Table 1.
Best-fit parameters of the relation log SFRFUV,corr/SFRMS(M⋆, z)) = k1(1 − cos(i)) + k2, where SFRFUV,corr is measured using three different methods.
| Local z ~ 0 |
COSMOS z ~ 0.7 |
|||||||
|---|---|---|---|---|---|---|---|---|
| Method | N | k1 | k2 | σ2 | N | k1 | k2 | σ2 |
| No corr | 3489 |
|
|
|
575 |
|
|
|
| UV slope | 3489 |
|
|
|
56 |
|
|
|
| FUV + MIR | 3454 |
|
|
|
527 |
|
|
|
| FUV + RT | 3489 |
|
|
|
565 |
|
|
|
| Restricted z ~ 0 sample | Restricted z ~ 0.7 sample | |||||||
| No corr | 1021 | 
|
|
|
295 | 
|
|
|
| UV slope | 1021 | 
|
|
|
28 |
|
|
|
| FUV + MIR | 1015 |
|
|
|
284 |
|
|
|
| FUV + RT | 1021 |
|
|
|
295 |
|
|
|
Notes. An intrinsic scatter of variance σ2, assumed to be in the SFR direction, is also fitted following Foreman-Mackey (2017). N is the number of galaxies used for the fits. Errors represent the 5th and 95th percentiles of the parameters given by the MCMC.
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