radis.spectrum package¶

Submodules¶

Module contents¶

Spectrum-class module for post-processing.

PerfectAbsorber(s: Spectrum) → Spectrum[source]¶

Makes a new Spectrum with the same transmittance/absorbance as Spectrum s, but with radiance set to 0. Useful to get contribution of different slabs in line-of-sight calculations (see example).

Parameters: s (Spectrum) – Spectrum object
Returns: s_tr – Spectrum object, with only the transmittance, absorbance and/or abscoeff part of s, where radiance_noslit , emisscoeff and emissivity_noslit (if they exist) have been set to 0
Return type: Spectrum

Examples

Let’s say you have a total line of sight:

s_los = s1 > s2 > s3

If you now want to get the contribution of s2 to the line-of-sight emission, you can do:

(s2 > PerfectAbsorber(s3)).plot('radiance_noslit')

And the contribution of s1 would be:

(s1 > PerfectAbsorber(s2>s3)).plot('radiance_noslit')

See more examples in Line-of-Sight module

Radiance(s: Spectrum) → Spectrum[source]¶

Returns a new Spectrum with only the radiance component of s

Parameters: s (Spectrum) – Spectrum object
Returns: s_tr – Spectrum object, with only radiance defined
Return type: Spectrum

Examples

This function is useful to use Spectrum algebra operations:

s = calc_spectrum(...)   # contains emission & absorption arrays
rad = Radiance(s)        # contains radiance array only
rad -= 0.1    # arithmetic operation is applied to Radiance only

Equivalent to:

rad = s.take('radiance')

Radiance_noslit(s: Spectrum) → Spectrum[source]¶

Returns a new Spectrum with only the radiance_noslit component of s

Parameters: s (Spectrum) – Spectrum object
Returns: s_tr – Spectrum object, with only radiance_noslit defined
Return type: Spectrum

Examples

This function is useful to use Spectrum algebra operations:

s = calc_spectrum(...)   # contains emission & absorption arrays
rad = Radiance_noslit(s) # contains 'radiance_noslit' array only
rad -= 0.1    # arithmetic operation is applied to Radiance_noslit only

Equivalent to:

rad = s.take('radiance_noslit')

class Spectrum(quantities, units=None, conditions=None, cond_units=None, populations=None, lines=None, wunit=None, name=None, references={}, check_wavespace=True, **kwargs)[source]¶

Bases: object

This class holds results calculated with the SpectrumFactory calculation, with other radiative codes, or experimental data. It can be used to plot different quantities a posteriori, or manipulate output units (for instance convert a spectral radiance per wavelength units to a spectral radiance per wavenumber).

See more information on how to generate, edit or combine Spectrum objects on the Spectrum object guide.

Parameters

quantities (dict of tuples {'quantity':(w, a)} or dict {'wavelength/wavenumber': w, quantity': a}) – where quantities are spectral quantities (absorbance, radiance, etc.) and wavenum is in \(cm^{-1}\) or \(nm\) (see waveunit) Example:

# w, k, I are numpy arrays for wavenumbers, absorption coefficient, and radiance.
from radis import Spectrum
s = Spectrum({"wavenumber":w, "abscoeff":k, "radiance_noslit":I}, wunit='cm-1',
             units={"radiance_noslit":"mW/cm2/sr/nm", "abscoeff":"cm-1"})

Or:

s = Spectrum({"abscoeff":(w,k), "radiance_noslit":(w,I)},
             wunit="cm-1"
             units={"radiance_noslit":"mW/cm2/sr/nm", "abscoeff":"cm-1"})

See also: from_array() and from_txt()

units (dict) – units for quantities

Other Parameters

conditions (dict) – physical conditions and calculation parameters
wunit ('nm', 'cm-1', 'nm_vac' or None) – wavelength in air ('nm'), wavenumber ('cm-1'), or wavelength in vacuum ('nm_vac'). If None, 'wavespace' must be defined in conditions. Quantities should be evenly distributed along this space for fast convolution with the slit function
cond_units (dict) – units for conditions

Other Parameters

name (str, or None) – Give a name to this Spectrum object (automatically used in plots; useful for multislab configurations). Default None
populations (dict) – a dictionary of all species, and levels. Should be compatible with other radiative codes such as Specair output. Suggested format: {molecules: {isotopes: {elec state: rovib levels}}} e.g:
```
{'CO2':{1: 'X': df}}   # with df a Pandas Dataframe
```
lines (pandas Dataframe) – all lines in databank (necessary for using line_survey()). Warning if you want to play with the lines content: The signification of columns in lines may be specific to a database format. Plus, some additional columns may have been added by the calculation (e.g: Ei and S for emission integral and linestrength in SpectrumFactory). Refer to the code to know what they mean (and their units)

references (dict) – a dict of doi of references used to compute this object. Automatically returned with the full bibtex entry by cite() It can also be set a posteriori. Example

s = Spectrum()
s.references = {"10.1016/j.jqsrt.2010.05.001": "HITEMP-2010 database",
              "10.1016/j.jqsrt.2018.09.027":["calculation", "post-processing"],  # RADIS main paper. Automatically added
              "10.1016/j.jqsrt.2020.107476":"DIT algorithm"}
              )
s.cite()

Returns :

Used for DIT algorithm
----------------------
@article{van_den_Bekerom_2021,
    doi = {10.1016/j.jqsrt.2020.107476},
    url = {https://doi.org/10.1016%2Fj.jqsrt.2020.107476},
    year = 2021,
    month = {mar},
    publisher = {Elsevier {BV}},
    volume = {261},
    pages = {107476},
    author = {D.C.M. van den Bekerom and E. Pannier},
    title = {A discrete integral transform for rapid spectral synthesis},
    journal = {Journal of Quantitative Spectroscopy and Radiative Transfer}
}

Used for HITEMP-2010 database
-----------------------------
@article{Rothman_2010,
    doi = {10.1016/j.jqsrt.2010.05.001},
    url = {https://doi.org/10.1016%2Fj.jqsrt.2010.05.001},
    year = 2010,
    month = {oct},
    publisher = {Elsevier {BV}},
    volume = {111},
    number = {15},
    pages = {2139--2150},
    author = {L.S. Rothman and I.E. Gordon and R.J. Barber and H. Dothe and R.R. Gamache and A. Goldman and V.I. Perevalov and S.A. Tashkun and J. Tennyson},
    title = {{HITEMP}, the high-temperature molecular spectroscopic database},
    journal = {Journal of Quantitative Spectroscopy and Radiative Transfer}
}

Used for calculation, post-processing
-------------------------------------
@article{Pannier_2019,
    doi = {10.1016/j.jqsrt.2018.09.027},
    url = {https://doi.org/10.1016%2Fj.jqsrt.2018.09.027},
    year = 2019,
    month = {jan},
    publisher = {Elsevier {BV}},
    volume = {222-223},
    pages = {12--25},
    author = {Erwan Pannier and Christophe O. Laux},
    title = {{RADIS}: A nonequilibrium line-by-line radiative code for {CO}2 and {HITRAN}-like database species},
    journal = {Journal of Quantitative Spectroscopy and Radiative Transfer}
}

</details>

warnings (boolean) – if True, test if inputs are valid, e.g, spectra are evenly distributed in wavelength, and raise a warning if not. Note that this take ~ 3.5 ms for a 20k points spectrum, when the rest of the creation process is only ~ 1.8ms (makes it 3 times longer, and can be a problem if hundreds of spectra are created in a row). Default True

Examples

Manipulate a Spectrum calculated by RADIS:

s = calc_spectrum(2125, 2300, Tgas=2000, databank='CDSD')
s.print_conditions()
s.plot('absorbance')
s.line_survey(overlay='absorbance')
s.plot('radiance_noslit', wunits='cm-1', Iunits='W/m2/sr/cm-1')
s.apply_slit(5)
s.plot('radiance')
w, t = s.get('transmittance_noslit')  # for use in multi-slabs configs

Any tuple of numpy arrays (w, I) can also be converted into a Spectrum object from the Spectrum class directly, or using the calculated_spectrum() function. All the following methods are equivalent:

from radis import Spectrum, calculated_spectrum
s1 = calculated_spectrum(w, I, wunit='nm', Iunit='mW/cm2/sr/nm')
s2 = Spectrum.from_array(w, I, 'radiance_noslit',
                       wunit='nm', unit='mW/cm2/sr/nm')
s3 = Spectrum({'radiance_noslit': (w, I)},
              units={'radiance_noslit':'mW/cm2/sr/nm'},
              wunit='nm')

See more examples in the [Spectrum] page.

Spectrum objects can be stored, retrieved, rescaled, resampled:

from radis import load_spec
s = load_spec('co_calculation.spec')
s.rescale_path_length(0.5)                  # calculate for new path_length
s.rescale_mole_fraction(0.02)   # calculate for new mole fraction
s.resample(w_new)               # resample on new wavespace
s.store('co_calculation2.spec')

Notes

Implementation:

quantities are stored in the self._q dictionary. They are better accessed with the get() method that deals with units and wavespace

Wavebase:

quantites are stored either in wavenum or wavelength base, but this doesnt matter as they are retrieved / plotted with the get() and plot() methods which have units as input arguments

conditions[source]¶

Stores computation / measurement conditions

Type: dict

c[source]¶

convenience wrapper to conditions:

s.c["calculation_time"] is s.conditions["calculation_time"]
>> True

Type: dict

populations[source]¶

Stores molecules, isotopes, electronic states and vibrational or rovibrational populations

Type: dict

References

Spectrum: See the Spectrum object page

apply_slit(slit_function, unit='nm', shape: ['triangular', 'trapezoidal', 'gaussian'] = 'triangular', center_wavespace=None, norm_by='area', mode='valid', plot_slit=False, store=True, slit_dispersion=None, slit_dispersion_threshold=0.01, auto_recenter_crop=True, assert_evenly_spaced=True, verbose=True, inplace=True, *args, **kwargs)[source]¶

Apply an instrumental slit function to all quantities in Spectrum. Slit function can be generated with usual shapes (see shape=) or imported from an experimental slit function (path to a text file or numpy array of shape n*2). Convoluted spectra are cut on the edge compared to non-convoluted spectra, to remove side effects. See mode= to change this behaviour.

