Coefficients for KYNEBBRR model

The tables attached contain coefficients A', B', C', D' for polynomial approximations of polarization degree versus energy computed for X-ray single-temperature blackbody radiation passing through a passive constant-density slab. The models were originally computed with TITAN (Dumont et al., 2003) and STOKES (Goosmann and Gaskell, 2007) codes. The details of the modelling with full description of these tables are given in the doctoral thesis Podgorný (2023) and in less detail in Ratheesh et al. (2023). The method and origins date back to Taverna et al. (2021). Once computed in high energy resolution in the limit of high ionization, the polarization degree versus energy was smoothed at 1-9 keV range and at 9-20 keV range, using y = A'x^3 + B'x^2 + C'x + D'.Usage:First unzip the main file. Then each table in the main directory contains in the 1st column a value of cosine of the emission angle measured from the disc normal. In the 2nd to 5th column values of the coefficients A', B', C', D' obtained by the Python numpy.polyfit routine in the 1-9 keV range. The same for 9-20 keV range is in the 6th to 9th columns. Each table is called "n18", according to the n_H = 10¹⁸ cm^-3 density used and then with "xiBB", suggesting the blackbody normalization of the illumination in photoionization equlibrium. Then the number after "T" in the name of each file sets the single-temperature value of the blackbody in keV, i.e. 0.50 keV, 0.80 keV, 1.15 keV, or 1.40 keV. Last number in the file name after "tau" is the total Thomson optical depth, given by the slab height in STOKES, i.e. 0.2, 0.4, 0.67, 1, 1.3, 1.5, 2, 3, 5, 7, or 10 values. As such, the tables are ready to use inside the KYNEBBRR routine, which integrates them accross the accretion disc, taking into account all relativistic effects. This routine is part of the KY codes (Dovčiak et al. 2004, 2011, Taverna et al. 2020, Mikušincová et al. 2023), which are suitable for fitting with XSPEC (Arnaud, 1996).