Merge branch 'master' of bitbucket.org:glavaux/cosmotool
This commit is contained in:
Guilhem Lavaux
commit
15a98787d2
@ -36,7 +36,7 @@ target_link_libraries(testPool ${tolink})
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if (HDF5_FOUND)
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include_directories(${HDF5_INCLUDE_PATH})
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SET(tolink ${tolink} ${ZLIB})
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SET(tolink ${tolink} ${HDF5_CPP_LIBRARY} ${HDF5_LIBRARY} ${ZLIB})
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add_executable(testReadFlash testReadFlash.cpp)
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target_link_libraries(testReadFlash ${tolink})
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@ -9,6 +9,7 @@ SET(CosmoTool_SRCS
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growthFactor.cpp
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cosmopower.cpp
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cic.cpp
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tf_fit.c
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)
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IF (Boost_FOUND)
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@ -109,6 +109,23 @@ static double powG(double y)
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return y * (-6 * a + (2 + 3 * y) *log((a + 1)/(a - 1)));
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}
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extern "C" {
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void TFset_parameters(float omega0hh, float f_baryon, float Tcmb);
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float TFfit_onek(float k, float *tf_baryon, float *tf_cdm);
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void TFfit_hmpc(float omega0, float f_baryon, float hubble, float Tcmb,
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int numk, float *k, float *tf_full, float *tf_baryon, float *tf_cdm);
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float TFsound_horizon_fit(float omega0, float f_baryon, float hubble);
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float TFk_peak(float omega0, float f_baryon, float hubble);
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float TFnowiggles(float omega0, float f_baryon, float hubble,
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float Tcmb, float k_hmpc);
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float TFzerobaryon(float omega0, float hubble, float Tcmb, float k_hmpc);
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}
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double CosmoPower::powerEfstathiou(double k)
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{
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double a = 6.4/Gamma0;
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@ -122,6 +139,12 @@ double CosmoPower::powerEfstathiou(double k)
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return normPower * pow(k,n) * pow(1+pow(f,nu),(-2/nu));
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}
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void CosmoPower::updateHuWigglesOriginal()
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{
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TFset_parameters( (OMEGA_C+OMEGA_B)*h*h,
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OMEGA_B/(OMEGA_C+OMEGA_B), Theta_27*2.7);
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}
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void CosmoPower::updateHuWigglesConsts()
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{
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double f_b = OMEGA_B / OMEGA_0;
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@ -343,6 +366,9 @@ double CosmoPower::power(double k)
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return (this->*eval)(k);
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}
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double CosmoPower::powerHuWigglesOriginal(double k)
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{
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}
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void CosmoPower::setFunction(CosmoFunction f)
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{
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@ -355,6 +381,10 @@ void CosmoPower::setFunction(CosmoFunction f)
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updateHuWigglesConsts();
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eval = &CosmoPower::powerHuWiggles;
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break;
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case HU_WIGGLES_ORIGINAL:
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updateHuWigglesOriginal();
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eval = &CosmoPower::powerHuWigglesOriginal;
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break;
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case HU_BARYON:
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eval = &CosmoPower::powerHuBaryons;
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break;
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@ -382,3 +412,4 @@ void CosmoPower::setNormalization(double A_K)
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{
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normPower = A_K;///power(0.002);
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}
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@ -83,7 +83,8 @@ namespace CosmoTool {
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POWER_BARDEEN,
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POWER_SUGIYAMA,
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POWER_BDM,
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POWER_TEST
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POWER_TEST,
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HU_WIGGLES_ORIGINAL
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};
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CosmoPower();
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@ -95,6 +96,7 @@ namespace CosmoTool {
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void normalize(double k_min = -1, double k_max = -1);
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void setNormalization(double A_K);
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void updateHuWigglesConsts();
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void updateHuWigglesOriginal();
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double eval_theta_theta(double k);
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double power(double k);
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@ -111,7 +113,7 @@ namespace CosmoTool {
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double powerSugiyama(double k);
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double powerBDM(double k);
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double powerTest(double k);
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double powerHuWigglesOriginal(double k);
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};
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};
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@ -36,6 +36,7 @@ knowledge of the CeCILL license and that you accept its terms.
