1.  white noise

2.  ffp10 noise

3.  ffp10 noise + residual masking

Clfsky0.7_Rfsky0.6
Clfsky0.7_Rfsky0.7
Clfsky0.8_Rfsky0.6
Clfsky0.8_Rfsky0.7
Clfsky0.9_Rfsky0.5
Clfsky0.9_Rfsky0.6
Clfsky0.9_Rfsky0.7

4.  test no fg :

4.1  last results simus + tests

test + white noise

simus + white noise

test + ffp10 noise

test + ffp10 noise

4.2  Results :

5.  planck data

xVll cov

6.  simulations

end-to-end simulations

Clfsky = 0.5

white noise

xVll cov

MC cov

ffp10 noise

Clfsky = 0.8

white noise

ffp10 noise

7.  tests

Fixed fixed coeff alpha

with fg residuals

7.1  Old results on Simulations (no more actual)

8.  fsky=0.5

dust mask	residual mask

9.  fsky=0.7

dust mask	residual mask

9.1  preliminary tests

• nside=16
• cosine beam
  • l1 = 2ns-1
  • l2 = 3ns-1
• fsky = 0.5

10.  masks :

• dust mask : based on PySM dust template at 353. A cut is applied on the power of the signal
• residuals mask : cut for which the pixel have the largest residuals power :

{$ m = (1- \alpha_D - \alpha_S)^{-1} \cdot (\delta_D f_{353} + \delta_S f_{30} + \bar n_d + \alpha_D < n_D > + \alpha_S < n_S > $}

{$ v = (1- \alpha_D - \alpha_S)^{-2} \cdot (\sigma^2 (n_D) + \alpha_D^2 \sigma^2 (n_D) + \alpha_S^2 \sigma^2 (n_S) $}

{$ R = m / \sqrt(v / 300) $}

{$ \sqrt{R_Q^2 + R_U^2} $} is the map of the power of the residuals. A cute is applied on the sky based on the amplitude of the pixel of this map.

dust mask	residual mask

11.  white noise :

noise :

no noise :

12.  ffp10 noise :

dust mask :

residual mask :

13.  beam cosine test :

l2 = 3*nside-1

l1 = 2	l1 = 31