Table 3
NuSTAR X-ray best fit spectral results for the eight sources analyzed (see text).
Parameter | NGC 1194 | NGC 1386 | NGC 2273 | NGC 2960 | NGC 3079 | NGC 3393 | NGC 4388 | IC 2560 |
|
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Best fit model | MYT D | T | T | MYT | MYT | T | MYT D | T |
χ2/ν | 113/112 | 32/25 | 123/113 | 6/5a | 189/152 | 49/69 | 693/681 | 125/104 |
Γ | 1.59 ± 0.15 | >2.6 | 2.1 ± 0.1 | 1.9 (f) | 1.8 ± 0.2 | 1.8 ± 0.2 | 1.65 ± 0.08 | 2.7 ± 0.1 |
NH [cm-2] | 1.4![]() |
(5 ± 1) × 1024 | >7.3 × 1024 | 5![]() |
(2.5 ± 0.3) × 1024 | 2.2![]() |
4.4 ± 0.6 × 1023 | >6.7 × 1024 |
AZ90b | 0.003![]() |
0.07 ± 0.01 | 0.07![]() |
1.5![]() |
0.014![]() |
0.017![]() |
0.006![]() |
0.046![]() |
AS90c | ~0 | – | – | 1 (f) | 1 (f) | – | ~0 | – |
AL90 | =AS90 | – | – | =AS90 | =AS90 | – | =AS90 | – |
AS00c | 0.8![]() |
– | – | – | – | – | 1.7![]() |
– |
AL00 | =AS00 | – | – | – | – | – | =AS00 | – |
θ tor | – | <40 | 73![]() |
– | – | 79 ± 1 | – | 53 ± 23 |
fs [%] | 3 ± 1 | <0.5 | <0.03 | – | 1.0![]() |
<0.4 | 8 ± 2 | <0.1 |
F2−10 [erg cm-2 s-1] | 1.2 × 10-12 | 2.8 × 10-13 | 9.5 × 10-13 | 5.8 × 10-14 | 6.2 × 10-13 | 5.1 × 10-13 | 7.8 × 10-12 | 4.0 × 10-13 |
F10−40 [erg cm-2 s-1] | 1.1 × 10-11 | 1.4 × 10-12 | 5.3 × 10-12 | 3.0 × 10-13 | 1.2 × 10-11 | 1.2 × 10-11 | 3.2 × 10-11 | 1.3 × 10-12 |
![]() |
6.0 × 1042 | 8.0 × 1041 | 1.3 × 1043 | 2.6 × 1041 | 1.4 × 1042 | 2.0 × 1043 | 3.9 × 1042 | 9.5 × 1042 |
![]() |
9.6 × 1042 | 1.5 × 1041 | 9.3 × 1042 | 3.1 × 1041 | 1.6 × 1042 | 2.3 × 1043 | 5.7 × 1042 | 2.9 × 1042 |
FPMB/FPMA | 0.99 ± 0.06 | 1.1 ± 0.2 | 1.0 ± 0.1 | 0.9![]() |
1.06 ± 0.08 | 1.0 ± 0.1 | 1.02 ± 0.03 | 1.0 ± 0.1 |
|
||||||||
λ Edd e | 0.012 ± 0.003 | 0.09![]() |
0.23 ± 0.06 | 0.0030![]() |
0.08![]() |
0.09 ± 0.02 | 0.06 ± 0.02 | 0.4 ± 0.1 |
Notes. T = Torus, MYT = MYTorus, MYT D = MYTorus decoupled.
Data for NGC 2960 are just a NuSTAR 3σ detection, so we used the Cash statistic (Cash 1979) for fitting purposes. We report the reduced χ2 just for its straightforward interpretation.
Following Murphy & Yaqoob (2009), AS90, AL90, AS00, AL00 are just multiplicative factors of the respective components, and such, lack physical units. To obtain normalizations at 1 keV in units of photons keV-1 cm-2 s-1, the reader should multiply these factors for the primary normalization, i.e. AZ90.
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