Mozdzierski et al., 2014, Acta Astronomica 64,89: 
A CCD Search for Variable Stars of Spectral Type B
in the Northern Hemisphere Open Clusters. IX. NGC 457

Table with positions and photometry of stars in the open cluster NGC 457
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Columns contain the following entries:

(1): Star number in the WEBDA database; '-' if a star is not listed in WEBDA.
     Note: There are duplicate star numbers for some stars in WEBDA. 
     The number given in this column usually comes from the oldest 
     numbering system incorporated in WEBDA. There are three differences in numbering 
     with respect to those given in Table 3 of the paper:
     Star at (1 19 41.30   +58 17 27.4) is star no. 1 (6166 in the paper)
     Star at (1 19 37.35   +58 15 41.9) is star no. 18 (3233 in the paper)
     Star at (1 19 25.11   +58 15 58.1) is star no. 47 (6798 in the paper)

(2),(3),(4): Right ascension (epoch J2000.0) in hours, minutes and seconds.
(5),(6),(7): Declination (epoch J2000.0) in degrees, arcmin and arcsec.
(8): I_c magnitude; '---' if not available.
     Note: The I_c magnitudes were also derived for some faint stars that had 
     no instrumental magnitudes in V. Given the small color term in the
     transformation to I_c, a mean color corresponding to the color for 
     low main-sequence members of NGC 457 was assumed. The I_c magnitudes 
     derived in this way are given with an accuracy of 0.001 mag, the remaining
     ones, with an accuracy of 0.0001 mag.
(9): Uncertainty of the I_c magniutude; '---' if not available.
     Note: the uncertainty does not include transformation errors.
(10): V magnitude; '---' if not available.
(11): Uncertainty of the V magniutude; '---' if not available.
(12): B magnitude; '---' if not available.
(13): Uncertainty of the B magniutude; '---' if not available.
(14): Alpha index; '---' if not available.
(15): Uncertainty of the alpha index; '---' if not available.
(16): Alpha' index; '---' if not available.
(17): Uncertainty of the alpha' index; '---' if not available.

General notes:
1. For some faint stars we provide coordinates, but do not provide photometry.
This is due to the fact that they were detected in a sufficient number of frames to derive 
reliable coordinates, but their photometry was too poor to be reliable.

2. The following transformation equations were used to get the BVI_c magnitudes provided 
   in the table:
New Bialkow observations (run 3, 2010-2011, designations as in the paper):
   B = b + (0.200 +/- 0.008)*(b-v) + (13.8662 +/- 0.0023)
   V = v + (-0.058 +/- 0.004)*(v-i_c) + (13.4881 +/- 0.0022)
   I_c = i_c + (-0.071 +/- 0.006)*(v-i_c) + (12.9794 +/- 0.0030)

Old Bialkow observations (run 2, 1999-2002):
   V = v + 0.0703 + 0.2951
   (V-I_c) = 1.0685*(v-i_c) + 1.1360
   (B-V) = 1.1391*(b-v) + 16.6189
(The photometry based on old Bialkow observations is provided only for stars from 
 outside the field covered in run 3.)