Table 1.
Posterior distributions of the parameters of the three models considered in this study.
Linear | Double power-law | M+13 prior | |
---|---|---|---|
log f0, j | ![]() |
![]() |
![]() |
V0/km s−1 | – | ![]() |
![]() |
αj | ![]() |
![]() |
![]() |
βj | – | ![]() |
![]() |
log f0, M | ![]() |
![]() |
![]() |
αM | ![]() |
![]() |
![]() |
βM | – | ![]() |
![]() |
log f0, V | ![]() |
![]() |
![]() |
αV | ![]() |
![]() |
![]() |
βV | – | ![]() |
![]() |
σlog f | ![]() |
![]() |
![]() |
Notes. The three columns are for the linear (Eq. (11)), double power law (Eq. (12)) and M+13 prior models, respectively (Eq. (13)). The four row blocks, instead, refer to the retained fraction of angular momentum fj, the star formation efficiency fM, the ratio of asymptotic-to-virial velocity fV, and their intrinsic scatter σlog f. The posteriors of the parameters are all summarised with their 16th–50th–84th percentiles.
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