Checking the reliability of equivalent width R23 for estimating metallicities of galaxies

TL;DR

This study assesses the reliability of using equivalent width R23 instead of flux R23 for galaxy metallicity estimates, identifies biases, and proposes a correction method to improve accuracy.

Contribution

It introduces a correction based on (g-r) color to enhance the EW-R23 method's reliability for estimating galaxy metallicities.

Findings

EW-R23 introduces biases affecting log(O/H) by -0.2 to 0.1 dex.

Correction using polynomial fits reduces discrepancies to ~0.1 dex.

Over 92% of galaxies achieve accurate metallicity estimates after correction.

Abstract

We verify whether the O/H abundances of galaxies can be derived from the equivalent width (EW) R23 instead of the extinction-corrected flux R23, and eventually propose a method of improving the reliability of this empirical method, which is often used for the non-flux calibrated spectra of galaxies. We select 37,173 star-forming galaxies from the SDSS-DR2, which offers a wide range of properties to test the EW method. The EW-R23 method brings with it a significant bias: for the bulk of SDSS galaxies, it may affect the determination of log(O/H) by factors ranging from -0.2 to 0.1 dex and for some galaxies by factors ranging from -0.5 to 0.2 dex. We characterize this discrepancy (or bias) by alpha = (I_[OII]/I_Hbeta)/(EW_[OII]/EW_Hbeta), which is virtually independent of dust extinction, while tightly correlating with Dn(4000), although at a lower significance, with (g-r) colors. The EW-R23 method cannot be used as a proxy for the extinction-corrected flux R23 method. From analytical third-order polynomial fits of alpha versus (g-r) colors, we have been able to correct the EW-R23 method. With this additional and easy correction, the EW-R23 method provides O/H abundance values similar to those derived from the extinction-corrected flux R23 method with an accuracy of ~0.1 dex for >92% of the SDSS galaxies.