Warning with units: read about 'unit' and 'return_unit' parameters.

Parameters

slit_function (float or str or array) –

If float:
generate slit function with FWHM of slit function (in nm or cm-1 depending on unit=). A (top, base) tuple of (float, float) is required when asking for a trapezoidal slit function.

If .txt:
import experimental slit function from .txt file: format must be 2-columns with wavelengths and intensity (doesn’t have to be normalized)

If array:
format must be 2-columns with wavelengths and intensity (doesn’t have to be normalized) It is recommended to truncate the input slit function to its minimum useful spectral extension (see Notes of convolve_with_slit()).
unit ('nm' or 'cm-1') – unit of slit_function (FWHM, or imported file)
shape ('triangular', 'trapezoidal', 'gaussian', or any of SLIT_SHAPES) –

which shape to use when generating a slit. Will call,
respectively, triangular_slit(), trapezoidal_slit(), gaussian_slit(). Default ‘triangular’
center_wavespace (float, or None) – center of slit when generated (in unit). Not used if slit is imported.
norm_by ('area', 'max') – normalisation type: - 'area' normalizes the slit function to an area

of 1. It conserves energy, and keeps the same units.
- 'max' normalizes the slit function to a maximum of 1. The convoluted spectrum units change (they are multiplied by the spectrum waveunit, e.g: a radiance non convoluted in mW/cm2/sr/nm on a wavelength (nm). range will yield a convoluted radiance in mW/cm2/sr. Note that the slit is set to 1 in the Spectrum wavespace (i.e: a Spectrum calculated in cm-1 will have a slit set to 1 in cm-1).
Default 'area'
mode ('valid', 'same') –

'same' returns output of same length as initial spectra,
but boundary effects are still visible. 'valid' returns output of length len(spectra) - len(slit) + 1, for which lines outside of the calculated range have no impact. Default 'valid'.

Other Parameters

assert_evenly_spaced (boolean, or 'resample') – for the convolution to be accurate, w should be evenly spaced. If assert_evenly_spaced=True, then we check this is the case, and raise an error if arrays is not evenly spaced. If 'resample', then we resample w and I if needed. Recommended, but it takes some time.
auto_recenter_crop (bool) – if True, recenter slit and crop zeros on the side when importing an experimental slit. Default True. See recenter_slit(), crop_slit()
plot_slit (boolean) – if True, plot slit
store (boolean) – if True, store slit in the Spectrum object so it can be retrieved with get_slit() and plot with plot_slit(). Default True
slit_dispersion (func of (lambda, in 'nm'), or None) – spectrometer reciprocal function : dÎ»/dx(Î») (in nm) If not None, then the slit_dispersion function is used to correct the slit function for the whole range. Can be important if slit function was measured far from the measured spectrum (e.g: a slit function measured at 632.8 nm will look broader at 350 nm because the spectrometer dispersion is higher at 350 nm. Therefore it should be corrected) Default None

Warning

slit dispersion function is assumed to be given in nm if your spectrum is stored in cm-1 the wavenumbers are converted to wavelengths before being forwarded to the dispersion function

See test_auto_correct_dispersion() for an example of the slit dispersion effect.

A Python implementation of the slit dispersion:
```
>>> def f(lbd):
>>>    return  w/(2*f)*(tan(Î¦)+sqrt((2*d/m/(w*1e-9)*cos(Î¦))^2-1))
```
Theoretical / References:
```
>>> dÎ»/dx ~ d/mf    # at first order
>>> dÎ»/dx = w/(2*f)*(tan(Î¦)+sqrt((2*d/m/(w)*cos(Î¦))^2-1))  # cf
```
with:
- Î¦: spectrometer angle (Â°)
- f: focal length (mm)
- m: order of dispersion
- d: grooves spacing (mm) = 1/gr with gr in (gr/mm)
See Laux 1999 “Experimental study and modeling of infrared air plasma radiation” for more information
slit_dispersion_warning_threshold (float) – if not None, check that slit dispersion is about constant (< threshold change) on the calculated range. Default 0.01 (1%). See offset_dilate_slit_function()
inplace (bool) – if True, adds convolved arrays directly in the Spectrum. If False, returns a new Spectrum with only the convolved arrays. Note: if you want a new Spectrum with both the convolved and non convolved quantities, use
```
s.copy().apply_slit()
```
*args, **kwargs – are forwarded to slit generation or import function
verbose (bool) – print stuff
energy_threshold (float) – tolerance fraction when resampling. Default 1e-3 (0.1%) If areas before and after resampling differ by more than that an error is raised.

Returns

Spectrum – Allows chaining. If inplace=False, return a new Spectrum with the new spectral arrays only.

Return type

same Spectrum, with new spectral arrays.

Notes

Units:

the slit function is first converted to the wavespace (wavelength/wavenumber) that the Spectrum is stored in, and applied to the spectral quantities in their native wavespace.

Implementation:

convolve_with_slit() is applied to all quantities in get_vars() that ends with _noslit. Generate a triangular instrumental slit function (or any other shape depending of shape=) with base slit_function_base (Uses the central wavelength of the spectrum for the slit function generation)

We deal with several special cases (which makes the code a little heavy, but the method very versatile):

when slit unit and spectrum unit arent the same
when spectrum is not evenly spaced

Examples

s.apply_slit(1.2, 'nm')

This applies the instrumental function to all available spectral arrays. To manually apply the slit to a particular spectral array, use take()

s.take('transmittance_noslit').apply_slit(1.2, 'nm')

See convolve_with_slit() for more details on Units and Normalization

The slit is made considering the “center wavelength” which is the mean wavelength of the full spectrum you are applying it to.

Line Survey

GPU Accelerated Spectra

Calculate non-LTE spectra of carbon-monoxide

Calculate a spectrum from ExoMol

c[source]¶

cite(format='bibentry')[source]¶

Prints bibliographic references used to compute this spectrum, as stored in the references dictionary. Default references known to RADIS are listed in radis.db.references.doi.

Parameters: format (default 'bibentry'. See more in habanero.content_negotiation())

Examples

from radis import calc_spectrum
s = calc_spectrum(
    1900,
    2300,  # cm-1
    molecule="CO",
    isotope="1,2,3",
    pressure=1.01325,  # bar
    Tvib=2000,  #
    Trot=300,
    mole_fraction=0.1,
    path_length=1,  # cm
    databank="hitran",
)
s.cite()

Returns :

Used for algorithm
------------------
@article{van_den_Bekerom_2021,
    doi = {10.1016/j.jqsrt.2020.107476},
    url = {https://doi.org/10.1016%2Fj.jqsrt.2020.107476},
    year = 2021,
    month = {mar},
    publisher = {Elsevier {BV}},
    volume = {261},
    pages = {107476},
    author = {D.C.M. van den Bekerom and E. Pannier},
    title = {A discrete integral transform for rapid spectral synthesis},
    journal = {Journal of Quantitative Spectroscopy and Radiative Transfer}
}

Used for calculation, rovibrational energies
--------------------------------------------
@article{Pannier_2019,
    doi = {10.1016/j.jqsrt.2018.09.027},
    url = {https://doi.org/10.1016%2Fj.jqsrt.2018.09.027},
    year = 2019,
    month = {jan},
    publisher = {Elsevier {BV}},
    volume = {222-223},
    pages = {12--25},
    author = {Erwan Pannier and Christophe O. Laux},
    title = {{RADIS}: A nonequilibrium line-by-line radiative code for {CO}2 and {HITRAN}-like database species},
    journal = {Journal of Quantitative Spectroscopy and Radiative Transfer}
}

Used for data retrieval
-----------------------
@article{Ginsburg_2019,
    doi = {10.3847/1538-3881/aafc33},
    url = {https://doi.org/10.3847%2F1538-3881%2Faafc33},
    year = 2019,
    month = {feb},
    publisher = {American Astronomical Society},
    volume = {157},
    number = {3},
    pages = {98},
    author = {Adam Ginsburg and Brigitta M. Sip{\H{o}}cz and C. E. Brasseur and Philip S. Cowperthwaite and Matthew W. Craig and Christoph Deil and James Guillochon and Giannina Guzman and Simon Liedtke and Pey Lian Lim and Kelly E. Lockhart and Michael Mommert and Brett M. Morris and Henrik Norman and Madhura Parikh and Magnus V. Persson and Thomas P. Robitaille and Juan-Carlos Segovia and Leo P. Singer and Erik J. Tollerud and Miguel de Val-Borro and Ivan Valtchanov and Julien Woillez and},
    title = {astroquery: An Astronomical Web-querying Package in Python},
    journal = {The Astronomical Journal}
}

Used for line database
----------------------
@article{Gordon_2017,
    doi = {10.1016/j.jqsrt.2017.06.038},
    url = {https://doi.org/10.1016%2Fj.jqsrt.2017.06.038},
    year = 2017,
    month = {dec},
    publisher = {Elsevier {BV}},
    volume = {203},
    pages = {3--69},
    author = {I.E. Gordon and L.S. Rothman and C. Hill and R.V. Kochanov and Y. Tan and P.F. Bernath and M. Birk and V. Boudon and A. Campargue and K.V. Chance and B.J. Drouin and J.-M. Flaud and R.R. Gamache and J.T. Hodges and D. Jacquemart and V.I. Perevalov and A. Perrin and K.P. Shine and M.-A.H. Smith and J. Tennyson and G.C. Toon and H. Tran and V.G. Tyuterev and A. Barbe and A.G. Cs{\'{a}}sz{\'{a}}r and V.M. Devi and T. Furtenbacher and J.J. Harrison and J.-M. Hartmann and A. Jolly and T.J. Johnson and T. Karman and I. Kleiner and A.A. Kyuberis and J. Loos and O.M. Lyulin and S.T. Massie and S.N. Mikhailenko and N. Moazzen-Ahmadi and H.S.P. Müller and O.V. Naumenko and A.V. Nikitin and O.L. Polyansky and M. Rey and M. Rotger and S.W. Sharpe and K. Sung and E. Starikova and S.A. Tashkun and J. Vander Auwera and G. Wagner and J. Wilzewski and P. Wcis{\l}o and S. Yu and E.J. Zak},
    title = {The {HITRAN}2016 molecular spectroscopic database},
    journal = {Journal of Quantitative Spectroscopy and Radiative Transfer}
}

