Table 5.
Model selection for different inter-pulsar correlation models for a CRS.
| ID | Model | DR2full |
DR2full+ | DR2new |
DR2new+ | ||
|---|---|---|---|---|---|---|---|
| ENTERPRISE | FORTYTWO | ENTERPRISE | ENTERPRISE | FORTYTWO | ENTERPRISE | ||
| 1 | PSRN + CURN | – | – | – | – | – | – |
| 2 | PSRN + GWB | 4 | 5 | 4 | 60 | 62 | 65 |
| 3 | PSRN + CLK | < 0.01 | < 0.01 | < 0.01 | 0.2 | 1.2 | 0.3 |
| 4 | PSRN + EPH | < 0.01 | ∼10−4 | < 0.01 | 0.2 | 0.2 | 1.3 |
| 5 | PSRN + CURN + CLK | 2 | 1 | 2.7 | 0.8 | 2 | 1.6 |
| 6 | PSRN + CURN + EPH | 1 | 0.1 | 1 | 1 | 1 | 1.6 |
| 7 | PSRN + GWB + CURN | 3 | 3 | 4 | 27 | 13 | 25 |
| 8 | PSRN + GWB + CLK | 5 | 12 | 7 | 28 | 35 | 57 |
| 9 | PSRN + GWB + EPH | 3 | 3 | 3.6 | 33 | 29 | 43 |
Notes. We present BFs for different CRS models against the CURN model. We assumed the DE440 SSE fit and used the PSRN+CURN model as the reference model. The model component acronyms are: (i) PSRN = individual Pulsar noise, (ii) CURN = common uncorrelated red noise, (iii) GWB = gravitational wave background with quadrupolar (HD) angular correlation, (iv) CLK = common signal with monopolar spatial correlation, as expected from a clock error, (v) EPH = common signal with dipolar spatial correlation, as expected from SSE errors.
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