Paving the Way for Euclid and JWST via Optimal Selection of High-z Quasars

TL;DR

This paper presents a probabilistic, density-based method using Gaussian mixtures and deconvolution to efficiently select high-redshift quasars (z=6-8) for follow-up, improving completeness and efficiency over previous techniques.

Contribution

The authors develop a novel probabilistic selection technique utilizing Gaussian mixture models and deconvolution to identify high-z quasars more effectively.

Findings

Achieves >75% completeness and >15% efficiency in selecting 6<z<8 quasars.

Successfully recovers 80% of known z>7 quasars within the survey area.

Demonstrates potential for optimized quasar candidate selection for Euclid and JWST.

Abstract

We introduce a probabilistic approach to select 6<z<8 quasar candidates for spectroscopic follow-up, which is based on density estimation in the high-dimensional space inhabited by the optical and near-infrared photometry. Density distributions are modeled as Gaussian mixtures with principled accounting of errors using the extreme deconvolution (XD) technique, generalizing an approach successfully used to select lower redshift (z<3) quasars. We train the probability density of contaminants on 733,694 7-d flux measurements from the 1076 square degrees overlapping area from the DECaLS (z), VIKING (YJHK), and unWISE (W1W2) imaging surveys, after requiring they dropout of DECaLS g and r, whereas the distribution of high-z quasars are trained on synthetic model photometry. Extensive simulations based on these density distributions and current estimates of the quasar luminosity function indicate that this method achieves a completeness of >75% and an efficiency of >15% for selecting quasars at 6<z<8 with J<21.5. Among the classified sources are 8 known 6<z<7 quasars, of which 2/8 are selected suggesting a completeness ~25%, whereas classifying the 6 known (J<21.5) quasars at z>7 from the entire sky, we select 5/6 or a completeness of ~80%.The failure to select the majority of 6<z<7 quasars arises because our model of quasar SEDs underestimates the scatter in the distribution of fluxes. This new optimal approach to quasar selection paves the way for efficient spectroscopic follow-up of Euclid quasar candidates with ground based telescopes and JWST.