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High precision measurements of stellar spectroscopic line profiles and theirchanges over time contain very valuable information about the physics of thestellar photosphere (stellar activity) and can be used to characterizeextrasolar planets via the Rossiter-McLaughlin effect or from reflected lightfrom the planet.  In this paper we present a new method for measuring small changes in the meanline profile of a spectrum by performing what we call differential LeastSquares Deconvolution (dLSD). The method consists in finding the convolutionfunction (or kernel) required to transform a high signal-to-noise ratiotemplate of the star into each observed spectrum. Compared to similartechniques, the method presented here does not require any assumptions on thetemplate spectrum (eg. no line-list or cross-correlation mask required).  We show that our implementation of dLSD is able to perform -at least- as goodas other techniques by applying it to star-planet obliquity measurements ofexoplanet HD183799 during its transit. Among other things, the method shouldenable model independent detection of light reflected by an exoplanet.

monthly notices of the royal astronomical society

A differential Least Squares Deconvolution method for high precision  spectroscopy of stars and exoplanets I. Application to obliquity measurements  of HARPS observations of HD189733b