Precision Spectrophotometry at the Level of 0.1

Precision Spectrophotometry at the Level of 0.1

Accurate relative spectrophotometry is critical for many science applications. Small wavelength-scale residuals in the flux calibration can significantly impact the measurements of weak emission and absorption features in the spectra. Using Sloan Digital Sky Survey data, we demonstrate that the aver...

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Bibliographic Details
Published in:The Astronomical journal 2011-11, Vol.142 (5), p.153-jQuery1323896817551='48'
Main Author: Yan, Renbin
Format: Article
Language:eng
Subjects:
ABSORPTION
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
CALIBRATION
COSMIC RADIO SOURCES
DATA ANALYSIS
EVOLUTION
Flux
GALACTIC EVOLUTION
GALAXIES
Intervals
QUASARS
RED SHIFT
SORPTION
Spectra
SPECTROPHOTOMETRY
Spectroscopy
Wavelengths
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Summary:Accurate relative spectrophotometry is critical for many science applications. Small wavelength-scale residuals in the flux calibration can significantly impact the measurements of weak emission and absorption features in the spectra. Using Sloan Digital Sky Survey data, we demonstrate that the average spectra of carefully selected red-sequence galaxies can be used as a spectroscopic standard to improve the relative spectrophotometry precision to 0.1% on small wavelength scales (from a few to hundreds of Angstroms). We achieve this precision by comparing stacked spectra across tiny redshift intervals. The redshift intervals must be small enough that any systematic stellar population evolution is minimized and is less than the spectrophotometric uncertainty. This purely empirical technique does not require any theoretical knowledge of true galaxy spectra. It can be applied to all large spectroscopic galaxy redshift surveys that sample a large number of galaxies in a uniform population.
ISSN:1538-3881
0004-6256
1538-3881