[vsnet-chat 2586] TmzV85 sequence updated

["Bruce Sumner" <b.sumner@bom.gov.au>]

Dear observers,

Here is a corrected sequence for this variable, based on field
photometry obtained by Arne Henden. 

     TmzV85   (UG)   Range: 13.518.4V
     Position:   10 43 56.87  +58 07 32.5 (J2000, Yamaoka)
     Magnitude:  V=18.381   V=0.173        (Henden)

ID      RA  (2000)  DEC       X    Y  N    V      ERR     BV    ERR 

1   10 44 38.6  +58 03 33   332 -240  2  12.292  0.006   0.850  0.005
2   10 43 32.9  +58 11 43  -189  249  2  13.262  0.006   0.213  0.004
3   10 43 44.4  +58 06 08   -98  -85  2  13.556  0.006   0.919  0.006
4   10 44 34.7  +58 08 22   300   49  2  14.245  0.000   0.840  0.007
5   10 44 38.7  +58 08 23   332   50  2  14.667  0.006   0.797  0.003
6   10 43 38.4  +58 09 15  -145  102  2  15.582  0.008   0.576  0.006
7   10 44 21.4  +58 02 56   195 -277  2  16.548  0.000   0.532  0.011
8   10 44 18.9  +58 04 18   175 -195  2  17.166  0.023   0.569  0.045
9   10 43 54.3  +58 07 11   -20  -22  2  17.633  0.037   1.145  0.027
10  10 44 04.3  +58 07 43    59   10  2  17.844  0.016   0.620  0.136
11  10 43 28.5  +58 05 43  -224 -110  2  18.607  0.033   0.345  0.120 

Notes:

The position is from Yamaoka, (vsnet-alert 4059) and the quiescent
magnitude is from Henden (vsnet-alert4060). These two messages 
confirm that TmzV85 is the SW component of a very close double. In 
fact Henden suggests that the NE component is a very faint background 
galaxy. 

There are large errors in the B-V values of the two faintest 
comparison stars, so take care if you need to use these values.

Bruce Sumner
21 January 2000

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