Specutils Documentation

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The specutils package provides a basic interface for the loading, manipulation, and common forms of analysis of spectroscopic data. These generic data containers and accompanying modules will provide a toolbox that the astronomical community can use to build more domain-specific packages. For more details about the underlying principles, see APE13, the guiding document for spectroscopic development in the Astropy Project.

Note

While specutils is available for general use, the API is in an early enough development stage that some interfaces may change if user feedback and experience warrants it.

Getting started with specutils

As a basic example, consider an emission line galaxy spectrum from the SDSS. We will use this as a proxy for a spectrum you may have downloaded from some archive, or reduced from your own observations.

We begin with some basic imports:

>>> from astropy.io import fits
>>> from astropy import units as u
>>> import numpy as np
>>> from matplotlib import pyplot as plt
>>> from astropy.visualization import quantity_support
>>> quantity_support()  # for getting units on the axes below  # doctest: +IGNORE_OUTPUT

Now we load the dataset from it’s canonical source:

>>> f = fits.open('https://dr14.sdss.org/optical/spectrum/view/data/format=fits/spec=lite?plateid=1323&mjd=52797&fiberid=12')  # doctest: +IGNORE_OUTPUT +REMOTE_DATA
>>> # The spectrum is in the second HDU of this file.
>>> specdata = f[1].data # doctest: +REMOTE_DATA
>>> f.close() # doctest: +REMOTE_DATA

Then we re-format this dataset into astropy quantities, and create a Spectrum1D object:

>>> from specutils import Spectrum1D
>>> lamb = 10**specdata['loglam'] * u.AA # doctest: +REMOTE_DATA
>>> flux = specdata['flux'] * 10**-17 * u.Unit('erg cm-2 s-1 AA-1') # doctest: +REMOTE_DATA
>>> spec = Spectrum1D(spectral_axis=lamb, flux=flux) # doctest: +REMOTE_DATA

And we plot it:

>>> lines = plt.step(spec.spectral_axis, spec.flux) # doctest: +REMOTE_DATA

(Source code)

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Now maybe you want the equivalent width of a spectral line. That requires normalizing by a continuum estimate:

>>> from specutils.fitting import fit_generic_continuum
>>> cont_norm_spec = spec / fit_generic_continuum(spec)(spec.spectral_axis) # doctest: +REMOTE_DATA
>>> lines = plt.step(cont_norm_spec.wavelength, cont_norm_spec.flux) # doctest: +REMOTE_DATA
>>> plt.xlim(654*u.nm, 660*u.nm)  # doctest: +IGNORE_OUTPUT +REMOTE_DATA

(Source code)

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But then you can apply a single function over the region of the spectrum containing the line:

>>> from specutils import SpectralRegion
>>> from specutils.analysis import equivalent_width
>>> equivalent_width(cont_norm_spec, regions=SpectralRegion(6562*u.AA, 6575*u.AA)) 
<Quantity -14.78092438 Angstrom>

While there are other tools and spectral representations detailed more below, this gives a test of the sort of analysis specutils enables.