Jump to content

Cosmic background radiation: Difference between revisions

From Wikipedia, the free encyclopedia
Browse history interactively
← Previous edit
Content deleted Content added
VisualWikitext
m Reverted 1 edit by 167.102.157.165 identified as test/vandalism using STiki
remove PROD. If this is similar to another article, I recommend merging. If you still want to delete, this should be discussed at AfD. The article is 22+ years old and has had 115 editors and IPs.
 
(48 intermediate revisions by 42 users not shown)
Line 1: Line 1:

⚫
{{distinguish|cosmic microwave background radiation|cosmic infrared background radiation}}
{{Short description|Electromagnetic radiation from the Big Bang}}
⚫
{{distinguish|cosmic microwave background|cosmic infrared background}}
{{Physical cosmology}}
{{Physical cosmology}}
[[Image:Cobe-cosmic-background-radiation.gif|thumb|256px|Temperature of the cosmic background radiation spectrum as determined with the COBE satellite: uncorrected (top), corrected for the dipole term due to our peculiar velocity (middle), and corrected for contributions from the dipole term and from our galaxy (bottom).]]
[[Image:Cobe-cosmic-background-radiation.gif|thumb|256px|Temperature of the cosmic background radiation spectrum based on [[Cosmic Background Explorer|COBE]] data: uncorrected (top); corrected for the dipole term due to our [[peculiar velocity]] (middle); corrected additionally for contributions from our galaxy (bottom).]]


'''Cosmic background radiation''' is [[electromagnetic radiation]] from the sky with no discernible source. The origin of this radiation depends on the region of the [[electromagnetic spectrum|spectrum]] that is observed. One component is the [[cosmic microwave background radiation]]. This component is [[redshifted]] [[photon]]s that have freely streamed from an [[Recombination (cosmology)|epoch when the Universe became transparent]] for the first time to radiation. Its discovery and detailed observations of its properties are considered one of the major confirmations of the [[Big Bang]]. The discovery (by chance in 1965) of the cosmic background radiation suggests that the early universe was dominated by a radiation field, a field of extremely high temperature and pressure.<ref>{{cite news|url=http://whatisusa.info/the-first-minutes-of-the-big-bang/|title=First minutes of the Big Bang|publisher=What is USA News|date=12 March 2014 | accessdate=2013-11-19}}</ref>
'''Cosmic background radiation''' is [[electromagnetic radiation]] that fills all space. The origin of this radiation depends on the region of the [[electromagnetic spectrum|spectrum]] that is observed. One component is the [[cosmic microwave background]]. This component is [[redshifted]] [[photon]]s that have freely streamed from an [[Recombination (cosmology)|epoch when the Universe became transparent]] for the first time to radiation. Its discovery and detailed observations of its properties are considered one of the major confirmations of the [[Big Bang]]. The discovery (by chance in 1965) of the cosmic background radiation suggests that the early universe was dominated by a radiation field, a field of extremely high temperature and pressure.<ref>{{cite news|url=http://whatisusa.info/the-first-minutes-of-the-big-bang/|title=First minutes of the Big Bang|publisher=What is USA News|date=12 March 2014|access-date=2013-11-19|archive-url=https://web.archive.org/web/20140312121214/http://whatisusa.info/the-first-minutes-of-the-big-bang/|archive-date=12 March 2014|url-status=dead}}</ref>


The [[Sunyaev–Zel'dovich effect]] shows the phenomena of radiant cosmic background radiation interacting with "electron" clouds distorting the spectrum of the radiation.
The [[Sunyaev–Zel'dovich effect]] shows the phenomena of radiant cosmic background radiation interacting with "[[electron]]" clouds distorting the spectrum of the radiation.


There is also background radiation in the [[infrared]], [[x-ray]]s, etc., with different causes, and they can sometimes be resolved into an individual source. See [[cosmic infrared background]] and [[X-ray background]]. See also [[cosmic neutrino background]] and [[extragalactic background light]].
There is also background radiation in the [[infrared]], [[x-ray]]s, etc., with different causes, and they can sometimes be resolved into an individual source. See [[cosmic infrared background]] and [[X-ray background]]. See also [[cosmic neutrino background]] and [[extragalactic background light]].
Line 12: Line 14:


