Velocities from Cross-Correlation: A Guide for Self-Improvement

dc.creatorPrieto, Carlos Allende
dc.date2007-07-18
dc.date.accessioned2026-07-07T11:17:54Z
dc.date.available2026-07-07T11:17:54Z
dc.descriptionThe measurement of Doppler velocity shifts in spectra is a ubiquitous theme in astronomy, usually handled by computing the cross-correlation of the signals, and finding the location of its maximum. This paper addresses the problem of the determination of wavelength or velocity shifts among multiple spectra of the same, or very similar, objects. We implement the classical cross-correlation method and experiment with several simple models to determine the location of the maximum of the cross-correlation function. We propose a new technique, 'self-improvement', to refine the derived solutions by requiring that the relative velocity for any given pair of spectra is consistent with all others. By exploiting all available information, spectroscopic surveys involving large numbers of similar objects may improve their precision significantly. As an example, we simulate the analysis of a survey of G-type stars with the SDSS instrumentation. Applying 'self-improvement' refines relative radial velocities by more than 50% at low signal-to-noise ratio. The concept is equally applicable to the problem of combining a series of spectroscopic observations of the same object, each with a different Doppler velocity or instrument-related offset, into a single spectrum with an enhanced signal-to-noise ratio.
dc.description7 pages, 3 figures, uses emulateapj.cls; to appear in the Astronomical Journal; see http://hebe.as.utexas.edu/stools/ to obtain the companion software
dc.identifierhttps://arxiv.org/abs/0707.2764
dc.identifierhttp://arxiv.org/abs/0707.2764
dc.identifierAstron.J.134:1843-1848,2007
dc.identifierdoi:10.1086/522051
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/193168
dc.subjectAstrophysics
dc.titleVelocities from Cross-Correlation: A Guide for Self-Improvement
dc.typetext

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