   16 24 57.2  +39 09 40   -54   13  4  16.862  0.018   0.516  0.008   
13   16 24 57.5  +39 09 14   -50  -12  4  17.277  0.009   1.481  0.018   
14   16 24 53.3  +39 09 36   -99    9  4  18.278  0.029   0.510  0.029   


b) Wide-colour extension for CCD calibration

     16 24 34.5  +39 05 32  -318 -235  4  16.278  0.014   0.510  0.008   


Notes:

1. This is a recently discovered UGSU-type dwarf nova, the discovery of 
which was announced in IBVS 4360, where the variable was called var43 Her.

2. There is a Preliminary AAVSO 'e' chart dated 06/1997, with six PEP(V)
magnitudes included. These magnitudes are from S. Antipin (IBVS 4360). 
Five of the magnitudes are common to both sequences:

                         ID   Henden  AAVSO  Antipin

                         2    12.334   13.1   13.14
                         3    12.515   13.8   13.86	
                         4    12.836   14.1   14.10
                         7    14.086   14.9   14.92
                         8    14.995   16.2   16.15

3. Antipin's (and hence the AAVSO) magnitudes are 1 magnitude or more 
fainter than those derived here. This results from Antipin's magnitudes 
being misinterpreted as V magnitudes, when it fact they are photographic 
magnitudes derived from photographic plates taken in Crimea and now in 
the Moscow plate collection. In actual fact Antipin's magnitudes are 
closely related to B magnitudes.

4. Superhumps were detected by Vanmunster 1999, vsnet-obs 4075, showing 
this to be a SU UMa-type dwarf nova. 

5. Varies at minimum between about V=17.5 and V=17.8.



Bruce Sumner
Revised 9 July 1999
Revised AAH 5 October 1999