1896:
1896:
[[Charles Édouard Guillaume]] estimates the "radiation of the stars" to be 5.6 [[Kelvin|K]]. [http://redshift.vif.com/JournalFiles/Pre2001/V02NO3PDF/V02N3ASS.PDF Ref (PDF)]
[[Charles Édouard Guillaume]] estimates the "radiation of the stars" to be 5.6&nbsp;[[Kelvin|K]].<ref name="history">{{cite journal|url=http://redshift.vif.com/JournalFiles/Pre2001/V02NO3PDF/V02N3ASS.PDF|title=History of the 2.7 K Temperature Prior to Penzias and Wilson|first1=A. K. T.|last1=Assis|first2=M. C. D.|last2=Neves|journal=Apeiron|volume=2|number=3|date=3 July 1995}}</ref>


1926:
1926:
Sir [[Arthur Eddington]] estimates the non-thermal radiation of [[starlight]] in the galaxy has an effective temperature of 3.2 K. [http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1927Sci....66...81E&amp;db_key=AST&amp;data_type=HTML&amp;format=&amp;high=42ca922c9c22437]
Sir [[Arthur Eddington]] estimates the non-thermal radiation of [[starlight]] in the galaxy has an effective temperature of 3.2&nbsp;K. [http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1927Sci....66...81E&amp;db_key=AST&amp;data_type=HTML&amp;format=&amp;high=42ca922c9c22437]


1930s:
1930s:
[[Erich Regener]] calculates that the non-thermal spectrum of cosmic rays in the galaxy has an effective temperature of 2.8 K
[[Erich Regener]] calculates that the non-thermal spectrum of cosmic rays in the galaxy has an effective temperature of 2.8&nbsp;K.<ref name="history"/>


1931:
1931:
The term ''microwave'' first appears in print: ""When trials with wavelengths as low as 18 cm were made known, there was undisguised surprise that the problem of the micro-wave had been solved so soon." ''Telegraph & Telephone Journal'' XVII. 179/1"
The term ''microwave'' first appears in print: "When trials with wavelengths as low as 18&nbsp;cm were made known, there was undisguised surprise that the problem of the micro-wave had been solved so soon." ''Telegraph & Telephone Journal'' XVII. 179/1"


1938:
1938:
[[Nobel Prize]] winner (1920) [[Walther Nernst]] reestimates the cosmic ray temperature as 0.75 K
[[Walther Nernst]] re-estimates the cosmic ray temperature as 0.75&nbsp;K.<ref name="history"/>


1946:
1946:
Line 30: Line 32:


1946:
1946:
[[Robert Dicke]] predicts a microwave background radiation temperature of 20 K (ref: Helge Kragh)
[[Robert Dicke]] predicts a microwave background radiation temperature of 20&nbsp;K (ref: Helge Kragh)


1946:
1946:
Robert Dicke predicts a microwave background radiation temperature of "less that 20 K" but later revised to 45 K (ref: Stephen G. Brush)
Robert Dicke predicts a microwave background radiation temperature of "less than 20&nbsp;K" but later revised to 45&nbsp;K (ref: Stephen G. Brush).


1946:
1946:
[[George Gamow]] estimates a temperature of 50 K
[[George Gamow]] estimates a temperature of 50&nbsp;K.<ref name="history"/>


1948:
1948:
[[Ralph Alpher]] and [[Robert Herman]] re-estimate Gamow's estimate at 5 K.
[[Ralph Alpher]] and [[Robert Herman]] re-estimate Gamow's estimate at 5&nbsp;K.<ref name="history"/>


1949:
1949:
Ralph Alpher and Robert Herman re-re-estimate Gamow's estimate at 28 K.
Ralph Alpher and Robert Herman re-re-estimate Gamow's estimate at 28&nbsp;K.


1960s:
1960s:
Robert Dicke re-estimates a MBR (microwave background radiation) temperature of 40 K (ref: Helge Kragh)
Robert Dicke re-estimates a MBR (microwave background radiation) temperature of 40&nbsp;K (ref: Helge Kragh).


1965:
1960s:
[[Arno Penzias]] and [[Robert Woodrow Wilson]] measure the temperature to be approximately 3 K. Robert Dicke, [[P. J. E. Peebles]], P. G. Roll and [[David Todd Wilkinson|D. T. Wilkinson]] interpret this radiation as a signature of the Big Bang.
[[Arno Penzias]] and [[Robert Woodrow Wilson]] measure the temperature to be approximately 3&nbsp;K. Robert Dicke, [[P. J. E. Peebles]], P. G. Roll and [[David Todd Wilkinson|D. T. Wilkinson]] interpret this radiation as a signature of the Big Bang.<ref name="history"/>


==See also==
==See also==
{{Portal|Physics|Cosmology|Space}}
{{Portal|Physics|Space}}
* [[Hot dark matter]]
* [[Hot dark matter]]
* [[Irradiation]]
* [[Irradiation]]
* [[Unruh effect]]


