RVSAO 2.0: Digital Redshifts and Radial Velocities

• Published in: Publications of the Astronomical Society of the Pacific 1998-08, Vol.110 (750), p.934-977
• Main Authors: Kurtz, Michael J., Mink, Douglas J.
• Format: Article
• Language: English
• Subjects: Absorption spectra; Astronomical objects; Calibration; Emission spectra; Galaxies; Line spectra; Radial velocity; Red shift; Spectral correlation; Wavelengths
• ISSN: 0004-6280; 1538-3873
• DOI: 10.1086/316207

RVSAO is a set of programs to obtain redshifts and radial velocities from digital spectra. RVSAO operates in the IRAF environment. The heart of the system isxcsao, which implements the cross‐correlation method and is a direct descendant of the system built byTonry & Davis.emsaouses intelligent heuristics to search for emission lines in spectra, and then fits them to obtain a redshift.sumspecshifts and sums spectra to build templates for cross‐correlation.linespecbuilds synthetic spectra given a list of spectral lines.bcvcorrcorrects velocities for the motion of the Earth. We discuss in detail the parameters necessary to runxcsaoandemsaoproperly. We discuss the reliability and error associated withxcsao‐derived redshifts. We develop an internal error estimator, and we show how large, stable surveys can be used to develop more accurate error estimators. We also develop a new methodology for building spectral templates for galaxy redshifts, using the new templates for the FAST spectrograph as an example. We show how to obtain correlation velocities using emission‐line templates. Emission‐line correlations are substantially more efficient than the previous standard technique, automated emission‐line fitting. Using this machinery, the blunder rate for redshift measurements can be kept near zero; the automation rate for FAST spectra is ∼95%. We useemsaoto measure the instrumental zero‐point offset and instrumental stability of the Z‐Machine and FAST spectrographs. We compare the use of RVSAO with new methods, which use singular value decomposition and χ2fitting techniques, and conclude that the methods we use are either equal or superior. We show that a two‐dimensional spectral classification of galaxy spectra can be developed using our emission‐ and absorption‐line templates as physically orthogonal basis vectors.