radis.lbl package¶

Submodules¶

Module contents¶

Core of the line-by-line calculations

class LevelsList(parfunc, bands, levelsfmt, sortby='Ei', copy_lines=False, verbose=True)[source]¶

Bases: object

A class to generate a Spectrum from a list of precalculated bands at a given reference temperature.

Warning

only valid under optically thin conditions!!

E_bands[source]¶
Qref[source]¶
Qvib_ref[source]¶
Trot_ref[source]¶
Tvib_ref[source]¶
bands[source]¶
bands_ref[source]¶
copy_lines[source]¶
cum_weight[source]¶
eq_spectrum(Tgas, overpopulation=None, mole_fraction=None, path_length=None, save_rescaled_bands=False)[source]¶

See eq_spectrum()

Warning

only valid under optically thin conditions!!

Parameters
  • … same as usually. If None, then the reference value (used to

  • calculate bands) is used

Other Parameters

save_rescaled_bands (boolean) – save updated bands. Take some time as it requires rescaling all bands individually (which is only done on the MergedSlabs usually) Default False

levelsfmt[source]¶
lvl_index[source]¶
mole_fraction_ref[source]¶
non_eq_spectrum(Tvib=None, Trot=None, Ttrans=None, vib_distribution='boltzmann', overpopulation=None, mole_fraction=None, path_length=None, save_rescaled_bands=False)[source]¶

See non_eq_spectrum()

Warning

only valid under optically thin conditions!!

Parameters
  • … same as usually. If None, then the reference value (used to

  • calculate bands) is used

Other Parameters

save_rescaled_bands (boolean) – save updated bands. Take some time as it requires rescaling all bands individually (which is only done on the MergedSlabs usually) Default False

Notes

Implementation:

Generation of a new spectrum is done by recombination of the precalculated bands with

parfunc[source]¶
path_length_ref[source]¶
plot_vib_populations(nfig=None, **kwargs)[source]¶

Plot current distribution of vibrational levels.

By constructions populations are shown as divided by the state degeneracy, i.e, g = gv * (2J+1) * gi * gs

Parameters
  • nfig (str, int) – name of Figure to plot on

  • kwargs (**dict) – arguments are forwarded to plot()

sorted_bands[source]¶
verbose[source]¶
vib_distribution_ref[source]¶
vib_levels[source]¶
class SpectrumFactory(wmin=None, wmax=None, wunit=cm - 1, wavenum_min=None, wavenum_max=None, wavelength_min=None, wavelength_max=None, Tref=296, pressure=1.01325, mole_fraction=1, path_length=1, wstep=0.01, molecule=None, isotope='all', medium='air', truncation=50, neighbour_lines=0, pseudo_continuum_threshold=0, self_absorption=True, chunksize=None, optimization='simple', folding_thresh=1e-06, zero_padding=- 1, broadening_method='voigt', cutoff=0, parsum_mode='full summation', verbose=True, warnings=True, save_memory=False, export_populations=None, export_lines=False, **kwargs)[source]¶

Bases: radis.lbl.bands.BandFactory

A class to put together all functions related to loading CDSD / HITRAN databases, calculating the broadenings, and summing over all the lines.

Parameters
  • wmin, wmax (float or Quantity) – a hybrid parameter which can stand for minimum (maximum) wavenumber or minimum (maximum) wavelength depending upon the unit accompanying it. If dimensionless, wunit is considered as the accompanying unit.

  • wunit ('nm', 'cm-1') – the unit accompanying wmin and wmax. Can only be passed with wmin and wmax. Default is "cm-1".

  • wavenum_min, wavenum_max (float(cm^-1) or Quantity) – minimum (maximum) wavenumber to be processed in \(cm^{-1}\). use astropy.units to specify arbitrary inverse-length units.

  • wavelength_min, wavelength_max (float(nm) or Quantity) – minimum (maximum) wavelength to be processed in \(nm\). This wavelength can be in 'air' or 'vacuum' depending on the value of the parameter medium=. use astropy.units to specify arbitrary length units.

  • pressure (float(bar) or Quantity) – partial pressure of gas in bar. Default 1.01325 (1 atm). use astropy.units to specify arbitrary pressure units. For example, 1013.25 * u.mbar.