Used for partition function
---------------------------
@article{Gamache_2021,
    doi = {10.1016/j.jqsrt.2021.107713},
    url = {https://doi.org/10.1016%2Fj.jqsrt.2021.107713},
    year = 2021,
    month = {sep},
    publisher = {Elsevier {BV}},
    volume = {271},
    pages = {107713},
    author = {Robert R. Gamache and Bastien Vispoel and Michaël Rey and Andrei Nikitin and Vladimir Tyuterev and Oleg Egorov and Iouli E. Gordon and Vincent Boudon},
    title = {Total internal partition sums for the {HITRAN}2020 database},
    journal = {Journal of Quantitative Spectroscopy and Radiative Transfer}
}
@article{Kochanov_2016,
    doi = {10.1016/j.jqsrt.2016.03.005},
    url = {https://doi.org/10.1016%2Fj.jqsrt.2016.03.005},
    year = 2016,
    month = {jul},
    publisher = {Elsevier {BV}},
    volume = {177},
    pages = {15--30},
    author = {R.V. Kochanov and I.E. Gordon and L.S. Rothman and P. Wcis{\l}o and C. Hill and J.S. Wilzewski},
    title = {{HITRAN} Application Programming Interface ({HAPI}): A comprehensive approach to working with spectroscopic data},
    journal = {Journal of Quantitative Spectroscopy and Radiative Transfer}
}

Used for spectroscopic constants
--------------------------------
@article{Guelachvili_1983,
    doi = {10.1016/0022-2852(83)90203-5},
    url = {https://doi.org/10.1016%2F0022-2852%2883%2990203-5},
    year = 1983,
    month = {mar},
    publisher = {Elsevier {BV}},
    volume = {98},
    number = {1},
    pages = {64--79},
    author = {G. Guelachvili and D. de Villeneuve and R. Farrenq and W. Urban and J. Verges},
    title = {Dunham coefficients for seven isotopic species of {CO}},
    journal = {Journal of Molecular Spectroscopy}
}

Cite all references used

See also

RefTracker, doi

compare_with(other, spectra_only=False, plot=True, wunit='default', verbose=True, rtol=1e-05, ignore_nan=False, ignore_outliers=False, normalize=False, **kwargs)[source]¶

Compare Spectrum with another Spectrum object.

Parameters

other (type Spectrum) – another Spectrum to compare with
spectra_only (boolean, or str) – if True, only compares spectral quantities (in the same waveunit) and not lines or conditions. If str, compare a particular quantity name. If False, compare everything (including lines and conditions and populations). Default False
plot (boolean) – if True, use plot_diff to plot all quantities for the 2 spectra and the difference between them. Default True.
wunit ("nm", "cm-1", "default") – in which wavespace to compare (and plot). If "default", natural wavespace of first Spectrum is taken.
rtol (float) – relative difference to use for spectral quantities comparison
ignore_nan (boolean) – if True, nans are ignored when comparing spectral quantities
ignore_outliers (boolean, or float) –

if not False, outliers are discarded. i.e, output is determined by:
```
out = (~np.isclose(I, Ie, rtol=rtol, atol=0)).sum()/len(I) < ignore_outliers
```
normalize (bool) – Normalize the spectra to be ploted

Other Parameters

kwargs (dict) – arguments are forwarded to plot_diff()

Returns

equals – return True if spectra are equal (respective to tolerance defined by rtol and other input conditions)

Return type

boolean

Examples

Compare two Spectrum objects, or specifically the transmittance:

s1.compare_with(s2)
s1.compare_with(s2, 'transmittance')

Note that you can also simply use s1 == s2, that uses compare_with() internally:

s1 == s2       # will return True or False

See also

compare_spectra()

cond_units[source]¶

conditions[source]¶

computation conditions, or experimetnal parameters, or any metadata you need to store with the Spectrum object.

Type: dict

copy(copy_lines=True, quantity='all', copy_arrays=True)[source]¶

Returns a copy of this Spectrum object (performs a smart deepcopy)

Parameters

copy_lines (bool) – default True
quantity (‘all’, or one of ‘radiance_noslit’, ‘absorbance’, etc.) – if not ‘all’, copy only one quantity. Default 'all'
copy_arrays (bool) – if False, returned array’s quantity is a pointer to the original Spectrum. Faster, but warning, changing them will then change the original Spectrum. Default True

Examples

crop(wmin=None, wmax=None, wunit='default', inplace=True)[source]¶

Crop spectrum to wmin-wmax range in wunit (inplace)

Parameters

wmin, wmax (float, or None) – boundaries of spectral range (in wunit)
wunit ('nm', 'cm-1', 'nm_vac') – which waveunit to use for wmin, wmax. If default: use the default Spectrum wavespace defined with get_waveunit().

Other Parameters

inplace (bool) – if True, modifies the Spectrum object directly. Else, returns a copy. Default True.

Returns

s – Cropped Spectrum. If inplace=True, Spectrum has been updated directly anyway. Allows chaining

Return type

Spectrum

Examples

Crop to experimental Spectrum, and compare:

from radis import calc_spectrum, load_spec, plot_diff
s = calc_spectrum(...)
s_exp = load_spec('typical_result.spec')
s.crop(s_exp.get_wavelength.min(), s_exp.get_wavelength.max(), 'nm')
plot_diff(s_exp, s)

Load an experimental spectrum

See also

radis.spectrum.operations.crop()

MergeSlabs(): if used with ``resample=’full’,

out, this, to

file[source]¶

classmethod from_array(w, I, quantity, wunit=None, Iunit=None, waveunit=None, unit=None, *args, **kwargs)[source]¶

Construct Spectrum from 2 arrays.

Parameters

w, I (array) – waverange and vector
quantity (str) – spectral quantity name
wunit ('nm', 'cm-1', 'nm_vac') – unit of waverange: wavelength in air ('nm' or 'nm_air'), wavenumber ('cm-1'), or wavelength in vacuum ('nm_vac'). If None, then w must be a dimensionned array.
Iunit (str) – spectral quantity unit (arbitrary). Ex: 'mW/cm2/sr/nm' for radiance_noslit If None, then I must be a dimensionned array.
*args, **kwargs – see Spectrum doc

Other Parameters

conditions (dict) – physical conditions and calculation parameters
cond_units (dict) – units for conditions
populations (dict) – a dictionary of all species, and levels. Should be compatible with other radiative codes such as Specair output. Suggested format: {molecules: {isotopes: {elec state: rovib levels}}} e.g:
```
{'CO2':{1: 'X': df}}   # with df a Pandas Dataframe
```
lines (pandas Dataframe) – all lines in databank (necessary for using line_survey()). Warning if you want to play with the lines content: The signification of columns in lines may be specific to a database format. Plus, some additional columns may have been added by the calculation (e.g: Ei and S for emission integral and linestrength in SpectrumFactory). Refer to the code to know what they mean (and their units)

Returns

creates a Spectrum object

Return type

Spectrum

Examples

Create a spectrum:

from radis import Spectrum
s = Spectrum.from_array(w, I, 'radiance_noslit',
                       wunit='nm', unit='mW/cm2/sr/nm')

Dimensionned arrays can also be used directly

import astropy.units as u
w = np.linspace(200, 300) * u.nm
I = np.random.rand(len(w)) * u.mW/u.cm**2/u.sr/u.nm
s = Spectrum.from_array(w, I, 'radiance_noslit')

To create a spectrum with absorption and emission components (e.g: radiance_noslit and transmittance_noslit, or emisscoeff and abscoeff) call the Spectrum class directly. Ex:

from radis import Spectrum
s = Spectrum({'abscoeff': (w, A), 'emisscoeff': (w, E)},
             units={'abscoeff': 'cm-1', 'emisscoeff':'W/cm2/sr/nm'},
             wunit='nm')

classmethod from_hdf5(file, wmin=None, wmax=None, wunit=None, columns=None, engine='pytables')[source]¶

Generates a Spectrum from an HDF5 file. Uses hdf2spec()

Other Parameters

wmin, wmax (float) – range of wmin, wmax to load , using wunit (if None, load everything)
columns (list of str) – spectral arrays to load (if None, load everything)

Examples

Spectrum.from_hdf5("rad_hdf.h5", wmin=2100, wmax=2200, columns=['abscoeff', 'emisscoeff'])

See also

to_hdf5()

classmethod from_spec(file)[source]¶: Generates a Spectrum from a .spec [json] file. Uses load_spec()

classmethod from_specutils(spectrum, var='radiance')[source]¶

Convert a specutils specutils.spectra.spectrum1d.Spectrum1D to a radis Spectrum object.

Parameters

spectrum (a specutils specutils.spectra.spectrum1d.Spectrum1D)
var (str) – spectral array, default "radiance"

Examples

Taken from the Specutils website (https://specutils.readthedocs.io/en/stable/#getting-started-with-specutils)

from astropy.io import fits
from astropy import units as u
from specutils import Spectrum1D

f = fits.open('https://data.sdss.org/sas/dr16/sdss/spectro/redux/26/spectra/1323/spec-1323-52797-0012.fits')
# The spectrum is in the second HDU of this file.
specdata = f[1].data

lamb = 10**specdata['loglam'] * u.AA
flux = specdata['flux'] * 10**-17 * u.Unit('erg cm-2 s-1 AA-1')
spec = Spectrum1D(spectral_axis=lamb, flux=flux)

from radis import Spectrum
s = Spectrum.from_specutils(spec)
s.plot(wunit='nm')

See also

to_specutils()

classmethod from_txt(file, quantity, wunit, unit, waveunit=None, *args, **kwargs)[source]¶

Construct Spectrum from txt file.

