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Table 1

Results of the spectral fit parameters obtained from the average EPIC+ISGRI spectra of IGR J08262−3736 (see Sect. 3.1).

Model NH Γ NHb f k TBB RBB F0.5−2   keV F2−10   keV F20−40   keV CMOS1 (CMOS2) CISGRI /d.o.f.

1 1.4  ±  0.1 1.52  ±  0.05 0.10  ±  0.01 132 16.0 6.0 4.0 1.03  ±  0.03 (1.01  ±  0.03) 0.7  ±  0.2 1.1/380
0.60  ±  0.07 1.3  ±  0.1 1.2  ±  0.2 0.18  ±  0.03 1.0 5.3 3.6 1.00  ±  0.03 (1.00  ±  0.03) 0.6 0.9/380
2 0.80  ±  0.06 1.8  ±  0.1 3.8  ±  0.7 0.63  ±  0.04 4.5 6.5 4.4 1.00  ±  0.03 (1.00  ±  0.03) 1.2  ±  0.4 0.9/380

Notes. The leftmost column indicates the spectral model used in Xspec. Model 1 is phabs*(BB+pow), model 2 is phabs*pcfabs*pow (phabs is the absorption component, pow the powerlaw, BB the blackbody, and pcfabs the partial covering). We indicated with Γ the power-law photon index, NH the absorption column density in units of 1022 cm-2, f the covering fraction in the partial covering model (the local absorption component is indicated with NHb in units of 1022 cm-2), and kTBB (RBB) the temperature (radius) of the BB component in keV (km). For RBB we considered a source distance of 6.1 kpc (see Sect. 1). For the model that includes the BB component (Model 1), we report both the best fit values obtained with a hotter (kT ~ 1 keV) and colder (kT ~ 0.1 keV) emitting surface. We also reported the normalization constants CMOS1, CMOS2, and CISGRI for the MOS1, MOS2 and ISGRI spectra, respectively (we fixed the EPIC-pn constant to 1 as a reference). The unabsorbed fluxes (units of 10-12 erg/cm2/s) in the 0.5–2 keV, 2–10 keV, and 20–40 keV are indicated in all cases with F0.5−2   keV, F2−10   keV, and F20−40   keV, respectively.

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