On top of LCDM the following are added:
To build the sky models the experiment bandpasses are already required. So far nominal tophat bands are being used - a complete list of the center and width is in this spreadsheet. The CMB-S4 specific band list is CMB-S4 frequency bands v1.99. What a tophat bandpass actually means is a little tricky and discussed in Bandpass Convention - What does flat mean. Models 00/05/06/07/09 use nu^-2 in spectral radiance (SR) units, while models 01/02/03 use nu^0 in SR units. (What 04 uses is not known.) Model 08 is delta function bandpass.
Sky model 00
This Gaussian dust + Gaussian Sync. Since the dust and sync levels are set to the levels found in the BICEP/Keck field it wouldn't make any sense to use this model for a large sky fraction.
Sky Model 01
This is PySM run in a1d1f1s1 mode - i.e. with the default settings for AME, dust, free-free and synchrotron.
Sky Model 02
Sky Model 03
Versus 02 this switches the dust model to a Hensley/Draine model and is dubbed a2d7f1s3. (02 to 03 also marks the switch from pysm_1.0 to pysm_2.0 so the s2, f1, s3 components in principle may change.)
Sky Model 04
This model switches the dust model to a Tuhin Ghosh provided model which implements dust decorrelation. See HI-based dust polarization model for r forecasts. The AME, sync and free-free components remain the same as 03
Sky Model 05
This is a toy model of dust which is highly decorrelated. See Toy highly decorrelated dust model. There is NO AME/sync/Free-free - only dust.
Sky Model 06
Sky Model 07
This is "amplitude modulated Gaussian" as described at Amplitude modulated Gaussian dust sims. Sync is modulated with the same amplitude template as dust (which is clearly not proper).
Sky Model 08
This MKD multilayer model from arxiv/1706.04162.
Sky Model 09
This is the Vansyngel Model.