/*******************************************************************************
 * This file is part of SWIFT.
 * Copyright (c) 2017 Matthieu Schaller (schaller@strw.leidenuniv.nl)
 *
 * This program is free software: you can redistribute it and/or modify
 * it under the terms of the GNU Lesser General Public License as published
 * by the Free Software Foundation, either version 3 of the License, or
 * (at your option) any later version.
 *
 * This program is distributed in the hope that it will be useful,
 * but WITHOUT ANY WARRANTY; without even the implied warranty of
 * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE.  See the
 * GNU General Public License for more details.
 *
 * You should have received a copy of the GNU Lesser General Public License
 * along with this program.  If not, see <http://www.gnu.org/licenses/>.
 *
 ******************************************************************************/
/**
 * @file src/cooling/PS2020/cooling.c
 * @brief PS2020 cooling functions
 */

/* Config parameters. */
#include <config.h>

/* Some standard headers. */
#include <float.h>
#include <hdf5.h>
#include <math.h>
#include <time.h>

/* Local includes. */
#include "active.h"
#include "adiabatic_index.h"
#include "chemistry.h"
#include "cooling.h"
#include "cooling_rates.h"
#include "cooling_struct.h"
#include "cooling_subgrid.h"
#include "cooling_tables.h"
#include "entropy_floor.h"
#include "error.h"
#include "exp10.h"
#include "hydro.h"
#include "interpolate.h"
#include "io_properties.h"
#include "parser.h"
#include "part.h"
#include "physical_constants.h"
#include "space.h"
#include "star_formation.h"
#include "units.h"

/* Maximum number of iterations for
 * bisection integration schemes */
static const int bisection_max_iterations = 150;

/* Tolerances for termination criteria. */
static const float explicit_tolerance = 0.05;
static const float bisection_tolerance = 1.0e-6;
static const double bracket_factor = 1.5;

/**
 * @brief Common operations performed on the cooling function at a
 * given time-step or redshift. Predominantly used to read cooling tables
 * above and below the current redshift, if not already read in.
 *
 * Also calls the additional H reionisation energy injection if need be.
 *
 * @param cosmo The current cosmological model.
 * @param pressure_floor Properties of the pressure floor.
 * @param cooling The #cooling_function_data used in the run.
 * @param s The space data, including a pointer to array of particles
 */
void cooling_update(const struct cosmology *cosmo,
                    const struct pressure_floor_props *pressure_floor,
                    struct cooling_function_data *cooling, struct space *s) {

  /* Extra energy for reionization? */
  if (!cooling->H_reion_done) {

    /* Does this timestep straddle Hydrogen reionization? If so, we need to
     * input extra heat */
    if (cosmo->z <= cooling->H_reion_z && cosmo->z_old > cooling->H_reion_z) {

      if (s == NULL) error("Trying to do H reionization on an empty space!");

      /* Inject energy to all particles */
      cooling_Hydrogen_reionization(cooling, cosmo, pressure_floor, s);

      /* Flag that reionization happened */
      cooling->H_reion_done = 1;
    }
  }
}

/**
 * @brief Compute the internal energy of a #part based on the cooling function
 * but for a given temperature.
 *
 * This is used e.g. for particles in HII regions that are set to a constant
 * temperature, but their internal energies should reflect the particle
 * composition .
 *
 * @param phys_const #phys_const data structure.
 * @param hydro_props The properties of the hydro scheme.
 * @param us The internal system of units.
 * @param cosmo #cosmology data structure.
 * @param cooling #cooling_function_data struct.
 * @param p #part data.
 * @param xp Pointer to the #xpart data.
 * @param T temperature of the gas (internal units).
 */
float cooling_get_internalenergy_for_temperature(
    const struct phys_const *phys_const, const struct hydro_props *hydro_props,
    const struct unit_system *us, const struct cosmology *cosmo,
    const struct cooling_function_data *cooling, const struct part *p,
    const struct xpart *xp, const float T) {

#ifdef SWIFT_DEBUG_CHECKS
  if (cooling->Redshifts == NULL)
    error(
        "Cooling function has not been initialised. Did you forget the "
        "--temperature runtime flag?");
#endif

  /* Get the Hydrogen mass fraction */
  float const *metal_fraction =
      chemistry_get_metal_mass_fraction_for_cooling(p);
  const float XH = metal_fraction[chemistry_element_H];

  /* Normal case --> Interpolate the table */

  /* Convert Hydrogen mass fraction into Hydrogen number density */
  const float rho = hydro_get_physical_density(p, cosmo);
  const double n_H = rho * XH / phys_const->const_proton_mass;
  const double n_H_cgs = n_H * cooling->number_density_to_cgs;

  /* Get this particle's metallicity ratio to solar.
   *
   * Note that we do not need the individual element's ratios that
   * the function also computes. */
  float dummy[colibre_cooling_N_elementtypes];
  const float logZZsol = abundance_ratio_to_solar(p, cooling, dummy);

  /* compute hydrogen number density, metallicity and redshift indices and
   * offsets  */

  float d_red, d_met, d_n_H;
  int red_index, met_index, n_H_index;

  get_index_1d(cooling->Redshifts, colibre_cooling_N_redshifts, cosmo->z,
               &red_index, &d_red);
  get_index_1d(cooling->Metallicity, colibre_cooling_N_metallicity, logZZsol,
               &met_index, &d_met);
  get_index_1d(cooling->nH, colibre_cooling_N_density, log10(n_H_cgs),
               &n_H_index, &d_n_H);

  /* Compute the log10 of the temperature by interpolating the table */
  const double log_10_U =
      colibre_convert_temp_to_u(log10(T), cosmo->z, n_H_index, d_n_H, met_index,
                                d_met, red_index, d_red, cooling);

  /* Undo the log! */
  return exp10(log_10_U);
}

/**
 * @brief Compute the temperature based on gas properties.
 *
 * The temperature returned is consistent with the cooling rates.
 *
 * @param phys_const #phys_const data structure.
 * @param cosmo #cosmology data structure.
 * @param cooling #cooling_function_data struct.
 * @param rho_phys Density of the gas in internal physical units.
 * @param logZZsol Logarithm base 10 of the gas' metallicity in units of solar
 * metallicity.
 * @param XH The Hydrogen abundance of the gas.
 * @param u_phys Internal energy of the gas in internal physical units.
 * @param HII_region Is this patch of gas in an HII region?
 */
float cooling_get_temperature_from_gas(
    const struct phys_const *phys_const, const struct cosmology *cosmo,
    const struct cooling_function_data *cooling, const float rho_phys,
    const float logZZsol, const float XH, const float u_phys,
    const int HII_region) {

  if (HII_region)
    error("HII regions are not implemented in the EAGLE-XL flavour");

  /* Convert to CGS */
  const double u_cgs = u_phys * cooling->internal_energy_to_cgs;

  /* Get density in Hydrogen number density */
  const double n_H = rho_phys * XH / phys_const->const_proton_mass;
  const double n_H_cgs = n_H * cooling->number_density_to_cgs;

  /* Normal case --> Interpolate the table */

  /* compute hydrogen number density, metallicity and redshift indices and
   * offsets  */
  float d_red, d_met, d_n_H;
  int red_index, met_index, n_H_index;

  get_index_1d(cooling->Redshifts, colibre_cooling_N_redshifts, cosmo->z,
               &red_index, &d_red);
  get_index_1d(cooling->Metallicity, colibre_cooling_N_metallicity, logZZsol,
               &met_index, &d_met);
  get_index_1d(cooling->nH, colibre_cooling_N_density, log10(n_H_cgs),
               &n_H_index, &d_n_H);

  /* Compute the log10 of the temperature by interpolating the table */
  const double log_10_T =
      colibre_convert_u_to_temp(log10(u_cgs), cosmo->z, n_H_index, d_n_H,
                                met_index, d_met, red_index, d_red, cooling);

  /* Undo the log! */
  return exp10(log_10_T);
}

/**
 * @brief Compute the temperature of a #part based on the cooling function.
 *
 * The temperature returned is consistent with the cooling rates or
 * is the temperature of an HII region if the particle is flagged as such.
 *
 * @param phys_const #phys_const data structure.
 * @param hydro_props The properties of the hydro scheme.
 * @param us The internal system of units.
 * @param cosmo #cosmology data structure.
 * @param cooling #cooling_function_data struct.
 * @param p #part data.
 * @param xp Pointer to the #xpart data.
 */
float cooling_get_temperature(const struct phys_const *phys_const,
                              const struct hydro_props *hydro_props,
                              const struct unit_system *us,
                              const struct cosmology *cosmo,
                              const struct cooling_function_data *cooling,
                              const struct part *p, const struct xpart *xp) {

