Table 1.
Properties of the observations and data products used in the analysis of this paper, listed per 100-day MJD bin.
| MJD | Telescope | G | ν | δν | Tsys | Back end | tsub | Nsub | Nepoch |
|---|---|---|---|---|---|---|---|---|---|
| (K Jy−1) | (MHz) | (MHz) | (K) | (s) | |||||
| 53000–53100 | Parkes | 0.66 | 685 | 64 | 45 | Wide-band correlator | 60 | 33 | 3 |
| 53100–53200 | Parkes | 0.74 | 1400 | 256 | 22 | Wide-band correlator | 60 | 22 | 3 |
| 53200–53300 | GBT | 2.00 | 820 | 48 | 35 | BCPM | 180 | 47 | 4 |
| 53300–53400 | GBT | 2.00 | 820 | 48 | 35 | BCPM/SPIGOT | 180/20 | 187 | 2 |
| 53400–53500 | GBT | 2.00 | 820 | 48 | 35 | BCPM/SPIGOT | 20 | 376 | 2 |
| 53500–53600 | GBT | 2.00 | 820 | 48 | 35 | BCPM/SPIGOT | 20 | 869 | 9 |
| 53600–53700 | GBT | 2.00 | 820 | 48 | 35 | BCPM/SPIGOT | 20 | 374 | 3 |
| 53700–53800 | GBT | 2.00 | 820 | 48 | 35 | BCPM/SPIGOT | 20 | 951 | 9 |
| 53800–53900 | GBT | 2.00 | 820 | 48 | 35 | SPIGOT | 20 | 567 | 7 |
| 53900–54000 | GBT | 2.00 | 820 | 48 | 35 | SPIGOT | 20 | 65 | 4 |
| 54000–54100 | GBT | 2.00 | 820 | 48 | 35 | SPIGOT | 20 | 285 | 6 |
| 54100–54200 | GBT | 2.00 | 820 | 48 | 35 | SPIGOT | 20 | 284 | 5 |
| 54200–54300 | – | – | – | – | – | – | – | 0 | 0 |
| 54300–54400 | GBT | 2.00 | 820 | 48 | 35 | SPIGOT | 20 | 5 | 1 |
| 54400–54500 | GBT | 2.00 | 820 | 48 | 35 | SPIGOT | 20 | 50 | 6 |
Notes. Columns 3–6 show the telescope gain (G), the observing frequency (ν), the observation bandwidth (δν) and the typical system-noise temperature (Tsys) of each observational setup, respectively. Column 8 shows the integration time (tsub) of each sub-integration in the original data. The second-to-last column shows the final number of sub-integrations contained in each MJD bin, after omitting those that were plagued by RFI and applying a cut-off to the distribution of uncertainties in our subsequent timing analysis (see Sect. 3.1). The last column shows the number of observing epochs (separated by at least one day) corresponding to the data in each MJD bin.
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