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dc.contributor.authorDavey, B. L. K.*
dc.contributor.authorCocke, W. J.*
dc.contributor.authorBates, R. H. T.*
dc.contributor.authorMcCarthy, D. W., jr.*
dc.contributor.authorChristou, J. C.*
dc.contributor.authorCobb, M. L.*
dc.date.accessioned2017-06-05T19:12:41Z
dc.date.available2017-06-05T19:12:41Z
dc.date.issued1988-12
dc.identifier.citationAJ 98: 1040-1048 (Sept. 1989)en
dc.identifier.urihttp://hdl.handle.net/10150/623921
dc.description.abstractOne -dimensional infrared speckle scans of Ross 614 AB were recorded at a wavelength of 2.2μm. For each scan an estimate of the instantaneous quality of the seeing was calculated and the scan was binned accordingly. The three bins corresponding to the three best seeing conditions were further processed by applying the shift -and -add algorithm to the set of images contained within each bin, thereby generating three shift- and -add images with differing shift -and -add point -spread- functions. After windowing the shift -and -add images (using edge -extension) to reduce the effect of contamination, we have obtained parameters corresponding to the separation and brightness ratio of a two component model of the double star Ross 614 AB by deconvolving the three shift -and -add images with the aid of the zero-and -add technique. Least squares analysis on the positions of the clusters of zeros found from zero- and -add yields a separation of 1.04 arcseconds and a brightness ratio of 4.3 for the binary system at this wavelength. An extension of the processing, which takes explicit account of the nonlinear motion of the scanning mechanism gives improved estimates of 1.04 arcseconds and 3.9 for the separation and brightness ratio, respectively.
dc.language.isoen_USen
dc.publisherSteward Observatory, The University of Arizona (Tucson, Arizona)en
dc.relation.ispartofseriesPreprints of the Steward Observatory #850en
dc.relation.urlhttp://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1989AJ.....98.1040D&db_key=AST&data_type=HTML&format=&high=3ed65e9cd023926en
dc.rightsCopyright © All Rights Reserved.en
dc.sourceSteward Observatory Parker Library SO QB 4 .S752 ARCHen
dc.subjectBinary starsen
dc.subjectSeeingen
dc.subjectSpeckle interferometryen
dc.subjectImage processingen
dc.titleInfrared Speckle Observations of Binary Ross 614 AB: Combined Shift-and-Add and Zero-and-Add Analysisen_US
dc.typetexten
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.description.collectioninformationThis title from the Steward Observatory Preprints collection is made available by the Steward Observatory Parker Library and the University Libraries, The University of Arizona. If you have questions about titles in this collection, please contact Parker Library librarian Betty Fridena, bfridena@as.arizona.edu.en
refterms.dateFOA2018-07-15T02:59:33Z
html.description.abstractOne -dimensional infrared speckle scans of Ross 614 AB were recorded at a wavelength of 2.2μm. For each scan an estimate of the instantaneous quality of the seeing was calculated and the scan was binned accordingly. The three bins corresponding to the three best seeing conditions were further processed by applying the shift -and -add algorithm to the set of images contained within each bin, thereby generating three shift- and -add images with differing shift -and -add point -spread- functions. After windowing the shift -and -add images (using edge -extension) to reduce the effect of contamination, we have obtained parameters corresponding to the separation and brightness ratio of a two component model of the double star Ross 614 AB by deconvolving the three shift -and -add images with the aid of the zero-and -add technique. Least squares analysis on the positions of the clusters of zeros found from zero- and -add yields a separation of 1.04 arcseconds and a brightness ratio of 4.3 for the binary system at this wavelength. An extension of the processing, which takes explicit account of the nonlinear motion of the scanning mechanism gives improved estimates of 1.04 arcseconds and 3.9 for the separation and brightness ratio, respectively.


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