#ifdef SWIFT_DEBUG_CHECKS
  if (cooling->Redshifts == NULL)
    error(
        "Cooling function has not been initialised. Did you forget the "
        "--temperature runtime flag?");
#endif

  /* Get quantities in physical frame */
  const float u_phys = hydro_get_physical_internal_energy(p, xp, cosmo);
  const float rho_phys = hydro_get_physical_density(p, cosmo);

  /* Get the Hydrogen mass fraction */
  float const *metal_fraction =
      chemistry_get_metal_mass_fraction_for_cooling(p);
  const float XH = metal_fraction[chemistry_element_H];

  /* Get this particle's metallicity ratio to solar.
   *
   * Note that we do not need the individual element's ratios that
   * the function also computes. */
  float dummy[colibre_cooling_N_elementtypes];
  const float logZZsol = abundance_ratio_to_solar(p, cooling, dummy);

  /* Are we in an HII region? */
  const int HII_region = 0; /* No HII regions in the EAGLE-XL flavour */

  return cooling_get_temperature_from_gas(phys_const, cosmo, cooling, rho_phys,
                                          logZZsol, XH, u_phys, HII_region);
}

/**
 * @brief Compute the electron number density of a #part based on the cooling
 * function.
 *
 * The electron density returned is in physical internal units.
 *
 * Note that particles that are star-forming are ignored and
 * will return an electron density of zero.
 *
 * @param phys_const #phys_const data structure.
 * @param hydro_props The properties of the hydro scheme.
 * @param us The internal system of units.
 * @param cosmo #cosmology data structure.
 * @param cooling #cooling_function_data struct.
 * @param p #part data.
 * @param xp Pointer to the #xpart data.
 */
double cooling_get_electron_density(const struct phys_const *phys_const,
                                    const struct hydro_props *hydro_props,
                                    const struct unit_system *us,
                                    const struct cosmology *cosmo,
                                    const struct cooling_function_data *cooling,
                                    const struct part *p,
                                    const struct xpart *xp) {

  /* Do not include star-forming particles */
  if (star_formation_get_SFR(p, xp) > 0) return 0.;

  /* Get quantities in physical frame */
  const float u_phys = hydro_get_physical_internal_energy(p, xp, cosmo);
  const float rho_phys = hydro_get_physical_density(p, cosmo);

  /* Get the Hydrogen mass fraction */
  float const *metal_fraction =
      chemistry_get_metal_mass_fraction_for_cooling(p);
  const float XH = metal_fraction[chemistry_element_H];

  /* Get this particle's metallicity ratio to solar. */
  float abundance_ratio[colibre_cooling_N_elementtypes];
  const float logZZsol = abundance_ratio_to_solar(p, cooling, abundance_ratio);

  /* Convert to CGS */
  const double u_cgs = u_phys * cooling->internal_energy_to_cgs;
  const double log10_u_cgs = log10(u_cgs);

  /* Get density in Hydrogen number density */
  const double n_H = rho_phys * XH / phys_const->const_proton_mass;
  const double n_H_cgs = n_H * cooling->number_density_to_cgs;

  /* compute hydrogen number density, metallicity and redshift indices and
   * offsets  */
  float d_red, d_met, d_n_H;
  int red_index, met_index, n_H_index;

  get_index_1d(cooling->Redshifts, colibre_cooling_N_redshifts, cosmo->z,
               &red_index, &d_red);
  get_index_1d(cooling->Metallicity, colibre_cooling_N_metallicity, logZZsol,
               &met_index, &d_met);
  get_index_1d(cooling->nH, colibre_cooling_N_density, log10(n_H_cgs),
               &n_H_index, &d_n_H);

  /* Compute the electron density in CGS by interpolating the table */
  const double n_e_cgs = colibre_electron_density(
      log10_u_cgs, cosmo->z, n_H_cgs, abundance_ratio, n_H_index, d_n_H,
      met_index, d_met, red_index, d_red, cooling);

  /* Convert back to internal units */
  const double n_e = n_e_cgs / cooling->number_density_to_cgs;

  return n_e;
}

/**
 * @brief Compute the electron pressure of a #part based on the cooling
 * function.
 *
 * Returns the total electron pressure of the particle, P_e * V, in code units.
 * Note that particles that are star-forming are ignored and
 * will return an electron pressure of zero.
 *
 * @param phys_const #phys_const data structure.
 * @param hydro_props The properties of the hydro scheme.
 * @param us The internal system of units.
 * @param cosmo #cosmology data structure.
 * @param cooling #cooling_function_data struct.
 * @param p #part data.
 * @param xp Pointer to the #xpart data.
 */
double cooling_get_electron_pressure(
    const struct phys_const *phys_const, const struct hydro_props *hydro_props,
    const struct unit_system *us, const struct cosmology *cosmo,
    const struct cooling_function_data *cooling, const struct part *p,
    const struct xpart *xp) {

#ifdef SWIFT_DEBUG_CHECKS
  if (cooling->Redshifts == NULL)
    error(
        "Cooling function has not been initialised. Did you forget the "
        "--temperature runtime flag?");
#endif

  /* Do not include star-forming particles */
  if (star_formation_get_SFR(p, xp) > 0) return 0.;

  /* Get quantities in physical frame */
  const float u_phys = hydro_get_physical_internal_energy(p, xp, cosmo);
  const float rho_phys = hydro_get_physical_density(p, cosmo);

  /* Get the Hydrogen mass fraction */
  float const *metal_fraction =
      chemistry_get_metal_mass_fraction_for_cooling(p);
  const float XH = metal_fraction[chemistry_element_H];

  /* Get density in Hydrogen number density */
  const double n_H = rho_phys * XH / phys_const->const_proton_mass;
  const double n_H_cgs = n_H * cooling->number_density_to_cgs;

  /* Get this particle's metallicity ratio to solar.
   *
   * Note that we do not need the individual element's ratios that
   * the function also computes. */
  float abundance_ratio[colibre_cooling_N_elementtypes];
  const float logZZsol = abundance_ratio_to_solar(p, cooling, abundance_ratio);

  /* Convert to CGS */
  const double u_cgs = u_phys * cooling->internal_energy_to_cgs;
  const double log_u_cgs = log10(u_cgs);

  /* Compute hydrogen number density, metallicity and redshift indices and
   * offsets */
  float d_red, d_met, d_n_H, d_U;
  int red_index, met_index, n_H_index, U_index;

  get_index_1d(cooling->Redshifts, colibre_cooling_N_redshifts, cosmo->z,
               &red_index, &d_red);
  get_index_1d(cooling->Metallicity, colibre_cooling_N_metallicity, logZZsol,
               &met_index, &d_met);
  get_index_1d(cooling->nH, colibre_cooling_N_density, log10(n_H_cgs),
               &n_H_index, &d_n_H);
  get_index_1d(cooling->Therm, colibre_cooling_N_internalenergy, log_u_cgs,
               &U_index, &d_U);

  /* n_e / n_H */
  const double electron_fraction = interpolation4d_plus_summation(
      cooling->table.Uelectron_fraction, abundance_ratio, element_H,
      colibre_cooling_N_electrontypes - 4, red_index, U_index, met_index,
      n_H_index, d_red, d_U, d_met, d_n_H, colibre_cooling_N_redshifts,
      colibre_cooling_N_internalenergy, colibre_cooling_N_metallicity,
      colibre_cooling_N_density, colibre_cooling_N_electrontypes);

  const double num_H = hydro_get_mass(p) * XH / phys_const->const_proton_mass;

  /* Interpolate the temperature */
  const double log_10_T =
      colibre_convert_u_to_temp(log_u_cgs, cosmo->z, n_H_index, d_n_H,
                                met_index, d_met, red_index, d_red, cooling);

  return num_H * electron_fraction * phys_const->const_boltzmann_k *
         exp10(log_10_T);
}

/**
 * @brief Compute the y-Compton contribution of a #part based on the cooling
 * function.
 *
 * This is eq. (2) of McCarthy et al. (2017).
 *
 * Note that particles that are star-forming are ignored and
 * will return a Compton Y value of 0.
 *
 * @param phys_const #phys_const data structure.
 * @param hydro_props The properties of the hydro scheme.
 * @param us The internal system of units.
 * @param cosmo #cosmology data structure.
 * @param cooling #cooling_function_data struct.
 * @param p #part data.
 * @param xp Pointer to the #xpart data.
 */
double cooling_get_ycompton(const struct phys_const *phys_const,
                            const struct hydro_props *hydro_props,
                            const struct unit_system *us,
                            const struct cosmology *cosmo,
                            const struct cooling_function_data *cooling,
                            const struct part *p, const struct xpart *xp) {

