*** Mean Compton Y with Battaglia et al.(2012) Profile *** This version uses Battaglia et al.(2012)'s pressure profile, and attempts to reproduce the result presented in Hill et al., arXiv:1507.01583 August 2, 2015: E.Komatsu Ref: Barbosa, Bartlett, Blanchard & Oukbir, A&A, 314, 13 (1996) Battaglia et al., ApJ, 758, 75 (2012) Dolag, Komatsu & Sunyaev, arXiv:1509.05134 This code calculates the mean Compton Y: = int dz dV/dz int dlnM dn/dlnM Y where dV/dz is the comoving volume element, dn/dlnM is the halo mass function, and Y is the monopole of the 2d Fourier transform of the Compton Y profile. To compute the mean Y, it is necessary to use the linear matter power spectrum. We provide the sample data, "wmap9_matterpower.dat", which was generated using CAMB code for the WMAP9 "Combined data" parameters given in Table 2 of Hinshaw et al., ApJS, 208, 19 (2013). The input file for CAMB is also provided (wmap9_params.ini). NOTE THAT THIS POWER SPECTRUM IS COMPUTED AT Z=0. We also provide the matter power spectrum used by Magneticum Pathfinder Simulation in "wavenumber_pk_at_z=0_magneticum.txt". This power spectrum was generated by Eisentein&Hu's fitting function (which can be computed by one of the codes in CRL). Finally, we also provide the matter power spectrum of Planck2015 with lensing in "planck15_matterpower.dat". (The CAMB parameter file is "planck15_params.ini".) << NOTE ON NFW CONCENTRATION PARAMETER >> The default concentration parameter is Duffy et al. (2008): cvir=7.85d0*(mvir/2d12)**(-0.081)/(1d0+z)**0.71 You may also use the concentration parameter of Seljak (2000): cvir=10d0*(mvir/3.42d12)**(-0.2)/(1d0+z) which was originally used by Komatsu&Seljak (2002). << NOTE ON MASS FUNCTION >> The default mass function is Eq.(8)-(12) of Tinker et al. (2010) for Delta=200. Three more mass functions are provided: - Sheth&Tormen (mf_shethtormen.f90) - Jenkins et al. (mf_jenkins.f90; which was originally used by Komatsu&Seljak 2002). - Bocquet et al. with Delta=200m and "Hydro" - Bocquet et al. with Delta=200m and "DM Only" - Tinker et al. (2008) To use these mass functions, change the following: 1. In Makefile, change "mf_magneticum.o" to: "mf_jenkins.o", "mf_shethtormen.o", "mf_magneticum.o", "mf_magneticum_dm.o", "mf_tinker_redshift.o", or 2. For Jenkins et al. and Sherth&Tormen, change "mf(lnnu,z)" to "mf(lnnu)" in integrand.f90 [because Jenkins et al.'s and Sheth&Tormen's functions do not have explicit redshift dependence]. Specifically: dndlnRh=(3d0/4d0/pi)*dlnnudlnRh*mf(lnnu,z)/Rh**3d0 to dndlnRh=(3d0/4d0/pi)*dlnnudlnRh*mf(lnnu)/Rh**3d0 in integrand.f90. 3. Also, since Jenkins et al. use a different mass definition, you need to comment out ! Sheth&Tormen and Tinker et al.'s mass functions are given for the ! overdensity mass M200d (with respect to the mean mass density rather than ! the critical density). CALL mvir2mdel(mvir,rs,cvir,200d0*omega*rhoc,m200d) Rh=(3d0*m200d/4d0/pi/om0/2.775d11)**(1d0/3d0) ! h^-1 Mpc and use ! Alternatively, one may wish to use Jenkins et al.'s mass function, ! which is given for the overdensity mass M180d (with respect to the mean ! mass density rather than the critical density). CALL mvir2mdel(mvir,rs,cvir,180d0*omega*rhoc,m180d) in "integrand.f90". - To compile and use the program, edit Makefile and simply "make" - It will generate an executable called "meany" - Running meany will generate the data file called "redshift_dydln1pz_yz.txt", which contains: 1st: redshift 2nd: dY/dln(1+z) 3rd: Y(=1.606e-6,which is only slightly larger than the value found by Hill et al. (=1.583e-6).