... 33

Based on observations collected with the 1.83 m Cima-Ekar telescope of the Padova Astronomical Observatory and with the 1.52 m Cassini telescope of the Bologna Astronomical Observatory.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

...

Table 2 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/458/225

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... and C

J2000 coordinates of the target stars: GR 290:   $\alpha = 01$$^{\rm h}$35$^{\rm m}$09.71$^{\rm s}$,  $\delta = +30$$^{\circ}$41$^\prime$ 57.1 $^{\prime\prime}$;  Var A ([HS53] A):   $\alpha = 01$$^{\rm h}$32$^{\rm m}$32.52$^{\rm s}$,  $\delta = +30$$^{\circ}$30$^\prime$ 22.4 $^{\prime\prime}$;  Var B ([HS53] B):   $\alpha = 01$$^{\rm h}$33$^{\rm m}$49.23$^{\rm s}$,  $\delta = +30$$^{\circ}$38$^\prime$ 09.1 $^{\prime\prime}$;  Var C ([HS53] C):   $\alpha = 01$$^{\rm h}$33$^{\rm m}$35.12$^{\rm s}$,  $\delta = +30$$^{\circ}$36$^\prime$ 00.4 $^{\prime\prime}$;  UIT3 ([MBH96] 3):   $\alpha = 01$$^{\rm h}$32$^{\rm m}$37.70$^{\rm s}$,  $\delta = +30$$^{\circ}$40$^\prime$ 05.7 $^{\prime\prime}$.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... procedures

IRAF is distributed by the NOAO, which is operated by AURA under contract with NSF.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

... system

In the calibration diagrams we found for the B and V magnitudes reported by Ivanov et al. (1993) a dispersion larger than for those of Sandage & Johnson (1974). This can be attributed either to a photometric variability of the Ivanov et al. stars and/or to their larger measurement errors. We also note that in SIMBAD the star IFM-B33a of the Ivanov et al. catalogue has the same coordinates as the Sandage-Johnson standard A14, which is one magnitude brighter, and we have found that the last value is the right one.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.

...-band

In our B and V observations the images of Var C are elongated to the West due to the presence of a much fainter, and probably redder, star separated by about 2 arcsec, whose contribution to the B and V mag of Var C is small.

.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.