Parameters

file (str) – file name
quantity (str) – spectral quantity name
wunit ('nm', 'cm-1', 'nm_vac') – unit of waverange: wavelength in air ('nm'), wavenumber ('cm-1'), or wavelength in vacuum ('nm_vac').
unit (str) – spectral quantity unit
*args, **kwargs – the following inputs are forwarded to loadtxt: 'delimiter', 'skiprows' The rest if forwarded to Spectrum. see Spectrum doc

Other Parameters

delimiter (',', etc.) – see numpy.loadtxt()
skiprows (int) – see numpy.loadtxt()
argsort (bool) – sorts the arrays in file by wavespace. Convenient way to load a file where points have been manually added at the end. Default False.
*Optional Spectrum parameters*
conditions (dict) – physical conditions and calculation parameters
cond_units (dict) – units for conditions
populations (dict) – a dictionary of all species, and levels. Should be compatible with other radiative codes such as Specair output. Suggested format: {molecules: {isotopes: {elec state: rovib levels}}} e.g:
```
{'CO2':{1: 'X': df}}   # with df a Pandas Dataframe
```
lines (pandas Dataframe) – all lines in databank (necessary for using line_survey()). Warning if you want to play with the lines content: The signification of columns in lines may be specific to a database format. Plus, some additional columns may have been added by the calculation (e.g: Ei and S for emission integral and linestrength in SpectrumFactory). Refer to the code to know what they mean (and their units)

Returns

s – creates a Spectrum object

Return type

Spectrum

Examples

Generate an experimental spectrum from txt. In that example the delimiter key is forwarded to loadtxt():

from radis import Spectrum
s = Spectrum.from_txt('spectrum.csv', 'radiance', wunit='nm',
                          unit='W/cm2/sr/nm', delimiter=',')

To create a spectrum with absorption and emission components (e.g: radiance_noslit and transmittance_noslit, or emisscoeff and abscoeff) call the Spectrum class directly. Ex:

from radis import Spectrum
s = Spectrum({'abscoeff': (w, A), 'emisscoeff': (w, E)},
             units={'abscoeff': 'cm-1', 'emisscoeff':'W/cm2/sr/nm'},
             wunit='nm')

Notes

Internally, the numpy loadtxt() function is used and transposed:

w, I = np.loadtxt(file).T

You can use 'delimiter' and ‘skiprows' as arguments.

generate_perf_profile()[source]¶

Generate a visual/interactive performance profile diagram using tuna

Examples

s = calc_spectrum(...)
s.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

See also

print_perf_profile()

get(var: ['radiance'], wunit='default', Iunit='default', copy=True, trim_nan=False, return_units=False)[source]¶

Retrieve a spectral quantity from a Spectrum object. You can select wavespace unit, intensity unit, or propagation medium.

Parameters

var (variable ('absorbance', 'transmittance', 'xsection' etc.)) – Should be a defined quantity among CONVOLUTED_QUANTITIES or NON_CONVOLUTED_QUANTITIES. To get the full list of spectral arrays defined in this Spectrum object use the get_vars() method.
wunit ('nm', 'cm', 'nm_vac'.) – wavespace unit: wavelength in air ('nm'), wavenumber ('cm-1'), or wavelength in vacuum ('nm_vac'). if "default", default unit for waveunit is used. See get_waveunit().
Iunit (unit for variable var) – if "default", default unit for quantity var is used. See the units attribute. For var="radiance", one can use per wavelength (~ ‘W/m2/sr/nm’) or per wavenumber (~ ‘W/m2/sr/cm-1’) units

Note

if using default, the returned unit may be different from Spectrum.units[var]. e.g, for a Spectrum with radiance stored in ‘mW/cm2/sr/nm’, getting it with wunit='cm-1', Iunit='default' will return Iunit in ‘mW/cm2/sr/cm-1’ for consistency. Use return_units to be sure about which units are used.

Other Parameters

copy (bool) – if True, returns a copy of the stored quantity (modifying it wont change the Spectrum object). Default True.
trim_nan (bool) – if True, removes nan on the sides of the spectral array (and corresponding wavespace). Default False.
return_units (bool) – if True, return dimensioned Astropy arrays. Is using return_units = 'as_str', return wunit and Iunit as extra variables, i.e, w, I, wunit, Iunit = s.get(..., return_units='as_str') Default False

Returns

w, I – wavespace, quantity (ex: wavelength, radiance_noslit). For numpy users, note that these are copies (values) of the Spectrum quantity and not a view (reference): if you modify them the Spectrum is not changed

Return type

array-like

Examples

Get transmittance in cm-1:

w, I = s.get('transmittance_noslit', wunit='cm-1')

Get radiance (in wavelength in air):

_, R = s.get('radiance_noslit', wunit='nm', Iunit='W/cm2/sr/nm')

Use with return_units to get dimensioned Astropy Quantities

w, R  = s.get('radiance_noslit', return_units=True)

get_baseline(algorithm='als', **kwargs)[source]¶

Calculate and returns a baseline

Parameters

s (Spectrum) – Spectrum which needs a baseline
var (str) – on which spectral quantity to read the baseline. Default 'radiance'. See SPECTRAL_QUANTITIES
algorithm (‘als’, ‘polynomial’) – Asymmetric least square or Polynomial fit
**kwargs (dict) – additional parameters to send to the algorithm. By default, for ‘polynomial’:

**kwargs = **{“deg”: 1, “max_it”:500}

for ‘als’:

**kwargs = {“asymmetry_param”: 0.05,
“smoothness_param”: 1e6}

Returns

baseline – Spectrum object where intenisity is the baseline of s

Return type

Spectrum

Examples

See also

get_baseline()

get_conditions()[source]¶: Get all physical / computational parameters.

See also

print_conditions(), the Spectrum page

get_integral(var, wunit='default', Iunit='default', **kwargs)[source]¶

Returns integral of variable ‘var’ over waverange.

Parameters

var (str) – spectral quantity to integate
wunit (str) – over which waverange to integrated. If default, use the default Spectrum wavespace defined with get_waveunit().
Iunit (str) – default 'default'

Warning

this is the unit of the quantity, not the unit of the integral. Don’t forget to multiply by wunit

Other Parameters

kwargs (**dict) – forwarded to get()

Returns

integral – integral in [Iunit]*[wunit]

Return type

float

See also

get_power(), the Spectrum page

get_name()[source]¶

Return Spectrum name.

If not defined, returns either the file name if Spectrum was loaded from a file, or the 'spectrum{id}' with the Python id object

get_populations(molecule=None, isotope=None, electronic_state=None, show_warning=True)[source]¶

Return populations that are featured in the spectrum, either as upper or lower levels.

Parameters

molecule (str, or None) – if None, only one molecule must be defined. Else, an error is raised
isotope (int, or None) – isotope number. if None, only one isotope must be defined. Else, an error is raised
electronic_state (str) – if None, only one electronic state must be defined. Else, an error is raised
show_warning (bool) – if False, turns off warning about meaning of populations, see Notes and discussion on https://github.com/radis/radis/issues/508.

Returns

pandas dataframe of levels, where levels are the index,
and ‘Evib’ and ‘nvib’ are featured

Notes

Structure:

{molecule: {isotope: {electronic_state: {'vib': pandas Dataframe,    # (copy of) vib levels
                                         'rovib': pandas Dataframe,  # (copy of) rovib levels
                                         'Ia': float    # isotopic abundance
                                         }}}}

(If Spectrum generated with RADIS, structure should match that of SpectrumFactory.get_populations())

Examples

An example on how different are populations used for partition function and spectrum calculations

#%% CO2 example
# For instance, plot populations of a given vibrational level, v1,v2,v3=(0,1,0)
import radis
s = radis.test_spectrum(molecule="CO2", Tvib=3000, Trot=1000,
                        export_lines=True,
                        export_populations="rovib",
                        isotope=1)
pops = s.get_populations("CO2")["rovib"]

import matplotlib.pyplot as plt
pops.query("v1==0 & v2==1 & v3==0").plot("j", "n",
                                         label="pops. used to compute partition functions")
s.lines.query("v1l==0 & v2l==1 & v3l==0").plot("jl", "nl", ax=plt.gca(), kind="scatter", color="r",
                                               label="pops. of visible absorbing lines")
plt.legend()
plt.xlim((0,70))

See populations of computed levels

See also

plot_populations(), line_survey()

get_power(unit='mW/cm2/sr')[source]¶

Returns integrated radiance (no slit) power density.

Parameters: Iunit (str) – power unit.
Returns: P – radiated power in unit
Return type: float

Examples

s.get_power('W/cm2/sr')

See also

get_integral(), the Spectrum page

get_quantities(which=None)[source]¶: Returns all spectral quantities stored in this object (convoluted or non convoluted). Wrapper to get_vars()

get_radiance(Iunit='mW/cm2/sr/nm', copy=True)[source]¶

Return radiance in whatever unit, and can even convert from ~1/nm to ~1/cm-1 (and the other way round)

Other Parameters: copy (boolean) – if True, returns a copy of the stored waverange (modifying it wont change the Spectrum object). Default True.

get_radiance_noslit(Iunit='mW/cm2/sr/nm', copy=True)[source]¶

Return radiance (non convoluted) in whatever unit, and can even convert from ~1/nm to ~1/cm-1 (and the other way round)

Other Parameters: copy (boolean) – if True, returns a copy of the stored waverange (modifying it wont change the Spectrum object). Default True.

get_rovib_levels(molecule=None, isotope=None, electronic_state=None, first=None)[source]¶

Return rovibrational levels calculated in the spectrum (energies, populations)

Parameters

molecule (str, or None) – if None, only one molecule must be defined. Else, an error is raised
isotope (int, or None) – isotope number. if None, only one isotope must be defined. Else, an error is raised
electronic_state (str) – if None, only one electronic state must be defined. Else, an error is raised
first (int, or ‘all’ or None) – only show the first N levels. If None or ‘all’, all levels are shown

Returns

out – pandas dataframe of levels, where levels are the index, and ‘Evib’ and ‘nvib’ are featured

Return type

pandas DataFrame

get_slit(wunit='same')[source]¶

Get slit function that was applied to the Spectrum.

