Difference between revisions of "W and gamma"

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(''Nick writing on behalf of Mat'')
 
(''Nick writing on behalf of Mat'')
  
From the sigma8(z) constraints posted here, we looked into how weel we can constrain w and delta gamma, where delta gamma is some
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From the sigma8(z) constraints posted here, we looked into how weel we can constrain w and delta gamma, where delta gamma quantifies a departure from the GR growth rate gamma ( see [https://arxiv.org/pdf/1201.2434.pdf Weinberg et al. 2012])
  
[https://arxiv.org/pdf/1201.2434.pdf Weinberg et al. 2012]
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[[File:s8resTP.png |800px]]
  
We've modified our cluster cosmology code to do sigma8(z). Here we are showing sigma8(z) constraints marginalized over LCDM and cluster scaling relation parameters using CMB halo lensing as the cluster mass calibration. For reference this is the same setup as the results shown on Feb 27th 2017 at SLAC. Note that for this telescope setup the 7m has a 1.3' beam at 150 GHz, and 5m has a 1.8' beam at 150 GHz. One addition over the past week is we are no include mass and redshift dependent scatter.
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Temperature plus polarization CMB Halo mass calibration
  
[[File:s8errs.png]]
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[[File:s8resP.png |800px]]
  
Here is sigma8(z) using optical weak lensing mass calibration (HSC-like WL survey)
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Polarization only CMB Halo mass calibration
  
[[File:s8errsowl.png]]
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If we
 
 
Following these results all the way through to mnu and w we get the results shown below
 
 
 
[[File:mnu_pars_CMBLens.png |800px]]
 
 
 
[[File:w_pars_CMBLens.png |800px]]
 

Revision as of 10:23, 15 March 2017

(Nick writing on behalf of Mat)

From the sigma8(z) constraints posted here, we looked into how weel we can constrain w and delta gamma, where delta gamma quantifies a departure from the GR growth rate gamma ( see Weinberg et al. 2012)

S8resTP.png

Temperature plus polarization CMB Halo mass calibration

S8resP.png

Polarization only CMB Halo mass calibration

If we