Table 1.
Open in new tab

Spectral fits of the diffuse X-ray emission in NGC 2359.

ModelkT1|$A_{1}^{a}$||$f_{1}^{b}$||$F_{1}^{b}$|kT2|$A_{2}^{a}$||$f_{2}^{b}$||$F_{2}^{b}$|χ2/d.o.f.
(keV)(cm−5)(cgs)(cgs)(keV)(cm−5)(cgs)(cgs)
A0.180|$^{+0.002}_{-0.002}$|2.26 × 10−34.2 × 10−141.2 × 10−12––––280.82/58.10 = 3.30
B0.175|$^{+0.002}_{-0.002}$|2.20 × 10−34.6 × 10−141.2 × 10−12––––249.20/84.19 = 2.96
C0.161|$^{+0.013}_{-0.010}$|2.70 × 10−33.5 × 10−141.2 × 10−124.6|$^{+3.2}_{-1.4}$|1.10 × 10−43.0 × 10−141.1 × 10−1384.13/83 = 1.01
D0.160|$^{+0.013}_{-0.011}$|2.72 × 10−33.6 × 10−141.2 × 10−124.5|$^{+3.2}_{-1.5}$|1.05 × 10−42.9 × 10−148.0 × 10−1483.09/82 = 1.01
E0.173|$^{+0.003}_{-0.018}$|2.04 × 10−33.5 × 10−141.1 × 10−124.9|$^{+2.4}_{-1.3}$|1.07 × 10−42.9 × 10−148.0 × 10−14125.92/135 = 0.93
Fc0.157|$^{+0.020}_{-0.011}$|3.60 × 10−33.7 × 10−141.6 × 10−124.8|$^{+2.2}_{-1.4}$|1.10 × 10−42.8 × 10−148.3 × 10−14125.47/134 = 0.94
ModelkT1|$A_{1}^{a}$||$f_{1}^{b}$||$F_{1}^{b}$|kT2|$A_{2}^{a}$||$f_{2}^{b}$||$F_{2}^{b}$|χ2/d.o.f.
(keV)(cm−5)(cgs)(cgs)(keV)(cm−5)(cgs)(cgs)
A0.180|$^{+0.002}_{-0.002}$|2.26 × 10−34.2 × 10−141.2 × 10−12––––280.82/58.10 = 3.30
B0.175|$^{+0.002}_{-0.002}$|2.20 × 10−34.6 × 10−141.2 × 10−12––––249.20/84.19 = 2.96
C0.161|$^{+0.013}_{-0.010}$|2.70 × 10−33.5 × 10−141.2 × 10−124.6|$^{+3.2}_{-1.4}$|1.10 × 10−43.0 × 10−141.1 × 10−1384.13/83 = 1.01
D0.160|$^{+0.013}_{-0.011}$|2.72 × 10−33.6 × 10−141.2 × 10−124.5|$^{+3.2}_{-1.5}$|1.05 × 10−42.9 × 10−148.0 × 10−1483.09/82 = 1.01
E0.173|$^{+0.003}_{-0.018}$|2.04 × 10−33.5 × 10−141.1 × 10−124.9|$^{+2.4}_{-1.3}$|1.07 × 10−42.9 × 10−148.0 × 10−14125.92/135 = 0.93
Fc0.157|$^{+0.020}_{-0.011}$|3.60 × 10−33.7 × 10−141.6 × 10−124.8|$^{+2.2}_{-1.4}$|1.10 × 10−42.8 × 10−148.3 × 10−14125.47/134 = 0.94

Notes:aThe normalization parameters is defined as |$A = 1\times 10^{-14}\int n_\mathrm{e}n_\mathrm{H}\mathrm{d}V/4 \pi d^{2}$|⁠, where d, ne, and V are the distance, electron density, and volume in cgs units, respectively.

bf and F represent the absorbed and unabsorbed fluxes. Fluxes are computed in the 0.3–2.0 keV energy range. All fluxes are in cgs units (erg cm−2 s−1).

cModel F was performed with a variable absorption column density. This model resulted in NH = 5.15 × 1021 cm−2.

Table 1.
Open in new tab

Spectral fits of the diffuse X-ray emission in NGC 2359.

