Editing Sunyaev–Zeldovich effect (section)

== Thermal effects ==
The distortion of the CMB resulting from a large number of high energy electrons is known as the thermal Sunyaev–Zeldovich effect. The thermal Sunyaev–Zeldovich effect is most commonly studied in [[galaxy cluster]]s. By comparing the Sunyaev–Zeldovich effect and [[X-ray emission]] data, the thermal structure of the cluster can be studied, and if the temperature profile is known, Sunyaev–Zeldovich data can be used to determine the baryonic mass of the cluster along the line of sight.<ref name=":03">{{Cite journal|last=Birkinshaw|first=M|date=March 1999|title=The Sunyaev–Zel'dovich effect|url=https://linkinghub.elsevier.com/retrieve/pii/S0370157398000805|journal=Physics Reports|volume=310|issue=2–3|pages=97–195|doi=10.1016/S0370-1573(98)00080-5|arxiv=astro-ph/9808050|bibcode=1999PhR...310...97B|hdl=1983/5d24f14a-26e0-44d3-8496-5843b108fec5|s2cid=119330362}}</ref> Comparing Sunyaev–Zeldovich and X-ray data can also be used to determine the Hubble constant using the angular diameter distance of the cluster.<ref>{{Cite journal|last1=Birkinshaw|first1=M.|last2=Hughes|first2=J. P.|date=January 1994|title=A measurement of the Hubble constant from the X-ray properties and the Sunyaev-Zel'dovich effect of Abell 2218|journal=The Astrophysical Journal|language=en|volume=420|pages=33|doi=10.1086/173540|bibcode=1994ApJ...420...33B|issn=0004-637X|doi-access=free}}</ref> These thermal distortions can also be measured in [[supercluster]]s and in gases in the local group, although they are less significant and more difficult to detect. In superclusters, the effect is not strong (< 8 μK), but with precise enough equipment, measuring this distortion can give a glimpse into large-scale structure formation. Gases in the local group may also cause anisotropies in the CMB due to the thermal Sunyaev–Zeldovich effect which must be taken into account when measuring the CMB for certain angular scales.<ref name=":03" />