Returns: wslit, Islit – slit function with wslit in Spectrum waveunit. See get_waveunit()
Return type: array

get_vars(which=None)[source]¶: Returns all spectral quantities stored in this object (convoluted or non convoluted)

get_vib_levels(molecule=None, isotope=None, electronic_state=None, first=None)[source]¶

Return vibrational levels in the spectrum (energies, populations)

Parameters

molecule (str, or None) – if None, only one molecule must be defined. Else, an error is raised
isotope (int, or None) – isotope number. if None, only one isotope must be defined. Else, an error is raised
electronic_state (str) – if None, only one electronic state must be defined. Else, an error is raised
first (int, or ‘all’ or None) – only show the first N levels. If None or ‘all’, all levels are shown

Returns

out – pandas dataframe of levels, where levels are the index, and ‘Evib’ and ‘nvib’ are featured

Return type

pandas DataFrame

get_wavelength(medium='air', which=None, copy=True)[source]¶

Return wavelength in defined medium.

Parameters: medium ('air', 'vacuum') – returns wavelength as seen in air, or vacuum. Default 'air'. See vacuum2air(), air2vacuum()
Other Parameters: copy (boolean) – if True, returns a copy of the stored waverange (modifying it wont change the Spectrum object). Default True.
Returns: w – (a copy of) spectrum wavelength for convoluted or non convoluted quantities
Return type: array_like

See also

the Spectrum page

get_wavenumber(which=None, copy=True)[source]¶

Return wavenumber (if the same for all quantities)

Other Parameters: copy (boolean) – if True, returns a copy of the stored waverange (modifying it wont change the Spectrum object). Default True.
Returns: w – (a copy of) spectrum wavenumber for convoluted or non convoluted quantities
Return type: array_like

get_waveunit()[source]¶: Returns whether this spectrum is defined in wavelength (nm) or wavenumber (cm-1)

has_nan(ignore_wavespace=True) → bool[source]¶

Parameters: s (Spectrum) – radis Spectrum.
Returns: b – returns whether Spectrum has nan
Return type: bool

Note

print(s) will also show which spectral quantities have ````nan.

is_at_equilibrium(check='warn', verbose=False)[source]¶

Returns whether this spectrum is at (thermal) equilibrium. Reads the thermal_equilibrium key in Spectrum conditions. It does not imply chemical equilibrium (mole fractions are still arbitrary)

If they are defined, also check that the following assertions are True:

Tvib = Trot = Tgas self_absorption = True overpopulation = None

If they are not, still trust the value in Spectrum conditions, but raise a warning.

Other Parameters

check ('warn', 'error', 'ignore') – what to do if Spectrum conditions dont match the given equilibrium state: raise a warning, raise an error, or just ignore and dont even check. Default 'warn'.
verbose (bool) – if True, print why is the spectrum is not at equilibrium, if applicable.

is_optically_thin()[source]¶

Returns whether the spectrum is optically thin, based on the value on the self_absorption key in conditions.

If not given, raises an error

line_survey(overlay=None, wunit='cm-1', Iunit='hitran', medium='air', cutoff=None, plot='S', lineinfo=['int', 'A', 'El'], barwidth='hwhm_voigt', yscale='log', writefile=None, *args, **kwargs)[source]¶

Plot Line Survey (all linestrengths used for calculation) Output in: Plotly (html)

Parameters

overlay (tuple (w, I, [name], [units]), or list or tuples) – plot (w, I) on a secondary axis. Useful to compare linestrength with calculated / measured data:
```
LineSurvey(overlay='abscoeff')
```
wunit ('nm', 'cm-1') – wavelength / wavenumber units
Iunit ('hitran', 'splot') – Linestrength output units:
- 'hitran': (cm-1/(molecule/cm-2))
- 'splot' : (cm-1/atm) (Spectraplot units 2)
Note: if not None, cutoff criteria is applied in this unit. Not used if plot is not ‘S’
medium ('air', 'vacuum') – show wavelength either in air or vacuum. Default 'air'
plot (str) – what to plot. Default 'S' (scaled line intensity). But it can be any key in the lines, such as population ('nu'), or Einstein coefficient ('Aul')
lineinfo (list, or 'all') – extra line information to plot. Should be a column name in the databank (s.lines). For instance: 'int', 'selbrd', etc… Default ['int']

Other Parameters

writefile (str) – if not None, a valid filename to save the plot under .html format.
If None, use the fig object returned to show the plot.
- yscale ('log', 'linear') – Default 'log'
- barwidth (float or str) –
  
  if float, width of bars, in wunit, as a fraction of full-range; i.e.
  barwidth=0.01
  makes bars span 1% of the full range. if str, uses the column as width. Example
  barwidth = 'hwhm_voigt'
  returns
  
  fig (a Plotly figure.) – If using a Jupyter Notebook, the plot will appear. Else, use writefile to export to an html file.
  
  Plot in Plotly. See Output in [1]_

An example using the SpectrumFactory to generate a spectrum:

from radis import SpectrumFactory
sf = SpectrumFactory(
                     wavenum_min=2380,
                     wavenum_max=2400,
                     mole_fraction=400e-6,
                     path_length=100,  # cm
                     isotope=[1],
                     export_lines=True,    # required for LineSurvey!
                     db_use_cached=True)
sf.load_databank('HITRAN-CO2-TEST')
s = sf.eq_spectrum(Tgas=1500)
s.apply_slit(0.5)
s.line_survey(overlay='radiance_noslit', barwidth=0.01, lineinfo="all")  # or barwidth='hwhm_voigt'

See the output in Examples

Line Survey

See populations of computed levels

1: RADIS Online Documentation (LineSurvey)
2: SpectraPlot

LineSurvey(), the Spectrum page

lines[source]¶

informations on emitting or absorbing lines that contribute to the spectrum.

plot(var: ['radiance'] = None, wunit='default', Iunit='default', show_points=False, nfig=None, yscale='linear', show_medium='vacuum_only', normalize=False, force=False, plot_by_parts=False, show=False, show_ruler=False, **kwargs)[source]¶

Plot a Spectrum object.

Note

default plotting library and templates can be edited in radis.config [“plot”]

Parameters

var (variable (absorbance, transmittance, transmittance_noslit, xsection, etc.)) – For full list see get_vars(). If None, plot the first thing in the Spectrum. Default None.
wunit ('default', 'nm', 'cm-1', 'nm_vac',) – wavelength air, wavenumber, or wavelength vacuum. If 'default', Spectrum get_waveunit() is used.
Iunit (unit for variable) – if default, default unit for quantity var is used. for radiance, one can use per wavelength (~ W/m2/sr/nm) or per wavenumber (~ W/m2/sr/cm-1) units

Other Parameters

show_points (boolean) – show calculated points. Default True.
nfig (int, None, or ‘same’) – plot on a particular figure. ‘same’ plots on current figure. For instance:
```
s1.plot()
s2.plot(nfig='same')
```
show_medium (bool, 'vacuum_only') – if True and wunit are wavelengths, plot the propagation medium in the xaxis label ([air] or [vacuum]). If 'vacuum_only', plot only if wunit=='nm_vac'. Default 'vacuum_only' (prevents from inadvertently plotting spectra with different propagation medium on the same graph).
yscale (‘linear’, ‘log’) – plot yscale
normalize (boolean, or tuple.) – option to normalize quantity to 1 (ex: for radiance). Default False
plot_by_parts (bool) – if True, look for discontinuities in the wavespace and plot the different parts without connecting lines. Useful for experimental spectra produced by overlapping step-and-glue. Additional parameters read from kwargs : split_threshold and cutwings. See more in split_and_plot_by_parts().
force (bool) – plotting on an existing figure is forbidden if labels are not the same. Use force=True to ignore that.
show (bool) – show figure. Default False. Will still show the figure in interactive mode, e.g, %matplotlib inline in a Notebook.
show_ruler (bool) – if True, add a ruler tool to the Matplotlib toolbar. Convenient to measure distances between peaks, etc.

Warning

still experimental in 0.9.30 ! Try it, feedback welcome !
**kwargs (**dict) – kwargs forwarded as argument to plot (e.g: lineshape attributes: lw=3, color='r')

Returns

line plot

Return type

line

Examples

Plot an experimental_spectrum() in arbitrary units:

s = experimental_spectrum(..., Iunit='mW/cm2/sr/nm')
s.plot(Iunit='W/cm2/sr/cm-1')

See more examples in the plot Spectral quantities page.

Load an experimental spectrum

Remove a baseline

GPU Accelerated Spectra

Calculate non-LTE spectra of carbon-monoxide

Use different plot themes

Calculate a large spectrum by part

Calculate a spectrum from ExoMol

Post-process using Specutils

See also

plot_diff(), the Spectrum page

plot_populations(what=None, nunit='', correct_for_abundance=False, **kwargs)[source]¶

Plots vib populations if given and format is valid.

Parameters

what (‘vib’, ‘rovib’, None) – if None plot everything
nunit (‘’, ‘cm-3’) – plot either in a fraction of vibrational levels, or a molecule number in in cm-3
correct_for_abundance (boolean) – if True, multiplies each population by the isotopic abundance (as it is done during the calculation of emission integral)
kwargs (**dict) – are forwarded to the plot

Examples

See populations of computed levels

See also

get_populations(), line_survey()

plot_slit(wunit=None, waveunit=None)[source]¶

Plot slit function that was applied to the Spectrum.

If dispersion was used (see apply_slit()) the different slits are built again and plotted too (dotted).

