Table 4.
Fitting power law continuum to individual one hour spectra for the quasar J022836.08+000939.
ID | Uncorrected | Margala | Our correction | Our correction | DR16 | ||||||||||
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
(σ = const.) | (σ = const.) | (σ = f(λ)) | (σ = const.) | ||||||||||||
−α | σα | ![]() |
−α | σα | ![]() |
−α | σα | ![]() |
−α | σα | ![]() |
−α | σα | ![]() |
|
1 | −0.59 | 0.01 | 1.32 | −1.11 | 0.01 | 1.39 | −1.27 | 0.01 | 1.44 | −1.28 | 0.01 | 1.41 | −1.11 | 0.01 | 1.51 |
2 | −0.61 | 0.01 | 1.26 | −1.03 | 0.01 | 1.34 | −1.17 | 0.01 | 1.39 | −1.22 | 0.01 | 1.36 | −1.05 | 0.01 | 1.43 |
3 | −0.58 | 0.01 | 1.64 | −1.04 | 0.01 | 1.81 | −1.17 | 0.01 | 1.92 | −1.21 | 0.01 | 1.86 | −1.08 | 0.01 | 2.01 |
4 | 0.41 | 0.01 | 1.34 | −0.57 | 0.01 | 1.49 | −0.64 | 0.01 | 1.57 | −0.72 | 0.01 | 1.48 | −0.68 | 0.02 | 1.63 |
5 | 0.08 | 0.01 | 1.11 | −0.76 | 0.02 | 1.22 | −0.94 | 0.02 | 1.30 | −1.07 | 0.02 | 1.22 | −0.96 | 0.01 | 1.14 |
6 | 0.08 | 0.01 | 1.19 | −0.73 | 0.01 | 1.28 | −0.77 | 0.01 | 1.32 | −0.86 | 0.01 | 1.27 | −0.85 | 0.01 | 1.33 |
7 | −0.17 | 0.01 | 0.97 | −1.23 | 0.01 | 1.11 | −1.26 | 0.01 | 1.15 | −1.32 | 0.01 | 1.08 | −1.15 | 0.02 | 1.25 |
8 | 0.46 | 0.02 | 1.25 | −0.45 | 0.02 | 1.35 | −0.64 | 0.02 | 1.43 | −0.76 | 0.02 | 1.36 | −0.57 | 0.02 | 1.29 |
μ | −0.11 | 1.26 | −0.86 | 1.37 | −0.98 | 1.44 | −1.05 | 1.38 | −0.93 | 1.45 | |||||
σμ | 0.42 | 0.26 | 0.25 | 0.23 | 0.20 | ||||||||||
![]() |
0.15 | 0.09 | 0.09 | 0.08 | 0.07 |
Notes. The σ on the second line of the header refers to the seeing profile i.e. Eq. (6). The first column corresponds to the ID in Table 2. Columns 2–4 relate to uncorrected spectra. The second and the third columns give the best-fit spectral index, Eq. (18), and its error (σα). The fourth column is the best-fit normalised , i.e. Eq. (19) normalised by the number of degrees of freedom in the fit. The same pattern of three columns is repeated for each of the four correction methods. The last three lines in this table labelled μ, σμ, and
, give the unweighted mean spectral index, its standard deviation, and in the last line, the error on the mean. For comparison, the best-fit spectral index obtained (in the same way) using the SDSS DR7 spectrum is −0.65 ± 0.02. The mean value of
gives an indication of the overall quality of fit.
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