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#ifndef __COSMOTOOLBOX_HPP
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#define __COSMOTOOLBOX_HPP
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#include <sys/types.h>
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#include <map>
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#include <string>
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337
src/tf_fit.c
Normal file
337
src/tf_fit.c
Normal file
@ -0,0 +1,337 @@
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/* The following routines implement all of the fitting formulae in
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Eisenstein \& Hu (1997) */
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/* There are two sets of routines here. The first set,
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TFfit_hmpc(), TFset_parameters(), and TFfit_onek(),
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calculate the transfer function for an arbitrary CDM+baryon universe using
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the fitting formula in Section 3 of the paper. The second set,
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TFsound_horizon_fit(), TFk_peak(), TFnowiggles(), and TFzerobaryon(),
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calculate other quantities given in Section 4 of the paper. */
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#include <math.h>
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#include <stdio.h>
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void TFset_parameters(float omega0hh, float f_baryon, float Tcmb);
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float TFfit_onek(float k, float *tf_baryon, float *tf_cdm);
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void TFfit_hmpc(float omega0, float f_baryon, float hubble, float Tcmb,
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int numk, float *k, float *tf_full, float *tf_baryon, float *tf_cdm);
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float TFsound_horizon_fit(float omega0, float f_baryon, float hubble);
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float TFk_peak(float omega0, float f_baryon, float hubble);
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float TFnowiggles(float omega0, float f_baryon, float hubble,
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float Tcmb, float k_hmpc);
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float TFzerobaryon(float omega0, float hubble, float Tcmb, float k_hmpc);
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/* ------------------------ DRIVER ROUTINE --------------------------- */
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/* The following is an example of a driver routine you might use. */
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/* Basically, the driver routine needs to call TFset_parameters() to
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set all the scalar parameters, and then call TFfit_onek() for each
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wavenumber k you desire. */
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/* While the routines use Mpc^-1 units internally, this driver has been
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written to take an array of wavenumbers in units of h Mpc^-1. On the
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other hand, if you want to use Mpc^-1 externally, you can do this by
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altering the variables you pass to the driver:
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omega0 -> omega0*hubble*hubble, hubble -> 1.0 */
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/* INPUT: omega0 -- the matter density (baryons+CDM) in units of critical
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f_baryon -- the ratio of baryon density to matter density
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hubble -- the Hubble constant, in units of 100 km/s/Mpc
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Tcmb -- the CMB temperature in Kelvin. T<=0 uses the COBE value 2.728.
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numk -- the length of the following zero-offset array
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k[] -- the array of wavevectors k[0..numk-1] */
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/* INPUT/OUTPUT: There are three output arrays of transfer functions.
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All are zero-offset and, if used, must have storage [0..numk-1] declared
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in the calling program. However, if you substitute the NULL pointer for
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one or more of the arrays, then that particular transfer function won't
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be outputted. The transfer functions are:
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tf_full[] -- The full fitting formula, eq. (16), for the matter
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transfer function.
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tf_baryon[] -- The baryonic piece of the full fitting formula, eq. 21.