Parameters

wunit ('nm', 'cm-1', or None) – plot slit in wavelength or wavenumber. If None, use the unit the slit in which the slit function was given. Default None

Returns

fix, ax (matplotlib objects) – figure and ax
.. minigallery:: radis.spectrum.spectrum.Spectrum.plot_slit

See also

the Spectrum page

populations[source]¶

populations of rovibrational levels used to compute partition functions of the spectrum

print_conditions(**kwargs)[source]¶

Prints all physical / computational parameters.

Parameters: kwargs (dict) – refer to print_conditions()

Examples

::: s.print_conditions()

You can also simply print the Spectrum object directly:

print(s)

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

Prints Profiler output dictionary in a structured manner.

Example

Spectrum.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_LDM_lineshapes        0.012s
            LDM_Initialized_vectors          0.000s
            LDM_closest_matching_line        0.001s
            LDM_Distribute_lines             0.001s
            LDM_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.

See also

generate_perf_profile()

references[source]¶

resample(w_new, unit='same', out_of_bounds='nan', energy_threshold='default', print_conservation=False, inplace=True, if_conflict_drop=None, **kwargs)[source]¶

Resample spectrum over a new wavelength/wavenumber range.

Warning

This may result in information loss. Resampling is done with oversampling and spline interpolation. These parameters can be adjusted, and energy conservation ensured with the appropriate parameters.

To minimize information loss, always resample the high-resolution spectrum over the low-resolution spectrum, i.e.

s_highres.resample(s_lowres)

Fills with 'nan' or transparent medium (transmittance 1, radiance 0) when out of bound (see out_of_bounds)

Parameters

w_new (array, or Spectrum) – new wavespace to resample the spectrum on. Must be inclosed in the current wavespace (we won’t extrapolate) One can also give a Spectrum directly:
```
s1.resample(s2.get_wavenumber())
s1.resample(s2)            # also valid
```
unit ('same', 'nm', 'cm-1', 'nm_vac') – unit of new wavespace. It 'same' it is assumed to be the current waveunit. Default 'same'. The spectrum waveunit is changed to this unit after resampling (i.e: a spectrum calculated and stored in cm-1 but resampled in nm will be stored in nm from now on). If 'nm', wavelength in air. If 'nm_vac', wavelength in vacuum.
out_of_bounds ('transparent', 'nan', 'error') – what to do if resampling is out of bounds. 'transparent': fills with transparent medium. ‘nan’: fill with nan. 'error': raises an error. Default 'nan'
medium ('air', 'vacuum', or 'default') – in which medium is the new waverange is calculated if it is given in ‘nm’. Ignored if unit=’cm-1’

Other Parameters

energy_threshold (float or None or 'default') -- if energy conservation (integrals on the intersecting range) is above this threshold, raise an error. If ``None, dont check for energy conservation. If 'default', look up the value in radis.config [“RESAMPLING_TOLERANCE_THRESHOLD”] Default 'default'
print_conservation (boolean) – if True, prints energy conservation. Default False.
inplace (boolean) – if True, modifies the Spectrum object directly. Else, returns a copy. Default True.
**kwargs (**dict) – all other arguments are sent to radis.misc.signal.resample()

Returns

Spectrum – object has been modified anyway.

Return type

resampled Spectrum object. If using inplace=True, the Spectrum

Examples

Convert a Spectrum in wavenumber to wavelengths:

s_nm = s.resample(s.get_wavelength(), "nm", inplace=False)

resample_even(energy_threshold=0.005, print_conservation=False, inplace=True)[source]¶

Resample spectrum over the same waverange, but evenly spaced.

Warning

This may result in information loss. Resampling is done with oversampling and spline interpolation. These parameters can be adjusted, and energy conservation ensured with the appropriate parameters.

Parameters

energy_threshold (float or None) – if energy conservation (integrals on the intersecting range) is above this threshold, raise an error. If None, dont check for energy conservation Default 5e-3 (0.5%)
print_conservation (boolean) – if True, prints energy conservation. Default False.
inplace (boolean) – if True, modifies the Spectrum object directly. Else, returns a copy. Default True.
**kwargs (**dict) – all other arguments are sent to radis.misc.signal.resample()

Returns

Spectrum – object has been modified anyway.

Return type

resampled Spectrum object. If using inplace=True, the Spectrum

Examples

rescale_mole_fraction(new_mole_fraction, old_mole_fraction=None, inplace=True, ignore_warnings=False, force=False, verbose=True)[source]¶

Update spectrum with new molar fraction Convoluted values (with slit) are dropped in the process.

Parameters

new_mole_fraction (float) – new mole fraction
old_mole_fraction (float, or None) – if None, current mole fraction (conditions[‘mole_fraction’]) is used

Other Parameters

inplace (boolean) – if True, modifies the Spectrum object directly. Else, returns a copy. Default True.
force (boolean) – if False, won’t allow rescaling to 0 (not to loose information). Default False

Returns

s – Cropped Spectrum. If inplace=True, Spectrum has been updated directly anyway. Allows chaining

Return type

Spectrum

Examples

s.rescale_mole_fraction(0.2)

Notes

Implementation:

similar to rescale_path_length() but we have to scale abscoeff & emisscoeff Note that this is valid only for small changes in mole fractions. Then, the change in line broadening becomes significant

See also

the Spectrum page

rescale_path_length(new_path_length, old_path_length=None, inplace=True, force=False)[source]¶

Rescale spectrum to new path length. Starts from absorption coefficient and emission coefficient, and solves the RTE again for the new path length Convoluted values (with slit) are dropped in the process.

Parameters

new_path_length (float) – new path length
old_path_length (float, or None) – if None, current path length (conditions[‘path_length’]) is used

Other Parameters

inplace (boolean) – if True, modifies the Spectrum object directly. Else, returns a copy. Default True.
force (boolean) – if False, won’t allow rescaling to 0 (not to loose information). Default False

Returns

s – Cropped Spectrum. If inplace=True, Spectrum has been updated directly anyway. Allows chaining

Return type

Spectrum

Examples

for path in [0.1, 10, 100]:
    s.rescale_path_length(10, inplace=False).plot(nfig='same')

Additionally, you can also use astropy units in the input arguments, for example:

# preparing a test spectrum :
import radis
s = radis.test_spectrum()

# rescaling :
import astropy.units as u
s.rescale_path_length(1 * u.km).plot()

Notes

Implementation:

To deal with all the input cases, we first make a list of what has to be recomputed, and what has to be recalculated

See also

the Spectrum page

save(*args, **kwargs)[source]¶

Alias to Spectrum.store.

See Spectrum.store for documentation

savetxt(filename, var, wunit='default', Iunit='default')[source]¶

Export spectral quantity var to filename.

(note that by doing this you will loose additional information, such: as the calculation conditions or the units. You better save a Spectrum object under a .spec file with store() and load it afterwards with load_spec())

Parameters

filename (str) – file name
var (str) – which spectral variable ot export

Other Parameters

wunit, Iunit, medium (str) – see get() for more information

Notes

Export variable as:

np.savetxt(filename, np.vstack(self.get(var, wunit=wunit, Iunit=Iunit,
                                    medium=medium)).T, header=header)

See also

store(), save(), the Spectrum page

sort(inplace=True)[source]¶

Sort the Spectrum by wavelength / wavenumber.

Parameters: inplace (bool, optional) – if True, modifies the Spectrum object directly. The default is True.
Returns: s – sorted Spectrum. If inplace=True, Spectrum has been updated directly anyway. Allows chaining.
Return type: Spectrum

Examples

store(path, discard=['lines', 'populations'], compress=True, add_info=None, add_date=None, if_exists_then='error', verbose=True)[source]¶

Save a Spectrum object in JSON format. Object can be recovered with load_spec(). If many Spectrum are saved in a same folder you can view their properties with the SpecDatabase structure.

Parameters

path (path to folder (database) or file) – if a folder, file is saved to database and name is generated automatically. if a file name, then Spectrum is saved to this file and the later formatting options dont apply
file (str) – explicitely give a filename to save
compress (boolean) – if False, save under text format, readable with any editor. if True, saves under binary format. Faster and takes less space. If 2, removes all quantities that can be regenerated with s.update(), e.g, transmittance if abscoeff and path length are given, radiance if emisscoeff and abscoeff are given in non-optically thin case, etc. Default True.
add_info (list) – append these parameters and their values if they are in conditions example:
```
add_info = ['Tvib', 'Trot']
```
discard (list of str) – parameters to exclude, for instance to save some memory for instance Default [lines, populations]: retrieved Spectrum looses the line_survey() ability, and plot_populations() (but it saves tons of memory!)
if_exists_then ('increment', 'replace', 'error', 'ignore') – what to do if file already exists. If increment an incremental digit is added. If replace file is replaced (yeah). If 'ignore' no file is created. If error (or anything else) an error is raised. Default error

Return type

Returns filename used

Notes

If many spectra are stored in a folder, it may be time to set up a SpecDatabase structure to easily see all Spectrum conditions and get Spectrum that suits specific parameters.

Examples

Store a spectrum in compressed mode, regenerate quantities after loading:

from radis import load_spec
s.store('test.spec', compress=True)   # s is a Spectrum
s2 = load_spec('test.spec')
s2.update()                           # regenerate missing quantities

take(var, copy_lines=False, copy_arrays=True)[source]¶

Parameters

var (str) – spectral quantity ('absorbance', 'transmittance', 'xsection' etc.)

Other Parameters

copy_lines (bool) – if True, export s.lines. Default False
copy_arrays (bool) – if False, returned array’s quantity is a pointer to the original Spectrum. Faster, but warning, changing them will then change the original Spectrum. Default True

Returns

s – same Spectrum with only the var spectral quantity

Return type

Spectrum

Examples

Use take to chain other commands

s.take('radiance').normalize().plot()

to_hdf5(file, engine='pytables')[source]¶

Stores the Spectrum under HDF5 format. Uses spec2hdf()

Examples

s.to_hdf5('spec01.h5')

See also

from_hdf5()

to_json(*args, **kwargs)[source]¶

Alias to Spectrum.store(compress=False).

