(6.5 $\pm$ 0.1) keV, and get $\chi^2$/$\nu$ = 32/25. A scattered power law is not required by the data (Figure \[fig:subfig2\]). The central source is then obscured by Compton-thick material of column density $N_{\rm H}$ = (5 $\pm$ 1) $\times$ 10$^{24}$ cm$^{-2}$. Best fit parameters are given in Table \[table:table\]. We note that our results are in agreement with @2015ApJ...805...41B, where they focused on the `Torus` model for a covering factor estimate.

### NGC 2273

The mass of the SMBH nested in the barred spiral galaxy NGC 2273 was measured by @2011ApJ...727...20K to be M$_{BH}$ = (7.5 $\pm$ 0.4) $\times$ 10$^6$ M$_{\odot}$. The reported parameters put the maser disk very close to the central engine (0.028 - 0.084 pc). This makes NGC 2273 an outlier in some relations [@2013MNRAS.436.3388C]. In order to determine whether it is truly an outlier or whether emission at larger radii is missed by the VLBI observations, we derive radii from the more sensitive single dish spectra taken with the Green Bank Telescope [@2011ApJ...727...20K]. To do so, we assume a systemic velocity of 1840 km/s (from NED[^4]), a SMBH mass of 7.5 $\times$ 10$^6$ M$_{\odot}$ [@2011ApJ...727...20K] and Keplerian rotation [@2011ApJ...727...20K]. From the highest and lowest velocity 