Abstract
Table obssum.dat contains an observing summary for all pulsars in the LOFAR census sample. DM measurements and mean flux densities in 110-188MHz frequency range are listed for 158 detected sources. For the non-detected pulsars the upper limits on mean flux density values are given. Spectral fits for 165 pulsars with flux densities measured at more than one frequency (census or literature) are presented in table1pl.dat (a single power-law spectral model, 1PL), table2pl.dat (a power-law with one break, 2PL) or in table3pl.dat (2 breaks, 3PL). For 1PL models, the measured flux density values were modeled as random variables, normally distributed in base 10 log space with mean<SUB>lgS=lg(S0)+a*lg(f/f0) and dispersion sigma</SUB>lgS. For the spectra consisting of small number of measurements, sigma_lgS was set by the reported flux density errors. For the spectra consisting of larger number of measurements, an additional scatter (sigma<SUB>unkn</SUB>lgS) was added in quadrature to sigma_lgS and fitted for. This additional parameter represents intrinsic flux variability or any kind of unaccounted propagation or instrumental error. For 2PL models, mean_logS was defined as lg(S0)+(alo)*lg(f/f0) for f<fbr and as lg(S0)+(ahi)*lg(f/fbr)+(alo)*lg(fbr/f0) for f>fbr. For 3PL models mean_lgS was modified accordingly. A 2PL or 3PL model was preferred over a 1PL model in the cases where either of the former gave a significantly smaller sigma<SUB>unkn</SUB>lgS. (5 data files).
