Distance (astronomy) | Wikipedia audio article
Channel: wikipedia tts
Date: 2018-12-31

This is an audio version of the Wikipedia Article:
https://en.wikipedia.org/wiki/Cosmic_distance_ladder


00:01:00 1 Direct measurement
00:01:25 1.1 Astronomical unit
00:02:33 1.2 Parallax
00:07:28 2 Standard candles
00:09:37 2.1 Problems
00:11:53 3 Standard siren
00:13:02 4 Standard ruler
00:14:36 5 Galactic distance indicators
00:17:48 5.1 Main sequence fitting
00:18:53 6 Extragalactic distance scale
00:19:29 6.1 Wilson–Bappu effect
00:20:27 6.2 Classical Cepheids
00:23:37 6.3 Supernovae
00:23:52 6.3.1 Measuring a supernova's photosphere
00:25:32 6.3.2 Type Ia light curves
00:28:12 6.3.3 Novae in distance determinations
00:29:34 6.4 Globular cluster luminosity function
00:31:31 6.5 Planetary nebula luminosity function
00:32:55 6.6 Surface brightness fluctuation method
00:33:47 6.7 D–σ relation
00:35:23 7 Overlap and scaling
00:38:30 8 See also



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SUMMARY
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The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are "close enough" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.
The ladder analogy arises because no single technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.