  • mole_fraction (float [ 0 - 1]) – species mole fraction. Default 1. Note that the rest of the gas is considered to be air for collisional broadening.

  • path_length (float(cm) or Quantity) – path length in cm. Default 1. use astropy.units to specify arbitrary length units.

  • molecule (int, str, or None) – molecule id (HITRAN format) or name. If None, the molecule can be infered from the database files being loaded. See the list of supported molecules in MOLECULES_LIST_EQUILIBRIUM and MOLECULES_LIST_NONEQUILIBRIUM. Default None.

  • isotope (int, list, str of the form '1,2', or 'all') – isotope id (sorted by relative density: (eg: 1: CO2-626, 2: CO2-636 for CO2). See HITRAN documentation for isotope list for all species. If ‘all’, all isotopes in database are used (this may result in larger computation times!). Default 'all'

  • medium ('air', 'vacuum') – propagating medium when giving inputs with 'wavenum_min', 'wavenum_max'. Does not change anything when giving inputs in wavenumber. Default 'air'

Other Parameters
  • Tref (K) – Reference temperature for calculations (linestrength temperature correction). HITRAN database uses 296 Kelvin. Default 296 K

  • self_absorption (boolean) – Compute self absorption. If False, spectra are optically thin. Default True.

  • truncation (float (\(cm^{-1}\))) – Half-width over which to compute the lineshape, i.e. lines are truncated on each side after truncation (\(cm^{-1}\)) from the line center. If None, use no truncation (lineshapes spread on the full spectral range). Default is 300 \(cm^{-1}\)

    Note

    Large values (> 50) can induce a performance drop (computation of lineshape typically scale as \(~truncation ^2\) ). The default 300 was chosen to maintain a good accuracy, and still exhibit the sub-Lorentzian behavior of most lines far (few hundreds \(cm^{-1}\)) from the line center.

  • neighbour_lines (float (\(cm^{-1}\))) – The calculated spectral range is increased (by neighbour_lines cm-1 on each side) to take into account overlaps from out-of-range lines. Default is 0 \(cm^{-1}\).​

  • wstep (float (cm-1) or 'auto') – Resolution of wavenumber grid. Default 0.01 cm-1. If 'auto', it is ensured that there are slightly more points for each linewidth than the value of "GRIDPOINTS_PER_LINEWIDTH_WARN_THRESHOLD" in radis.config (~/radis.json)

    Note

    wstep = ‘auto’ is optimized for performances while ensuring accuracy, but is still experimental in 0.9.30. Feedback welcome!

  • cutoff (float (~ unit of Linestrength: cm-1/(#.cm-2))) – discard linestrengths that are lower that this, to reduce calculation times. 1e-27 is what is generally used to generate databases such as CDSD. If 0, no cutoff. Default 1e-27.

  • parsum_mode (‘full summation’, ‘tabulation’) – how to compute partition functions, at nonequilibrium or when partition function are not already tabulated. 'full summation' : sums over all (potentially millions) of rovibrational levels. 'tabulation' : builds an on-the-fly tabulation of rovibrational levels (500 - 4000x faster and usually accurate within 0.1%). Default full summation'

    Note

    parsum_mode= ‘tabulation’ is new in 0.9.30, and makes nonequilibrium calculations of small spectra extremelly fast. Will become the default after 0.9.31.

  • pseudo_continuum_threshold (float) – if not 0, first calculate a rough approximation of the spectrum, then moves all lines whose linestrength intensity is less than this threshold of the maximum in a semi-continuum. Values above 0.01 can yield significant errors, mostly in highly populated areas. 80% of the lines can typically be moved in a continuum, resulting in 5 times faster spectra. If 0, no semi-continuum is used. Default 0.

  • save_memory (boolean) – if True, removes databases calculated by intermediate functions (for instance, delete the full database once the linestrength cutoff criteria was applied). This saves some memory but requires to reload the database & recalculate the linestrength for each new parameter. Default False.

  • export_populations ('vib', 'rovib', None) – if not None, store populations in Spectrum. Either store vibrational populations (‘vib’) or rovibrational populations (‘rovib’). Default None

  • export_lines (boolean) – if True, saves details of all calculated lines in Spectrum. This is necessary to later use line_survey(), but can take some space. Default False.

