<p>A spectrum of, say, a star or a galaxy, consists of wavelengths emitted from various physical processes. In the case of the star, there is the blackbody spectrum that reflects the temperature of all of its gas, whether it is hydrogen, helium, or metals. On top of this, there are <em>lines</em>, i.e. emission from certain atomic transitions that are excited and then de-excite emitting photons in a very narrow wavelength interval. The blackbody spectrum is said to comprise the continuum of the total spectrum.</p>

<p>In the case of galaxies, the continuum consists of the combined spectrum of many different stars' different blackbody spectra, infrared light from dust, etc. On top of this, there are lines, e.g. from nebular processes such as my favorite line Lyman $\alpha$, which is emitted when hard UV radiation from hot O and B stars ionize their surrounding neutral hydrogen, which subsequently recombines emitting mostly Lyman $\alpha$.</p>

<p>If we want to measure the total flux in a given line, we are usually only interested in the flux that comes from a particular physical process, and not the part of the flux that comes from the "underlying" sources which contribute to the continuum. Hence, we need to <em>subtract the continuum</em>. This is usually done by fitting some functional form to the continuum (e.g. a straight line or a second order polynomial), substract this fit from the spectrum, and finally integrate from one side of the line to the other in the resulting "continuum-subtracted spectrum".</p>

<p>In the top figure below, the total spectrum's flux density$^\dagger$ is in black, and the fit is the red lines. Underneath is drawn the continuum-subtracted spectrum, and a few dashed green lines show some lines that rise above the continuum. The integrated line flux is indicated by light red.</p>

<p><a href="https://i.sstatic.net/z04nX.png" rel="nofollow noreferrer"><img src="https://i.sstatic.net/z04nX.png" alt="specs"></a></p>

<p>$^\dagger$<sub>Note that many authors use the term "flux" where it should actually be "flux density". Integrating flux <em>density</em> in $\mathrm{erg}\,\mathrm{s}^{-1}\,\mathrm{cm}^{-2}\,\mathrm{Å}^{-1}$ over wavelength in Å$^{-1}$ gives <em>flux</em> in $\mathrm{erg}\,\mathrm{s}^{-1}\,\mathrm{cm}^{-2}$.</sub></p>

CC BY-SA 3.0
2015-10-05T11:51:35.333Z
2015-10-05T15:08:52.557Z
2015-10-05T15:08:52.557Z
pela
<p>What is the exact definition of a "continuum-subtracted spectrum", such that one finds in SDSS spectra? </p>

<p><a href="http://classic.sdss.org/dr7/dm/flatFiles/spSpec.html#specmask" rel="nofollow">http://classic.sdss.org/dr7/dm/flatFiles/spSpec.html#specmask</a></p>

<p>Is there a definition somewhere? Thanks</p>

<spectra><sky-survey>
Definition question: continuum-subtracted spectrum
ShanZhengYang
# Definition question: continuum-subtracted spectrum

(Asked by: username_0 on 2015-10-05)

What is the exact definition of a "continuum-subtracted spectrum", such that one finds in SDSS spectra?

<http://classic.sdss.org/dr7/dm/flatFiles/spSpec.html#specmask>

Is there a definition somewhere? Thanks

**Tags:** spectra, sky-survey


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## 1 answers

### Answer by username_1 on 2015-10-05. Score: 2 | Accepted answer

A spectrum of, say, a star or a galaxy, consists of wavelengths emitted from various physical processes. In the case of the star, there is the blackbody spectrum that reflects the temperature of all of its gas, whether it is hydrogen, helium, or metals. On top of this, there are *lines*, i.e. emission from certain atomic transitions that are excited and then de-excite emitting photons in a very narrow wavelength interval. The blackbody spectrum is said to comprise the continuum of the total spectrum.

In the case of galaxies, the continuum consists of the combined spectrum of many different stars' different blackbody spectra, infrared light from dust, etc. On top of this, there are lines, e.g. from nebular processes such as my favorite line Lyman $\alpha$, which is emitted when hard UV radiation from hot O and B stars ionize their surrounding neutral hydrogen, which subsequently recombines emitting mostly Lyman $\alpha$.

If we want to measure the total flux in a given line, we are usually only interested in the flux that comes from a particular physical process, and not the part of the flux that comes from the "underlying" sources which contribute to the continuum. Hence, we need to *subtract the continuum*. This is usually done by fitting some functional form to the continuum (e.g. a straight line or a second order polynomial), substract this fit from the spectrum, and finally integrate from one side of the line to the other in the resulting "continuum-subtracted spectrum".

In the top figure below, the total spectrum's flux density$^\dagger$ is in black, and the fit is the red lines. Underneath is drawn the continuum-subtracted spectrum, and a few dashed green lines show some lines that rise above the continuum. The integrated line flux is indicated by light red.

[![specs](https://i.sstatic.net/z04nX.png)](https://i.sstatic.net/z04nX.png)

$^\dagger$Note that many authors use the term "flux" where it should actually be "flux density". Integrating flux *density* in $\mathrm{erg}\,\mathrm{s}^{-1}\,\mathrm{cm}^{-2}\,\mathrm{Å}^{-1}$ over wavelength in Å$^{-1}$ gives *flux* in $\mathrm{erg}\,\mathrm{s}^{-1}\,\mathrm{cm}^{-2}$.


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