==References==
==References==
Line 59: Line 62:


==External links==
==External links==
*[http://heasarc.nasa.gov/docs/objects/background/background.html The Diffuse X-ray and Gamma-ray Background & Deep Fields]
*[https://web.archive.org/web/20111017181402/http://heasarc.nasa.gov/docs/objects/background/background.html The Diffuse X-ray and Gamma-ray Background & Deep Fields]


[[Category:Cosmic background radiation| ]]
[[Category:Observational astronomy]]
[[Category:Observational astronomy]]
[[Category:Physical cosmology]]
[[Category:Physical cosmology]]
[[Category:Cosmic background radiation| ]]
[[Category:Concepts in astronomy]]
[[Category:Electromagnetic radiation]]

[[ca:Fons cosmològic]]
[[de:Hintergrundstrahlung]]
[[it:Radiazione cosmica di fondo]]
[[nl:Kosmische achtergrondstraling]]
[[ja:宇宙背景放射]]
[[fi:Kosminen taustasäteily]]

Latest revision as of 00:56, 11 January 2024

Not to be confused with cosmic microwave background or cosmic infrared background.
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
Temperature of the cosmic background radiation spectrum based on COBE data: uncorrected (top); corrected for the dipole term due to our peculiar velocity (middle); corrected additionally for contributions from our galaxy (bottom).

Cosmic background radiation is electromagnetic radiation that fills all space. The origin of this radiation depends on the region of the spectrum that is observed. One component is the cosmic microwave background. This component is redshifted photons that have freely streamed from an epoch when the Universe became transparent for the first time to radiation. Its discovery and detailed observations of its properties are considered one of the major confirmations of the Big Bang. The discovery (by chance in 1965) of the cosmic background radiation suggests that the early universe was dominated by a radiation field, a field of extremely high temperature and pressure.[1]

The Sunyaev–Zel'dovich effect shows the phenomena of radiant cosmic background radiation interacting with "electron" clouds distorting the spectrum of the radiation.

There is also background radiation in the infrared, x-rays, etc., with different causes, and they can sometimes be resolved into an individual source. See cosmic infrared background and X-ray background. See also cosmic neutrino background and extragalactic background light.

Timeline of significant events

[edit]

1896: Charles Édouard Guillaume estimates the "radiation of the stars" to be 5.6 K.[2]

1926: Sir Arthur Eddington estimates the non-thermal radiation of starlight in the galaxy has an effective temperature of 3.2 K. [1]

1930s: Erich Regener calculates that the non-thermal spectrum of cosmic rays in the galaxy has an effective temperature of 2.8 K.[2]

1931: The term microwave first appears in print: "When trials with wavelengths as low as 18 cm were made known, there was undisguised surprise that the problem of the micro-wave had been solved so soon." Telegraph & Telephone Journal XVII. 179/1"

1938: Walther Nernst re-estimates the cosmic ray temperature as 0.75 K.[2]

1946: The term "microwave" is first used in print in an astronomical context in an article "Microwave Radiation from the Sun and Moon" by Robert Dicke and Robert Beringer.

1946: Robert Dicke predicts a microwave background radiation temperature of 20 K (ref: Helge Kragh)

1946: Robert Dicke predicts a microwave background radiation temperature of "less than 20 K" but later revised to 45 K (ref: Stephen G. Brush).

1946: George Gamow estimates a temperature of 50 K.[2]

1948: Ralph Alpher and Robert Herman re-estimate Gamow's estimate at 5 K.[2]

1949: Ralph Alpher and Robert Herman re-re-estimate Gamow's estimate at 28 K.

1960s: Robert Dicke re-estimates a MBR (microwave background radiation) temperature of 40 K (ref: Helge Kragh).

1965: Arno Penzias and Robert Woodrow Wilson measure the temperature to be approximately 3 K. Robert Dicke, P. J. E. Peebles, P. G. Roll and D. T. Wilkinson interpret this radiation as a signature of the Big Bang.[2]

See also

[edit]

References

[edit]
  1. ^ "First minutes of the Big Bang". What is USA News. 12 March 2014. Archived from the original on 12 March 2014. Retrieved 2013-11-19.
  2. ^ a b c d e f Assis, A. K. T.; Neves, M. C. D. (3 July 1995). "History of the 2.7 K Temperature Prior to Penzias and Wilson" (PDF). Apeiron. 2 (3).
[edit]
Retrieved from "https://en.wikipedia.org/enwiki/w/index.php?title=Cosmic_background_radiation&oldid=1194844098"