See Spectrum. store() for documentation

to_pandas(copy=True)[source]¶

Convert a Spectrum to a Pandas DataFrame

Returns: pd.DataFrame – units are stored in attributes df.attrs
Return type: pandas DataFrame where columns are spectral arrays, and

Notes

Pandas does not support units yet. pint-pandas is an advanced project but not fully working. See discussion in https://github.com/pandas-dev/pandas/issues/10349

For the moment, we store units as metadata

to_specutils(var=None, wunit='default', Iunit='default')[source]¶

Convert a radis Spectrum object to specutils specutils.spectra.spectrum1d.Spectrum1D

Parameters

var (‘radiance’, ‘radiance_noslit’, etc.) – which spectral array to convert. If None and only one spectral arry is defined, use it.
wunit ('nm', 'cm', 'nm_vac'.) – wavespace unit: wavelength in air ('nm'), wavenumber ('cm-1'), or wavelength in vacuum ('nm_vac'). if "default", default unit for waveunit is used. See get_waveunit().

Note

specutils handles wavelengths in vacuum only. If using 'nm' wavelengths will be converted to wavelengths in vacuum. We recommend using 'nm_air' or 'nm_vac' to avoid any confusion.
Iunit (unit for variable var) – if "default", default unit for quantity var is used. See the units attribute. For var="radiance", one can use per wavelength (~ ‘W/m2/sr/nm’) or per wavenumber (~ ‘W/m2/sr/cm-1’) units
.. note:: – nan, that may have been added on the wings of the spectra if a slit has been applied, are removed using trim_nan parameter of get() . The waverange in the 1DSpectrum object may therefore be cropped.

Examples

spectrum = s.to_specutils()

Add uncertainties by reading a spectrum noise region with SpectralRegion and noise_region_uncertainty()

from specutils import SpectralRegion
from specutils.manipulation import noise_region_uncertainty
noise_region = SpectralRegion(2012 / u.cm, 2009 / u.cm)
spectrum = noise_region_uncertainty(spectrum, noise_region)

Find lines out of the noise using find_lines_threshold()

from specutils.fitting import find_lines_threshold
lines = find_lines_threshold(spectrum)

Post-process using Specutils

See also

from_specutils()

trim(inplace=True)[source]¶

Remove nan common to all arrays on each side of the Spectrum.

Returns a smaller Spectrum (inplace or not).

Returns: s – directly anyway. Allows chaining.
Return type: Spectrum : trimmed Spectrum. If inplace=True, Spectrum has been updated

units[source]¶

units for spectral quantities.

Type: dict

update(quantity='all', optically_thin='default', verbose=True)[source]¶

Calculate missing quantities: ex: if path_length and emisscoeff are given, recalculate radiance_noslit.

Parameters

spec (Spectrum)
quantity (str) – name of the spectral quantity to recompute. If ‘same’, only the quantities in the Spectrum are recomputed. If ‘all’, then all quantities that can be derived are recomputed. Default ‘all’.
optically_thin (True, False, or ‘default’) – determines whether to calculate radiance with or without self absorption. If ‘default’, the value is determined from the self_absorption key in Spectrum.conditions. If not given, False is taken. Default ‘default’ Also updates the self_absorption value in conditions (creates it if doesnt exist

Examples

Initialize a spectrum from the absorption coefficient, retrieve the transmittance or the emission coefficient :

s = Spectrum.from_array([1900.  , 1900.01, 1900.02, 1900.03, 1900.04, 1900.05, 1900.06,
                         1900.07, 1900.08, 1900.09],
                        [2.71414065e-06, 2.88341489e-06, 3.06942277e-06, 3.27445689e-06,
                         3.50121831e-06, 3.75290756e-06, 4.03334037e-06, 4.34709612e-06,
                         4.69971017e-06, 5.09792551e-06],
                        'abscoeff',
                        wunit='cm-1',
                        Iunit='cm-1',
                        conditions={'path_length':1, # cm
                                    'thermal_equilibrium':True,
                                    'Tgas':700,  # K
                                    })
s.update('transmittance_noslit')
s.update('emisscoeff')

See also

the Spectrum page

Transmittance(s: Spectrum) → Spectrum[source]¶

Returns a new Spectrum with only the transmittance component of s

Parameters: s (Spectrum) – Spectrum object
Returns: s_tr – Spectrum object, with only the transmittance, absorbance and/or abscoeff part of s, where radiance_noslit , emisscoeff and emissivity_noslit (if they exist) have been set to 0
Return type: Spectrum

Examples

This function is useful to use Spectrum algebra operations:

s = calc_spectrum(...)   # contains emission & absorption arrays
tr = Transmittance(s)    # contains 'radiance_noslit' array only
tr -= 0.1    # arithmetic operation is applied to Transmittance only

Equivalent to:

rad = s.take('transmittance')

Transmittance_noslit(s: Spectrum) → Spectrum[source]¶

Returns a new Spectrum with only the transmittance_noslit component of s

Parameters: s (Spectrum) – Spectrum object
Returns: s_tr – Spectrum object, with only transmittance_noslit defined
Return type: Spectrum

Examples

This function is useful to use Spectrum algebra operations:

s = calc_spectrum(...)   # contains emission & absorption arrays
tr = Transmittance_noslit(s) # contains 'radiance_noslit' array only
tr -= 0.1    # arithmetic operation is applied to Transmittance_noslit only

Equivalent to:

rad = s.take('transmittance_noslit')

calculated_spectrum(w, I, wunit='nm', Iunit='mW/cm2/sr/nm', conditions=None, cond_units=None, populations=None, name=None) → Spectrum[source]¶

Convert (w, I) into a Spectrum object that has unit conversion, plotting and slit convolution capabilities.

Parameters

w (np.array) – wavelength, or wavenumber
I (np.array) – intensity (no slit)
wunit ('nm', 'cm-1', 'nm_vac') – wavespace unit: wavelength in air ('nm'), wavenumber ('cm-1'), or wavelength in vacuum ('nm_vac'). Default 'nm'.
Iunit (str) – intensity unit (can be ‘counts’, ‘mW/cm2/sr/nm’, etc…). Default ‘mW/cm2/sr/nm’ (note that non-convoluted Specair spectra are in ‘mW/cm2/sr/µm’)

Other Parameters

conditions (dict) – (optional) calculation conditions to be stored with Spectrum. Default None
cond_units (dict) – (optional) calculation conditions units. Default None
populations (dict) – populations to be stored in Spectrum. Default None
name (str) – (optional) give a name

Examples

# w, I are numpy arrays for wavelength and radiance
from radis import calculated_spectrum
s = calculated_spectrum(w, I, wunit='nm', Iunit='W/cm2/sr/nm')     # creates 'radiance_noslit'

experimental_spectrum(w, I, wunit='nm', Iunit='count', conditions={}, cond_units=None, name=None) → Spectrum[source]¶

Convert (w, I) into a Spectrum object that has unit conversion and plotting capabilities. Convolution is not available as the spectrum is assumed to have be measured experimentally (hence it is already convolved with the slit function)

Parameters

w (np.array) – wavelength, or wavenumber
I (np.array) – intensity
wunit ('nm', 'cm-1', 'nm_vac') – wavespace unit: wavelength in air ('nm'), wavenumber ('cm-1'), or wavelength in vacuum ('nm_vac'). Default 'nm'.
Iunit (str) – intensity unit (can be 'count', ‘mW/cm2/sr/nm’, etc…). Default 'count' (i.e., non calibrated output)

Other Parameters

conditions (dict) – (optional) calculation conditions to be stored with Spectrum
cond_units (dict) – (optional) calculation conditions units
name (str) – (optional) give a name

Examples

Load and plot an experimental spectrum:

from numpy import loadtxt
from radis import experimental_spectrum
w, I = loadtxt('my_file.txt').T    # transpose is often useful, depending on your data.
s = experimental_spectrum(w, I, Iunit='mW/cm2/sr/nm')             # creates 'radiance'
s.plot()

get_diff(s1: Spectrum, s2: Spectrum, var, wunit='default', Iunit='default', resample=True, diff_window=0)[source]¶

Get the difference between 2 spectra.

Basically returns w1, I1 - I2 where (w1, I1) and (w2, I2) are the values of s1 and s2 for variable var. (w2, I2) is linearly interpolated if needed.

\[dI = I_1 - I_2\]

Parameters

s1, s2 (Spectrum objects) – 2 spectra to compare.
var (str) – spectral quantity (ex: 'radiance', 'transmittance'…)
wunit ('nm', 'cm-1', 'nm_vac') – waveunit to compare in: wavelength air, wavenumber, wavelength vacuum
Iunit (str) – if 'default' use s1 unit for variable var
medium (‘air’, ‘vacuum’, default’) – propagating medium to compare in (if in wavelength)

Other Parameters

resample (bool) – if not True, wavelength must be equals. Else, resample s2 on s1 if needed.
diff_window (int) – If non 0, calculates diff by offsetting s1 by diff_window number of units on either side, and returns the minimum. Compensates for experimental errors on the w axis. Default 0. (look up code for more details…)

Returns

w1, Idiff – difference interpolated on the wavespace range of the first Spectrum

Return type

array

Notes

Uses curve_substract() internally

get_distance(s1: Spectrum, s2: Spectrum, var, wunit='default', Iunit='default', resample=True)[source]¶

Get a regularized Euclidian distance between two spectra s1 and s2

This regularized Euclidian distance minimizes the effect of a small shift in wavelength between the two spectra

\[D(w_1)[i] = \sqrt{ \sum_j (\hat{I_1}[i] - \hat{I_2}[j] )^2 + (\hat{w_1}[i] - \hat{w_2}[j])^2}\]

Where values are normalized as:

\[\hat{A} = \frac{A}{max(A) - min(A)}\]

If waveranges dont match, s2 is interpolated over s1.

Warning

This is a distance on both the waverange and the intensity axis. It may be used to compensate for a small offset in your experimental spectrum (due to wavelength calibration, for instance) but can lead to wrong fits easily. Plus, it is very cost-intensive! Better use get_residual() for an automatized procedure.

