The effect of emission lines on the performance of photometric redshift estimation algorithms

TL;DR

This study examines how strong emission lines influence the accuracy of empirical photometric redshift estimation methods, highlighting the importance of emission lines and comprehensive spectroscopic coverage for improved results.

Contribution

Develops a PCA-based stochastic mock catalogue generation technique to simulate realistic spectra with emission lines, aiding in evaluating photometric redshift methods.

Findings

Photometric noise dominates redshift uncertainty.

Emission lines help resolve colour space degeneracies.

Good spectroscopic coverage is essential for empirical methods.

Abstract

We investigate the effect of strong emission line galaxies on the performance of empirical photometric redshift estimation methods. In order to artificially control the contribution of photometric error and emission lines to total flux, we develop a PCA-based stochastic mock catalogue generation technique that allows for generating infinite signal-to-noise ratio model spectra with realistic emission lines on top of theoretical stellar continua. Instead of running the computationally expensive stellar population synthesis and nebular emission codes, our algorithm generates realistic spectra with a statistical approach, and - as an alternative to attempting to constrain the priors on input model parameters - works by matching output observational parameters. Hence, it can be used to match the luminosity, colour, emission line and photometric error distribution of any photometric sample with sufficient flux-calibrated spectroscopic follow-up. We test three simple empirical photometric estimation methods and compare the results with and without photometric noise and strong emission lines. While photometric noise clearly dominates the uncertainty of photometric redshift estimates, the key findings are that emission lines play a significant role in resolving colour space degeneracies and good spectroscopic coverage of the entire colour space is necessary to achieve good results with empirical photo-z methods. Template fitting methods, on the other hand, must use a template set with sufficient variation in emission line strengths and ratios, or even better, first estimate the redshift empirically and fit the colours with templates at the best-fit redshift to calculate the K-correction and various physical parameters.