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tokens: to calculate N H values for all targets studied. For 1ES 0229+200, the calculated value of N is (13.00 ± 0.37) × 10 20 cm −2 . This value is larger than the one from the LAB survey (8.06 × 10 20 cm −2 ) and consistent with the one provided by Willingale et al. ( 2013 ,10.80 × 10 20 cm −2 ). The value is also higher than free N H = (10.6–10.8) × 10 20 cm −2 , calculated by Kaufmann et al. ( 2011 ). For PKS 0548−322, the calculated value of N is (3.10 ± 0.10) × 10 20 cm −2 . This value is larger than the one from the LAB survey (2.58 × 10 20 cm −2 ) and consistent with the one provided by Willingale et al. ( 2013 , 2.87 × 10 20 cm −2 ). However, Sambruna Mushotzky ( 1998 ) have found a significantly higher value of N H of 1.03 × 10 21 cm −2 , which is needed to explain X-ray properties of PKS 0548−322. For 1ES 1741+196, the calculated value of N is (10.47 ± 0.41) × 10 20 cm −2 . This value is larger than the one from the LAB survey (7.32 × 10 20 cm −2 ) and consistent with the one provided by Willingale et al. ( 2013 , 9.58 × 10 20 cm −2 ). For 1ES 2344+514, the calculated value of N is (17.34 ± 0.15) × 10 20 cm −2 . This value is larger than the one from the LAB survey (15.10 × 10 20 cm −2 ); however, it is smaller than the one provided by Willingale et al. ( 2013 , 24.60 × 10 20 cm −2 ). We note here that the reddening E ( B − V ) and the atomic hydrogen column density ( N H ) are related. According to recent work, Liszt ( 2014 ) has described this dependence by the following formula N H = 8.3 × 10 21 E ( B − V ). The formula gives N H values of 9.7 × 10 20 , 2.5 × 10 20 , 0.6 × 10 20 , 6.3 × 10 20 , and 15 × 10 20 for 1ES 0229+200, PKS 0548−322, RX J 1136+6737, 1ES 1741+196, and 1ES 2344+514, respectively. The quoted values are consistent with the ones from the LAB survey and do not indicate a need for an additional absorption. All values of N H values, including the catalogue ones, are collected in Table 5 . Table 5. Summary of Galactic column densities values. Notes . (1) Source name; (2)–(4) N H as provided by Kalberla et al. ( 2005 ), Dickey Lockman ( 1990 ), and Willingale et al. ( 2013 ), respectively; (6) N H value calculated as a result of this work. All values are given in 10 20 cm −2 . 4.2 Constrains on the model parameters The model used to describe the IR to X-ray emission of the blazars is characterized by the host galaxy, curvature seen in the X-ray spectrum, total absorption (which includes both Galactic component and possibly additional ones), and UV excess. The host galaxy, understood as the entire component described with the template by Silva ( 1999 ), is well constrained with the model used. Still, the remaining three parameters cannot be disentangled only using information from the X-ray spectral fitting. The limitations on three entangled parameters are as follows: β : For all of the blazars studied, the convex curvature of the X-ray spectrum is assumed. This implies that negative values of β are not accepted.