Best-fit parameters of spectral fitting by the two-temperature CIE model. |$^*$|
| . | No. 5 . | No. 8a . | No. 9 . | No. 12 . |
|---|---|---|---|---|
| |$N_{\rm H(ISM)}$| (10 |$^{22}$| Hcm |$^{-2}$| ) . | 1.047 . | 0.831 . | 1.148 . | 1.698 . |
| |${N_{\rm H}}\ (10^{22}$| Hcm |$^{-2}$| ) | 0.34 |$^{+0.04}_{\,-0.04}$| | 0.44 |$^{+0.03}_{\,-0.03}$| | 0.39 |$^{+0.13}_{\,-0.14}$| | 0.21 |$^{+0.08}_{\,-0.08}$| |
| |$Z_{\solar}$||$^\dag $| | 0.58 |$^{+0.11}_{\,-0.11}$| | 0.75 |$^{+0.10}_{\,-0.09}$| | 0.60 |$^{+0.41}_{\,-0.26}$| | 0.60 |$^{+0.17}_{\,-0.14}$| |
| |${k_{\rm {B}}T}_{\rm {low}}$| (keV) | 0.62 |$^{+0.02}_{\,-0.01}$| | 0.62 |$^{+0.01}_{\,-0.01}$| | 0.65 |$^{+0.19}_{\,-0.06}$| | 0.74 |$^{+0.07}_{\,-0.11}$| |
| |$EM_{\rm {low}}$| (10 |$^{57}$| cm |$^{-3})$||$^\ddag $| | 0.70 |$^{+0.13}_{\,-0.11}$| | 0.92 |$^{+0.11}_{\,-0.10}$| | 0.20 |$^{+0.12}_{\,-0.08}$| | 0.39 |$^{+0.11}_{\,-0.09}$| |
| |${k_{\rm {B}}T}_{\rm {high}}$| (keV) | 2.27 |$^{+0.27}_{\,-0.18}$| | 1.92 |$^{+0.07}_{\,-0.06}$| | 3.08 |$^{+1.57}_{\,-0.64}$| | 2.06 |$^{+0.48}_{\,-0.27}$| |
| |$EM_{\rm {high}}$| (10 |$^{57}$| cm |$^{-3})$||$^\ddag $| | 0.13 |$^{+0.02}_{\,-0.02}$| | 0.33 |$^{+0.02}_{\,-0.02}$| | 0.05 |$^{+0.01}_{\,-0.01}$| | 0.11 |$^{+0.04}_{\,-0.03}$| |
| |$\chi^{2}/$| d.o.f. ( |$\chi^{2}_{\rm {red}}$| ) | 376.13 |$/$| 279 (1.35) | 509.44 |$/$| 327 (1.56) | 115.31 |$/$| 102 (1.13) | 202.78 |$/$| 171 (1.19) |
| . | No. 5 . | No. 8a . | No. 9 . | No. 12 . |
|---|---|---|---|---|
| |$N_{\rm H(ISM)}$| (10 |$^{22}$| Hcm |$^{-2}$| ) . | 1.047 . | 0.831 . | 1.148 . | 1.698 . |
| |${N_{\rm H}}\ (10^{22}$| Hcm |$^{-2}$| ) | 0.34 |$^{+0.04}_{\,-0.04}$| | 0.44 |$^{+0.03}_{\,-0.03}$| | 0.39 |$^{+0.13}_{\,-0.14}$| | 0.21 |$^{+0.08}_{\,-0.08}$| |
| |$Z_{\solar}$||$^\dag $| | 0.58 |$^{+0.11}_{\,-0.11}$| | 0.75 |$^{+0.10}_{\,-0.09}$| | 0.60 |$^{+0.41}_{\,-0.26}$| | 0.60 |$^{+0.17}_{\,-0.14}$| |
| |${k_{\rm {B}}T}_{\rm {low}}$| (keV) | 0.62 |$^{+0.02}_{\,-0.01}$| | 0.62 |$^{+0.01}_{\,-0.01}$| | 0.65 |$^{+0.19}_{\,-0.06}$| | 0.74 |$^{+0.07}_{\,-0.11}$| |
| |$EM_{\rm {low}}$| (10 |$^{57}$| cm |$^{-3})$||$^\ddag $| | 0.70 |$^{+0.13}_{\,-0.11}$| | 0.92 |$^{+0.11}_{\,-0.10}$| | 0.20 |$^{+0.12}_{\,-0.08}$| | 0.39 |$^{+0.11}_{\,-0.09}$| |
| |${k_{\rm {B}}T}_{\rm {high}}$| (keV) | 2.27 |$^{+0.27}_{\,-0.18}$| | 1.92 |$^{+0.07}_{\,-0.06}$| | 3.08 |$^{+1.57}_{\,-0.64}$| | 2.06 |$^{+0.48}_{\,-0.27}$| |
| |$EM_{\rm {high}}$| (10 |$^{57}$| cm |$^{-3})$||$^\ddag $| | 0.13 |$^{+0.02}_{\,-0.02}$| | 0.33 |$^{+0.02}_{\,-0.02}$| | 0.05 |$^{+0.01}_{\,-0.01}$| | 0.11 |$^{+0.04}_{\,-0.03}$| |
| |$\chi^{2}/$| d.o.f. ( |$\chi^{2}_{\rm {red}}$| ) | 376.13 |$/$| 279 (1.35) | 509.44 |$/$| 327 (1.56) | 115.31 |$/$| 102 (1.13) | 202.78 |$/$| 171 (1.19) |
The errors are 90% confidence level.
Values are ratios to the solar.
The distance to Cyg OB2 is assumed to be 1.7kpc (Hanson (2003)).
