Difference between revisions of "Vansyngel Model"
| Line 19: | Line 19: | ||
The color stretch is shown on the y-axis label and is held the same across each Q/U pair. | The color stretch is shown on the y-axis label and is held the same across each Q/U pair. | ||
| − | [[File: | + | [[File:171208_f2a.gif]] |
| − | [[File: | + | [[File:171208_f2b.gif]] |
| − | [[File: | + | [[File:171208_f2c.gif]] |
Revision as of 15:27, 8 December 2017
Dec 8 2017, Clem Pryke
Flavien Vansyngel has kindly provided a set of files for a new model based on arxiv/1611.02577. This model includes dust and synchrotron components and becomes CMB-S4 model 09.
Here are plots comparing the full sky to Planck and PySM model a2d4f1s3 (CMB-S4 model 02) in a similar style to previous posting Checking PySM maps. (These plots are in Healpix Q/U convention and can be compared to Planck 2015 paper I fig 8. Planck has been downgraded all the way to nside=16 to suppress noise while the other plots are nearest neighbor sampled from nside=512.) All the plots are on the same +/-15uK color stretch. We see that PySM follows Planck much more closely on the largest scales.
Of course what we are interested in for CMB-S4 is the behavior in clean regions off the galactic plane. Here are zoom plots around the BICEP/Keck region. (These are in celestial coords with IAU Q/U convention. Planck is nside=128 this time.) The color stretch is shown on the y-axis label and is held the same across each Q/U pair.
