Steps Towards a Fully Automated Classification and Redshift-measurement Pipeline for LAMOST Spectra. I. Continuum level and wavelength estimation for galaxies

Details Steps Towards a Fully Automated Classification and Redshift-measurement Pipeline for LAMOST Spectra. I. Continuum level and wavelength estimation for galaxies Steps Towards a Fully Automated Classification and Redshift-measurement Pipeline for LAMOST Spectra. I. Continuum level and wavelength estimation for galaxies

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001chjaa...1..563l&link_type=abstract

Chinese Journal of Astronomy & Astrophysics, Vol. 1, pp. 563-572

Astronomy and Astrophysics

Astrophysics

2

Methods: Data Analysis, Techniques: Spectroscopic, Galaxies: Emission Lines, Galaxies: Absorption Lines

Scientific paper

The Large Sky-Area Multi-Object Spectroscopic Telescope (LAMOST) under construction by the National Astronomical Observatories will yield up to four thousand multi-fiber spectra of stars and galaxies per field. The present series of papers describes the automated data-reduction pipeline currently being designed in order to cope with the anticipated flood of spectrographic data. In this preliminary paper, we present an automated method for estimating the continuum level, the positions of strong lines and the 4000 Å break in galaxy spectra. In order to obtain detailed information on the continuum, we use a wavelet filter bank. After continuum fitting, our software searches for a 4000 Å break and distinguishes between emission-line galaxies (ELGs) and non-ELGs according to whether the break is small or large. It then searches for strong lines and measures the intensities of emission lines and the equivalent widths of absorption lines. For non-ELGs, the absorption lines are identified automatically yielding redshift measurements.

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