ModelkT1|$A_{1}^{a}$||$f_{1}^{b}$||$F_{1}^{b}$|kT2|$A_{2}^{a}$||$f_{2}^{b}$||$F_{2}^{b}$|χ2/d.o.f.
(keV)(cm−5)(cgs)(cgs)(keV)(cm−5)(cgs)(cgs)
A0.180|$^{+0.002}_{-0.002}$|2.26 × 10−34.2 × 10−141.2 × 10−12––––280.82/58.10 = 3.30
B0.175|$^{+0.002}_{-0.002}$|2.20 × 10−34.6 × 10−141.2 × 10−12––––249.20/84.19 = 2.96
C0.161|$^{+0.013}_{-0.010}$|2.70 × 10−33.5 × 10−141.2 × 10−124.6|$^{+3.2}_{-1.4}$|1.10 × 10−43.0 × 10−141.1 × 10−1384.13/83 = 1.01
D0.160|$^{+0.013}_{-0.011}$|2.72 × 10−33.6 × 10−141.2 × 10−124.5|$^{+3.2}_{-1.5}$|1.05 × 10−42.9 × 10−148.0 × 10−1483.09/82 = 1.01
E0.173|$^{+0.003}_{-0.018}$|2.04 × 10−33.5 × 10−141.1 × 10−124.9|$^{+2.4}_{-1.3}$|1.07 × 10−42.9 × 10−148.0 × 10−14125.92/135 = 0.93
Fc0.157|$^{+0.020}_{-0.011}$|3.60 × 10−33.7 × 10−141.6 × 10−124.8|$^{+2.2}_{-1.4}$|1.10 × 10−42.8 × 10−148.3 × 10−14125.47/134 = 0.94
ModelkT1|$A_{1}^{a}$||$f_{1}^{b}$||$F_{1}^{b}$|kT2|$A_{2}^{a}$||$f_{2}^{b}$||$F_{2}^{b}$|χ2/d.o.f.
(keV)(cm−5)(cgs)(cgs)(keV)(cm−5)(cgs)(cgs)
A0.180|$^{+0.002}_{-0.002}$|2.26 × 10−34.2 × 10−141.2 × 10−12––––280.82/58.10 = 3.30
B0.175|$^{+0.002}_{-0.002}$|2.20 × 10−34.6 × 10−141.2 × 10−12––––249.20/84.19 = 2.96
C0.161|$^{+0.013}_{-0.010}$|2.70 × 10−33.5 × 10−141.2 × 10−124.6|$^{+3.2}_{-1.4}$|1.10 × 10−43.0 × 10−141.1 × 10−1384.13/83 = 1.01
D0.160|$^{+0.013}_{-0.011}$|2.72 × 10−33.6 × 10−141.2 × 10−124.5|$^{+3.2}_{-1.5}$|1.05 × 10−42.9 × 10−148.0 × 10−1483.09/82 = 1.01
E0.173|$^{+0.003}_{-0.018}$|2.04 × 10−33.5 × 10−141.1 × 10−124.9|$^{+2.4}_{-1.3}$|1.07 × 10−42.9 × 10−148.0 × 10−14125.92/135 = 0.93
Fc0.157|$^{+0.020}_{-0.011}$|3.60 × 10−33.7 × 10−141.6 × 10−124.8|$^{+2.2}_{-1.4}$|1.10 × 10−42.8 × 10−148.3 × 10−14125.47/134 = 0.94

Notes:aThe normalization parameters is defined as |$A = 1\times 10^{-14}\int n_\mathrm{e}n_\mathrm{H}\mathrm{d}V/4 \pi d^{2}$|⁠, where d, ne, and V are the distance, electron density, and volume in cgs units, respectively.

bf and F represent the absorbed and unabsorbed fluxes. Fluxes are computed in the 0.3–2.0 keV energy range. All fluxes are in cgs units (erg cm−2 s−1).

cModel F was performed with a variable absorption column density. This model resulted in NH = 5.15 × 1021 cm−2.

Close
This Feature Is Available To Subscribers Only

Sign In or Create an Account

Close

This PDF is available to Subscribers Only

View Article Abstract & Purchase Options

For full access to this pdf, sign in to an existing account, or purchase an annual subscription.

Close