Editing Sunyaev–Zeldovich effect (section)

== Observations ==
[[File:ALMA’s_Hole_in_the_Universe.jpg|alt=This picture taken by the Atacama Large Millimeter Array is known to be one of the most galaxy clusters, known as RX J1347-1145|thumb|First measurements of the thermal Sunyaev–Zeldovich effect from the [[Atacama Large Millimeter Array]] with one of the most massive galaxy clusters known, [[RX J1347.5−1145|RX J1347.5-1145]].<ref>{{cite web|title=ALMA's Hole in the Universe|url=https://www.eso.org/public/images/potw1708a/|access-date=20 February 2017|website=eso.org}}</ref>]]
In 1984, researchers from the [[Cavendish Astrophysics Group|Cambridge Radio Astronomy Group]] and the [[Owens Valley Radio Observatory]] first detected the Sunyaev–Zeldovich effect from [[Galaxy cluster|clusters of galaxies]].<ref>{{Cite journal|last1=Birkinshaw|first1=M.|last2=Gull|first2=S.F.|last3=Hardebeck|first3=H.|date=1984|title=The Sunyaev-Zeldovich effect towards three clusters of galaxies|url=https://www.nature.com/articles/309034a0|journal=Nature|volume=309|issue=5963|pages=34–35|bibcode=1984Natur.309...34B|doi=10.1038/309034a0|s2cid=4276748}}</ref> Ten years later, the [[Ryle Telescope]] was used to image a [[Galaxy cluster|cluster of galaxies]] in the Sunyaev–Zeldovich effect for the first time.<ref>{{cite arXiv|last=Saunders|first=Richard|date=1996-11-26|title=Sunyaev-Zel'dovich observations with the Ryle Telescope|eprint=astro-ph/9611213}}</ref>

In 1987 the [[Cosmic Background Explorer|Cosmic Background Explorer (COBE)]] satellite observed the CMB and gave more accurate data for anisotropies in the CMB, allowing for more accurate analysis of the Sunyaev–Zeldovich effect.<ref name=":03" />

Instruments built specifically to study the effect include the Sunyaev–Zeldovich camera on the [[Atacama Pathfinder Experiment]],<ref>{{Cite journal|last1=Schwan|first1=D.|last2=Ade|first2=P. a. R.|last3=Basu|first3=K.|last4=Bender|first4=A. N.|last5=Bertoldi|first5=F.|last6=Cho|first6=H.-M.|author6-link=Hsiao-Mei Cho|last7=Chon|first7=G.|last8=Clarke|first8=John|last9=Dobbs|first9=M.|last10=Ferrusca|first10=D.|last11=Güsten|first11=R.|date=2011-09-01|title=Invited Article: Millimeter-wave bolometer array receiver for the Atacama pathfinder experiment Sunyaev-Zel'dovich (APEX-SZ) instrument|url=https://aip.scitation.org/doi/full/10.1063/1.3637460|journal=Review of Scientific Instruments|volume=82|issue=9|pages=091301|doi=10.1063/1.3637460|pmid=21974566|arxiv=1008.0342|bibcode=2011RScI...82i1301S|s2cid=33402455|issn=0034-6748}}</ref> and the [[Sunyaev–Zel'dovich Array|Sunyaev–Zeldovich Array]], which both saw first light in 2005. In 2012, the [[Atacama Cosmology Telescope]] (ACT) performed the first statistical detection of the kinematic SZ effect.<ref>{{Cite journal|last1=Hand|first1=Nick|last2=Addison|first2=Graeme E.|last3=Aubourg|first3=Eric|last4=Battaglia|first4=Nick|last5=Battistelli|first5=Elia S.|last6=Bizyaev|first6=Dmitry|last7=Bond|first7=J. Richard|last8=Brewington|first8=Howard|last9=Brinkmann|first9=Jon|last10=Brown|first10=Benjamin R.|last11=Das|first11=Sudeep|display-authors=29|date=2012|title=Detection of Galaxy Cluster Motions with the Kinematic Sunyaev–Zeldovich Effect|journal=Physical Review Letters|volume=109|issue=4|pages=041101|arxiv=1203.4219|bibcode=2012PhRvL.109d1101H|doi=10.1103/PhysRevLett.109.041101|pmid=23006072|first21=Matt|first12=Kyle S.|last13=Devlin|first13=Mark J.|first14=Joanna|last15=Dunner|first15=Rolando|first16=Daniel J.|first18=Megan B.|last17=Fowler|first17=Joseph W.|last18=Gralla|last19=Hajian|last16=Eisenstein|last20=Halpern|first20=Mark|last21=Hilton|last12=Dawson|first26=Kent D.|last22=Hincks|last27=Kosowsky|last24=Hughes|first23=Renée|first24=John P.|last25=Infante|first25=Leopoldo|last26=Irwin|last29=Malanushenko|first27=Arthur|first19=Amir|last28=Lin|first28=Yen-Ting|first22=Adam D.|first29=Elena|last30=Malanushenko|first30=Viktor|s2cid=11392448|last23=Hlozek|last14=Dunkley}}</ref> In 2012 the kinematic SZ effect was detected in an individual object for the first time in [[MACS J0717.5+3745]].<ref>{{Cite journal|last1=Mroczkowski|first1=Tony|last2=Dicker|first2=Simon|last3=Sayers|first3=Jack|last4=Reese|first4=Erik D.|last5=Mason|first5=Brian|last6=Czakon|first6=Nicole|last7=Romero|first7=Charles|last8=Young|first8=Alexander|last9=Devlin|first9=Mark|last10=Golwala|first10=Sunil|last11=Korngut|first11=Phillip|title=A Multi-Wavelength Study of the Sunyaev-Zel'dovich Effect in the Triple-Merger Cluster Macs J0717.5+3745 with Mustang and Bolocam|date=2012-12-10|url=https://iopscience.iop.org/article/10.1088/0004-637X/761/1/47|journal=The Astrophysical Journal|volume=761|issue=1|pages=47|doi=10.1088/0004-637X/761/1/47|arxiv=1205.0052|bibcode=2012ApJ...761...47M|s2cid=50951413|issn=0004-637X}}</ref>