  • chunksize (int, or None) – Splits the lines database in several chuncks during calculation, else the multiplication of lines over all spectral range takes too much memory and slows the system down. Chunksize let you change the default chunck size. If None, all lines are processed directly. Usually faster but can create memory problems. Default None

  • optimization ("simple", "min-RMS", None) – If either "simple" or "min-RMS" DLM optimization for lineshape calculation is used: - "min-RMS" : weights optimized by analytical minimization of the RMS-error (See: [Spectral-Synthesis-Algorithm]) - "simple" : weights equal to their relative position in the grid

    If using the DLM optimization, broadening method is automatically set to 'fft'. If None, no lineshape interpolation is performed and the lineshape of all lines is calculated.

    Refer to [Spectral-Synthesis-Algorithm] for more explanation on the DLM method for lineshape interpolation.

    Default "min-RMS"

  • folding_thresh (float) – Folding is a correction procedure thet is applied when the lineshape is calculated with the fft broadening method and the linewidth is comparable to wstep, that prevents sinc(v) modulation of the lineshape. Folding continues until the lineshape intensity is below folding_threshold. Setting to 1 or higher effectively disables folding correction.

    Range: 0.0 < folding_thresh <= 1.0 Default: 1e-6

  • zero_padding (int) – Zero padding is used in conjunction with the fft broadening method to prevent circular convolution at the cost of performance. When set to -1, padding is set equal to the spectrum length, which guarantees a linear convolution.

    Range: 0 <= zero_padding <= len(w), or zero_padding = -1 Default: -1

  • broadening_method ("voigt", "convolve", "fft") – Calculates broadening with a direct voigt approximation (‘voigt’) or by convoluting independantly calculated Doppler and collisional broadening (‘convolve’). First is much faster, 2nd can be used to compare results. This SpectrumFactory parameter can be manually adjusted a posteriori with:

    sf = SpectrumFactory(...)
    sf.params.broadening_method = 'voigt'
    

    Fast fourier transform 'fft' is only available if using the DLM lineshape calculation optimization. Because the DLM convolves all lines at the same time, and thus operates on large arrays, 'fft' becomes more appropriate than convolutions in real space ('voit', 'convolve' )

    By default, use "fft" for any optimization, and "voigt" if optimization is None .

  • warnings (bool, or one of ['warn', 'error', 'ignore'], dict) – If one of ['warn', 'error', 'ignore'], set the default behaviour for all warnings. Can also be a dictionary to set specific warnings only. Example:

    warnings = {'MissingSelfBroadeningWarning':'ignore',
                'NegativeEnergiesWarning':'ignore',
                'HighTemperatureWarning':'ignore'}
    

    See default_warning_status for more information.

  • verbose (boolean, or int) – If False, stays quiet. If True, tells what is going on. If >=2, gives more detailed messages (for instance, details of calculation times). Default True.

Examples

An example using SpectrumFactory, load_databank(), the Spectrum methods, and units

from radis import SpectrumFactory
from astropy import units as u
sf = SpectrumFactory(wavelength_min=4165 * u.nm,
                     wavelength_max=4200 * u.nm,
                     isotope='1,2',
                     truncation=10,  # cm-1
                     optimization=None,
                     medium='vacuum',
                     verbose=1,    # more for more details
                     )
sf.load_databank('HITRAN-CO2-TEST')        # predefined in ~/radis.json
s = sf.eq_spectrum(Tgas=300 * u.K, path_length=1 * u.cm)
s.rescale_path_length(0.01)    # cm
s.plot('radiance_noslit', Iunit='µW/cm2/sr/nm')

Refer to the online Examples for more cases.

Notes

Inheritance diagram of radis.lbl.factory.SpectrumFactory

High-level wrapper to SpectrumFactory:

Main Methods:

For advanced use:

Inputs and parameters can be accessed a posteriori with :

  • input : physical input

  • params : computational parameters

  • misc : miscallenous parameters (don’t change output)

See also

calc_spectrum()

eq_spectrum(Tgas, mole_fraction=None, path_length=None, pressure=None, name=None) radis.spectrum.spectrum.Spectrum[source]¶

Generate a spectrum at equilibrium.

