2 Observations

In order to obtain the correct pulsation frequencies of HR 5437 and study its character we observed this star from 9 to 17 April 1997 and on March 6, 1998 using the 85 cm telescope at the Xinglong Station of Beijing Astronomical Observatory. The 4-channel photometer (Michel & Chevreton 1991) with Strömgren v filter was used. The star SAO 16408 was used as comparison, and SAO 16394 was used as check star. The three stars and sky background were observed simultaneously. The integration time was one minute. The value of each data point is the magnitude difference (HR 5437 - SAO 16408) normalized to zero. No evidence for any variability of SAO 16408 was found, but SAO 16394 was discovered unexpectedly to be a new $\delta$ Scuti star (Liu et al. 1998). The measuring error is about 3 mmag. Seven tracks of data were obtained for HR 5437 from 1997 to 1998 covering a period of 332 days. The observing log is given in Table 1, where time duration is the length of observational run (in days) during each night, point number is the amount of data points during each night.

  

Table 1: Observing log of HR 5437 (1997-1998)