We also fit the line widths of mainly oxygen and iron lines.
In this case we also fit each user separately, and we perform the prediction in an online manner.
We also fit the immediate fair innocent weak condition from Wetmore et al. (2015) and reached similar conclusions.
We also fit two nonlinear models that restricted the AGB estimate to be positive with an upper limit.
To verify our results, we also fit the ETAS model to the original dataset with some higher magnitude thresholds, M2.5 and M3.0.
We also fit two more models to the current data: the beta Burr III (BBIII) (Gomes et al. 2013) and beta Weibull (BW) (Lee et al. 2007) distributions.
We also fit our theoretical models to the burst oscillation data of the low mass X-ray binary XTE J1814-338, and find that the 90% confidence lower limit of the neutron star's dimensionless radius-to-mass ratio is 4.2.
The Pre-diagnosis model used all data collected from healthy participants, but only pre-diagnosis data from depressed participants, to address Hypothesis 2. We also fit an 'intercept-only' model, in which all predictors are zero-weighted to simulate a model under a null hypothesis.
For comparison, we also fit the extinction curve of Rieke et al. (1989), which is actually the RV = 3.1-type extinction, and the model also works very well with dn/da ℝ a−2.1e−a/0.08 for amorphous silicates and dn/da ℝ a−3.0e−a/0.28 for graphite.
We also fit a simple exponential to every FRAP experiment.
We also fit the simplest model conditioned on the first infection including it into the analysis.
