*** dlnP(k,z)/dz of Non-linear Matter Spectra from Peacock&Dodds (1996); Ma et al. (1999); and Halofit [Smith et al. (2003)] ***
January 1, 2012: E.Komatsu

There are two programs:

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I. "generate_pkz.f90"
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This program generates 2-dimensional arrays of non-linear matter power spectra, P(k,z), as a function of wavenumbers k [in units of h/Mpc] and redshifts z, using 3 different empirical prescriptions in the literature:

1. Peacock and Dodds, MNRAS, 280, L19 (1996), which uses the scaling argument developed by HKLM, calibrated to N-body simulations.
2. Ma et al., ApJL, 521, L1 (1999), which extends Peacock&Dodds by including effects of dynamical dark energy models.
3. Halofit [Smith et al., MNRAS, 341, 1311 (2003)], which uses a halo model calibrated to N-body simulations.

*** P(k) is in units of h^-3 Mpc^3, and k is in units of h Mpc^-1 ***
(This is the same as CAMB definition.)

In order to calculate non-linear power spectra, we need the input linear power spectrum. For this purpose we provide the sample data, "wmap5baosn_max_likelihood_matterpower.dat," which was generated using CAMB code for the maximum likelihood parameters given in Table I of Komatsu et al.(2008) [WMAP 5-year interpretation paper] with "WMAP5+BAO+SN". The input file for CAMB is also provided (wmap5baosn_max_likelihood_params.ini). NOTE THAT THIS POWER SPECTRUM IS COMPUTED AT Z=0.

Another power spectrum, evolved back to z=30, is provided as "wmap5baosn_max_likelihood_matterpower_at_z=30.dat".

In addition, we provide the linear power spectrum WITHOUT BARYONIC OSCILLATION, computed from Eisenstein&Hu's smooth transfer function. This was computed by "compute_pk_nowiggle," which is available also on CRL. The data are called "wavenumber_pknowiggle.txt" for z=0 and "wavenumber_pknowiggle_at_z=30.txt" for z=30.

Finally, we provide the non-linear power spectrum computed from the 3rd-order perturbation theory (3PT) for z=0, which can be compared with the outputs of this program. It is called "wavenumber_pkd_p11.txt" and the format is: (1st) wavenumber [h/Mpc]; (2nd) non-linear P(k) [Mpc^3/h^3]; (3rd) linear P(k )[Mpc^3/h^3]. These data were generated by "compute_pkd," which is available also on CRL.

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II. "compute_dlnpkdz.f90"
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This program reads in the arrays generated by "generate_pkz" and calculates dlnP(k,z)/dz as a function of z for a given input value of k [h Mpc^-1].

- To compile and use the program, edit Makefile and simply "make"
- It will generate executables called "generate_pkz" and "compute_dlnpkdz"
- Running "generate_pkz" will generate 3 output files:
  - redshift_wavenumber_pkpd96.txt: Peacock&Dodds (1996)
  - redshift_wavenumber_pkma99.txt: Ma et al. (1999)
  - redshift_wavenumber_pkhalofit.txt: Halofit [Smith et al. (2003)]

The format is
(1st) redshift
(2nd) wavenumber [h Mpc^-1]
(3nd) P(k,z) [h^-3 Mpc^3]

- Running "compute_dlnpkdz" will generate 3 output files:
  - redshift_dlnpkdzpd96.txt: Peacock&Dodds (1996)
  - redshift_dlnpkdzma99.txt: Ma et al. (1999)
  - redshift_dlnpkdzhalofit.txt: Halofit [Smith et al. (2003)]

The format is
(1st) redshift
(2nd) dlnP(k,z)/dz