Parameters
  • Tgas (float or Quantity) – Gas temperature (K)

  • mole_fraction (float) – database species mole fraction. If None, Factory mole fraction is used.

  • path_length (float or Quantity) – slab size (cm). If None, the default Factory path_length is used.

  • pressure (float or Quantity) – pressure (bar). If None, the default Factory pressure is used.

  • name (str) – output Spectrum name (useful in batch)

Returns

s –

Returns a Spectrum object

Use the get() method to get something among ['radiance', 'radiance_noslit', 'absorbance', etc...]

Or directly the plot() method to plot it. See [1]_ to get an overview of all Spectrum methods

Return type

Spectrum

Examples

::

from radis import SpectrumFactory sf = SpectrumFactory( wavenum_min=2900, wavenum_max=3200, molecule=”OH”, wstep=0.1, ) sf.fetch_databank(“hitemp”)

s1 = sf.eq_spectrum(Tgas=300, path_length=1, pressure=0.1) s2 = sf.eq_spectrum(Tgas=500, path_length=1, pressure=0.1)

References

1

RADIS doc: Spectrum how to?

eq_spectrum_gpu(Tgas, mole_fraction=None, path_length=None, pressure=None, name=None) radis.spectrum.spectrum.Spectrum[source]¶

Generate a spectrum at equilibrium with calculation of lineshapes and broadening done on the GPU.

Note

This method requires CUDA compatible hardware to execute. For more information on how to setup your system to run GPU-accelerated methods using CUDA and Cython, check GPU Spectrum Calculation on RADIS

Parameters
  • Tgas (float or Quantity) – Gas temperature (K)

  • mole_fraction (float) – database species mole fraction. If None, Factory mole fraction is used.

  • path_length (float or Quantity) – slab size (cm). If None, the default Factory path_length is used.

  • pressure (float or Quantity) – pressure (bar). If None, the default Factory pressure is used.

  • name (str) – output Spectrum name (useful in batch)

Returns

s –

Returns a Spectrum object

Use the get() method to get something among ['radiance', 'radiance_noslit', 'absorbance', etc...]

Or directly the plot() method to plot it. See [1]_ to get an overview of all Spectrum methods

Return type

Spectrum

See also

eq_spectrum()

fit_spectrum(s_exp, model, fit_parameters, bounds={}, plot=False, solver_options={'maxiter': 300}, **kwargs) Union[radis.spectrum.spectrum.Spectrum, scipy.optimize.optimize.OptimizeResult][source]¶

Fit an experimental spectrum with an arbitrary model and an arbitrary number of fit parameters.

Parameters
  • s_exp (Spectrum) – experimental spectrum. Should have only spectral array only. Use take(), e.g:

    sf.fit_spectrum(s_exp.take('transmittance'))
    
  • model (func -> Spectrum) – a line-of-sight model returning a Spectrum. Example : Tvib12Tvib3Trot_NonLTEModel()

  • fit_parameters (dict) –

    example:

    {fit_parameter:initial_value}
    
  • bounds (dict, optional) –

    example:

    {fit_parameter:[min, max]}
    
  • fixed_parameters (dict) –

    fixed parameters given to the model. Example:

    fit_spectrum(fixed_parameters={"vib_distribution":"treanor"})
    
Other Parameters
  • plot (bool) – if True, plot spectra as they are computed; and plot the convergence of the residual. Default False

  • solver_options (dict) – parameters forwarded to the solver. More info in minimize Example:

    {"maxiter": (int)  max number of iteration default ``300``,
     }
    
  • kwargs (dict) – forwarded to fit_spectrum()

Returns

  • s_best (Spectrum) – best spectrum

  • res (OptimizeResults) – output of minimize

Examples

See a one-temperature fit example and a non-LTE fit example

More advanced tools for interactive fitting of multi-dimensional, multi-slabs spectra can be found in fitroom.

generate_perf_profile()[source]¶

Generate a visual/interactive performance profile diagram for the last calculated spectrum

Examples

sf = SpectrumFactory(...)
sf.eq_spectrum(...)
sf.generate_perf_profile()

See typical output in https://github.com/radis/radis/pull/325

https://user-images.githubusercontent.com/16088743/128018032-6049be72-1881-46ac-9d7c-1ed89f9c4f42.png

Note

You can also profile with tuna directly:

python -m cProfile -o program.prof your_radis_script.py
tuna your_radis_script.py
non_eq_spectrum(Tvib, Trot, Ttrans=None, mole_fraction=None, path_length=None, pressure=None, vib_distribution='boltzmann', rot_distribution='boltzmann', overpopulation=None, name=None) radis.spectrum.spectrum.Spectrum[source]¶

Calculate emission spectrum in non-equilibrium case. Calculates absorption with broadened linestrength and emission with broadened Einstein coefficient.

