| Interstellar absorption | |
| N H (10|$^{22}\:$|cm|$^{2}$|) | 0.053 (|$\lt $|0.252) |
| Plasma component† | |
| |$kT$| (keV) | |$0.74\pm 0.10$| |
| Z (solar) | 0.3 (fixed) |
| Normalization | |$3.5^{+4.6}_{-1.2}\times 10^{-7}$| |
| Gaussian component | |
| |$E_{\rm center}$| | 1.04|$^{+0.03}_{-0.02}$| |
| |$\sigma$| | 0 (fixed) |
| Normalization (photon|$\:$|s|$^{-1}\:$|cm|$^{-2}$|) | 1.5|$^{+0.3}_{-0.1}\times 10^{-8}$| |
| Power law component | |
| |$\Gamma$| | |$1.0\pm 0.1$| |
| Normalization (keV|$^{-1}$| s|$^{-1}\:$|cm|$^{-2}$| at 1|$\:$|keV) | 2.1|$^{+0.3}_{-0.2}\times 10^{-7}$| |
| X-ray flux, luminosity‡ | |
| |$F_{\rm X}$| in 0.3–7|$\:$|keV (erg|$\:$|s|$^{-1}\:$|cm|$^{-2}$|) | 2.3 |$\times 10^{-15}$| |
| |$L_{\rm X}$| in 0.3–7|$\:$|keV (erg|$\:$|s|$^{-1}$|) | 3.6 |$\times 10^{29}$| |
| |$\chi ^{2}/$|d.o.f | 1.28 |
| d.o.f | 19 |
| Interstellar absorption | |
| N H (10|$^{22}\:$|cm|$^{2}$|) | 0.053 (|$\lt $|0.252) |
| Plasma component† | |
| |$kT$| (keV) | |$0.74\pm 0.10$| |
| Z (solar) | 0.3 (fixed) |
| Normalization | |$3.5^{+4.6}_{-1.2}\times 10^{-7}$| |
| Gaussian component | |
| |$E_{\rm center}$| | 1.04|$^{+0.03}_{-0.02}$| |
| |$\sigma$| | 0 (fixed) |
| Normalization (photon|$\:$|s|$^{-1}\:$|cm|$^{-2}$|) | 1.5|$^{+0.3}_{-0.1}\times 10^{-8}$| |
| Power law component | |
| |$\Gamma$| | |$1.0\pm 0.1$| |
| Normalization (keV|$^{-1}$| s|$^{-1}\:$|cm|$^{-2}$| at 1|$\:$|keV) | 2.1|$^{+0.3}_{-0.2}\times 10^{-7}$| |
| X-ray flux, luminosity‡ | |
| |$F_{\rm X}$| in 0.3–7|$\:$|keV (erg|$\:$|s|$^{-1}\:$|cm|$^{-2}$|) | 2.3 |$\times 10^{-15}$| |
| |$L_{\rm X}$| in 0.3–7|$\:$|keV (erg|$\:$|s|$^{-1}$|) | 3.6 |$\times 10^{29}$| |
| |$\chi ^{2}/$|d.o.f | 1.28 |
| d.o.f | 19 |
*The model assumes tbabs (apec |$+$| Gaussian |$+$| power-law).
†The normalization is defined as |$10^{-14}/(4\pi D^2){\it {EM}}$|, where D is the distance to the Carina Nebula in cm and |${\it EM}$| is the plasma emission measure in cm|$^{-3}$|. The elemental abundances are given relative to the solar photospheric values measured by Anders and Grevesse (1989).
‡A distance of |$2.3\:$|kpc is assumed. The total flux and luminosity of all point sources are |$\times 400$| of these values.
| Interstellar absorption | |
| N H (10|$^{22}\:$|cm|$^{2}$|) | 0.053 (|$\lt $|0.252) |
| Plasma component† | |
| |$kT$| (keV) | |$0.74\pm 0.10$| |
| Z (solar) | 0.3 (fixed) |
| Normalization | |$3.5^{+4.6}_{-1.2}\times 10^{-7}$| |
| Gaussian component | |
| |$E_{\rm center}$| | 1.04|$^{+0.03}_{-0.02}$| |
| |$\sigma$| | 0 (fixed) |
| Normalization (photon|$\:$|s|$^{-1}\:$|cm|$^{-2}$|) | 1.5|$^{+0.3}_{-0.1}\times 10^{-8}$| |
| Power law component | |
| |$\Gamma$| | |$1.0\pm 0.1$| |
| Normalization (keV|$^{-1}$| s|$^{-1}\:$|cm|$^{-2}$| at 1|$\:$|keV) | 2.1|$^{+0.3}_{-0.2}\times 10^{-7}$| |
| X-ray flux, luminosity‡ | |
| |$F_{\rm X}$| in 0.3–7|$\:$|keV (erg|$\:$|s|$^{-1}\:$|cm|$^{-2}$|) | 2.3 |$\times 10^{-15}$| |
| |$L_{\rm X}$| in 0.3–7|$\:$|keV (erg|$\:$|s|$^{-1}$|) | 3.6 |$\times 10^{29}$| |
| |$\chi ^{2}/$|d.o.f | 1.28 |
| d.o.f | 19 |
| Interstellar absorption | |
| N H (10|$^{22}\:$|cm|$^{2}$|) | 0.053 (|$\lt $|0.252) |
| Plasma component† | |
| |$kT$| (keV) | |$0.74\pm 0.10$| |
| Z (solar) | 0.3 (fixed) |
| Normalization | |$3.5^{+4.6}_{-1.2}\times 10^{-7}$| |
| Gaussian component | |
| |$E_{\rm center}$| | 1.04|$^{+0.03}_{-0.02}$| |
| |$\sigma$| | 0 (fixed) |
| Normalization (photon|$\:$|s|$^{-1}\:$|cm|$^{-2}$|) | 1.5|$^{+0.3}_{-0.1}\times 10^{-8}$| |
| Power law component | |
| |$\Gamma$| | |$1.0\pm 0.1$| |
| Normalization (keV|$^{-1}$| s|$^{-1}\:$|cm|$^{-2}$| at 1|$\:$|keV) | 2.1|$^{+0.3}_{-0.2}\times 10^{-7}$| |
| X-ray flux, luminosity‡ | |
| |$F_{\rm X}$| in 0.3–7|$\:$|keV (erg|$\:$|s|$^{-1}\:$|cm|$^{-2}$|) | 2.3 |$\times 10^{-15}$| |
| |$L_{\rm X}$| in 0.3–7|$\:$|keV (erg|$\:$|s|$^{-1}$|) | 3.6 |$\times 10^{29}$| |
| |$\chi ^{2}/$|d.o.f | 1.28 |
| d.o.f | 19 |
*The model assumes tbabs (apec |$+$| Gaussian |$+$| power-law).
†The normalization is defined as |$10^{-14}/(4\pi D^2){\it {EM}}$|, where D is the distance to the Carina Nebula in cm and |${\it EM}$| is the plasma emission measure in cm|$^{-3}$|. The elemental abundances are given relative to the solar photospheric values measured by Anders and Grevesse (1989).
‡A distance of |$2.3\:$|kpc is assumed. The total flux and luminosity of all point sources are |$\times 400$| of these values.
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