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Author
dc.contributor.author
Yip, C-W 
Author
dc.contributor.author
Mahoney, MW 
Author
dc.contributor.author
Szalay, AS 
Author
dc.contributor.author
Csabai, I 
Author
dc.contributor.author
Budavári, T 
Author
dc.contributor.author
Wyse, RFG 
Author
dc.contributor.author
Dobos, L 
Availability Date
dc.date.accessioned
2020-08-10T11:44:50Z
Availability Date
dc.date.available
2020-08-10T11:44:50Z
Release
dc.date.issued
2014
uri
dc.identifier.uri
http://hdl.handle.net/10831/48638
Abstract
dc.description.abstract
Understanding the diversity in spectra is the key to determining the physical parameters of galaxies. The optical spectra of galaxies are highly convoluted with continuum and lines that are potentially sensitive to different physical parameters. Defining the wavelength regions of interest is therefore an important question. In this work, we identify informative wavelength regions in a single-burst stellar population model using the CUR Matrix Decomposition. Simulating the Lick/IDS spectrograph configuration, we recover the widely used Dn (4000), Hβ, and HδA to be most informative. Simulating the Sloan Digital Sky Survey spectrograph configuration with a wavelength range 3450-8350 Å and a model-limited spectral resolution of 3 Å, the most informative regions are: first region - the 4000 Å break and the Hδ line; second region - the Fe-like indices; third region - the Hβ line; and fourth region - the G band and the Hγ line. A principal component analysis on the first region shows that the first eigenspectrum tells primarily the stellar age, the second eigenspectrum is related to the age-metallicity degeneracy, and the third eigenspectrum shows an anti-correlation between the strengths of the Balmer and the Ca K and H absorptions. The regions can be used to determine the stellar age and metallicity in early-type galaxies that have solar abundance ratios, no dust, and a single-burst star formation history. The region identification method can be applied to any set of spectra of the user's interest, so that we eliminate the need for a common, fixed-resolution index system. We discuss future directions in extending the current analysis to late-type galaxies. ASCII formatted tables of the regional eigenspectra are available. © 2014. The American Astronomical Society. All rights reserved.
Language
dc.language
Angol
Title
dc.title
Objective identification of informative wavelength regions in galaxy spectra
Type
dc.type
folyóiratcikk
Date Change
dc.date.updated
2020-05-28T13:51:26Z
Doi ID
dc.identifier.doi
10.1088/0004-6256/147/5/110
Wos ID
dc.identifier.wos
000334591900017
ID Scopus
dc.identifier.scopus
84898977992
MTMT ID
dc.identifier.mtmt
2585851
Issue Number
dc.identifier.issue
5
abbreviated journal
dc.identifier.jabbrev
ASTRON J
Journal
dc.identifier.jtitle
ASTRONOMICAL JOURNAL
Volume Number
dc.identifier.volume
147
Release Date
dc.description.issuedate
2014
department of Author
dc.contributor.institution
Alba Regia Egyetemi Központ
department of Author
dc.contributor.institution
Fizika Doktori Iskola
department of Author
dc.contributor.institution
Fizikai Intézet
department of Author
dc.contributor.institution
Mérnöki Intézet
department of Author
dc.contributor.institution
Komplex Rendszerek Fizikája Tanszék
Author institution
dc.contributor.department
Komplex Rendszerek Fizikája Tanszék
Author institution
dc.contributor.department
Komplex Rendszerek Fizikája Tanszék


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Objective identification of informative wavelength regions in galaxy spectra
 

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