Editing Brown dwarf (section)

=== Observational techniques ===
[[File:BrownDwarfs Comparison 01.png|thumb|Brown dwarfs {{nowrap|[[Teide 1]]}}, [[Gliese 229]]B, and [[WISE 1828+2650]] compared to red dwarf [[Gliese 229A]], Jupiter and our Sun]]

[[Coronagraph]]s have recently been used to detect faint objects orbiting bright visible stars, including Gliese 229B.

Sensitive telescopes equipped with charge-coupled devices (CCDs) have been used to search distant star clusters for faint objects, including Teide 1.

Wide-field searches have identified individual faint objects, such as [[Kelu-1]] (30 light-years away).

Brown dwarfs are often discovered in surveys to discover [[exoplanet]]s. [[Methods of detecting exoplanets]] work for brown dwarfs as well, although brown dwarfs are much easier to detect.

Brown dwarfs can be powerful emitters of radio emission due to their strong magnetic fields. Observing programs at the [[Arecibo Observatory]] and the [[Very Large Array]] have detected over a dozen such objects, which are also called [[Ultra-cool dwarf|ultracool dwarfs]] because they share common magnetic properties with other objects in this class.<ref name="ReferenceA">{{cite journal |last1=Route |first1=Matthew |last2=Wolszczan |first2=Alexander |title=The Second Arecibo Search for 5 GHz Radio Flares from Ultracool Dwarfs |journal=The Astrophysical Journal |date=20 October 2016 |volume=830 |issue=2 |page=85 |doi=10.3847/0004-637X/830/2/85 |arxiv=1608.02480 |bibcode=2016ApJ...830...85R |s2cid=119279978 |doi-access=free }}</ref> The detection of radio emission from brown dwarfs permits their magnetic field strengths to be measured directly.