  /* Do not include star-forming particles */
  if (star_formation_get_SFR(p, xp) > 0) return 0.;

  /* Get quantities in physical frame */
  const float u_phys = hydro_get_physical_internal_energy(p, xp, cosmo);
  const float rho_phys = hydro_get_physical_density(p, cosmo);
  const double m = hydro_get_mass(p);

  /* Get the Hydrogen mass fraction */
  float const *metal_fraction =
      chemistry_get_metal_mass_fraction_for_cooling(p);
  const float XH = metal_fraction[chemistry_element_H];

  /* Get this particle's metallicity ratio to solar. */
  float abundance_ratio[colibre_cooling_N_elementtypes];
  const float logZZsol = abundance_ratio_to_solar(p, cooling, abundance_ratio);

  /* Convert to CGS */
  const double u_cgs = u_phys * cooling->internal_energy_to_cgs;
  const double log10_u_cgs = log10(u_cgs);

  /* Get density in Hydrogen number density */
  const double n_H = rho_phys * XH / phys_const->const_proton_mass;
  const double n_H_cgs = n_H * cooling->number_density_to_cgs;

  /* compute hydrogen number density, metallicity and redshift indices and
   * offsets  */
  float d_red, d_met, d_n_H;
  int red_index, met_index, n_H_index;

  get_index_1d(cooling->Redshifts, colibre_cooling_N_redshifts, cosmo->z,
               &red_index, &d_red);
  get_index_1d(cooling->Metallicity, colibre_cooling_N_metallicity, logZZsol,
               &met_index, &d_met);
  get_index_1d(cooling->nH, colibre_cooling_N_density, log10(n_H_cgs),
               &n_H_index, &d_n_H);

  /* Compute the log10 of the temperature by interpolating the table */
  const double log10_T =
      colibre_convert_u_to_temp(log10_u_cgs, cosmo->z, n_H_index, d_n_H,
                                met_index, d_met, red_index, d_red, cooling);

  /* Compute the electron density in CGS by interpolating the table */
  const double n_e_cgs = colibre_electron_density(
      log10_u_cgs, cosmo->z, n_H_cgs, abundance_ratio, n_H_index, d_n_H,
      met_index, d_met, red_index, d_red, cooling);

  /* Convert back to internal units */
  const double n_e = n_e_cgs / cooling->number_density_to_cgs;

  return cooling->y_compton_factor * exp10(log10_T) * m * n_e / rho_phys;
}

/**
 * @brief Bisection integration scheme
 *
 * @param u_ini_cgs Internal energy at beginning of hydro step in CGS.
 * @param n_H_cgs Hydrogen number density in CGS.
 * @param redshift Current redshift.
 * @param n_H_index Particle hydrogen number density index.
 * @param d_n_H Particle hydrogen number density offset.
 * @param met_index Particle metallicity index.
 * @param d_met Particle metallicity offset.
 * @param red_index Redshift index.
 * @param d_red Redshift offset.
 * @param Lambda_He_reion_cgs Cooling rate coming from He reionization.
 * @param ratefact_cgs Multiplication factor to get a cooling rate.
 * @param cooling #cooling_function_data structure.
 * @param abundance_ratio Array of ratios of metal abundance to solar.
 * @param dt_cgs timestep in CGS.
 * @param ID ID of the particle (for debugging).
 */
static INLINE double bisection_iter(
    const double u_ini_cgs, const double n_H_cgs, const double redshift,
    int n_H_index, float d_n_H, int met_index, float d_met, int red_index,
    float d_red, double Lambda_He_reion_cgs, double ratefact_cgs,
    const struct cooling_function_data *cooling,
    const float abundance_ratio[colibre_cooling_N_elementtypes], double dt_cgs,
    long long ID) {

  /* Bracketing */
  double u_lower_cgs = max(u_ini_cgs, cooling->umin_cgs);
  double u_upper_cgs = max(u_ini_cgs, cooling->umin_cgs);

  /*************************************/
  /* Let's get a first guess           */
  /*************************************/

  double LambdaNet_cgs =
      Lambda_He_reion_cgs +
      colibre_cooling_rate(log10(u_ini_cgs), redshift, n_H_cgs, abundance_ratio,
                           n_H_index, d_n_H, met_index, d_met, red_index, d_red,
                           cooling, 0, 0, 0, 0);

  /*************************************/
  /* Let's try to bracket the solution */
  /*************************************/

  if (LambdaNet_cgs < 0) {

    /* we're cooling! */
    u_lower_cgs = max(u_lower_cgs / bracket_factor, cooling->umin_cgs);
    u_upper_cgs = max(u_upper_cgs * bracket_factor, cooling->umin_cgs);

    /* Compute a new rate */
    LambdaNet_cgs =
        Lambda_He_reion_cgs +
        colibre_cooling_rate(log10(u_lower_cgs), redshift, n_H_cgs,
                             abundance_ratio, n_H_index, d_n_H, met_index,
                             d_met, red_index, d_red, cooling, 0, 0, 0, 0);

    int i = 0;
    while (u_lower_cgs - u_ini_cgs - LambdaNet_cgs * ratefact_cgs * dt_cgs >
               0 &&
           i < bisection_max_iterations) {

      u_lower_cgs = max(u_lower_cgs / bracket_factor, cooling->umin_cgs);
      u_upper_cgs = max(u_upper_cgs / bracket_factor, cooling->umin_cgs);

      /* Compute a new rate */
      LambdaNet_cgs =
          Lambda_He_reion_cgs +
          colibre_cooling_rate(log10(u_lower_cgs), redshift, n_H_cgs,
                               abundance_ratio, n_H_index, d_n_H, met_index,
                               d_met, red_index, d_red, cooling, 0, 0, 0, 0);

      /* If the energy is below or equal the minimum energy and we are still
       * cooling, return the minimum energy */
      if ((u_lower_cgs <= cooling->umin_cgs) && (LambdaNet_cgs < 0.))
        return cooling->umin_cgs;

      i++;
    }

    if (i >= bisection_max_iterations) {
      error(
          "particle %llu exceeded max iterations searching for bounds when "
          "cooling \n more info: n_H_cgs = %.4e, u_ini_cgs = %.4e, redshift = "
          "%.4f\n"
          "n_H_index = %i, d_n_H = %.4f\n"
          "met_index = %i, d_met = %.4f, red_index = %i, d_red = %.4f, initial "
          "Lambda = %.4e",
          ID, n_H_cgs, u_ini_cgs, redshift, n_H_index, d_n_H, met_index, d_met,
          red_index, d_red,
          colibre_cooling_rate(log10(u_ini_cgs), redshift, n_H_cgs,
                               abundance_ratio, n_H_index, d_n_H, met_index,
                               d_met, red_index, d_red, cooling, 0, 0, 0, 0));
    }
  } else {

    /* we are heating! */
    u_lower_cgs /= bracket_factor;
    u_upper_cgs *= bracket_factor;

    /* Compute a new rate */
    LambdaNet_cgs =
        Lambda_He_reion_cgs +
        colibre_cooling_rate(log10(u_upper_cgs), redshift, n_H_cgs,
                             abundance_ratio, n_H_index, d_n_H, met_index,
                             d_met, red_index, d_red, cooling, 0, 0, 0, 0);

    int i = 0;
    while (u_upper_cgs - u_ini_cgs - LambdaNet_cgs * ratefact_cgs * dt_cgs <
               0 &&
           i < bisection_max_iterations) {

      u_lower_cgs *= bracket_factor;
      u_upper_cgs *= bracket_factor;

      /* Compute a new rate */
      LambdaNet_cgs =
          Lambda_He_reion_cgs +
          colibre_cooling_rate(log10(u_upper_cgs), redshift, n_H_cgs,
                               abundance_ratio, n_H_index, d_n_H, met_index,
                               d_met, red_index, d_red, cooling, 0, 0, 0, 0);
      i++;
    }

    if (i >= bisection_max_iterations) {
      message("Aborting...");
      message("particle %llu", ID);
      message("n_H_cgs = %.4e", n_H_cgs);
      message("u_ini_cgs = %.4e", u_ini_cgs);
      message("redshift = %.4f", redshift);
      message("indices nH, met, red = %i, %i, %i", n_H_index, met_index,
              red_index);
      message("index weights nH, met, red = %.4e, %.4e, %.4e", d_n_H, d_met,
              d_red);
      fflush(stdout);
      message(
          "cooling rate = %.4e",
          colibre_cooling_rate(log10(u_ini_cgs), redshift, n_H_cgs,
                               abundance_ratio, n_H_index, d_n_H, met_index,
                               d_met, red_index, d_red, cooling, 0, 0, 0, 0));
      error(
          "particle %llu exceeded max iterations searching for bounds when "
          "cooling",
          ID);
    }
  }