Parameters
  • Tvib (float) – vibrational temperature [K] can be a tuple of float for the special case of more-than-diatomic molecules (e.g: CO2)

  • Trot (float) – rotational temperature [K]

  • Ttrans (float) – translational temperature [K]. If None, translational temperature is taken as rotational temperature (valid at 1 atm for times above ~ 2ns which is the RT characteristic time)

  • mole_fraction (float) – database species mole fraction. If None, Factory mole fraction is used.

  • path_length (float or Quantity) – slab size (cm). If None, the default Factory path_length is used.

  • pressure (float or Quantity) – pressure (bar). If None, the default Factory pressure is used.

Other Parameters
  • vib_distribution ('boltzmann', 'treanor') – vibrational distribution

  • rot_distribution ('boltzmann') – rotational distribution

  • overpopulation (dict, or None) –

    add overpopulation factors for given levels:

    {level:overpopulation_factor}
    
  • name (str) – output Spectrum name (useful in batch)

Returns

s –

Returns a Spectrum object

Use the get() method to get something among ['radiance', 'radiance_noslit', 'absorbance', etc...]

Or directly the plot() method to plot it. See [1]_ to get an overview of all Spectrum methods

Return type

Spectrum

Examples

::

from radis import SpectrumFactory sf = SpectrumFactory( wavenum_min=2000, wavenum_max=3000, molecule=”CO”, wstep=0.1, ) sf.fetch_databank(“hitemp”)

s1 = sf.non_eq_spectrum(Tvib=2000, Trot=600, path_length=1, pressure=0.1) s2 = sf.non_eq_spectrum(Tvib=2000, Trot=600, path_length=1, pressure=0.1)

References

1

RADIS doc: Spectrum how to?

optically_thin_power(Tgas=None, Tvib=None, Trot=None, Ttrans=None, vib_distribution='boltzmann', rot_distribution='boltzmann', mole_fraction=None, path_length=None, unit='mW/cm2/sr')[source]¶

Calculate total power emitted in equilibrium or non-equilibrium case in the optically thin approximation: it sums all emission integral over the total spectral range.

Warning

this is a fast implementation that doesnt take into account the contribution of lines outside the given spectral range. It is valid for spectral ranges surrounded by no lines, and spectral ranges much broaded than the typical line broadening (~ 1-10 cm-1 in the infrared)

If what you’re looking for is an accurate simulation on a narrow spectral range you better calculate the spectrum (that does take all of that into account) and integrate it with get_power()

Parameters
  • Tgas (float) – equilibrium temperature [K] If doing a non equilibrium case it should be None. Use Ttrans for translational temperature

  • Tvib (float) – vibrational temperature [K]

  • Trot (float) – rotational temperature [K]

  • Ttrans (float) – translational temperature [K]. If None, translational temperature is taken as rotational temperature (valid at 1 atm for times above ~ 2ns which is the RT characteristic time)

  • mole_fraction (float) – database species mole fraction. If None, Factory mole fraction is used.

  • path_length (float) – slab size (cm). If None, Factory mole fraction is used.

  • unit (str) – output unit. Default 'mW/cm2/sr'

Returns

float – see unit=.

Return type

Returns total power density in mW/cm2/sr (unless different unit is chosen),

predict_time()[source]¶

predict_time(self) uses the input parameters like Spectral Range, Number of lines, wstep, truncation to predict the estimated calculation time for the Spectrum broadening step(bottleneck step) for the current optimization and broadening_method. The formula for predicting time is based on benchmarks performed on various parameters for different optimization, broadening_method and deriving its time complexity.

