Editing Sunyaev–Zeldovich effect (section)

== Kinematic effects ==
The kinematic Sunyaev–Zeldovich effect is caused when a galaxy cluster is moving relative to the [[Hubble's law|Hubble flow]]. The kinematic Sunyaev–Zeldovich effect gives a method for calculating the peculiar velocity:
<math display="block">\Delta T_\text{kin} = - T_\text{CMB}\frac {V_p} {c} \tau</math>
where <math>V_p</math> is the peculiar velocity, and <math>\tau</math> is the optical depth.<ref>{{cite journal| last1=Tartari|first1=A.| last2=Boella|first2=G.|last3=Candotti|first3=M.|last4=Gervasi|first4=M.|last5=Natale|first5=V.| last6=Passerini|first6=A.| last7=Sironi|first7=G.|last8=Zannoni|first8=M.|date=2003-07-09|title=Sunyaev Zel'dovich effect studies with MASTER|journal=Memorie della Societa Astronomica Italiana Supplementi|volume=2|page=44|arxiv=astro-ph/0307166| bibcode=2003MSAIS...2...44T}}</ref> In order to use this equation, the thermal and kinematic effects need to be separated. The effect is relatively weak for most galaxy clusters. Using [[gravitational lens]]ing, the peculiar velocity can be used to determine other velocity components for a specific galaxy cluster.<ref name=":03" /> These kinematic effects can be used to determine the Hubble constant and the behavior of clusters.