  /********************************************/
  /* We now have an upper and lower bound.    */
  /* Let's iterate by reducing the bracketing */
  /********************************************/

  /* bisection iteration */
  int i = 0;
  double u_next_cgs;

  do {

    /* New guess */
    u_next_cgs = 0.5 * (u_lower_cgs + u_upper_cgs);

    /* New rate */
    LambdaNet_cgs =
        Lambda_He_reion_cgs +
        colibre_cooling_rate(log10(u_next_cgs), redshift, n_H_cgs,
                             abundance_ratio, n_H_index, d_n_H, met_index,
                             d_met, red_index, d_red, cooling, 0, 0, 0, 0);

    /* Where do we go next? */
    if (u_next_cgs - u_ini_cgs - LambdaNet_cgs * ratefact_cgs * dt_cgs > 0.0) {
      u_upper_cgs = u_next_cgs;
    } else {
      u_lower_cgs = u_next_cgs;
    }

    i++;
  } while (fabs(u_upper_cgs - u_lower_cgs) / u_next_cgs > bisection_tolerance &&
           i < bisection_max_iterations);

  if (i >= bisection_max_iterations)
    error("Particle id %llu failed to converge", ID);

  return u_upper_cgs;
}

/**
 * @brief Apply the cooling function to a particle.
 *
 * We want to compute u_new such that u_new = u_old + dt * du/dt(u_new, X),
 * where X stands for the metallicity, density and redshift. These are
 * kept constant.
 *
 * We first compute du/dt(u_old). If dt * du/dt(u_old) is small enough, we
 * use an explicit integration and use this as our solution.
 *
 * Otherwise, we try to find a solution to the implicit time-integration
 * problem. This leads to the root-finding problem:
 *
 * f(u_new) = u_new - u_old - dt * du/dt(u_new, X) = 0
 *
 * A bisection scheme is used.
 * This is done by first bracketing the solution and then iterating
 * towards the solution by reducing the window down to a certain tolerance.
 * Note there is always at least one solution since
 * f(+inf) is < 0 and f(-inf) is > 0.
 *
 * @param phys_const The physical constants in internal units.
 * @param us The internal system of units.
 * @param cosmo The current cosmological model.
 * @param hydro_properties the hydro_props struct
 * @param floor_props Properties of the entropy floor.
 * @param pressure_floor Properties of the pressure floor.
 * @param cooling The #cooling_function_data used in the run.
 * @param p Pointer to the particle data.
 * @param xp Pointer to the extended particle data.
 * @param dt The cooling time-step of this particle.
 * @param dt_therm The hydro time-step of this particle.
 * @param time Time since Big Bang
 */
void cooling_cool_part(const struct phys_const *phys_const,
                       const struct unit_system *us,
                       const struct cosmology *cosmo,
                       const struct hydro_props *hydro_properties,
                       const struct entropy_floor_properties *floor_props,
                       const struct pressure_floor_props *pressure_floor,
                       const struct cooling_function_data *cooling,
                       struct part *p, struct xpart *xp, const float dt,
                       const float dt_therm, const double time) {

  /* No cooling happens over zero time */
  if (dt == 0.) {

    /* But we still set the subgrid properties to a valid state */
    cooling_set_particle_subgrid_properties(
        phys_const, us, cosmo, hydro_properties, floor_props, cooling, p, xp);

    return;
  }

#ifdef SWIFT_DEBUG_CHECKS
  if (cooling->Redshifts == NULL)
    error(
        "Cooling function has not been initialised. Did you forget the "
        "--cooling runtime flag?");
#endif

  /* Get internal energy at the last kick step */
  const float u_start = hydro_get_physical_internal_energy(p, xp, cosmo);

  /* Get the change in internal energy due to hydro forces */
  const float hydro_du_dt = hydro_get_physical_internal_energy_dt(p, cosmo);

  /* Get internal energy at the end of the next kick step (assuming dt does not
   * increase) */
  double u_0 = (u_start + hydro_du_dt * dt_therm);

  /* Check for minimal energy */
  u_0 = max(u_0, hydro_properties->minimal_internal_energy);

  /* Convert to CGS units */
  const double u_0_cgs = u_0 * cooling->internal_energy_to_cgs;
  const double dt_cgs = dt * units_cgs_conversion_factor(us, UNIT_CONV_TIME);

  /* Change in redshift over the course of this time-step
     (See cosmology theory document for the derivation) */
  const double delta_redshift = -dt * cosmo->H * cosmo->a_inv;

  /* Get this particle's abundance ratios compared to solar
   * Note that we need to add S and Ca that are in the tables but not tracked
   * by the particles themselves.
   * The order is [H, He, C, N, O, Ne, Mg, Si, S, Ca, Fe, OA] */
  float abundance_ratio[colibre_cooling_N_elementtypes];
  float logZZsol = abundance_ratio_to_solar(p, cooling, abundance_ratio);

  /* Get the Hydrogen and Helium mass fractions */
  float const *metal_fraction =
      chemistry_get_metal_mass_fraction_for_cooling(p);
  const float XH = metal_fraction[chemistry_element_H];

  /* convert Hydrogen mass fraction into Hydrogen number density */
  const double n_H =
      hydro_get_physical_density(p, cosmo) * XH / phys_const->const_proton_mass;
  const double n_H_cgs = n_H * cooling->number_density_to_cgs;

  /* ratefact = n_H * n_H / rho; Might lead to round-off error: replaced by
   * equivalent expression  below */
  const double ratefact_cgs = n_H_cgs * (XH * cooling->inv_proton_mass_cgs);

  /* compute hydrogen number density, metallicity and redshift indices and
   * offsets (These are fixed for any value of u, so no need to recompute them)
   */

  float d_red, d_met, d_n_H;
  int red_index, met_index, n_H_index;

  get_index_1d(cooling->Redshifts, colibre_cooling_N_redshifts, cosmo->z,
               &red_index, &d_red);
  get_index_1d(cooling->Metallicity, colibre_cooling_N_metallicity, logZZsol,
               &met_index, &d_met);
  get_index_1d(cooling->nH, colibre_cooling_N_density, log10(n_H_cgs),
               &n_H_index, &d_n_H);

  /* Start by computing the cooling (heating actually) rate from Helium
     re-ionization as this needs to be added on no matter what */

  /* Get helium and hydrogen reheating term */
  const double Helium_reion_heat_cgs =
      eagle_helium_reionization_extraheat(cosmo->z, delta_redshift, cooling);

  /* Convert this into a rate */
  const double Lambda_He_reion_cgs =
      Helium_reion_heat_cgs / (dt_cgs * ratefact_cgs);

  /* Let's compute the internal energy at the end of the step */
  double u_final_cgs;

  /* First try an explicit integration (note we ignore the derivative) */
  const double LambdaNet_cgs =
      Lambda_He_reion_cgs +
      colibre_cooling_rate(log10(u_0_cgs), cosmo->z, n_H_cgs, abundance_ratio,
                           n_H_index, d_n_H, met_index, d_met, red_index, d_red,
                           cooling, 0, 0, 0, 0);

  /* if cooling rate is small, take the explicit solution */
  if (fabs(ratefact_cgs * LambdaNet_cgs * dt_cgs) <
      explicit_tolerance * u_0_cgs) {

    u_final_cgs = u_0_cgs + ratefact_cgs * LambdaNet_cgs * dt_cgs;

  } else {

    u_final_cgs =
        bisection_iter(u_0_cgs, n_H_cgs, cosmo->z, n_H_index, d_n_H, met_index,
                       d_met, red_index, d_red, Lambda_He_reion_cgs,
                       ratefact_cgs, cooling, abundance_ratio, dt_cgs, p->id);
  }

  /* Convert back to internal units */
  double u_final = u_final_cgs * cooling->internal_energy_from_cgs;

  /* We now need to check that we are not going to go below any of the limits */

  /* Absolute minimum */
  const double u_minimal = hydro_properties->minimal_internal_energy;
  u_final = max(u_final, u_minimal);

  /* Limit imposed by the entropy floor */
  const double A_floor = entropy_floor(p, cosmo, floor_props);
  const double rho_physical = hydro_get_physical_density(p, cosmo);
  const double u_floor =
      gas_internal_energy_from_entropy(rho_physical, A_floor);
  u_final = max(u_final, u_floor);