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tf_cdm[] -- The CDM piece of the full fitting formula, eq. 17. */
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/* Again, you can set these pointers to NULL in the function call if
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you don't want a particular output. */
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/* Various intermediate scalar quantities are stored in global variables,
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so that you might more easily access them. However, this also means that
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you would be better off not simply #include'ing this file in your programs,
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but rather compiling it separately, calling only the driver, and using
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extern declarations to access the intermediate quantities. */
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/* ----------------------------- DRIVER ------------------------------- */
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void TFfit_hmpc(float omega0, float f_baryon, float hubble, float Tcmb,
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int numk, float *k, float *tf_full, float *tf_baryon, float *tf_cdm)
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/* Remember: k[0..numk-1] is in units of h Mpc^-1. */
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{
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int j;
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float tf_thisk, baryon_piece, cdm_piece;
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TFset_parameters(omega0*hubble*hubble, f_baryon, Tcmb);
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for (j=0;j<numk;j++) {
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tf_thisk = TFfit_onek(k[j]*hubble, &baryon_piece, &cdm_piece);
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if (tf_full!=NULL) tf_full[j] = tf_thisk;
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if (tf_baryon!=NULL) tf_baryon[j] = baryon_piece;
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if (tf_cdm!=NULL) tf_cdm[j] = cdm_piece;
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}
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return;
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}
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/* ------------------------ FITTING FORMULAE ROUTINES ----------------- */
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/* There are two routines here. TFset_parameters() sets all the scalar
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parameters, while TFfit_onek() calculates the transfer function for a
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given wavenumber k. TFfit_onek() may be called many times after a single
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call to TFset_parameters() */
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/* Global variables -- We've left many of the intermediate results as
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global variables in case you wish to access them, e.g. by declaring
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them as extern variables in your main program. */
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/* Note that all internal scales are in Mpc, without any Hubble constants! */
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float omhh, /* Omega_matter*h^2 */
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obhh, /* Omega_baryon*h^2 */
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theta_cmb, /* Tcmb in units of 2.7 K */
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z_equality, /* Redshift of matter-radiation equality, really 1+z */
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k_equality, /* Scale of equality, in Mpc^-1 */
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z_drag, /* Redshift of drag epoch */
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R_drag, /* Photon-baryon ratio at drag epoch */
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R_equality, /* Photon-baryon ratio at equality epoch */
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sound_horizon, /* Sound horizon at drag epoch, in Mpc */
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k_silk, /* Silk damping scale, in Mpc^-1 */
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alpha_c, /* CDM suppression */
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beta_c, /* CDM log shift */
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alpha_b, /* Baryon suppression */
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beta_b, /* Baryon envelope shift */
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beta_node, /* Sound horizon shift */
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k_peak, /* Fit to wavenumber of first peak, in Mpc^-1 */
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sound_horizon_fit, /* Fit to sound horizon, in Mpc */
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alpha_gamma; /* Gamma suppression in approximate TF */
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/* Convenience from Numerical Recipes in C, 2nd edition */
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static float sqrarg;
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#define SQR(a) ((sqrarg=(a)) == 0.0 ? 0.0 : sqrarg*sqrarg)
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static float cubearg;
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#define CUBE(a) ((cubearg=(a)) == 0.0 ? 0.0 : cubearg*cubearg*cubearg)
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static float pow4arg;
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#define POW4(a) ((pow4arg=(a)) == 0.0 ? 0.0 : pow4arg*pow4arg*pow4arg*pow4arg)
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/* Yes, I know the last one isn't optimal; it doesn't appear much */
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void TFset_parameters(float omega0hh, float f_baryon, float Tcmb)
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/* Set all the scalars quantities for Eisenstein & Hu 1997 fitting formula */
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/* Input: omega0hh -- The density of CDM and baryons, in units of critical dens,
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multiplied by the square of the Hubble constant, in units
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of 100 km/s/Mpc */
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/* f_baryon -- The fraction of baryons to CDM */
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/* Tcmb -- The temperature of the CMB in Kelvin. Tcmb<=0 forces use
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of the COBE value of 2.728 K. */
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/* Output: Nothing, but set many global variables used in TFfit_onek().
