Hi everyone,
1. I want to constrain a model for dark energy using only the background data, e.g. supernovae data. How can I use paramnames_background.paramnames file? Since Ωbh2 and Ω_ch2 have not been included in this file, I fixed both the omega_b.h2 and omega_c.h2 values and left the range for the derived parameter Ω_m in params_CMB.derived_ranges unchanged. Unfortunately, I'm not able to produce contours (even for LCDM) for H_0, Ω_m and ΩΛ like what we see for A. Reiss. Am I missing something here?
2. If I use HST dataset, should I change HST.F90 file for my time dependent dark energy equation of state w=w(a)? It looks like this likelihood is merely for LCDM.
Any help would be appreciated.
Problem with HST.f90 and using only Sn data.
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Re: Problem with HST.f90 and using only Sn data.
For pure background the result only depends on \Omega_m h^2, so \Omega_b h^2 can be fixed to any sensible value. \Omega_c h^2 is then determined via \Omega_m, H_0.
For funny dark energy models the local H0 measurements certainly don't necessarily translate into constraint on H(z=0). It would be better to use a constraint on the magnitude and combine with the supernovae. This is optional provided with Cobaya but not cosmomc by default.
For funny dark energy models the local H0 measurements certainly don't necessarily translate into constraint on H(z=0). It would be better to use a constraint on the magnitude and combine with the supernovae. This is optional provided with Cobaya but not cosmomc by default.