  /* Expected change in energy over the next kick step
     (assuming no change in dt) */
  const double delta_u = u_final - max(u_start, u_floor);

  /* Determine if we are in the slow- or rapid-cooling regime,
   * by comparing dt / t_cool to the rapid_cooling_threshold.
   *
   * Note that dt / t_cool = fabs(delta_u) / u_start. */
  const double dt_over_t_cool = fabs(delta_u) / max(u_start, u_floor);

  /* If rapid_cooling_threshold < 0, always use the slow-cooling
   * regime. */
  if ((cooling->rapid_cooling_threshold >= 0.0) &&
      (dt_over_t_cool >= cooling->rapid_cooling_threshold)) {

    /* Rapid-cooling regime. */

    /* Update the particle's u and du/dt */
    hydro_set_physical_internal_energy(p, xp, cosmo, u_final);
    hydro_set_drifted_physical_internal_energy(p, cosmo, pressure_floor,
                                               u_final);
    hydro_set_physical_internal_energy_dt(p, cosmo, 0.);

  } else {

    /* Slow-cooling regime. */

    /* Update du/dt so that we can subsequently drift internal energy. */
    const float cooling_du_dt = delta_u / dt_therm;

    /* Update the internal energy time derivative */
    hydro_set_physical_internal_energy_dt(p, cosmo, cooling_du_dt);
  }

  /* Store the radiated energy */
  xp->cooling_data.radiated_energy -= hydro_get_mass(p) * (u_final - u_0);

  /* set subgrid properties and hydrogen fractions */
  cooling_set_particle_subgrid_properties(
      phys_const, us, cosmo, hydro_properties, floor_props, cooling, p, xp);
}

/**
 * @brief Computes the cooling time-step.
 *
 * The time-step is not set by the properties of cooling.
 *
 * @param cooling The #cooling_function_data used in the run.
 * @param phys_const #phys_const data struct.
 * @param us The internal system of units.
 * @param cosmo #cosmology struct.
 * @param hydro_props the properties of the hydro scheme.
 * @param p #part data.
 * @param xp extended particle data.
 */
__attribute__((always_inline)) INLINE float cooling_timestep(
    const struct cooling_function_data *cooling,
    const struct phys_const *phys_const, const struct cosmology *cosmo,
    const struct unit_system *us, const struct hydro_props *hydro_props,
    const struct part *p, const struct xpart *xp) {

  return FLT_MAX;
}

/**
 * @brief Sets the cooling properties of the (x-)particles to a valid start
 * state.
 *
 * @param phys_const #phys_const data structure.
 * @param us The internal system of units.
 * @param hydro_props The properties of the hydro scheme.
 * @param cosmo #cosmology data structure.
 * @param cooling #cooling_function_data struct.
 * @param p #part data.
 * @param xp Pointer to the #xpart data.
 */
__attribute__((always_inline)) INLINE void cooling_first_init_part(
    const struct phys_const *phys_const, const struct unit_system *us,
    const struct hydro_props *hydro_props, const struct cosmology *cosmo,
    const struct cooling_function_data *cooling, struct part *p,
    struct xpart *xp) {

  xp->cooling_data.radiated_energy = 0.f;
  p->cooling_data.subgrid_temp = -1.f;
  p->cooling_data.subgrid_dens = -1.f;
}

/**
 * @brief Compute the fraction of Hydrogen that is in HI based
 * on the pressure of the gas.
 *
 * For particles on the entropy floor, we use pressure equilibrium to
 * infer the properties of the particle.
 *
 * @param us The internal system of units.
 * @param phys_const The physical constants.
 * @param hydro_props The properties of the hydro scheme.
 * @param cosmo The cosmological model.
 * @param floor_props The properties of the entropy floor.
 * @param cooling The properties of the cooling scheme.
 * @param p The #part.
 * @param xp The #xpart.
 */
float cooling_get_particle_subgrid_HI_fraction(
    const struct unit_system *us, const struct phys_const *phys_const,
    const struct cosmology *cosmo, const struct hydro_props *hydro_props,
    const struct entropy_floor_properties *floor_props,
    const struct cooling_function_data *cooling, const struct part *p,
    const struct xpart *xp) {

  /* Physical density of this particle */
  const float rho_phys = hydro_get_physical_density(p, cosmo);

  /* Limit imposed by the entropy floor */
  const double A_EOS = entropy_floor(p, cosmo, floor_props);
  const double u_EOS = gas_internal_energy_from_entropy(rho_phys, A_EOS);
  const double u_EOS_max = u_EOS * exp10(cooling->dlogT_EOS);

  const float log10_u_EOS_max_cgs =
      log10f(u_EOS_max * cooling->internal_energy_to_cgs + FLT_MIN);

  /* Get the total metallicity in units of solar */
  float abundance_ratio[colibre_cooling_N_elementtypes];
  const float logZZsol = abundance_ratio_to_solar(p, cooling, abundance_ratio);

  /* Get the Hydrogen abundance */
  const float *const metal_fraction =
      chemistry_get_metal_mass_fraction_for_cooling(p);
  const float XH = metal_fraction[chemistry_element_H];

  /* Get the particle pressure */
  const float P_phys = hydro_get_physical_pressure(p, cosmo);

  /* Get physical internal energy */
  const float u_phys = hydro_get_physical_internal_energy(p, xp, cosmo);

  /* Are we in an HII region? */
  const int HII_region = 0; /* No HII regions in the EAGLE-XL flavour */

  /* Get the particle's temperature */
  const float T = cooling_get_temperature_from_gas(
      phys_const, cosmo, cooling, rho_phys, logZZsol, XH, u_phys, HII_region);
  const float log10_T = log10f(T);

  return compute_subgrid_property(
      cooling, phys_const, floor_props, cosmo, rho_phys, logZZsol, XH, P_phys,
      log10_T, log10_u_EOS_max_cgs, HII_region, abundance_ratio,
      log10(u_phys * cooling->internal_energy_to_cgs),
      cooling_compute_subgrid_HI_fraction);
}

/**
 * @brief Compute the fraction of Hydrogen that is in HII based
 * on the pressure of the gas.
 *
 * For particles on the entropy floor, we use pressure equilibrium to
 * infer the properties of the particle.
 *
 * @param us The internal system of units.
 * @param phys_const The physical constants.
 * @param hydro_props The properties of the hydro scheme.
 * @param cosmo The cosmological model.
 * @param floor_props The properties of the entropy floor.
 * @param cooling The properties of the cooling scheme.
 * @param p The #part.
 * @param xp The #xpart.
 */
float cooling_get_particle_subgrid_HII_fraction(
    const struct unit_system *us, const struct phys_const *phys_const,
    const struct cosmology *cosmo, const struct hydro_props *hydro_props,
    const struct entropy_floor_properties *floor_props,
    const struct cooling_function_data *cooling, const struct part *p,
    const struct xpart *xp) {

  /* Physical density of this particle */
  const float rho_phys = hydro_get_physical_density(p, cosmo);

  /* Limit imposed by the entropy floor */
  const double A_EOS = entropy_floor(p, cosmo, floor_props);
  const double u_EOS = gas_internal_energy_from_entropy(rho_phys, A_EOS);
  const double u_EOS_max = u_EOS * exp10(cooling->dlogT_EOS);

  const float log10_u_EOS_max_cgs =
      log10f(u_EOS_max * cooling->internal_energy_to_cgs + FLT_MIN);

  /* Get the total metallicity in units of solar */
  float abundance_ratio[colibre_cooling_N_elementtypes];
  const float logZZsol = abundance_ratio_to_solar(p, cooling, abundance_ratio);

  /* Get the Hydrogen abundance */
  const float *const metal_fraction =
      chemistry_get_metal_mass_fraction_for_cooling(p);
  const float XH = metal_fraction[chemistry_element_H];

  /* Get the particle pressure */
  const float P_phys = hydro_get_physical_pressure(p, cosmo);

  /* Get physical internal energy */
  const float u_phys = hydro_get_physical_internal_energy(p, xp, cosmo);

  /* Are we in an HII region? */
  const int HII_region = 0; /* No HII regions in the EAGLE-XL flavour */

  /* Get the particle's temperature */
  const float T = cooling_get_temperature_from_gas(
      phys_const, cosmo, cooling, rho_phys, logZZsol, XH, u_phys, HII_region);
  const float log10_T = log10f(T);

  return compute_subgrid_property(
      cooling, phys_const, floor_props, cosmo, rho_phys, logZZsol, XH, P_phys,
      log10_T, log10_u_EOS_max_cgs, HII_region, abundance_ratio,
      log10(u_phys * cooling->internal_energy_to_cgs),
      cooling_compute_subgrid_HII_fraction);
}

