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[vsnet-sequence 199] ROTSE3 J0151 sequence



ID:  ROTSE3 J015118.59-022300.1 Type: CV  Range: 14.6V-<20.1V
Position:  01 51 18.60 -02 23 00.4 (J2000, from .dat file)
Magnitude:  V=20.698  B-V:+0.026
Sequence:  CCD(V) A. Henden & M. Simonsen

a) Comparison star sequence

ID   RA            DEC         N    V      ERR    B-V     ERR    U-B     ERR
V-R     ERR    R-I     ERR

1    01 51 44.09  -02 18 51.0  1  12.775  0.000  +0.497  0.000  NULL    NULL
+0.419  0.000  +0.373  0.000
2    01 51 42.39  -02 25 55.5  1  13.133  0.000  +0.849  0.001  NULL    NULL
+0.489  0.000  +0.472  0.001
3    01 51 06.00  -02 23 58.0  2  13.413  0.006  +0.751  0.023  NULL    NULL
+0.409  0.004  +0.363  0.004
4    01 51 14.93  -02 20 40.7  2  13.561  0.006  +0.661  0.021  NULL    NULL
+0.359  0.006  +0.333  0.009
5    01 51 20.28  -02 15 46.2  1  14.351  0.001  +0.800  0.001  NULL    NULL
+0.472  0.001  +0.436  0.001
6    01 51 21.46  -02 26 15.2  2  14.562  0.008  +0.863  0.018  NULL    NULL
+0.475  0.003  +0.451  0.005
7    01 51 22.05  -02 24 10.9  2  14.753  0.006  +0.555  0.024  NULL    NULL
+0.322  0.006  +0.345  0.002
8    01 51 16.62  -02 20 16.7  2  14.994  0.006  +0.852  0.018  NULL    NULL
+0.465  0.011  +0.414  0.008
9    01 51 38.76  -02 20 41.5  2  15.681  0.022  +0.927  0.010  NULL    NULL
+0.547  0.021  +0.505  0.006
10   01 51 43.13  -02 20 49.0  1  16.053  0.002  +0.918  0.004  NULL    NULL
+0.543  0.003  +0.474  0.004
11   01 51 33.98  -02 23 55.7  2  16.811  0.011  +0.692  0.018  NULL    NULL
+0.411  0.006  +0.410  0.011
12   01 51 43.15  -02 22 45.9  1  17.099  0.005  +0.671  0.008  NULL    NULL
+0.367  0.008  +0.369  0.010
13   01 51 00.92  -02 24 54.8  2  17.892  0.019  +0.788  0.040  NULL    NULL
+0.474  0.021  +0.442  0.015
14   01 51 17.46  -02 23 44.5  2  18.014  0.008  +0.771  0.035  NULL    NULL
+0.421  0.016  +0.415  0.004
15   01 51 23.83  -02 22 12.2  2  18.548  0.001  +0.625  0.005  NULL    NULL
+0.417  0.001  +0.425  0.028

Notes:

a)  Note that labeled comparison stars above magnitude 12.5 may be in error
due to camera saturation.  Consider these stars suspect until further
photometry can be done.

Vance Petriew
Revised 10 November 2002


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