Difference between revisions of "Update on Neff Forecasts"

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Dan writing
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Dan writing (input from Erminia, Joel and Alex)
  
I will present updates on the forecasting for N<sub>eff</sub>
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I will present updates on the forecasting for N<sub>eff</sub> and how it will impact the target of &sigma;(N<sub>eff</sub>) = 0.027.
 
.  
 
.  
 
== Temperature versus Polarization ==
 
== Temperature versus Polarization ==
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As shown in the figure below, TE drives the constraints for N<sub>eff</sub>.  Reaching the target is particularly sensitive to TE with l > 2000.
  
 
[[File:Low_ell_TE.png|500px]]
 
[[File:Low_ell_TE.png|500px]]
   
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A consequence of this statement is that our N<sub>eff</sub> is not particularly sensitive to component separation. Specifically, we can use Planck TT for l < 1500 and foregrounds in EE are sufficiently low to recover these constraint.  Detailed studies of component separation will be presented in a separate post, but this severs only to motivate why we have ignored it here.
 +
 
 
== Point Sources and Atmosphere ==
 
== Point Sources and Atmosphere ==
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Point sources act much like an additional source of noise (modulo the correction from the beam).  Point sources in TT therefore affect the information we can recover from both TT and TE at high-l.  We take the TT point source contribution to be
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D<sub>TT,ps</sub>(l=3000) = 6 ( &mu;K)&sup2;
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D<sub>EE,ps</sub>(l=3000) = 0.003&times; 6 ( &mu;K)&sup2;
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where we use the few percent polarization fraction of the point sources to estimate D<sub>EE,ps</sub>(l=3000).  In practice, the polarization fraction would have to be order 1 to have any effect on our forecasts. 
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We will determine that atmospheric noise from the model presented at the SLAC meeting:
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N<sub>l</sub><sup>TT</sup>= N<sub>0</sub><sup>TT</sup>(1+ (l /3400)<sup>-4.7</sup>)
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N<sub>l</sub><sup>EE</sup>= N<sub>0</sub><sup>EE</sup>(1+ (l /340)<sup>-4.7</sup>)
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where the factor of 10 reduction in l<sub>knee</sub><sup>EE</sup> was estimated from the polarization fraction. 
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[[File:S4_all.png|450px]] [[File:S4_atm.png|450px]]
 
[[File:S4_all.png|450px]] [[File:S4_atm.png|450px]]
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The impact of the point sources is more important at low noise, as the point sources at like an irreducible noise source in TT.  At higher noise, the atmosphere is more important as it
 +
 +
We can also consider the impact of the atmosphere in polarization by changing the model to
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N<sub>l</sub><sup>EE</sup>= N<sub>0</sub><sup>EE</sup>(1+ (l /l<sub>knee</sub>)<sup>&alpha;=-4.7, -4</sup>)
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[[File:Ell_knee_Neff.png|450px]] [[File:Ell_knee_ns.png|450px]]
 
[[File:Ell_knee_Neff.png|450px]] [[File:Ell_knee_ns.png|450px]]
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We noise that the atmosphere has a relatively small impact on N<sub>eff</sub>, presumably because the information is coming from smaller angular scales.  However, this is not a universal property of the cosmological parameters, as we can see from n<sub>s</sub>.
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'''Summary:'''  Reasonable expectations for point sources and atmosphere have a relatively small impact on our ability to reach the N<sub>eff</sub> target.  10 percent changes do occur, but this likely lies within the accuracy of the forecasts themselves.
  
 
== Beam / Pointing Calibration ==
 
== Beam / Pointing Calibration ==
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 +
  
 
[[File:S4_beam.png|500px]]
 
[[File:S4_beam.png|500px]]
  
 
[[File:Beam_shape.png|450px]] [[File:ACT_beam.png|450px]]
 
[[File:Beam_shape.png|450px]] [[File:ACT_beam.png|450px]]

Revision as of 18:08, 27 April 2017

Dan writing (input from Erminia, Joel and Alex)

I will present updates on the forecasting for Neff and how it will impact the target of σ(Neff) = 0.027. .

Temperature versus Polarization

As shown in the figure below, TE drives the constraints for Neff. Reaching the target is particularly sensitive to TE with l > 2000.

Low ell TE.png

A consequence of this statement is that our Neff is not particularly sensitive to component separation. Specifically, we can use Planck TT for l < 1500 and foregrounds in EE are sufficiently low to recover these constraint. Detailed studies of component separation will be presented in a separate post, but this severs only to motivate why we have ignored it here.

Point Sources and Atmosphere

Point sources act much like an additional source of noise (modulo the correction from the beam). Point sources in TT therefore affect the information we can recover from both TT and TE at high-l. We take the TT point source contribution to be

DTT,ps(l=3000) = 6 ( μK)²

DEE,ps(l=3000) = 0.003× 6 ( μK)²

where we use the few percent polarization fraction of the point sources to estimate DEE,ps(l=3000). In practice, the polarization fraction would have to be order 1 to have any effect on our forecasts.

We will determine that atmospheric noise from the model presented at the SLAC meeting:

NlTT= N0TT(1+ (l /3400)-4.7)

NlEE= N0EE(1+ (l /340)-4.7)

where the factor of 10 reduction in lkneeEE was estimated from the polarization fraction.


S4 all.png S4 atm.png

The impact of the point sources is more important at low noise, as the point sources at like an irreducible noise source in TT. At higher noise, the atmosphere is more important as it

We can also consider the impact of the atmosphere in polarization by changing the model to

NlEE= N0EE(1+ (l /lknee)α=-4.7, -4)


Ell knee Neff.png Ell knee ns.png

We noise that the atmosphere has a relatively small impact on Neff, presumably because the information is coming from smaller angular scales. However, this is not a universal property of the cosmological parameters, as we can see from ns.

Summary: Reasonable expectations for point sources and atmosphere have a relatively small impact on our ability to reach the Neff target. 10 percent changes do occur, but this likely lies within the accuracy of the forecasts themselves.

Beam / Pointing Calibration

S4 beam.png

Beam shape.png ACT beam.png