/**
 * @brief Compute the fraction of Hydrogen that is in H2 based
 * on the pressure of the gas.
 *
 * For particles on the entropy floor, we use pressure equilibrium to
 * infer the properties of the particle.
 *
 * @param us The internal system of units.
 * @param phys_const The physical constants.
 * @param hydro_props The properties of the hydro scheme.
 * @param cosmo The cosmological model.
 * @param floor_props The properties of the entropy floor.
 * @param cooling The properties of the cooling scheme.
 * @param p The #part.
 * @param xp The #xpart.
 */
float cooling_get_particle_subgrid_H2_fraction(
    const struct unit_system *us, const struct phys_const *phys_const,
    const struct cosmology *cosmo, const struct hydro_props *hydro_props,
    const struct entropy_floor_properties *floor_props,
    const struct cooling_function_data *cooling, const struct part *p,
    const struct xpart *xp) {

  /* Physical density of this particle */
  const float rho_phys = hydro_get_physical_density(p, cosmo);

  /* Limit imposed by the entropy floor */
  const double A_EOS = entropy_floor(p, cosmo, floor_props);
  const double u_EOS = gas_internal_energy_from_entropy(rho_phys, A_EOS);
  const double u_EOS_max = u_EOS * exp10(cooling->dlogT_EOS);

  const float log10_u_EOS_max_cgs =
      log10f(u_EOS_max * cooling->internal_energy_to_cgs + FLT_MIN);

  /* Get the total metallicity in units of solar */
  float abundance_ratio[colibre_cooling_N_elementtypes];
  const float logZZsol = abundance_ratio_to_solar(p, cooling, abundance_ratio);

  /* Get the Hydrogen abundance */
  const float *const metal_fraction =
      chemistry_get_metal_mass_fraction_for_cooling(p);
  const float XH = metal_fraction[chemistry_element_H];

  /* Get the particle pressure */
  const float P_phys = hydro_get_physical_pressure(p, cosmo);

  /* Get physical internal energy */
  const float u_phys = hydro_get_physical_internal_energy(p, xp, cosmo);

  /* Are we in an HII region? */
  const int HII_region = 0; /* No HII regions in the EAGLE-XL flavour */

  /* Get the particle's temperature */
  const float T = cooling_get_temperature_from_gas(
      phys_const, cosmo, cooling, rho_phys, logZZsol, XH, u_phys, HII_region);
  const float log10_T = log10f(T);

  return compute_subgrid_property(
      cooling, phys_const, floor_props, cosmo, rho_phys, logZZsol, XH, P_phys,
      log10_T, log10_u_EOS_max_cgs, HII_region, abundance_ratio,
      log10(u_phys * cooling->internal_energy_to_cgs),
      cooling_compute_subgrid_H2_fraction);
}

/**
 * @brief Compute the temperature of the gas.
 *
 * For particles on the entropy floor, we use pressure equilibrium to
 * infer the properties of the particle.
 *
 * @param us The internal system of units.
 * @param phys_const The physical constants.
 * @param hydro_props The properties of the hydro scheme.
 * @param cosmo The cosmological model.
 * @param floor_props The properties of the entropy floor.
 * @param cooling The properties of the cooling scheme.
 * @param p The #part.
 * @param xp The #xpart.
 */
float cooling_get_particle_subgrid_temperature(
    const struct unit_system *us, const struct phys_const *phys_const,
    const struct cosmology *cosmo, const struct hydro_props *hydro_props,
    const struct entropy_floor_properties *floor_props,
    const struct cooling_function_data *cooling, const struct part *p,
    const struct xpart *xp) {

  /* Physical density of this particle */
  const float rho_phys = hydro_get_physical_density(p, cosmo);

  /* Limit imposed by the entropy floor */
  const double A_EOS = entropy_floor(p, cosmo, floor_props);
  const double u_EOS = gas_internal_energy_from_entropy(rho_phys, A_EOS);
  const double u_EOS_max = u_EOS * exp10(cooling->dlogT_EOS);

  const float log10_u_EOS_max_cgs =
      log10f(u_EOS_max * cooling->internal_energy_to_cgs + FLT_MIN);

  /* Get the total metallicity in units of solar */
  float abundance_ratio[colibre_cooling_N_elementtypes];
  const float logZZsol = abundance_ratio_to_solar(p, cooling, abundance_ratio);

  /* Get the Hydrogen abundance */
  const float *const metal_fraction =
      chemistry_get_metal_mass_fraction_for_cooling(p);
  const float XH = metal_fraction[chemistry_element_H];

  /* Get the particle pressure */
  const float P_phys = hydro_get_physical_pressure(p, cosmo);

  /* Get physical internal energy */
  const float u_phys = hydro_get_physical_internal_energy(p, xp, cosmo);

  /* Are we in an HII region? */
  const int HII_region = 0; /* No HII regions in the EAGLE-XL flavour */

  /* Get the particle's temperature */
  const float T = cooling_get_temperature_from_gas(
      phys_const, cosmo, cooling, rho_phys, logZZsol, XH, u_phys, HII_region);
  const float log10_T = log10f(T);

  return compute_subgrid_property(
      cooling, phys_const, floor_props, cosmo, rho_phys, logZZsol, XH, P_phys,
      log10_T, log10_u_EOS_max_cgs, HII_region, abundance_ratio,
      log10(u_phys * cooling->internal_energy_to_cgs),
      cooling_compute_subgrid_temperature);
}

/**
 * @brief Compute the physical density of the gas.
 *
 * For particles on the entropy floor, we use pressure equilibrium to
 * infer the properties of the particle.
 *
 * Note that we return the density in physical coordinates.
 *
 * @param us The internal system of units.
 * @param phys_const The physical constants.
 * @param hydro_props The properties of the hydro scheme.
 * @param cosmo The cosmological model.
 * @param floor_props The properties of the entropy floor.
 * @param cooling The properties of the cooling scheme.
 * @param p The #part.
 * @param xp The #xpart.
 */
float cooling_get_particle_subgrid_density(
    const struct unit_system *us, const struct phys_const *phys_const,
    const struct cosmology *cosmo, const struct hydro_props *hydro_props,
    const struct entropy_floor_properties *floor_props,
    const struct cooling_function_data *cooling, const struct part *p,
    const struct xpart *xp) {

  /* Physical density of this particle */
  const float rho_phys = hydro_get_physical_density(p, cosmo);

  /* Limit imposed by the entropy floor */
  const double A_EOS = entropy_floor(p, cosmo, floor_props);
  const double u_EOS = gas_internal_energy_from_entropy(rho_phys, A_EOS);
  const double u_EOS_max = u_EOS * exp10(cooling->dlogT_EOS);

  const float log10_u_EOS_max_cgs =
      log10f(u_EOS_max * cooling->internal_energy_to_cgs + FLT_MIN);

  /* Get the total metallicity in units of solar */
  float abundance_ratio[colibre_cooling_N_elementtypes];
  const float logZZsol = abundance_ratio_to_solar(p, cooling, abundance_ratio);

  /* Get the Hydrogen abundance */
  const float *const metal_fraction =
      chemistry_get_metal_mass_fraction_for_cooling(p);
  const float XH = metal_fraction[chemistry_element_H];

  /* Get the particle pressure */
  const float P_phys = hydro_get_physical_pressure(p, cosmo);

  /* Get the particle's temperature */
  const float T = cooling_get_temperature(phys_const, hydro_props, us, cosmo,
                                          cooling, p, xp);
  const float log10_T = log10f(T);

  /* Are we in an HII region? */
  const int HII_region = 0; /* No HII regions in the EAGLE-XL flavour */

  const float u_start = hydro_get_physical_internal_energy(p, xp, cosmo);
  const double u_0_cgs = u_start * cooling->internal_energy_to_cgs;

  return compute_subgrid_property(
      cooling, phys_const, floor_props, cosmo, rho_phys, logZZsol, XH, P_phys,
      log10_T, log10_u_EOS_max_cgs, HII_region, abundance_ratio, log10(u_0_cgs),
      cooling_compute_subgrid_density);
}

/**
 * @brief Set the subgrid properties (rho, T) of the gas particle
 *
 * @param phys_const The physical constants in internal units.
 * @param us The internal system of units.
 * @param cosmo The current cosmological model.
 * @param hydro_props the hydro_props struct
 * @param floor_props Properties of the entropy floor.
 * @param cooling The #cooling_function_data used in the run.
 * @param p Pointer to the particle data.
 * @param xp Pointer to the extended particle data.
 */
void cooling_set_particle_subgrid_properties(
    const struct phys_const *phys_const, const struct unit_system *us,
    const struct cosmology *cosmo, const struct hydro_props *hydro_props,
    const struct entropy_floor_properties *floor_props,
    const struct cooling_function_data *cooling, struct part *p,
    struct xpart *xp) {

