Jump to content

Sunyaev–Zeldovich effect: Difference between revisions

From Wikipedia, the free encyclopedia
Browse history interactively
← Previous editNext edit →
Content deleted Content added
VisualWikitext
Citation bot (talk | contribs)
Bots
5,171,750 edits
Alter: pages. Add: issue. Formatted dashes. | You can use this bot yourself. Report bugs here. | Activated by Amigao | Category:Physical cosmology | via #UCB_Category
m →‎Overview: Moved link from Thermal (about wind?) to Thermal energy
Line 6: Line 6:
The Sunyaev–Zel'dovich effect can be divided into:
The Sunyaev–Zel'dovich effect can be divided into:


* [[thermal]] effects, where the CMB photons interact with electrons that have high energies due to their temperature
* [[Thermal energy|Thermal]] effects, where the CMB photons interact with electrons that have high energies due to their temperature
* [[kinematic]] effects, a second-order effect where the CMB photons interact with electrons that have high energies due to their bulk motion (also called the Ostriker–Vishniac effect, after [[Jeremiah P. Ostriker]] and [[Ethan Vishniac]].<ref>{{Cite journal|last=Ostriker|first=Jeremiah P.|last2=Vishniac|first2=Ethan T.|last-author-amp=yes|date=1986|title=Generation of Microwave Background Fluctuations from Nonlinear Perturbations at the Era of Galaxy Formation|url=|journal=Astrophysical Journal Letters|volume=306|page=L51|bibcode=1986ApJ...306L..51O|doi=10.1086/184704}}</ref>)
* [[Kinematic]] effects, a second-order effect where the CMB photons interact with electrons that have high energies due to their bulk motion (also called the Ostriker–Vishniac effect, after [[Jeremiah P. Ostriker]] and [[Ethan Vishniac]].<ref>{{Cite journal|last=Ostriker|first=Jeremiah P.|last2=Vishniac|first2=Ethan T.|last-author-amp=yes|date=1986|title=Generation of Microwave Background Fluctuations from Nonlinear Perturbations at the Era of Galaxy Formation|url=|journal=Astrophysical Journal Letters|volume=306|page=L51|bibcode=1986ApJ...306L..51O|doi=10.1086/184704}}</ref>)
* [[Polarization (waves)|polarization]]
* [[Polarization (waves)|polarization]]


Revision as of 18:18, 21 May 2020

Part of a series on
Physical cosmology
Full-sky image derived from nine years' WMAP data
Early universe
Backgrounds
Expansion · Future
Components · Structure
Components
Structure
Experiments
Scientists
Subject history

The Sunyaev–Zel'dovich effect (named after Rashid Sunyaev and Yakov B. Zel'dovich and often abbreviated as the SZ effect) is the distortion of the cosmic microwave background radiation (CMB) through inverse Compton scattering by high-energy electrons in galaxy clusters, in which the low-energy CMB photons receive an average energy boost during collision with the high-energy cluster electrons. Observed distortions of the cosmic microwave background spectrum are used to detect the disturbance of density in the universe. Using the Sunyaev–Zel'dovich effect, dense clusters of galaxies have been observed.

Overview

The Sunyaev–Zel'dovich effect can be divided into:

  • Thermal effects, where the CMB photons interact with electrons that have high energies due to their temperature
  • Kinematic effects, a second-order effect where the CMB photons interact with electrons that have high energies due to their bulk motion (also called the Ostriker–Vishniac effect, after Jeremiah P. Ostriker and Ethan Vishniac.[1])
  • polarization

Rashid Sunyaev and Yakov Zel'dovich predicted the effect, and conducted research in 1969, 1972, and 1980. The Sunyaev–Zel'dovich effect is of major astrophysical and cosmological interest. It can help determine the value of the Hubble constant. To distinguish the SZ effect due to galaxy clusters from ordinary density perturbations, both the spectral dependence and the spatial dependence of fluctuations in the cosmic microwave background are used. Analysis of CMB data at higher angular resolution (high -values) requires taking into account the Sunyaev–Zel'dovich effect.

Current research is focused on modelling how the effect is generated by the intracluster plasma in galaxy clusters, and on using the effect to estimate the Hubble constant and to separate different components in the angular average statistics of fluctuations in the background. Hydrodynamic structure formation simulations are being studied to gain data on thermal and kinetic effects in the theory.[2] Observations are difficult due to the small amplitude of the effect and to confusion with experimental error and other sources of CMB temperature fluctuations. However, since the Sunyaev–Zel'dovich effect is a scattering effect, its magnitude is independent of redshift. This is very important: it means that clusters at high redshift can be detected just as easily as those at low redshift. Another factor which facilitates high-redshift cluster detection is the angular scale versus redshift relation: it changes little between redshifts of 0.3 and 2, meaning that clusters between these redshifts have similar sizes on the sky. The use of surveys of clusters detected by their Sunyaev–Zel'dovich effect for the determination of cosmological parameters has been demonstrated by Barbosa et al. (1996). This might help in understanding the dynamics of dark energy in surveys (South Pole Telescope, Atacama Cosmology Telescope, Planck).

