Difference between revisions of "Forecastfiso planck"

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Cl^{tot} = Cl^{ad} + f_iso^2 Cl^{cdm iso} + 2* f_iso * Cl^{correlated}
 
Cl^{tot} = Cl^{ad} + f_iso^2 Cl^{cdm iso} + 2* f_iso * Cl^{correlated}
  
where Cl^{cdm iso} is generated such that it has the same primordial power A_s as the scalar perturbations, and similarly for Cl^{correlated}.
+
where Cl^{cdm iso} is generated such that it has the same primordial power A_s as the scalar perturbations, and similarly for Cl^{correlated}. And the anti-correlated CDM modes contributes to the total spectrum in an analogous way.
 +
 
 +
== Forecast ==
 +
Cosmology used in the forecast LCDM + f_iso. Fiducial value of f_iso=0. Use lensed TT/EE/TE spectra.
 +
 
 +
=== Correlated CDM isocurvature ===
 +
* vary beam
 +
[[File: isocorr_varybeam.png |700px]]
 +
 
 +
* vary noise
 +
[[File: isocorr_varynoise.png |700px]]
 +
 
 +
* fixed effort
 +
[[File: isocorr_fixedeffort.png |700px]]
 +
 
 +
 
 +
=== Anti-correlated CDM isocurvature ===
 +
* vary beam
 +
[[File: isoanti_varybeam.png |700px]]
 +
 
 +
* vary noise
 +
[[File: isoanti_varynoise.png |700px]]
 +
 
 +
* fixed effort
 +
[[File: isoanti_fixedeffort.png |700px]]
 +
 
 +
 
  
 
== Planck test ==
 
== Planck test ==
 
To check that we are getting reasonable results, we run the Fisher matrix with LCDM+Mnu+f_iso with Planck noise levels, beams, and fsky as specified in previous forecast checks.  
 
To check that we are getting reasonable results, we run the Fisher matrix with LCDM+Mnu+f_iso with Planck noise levels, beams, and fsky as specified in previous forecast checks.  
  
We tested for fiducial cosmology f_iso=0 with CDM isocurvature modes; The following constraints use TT/EE/TE lensed spectra.
+
We tested for fiducial cosmology f_iso=0 with 100% correlated CDM isocurvature modes; The following constraints use TT/EE/TE lensed spectra.
  
 
The following are the constraints we get:
 
The following are the constraints we get:

Latest revision as of 19:45, 2 June 2016

Overview

We can improve constraints on isocurvature perturbations from Planck with observations from S4.

Here we consider the curvaton model: there is one isocurvature mode: the CDM isocurvature, and the spectral index of the CDM mode is the same as that of the adiabatic scalar perturbations, n_s. In this scenario, the CDM mode is either totally correlated or anti-correlated with the adiabatic perturbations.

The parameter we are constraining is f_iso, the primordial fraction of CDM isocurvature amplitude to the scalar perturbation amplitude. Specifically, the final spectra is

Cl^{tot} = Cl^{ad} + f_iso^2 Cl^{cdm iso} + 2* f_iso * Cl^{correlated}

where Cl^{cdm iso} is generated such that it has the same primordial power A_s as the scalar perturbations, and similarly for Cl^{correlated}. And the anti-correlated CDM modes contributes to the total spectrum in an analogous way.

Forecast

Cosmology used in the forecast LCDM + f_iso. Fiducial value of f_iso=0. Use lensed TT/EE/TE spectra.

Correlated CDM isocurvature

  • vary beam
Isocorr varybeam.png
  • vary noise
Isocorr varynoise.png
  • fixed effort
Isocorr fixedeffort.png


Anti-correlated CDM isocurvature

  • vary beam
Isoanti varybeam.png
  • vary noise
Isoanti varynoise.png
  • fixed effort
Isoanti fixedeffort.png


Planck test

To check that we are getting reasonable results, we run the Fisher matrix with LCDM+Mnu+f_iso with Planck noise levels, beams, and fsky as specified in previous forecast checks.

We tested for fiducial cosmology f_iso=0 with 100% correlated CDM isocurvature modes; The following constraints use TT/EE/TE lensed spectra.

The following are the constraints we get:

LCDM+Mnu+f_iso=0
och2 0.001523
obh2 0.000163
onuh2 0.005396
10^9 As 0.2589
ns 0.00486
tau 0.0597
hubble 4.84
f_iso 0.00391

We are doing a literature search to find previous forecasts that uses a similar parameterization (as opposed to the alpha or beta parameterization) to compare our results.