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Understanding the diversity in spectra is the key to determining the physicalparameters of galaxies. The optical spectra of galaxies are highly convolutedwith continuum and lines which are potentially sensitive to different physicalparameters. Defining the wavelength regions of interest is therefore animportant question. In this work, we identify informative wavelength regions ina single-burst stellar populations model by using the CUR Matrix Decomposition.Simulating the Lick/IDS spectrograph configuration, we recover the widely usedDn(4000), Hbeta, and HdeltaA to be most informative. Simulating the SDSSspectrograph configuration with a wavelength range 3450-8350 Angstrom and amodel-limited spectral resolution of 3 Angstrom, the most informative regionsare: first region-the 4000 Angstrom break and the Hdelta line; secondregion-the Fe-like indices; third region-the Hbeta line; fourth region-the Gband and the Hgamma line. A Principal Component Analysis on the first regionshows that the first eigenspectrum tells primarily the stellar age, the secondeigenspectrum is related to the age-metallicity degeneracy, and the thirdeigenspectrum shows an anti-correlation between the strengths of the Balmer andthe Ca K and H absorptions. The regions can be used to determine the stellarage and metallicity in early-type galaxies which have solar abundance ratios,no dust, and a single-burst star formation history. The region identificationmethod can be applied to any set of spectra of the user's interest, so that weeliminate the need for a common, fixed-resolution index system. We discussfuture directions in extending the current analysis to late-type galaxies.

Objective Identification of Informative Wavelength Regions in Galaxy Spectra