Parameters

s1, s2 (Spectrum objects) – Spectrum
var (str) – spectral quantity
wunit ('nm', 'cm-1', 'nm_vac') – waveunit to compare in: wavelength air, wavenumber, wavelength vacuum
Iunit (str) – if 'default' use s1 unit for variable var
medium (‘air’, ‘vacuum’, default’) – propagating medium to compare in (if in wavelength)

Notes

Uses curve_distance() internally

get_ratio(s1: Spectrum, s2: Spectrum, var, wunit='default', Iunit='default', resample=True)[source]¶

Get the ratio between two spectra Basically returns w1, I1 / I2 where (w1, I1) and (w2, I2) are the values of s1 and s2 for variable var. (w2, I2) is linearly interpolated if needed.

\[R = I_1 / I_2\]

Parameters

s1, s2 (Spectrum objects) – Spectrum
var (str) – spectral quantity
wunit ('nm', 'cm-1', 'nm_vac') – waveunit to compare in: wavelength air, wavenumber, wavelength vacuum
Iunit (str) – if 'default' use s1 unit for variable var

Notes

Uses curve_divide() internally

get_residual(s1: Spectrum, s2: Spectrum, var, norm='L2', ignore_nan=False, diff_window=0, normalize=False, normalize_how='max', wunit='default', Iunit='default') → float[source]¶

Returns L2 norm of s1 and s2

For I1, I2, the values of variable var in s1 and s2, respectively, residual is calculated as:

For L2 norm:

\[res = \frac{\sqrt{\sum_i {(s_1[i]-s_2[i])^2}}}{N}.\]

For L1 norm:

\[res = \frac{\sqrt{\sum_i {|s_1[i]-s_2[i]|}}}{N}.\]

Parameters

s1, s2 (Spectrum objects) – if not on the same range, s2 is resampled on s1.
var (str) – spectral array
norm (‘L2’, ‘L1’) – which norm to use

Other Parameters

ignore_nan (boolean) – if True, ignore nan in the difference between s1 and s2 (ex: out of bound) when calculating residual. Default False. Note: get_residual will still fail if there are nan in initial Spectrum.
normalize (bool, or tuple) – if True, normalize the two spectra before calculating the residual. If a tuple (ex: (4168, 4180)), normalize on this range only. The unit is that of the first Spectrum by default (use wunit to change). Ex:
```
s_exp   # in 'nm'
s_calc  # in 'cm-1'
get_residual(s_exp, s_calc, normalize=(4178, 4180))  # interpreted as 'nm'
```
normalize_how ('max', 'area', 'mean') – how to normalize. 'max' is the default but may not be suited for very noisy experimental spectra. 'area' will normalize the integral to 1. 'mean' will normalize by the mean amplitude value
wunit (str) – used if normalized is a range. If 'default', use first spectrum unit.
Iunit (str) – if 'default', use first spectrum unit

Notes

0 values for I1 yield nans except if I2 = I1 = 0

when s1 and s2 dont have the size wavespace range, they are automatically resampled through get_diff on ‘s1’ range

Implementation of L2 norm:

np.sqrt((dI**2).sum())/len(dI)

Implementation of L1 norm:

np.abs(dI).sum()/len(dI)

get_residual_integral()[source]¶

Returns integral of the difference between two spectra s1 and s2, relatively to the integral of spectrum s1.

Compared to get_residual(), this tends to cancel the effect of the gaussian noise of an experimental spectrum.

res = trapz(I2-I1, w1) / trapz(I1, w1)

Note: when the considered variable is transmittance or transmittance_noslit, the upper integral is used (up to 1) to normalize the integral difference

res = trapz(I2-I1, w1) / trapz(1-I1, w1)

Parameters

s1, s2 (Spectrum objects) – Spectrum
var (str) – spectral quantity

Other Parameters

ignore_nan (boolean) – if True, ignore nan in the difference between s1 and s2 (ex: out of bound) when calculating residual. Default False. Note: get_residual_integral will still fail if there are nan in initial Spectrum.
wunit (str) – If 'default', use first spectrum unit.
Iunit (str) – if 'default', use first spectrum unit

Notes

For I1, I2, the values of ‘var’ in s1 and s2, respectively, residual is calculated as:

res = trapz(I2-I1, w1) / trapz(I1, w1)

0 values for I1 yield nans except if I2 = I1 = 0

when s1 and s2 dont have the size wavespace range, they are automatically resampled through get_diff on ‘s1’ range

plot_diff(s1: Spectrum, s2: Spectrum, var=None, wunit='default', Iunit='default', resample=True, method='diff', diff_window=0, show_points=False, label1=None, label2=None, figsize=None, title=None, nfig=None, normalize=False, yscale='linear', verbose=True, save=False, show=True, show_residual=False, lw_multiplier=1, diff_scale_multiplier=1, discard_centile=0, plot_medium='vacuum_only', legendargs={'loc': 'best'}, show_ruler=False)[source]¶

Plot two spectra, and the difference between them. method= allows you to plot the absolute difference, ratio, or both.

If waveranges dont match, s2 is interpolated over s1.

Parameters

s1, s2 (Spectrum objects)
var (str, or None) – spectral quantity to plot (ex: 'abscoeff'). If None, plot the first one in the Spectrum from 'radiance', 'radiance_noslit', 'transmittance', etc.
wunit ('default', 'nm', 'cm-1', 'nm_vac') – wavespace unit: wavelength air, wavenumber, wavelength vacuum. If 'default', use first spectrum wunit
Iunit (str) – if 'default', use first spectrum unit
method ('distance', 'diff', 'ratio', or list of them.) – If 'diff', plot difference of the two spectra. If 'distance', plot Euclidian distance (note that units are meaningless then) If 'ratio', plot ratio of two spectra Default 'diff'.

Warning

with 'distance', calculation scales as ~N^2 with N the number of points in a spectrum (against ~N with 'diff'). This can quickly override all memory.

Can also be a list:
```
method=['diff', 'ratio']
```
normalize (bool) – Normalize the spectra to be ploted

Other Parameters

plot yscale

yscale: ‘linear’, ‘log diff_window: int

If non 0, calculates diff by offsetting s1 by diff_window number of units on either side, and returns the minimum. Kinda compensates for experimental errors on the w axis. Default 0. (look up code to understand…)

show_points: boolean

if True, make all points appear with ‘o’

label1, label2: str

curve names

figsize

figure size

nfig: int, str

figure number of name

title: str

title

verbose: boolean

if True, plot stuff such as rescale ratio in normalize mode. Default True

save: str

Default is False. By default won’t save anything, type the path of the destination if you want to save it (format in the name).

show: Bool

Default is True. Will show the plots : bad if there are more than 20.

show_residual: bool

if True, calculates and shows on the graph the residual in L2 norm. See get_residual(). diff_window is used in the residual calculation too. normalize has no effect.

diff_scale_multiplier: float

dilate the diff plot scale. Default 1

discard_centile: int

if not 0, discard the firsts and lasts centile when setting the limits of the diff window. Example:

discard_centile=1     #  --> discards the smallest 1% and largest 1%
discard_centile=10    #  --> discards the smallest 10% and largest 10%

Useful to remove spikes in a ratio, for instance. Note that this does not change the values of the residual. It’s just a plot feature. Default 0

plot_medium: bool, 'vacuum_only'

if True and wunit are wavelengths, plot the propagation medium in the xaxis label ([air] or [vacuum]). If 'vacuum_only', plot only if wunit=='nm_vac'. Default 'vacuum_only' (prevents from inadvertently plotting spectra with different propagation medium on the same graph).

legendargs: dict

format arguments forwarded to the legend

show_ruler: bool

if True, add a ruler tool to the Matplotlib toolbar.

Warning

still experimental in 0.9.30 ! Try it, feedback welcome !

Returns

fig (figure) – fig
[ax0, ax1] (axes) – spectra and difference axis

Examples

Simple use:

from radis import plot_diff
plot_diff(s10, s50)                # s10, s50 are two spectra

Advanced use, plotting the total power in the label, and getting the figure and axes handle to edit them afterwards:

Punit = 'mW/cm2/sr'
fig, axes = plot_diff(s10, s50, 'radiance_noslit', figsize=(18,6),
      label1='brd 10 cm-1, P={0:.2f} {1}'.format(s10.get_power(unit=Punit),Punit),
      label2='brd 50 cm-1, P={0:.2f} {1}'.format(s50.get_power(unit=Punit),Punit)
      )
# modify fig, axes..

See an example in Compare two Spectra, which produces the output below:

https://radis.readthedocs.io/en/latest/_images/cdsd4000_vs_hitemp_3409K.svg

If you wish to plot in a logscale, it can be done in the following way:

fig, [ax0, ax1] = plot_diff(s0, s1, normalize=False, verbose=False)
ylim0 = ax0.get_ybound()
ax0.set_yscale("log")
ax0.set_ybound(ylim0)

Compare CO spectrum from the GEISA and HITRAN database

Calculate a spectrum from HITEMP

Compare CO xsections from the ExoMol and HITEMP database

transmittance_spectrum(w, T, wunit='nm', Tunit='', conditions=None, cond_units=None, name=None) → Spectrum[source]¶

Convert (w, I) into a Spectrum object that has unit conversion, plotting and slit convolution capabilities.

Parameters

w (np.array) – wavelength, or wavenumber
T (np.array) – transmittance (no slit)
wunit ('nm', 'cm-1', 'nm_vac') – wavespace unit: wavelength in air ('nm'), wavenumber ('cm-1'), or wavelength in vacuum ('nm_vac'). Default 'nm'.
Iunit (str) – intensity unit. Default "" (adimensionned)

Other Parameters

conditions (dict) – (optional) calculation conditions to be stored with Spectrum
cond_units (dict) – (optional) calculation conditions units
name (str) – (optional) give a name

Examples

# w, T are numpy arrays for wavelength and transmittance
from radis import transmittance_spectrum
s2 = transmittance_spectrum(w, T, wunit='nm')                       # creates 'transmittance_noslit'

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radis.spectrum package¶

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