  /* Physical density of this particle */
  const float rho_phys = hydro_get_physical_density(p, cosmo);

  /* Limit imposed by the entropy floor */
  const double A_EOS = entropy_floor(p, cosmo, floor_props);
  const double u_EOS = gas_internal_energy_from_entropy(rho_phys, A_EOS);
  const double u_EOS_max = u_EOS * exp10(cooling->dlogT_EOS);

  const float log10_u_EOS_max_cgs =
      log10f(u_EOS_max * cooling->internal_energy_to_cgs + FLT_MIN);

  /* Get the total metallicity in units of solar */
  float abundance_ratio[colibre_cooling_N_elementtypes];
  const float logZZsol = abundance_ratio_to_solar(p, cooling, abundance_ratio);

  /* Get the Hydrogen abundance */
  const float *const metal_fraction =
      chemistry_get_metal_mass_fraction_for_cooling(p);
  const float XH = metal_fraction[chemistry_element_H];

  /* Get the particle pressure */
  const float P_phys = hydro_get_physical_pressure(p, cosmo);

  /* Get physical internal energy */
  const float u_phys = hydro_get_physical_internal_energy(p, xp, cosmo);
  const double u_cgs = u_phys * cooling->internal_energy_to_cgs;

  /* Are we in an HII region? */
  const int HII_region = 0; /* No HII regions in the EAGLE-XL flavour */

  /* Get the particle's temperature */
  const float T = cooling_get_temperature_from_gas(
      phys_const, cosmo, cooling, rho_phys, logZZsol, XH, u_phys, HII_region);
  const float log10_T = log10f(T);

  p->cooling_data.subgrid_temp = compute_subgrid_property(
      cooling, phys_const, floor_props, cosmo, rho_phys, logZZsol, XH, P_phys,
      log10_T, log10_u_EOS_max_cgs, HII_region, abundance_ratio, log10(u_cgs),
      cooling_compute_subgrid_temperature);

  p->cooling_data.subgrid_dens = compute_subgrid_property(
      cooling, phys_const, floor_props, cosmo, rho_phys, logZZsol, XH, P_phys,
      log10_T, log10_u_EOS_max_cgs, HII_region, abundance_ratio, log10(u_cgs),
      cooling_compute_subgrid_density);
}

/**
 * @brief Returns the subgrid temperature of a particle.
 *
 * @param p The particle.
 * @param xp The extended particle data.
 * @return The subgrid temperature in internal units.
 */
float cooling_get_subgrid_temperature(const struct part *p,
                                      const struct xpart *xp) {
  return p->cooling_data.subgrid_temp;
}

/**
 * @brief Returns the subgrid density of a particle.
 *
 * @param p The particle.
 * @param xp The extended particle data.
 * @return The subgrid density in physical internal units.
 */
float cooling_get_subgrid_density(const struct part *p,
                                  const struct xpart *xp) {
  return p->cooling_data.subgrid_dens;
}

/**
 * @brief Returns the total radiated energy by this particle.
 *
 * @param xp #xpart data struct
 */
__attribute__((always_inline)) INLINE float cooling_get_radiated_energy(
    const struct xpart *xp) {

  return xp->cooling_data.radiated_energy;
}

/**
 * @brief Split the coolong content of a particle into n pieces
 *
 * @param p The #part.
 * @param xp The #xpart.
 * @param n The number of pieces to split into.
 */
void cooling_split_part(struct part *p, struct xpart *xp, double n) {

  xp->cooling_data.radiated_energy /= n;
}

/**
 * @brief Inject a fixed amount of energy to each particle in the simulation
 * to mimic Hydrogen reionization.
 *
 * @param cooling The properties of the cooling model.
 * @param cosmo The cosmological model.
 * @param pressure_floor Properties of the pressure floor.
 * @param s The #space containing the particles.
 */
void cooling_Hydrogen_reionization(
    const struct cooling_function_data *cooling, const struct cosmology *cosmo,
    const struct pressure_floor_props *pressure_floor, struct space *s) {

  struct part *parts = s->parts;
  struct xpart *xparts = s->xparts;

  /* Energy to inject in internal units */
  const float extra_heat =
      cooling->H_reion_heat_cgs * cooling->internal_energy_from_cgs;

  message("Applying extra energy for H reionization to non-star-forming gas!");

  /* Loop through particles and set new heat */
  for (size_t i = 0; i < s->nr_parts; i++) {

    struct part *p = &parts[i];
    struct xpart *xp = &xparts[i];

    if (part_is_inhibited(p, s->e)) continue;

    if (star_formation_get_SFR(p, xp) == 0.f) {
      const float old_u = hydro_get_physical_internal_energy(p, xp, cosmo);
      const float new_u = old_u + extra_heat;

      hydro_set_physical_internal_energy(p, xp, cosmo, new_u);
      hydro_set_drifted_physical_internal_energy(p, cosmo, pressure_floor,
                                                 new_u);
    }
  }
}

/**
 * @brief Initialises properties stored in the cooling_function_data struct
 *
 * @param parameter_file The parsed parameter file.
 * @param us Internal system of units data structure.
 * @param hydro_props the properties of the hydro scheme.
 * @param phys_const #phys_const data structure.
 * @param cooling #cooling_function_data struct to initialize.
 */
void cooling_init_backend(struct swift_params *parameter_file,
                          const struct unit_system *us,
                          const struct phys_const *phys_const,
                          const struct hydro_props *hydro_props,
                          struct cooling_function_data *cooling) {

  /* read some parameters */

  parser_get_param_string(parameter_file, "PS2020Cooling:dir_name",
                          cooling->cooling_table_path);

  /* Despite the names, the values of H_reion_heat_cgs and He_reion_heat_cgs
   * that are read in are actually in units of electron volts per proton mass.
   * We later convert to units just below */

  cooling->H_reion_done = 0;
  cooling->H_reion_z =
      parser_get_param_float(parameter_file, "PS2020Cooling:H_reion_z");
  cooling->H_reion_heat_cgs =
      parser_get_param_float(parameter_file, "PS2020Cooling:H_reion_eV_p_H");
  cooling->He_reion_z_centre =
      parser_get_param_float(parameter_file, "PS2020Cooling:He_reion_z_centre");
  cooling->He_reion_z_sigma =
      parser_get_param_float(parameter_file, "PS2020Cooling:He_reion_z_sigma");
  cooling->He_reion_heat_cgs =
      parser_get_param_float(parameter_file, "PS2020Cooling:He_reion_eV_p_H");

  /* Properties for the subgrid properties model ---------------------------- */
  cooling->dlogT_EOS = parser_get_param_float(
      parameter_file, "PS2020Cooling:delta_logTEOS_subgrid_properties");

  /* Optional parameters to correct the abundances */
  cooling->Ca_over_Si_ratio_in_solar = parser_get_opt_param_float(
      parameter_file, "PS2020Cooling:Ca_over_Si_in_solar", 1.f);
  cooling->S_over_Si_ratio_in_solar = parser_get_opt_param_float(
      parameter_file, "PS2020Cooling:S_over_Si_in_solar", 1.f);

  /* Convert H_reion_heat_cgs and He_reion_heat_cgs to cgs
   * (units used internally by the cooling routines). This is done by
   * multiplying by 'eV/m_H' in internal units, then converting to cgs units.
   * Note that the dimensions of these quantities are energy/mass = velocity^2
   */

  cooling->H_reion_heat_cgs *=
      phys_const->const_electron_volt / phys_const->const_proton_mass *
      units_cgs_conversion_factor(us, UNIT_CONV_ENERGY_PER_UNIT_MASS);

  cooling->He_reion_heat_cgs *=
      phys_const->const_electron_volt / phys_const->const_proton_mass *
      units_cgs_conversion_factor(us, UNIT_CONV_ENERGY_PER_UNIT_MASS);

  /* Compute conversion factors */
  cooling->pressure_to_cgs =
      units_cgs_conversion_factor(us, UNIT_CONV_PRESSURE);
  cooling->internal_energy_to_cgs =
      units_cgs_conversion_factor(us, UNIT_CONV_ENERGY_PER_UNIT_MASS);
  cooling->internal_energy_from_cgs = 1. / cooling->internal_energy_to_cgs;
  cooling->number_density_to_cgs =
      units_cgs_conversion_factor(us, UNIT_CONV_NUMBER_DENSITY);
  cooling->number_density_from_cgs = 1. / cooling->number_density_to_cgs;
  cooling->density_to_cgs = units_cgs_conversion_factor(us, UNIT_CONV_DENSITY);
  cooling->density_from_cgs = 1. / cooling->density_to_cgs;