Benchmarks: https://anandxkumar.github.io/Benchmark_Visualization_GSoC_2021/

Complexity vs Calculation Time Visualizations LBL>Voigt: LINK, DIT>Voigt: LINK, DIT>FFT: LINK

Returns

float

Return type

Predicted time in seconds.

print_perf_profile(number_format='{:.3f}', precision=16)[source]¶

Prints Profiler output dictionary in a structured manner for the last calculated spectrum

Examples

sf.print_perf_profile()

# output >>
    spectrum_calculation      0.189s ████████████████
        check_line_databank              0.000s
        check_non_eq_param               0.042s ███
        fetch_energy_5                   0.015s █
        calc_weight_trans                0.008s
        reinitialize                     0.002s
            copy_database                    0.000s
            memory_usage_warning             0.002s
            reset_population                 0.000s
        calc_noneq_population            0.041s ███
            part_function                    0.035s ██
            population                       0.006s
        scaled_non_eq_linestrength       0.005s
            map_part_func                    0.001s
            corrected_population_se          0.003s
        calc_emission_integral           0.006s
        applied_linestrength_cutoff      0.002s
        calc_lineshift                   0.001s
        calc_hwhm                        0.007s
        generate_wavenumber_arrays       0.001s
        calc_line_broadening             0.074s ██████
            precompute_DLM_lineshapes        0.012s
            DLM_Initialized_vectors          0.000s
            DLM_closest_matching_line        0.001s
            DLM_Distribute_lines             0.001s
            DLM_convolve                     0.060s █████
            others                           0.001s
        calc_other_spectral_quan         0.003s
        generate_spectrum_obj            0.000s
        others                           -0.016s
Other Parameters

precision (int, optional) – total number of blocks. Default 16.

calc_spectrum(wavenum_min=None, wavenum_max=None, wavelength_min=None, wavelength_max=None, Tgas=None, Tvib=None, Trot=None, pressure=1.01325, molecule=None, isotope='all', mole_fraction=1, path_length=1, databank='hitran', medium='air', wstep=0.01, truncation=50, neighbour_lines=0, cutoff=1e-27, parsum_mode='full summation', optimization='min-RMS', broadening_method='voigt', overpopulation=None, name=None, save_to='', use_cached=True, mode='cpu', export_lines=False, verbose=True, **kwargs) radis.spectrum.spectrum.Spectrum[source]¶

Multipurpose function to calculate a Spectrum.

Can automatically download databases (HITRAN/HITEMP) or use manually downloaded local databases, under equilibrium or non-equilibrium, with or without overpopulation, using either CPU or GPU.

It is a wrapper to SpectrumFactory class. For advanced used, please refer to the aforementionned class.

Parameters
  • wavenum_min, wavenum_max (float [\(cm^{-1}\)] or Quantity) –

    wavenumber range to be processed in \(cm^{-1}\). Use arbitrary units:

    import astropy.units as u
    calc_spectrum(2.5*u.um, 3.0*u.um, ...)
    
  • wavelength_min, wavelength_max (float [\(nm\)] or Quantity) – wavelength range to be processed in \(nm\). Wavelength in 'air' or 'vacuum' depending of the value of 'medium'.

  • Tgas (float [\(K\)]) – Gas temperature. If non equilibrium, is used for \(T_{translational}\). Default 300 K​

  • Tvib, Trot (float [\(K\)]) – Vibrational and rotational temperatures (for non-LTE calculations). If None, they are at equilibrium with Tgas ​.

  • pressure (float [\(bar\)] or Quantity) –

    partial pressure of gas in bar. Default 1.01325 (1 atm)​. Use arbitrary units:

    import astropy.units as u
    calc_spectrum(..., pressure=20*u.mbar)
    
  • molecule (int, str, list or None) – molecule id (HITRAN format) or name. For multiple molecules, use a list. The 'isotope', 'mole_fraction', 'databank' and 'overpopulation' parameters must then be dictionaries. If None, the molecule can be infered from the database files being loaded. See the list of supported molecules in MOLECULES_LIST_EQUILIBRIUM and MOLECULES_LIST_NONEQUILIBRIUM. Default None.​

  • isotope (int, list, str of the form '1,2', or 'all', or dict) – isotope id (sorted by relative density: (eg: 1: CO2-626, 2: CO2-636 for CO2). See [HITRAN-2016] documentation for isotope list for all species. If 'all', all isotopes in database are used (this may result in larger computation times!). Default 'all'.

