Editing AU Microscopii (section)

==Methods of observation==
[[File:Hubble captures blobs of material sweeping through stellar disc AU Microscopii.tif|thumb|Hubble observations of blobs of material sweeping through stellar disc.<ref>{{cite web |title=Hubble captures blobs of material sweeping through stellar disc |url=https://www.spacetelescope.org/images/opo1902a/ |website=www.spacetelescope.org |access-date=10 January 2019 |language=en}}</ref>]]
AU Mic's disk has been observed at a variety of different [[wavelength]]s, giving humans different types of information about the system. The light from the disk observed at [[visible light|optical wavelengths]] is stellar light that has reflected (scattered) off dust particles into Earth's line of sight. Observations at these wavelengths utilize a [[coronagraph|coronagraphic spot]] to block the bright light coming directly from the star.  Such observations provide high-resolution images of the disk. Because light having a wavelength longer than the size of a dust grain is scattered only poorly, comparing images at different wavelengths (visible and near-infrared, for example) gives humans information about the sizes of the dust grains in the disk.<ref name="ucbn0108">{{cite news | first=Robert | last=Sanders | title=Dust around nearby star like powder snow | publisher=UC Berkeley News | date=2007-01-08 | url=http://www.berkeley.edu/news/media/releases/2007/01/08_dust.shtml | access-date=2007-01-11 | archive-url= https://web.archive.org/web/20070115065231/http://www.berkeley.edu/news/media/releases/2007/01/08_dust.shtml| archive-date= 15 January 2007 | url-status= live}}</ref>

{{CSS image crop|Image=The 74 exocomet belts imaged by ALMA’s REASONS survey, showing belts of all shapes, sizes and ages (REASONS comboplot full nonames).jpg|bSize=1600|cWidth=160|cHeight=160|oTop=960|oLeft=800|Location=right|Description=millimeter observation of the disk from the REASONS survey<ref name="Martrá2025"/>}}

Optical observations have been made with the [[Hubble Space Telescope]] and [[Keck Telescope]]s.  The system has also been observed at [[infrared]] and sub-millimeter wavelengths with the [[James Clerk Maxwell Telescope]], [[Spitzer Space Telescope]], and the [[James Webb Space Telescope]]. This light is emitted directly by dust grains as a result of their internal heat (modified [[blackbody]] radiation). The disk cannot be resolved at these wavelengths, so such observations are measurements of the amount of light coming from the entire system. Observations at increasingly longer wavelengths give information about dust particles of larger sizes and at larger distances from the star.  
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