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[vsnet-campaign 480] V446 Her sequence
The current VSNET campaign on V446 Her might benefit from an
accurate comparison star sequence. Such a sequence follows.
Visual observers only need use the stars listed in Part a.
Regards,
Bruce Sumner
---------------
156 V446 HERCULIS (NA) Range: 2.8-18.8p
Position: 18 57 21.61 +13 14 28.9 (J2000, from .dat file)
Magnitude: V=16.121 B-V=0.472 (from .dat file)
ID RA (2000) DEC X Y N V ERR B-V ERR
a) Comparison star sequence
1 18 57 31.2 +13 16 46 139 137 7 12.518 0.054 1.282 0.075
2 18 57 23.6 +13 13 16 30 -73 7 12.586 0.045 0.614 0.053
3 18 57 09.4 +13 16 11 -178 102 7 13.236 0.016 0.891 0.013
4 18 57 02.7 +13 12 11 -276 -138 7 13.419 0.014 1.213 0.015
5 18 57 40.2 +13 17 11 271 162 7 13.777 0.019 0.526 0.012
6 18 57 22.8 +13 14 17 18 -13 7 14.048 0.019 0.941 0.018
7 18 57 15.7 +13 15 11 -86 42 7 14.459 0.011 0.872 0.017
8 18 57 26.4 +13 14 53 70 24 7 15.173 0.022 0.878 0.011
9 18 57 20.9 +13 14 13 -10 -16 7 15.693 0.015 2.132 0.058
10 18 57 20.4 +13 13 55 -18 -34 7 16.103 0.019 1.674 0.029
11 18 57 17.3 +13 13 46 -63 -43 7 16.506 0.032 1.868 0.080
12 18 57 27.1 +13 14 17 81 -12 7 17.414 0.043 1.270 0.036
13 18 57 20.2 +13 14 20 -20 -9 7 18.028 0.073 1.459 0.379
b) Wide-colour extension for CCD calibration
18 57 37.9 +13 09 38 238 -291 5 12.947 0.016 0.492 0.014
18 57 25.1 +13 08 56 51 -333 4 14.329 0.017 0.499 0.010
18 57 44.6 +13 10 55 336 -214 2 12.511 0.058 0.519 0.058
18 57 15.2 +13 16 13 -93 104 7 14.263 0.013 2.272 0.021
18 57 38.7 +13 17 13 249 164 7 14.511 0.027 2.295 0.023
18 57 31.8 +13 13 02 150 -87 7 13.319 0.011 2.333 0.015
Notes:
1. Stars 1 and 2 are saturated, and their magnitudes should be used
for guidance only.
2. There is a photoelectric sequence of some of the brighter stars in
this field in a paper by Stienon, PASP,75,45S,1963. The stars common
to the two sequences are:
Henden Stienon
Star V B-V V B-V
1 12.518 1.282 12.49 1.46
2 12.586 0.614 12.65 0.61
3 13.236 0.891 13.31 0.91
4 13.419 1.213 13.46 1.39
3. The bright star HD 175959 is located only 1.7 arcmin north of the
variable. It was measured by Stienon as follows: V=8.90 B-V=1.55.
4. This field is predominantly populated with red stars, and it is
impossible to create a sequence composed of stars of similar colour.
Observers should be aware that the bright half of this sequence are
mostly blue stars, whereas the fainter half of the sequence are
mostly red stars.
5. V446 Her is the NE optical member of a very tight quadruple
cluster of 18 and 19 magnitude stars, all located inside a circle of
5 arcsec diameter. Magnitudes of the individual components will be
reported later.
Bruce Sumner
6 September 2000
vsnet-adm@kusastro.kyoto-u.ac.jp
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