    For multiple molecules, use a dictionary with molecule names as keys

    isotope={'CO2':'1,2' ,  'CO':'1,2,3' }​
    
  • mole_fraction (float or dict) – database species mole fraction. Default 1.

    For multiple molecules, use a dictionary with molecule names as keys

    mole_fraction={'CO2': 0.8, 'CO':0.2}​
    
  • path_length (float [\(cm\)] or Quantity) –

    slab size. Default 1 cm​. Use arbitrary units:

    import astropy.units as u
    calc_spectrum(..., path_length=1000*u.km)
    
  • databank (str or dict) – can be either: - 'hitran', to fetch automatically the latest HITRAN version

    through fetch_astroquery() (based on [HAPI] ).

    • 'hitemp', to fetch automatically the latest HITEMP version through fetch_hitemp().

    • the name of a a valid database file, in which case the format is inferred. For instance, '.par' is recognized as hitran/hitemp format. Accepts wildcards '*' to select multiple files.

    • the name of a spectral database registered in your ~/radis.json configuration file. This allows to use multiple database files.

    Default 'hitran'. See DatabankLoader for more information on line databases, and DBFORMAT for your ~/radis.json file format.

    For multiple molecules, use a dictionary with molecule names as keys:

    databank='hitran'     # automatic download (or 'hitemp')
    databank='PATH/TO/05_HITEMP2019.par'    # path to a file
    databank='*CO2*.par' #to get all the files that have CO2 in their names (case insensitive)
    databank='HITEMP-2019-CO'   # user-defined database in Configuration file
    databank = {'CO2' : 'PATH/TO/05_HITEMP2019.par', 'CO' : 'hitran'}  # for multiple molecules
    
Other Parameters
  • medium ('air', 'vacuum') – propagating medium when giving inputs with 'wavenum_min', 'wavenum_max'. Does not change anything when giving inputs in wavenumber. Default ``’air’``​ .

  • wstep (float (\(cm^{-1}\)) or 'auto') – Resolution of wavenumber grid. Default 0.01 cm-1. If 'auto', it is ensured that there are slightly more or less than GRIDPOINTS_PER_LINEWIDTH_WARN_THRESHOLD points for each linewidth.

    Note

    wstep = ‘auto’ is optimized for performances while ensuring accuracy, but is still experimental in 0.9.30. Feedback welcome!

  • truncation (float (\(cm^{-1}\))) – Half-width over which to compute the lineshape, i.e. lines are truncated on each side after truncation (\(cm^{-1}\)) from the line center. If None, use no truncation (lineshapes spread on the full spectral range). Default is 300 \(cm^{-1}\)

    Note

    Large values (> 50) can induce a performance drop (computation of lineshape typically scale as \(~truncation ^2\) ). The default 300 was chosen to maintain a good accuracy, and still exhibit the sub-Lorentzian behavior of most lines far (few hundreds \(cm^{-1}\)) from the line center.

  • neighbour_lines (float (\(cm^{-1}\))) – The calculated spectral range is increased (by neighbour_lines cm-1 on each side) to take into account overlaps from out-of-range lines. Default is 0 \(cm^{-1}\).​

  • cutoff (float (~ unit of Linestrength: \(cm^{-1}/(molec.cm^{-2})\))) – discard linestrengths that are lower that this, to reduce calculation times. 1e-27 is what is generally used to generate line databases such as CDSD. If 0, no cutoff. Default 1e-27 .

  • parsum_mode (‘full summation’, ‘tabulation’) – how to compute partition functions, at nonequilibrium or when partition function are not already tabulated. 'full summation' : sums over all (potentially millions) of rovibrational levels. 'tabulation' : builds an on-the-fly tabulation of rovibrational levels (500 - 4000x faster and usually accurate within 0.1%). Default full summation'

    Note

    parsum_mode= ‘tabulation’ is new in 0.9.30, and makes nonequilibrium calculations of small spectra extremelly fast. Will become the default after 0.9.31.

