Image:Angular-size-redshift-relation.png
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[edit] Summary
The angular size redshift relation for a Lambda cosmology. This shows how the number of kiloparsecs per arcsecond changes with redshift. Note that after a redshift of about 1.5, objects appear larger with increasing distance. This was calculated using the web page of E. L. Wright http://www.astro.ucla.edu/~wright/CosmoCalc.html
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I, the copyright holder of this work, hereby release it into the public domain. This applies worldwide. In case this is not legally possible: Afrikaans | Alemannisch | Aragonés | العربية | Asturianu | Български | Català | Česky | Cymraeg | Dansk | Deutsch | Eʋegbe | Ελληνικά | English | Español | Esperanto | Euskara | Estremeñu | فارسی | Français | Galego | 한국어 | हिन्दी | Hrvatski | Ido | Bahasa Indonesia | Íslenska | Italiano | עברית | Kurdî / كوردی | Latina | Lietuvių | Latviešu | Magyar | Македонски | Bahasa Melayu | Nederlands | Norsk (bokmål) | Norsk (nynorsk) | 日本語 | Polski | Português | Ripoarisch | Română | Русский | Shqip | Slovenčina | Slovenščina | Српски / Srpski | Svenska | ไทย | Tagalog | Türkçe | Українська | Tiếng Việt | Walon | 中文(简体) | 中文(繁體) | zh-yue-hant | +/- |
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| Date/Time | Dimensions | User | Comment | |
|---|---|---|---|---|
| current | 11:01, 2 April 2006 | 400×269 (12 KB) | Hjb26 | (The en:angular size redshift relation for a Lambda cosmology This shows how the number of kiloparsecs per arcsecond changes with redshift. Note that after a redshift of about 1.5, objects appear ''larger'' with increasing) |
