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Home All issues Volume 498 / No 1 (April IV 2009) A&A, 498 1 (2009) 233-240 Full HTML
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Table 2:

X-ray spectral analysis of INS candidate XMM J1046.
  Absorbed blackbody fit Constant $N_{\rm H}$
OBSID Detector $N_{\rm H}$ kT $f_{\rm X,14}$ C d.o.f. Goodness kT C d.o.f. Goodness
    (1021 cm-2) (eV) (erg s-1 cm-2)     (%) (eV)     (%)
112580601 M1 $3.7^{\rm +1.4}_{-1.1}$ $132^{\rm +16}_{-17}$ 10.4(8) 19 21 43.7 134(5) 19 20 40.6
112580701 M1 $3.8^{\rm +2.2}_{-2.1}$ $124^{\rm +35}_{-23}$ $11.6^{\rm +1.5}_{-1.4}$ 15 21 11.2 $128_{-8}^{\rm +9}$ 15 20 12.6
160160101 M2 $5.6^{\rm +3 }_{-2.3}$ $103^{\rm +26}_{-21}$ $ 9.9^{\rm +1.1}_{-1.0}$ 19 13 81.6 $125_{-6}^{\rm +7}$ 20 12 87.2
160160901 M1/M2 $3.1^{\rm +0.8}_{-1.0}$ $132^{\rm +17}_{-12}$ 10.3(6) 25 32 13.1 126(4) 25 31 16.0
145780101 M1 $2.7^{\rm +2.2}_{-2.0}$ $124^{\rm +43}_{-26}$ $12.9^{\rm +1.7}_{-1.6}$ 15 24 3.6 $114_{-7}^{\rm +8}$ 16 23 4.0
160560101 M2 $5.9^{\rm +2.6}_{-4}$ $96^{\rm +45}_{-23}$ 11.5(1.2) 34 37 25.0 $121_{-6}^{\rm +7}$ 35 36 25.7
160560201 M1/M2 $1.4^{\rm +1.1}_{-0.9}$ $160^{\rm +28}_{-23}$ 11.6(9) 53 42 79.5 122(5) 56 41 88.8
160560301 M1/M2 $6.0^{\rm +2.3}_{-1.1}$ $ 92^{\rm + 9}_{-14}$ $10.5^{\rm +0.7}_{-0.8}$ 33 30 44.9 $115_{-3}^{\rm +4}$ 37 32 65.9
206010101 pn $4.0^{\rm +1.2}_{-1.0}$ $106^{\rm +14}_{-12}$ 9.0(6) 35 26 86.7 112(4) 35 25 89.1
311990101 pn/M2 $3.9^{\rm +0.7}_{-0.5}$ 122(8) 10.1(3) 62 65 38.1 127(2) 63 64 43.0
9488 ACIS-I $6.3^{\rm +0.7}_{-1.2}$ $103^{\rm +9}_{-8}$ 7.8(3) 13 20 12.9 $125_{-3}^{\rm +4}$ 18 18 37.7
Note: Only the set of 10 best XMM-Newton observations (see text) and the Chandra one are shown. The best fit parameters (derived using the maximum likelihood C statistic) listed are for an absorbed blackbody model for which all parameters were allowed to vary freely (middle column). The right column shows the blackbody temperatures obtained when the column density is held constant at the mean value, $N_{\rm H}=3.5\times10^{21}$ cm-2. Errors are 1$\sigma $. The observed flux $f_{\rm X,14}$ refers to ranges 0.15-3 keV and 0.5-3 keV for XMM-Newton and Chandra data, respectively, in units of 10-14 erg s-1 cm-2. The ``goodness-of-fit'' is derived from 1000 Monte Carlo simulated spectra.

Source LaTeX | All tables | In the text

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