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You can access them yourself, if you want. */
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/* Note: Units are always Mpc, never h^-1 Mpc. */
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{
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float z_drag_b1, z_drag_b2;
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float alpha_c_a1, alpha_c_a2, beta_c_b1, beta_c_b2, alpha_b_G, y;
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if (f_baryon<=0.0 || omega0hh<=0.0) {
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fprintf(stderr, "TFset_parameters(): Illegal input.\n");
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exit(1);
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}
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omhh = omega0hh;
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obhh = omhh*f_baryon;
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if (Tcmb<=0.0) Tcmb=2.728; /* COBE FIRAS */
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theta_cmb = Tcmb/2.7;
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z_equality = 2.50e4*omhh/POW4(theta_cmb); /* Really 1+z */
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k_equality = 0.0746*omhh/SQR(theta_cmb);
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z_drag_b1 = 0.313*pow(omhh,-0.419)*(1+0.607*pow(omhh,0.674));
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z_drag_b2 = 0.238*pow(omhh,0.223);
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z_drag = 1291*pow(omhh,0.251)/(1+0.659*pow(omhh,0.828))*
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(1+z_drag_b1*pow(obhh,z_drag_b2));
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R_drag = 31.5*obhh/POW4(theta_cmb)*(1000/(1+z_drag));
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R_equality = 31.5*obhh/POW4(theta_cmb)*(1000/z_equality);
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sound_horizon = 2./3./k_equality*sqrt(6./R_equality)*
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log((sqrt(1+R_drag)+sqrt(R_drag+R_equality))/(1+sqrt(R_equality)));
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k_silk = 1.6*pow(obhh,0.52)*pow(omhh,0.73)*(1+pow(10.4*omhh,-0.95));
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alpha_c_a1 = pow(46.9*omhh,0.670)*(1+pow(32.1*omhh,-0.532));
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alpha_c_a2 = pow(12.0*omhh,0.424)*(1+pow(45.0*omhh,-0.582));
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alpha_c = pow(alpha_c_a1,-f_baryon)*
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pow(alpha_c_a2,-CUBE(f_baryon));
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beta_c_b1 = 0.944/(1+pow(458*omhh,-0.708));
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beta_c_b2 = pow(0.395*omhh, -0.0266);
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beta_c = 1.0/(1+beta_c_b1*(pow(1-f_baryon, beta_c_b2)-1));
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y = z_equality/(1+z_drag);
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alpha_b_G = y*(-6.*sqrt(1+y)+(2.+3.*y)*log((sqrt(1+y)+1)/(sqrt(1+y)-1)));
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alpha_b = 2.07*k_equality*sound_horizon*pow(1+R_drag,-0.75)*alpha_b_G;
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beta_node = 8.41*pow(omhh, 0.435);
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beta_b = 0.5+f_baryon+(3.-2.*f_baryon)*sqrt(pow(17.2*omhh,2.0)+1);
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k_peak = 2.5*3.14159*(1+0.217*omhh)/sound_horizon;
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sound_horizon_fit = 44.5*log(9.83/omhh)/sqrt(1+10.0*pow(obhh,0.75));
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alpha_gamma = 1-0.328*log(431.0*omhh)*f_baryon + 0.38*log(22.3*omhh)*
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SQR(f_baryon);
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return;
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}
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float TFfit_onek(float k, float *tf_baryon, float *tf_cdm)
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/* Input: k -- Wavenumber at which to calculate transfer function, in Mpc^-1.
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*tf_baryon, *tf_cdm -- Input value not used; replaced on output if
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the input was not NULL. */
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/* Output: Returns the value of the full transfer function fitting formula.
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This is the form given in Section 3 of Eisenstein & Hu (1997).
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*tf_baryon -- The baryonic contribution to the full fit.
