<p>If  you were in deep space, i,e., a spot somewhere between galaxies, then the night sky would look a lot like the sky seen by astronauts in the ISS, when they look away from both the ecliptic plane and the galactic plane, minus the individual Galactic stars.  That is, it is like our deep sky photos in those directions that are dominated by galaxies, but no atmospheric distortions, no night sky lines, and no zodiacal light.  The spectrum is dominated by different things at different wavelengths, but basically it is the sum of the light of galaxies and perhaps intergalactic stars that escaped their galaxies.  At long radio waves, it is dominated by supernova remnants and AGN as self-absorbed synchrotron radiation, peaking between 1 and 10 Mhz (<a href="http://adsabs.harvard.edu/cgi-bin/bib_query?1977MNRAS.180..429S" rel="nofollow noreferrer">Simon 1977</a>).  The mm band is dominated by the microwave background radiation at 2.7 C. The far-ir is dominated by cold galaxy dust at 60 microns. The optical is dominated by galaxy thermal starlight at 1 micron.  The UV is dominated by hot stars at 0.2 microns (<a href="http://www.isas.jaxa.jp/en/feature/forefront/151030.html" rel="nofollow noreferrer">see summary</a>).  The Xray spectrum from 3 to about 45 keV (<a href="http://adsabs.harvard.edu/cgi-bin/bib_query?1980ApJ...235....4M" rel="nofollow noreferrer">Marshall et al 1980</a>, <a href="https://ned.ipac.caltech.edu/level5/Fabian/Fabian2.html" rel="nofollow noreferrer">Fabian 1992</a>) is well-fitted by a ~40 keV thermal bremsstrahlung model. Above 45 kev the spectrum falls and is thought to be the sum of many AGN at all redshifts.  The spectral energy density (SED) from radio to X-ray is shown in this diagram from the paper by <a href="https://arxiv.org/abs/1802.03694" rel="nofollow noreferrer">Hill et al. (2018)</a> <em>The Spectrum of the Universe</em>:</p>

<p><a href="https://i.sstatic.net/kMqXU.png" rel="nofollow noreferrer"><img src="https://i.sstatic.net/kMqXU.png" alt="Spectrum of the Universe from Hill et al. (2018)"></a>
The width of the line in the diagram shows the present uncertainties in the measurements.</p>

<p>Dark energy does not shine, it has an effect on the redshift as a function of time and thereby indirectly affects the shape of the background spectrum. </p>

CC BY-SA 4.0
2018-12-11T20:41:19.047Z
Great answer, but why not show a plot of the full background, from radio to gamma-rays, rather than just the X-rays. [Hill et al. (2018)](https://arxiv.org/abs/1802.03694) has a nice plot in their Fig. 8 :)
pela
CC BY-SA 4.0
2018-12-12T05:04:52.667Z
OK.  I will add that.
eshaya
CC BY-SA 4.0
2018-12-10T22:41:26.757Z
2018-12-12T21:24:57.287Z
2018-12-12T21:24:57.287Z
eshaya
<p>What frequency distribution law applies to a random point in deep space that is assumed to be far away from any particular source of radiation. </p>

<p>Can it be expressed by some form of Plancks/Bose-Einsteins/Fermi-Diracs laws or a mix of all of them? </p>

<p>What would be the mean frequency/wawelength?</p>

<p>Would the mysterious "dark energy" be a major contributor to the distribution?</p>

CC BY-SA 4.0
2018-12-12T09:34:42.747Z
Hi Jens, you asked a [similar question](https://physics.stackexchange.com/q/233801/70207) a few years ago on physics.SE. I don't know if you ever saw our answers, but as we answered then, the energy density of radiation and dark energy (and dark matter) decreases differently with the expansion of the Universe. Moreover, radiation provides a positive pressure, whereas dark energy provides a negative pressure. See also [this physics.SE answer](https://physics.stackexchange.com/a/196373/70207) for an overview of the various contributions to the electromagnetic frequency distribution.
pela
<radiation><interstellar-medium><wavelength><cosmic-microwave-background>
Deep space radiation distribution
Jens
# Deep space radiation distribution

(Asked by: username_0 on 2018-12-08)

What frequency distribution law applies to a random point in deep space that is assumed to be far away from any particular source of radiation.

Can it be expressed by some form of Plancks/Bose-Einsteins/Fermi-Diracs laws or a mix of all of them?

What would be the mean frequency/wawelength?

Would the mysterious "dark energy" be a major contributor to the distribution?

**Tags:** radiation, interstellar-medium, wavelength, cosmic-microwave-background
> **Comments:**
> **username_1**: Hi Jens, you asked a [similar question](https://physics.stackexchange.com/q/233801/70207) a few years ago on physics.SE. I don't know if you ever saw our answers, but as we answered then, the energy density of radiation and dark energy (and dark matter) decreases differently with the expansion of the Universe. Moreover, radiation provides a positive pressure, whereas dark energy provides a negative pressure. See also [this physics.SE answer](https://physics.stackexchange.com/a/196373/70207) for an overview of the various contributions to the electromagnetic frequency distribution.  

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## 1 answers

### Answer by username_2 on 2018-12-10. Score: 3

If you were in deep space, i,e., a spot somewhere between galaxies, then the night sky would look a lot like the sky seen by astronauts in the ISS, when they look away from both the ecliptic plane and the galactic plane, minus the individual Galactic stars. That is, it is like our deep sky photos in those directions that are dominated by galaxies, but no atmospheric distortions, no night sky lines, and no zodiacal light. The spectrum is dominated by different things at different wavelengths, but basically it is the sum of the light of galaxies and perhaps intergalactic stars that escaped their galaxies. At long radio waves, it is dominated by supernova remnants and AGN as self-absorbed synchrotron radiation, peaking between 1 and 10 Mhz ([Simon 1977](http://adsabs.harvard.edu/cgi-bin/bib_query?1977MNRAS.180..429S)). The mm band is dominated by the microwave background radiation at 2.7 C. The far-ir is dominated by cold galaxy dust at 60 microns. The optical is dominated by galaxy thermal starlight at 1 micron. The UV is dominated by hot stars at 0.2 microns ([see summary](http://www.isas.jaxa.jp/en/feature/forefront/151030.html)). The Xray spectrum from 3 to about 45 keV ([Marshall et al 1980](http://adsabs.harvard.edu/cgi-bin/bib_query?1980ApJ...235....4M), [Fabian 1992](https://ned.ipac.caltech.edu/level5/Fabian/Fabian2.html)) is well-fitted by a ~40 keV thermal bremsstrahlung model. Above 45 kev the spectrum falls and is thought to be the sum of many AGN at all redshifts. The spectral energy density (SED) from radio to X-ray is shown in this diagram from the paper by [Hill et al. (2018)](https://arxiv.org/abs/1802.03694) *The Spectrum of the Universe*:

[![Spectrum of the Universe from Hill et al. (2018)](https://i.sstatic.net/kMqXU.png)](https://i.sstatic.net/kMqXU.png)
The width of the line in the diagram shows the present uncertainties in the measurements.

Dark energy does not shine, it has an effect on the redshift as a function of time and thereby indirectly affects the shape of the background spectrum.

> **Comments:**
> **username_1**: Great answer, but why not show a plot of the full background, from radio to gamma-rays, rather than just the X-rays. [Hill et al. (2018)](https://arxiv.org/abs/1802.03694) has a nice plot in their Fig. 8 :)  
> **username_2**: OK.  I will add that.  

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