Empirical relations for cluster RR Lyrae (Kovacs+, 2001)

Computer Science

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Photometry, Stars: Horizontal Branch, Stars: Variable, Surveys

Scientific paper

This table (referred to as Table 2 in the above paper) consists of 4 subtables. They all contain (with the same format) the Fourier decompositions of fundamental mode RR Lyrae stars and color index averages (B-V and V-I, where I denotes the Kron-Cousins system). All averages are computed as averages of the observed magnitudes. Fourier decompositions refer to a *sine* series, given by the following expression V(t) = A0 + A1*sin[2*pi*(t-t0)*1*f0+phi1_] + A2*sin[2*pi*(t- t0)*2*f0+phi2] + ... The epoch t0 is set to zero for all stars. The Fourier decompositions are devoted to describe the form of the light curves and can not be used for predicting light curves, because of the various truncations used in the Julian Dates of the individual stars (e.g., t=HJD-2400000, etc). The structure of the data for each variable is as follows: Period Epoch A0 N sigma Cluster Color-index A1 phi1 ... A15 phi_15 Here *N* is the number of the data points used in the calculation of the Fourier decomposition, *sigma* is the standard deviation of the residuals of the fit, *Cluster* and *color index* are absent in file *fieldv.dat*, *color index* is absent in *clusv.dat*. In general, 15th order Fourier fit was used. Exact zero amplitudes and phases show where the order was lower than this. References to the data used in computing the Fourier decompositions and color averages, can be found in the above paper and references therein. Exceptions are variables from FW Lup down to the end of the file *fieldv.dat*, where the data were taken from various publications, including those of Lub (1977A&AS...29..345L), Layden (1997, Cat. ) and Schmidt & Seth (1996, Cat. ). (6 data files).

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