Observations

This picture taken by the Atacama Large Millimeter Array is known to be one of the most galaxy clusters, known as RX J1347-1145
First measurements of the thermal Sunyaev–Zel’dovich effect from the Atacama Large Millimeter Array with one of the most massive galaxy clusters known, RX J1347.5-1145.[3]

In 1984, researchers from the Cambridge Radio Astronomy Group and the Owens Valley Radio Observatory first detected the Sunyaev–Zel'dovich effect from clusters of galaxies [4]. Ten years later, the Ryle Telescope was used to image a cluster of galaxies in the Sunyaev–Zel'dovich effect for the first time.[citation needed]

Instruments built specifically to study the effect include the Sunyaev–Zel'dovich camera on the Atacama Pathfinder Experiment,[citation needed] and the Sunyaev–Zel'dovich 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.[5] In 2012 the kinematic SZ effect was detected in an individual object for the first time in MACS J0717.5+3745.[6]

References

  1. ^ Ostriker, Jeremiah P.; Vishniac, Ethan T. (1986). "Generation of Microwave Background Fluctuations from Nonlinear Perturbations at the Era of Galaxy Formation". Astrophysical Journal Letters. 306: L51. Bibcode:1986ApJ...306L..51O. doi:10.1086/184704. {{cite journal}}: Unknown parameter |last-author-amp= ignored (|name-list-style= suggested) (help)
  2. ^ Cunnama D., Faltenbacher F.; Passmoor S., Cress C.; Cress, C.; Passmoor, S. (2009). "The velocity-shape alignment of clusters and the kinetic Sunyaev–Zeldovich effect". MNRAS Letters. 397 (1): L41–L45. arXiv:0904.4765. Bibcode:2009MNRAS.397L..41C. doi:10.1111/j.1745-3933.2009.00680.x.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  3. ^ "ALMA's Hole in the Universe". www.eso.org. Retrieved 20 February 2017.
  4. ^ Birkinshaw, M.; Gull, S.F.; Hardebeck, H. (1984). "The Sunyaev-Zeldovich effect towards three clusters of galaxies". Nature. 309 (5963): 34–35. Bibcode:1984Natur.309...34B. doi:10.1038/309034a0.
  5. ^ Hand, Nick; Addison, Graeme E.; Aubourg, Eric; Battaglia, Nick; Battistelli, Elia S.; Bizyaev, Dmitry; Bond, J. Richard; Brewington, Howard; Brinkmann, Jon; Brown, Benjamin R.; Das, Sudeep; Dawson, Kyle S.; Devlin, Mark J.; Dunkley, Joanna; Dunner, Rolando; Eisenstein, Daniel J.; Fowler, Joseph W.; Gralla, Megan B.; Hajian, Amir; Halpern, Mark; Hilton, Matt; Hincks, Adam D.; Hlozek, Renée; Hughes, John P.; Infante, Leopoldo; Irwin, Kent D.; Kosowsky, Arthur; Lin, Yen-Ting; Malanushenko, Elena; et al. (2012). "Detection of Galaxy Cluster Motions with the Kinematic Sunyaev–Zel'dovich Effect". Physical Review Letters. 109 (4): 041101. arXiv:1203.4219. Bibcode:2012PhRvL.109d1101H. doi:10.1103/PhysRevLett.109.041101. PMID 23006072.
  6. ^ Mroczkowski, Tony; Dicker, Simon; Sayers, Jack; Reese, Erik D.; Mason, Brian; Czakon, Nicole; Romero, Charles; Young, Alexander; Devlin, Mark; Golwala, Sunil; Korngut, Phillip; Sarazin, Craig; Bock, James; Koch, Patrick M.; Lin, Kai-Yang; Molnar, Sandor M.; Pierpaoli, Elena; Umetsu, Keiichi; Zemcov, Michael (2012). "A Multi-wavelength Study of the Sunyaev–Zel'dovich Effect in the Triple-merger Cluster MACS J0717.5+3745 with MUSTANG and Bolocam". Astrophysical Journal. 761 (1): 47. arXiv:1205.0052. Bibcode:2012ApJ...761...47M. doi:10.1088/0004-637X/761/1/47.

Further reading

Retrieved from "https://en.wikipedia.org/w/index.php?title=Sunyaev–Zeldovich_effect&oldid=958036932"