  /* Store some constants in CGS units */
  const float units_kB[5] = {1, 2, -2, 0, -1};
  const double kB_cgs = phys_const->const_boltzmann_k *
                        units_general_cgs_conversion_factor(us, units_kB);
  const double proton_mass_cgs =
      phys_const->const_proton_mass *
      units_cgs_conversion_factor(us, UNIT_CONV_MASS);

  cooling->log10_kB_cgs = log10(kB_cgs);
  cooling->inv_proton_mass_cgs = 1. / proton_mass_cgs;
  cooling->proton_mass_cgs = proton_mass_cgs;
  cooling->T_CMB_0 = phys_const->const_T_CMB_0 *
                     units_cgs_conversion_factor(us, UNIT_CONV_TEMPERATURE);

  /* Get the minimal temperature allowed */
  cooling->Tmin = hydro_props->minimal_temperature;
  if (cooling->Tmin < 10.)
    error("PS2020 cooling cannot handle a minimal temperature below 10 K");

  /* Recover the minimal energy allowed (in internal units) */
  const double u_min = hydro_props->minimal_internal_energy;

  /* Convert to CGS units */
  cooling->umin_cgs = u_min * cooling->internal_energy_to_cgs;

#ifdef SWIFT_DEBUG_CHECKS
  /* Basic cross-check... */
  if (kB_cgs > 1.381e-16 || kB_cgs < 1.380e-16)
    error("Boltzmann's constant not initialised properly!");
#endif

  /* Compute the coefficient at the front of the Compton cooling expression */
  const double radiation_constant =
      4. * phys_const->const_stefan_boltzmann / phys_const->const_speed_light_c;
  const double compton_coefficient =
      4. * radiation_constant * phys_const->const_thomson_cross_section *
      phys_const->const_boltzmann_k /
      (phys_const->const_electron_mass * phys_const->const_speed_light_c);
  const float dimension_coefficient[5] = {1, 2, -3, 0, -5};

  /* This should be ~1.0178085e-37 g cm^2 s^-3 K^-5 */
  const double compton_coefficient_cgs =
      compton_coefficient *
      units_general_cgs_conversion_factor(us, dimension_coefficient);

#ifdef SWIFT_DEBUG_CHECKS
  const double expected_compton_coefficient_cgs = 1.0178085e-37;
  if (fabs(compton_coefficient_cgs - expected_compton_coefficient_cgs) /
          expected_compton_coefficient_cgs >
      0.01)
    error("compton coefficient incorrect.");
#endif

  /* And now the Compton rate */
  cooling->compton_rate_cgs = compton_coefficient_cgs * cooling->T_CMB_0 *
                              cooling->T_CMB_0 * cooling->T_CMB_0 *
                              cooling->T_CMB_0;

  /* Pre-factor for the Compton y terms */
  cooling->y_compton_factor =
      phys_const->const_thomson_cross_section * phys_const->const_boltzmann_k /
      (phys_const->const_speed_light_c * phys_const->const_speed_light_c *
       phys_const->const_electron_mass);

  /* Threshold in dt / t_cool above which we
   * are in the rapid cooling regime. If negative,
   * we never use this scheme (i.e. always drift
   * the internal energies). */
  cooling->rapid_cooling_threshold = parser_get_param_double(
      parameter_file, "PS2020Cooling:rapid_cooling_threshold");

  /* Finally, read the tables */
  read_cooling_header(cooling);
  read_cooling_tables(cooling);
}

/**
 * @brief Restore cooling tables (if applicable) after
 * restart
 *
 * @param cooling the #cooling_function_data structure
 * @param cosmo #cosmology structure
 */
void cooling_restore_tables(struct cooling_function_data *cooling,
                            const struct cosmology *cosmo) {

  read_cooling_header(cooling);
  read_cooling_tables(cooling);

  cooling_update(cosmo, /*pfloor=*/NULL, cooling, /*space=*/NULL);
}

/**
 * @brief Prints the properties of the cooling model to stdout.
 *
 * @param cooling #cooling_function_data struct.
 */
void cooling_print_backend(const struct cooling_function_data *cooling) {

  message(
      "Cooling function is 'PS2020' i.e. using the tables of "
      "Ploeckinger&Schaye (2020).");
}

/**
 * @brief Clean-up the memory allocated for the cooling routines
 *
 * We simply free all the arrays.
 *
 * @param cooling the cooling data structure.
 */
void cooling_clean(struct cooling_function_data *cooling) {

  /* Free the side arrays */
  free(cooling->Redshifts);
  free(cooling->nH);
  free(cooling->Temp);
  free(cooling->Metallicity);
  free(cooling->Therm);
  free(cooling->LogAbundances);
  free(cooling->Abundances);
  free(cooling->Abundances_inv);
  free(cooling->atomicmass);
  free(cooling->atomicmass_inv);
  free(cooling->Zsol);
  free(cooling->Zsol_inv);
  free(cooling->LogMassFractions);
  free(cooling->MassFractions);

  /* Free the tables */
  swift_free("cooling_table.Tcooling", cooling->table.Tcooling);
  swift_free("cooling_table.Ucooling", cooling->table.Ucooling);
  swift_free("cooling_table.Theating", cooling->table.Theating);
  swift_free("cooling_table.Uheating", cooling->table.Uheating);
  swift_free("cooling_table.Tefrac", cooling->table.Telectron_fraction);
  swift_free("cooling_table.Uefrac", cooling->table.Uelectron_fraction);
  swift_free("cooling_table.TfromU", cooling->table.T_from_U);
  swift_free("cooling_table.UfromT", cooling->table.U_from_T);
  swift_free("cooling_table.Umu", cooling->table.Umu);
  swift_free("cooling_table.Tmu", cooling->table.Tmu);
  swift_free("cooling_table.mueq", cooling->table.meanpartmass_Teq);
  swift_free("cooling_table.Hfracs", cooling->table.logHfracs_Teq);
  swift_free("cooling_table.Hfracs", cooling->table.logHfracs_all);
  swift_free("cooling_table.Teq", cooling->table.logTeq);
  swift_free("cooling_table.Peq", cooling->table.logPeq);
}

/**
 * @brief Write a cooling struct to the given FILE as a stream of bytes.
 *
 * @param cooling the struct
 * @param stream the file stream
 */
void cooling_struct_dump(const struct cooling_function_data *cooling,
                         FILE *stream) {

  /* To make sure everything is restored correctly, we zero all the pointers to
     tables. If they are not restored correctly, we would crash after restart on
     the first call to the cooling routines. Helps debugging. */
  struct cooling_function_data cooling_copy = *cooling;
  cooling_copy.Redshifts = NULL;
  cooling_copy.nH = NULL;
  cooling_copy.Temp = NULL;
  cooling_copy.Metallicity = NULL;
  cooling_copy.Therm = NULL;
  cooling_copy.LogAbundances = NULL;
  cooling_copy.Abundances = NULL;
  cooling_copy.Abundances_inv = NULL;
  cooling_copy.atomicmass = NULL;
  cooling_copy.LogMassFractions = NULL;
  cooling_copy.MassFractions = NULL;

  cooling_copy.table.Tcooling = NULL;
  cooling_copy.table.Theating = NULL;
  cooling_copy.table.Telectron_fraction = NULL;
  cooling_copy.table.Ucooling = NULL;
  cooling_copy.table.Uheating = NULL;
  cooling_copy.table.Uelectron_fraction = NULL;
  cooling_copy.table.T_from_U = NULL;
  cooling_copy.table.U_from_T = NULL;

  restart_write_blocks((void *)&cooling_copy,
                       sizeof(struct cooling_function_data), 1, stream,
                       "cooling", "cooling function");
}

/**
 * @brief Restore a hydro_props struct from the given FILE as a stream of
 * bytes.
 *
 * Read the structure from the stream and restore the cooling tables by
 * re-reading them.
 *
 * @param cooling the struct
 * @param stream the file stream
 * @param cosmo #cosmology structure
 */
void cooling_struct_restore(struct cooling_function_data *cooling, FILE *stream,
                            const struct cosmology *cosmo) {
  restart_read_blocks((void *)cooling, sizeof(struct cooling_function_data), 1,
                      stream, NULL, "cooling function");

  cooling_restore_tables(cooling, cosmo);
}
