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| subroutine | sed_routines::calc_sed |
| | Calculates stellar or dust emission SED from the i_obs() arrays. If keyword print_sed is not set TRUE, then it just returns. More...
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| subroutine | sed_routines::create_sed_arr |
| | Allocates sed arrays sed_arr(), sed_arr_dir(), sed_arr_sca(). More...
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| subroutine | sed_routines::calc_sed_arrays |
| | ! Sums up the i_obs at different wavelengths to obtain the total output sed in the input directions. Used only for the "sed" algorithm. More...
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| subroutine | sed_routines::sum_i_obs (il, sed_arr) |
| | Sums i_obs arrays to obtain emission SED. More...
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| subroutine | sed_routines::set_dust_emission |
| | Calculates the dust emission luminosity density and stores it into dens_stars_arr(). More...
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| subroutine | sed_routines::check_dens_stars_arr |
| | Compare the newly calculated dens_stars_arr() with dens_stars_arr_prev(). If the relative difference is smaller than conv_en_lim(), it assigns TRUE to cnflag_dust(), thus stopping the dust heating iterations. It not, it subtracts from dens_stars_arr() the luminosity already processed in the previous dust heating iterations and it updates dens_stars_arr_prev(). More...
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| subroutine | sed_routines::convert_ufield_ifield |
| | Calculates the constant factor conv_ufield_ifield(). Then transforms the stellar emission radiation field energy density u_final_uv_opt() into the integrated radiation field intensity in units of W/m^2/m. More...
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| subroutine | sed_routines::calc_dens_dustem |
| | Calculates the dust emission luminosity density in the case of the effective grain mode. More...
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| subroutine | sed_routines::calc_dens_dustem_equ |
| | Calculates the equilibrium emission for the grain mixture case. More...
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| subroutine | sed_routines::allocate_sto_arrays |
| | Allocates arrays used within the stochastically heated dust emission routines calc_dens_dustem_sto() and calc_dens_dustem_sto_lib(). More...
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| subroutine | sed_routines::deallocate_sto_arrays |
| | Deallocates arrays used within the stochastically heated dust emission routines calc_dens_dustem_sto() and calc_dens_dustem_sto_lib(). More...
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| subroutine | sed_routines::calc_dens_dustem_sto |
| | Calculates the stochastically heated emission at each position. More...
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| subroutine | sed_routines::calc_dens_dustem_sto_lib |
| | Calculates the stochastically heated emission at each position using the SED adaptive library approach of Natale et al.(2015). More...
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| subroutine | sed_routines::calc_t_dust_equil (qabs_arr, dust_size, rf_stars, rf_dust, t_dust, abs_en) |
| | Calculates the equilibrium dust temperature given the absorption Q coefficient, the radiation field intensity of the stellar emission and of the dust emission in [W/m/m^2]. The input qabs_arr coefficient can also have units [e.g. m^2], as for the effective grain emission calculation, without changing the output equilibrium temperature. The output absorbed energy abs_en is in units of W/m^2 times the units of the input qabs_arr. More...
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| subroutine | sed_routines::calc_rd_arr (dust_size) |
| | Calculates the moments of the dosage function (see Voit 1991, ApJ, 379, 122, needed for the dust stochastically heated calculation). More...
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| subroutine | sed_routines::set_units_dens_stars_arr |
| | Sets the units of dens_stars_arr() in the dust RT algorithms. These units are W/m/pc^3 where meters refers to the wavelength. More...
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| real(kind=real64) function | sed_routines::abs_en_diff (t_dust, kabs_arr_planck, abs_en, em_int) |
| | Calculates the difference between absorbed and emitted energy given the temperature T_dust. More...
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| real(kind=real64) function | sed_routines::bplanck (T_source, la) |
| | Returns black body specific intensity in W/m^2/m/sr at wavelength la [m] and for temperature T_source [K] (SI units) More...
