<p>The anisotropies in the CMB are caused by four effects; three <em>at</em> the surface of last scattering (SoLS), and one <em>after</em>:</p>

<ol>
<li><strong>Temperature differences</strong>

<ul>
<li>Denser regions will be more compressed and thus hotter, on average. Hence, an overdensity will result in a hotter spot, with a fractional fluctuation <span class="math-container">$\Delta T/T_0$</span>.</li>
</ul></li>
<li><strong>Gravitational redshift</strong>

<ul>
<li>Photons climbing up (or falling down) the gravitational potential <span class="math-container">$\phi$</span> of their SoLS will lose (or gain) energy. Hence, an overdensity will result in a colder spot, and an underdensity in a hotter spot. This effect is also called the non-integrated Sachs-Wolfe effect and changes the temperature by <span class="math-container">$\Delta T = \phi/3c^2$</span>, where <span class="math-container">$c$</span> is the speed of light.</li>
</ul></li>
<li><strong>Doppler shift</strong>

<ul>
<li>The SoLS has a bulk motion <span class="math-container">$\mathbf{v}$</span>. Generally, overdensities have gas infalling, and hence result in a colder spot. In the direction <span class="math-container">$\hat{\mathbf{n}}$</span>, the temperature difference will be <span class="math-container">$\Delta T = T_0 \mathbf{v}/c$</span>.</li>
</ul></li>
<li><strong>The integrated Sachs-Wolfe effect</strong>

<ul>
<li>If a potential well is getting shallower in time (which happens during dark-energy domination), photons receive a net blueshift in crossing the well and the CMB appears hotter. This gives a temperature difference of <span class="math-container">$\Delta T = 2\Delta\phi/c^2$</span>, where <span class="math-container">$\Delta\phi$</span> is the change in the potential while a photon traversed the potential well.</li>
</ul></li>
</ol>

<p>The total temperature fluctuation is the sum of all these terms. In general, the gravitational redshift will dominate over the temperature differences, which in turn dominates over the Doppler shift.</p>

<p>A review of the CMB fluctuations is given by <a href="https://ui.adsabs.harvard.edu/abs/2013IAUS..288...42C/abstract" rel="noreferrer">Challinor (2013)</a>.</p>

CC BY-SA 4.0
2019-10-11T14:30:40.840Z
2019-10-11T14:30:40.840Z
pela
<p>If I'm understanding this correctly the fluctuations in CMB are a result of the "last scatter" of photons when electrons joined together with nuclei that before this formed plasma. CMB is among other things used to see the early matter density fluctuations of the early universe, right?</p>

<p>So, how is this seen? Are the warmer parts in the maps where the matter is most dense? And are these spots warmer because more photons are coming from that spot, or because of some other reason?</p>

<big-bang-theory><cosmic-microwave-background><photons>
Understanding The Fluctuations In The CMB Maps
LabanLe
# Understanding The Fluctuations In The CMB Maps

(Asked by: username_0 on 2019-10-09)

If I'm understanding this correctly the fluctuations in CMB are a result of the "last scatter" of photons when electrons joined together with nuclei that before this formed plasma. CMB is among other things used to see the early matter density fluctuations of the early universe, right?

So, how is this seen? Are the warmer parts in the maps where the matter is most dense? And are these spots warmer because more photons are coming from that spot, or because of some other reason?

**Tags:** big-bang-theory, cosmic-microwave-background, photons


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## 1 answers

### Answer by username_1 on 2019-10-11. Score: 6 | Accepted answer

The anisotropies in the CMB are caused by four effects; three *at* the surface of last scattering (SoLS), and one *after*:

1. **Temperature differences**
   * Denser regions will be more compressed and thus hotter, on average. Hence, an overdensity will result in a hotter spot, with a fractional fluctuation $\Delta T/T\_0$.
2. **Gravitational redshift**
   * Photons climbing up (or falling down) the gravitational potential $\phi$ of their SoLS will lose (or gain) energy. Hence, an overdensity will result in a colder spot, and an underdensity in a hotter spot. This effect is also called the non-integrated Sachs-Wolfe effect and changes the temperature by $\Delta T = \phi/3c^2$, where $c$ is the speed of light.
3. **Doppler shift**
   * The SoLS has a bulk motion $\mathbf{v}$. Generally, overdensities have gas infalling, and hence result in a colder spot. In the direction $\hat{\mathbf{n}}$, the temperature difference will be $\Delta T = T\_0 \mathbf{v}/c$.
4. **The integrated Sachs-Wolfe effect**
   * If a potential well is getting shallower in time (which happens during dark-energy domination), photons receive a net blueshift in crossing the well and the CMB appears hotter. This gives a temperature difference of $\Delta T = 2\Delta\phi/c^2$, where $\Delta\phi$ is the change in the potential while a photon traversed the potential well.

The total temperature fluctuation is the sum of all these terms. In general, the gravitational redshift will dominate over the temperature differences, which in turn dominates over the Doppler shift.

A review of the CMB fluctuations is given by [Challinor (2013)](https://ui.adsabs.harvard.edu/abs/2013IAUS..288...42C/abstract).


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