Table 3.
Results of the X-ray spectral fitting for ABC sources with a complex (non power-law) model.
Name ALMA | Other name | Object type | Detector | Model | NH | ΓX | K | ΓR | KR | kT | KT | E1 | K1 | E2 | K2 | χ2 (d.o.f.) |
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
J0029+3456 | B2 0026+34 | AGN | EPIC | A * PL | ![]() |
![]() |
![]() |
0.47(28) | ||||||||
J0057+3021 | NGC 0315 | AGN | ACIS | PL+T | ![]() |
![]() |
![]() |
![]() |
0.83(115) | |||||||
EPIC | PL+T | ![]() |
![]() |
![]() |
![]() |
0.79(356) | ||||||||||
J0111−7302 | PMN J0111−7302 | AGN | EPIC | PL+T | ![]() |
![]() |
![]() |
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0.81(14) | |||||||
J0242−2132 | PKS 0240−217 | QSO | ACIS | A * PL | ![]() |
![]() |
![]() |
0.88(37) | ||||||||
EPIC | A * (PL+L) | ![]() |
![]() |
![]() |
![]() |
![]() |
0.80(969) | |||||||||
J0702−2841 | NGC 2325 | AGN | EPIC | PL+T | ![]() |
![]() |
![]() |
![]() |
0.64(323) | |||||||
J0758+3747 | NGC 2484 | QSO | EPIC | PL+T | ![]() |
![]() |
![]() |
![]() |
0.57(360) | |||||||
J0928−0409 | PKS J0928−0408 | QSO | EPIC | PL+L | ![]() |
![]() |
![]() |
![]() |
1.18(8) | |||||||
J1044+0655 | PKS 1042+071 | QSO | ACIS | PL+L | ![]() |
![]() |
![]() |
![]() |
0.94(115) | |||||||
J1109−3732 | NGC 3557 | AGN | ACIS | PL+T | ![]() |
![]() |
![]() |
![]() |
0.60(9) | |||||||
J1215−1731 | PKS 1213−17 | Blazar | XRT | A * (PL+R) | ![]() |
> 7.79 | ![]() |
< −2.63 | < 0.01 | 0.86(9) | ||||||
J1230+1223 | M 87 | AGN | XRT | PL+T | ![]() |
![]() |
![]() |
1.05(212) | ||||||||
ACIS | PL+T | ![]() |
![]() |
![]() |
![]() |
0.87(141) | ||||||||||
EPIC | A * (PL+T) | ![]() |
![]() |
![]() |
![]() |
![]() |
1.14(1153) | |||||||||
J1305−4928 | NGC 4945 | RS | ACIS | A * (T+R+L+L) | ![]() |
![]() |
![]() |
![]() |
![]() |
![]() |
![]() |
![]() |
![]() |
1.08(183) | ||
EPIC | A * (T+R+L+L) | ![]() |
![]() |
![]() |
![]() |
![]() |
![]() |
![]() |
![]() |
![]() |
0.90(227) | |||||
J1319−1239 | NGC 5077 | AGN | ACIS | PL+T | ![]() |
![]() |
![]() |
![]() |
0.27(6) | |||||||
J1321−4342 | NGC 5090 | RG | EPIC | A * (T+R) | ![]() |
![]() |
![]() |
![]() |
![]() |
0.66(189) | ||||||
J1336−3357 | IC 4296 | AGN | ACIS | PL+T | ![]() |
![]() |
![]() |
![]() |
0.78(89) | |||||||
EPIC | PL+T | ![]() |
![]() |
![]() |
![]() |
0.69(392) | ||||||||||
J1347+1217 | PKS 1345+12 | QSO | ACIS | A * (PL+L) | ![]() |
![]() |
![]() |
![]() |
![]() |
0.82(53) | ||||||
J1553+2348 | PKS 1551+23 | QSO | XRT | A * PL | ![]() |
![]() |
![]() |
0.84(7) | ||||||||
J1558−1409 | PKS 1555−140 | AGN | ACIS | T | ![]() |
![]() |
0.85(75) | |||||||||
EPIC | PL+T | ![]() |
![]() |
![]() |
![]() |
0.90(1434) | ||||||||||
J1627−2426 | PMN J1626−2426 | AGN | ACIS | R+L+L | −1.72∗ | < 0.01 | 3.11∗ | < 0.01 | ![]() |
0.90(11) | ||||||
J1711−3744 | PMN J1711−3744 | No type | ACIS | A * PL | ![]() |
![]() |
<28.93e4 | 1.10(22) | ||||||||
J1723−6500 | NGC 6328 | QSO | EPIC | A * PL | ![]() |
![]() |
![]() |
0.65(309) | ||||||||
J2033+2146 | PKS 2031+21 | QSO | XRT | A * PL | ![]() |
![]() |
![]() |
0.98(55) | ||||||||
J2157−6941 | PKS 2153−69 | QSO | ACIS | PL+T | ![]() |
![]() |
![]() |
![]() |
0.88(272) | |||||||
J2212−2518 | CRATES J221220.71−251828.4 | AGN | ACIS | P+T | ![]() |
![]() |
![]() |
![]() |
0.30(16) |
Notes. For each source we list the ALMA name (Name ALMA), the alternate name (Other name), the ABC type (Object type), and the X-ray detector (Detector). The column Model shows the model components used to fit the spectrum, namely an intrinsic photoelectric absorption component ZWABS (A), a power-law component (PL), a thermal component APEC (T), a gaussian line ZGAUSS (L), and a power law spectrum reflected from neutral material PEXRAV (R). We then list the intrinsic hydrogen column density (NH), the power-law spectral index (ΓX) and normalization K, the reflection component spectral index ΓR and normalization KR, the thermal component temperature (kT) and normalization KT, and the line(s) rest-frame energy (E1, E2) and normalization(s) (K1, K2). Finally, we list the fit χ2 and degrees of freedom (χ2, d.o.f.). NH is in 1022 cm−2. K is 10−4 keV cm−2 s−1. KR is 10−2 keV cm−2 s−1. kT, E1, and E2 are in keV. KT is 10−4 cm−5. K1 and K2 are in 10−4 cm−2 s−1. Parameters indicated with an asterisk (*) are unconstrained and fixed to their best fit value.
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