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| subroutine | sed_routines::set_lambda_arr_si |
| | Sets the lambda array in the mks units ( lambda_arr_SI()). It also sets delta_lambda_bin(), delta_lambda_bin_stars() and delta_lambda_bin_dust(). More...
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| real(kind=real64) function | sed_routines::zbrent_tdust (kabs_arr_planck, abs_en) |
| | Finds equilibrium dust temperature using Brent's method (modified version of the Van Wijngaarden–Dekker–Brent Method, see Numerical recipes in Fortran 77, Press et al.). More...
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| subroutine | sed_routines::prepare_dust_model |
| | Reads the input dust model files. Derive the dust model optical properties used in the calculation, interpolated at the same wavelengths as in lambda_arr() and same grain sizes as in the input grain size distributions. More...
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| subroutine | sed_routines::load_opacity_param |
| | Loads the Qabs, Qsca, Qext and gsca factors from the tables in the dust opacity directory (from the TRUST benchmark project) and interpolate them to the input wavelength grid. Note that a further interpolation is needed to match the grain sizes to the values of the input tables. This is done in interpolate_q_grain_fa(). More...
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| subroutine | sed_routines::load_fa_arr |
| | Loads the grain size distribution from the standard TRUST tables or from user provided files. More...
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| subroutine | sed_routines::interpolate_q_grain_fa |
| | Interpolate the qabs, qsca, qext and gsca arrays to the same grain sizes of the input grain size distribution tables. More...
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| subroutine | sed_routines::load_ct_ht_tables |
| | Loads specific enthalphy and specific heat capacity as a function of grain temperature from the input tables. In the standard mode, the tables are those provided in the TRUST RT benchmark project. Alternatively input tables can also be used, provided that they are in the same form as the TRUST tables. More...
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| subroutine | sed_routines::value_locate (val, array, ig0, ig1, reverse_order) |
| | Finds indeces of an array corresponding to the array value bin containing the input value val(). Note that the array should normally be sorted in ascending order. In case val is lower than array(0), it returns the indeces of the first two elements. If val is higher than array(size(array)-1), it returns indeces of last two elements. The input array can be in the reversing order if the reverse_order keyword is set TRUE. More...
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| subroutine | sed_routines::lin_interpolate (y0, y1, x0, x1, x, y) |
| | Interpolates linearly at a position x within the bin [x0,x1] given the boundary values y0=f(x0) and y1=f(x1). y0 and y1 are defined as arrays, so the subroutine can be used for multiple values provided that the x coordinates x0, x1 and x are the same. More...
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| subroutine | sed_routines::calc_total_opacity |
| | Calculates integrated opacity coefficients kabs_arr(), ksca_arr(), kext_arr() and scattering phase function parameter gsca_arr() from the tabulated opacity parameters and the input grain size distributions. The resulting values for the integrated coefficients depends slightly on the specific interpolation scheme. For this reason, we add the option to upload these values from an input file as well using the keyword load_av_opacities() and file_int_opacities(). In this case, the code checks that the values obtained by this routine and those uploaded through the input file file_av_opacities() do not vary more than 5%. This is necessary to guarantee consistency between the dust emission and the stellar emission calculations within a few percents. More...
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| subroutine | sed_routines::read_av_opacities |
| | If keyword input_av_opacities is TRUE, it reads input table of integrated/averaged opacity coefficients kext(), kabs(), kext() and scattering phase function gsca. Interpolates factors to input wavelength grid lambda_arr() and to reference wavelength lambda_ref(). Checks values are within 5% of those derived directly by integration/average of grain opacities coefficients. More...
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| subroutine | sed_routines::calc_planck_av_qabs |
| | Calculates planck averaged Qabs for the grains in the input grain size distributions and for a set of temperatures. More...
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| subroutine | sed_routines::calc_photon_energy |
| | Calculates energy of photons as a function of wavelength for the set of wavelength stored in lambda_arr_SI. The energy is in [J]. More...