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*tf_cdm -- The CDM contribution to the full fit. */
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/* Notes: Units are Mpc, not h^-1 Mpc. */
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{
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float T_c_ln_beta, T_c_ln_nobeta, T_c_C_alpha, T_c_C_noalpha;
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float q, xx, xx_tilde, q_eff;
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float T_c_f, T_c, s_tilde, T_b_T0, T_b, f_baryon, T_full;
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float T_0_L0, T_0_C0, T_0, gamma_eff;
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float T_nowiggles_L0, T_nowiggles_C0, T_nowiggles;
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k = fabs(k); /* Just define negative k as positive */
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if (k==0.0) {
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if (tf_baryon!=NULL) *tf_baryon = 1.0;
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if (tf_cdm!=NULL) *tf_cdm = 1.0;
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return 1.0;
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}
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q = k/13.41/k_equality;
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xx = k*sound_horizon;
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T_c_ln_beta = log(2.718282+1.8*beta_c*q);
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T_c_ln_nobeta = log(2.718282+1.8*q);
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T_c_C_alpha = 14.2/alpha_c + 386.0/(1+69.9*pow(q,1.08));
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T_c_C_noalpha = 14.2 + 386.0/(1+69.9*pow(q,1.08));
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|
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T_c_f = 1.0/(1.0+POW4(xx/5.4));
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T_c = T_c_f*T_c_ln_beta/(T_c_ln_beta+T_c_C_noalpha*SQR(q)) +
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(1-T_c_f)*T_c_ln_beta/(T_c_ln_beta+T_c_C_alpha*SQR(q));
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s_tilde = sound_horizon*pow(1+CUBE(beta_node/xx),-1./3.);
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xx_tilde = k*s_tilde;
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T_b_T0 = T_c_ln_nobeta/(T_c_ln_nobeta+T_c_C_noalpha*SQR(q));
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T_b = sin(xx_tilde)/(xx_tilde)*(T_b_T0/(1+SQR(xx/5.2))+
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alpha_b/(1+CUBE(beta_b/xx))*exp(-pow(k/k_silk,1.4)));
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f_baryon = obhh/omhh;
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T_full = f_baryon*T_b + (1-f_baryon)*T_c;
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/* Now to store these transfer functions */
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if (tf_baryon!=NULL) *tf_baryon = T_b;
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if (tf_cdm!=NULL) *tf_cdm = T_c;
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return T_full;
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}
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/* ======================= Approximate forms =========================== */
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float TFsound_horizon_fit(float omega0, float f_baryon, float hubble)
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/* Input: omega0 -- CDM density, in units of critical density
|
||||
f_baryon -- Baryon fraction, the ratio of baryon to CDM density.
|
||||
hubble -- Hubble constant, in units of 100 km/s/Mpc
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/* Output: The approximate value of the sound horizon, in h^-1 Mpc. */
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||||
/* Note: If you prefer to have the answer in units of Mpc, use hubble -> 1
|
||||
and omega0 -> omega0*hubble^2. */
|
||||
{
|
||||
float omhh, sound_horizon_fit_mpc;
|
||||
omhh = omega0*hubble*hubble;
|
||||
sound_horizon_fit_mpc =
|
||||
44.5*log(9.83/omhh)/sqrt(1+10.0*pow(omhh*f_baryon,0.75));
|
||||
return sound_horizon_fit_mpc*hubble;
|
||||
}
|
||||
|
||||
float TFk_peak(float omega0, float f_baryon, float hubble)
|
||||
/* Input: omega0 -- CDM density, in units of critical density
|
||||
f_baryon -- Baryon fraction, the ratio of baryon to CDM density.
|
||||
hubble -- Hubble constant, in units of 100 km/s/Mpc
|
||||
/* Output: The approximate location of the first baryonic peak, in h Mpc^-1 */
|
||||
/* Note: If you prefer to have the answer in units of Mpc^-1, use hubble -> 1
|
||||
and omega0 -> omega0*hubble^2. */
|
||||
{
|
||||
float omhh, k_peak_mpc;
|
||||
omhh = omega0*hubble*hubble;
|
||||
k_peak_mpc = 2.5*3.14159*(1+0.217*omhh)/TFsound_horizon_fit(omhh,f_baryon,1.0);
|
||||
return k_peak_mpc/hubble;
|
||||
}
|
||||
|
||||
float TFnowiggles(float omega0, float f_baryon, float hubble,
|
||||
float Tcmb, float k_hmpc)
|
||||
/* Input: omega0 -- CDM density, in units of critical density
|
||||
f_baryon -- Baryon fraction, the ratio of baryon to CDM density.