As of 2015, the [[South Pole Telescope|South Pole Telescope (SPT)]] had used the Sunyaev–Zeldovich effect to discover 415 galaxy clusters.<ref>{{Cite journal|last1=Bleem|first1=L. E.|last2=Stalder|first2=B.|last3=de Haan|first3=T.|last4=Aird|first4=K. A.|last5=Allen|first5=S. W.|last6=Applegate|first6=D. E.|last7=Ashby|first7=M. L. N.|last8=Bautz|first8=M.|last9=Bayliss|first9=M.|last10=Benson|first10=B. A.|last11=Bocquet|first11=S.|title=Galaxy Clusters Discovered Via the Sunyaev-Zel'dovich Effect in the 2500-Square-Degree SPT-Sz Survey|date=2015-01-29|url=https://iopscience.iop.org/article/10.1088/0067-0049/216/2/27|journal=The Astrophysical Journal Supplement Series|language=en|volume=216|issue=2|pages=27|doi=10.1088/0067-0049/216/2/27|arxiv=1409.0850|bibcode=2015ApJS..216...27B|hdl=1721.1/96784|s2cid=6663564|issn=1538-4365}}</ref> The Sunyaev–Zeldovich effect has been and will continue to be an important tool in discovering hundreds of galaxy clusters.

Recent experiments such as the OLIMPO balloon-borne telescope try to collect data in specific frequency bands and specific regions of the sky in order to pinpoint the Sunyaev–Zeldovich effect and give a more accurate map of certain regions of the sky.<ref>{{Cite journal|date=2007-03-01|title=The OLIMPO experiment|url=https://www.sciencedirect.com/science/article/abs/pii/S1387647306003253|journal=New Astronomy Reviews|language=en|volume=51|issue=3–4|pages=385–389|doi=10.1016/j.newar.2006.11.066|issn=1387-6473|last1=Nati|first1=F.|last2=Ade|first2=P.|last3=Boscaleri|first3=A.|last4=Brienza|first4=D.|last5=Calvo|first5=M.|last6=Colafrancesco|first6=S.|last7=Conversi|first7=L.|last8=De Bernardis|first8=P.|last9=De Petris|first9=M.|last10=Delbart|first10=A.|last11=Hargrave|first11=P.|last12=Iacoangeli|first12=A.|last13=Juin|first13=J.B.|last14=Magneville|first14=C.|last15=Marini Bettolo|first15=C.|last16=Masi|first16=S.|last17=Mauskopf|first17=P.|last18=Melchiorri|first18=F.|last19=Nati|first19=L.|last20=Orlando|first20=A.|last21=Rephaeli|first21=Y.|last22=Romeo|first22=G.|last23=Pansart|first23=J.P.|last24=Peterzen|first24=S.|last25=Piacentini|first25=F.|last26=Pisano|first26=G.|last27=Polenta|first27=G.|last28=Salvaterra|first28=L.|last29=Savini|first29=G.|last30=Tucker|first30=C.|bibcode=2007NewAR..51..385N|display-authors=1}}</ref>