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| subroutine | sed_routines::calc_gaussian_fe (t_dust, ic, ig) |
| | Calculates pt() in the large grain energy approximation (see section 4.4 Voit 1991). In case 1) the mean photon energy is very small compared to the grain equilibrium energy and 2) the width of the Gaussian approximation is more than 10% the equilibrium dust temperature, the code assign large_grain_energy = .FALSE. So the stochastically heated emission is calculated numerically from the current grain size to smaller sizes. More...
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| subroutine | sed_routines::calc_full_fe (ic, ig) |
| | Calculates the temperature probability distribution pt() using the numerical method of Gahathakurta & Draine 1989 with the modification of Voit 1991 (section 4.5). More...
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| subroutine | sed_routines::make_log_array (xmin, xmax, xarr) |
| | Makes array of values between xmin and xmax, equally spaced in logarithmic space. More...
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| subroutine | sed_routines::make_delta_array (xarr, delta_xarr_bin) |
| | Makes array of bin sizes that can be used for integration. More...
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| subroutine | sed_routines::convert_e_arr_to_t_arr (E_arr, T_arr, ic, ig) |
| | Converts grain enthalpy array into temperature array. More...
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| subroutine | sed_routines::interpolate_qabs_arr_planck (T_arr, qp_arr, ic, ig) |
| | Interpolates Planck averaged emissivity table at the set of input temperatures. More...
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| subroutine | sed_routines::calc_integrals_photon_abs_rate (dust_size) |
| | Calculates integrals of the photon absorbtion rate from a minimum lambda up to all the other possible values. More...
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| subroutine | sed_routines::calc_transition_matrices |
| | Calculates transitions matrices AA() and BB(). More...
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| subroutine | sed_routines::calc_edot_arr (dust_size, T_arr) |
| | Calculates cooling rate at all temperatures in Tarr. It also calculates continuous cooling term BB(i,i+1). More...
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| subroutine | sed_routines::calc_dosage_function_moment_integrals |
| | Calculates dosage function by differentiating the integrals of the photon absorption rate. These integrals are stored in the Rd_integrated array for the energies corresponding to the wavelength grid. The dosage function has to be calculated at the energies corresponding to the enthalpy difference for the levels defined by the grain temperature grid. So, first an interpolation of the Rd_integrated array is necessary. Then differentiation. Then calculation of moments of dosage function is performed up to all energies corresponding to the energy bins. More...
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| subroutine | sed_routines::interpolate_array (num, xarr_in, yarr_in, xarr_out, yarr_out) |
| | Performs linear interpolation for all the values in the arrays xarr_out and yarr_out given the values in the arrays xarr_in and yarr_in. More...
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| subroutine | sed_routines::interpolate_rd_integrated (num, delta_E_arr_in, rd_interpol_in) |
| | Interpolates Rd_integrated() array at the energies corresponding to the transitions between grain enthalphy levels. More...
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| subroutine | sed_routines::make_linear_array (xmin, xmax, xarr) |
| | Makes array of values between xmin and xmax, equally spaced in linear space. More...
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| subroutine | sed_routines::convert_t_arr_to_e_arr (T_arr, E_arr, ic, ig) |
| | Converts temperature array into grain enthalpy array (reverse of convert_E_arr_to_T_arr). More...
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| subroutine | sed_routines::prepare_stellar_emission_library |
| | Reads and interpolates stellar emission library defined in the input (see file_stellar_library() and stellar_library()). More...
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| subroutine | sed_routines::interpolate_lum_to_mass_lib |
| | Interpolates the values of the stellar luminosity-to-mass ratio in lum_to_mass_lib() to the wavelengths in the wavelength grid lambda_arr(). It stores the values in lum_to_mass_int() and deallocate lum_to_mass_lib(). More...
