Automated unsupervised classification of the Sloan Digital Sky Survey stellar spectra using k-means clustering

TL;DR

This paper demonstrates the use of k-means clustering for automated, unsupervised classification of SDSS stellar spectra, effectively distinguishing stellar types and estimating physical parameters with minimal computational effort.

Contribution

It introduces a novel application of k-means clustering to classify stellar spectra without prior physical models, including analysis of spectra with and without continuum.

Findings

16 classes for spectra with continuum, distinguishing stars by color and type

13 classes for spectra without continuum, better separating stars by metallicity

Classification can estimate physical parameters with small ranges, aiding stellar analysis

Abstract

(Abridged) This paper explores the use of k-means clustering as a tool for automated unsupervised classification of massive stellar spectral catalogs. The classification criteria are defined by the data and the algorithm, with no prior physical framework. We work with a representative set of stellar spectra associated with the SDSS SEGUE and SEGUE-2 programs. We classify the original spectra as well as the spectra with the continuum removed. The second set only contains spectral lines, and it is less dependent on uncertainties of the flux calibration. The classification of the spectra with continuum renders 16 major classes. Roughly speaking, stars are split according to their colors, with enough finesse to distinguish dwarfs from giants of the same effective temperature, but with difficulties to separate stars with different metallicities. Overall, there is no one-to-one correspondence between the classes we derive and the MK types. The classification of spectra without continuum renders 13 classes, the color separation is not so sharp, but it distinguishes stars of the same effective temperature and different metallicities. Some classes thus obtained present a fairly small range of physical parameters (200 K in effective temperature, 0.25 dex in surface gravity, and 0.35 dex in metallicity), so that the classification can be used to estimate the main physical parameters of some stars at a minimum computational cost. We also analyze the outliers of the classification. Most of them turn out to be failures of the reduction pipeline, but there are also high redshift QSOs, multiple stellar systems, dust-reddened stars, galaxies, and, finally, odd spectra whose nature we have not decipher. The template spectra representative of the classes are publicly available (ftp://stars:kmeans@ftp.iac.es).