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Astron. Astrophys. 360, 637-641 (2000)

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2. Observations and the data collection

In order to achieve the coverage of the light curve as long as possible, we have made use of three sources of the photometric data, summarized in Table 1.


[TABLE]

Table 1. Sources of the photometric data used for the analysis


B93b published a table of their UBVRI photometry, collected during the COYOTES multi-site campaign for monitoring of T Tau stars. Their measurements were obtained with the photoelectric photometers and are given in the absolute magnitude scale. Usually one to four observations were secured within a single night, which allowed us to conclude that their scatter was not larger than 0.02 mag for a given night.

A set of CCD data was obtained at Brno Observatory within January-April 1998. V 1080 Tau was observed using Newton 400/1750 mm, equipped with the CCD camera SBIG ST-7. The variable, the comparison star (GSC 1834-299) and the check star (GSC 1834-412) were placed in the same image. Usually a series of 5-10 closely spaced images was secured each night and an average brightness was determined. The brightness of V 1080 Tau was given with respect to the comparison star. The typical standard deviation of this average was about 0.017 mag(R). The comparison and the check star were stable within [FORMULA] mag(R) through the whole season.

We also included a set of 69 observations obtained with the photometer onboard the Hipparcos satellite in the [FORMULA] passband (Perryman et al. 1997). The [FORMULA] filter has its maximum roughly between the V and B filter. These [FORMULA] data were used just for determination of the period.

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© European Southern Observatory (ESO) 2000

Online publication: August 17, 2000
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