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Simulations for 4 HFI channels
for A and B split of the data
cmb, noise and fgs are coadded.

Version 2: Included two seperate noise map for A and B detector splits. Earlier version had 1 noise map
for both A and B.
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/mn/stornext/d5/unnif/hfi/simsAB/
all maps are in the uK units

beams (Bl_TEB.. files) and rms files (spatial variation) from Planck NPIPE (Kristian)
inputAB/

cmb
===
from Johannes
cmb/default.fits
cmb/beta_035_cmb_rotated.fits

convolved with HFI A/B beams and pixel window. lmax: 3xnside=6144

noise
=====
drawn from the rmsA/B-files (rms*N(0,1))

foregrounds
===========

dust: MBB
====

Amplitude maps from PySM. The templates are initially at Nside=512.
They have been ud_graded to Nside=2048, and then convolved with the HFI A/B beams and pixel window.
Convolved with HFI beams before applying the MBB projection, lmax: 3xnside=6144.
Reference frequencies [T,Q,U]=	[545. 353. 353.] GHz

Spatial variation of both spectral indices and dust temperature at Nside512 resolution. Templates from PySM d1s1, but ud_graded from 512 to 2048.

synch: power law
======

Amplitude maps from PySM. The templates are initially at Nside=512.
They have been ud_graded to Nside=2048, and then convolved with the HFI A/B beams and pixel window.
Convolved with HFI beams before applying the power law projection, lmax: 3xnside=6144.
Reference frequencies[T,Q,U]=	[ 0.408 23.    23.   ] GHz

Spatial variation of spectral indices at Nside512 resolution. Templates from PySM d1s1, but ud_graded from 512 to 2048.


4 cases:
======
There are 4 different cases which are the 4 combinations of with cb/no cb and with miscalibration/no miscalibration. The 4 cases where made with the python script simulate_cb_miscalibration.py