Table A.4.
Details of the spectral fit.
XMM Name | NH | Γ | Npo | N6.4 | EW6.4 | N6.7 | EW6.7 | N6.9 | EW6.9 | χ2/d.o.f | Flux |
---|---|---|---|---|---|---|---|---|---|---|---|
× 1022 cm−2 | eV | eV | eV | 0.2–10 keV | |||||||
4XMM J172511.3 |
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< 5 × 10−6 | < 8 | < 3 × 10−6 | < 7 | 2364/2299 | 3.56 × 10−11 |
4XMM J173058.9 |
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< 1 × 10−6 | < 50 | 69/82 | 1.52 × 10−12 |
XMMU J173029.8 |
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< 2 × 10−6 | < 160 |
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11/17 | 6.70 × 10−13 |
4XMM J174517.0 |
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339/326 | 9.59 × 10−13 |
4XMM J174728.9 |
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< 4 × 10−7 | < 1500 | < 5 × 10−7 | < 2000 | < 5 × 10−7 | < 2200 | 16/28 | 4.00 × 10−14 |
4XMM J173837.0 |
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< 8 × 10−7 | < 351 |
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23/42 | 2.06 × 10−13 |
4XMM J174033.8 |
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185/189 | 2.88 × 10−12 |
4XMM J174016.0 |
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736/607 | 5.14 × 10−12 |
4XMM J174809.8 |
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5+7 × 10−7 | 175+71 | < 7 × 10−7 | < 172 |
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50/48 | 2.96 × 10−13 |
4XMM J174009.0 |
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170/166 | 5.90 × 10−12 |
4XMM J174954.6 |
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< 3 × 10−6 | < 150 | 90/91 | 1.73 × 10−12 |
4XMM J175327.8 |
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< 2 × 10−6 | < 774 | < 2 × 10−6 | < 660 | < 2 × 10−6 | < 751 | 64/41 | 4.29 × 10−13 |
4XMM J174622.7 |
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192/187 | 5.13 × 10−13 |
4XMM J175452.0 |
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< 9 × 10−7 | < 206 | < 1 × 10−6 | < 529 | 33/41 | 2.68 × 10−13 |
4XMM J175301.3 |
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63/54 | 1.86 × 10−13 |
4XMM J174917.7 |
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107/108 | 1.31 × 10−12 |
4XMM J175244.4 |
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< 8 × 10−7 | < 388 |
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29/51 | 2.11 × 10−13 |
4XMM J174816.9 |
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159/164 | 8.50 × 10−13 |
4XMM J174445.6 |
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399/412 | 2.03 × 10−12 |
4XMM J175740.5 |
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113/92 | 7.63 × 10−13 |
4XMM J174906.8 |
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400/442 | 1.12 × 10−11 |
XMMU J175441.9 |
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33/26 | 4.31 × 10−13 |
4XMM J175511.6 |
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< 1 × 10−6 | < 263 | 69/76 | 3.06 × 10−13 |
4XMM J175525.0 |
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< 1 × 10−6 | < 33 |
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< 1 × 10−6 | < 55 | 171/170 | 1.84 × 10−12 |
4XMM J175328.4 |
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883/914 | 5.56 × 10−12 |
XMMU J180140.3 |
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< 4 × 10−8 | < 8 | < 6 × 10−6 | < 1500 | 25/27 | 2.31 × 10−13 |
Notes. The model used for spectral fit is power-law for the continuum plus three Gaussian at 6.4, 6.7, and 6.9 keV for iron emission complex. The spectral model is convolved with a Galactic absorption component tbabs. The normalization of power-law model Npo is given in units of photons keV−1 cm2 s−1 at 1 keV and the normalization of the lines are given in units of photons cm2 s−1 in the line energy.
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