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--- 20180914_decorr [2018/09/14 15:08] – pryke
+++ 20180914_decorr [2018/09/14 15:22] (current) – pryke
@@ Line 7: / Line 7: @@
 In this post I look at the decorrelation of the dust and sync patterns by comparing cross-spectra to the
 geometric mean of auto-spectra (the lower right panel of each plot).
-We see that only the 98 and 99 (multi-layer and Vansyngel) models are significantly decorrelated in dust.
+We see that only the 98 and 99 (multi-layer and Vansyngel) models are significantly decorrelated in dust,
+and none of them are significantly decorrelated in sync.
 I take the power spectra using anafast and the soft edge mask shown below.
@@ Line 14: / Line 15: @@
 {{180914_fm.gif}}
-*Dust plots*
+To recap the models are:
+  * 00=Toy Gaussian models for dust and sync with uniform amplitude over the sky at level appropriate for the BICEP/Keck patch (i.e. way too low for PICO large sky coverage).
+  * 91=PySM a1d1f1s1 [[https://arxiv.org/abs/1608.02841 | arxiv/1608.02841]]
+  * 92=PySM a2d4f1s3
+  * 93=PySM a2d7f1s3
+  * 96=Brandon's MHD model for dust and sync taken from /global/homes/b/bhensley/mhd_maps/maps_v1 on 180424
+  * 98=MKD multilayer dust model as described in [[https://arxiv.org/pdf/1706.04162.pdf | arxiv/1706.04162]]. Since only dust is provided this is added to PySM a2f1s3 as per models 92 and 93.
+  * 99=Vansyngel model as described in [[https://arxiv.org/abs/1611.02577 | arxiv/1611.02577]] with multi-frequency extension. This model provides both dust and sync (and no AME or free-free is added.)
+So we have 7 models for dust and 5 for sync.
+**Dust plots**
 {{180914_f0.gif}}
 {{180914_f1.gif}}
 {{180914_f2.gif}}
-{{180914_f3.gif}
+{{180914_f3.gif}}
 {{180914_f6.gif}}
@@ Line 26: / Line 39: @@
 {{180914_f9.gif}}
-*Sync plots*
+**Sync plots**
 {{180914_f0s.gif}}

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