  • optimization ("simple", "min-RMS", None) – If either "simple" or "min-RMS" LDM optimization for lineshape calculation is used:

    • "min-RMS" : weights optimized by analytical minimization of the RMS-error (See: [Spectral-Synthesis-Algorithm])

    • "simple" : weights equal to their relative position in the grid

    If using the LDM optimization, broadening method is automatically set to 'fft'. If None, no lineshape interpolation is performed and the lineshape of all lines is calculated. Refer to [Spectral-Synthesis-Algorithm] for more explanation on the LDM method for lineshape interpolation. Default "min-RMS".

  • overpopulation (dict) – dictionary of overpopulation compared to the given vibrational temperature. Default None. Example:

    overpopulation = {'CO2' : {'(00`0`0)->(00`0`1)': 2.5,
                               '(00`0`1)->(00`0`2)': 1,
                               '(01`1`0)->(01`1`1)': 1,
                               '(01`1`1)->(01`1`2)': 1 }
                     }​
    
  • export_lines (boolean) – if True, saves details of all calculated lines in Spectrum. This is necessary to later use line_survey(), but can take some space. Default False.

  • name (str) – name of the output Spectrum. If None, a unique ID is generated.

  • save_to (str) – save to a spec file which contains absorption & emission features, all calculation parameters, and can be opened with load_spec(). File can be reloaded and exported to text formats afterwards, see savetxt(). If file already exists, replace.

  • use_cached (boolean) – use cached files for line database and energy database. Default True.​

  • verbose (boolean, or int) – If False, stays quiet. If True, tells what is going on. If >=2, gives more detailed messages (for instance, details of calculation times). Default True.​

  • mode ('cpu', 'gpu') – if set to 'cpu', computes the spectra purely on the CPU. if set to 'gpu', offloads the calculations of lineshape and broadening steps to the GPU making use of parallel computations to speed up the process. Default 'cpu'. Note that mode='gpu' requires CUDA compatible hardware to execute. For more information on how to setup your system to run GPU-accelerated methods using CUDA and Cython, check GPU Spectrum Calculation on RADIS

  • **kwargs (other inputs forwarded to SpectrumFactory) – For instance: warnings. See SpectrumFactory documentation for more details on input.

Returns

Output spectrum:

  • Use the get() method to retrieve a spectral quantity ('radiance', 'radiance_noslit', 'absorbance', etc…)

  • Or the plot() method to plot it directly.

  • See [1]_ to get an overview of all Spectrum methods

Return type

Spectrum

References

1

RADIS doc: Spectrum how to?

​.. [2] RADIS GPU support: GPU Calculations on RADIS ​

Examples

Calculate a CO spectrum from the HITRAN database:

from radis import calc_spectrum
s = calc_spectrum(1900, 2300,         # cm-1
                  molecule='CO',
                  isotope='1,2,3',
                  pressure=1.01325,   # bar
                  Tgas=1000,
                  mole_fraction=0.1,
                  databank='hitran',  # or 'hitemp'
                  )
s.apply_slit(0.5, 'nm')
s.plot('radiance')

This example uses the apply_slit() and plot() methods. See also line_survey():

s.line_survey(overlay='radiance')

Calculate a CO2 spectrum from the CDSD-4000 database:

s = calc_spectrum(2200, 2400,   # cm-1
                  molecule='CO2',
                  isotope='1',
                  databank='/path/to/cdsd/databank/in/npy/format/',
                  pressure=0.1,  # bar
                  Tgas=1000,
                  mole_fraction=0.1,
                  mode='gpu'
                  )

s.plot('absorbance')

This example uses the eq_spectrum_gpu() method to calculate the spectrum on the GPU. The databank points to the CDSD-4000 databank that has been pre-processed and stored in numpy.npy format. ​ Refer to the online Examples for more cases, and to the Spectrum page for details on post-processing methods.

For more details on how to use the GPU method and process the database, refer to the examples linked above and the documentation on GPU support for RADIS. ​ .. minigallery:: radis.lbl.calc.calc_spectrum

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References

cite: RADIS is built on the shoulders of many state-of-the-art packages and databases. If using RADIS to compute spectra, make sure you cite all of them, for proper reproducibility and acknowledgement of the work ! See How to cite?

See also

SpectrumFactory