Table 4
Results of the model calculations for all 28 pulsars in our master list (A), and for the 19 youngest pulsars (τc < 10 Myr, Y).
| Sample | Single Maxwellian | Two Maxwellians | vl Gaussian | |||||||||||
|
|
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| N | σ | range | dℒ | σ 1 | range | σ 2 | range | w | range | dℒ | σ | range | ||
| (km s-1) | (km s-1) | (km s-1) | (%) | (km s-1) | ||||||||||
|
|
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| Isotropic models | A | 28 | 244 | 221–271 | ≡0 | 77 | 62–97 | 321 | 278–375 | 42 | 29–54 | −14 | 240 | 209–279 |
| Mixed models | A | 22 + 6 | 239 | 219–267 | −18 | 75 | 61–95 | 316 | 276–369 | 42 | 30–55 | −33 | ||
|
|
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| Isotropic models | Y | 19 | 277 | 247–314 | ≡0 | 83 | 62–117 | 335 | 287–398 | 32 | 17–47 | −6 | 263 | 223–314 |
| Mixed models | Y | 14 + 5 | 273 | 245–310 | −16 | 82 | 61–115 | 328 | 285-391 | 32 | 17–48 | −22 | ||
Notes. For the mixed models we give separately the number of pulsars from a semi-isotropic and an isotropic distribution (see Table D.1). For each model we give the best parameters and their approximate 68% range determined by setting Eq. (12) to unity. Within each sample we also give the differences in deviance dℒ (Eq. (13)) between each model and the model with a single isotropic Maxwellian, which gives an indication of their relative merits.
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