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| subroutine | sed_routines::bilinear_interpolation (xarr, yarr, farr, x, y, fout) |
| | Performs bilinear interpolation given the function farr, evaluated at the points (x1,y1), (x2,y1), (x1, y2), (x2,y2), and the output value coordinates (x,y). More...
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| subroutine | sed_routines::set_star_particle_luminosity (lambda_in) |
| | Sets stellar particle luminosities star_lum() for an input wavelength lambda_in. More...
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| subroutine | sed_routines::find_lambda_index (lambda_in, il) |
| | Finds index in lambda_arr corresponding to the input wavelength lambda_in. More...
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| subroutine | sed_routines::bin_rad_field |
| | Calculates integrals of the stellar emission radiation field spectra in the UV (<4430 A) and optical (> 4430) and assign each cell to a 2-dim bin of radiation field total intensity. Used in the SED library approach for the stochastically heated dust emission. More...
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| real(kind=real64), parameter | sed_routines::t0 =0 |
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| real(kind=real64), parameter | sed_routines::t1 =1E4 |
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| real(kind=real64), parameter | sed_routines::tol =1E-8 |
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| real(kind=real64) | sed_routines::conv_ufield_ifield |
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| real(kind=real64), dimension(:), allocatable | sed_routines::phot_energy |
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| real(kind=real64), dimension(:), allocatable | sed_routines::abs_int_rad_stars |
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| real(kind=real64), dimension(:), allocatable | sed_routines::abs_int_rad_dust |
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| real(kind=real64), dimension(0:2) | sed_routines::rd_arr |
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| logical | sed_routines::large_grain_energy |
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| real(kind=real64) | sed_routines::emin |
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| real(kind=real64) | sed_routines::emax |
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| real(kind=real64) | sed_routines::tmin |
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| real(kind=real64) | sed_routines::tmin_prev |
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| real(kind=real64) | sed_routines::tmax |
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| real(kind=real64) | sed_routines::tmax_prev |
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| real(kind=real64), dimension(:), allocatable | sed_routines::e_arr |
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| real(kind=real64), dimension(:), allocatable | sed_routines::t_arr |
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| real(kind=real64), dimension(:), allocatable | sed_routines::pt |
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| real(kind=real64), dimension(:), allocatable | sed_routines::qp_arr |
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| real(kind=real64), dimension(:), allocatable | sed_routines::delta_e_arr_bin |
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| integer, parameter | sed_routines::n_temp_pt = 300 |
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| real(kind=real64), dimension(:), allocatable | sed_routines::rd_integrated |
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| real(kind=real64), dimension(:,:), allocatable | sed_routines::aa |
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| real(kind=real64), dimension(:,:), allocatable | sed_routines::bb |
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| real(kind=real64), dimension(:), allocatable | sed_routines::re0 |
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| real(kind=real64), dimension(:), allocatable | sed_routines::re1 |
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| real(kind=real64), dimension(:), allocatable | sed_routines::re2 |
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| real(kind=real64), dimension(:), allocatable | sed_routines::edot_arr |
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| real(kind=real64), dimension(:), allocatable | sed_routines::tot_dust_em |
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| real(kind=real64), dimension(:,:), allocatable | sed_routines::dust_em_arr_fa |
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| real(kind=real64), dimension(:), allocatable | sed_routines::int_rf_uv |
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| real(kind=real64), dimension(:), allocatable | sed_routines::int_rf_opt |
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| real(kind=real64), dimension(:), allocatable | sed_routines::rf_uv_arr |
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| real(kind=real64), dimension(:), allocatable | sed_routines::rf_opt_arr |
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| real(kind=real64), dimension(:,:,:), allocatable | sed_routines::u_av_uv_opt |
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| real(kind=real64), dimension(:,:,:), allocatable | sed_routines::u_av_dust |
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| real(kind=real64), dimension(:,:), allocatable | sed_routines::count_spectra_uv_opt |
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1.8.11
