All Tables

Table 1: The INTEGRAL Data set. We selected all public and core programme revolutions when IGR J17252-3616 was within the ISGRI PCFOV of $29\hbox {$^\circ $ }\times 29 \hbox {$^\circ $ }$ . The observing time fraction was calculated as the ratio between the net exposure time on the source and the elapsed time during the visibility periods.
Table 2: Spectral analysis. The EPIC and ISGRI spectra were fitted together. Two models in Xspec were selected to fit the data. Model CPL is constant*wabs(bbody+vphabs(cutoffpl+gaussian)) and model CTT is constant*wabs(bbody+vphabs (compTT+gaussian)). The galactic absorption $N_{\textrm{\tiny H}}^{\textrm{\tiny gal}}$ was fixed. The errors are calculated at the 90% confidence level.
Table 3: Phase-resolved spectral analysis. We used the CTT model. All continuum and normalisation parameters were left free. A few parameters were fixed as for the average spectrum (see Table 2): $N_{\textrm{\tiny H}}^{\textrm{\tiny gal}}=1.5\times10^{22}\ \textrm{cm}^{-2}$ , $kT_{{\rm soft}}=0.5\ {\rm keV}$ , $kT_{0}=0.1\ {\rm keV}$ . Only pn data were used for the phase-resolved spectral analysis.
Table 4: Phase-resolved spectroscopy with all the spectral modeling parameters of model CTT except normalisations equal to the values of the average spectrum (see Table 2). Only pn data were used for the phase-resolved spectral analysis.