Editing Laplace transform (section)

===Spatial (not time) structure from astronomical spectrum===
The wide and general applicability of the Laplace transform and its inverse is illustrated by an application in astronomy which provides some information on the ''spatial distribution'' of matter of an [[Astronomy|astronomical]] source of [[radiofrequency]] [[thermal radiation]] too distant to [[Angular resolution|resolve]] as more than a point, given its [[flux density]] [[spectrum]], rather than relating the ''time'' domain with the spectrum (frequency domain).

Assuming certain properties of the object, e.g. spherical shape and constant temperature, calculations based on carrying out an inverse Laplace transformation on the spectrum of the object can produce the only possible [[Mathematical model|model]] of the distribution of matter in it (density as a function of distance from the center) consistent with the spectrum.<ref>{{citation |first1=M. |last1=Salem |first2=M. J. |last2=Seaton |year=1974 |title=I. Continuum spectra and brightness contours |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=167 |pages=493–510 |doi=10.1093/mnras/167.3.493|bibcode=1974MNRAS.167..493S |doi-access=free}}, and<br/>{{citation |first1=M. |last1=Salem |year=1974 |title=II. Three-dimensional models |journal=Monthly Notices of the Royal Astronomical Society |volume=167 |pages=511–516 |doi=10.1093/mnras/167.3.511|bibcode=1974MNRAS.167..511S |doi-access=free}}</ref> When independent information on the structure of an object is available, the inverse Laplace transform method has been found to be in good agreement.