|
||||
hubble -- Hubble constant, in units of 100 km/s/Mpc
|
||||
Tcmb -- Temperature of the CMB in Kelvin; Tcmb<=0 forces use of
|
||||
COBE FIRAS value of 2.728 K
|
||||
k_hmpc -- Wavenumber in units of (h Mpc^-1). */
|
||||
/* Output: The value of an approximate transfer function that captures the
|
||||
non-oscillatory part of a partial baryon transfer function. In other words,
|
||||
the baryon oscillations are left out, but the suppression of power below
|
||||
the sound horizon is included. See equations (30) and (31). */
|
||||
/* Note: If you prefer to use wavenumbers in units of Mpc^-1, use hubble -> 1
|
||||
and omega0 -> omega0*hubble^2. */
|
||||
{
|
||||
float k, omhh, theta_cmb, k_equality, q, xx, alpha_gamma, gamma_eff;
|
||||
float q_eff, T_nowiggles_L0, T_nowiggles_C0;
|
||||
|
||||
k = k_hmpc*hubble; /* Convert to Mpc^-1 */
|
||||
omhh = omega0*hubble*hubble;
|
||||
if (Tcmb<=0.0) Tcmb=2.728; /* COBE FIRAS */
|
||||
theta_cmb = Tcmb/2.7;
|
||||
|
||||
k_equality = 0.0746*omhh/SQR(theta_cmb);
|
||||
q = k/13.41/k_equality;
|
||||
xx = k*TFsound_horizon_fit(omhh, f_baryon, 1.0);
|
||||
|
||||
alpha_gamma = 1-0.328*log(431.0*omhh)*f_baryon + 0.38*log(22.3*omhh)*
|
||||
SQR(f_baryon);
|
||||
gamma_eff = omhh*(alpha_gamma+(1-alpha_gamma)/(1+POW4(0.43*xx)));
|
||||
q_eff = q*omhh/gamma_eff;
|
||||
|
||||
T_nowiggles_L0 = log(2.0*2.718282+1.8*q_eff);
|
||||
T_nowiggles_C0 = 14.2 + 731.0/(1+62.5*q_eff);
|
||||
return T_nowiggles_L0/(T_nowiggles_L0+T_nowiggles_C0*SQR(q_eff));
|
||||
}
|
||||
|
||||
/* ======================= Zero Baryon Formula =========================== */
|
||||
|
||||
float TFzerobaryon(float omega0, float hubble, float Tcmb, float k_hmpc)
|
||||
/* Input: omega0 -- CDM density, in units of critical density
|
||||
hubble -- Hubble constant, in units of 100 km/s/Mpc
|
||||
Tcmb -- Temperature of the CMB in Kelvin; Tcmb<=0 forces use of
|
||||
COBE FIRAS value of 2.728 K
|
||||
k_hmpc -- Wavenumber in units of (h Mpc^-1). */
|
||||
/* Output: The value of the transfer function for a zero-baryon universe. */
|
||||
/* Note: If you prefer to use wavenumbers in units of Mpc^-1, use hubble -> 1
|
||||
and omega0 -> omega0*hubble^2. */
|
||||
{
|
||||
float k, omhh, theta_cmb, k_equality, q, T_0_L0, T_0_C0;
|
||||
|
||||
k = k_hmpc*hubble; /* Convert to Mpc^-1 */
|
||||
omhh = omega0*hubble*hubble;
|
||||
if (Tcmb<=0.0) Tcmb=2.728; /* COBE FIRAS */
|
||||
theta_cmb = Tcmb/2.7;
|
||||
|
||||
k_equality = 0.0746*omhh/SQR(theta_cmb);
|
||||
q = k/13.41/k_equality;
|
||||
|
||||
T_0_L0 = log(2.0*2.718282+1.8*q);
|
||||
T_0_C0 = 14.2 + 731.0/(1+62.5*q);
|
||||
return T_0_L0/(T_0_L0+T_0_C0*q*q);
|
||||
}
|
||||
Loading…
Reference in New Issue
Block a user