Best-fit parameters of spectral fitting by the two-temperature CIE model. |$^*$|
| . | No. 5 . | No. 8a . | No. 9 . | No. 12 . |
|---|---|---|---|---|
| |$N_{\rm H(ISM)}$| (10 |$^{22}$| Hcm |$^{-2}$| ) . | 1.047 . | 0.831 . | 1.148 . | 1.698 . |
| |${N_{\rm H}}\ (10^{22}$| Hcm |$^{-2}$| ) | 0.34 |$^{+0.04}_{\,-0.04}$| | 0.44 |$^{+0.03}_{\,-0.03}$| | 0.39 |$^{+0.13}_{\,-0.14}$| | 0.21 |$^{+0.08}_{\,-0.08}$| |
| |$Z_{\solar}$||$^\dag $| | 0.58 |$^{+0.11}_{\,-0.11}$| | 0.75 |$^{+0.10}_{\,-0.09}$| | 0.60 |$^{+0.41}_{\,-0.26}$| | 0.60 |$^{+0.17}_{\,-0.14}$| |
| |${k_{\rm {B}}T}_{\rm {low}}$| (keV) | 0.62 |$^{+0.02}_{\,-0.01}$| | 0.62 |$^{+0.01}_{\,-0.01}$| | 0.65 |$^{+0.19}_{\,-0.06}$| | 0.74 |$^{+0.07}_{\,-0.11}$| |
| |$EM_{\rm {low}}$| (10 |$^{57}$| cm |$^{-3})$||$^\ddag $| | 0.70 |$^{+0.13}_{\,-0.11}$| | 0.92 |$^{+0.11}_{\,-0.10}$| | 0.20 |$^{+0.12}_{\,-0.08}$| | 0.39 |$^{+0.11}_{\,-0.09}$| |
| |${k_{\rm {B}}T}_{\rm {high}}$| (keV) | 2.27 |$^{+0.27}_{\,-0.18}$| | 1.92 |$^{+0.07}_{\,-0.06}$| | 3.08 |$^{+1.57}_{\,-0.64}$| | 2.06 |$^{+0.48}_{\,-0.27}$| |
| |$EM_{\rm {high}}$| (10 |$^{57}$| cm |$^{-3})$||$^\ddag $| | 0.13 |$^{+0.02}_{\,-0.02}$| | 0.33 |$^{+0.02}_{\,-0.02}$| | 0.05 |$^{+0.01}_{\,-0.01}$| | 0.11 |$^{+0.04}_{\,-0.03}$| |
| |$\chi^{2}/$| d.o.f. ( |$\chi^{2}_{\rm {red}}$| ) | 376.13 |$/$| 279 (1.35) | 509.44 |$/$| 327 (1.56) | 115.31 |$/$| 102 (1.13) | 202.78 |$/$| 171 (1.19) |
| . | No. 5 . | No. 8a . | No. 9 . | No. 12 . |
|---|---|---|---|---|
| |$N_{\rm H(ISM)}$| (10 |$^{22}$| Hcm |$^{-2}$| ) . | 1.047 . | 0.831 . | 1.148 . | 1.698 . |
| |${N_{\rm H}}\ (10^{22}$| Hcm |$^{-2}$| ) | 0.34 |$^{+0.04}_{\,-0.04}$| | 0.44 |$^{+0.03}_{\,-0.03}$| | 0.39 |$^{+0.13}_{\,-0.14}$| | 0.21 |$^{+0.08}_{\,-0.08}$| |
| |$Z_{\solar}$||$^\dag $| | 0.58 |$^{+0.11}_{\,-0.11}$| | 0.75 |$^{+0.10}_{\,-0.09}$| | 0.60 |$^{+0.41}_{\,-0.26}$| | 0.60 |$^{+0.17}_{\,-0.14}$| |
| |${k_{\rm {B}}T}_{\rm {low}}$| (keV) | 0.62 |$^{+0.02}_{\,-0.01}$| | 0.62 |$^{+0.01}_{\,-0.01}$| | 0.65 |$^{+0.19}_{\,-0.06}$| | 0.74 |$^{+0.07}_{\,-0.11}$| |
| |$EM_{\rm {low}}$| (10 |$^{57}$| cm |$^{-3})$||$^\ddag $| | 0.70 |$^{+0.13}_{\,-0.11}$| | 0.92 |$^{+0.11}_{\,-0.10}$| | 0.20 |$^{+0.12}_{\,-0.08}$| | 0.39 |$^{+0.11}_{\,-0.09}$| |
| |${k_{\rm {B}}T}_{\rm {high}}$| (keV) | 2.27 |$^{+0.27}_{\,-0.18}$| | 1.92 |$^{+0.07}_{\,-0.06}$| | 3.08 |$^{+1.57}_{\,-0.64}$| | 2.06 |$^{+0.48}_{\,-0.27}$| |
| |$EM_{\rm {high}}$| (10 |$^{57}$| cm |$^{-3})$||$^\ddag $| | 0.13 |$^{+0.02}_{\,-0.02}$| | 0.33 |$^{+0.02}_{\,-0.02}$| | 0.05 |$^{+0.01}_{\,-0.01}$| | 0.11 |$^{+0.04}_{\,-0.03}$| |
| |$\chi^{2}/$| d.o.f. ( |$\chi^{2}_{\rm {red}}$| ) | 376.13 |$/$| 279 (1.35) | 509.44 |$/$| 327 (1.56) | 115.31 |$/$| 102 (1.13) | 202.78 |$/$| 171 (1.19) |
The errors are 90% confidence level.
Values are ratios to the solar.
The distance to Cyg OB2 is assumed to be 1.7kpc (Hanson (2003)).
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