File:Cosmic distance ladder.jpg

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描述Cosmic distance ladder.jpg	English: For the calibration of relatively short distances the team observed Cepheid variables. These are pulsating stars which fade and brighten at rates that are proportional to their true brightness and this property allows astronomers to determine their distances. The researchers calibrated the distances to the Cepheids using a basic geometrical technique called parallax. With Hubble’s sharp-eyed Wide Field Camera 3 (WFC3), they extended the parallax measurements further than previously possible, across the Milky Way galaxy. To get accurate distances to nearby galaxies, the team then looked for galaxies containing both Cepheids and Type Ia supernovae. Type Ia supernovae always have the same intrinsic brightness and are also bright enough to be seen at relatively large distances. By comparing the observed brightness of both types of stars in those nearby galaxies, the team could then accurately measure the true brightness of the supernova. Using this calibrated rung on the distance ladder the accurate distance to additional 300 type Ia supernovae in far-flung galaxies was calculated. They compare those distance measurements with how the light from the supernovae is stretched to longer wavelengths by the expansion of space. Finally, they use these two values to calculate how fast the universe expands with time, called the Hubble constant.
日期	2016年6月2日, 17:30:00
來源	http://www.spacetelescope.org/images/heic1611a/
作者	NASA,ESA, A. Feild (STScI), and A. Riess (STScI/JHU)

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目前	2016年6月3日 (五) 10:04		1,280 × 832（155 KB）	Jmencisom	User created page with UploadWizard

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全域檔案使用狀況

以下其他 wiki 使用了這個檔案：

cs.wikipedia.org 的使用狀況
- Žebřík kosmických vzdáleností
en.wikipedia.org 的使用狀況
es.wikipedia.org 的使用狀況
- Escalera de distancias cósmicas
et.wikipedia.org 的使用狀況
- Mustand:Kosmiliste kauguse redel
eu.wikipedia.org 的使用狀況
- Lankide:Joxan Garaialde/Distantzia kosmikoen eskailera
- Distantzia kosmikoen eskailera
fa.wikipedia.org 的使用狀況
- نردبان فاصله کیهانی
fi.wikipedia.org 的使用狀況
- Kosmiset etäisyystikapuut
mk.wikipedia.org 的使用狀況
- Скала на вселенски растојанија
ms.wikipedia.org 的使用狀況
- Paralaks
- Paralaks dalam astronomi

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製作/提供者	NASA, ESA, A. Feild (STScI), and A. Riess (STScI/JHU)
來源	ESA/Hubble
簡稱	Cosmic distance ladder
影像標題	For the calibration of relatively short distances the team observed Cepheid variables. These are pulsating stars which fade and brighten at rates that are proportional to their true brightness and this property allows astronomers to determine their distances. The researchers calibrated the distances to the Cepheids using a basic geometrical technique called parallax. With Hubble’s sharp-eyed Wide Field Camera 3 (WFC3), they extended the parallax measurements further than previously possible, across the Milky Way galaxy. To get accurate distances to nearby galaxies, the team then looked for galaxies containing both Cepheids and Type Ia supernovae. Type Ia supernovae always have the same intrinsic brightness and are also bright enough to be seen at relatively large distances. By comparing the observed brightness of both types of stars in those nearby galaxies, the team could then accurately measure the true brightness of the supernova. Using this calibrated rung on the distance ladder the accurate distance to additional 300 type Ia supernovae in far-flung galaxies was calculated. They compare those distance measurements with how the light from the supernovae is stretched to longer wavelengths by the expansion of space. Finally, they use these two values to calculate how fast the universe expands with time, called the Hubble constant.
使用條款	Creative Commons Attribution 4.0 International License
資料產生的日期時間	2016年6月2日 (四) 17:30
聯絡資訊	http://www.spacetelescope.org Karl-Schwarzschild-Strasse 2 Garching bei M√ºnchen, , D-85748 Germany
IIM 版本	4

File:Cosmic distance ladder.jpg

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創用CC姓名標示4.0國際 ^{繁體中文 (已轉換拼寫)}

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創用CC姓名標示4.0國際 繁體中文 (已轉換拼寫)

2 6 2016

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19dbffefe7e6c83902c6c7639dd4c6eada50b465

158,582 位元組

832 像素

1,280 像素

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全域檔案使用狀況

詮釋資料

創用CC姓名標示4.0國際 ^{繁體中文 (已轉換拼寫)}