264  GK PERSEI   (Na+XP)   Range: 0.2-14.0V
     Position:   03 31 12.01  +43 54 15.9 (J2000, from .dat file)
     Magnitude:  V=12.966  B-V=0.944      (in .dat file)

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

a) Comparison star sequence

1    03 30 47.7  +43 52 50  -263  -86  3  12.217  0.000   0.689  0.007   
2    03 30 53.4  +43 56 19  -201  123  3  12.572  0.006   0.558  0.004   
3    03 31 32.5  +43 55 53   221   97  3  13.162  0.005   0.792  0.010   
4    03 31 25.3  +43 55 27   143   71  3  13.191  0.006   0.914  0.006   
5    03 31 26.3  +43 53 06   155  -70  3  13.339  0.010   1.207  0.010   
6    03 30 56.7  +43 55 30  -165   74  3  13.561  0.009   0.909  0.012   
7    03 31 20.5  +43 53 31    92  -45  3  13.666  0.005   0.793  0.005   
8    03 31 06.1  +43 52 31   -64 -105  3  13.711  0.005   0.779  0.009   
9    03 30 54.8  +43 51 21  -186 -175  3  13.955  0.005   0.574  0.004   
10   03 31 33.1  +43 56 25   228  129  3  13.980  0.008   0.797  0.007   
11   03 30 55.7  +43 50 21  -176 -235  3  14.066  0.010   0.937  0.012   


b) Wide-colour extension for CCD calibration

     03 30 51.2  +43 50 24  -225 -232  3  12.476  0.005   0.390  0.005   
     03 30 59.5  +43 55 49  -136   93  3  14.011  0.015   1.530  0.014   
     

Notes:

1. There are several bright stars in this field. The four brightest are
from Tycho-2, as follows:

             RA  (2000)   Dec       V           B-V
            03 32 05.1 +43 40 12   8.61+/-0.02  0.67
            03 30 51.5 +43 59 06   9.07+/-0.02  0.29
            03 31 56.0 +44 02 45   9.69+/-0.03  1.28
            03 30 06.9 +43 57 50  10.30+/-0.04  1.04

2. There is an AAVSO d chart dated March 1996 with a V sequence.
Correspondencies between the two sequences follow:

         ID     Henden    AAVSO
          2     12.572     126
          3     13.162     132
          4     13.191     132
          5     13.339     135
          6     13.561     136
          7     13.666     137
          8     13.711     137
          9     13.955     139
         10     13.980     138
         Red    14.011     139

3. There are two stars in this sequence with a magnitude of 132 and two
others with a magnitude of 137. Only one of each should be retained in a
final sequence.


Bruce Sumner
5 March 2002