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 00/05/06/08/09 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.)
On top of LCDM the following are added:
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 08
This is the model 06 with an alternate electron energy spectrum which gives a synchrotron spectrum closer to reality.
Sky Model 09
This is the Vansyngel Model.