Identifying Anomalous DESI Galaxy Spectra with a Variational Autoencoder

TL;DR

This paper demonstrates how Variational Autoencoders can effectively detect anomalies in DESI galaxy spectra, aiding in data quality control and discovery of unusual astrophysical objects.

Contribution

The study introduces a VAE-based method for anomaly detection in large spectral datasets, revealing its ability to compress data, identify artefacts, and uncover unique physical features.

Findings

VAE compresses spectra by a factor of 100 while retaining key features.

High reconstruction error and isolated latent space points indicate anomalies.

Latent space analysis reveals separation of object classes and spectral characteristics.

Abstract

The tens of millions of spectra being captured by the Dark Energy Spectroscopic Instrument (DESI) provide tremendous discovery potential. In this work we show how Machine Learning, in particular Variational Autoencoders (VAE), can detect anomalies in a sample of approximately 200,000 DESI spectra comprising galaxies, quasars and stars. We demonstrate that the VAE can compress the dimensionality of a spectrum by a factor of 100, while still retaining enough information to accurately reconstruct spectral features. We then detect anomalous spectra as those with high reconstruction error and those which are isolated in the VAE latent representation. The anomalies identified fall into two categories: spectra with artefacts and spectra with unique physical features. Awareness of the former can help to improve the DESI spectroscopic pipeline; whilst the latter can lead to the identification of new and unusual objects. To further curate the list of outliers, we use the Astronomaly package which employs Active Learning to provide personalised outlier recommendations for visual inspection. In this work we also explore the VAE latent space, finding that different object classes and subclasses are separated despite being unlabelled. We demonstrate the interpretability of this latent space by identifying tracks within it that correspond to various spectral characteristics. For example, we find tracks that correspond to increasing star formation and increase in broad emission lines along the Balmer series. In upcoming work we hope to apply the methods presented here to search for both systematics and astrophysically interesting objects in much larger datasets of DESI spectra.