Bayesian photometric redshifts with empirical training sets

TL;DR

This paper introduces a combined chi^2-template and empirical training set method for photometric redshift estimation, improving accuracy and reliability in ambiguous cases for large galaxy surveys.

Contribution

It presents a novel chi^2-empirical framework that derives PDFs from empirical models, enhancing photometric redshift accuracy and ambiguity detection.

Findings

<1% outliers for single-peak PDFs

Redshift errors <0.05 for most objects

78% of peaks correctly predicted as true

Abstract

We combine in a single framework the two complementary benefits of chi^2-template fits and empirical training sets used e.g. in neural nets: chi^2 is more reliable when its probability density functions (PDFs) are inspected for multiple peaks, while empirical training is more accurate when calibration and priors of query data and training set match. We present a chi^2-empirical method that derives PDFs from empirical models as a subclass of kernel regression methods, and apply it to the SDSS DR5 sample of >75,000 QSOs, which is full of ambiguities. Objects with single-peak PDFs show <1% outliers, rms redshift errors <0.05 and vanishing redshift bias. At z>2.5, these figures are 2x better. Outliers result purely from the discrete nature and limited size of the model, and rms errors are dominated by the instrinsic variety of object colours. PDFs classed as ambiguous provide accurate probabilities for alternative solutions and thus weights for using both solutions and avoiding needless outliers. E.g., the PDFs predict 78.0% of the stronger peaks to be correct, which is true for 77.9% of them. Redshift incompleteness is common in faint spectroscopic surveys and turns into a massive undetectable outlier risk above other performance limitations, but we can quantify residual outlier risks stemming from size and completeness of the model. We propose a matched chi^2-error scale for noisy data and show that it produces correct error estimates and redshift distributions accurate within Poisson errors. Our method can easily be applied to future large galaxy surveys, which will benefit from the reliability in ambiguity detection and residual risk quantification.