Details of the parameters utilized for estimating time delays between light curves in two different energy ranges. The peak value of the correlation function is denoted by |$\epsilon ^{z}_{\tau }$|, and the corresponding time delay is represented by |$\tau^{zdcf}_{\rm d}$|. Using the method outlined in (Gaskell & Peterson 1987), the error on the position of the peak of the correlation function is determined and is given by Δτd. A comparison between this error and the time bin size was conducted to ensure the accuracy of the result, with the larger value selected for our analysis. For further details, refer to Section 3.1.2.
| ID . | Epochs . | Bin size . | Δτd . | |$\epsilon ^{z}_{\tau }$| . | |$\tau ^{zdcf}_{\rm d}$| . |
|---|---|---|---|---|---|
| . | Year . | (ks) . | (ks) . | . | (ks) . |
| XMM1 | 2001 | 0.5 | 0.21 | 0.48 ± 0.05 | 0.31 ± 0.5 |
| XMM2 | 2005 | 0.5 | 0.46 | 0.50 ± 0.03 | 0.77 ± 0.5 |
| NU1 | 2015 | 0.5 | – | – | – |
| NU2 | 2015 | 0.5 | – | – | – |
| XRT† | 2019–2022 | 1.0 | 5.07 | 0.68 ± 0.05 | −1.88 ± 5.07 |
| ID . | Epochs . | Bin size . | Δτd . | |$\epsilon ^{z}_{\tau }$| . | |$\tau ^{zdcf}_{\rm d}$| . |
|---|---|---|---|---|---|
| . | Year . | (ks) . | (ks) . | . | (ks) . |
| XMM1 | 2001 | 0.5 | 0.21 | 0.48 ± 0.05 | 0.31 ± 0.5 |
| XMM2 | 2005 | 0.5 | 0.46 | 0.50 ± 0.03 | 0.77 ± 0.5 |
| NU1 | 2015 | 0.5 | – | – | – |
| NU2 | 2015 | 0.5 | – | – | – |
| XRT† | 2019–2022 | 1.0 | 5.07 | 0.68 ± 0.05 | −1.88 ± 5.07 |
Note.† In the case of XRT observation, the correlation parameters are calculated in the unit of days.
Details of the parameters utilized for estimating time delays between light curves in two different energy ranges. The peak value of the correlation function is denoted by |$\epsilon ^{z}_{\tau }$|, and the corresponding time delay is represented by |$\tau^{zdcf}_{\rm d}$|. Using the method outlined in (Gaskell & Peterson 1987), the error on the position of the peak of the correlation function is determined and is given by Δτd. A comparison between this error and the time bin size was conducted to ensure the accuracy of the result, with the larger value selected for our analysis. For further details, refer to Section 3.1.2.
| ID . | Epochs . | Bin size . | Δτd . | |$\epsilon ^{z}_{\tau }$| . | |$\tau ^{zdcf}_{\rm d}$| . |
|---|---|---|---|---|---|
| . | Year . | (ks) . | (ks) . | . | (ks) . |
| XMM1 | 2001 | 0.5 | 0.21 | 0.48 ± 0.05 | 0.31 ± 0.5 |
| XMM2 | 2005 | 0.5 | 0.46 | 0.50 ± 0.03 | 0.77 ± 0.5 |
| NU1 | 2015 | 0.5 | – | – | – |
| NU2 | 2015 | 0.5 | – | – | – |
| XRT† | 2019–2022 | 1.0 | 5.07 | 0.68 ± 0.05 | −1.88 ± 5.07 |
| ID . | Epochs . | Bin size . | Δτd . | |$\epsilon ^{z}_{\tau }$| . | |$\tau ^{zdcf}_{\rm d}$| . |
|---|---|---|---|---|---|
| . | Year . | (ks) . | (ks) . | . | (ks) . |
| XMM1 | 2001 | 0.5 | 0.21 | 0.48 ± 0.05 | 0.31 ± 0.5 |
| XMM2 | 2005 | 0.5 | 0.46 | 0.50 ± 0.03 | 0.77 ± 0.5 |
| NU1 | 2015 | 0.5 | – | – | – |
| NU2 | 2015 | 0.5 | – | – | – |
| XRT† | 2019–2022 | 1.0 | 5.07 | 0.68 ± 0.05 | −1.88 ± 5.07 |
Note.† In the case of XRT observation, the correlation parameters are calculated in the unit of days.
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