Abstract

An increasing number of astronomical instruments (on Earth and space-based) provide hyperspectral images, that is three-dimensional data cubes with two spatial dimensions and one spectral dimension. The intrinsic limitation in spatial resolution of these instruments implies that the spectra associated with pixels of such images are most often mixtures of the spectra of the “pure” components that exist in the considered region. In order to estimate the spectra and spatial abundances of these pure components, we here propose an original blind signal separation (BSS), that is to say an unsupervised unmixing method. Our approach is based on extensions and combinations of linear BSS methods that belong to two major classes of methods, namely nonnegative matrix factorization (NMF) and sparse component analysis (SCA). The former performs the decomposition of hyperspectral images, as a set of pure spectra and abundance maps, by using nonnegativity constraints, but the estimated solution is not unique: It highly depends on the initialization of the algorithm. The considered SCA methods are based on the assumption of the existence of points or tiny spatial zones where only one source is active (i.e., one pure component is present). These points or zones are then used to estimate the mixture and perform the decomposition. In real conditions, the assumption of perfect single-source points or zones is not always realistic. In such conditions, SCA yields approximate versions of the unknown sources and mixing coefficients. We propose to use part of these preliminary estimates from the SCA to initialize several runs of the NMF in order to refine these estimates and further constrain the convergence of the NMF algorithm. The proposed methods also estimate the number of pure components involved in the data and they provide error bars associated with the obtained solution. Detailed tests with synthetic data show that the decomposition achieved with such hybrid methods is nearly unique and provides good performance, illustrating the potential of applications to real data.

Highlights

  • Telescopes keep growing in diameter, and detectors are more and more sensitive and made up of an increasing number of pixels

  • Our approach was to combine two well-known classes of methods, namely nonnegative matrix factorization (NMF) and Sparse sparse component analysis (SCA), in order to leverage their respective advantages while compensating their disadvantages

  • We developed several hybrid methods based on this principle, depending on the considered SCA algorithm (SpaceCorr or MASS) and depending whether that SCA algorithm is used to set the initial values of spectra or abundances updated by our Monte-Carlo version of NMF, called MC-NMF

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Summary

Introduction

Telescopes keep growing in diameter, and detectors are more and more sensitive and made up of an increasing number of pixels. An alternative analysis was proposed by Juvela et al (1996), which is based on a Blind Signal Separation (BSS) approach It consists in decomposing spectral cubes (in their case, CO spectral maps) into the product of a small number of spectral components, or “end members”, and spatial “abundance” maps. This requires no a priori on spectral properties of the components, and this can provide deeper insights into the physical structure represented in the data, as demonstrated in this pioneering paper. A spectral cube can be modeled in two different ways: a spectral model where we consider the cube as a set of spectra and a spatial model where we consider the cube as a set of images (spectral bands) , as detailed hereafter

Spectral model
Spatial model
Problem statement
Estimation of number of sources
Compute the average gradient of all these eigenvalues:
Blind signal separation methods
Sparse component analysis based on single-source zones
Mixing matrix identification
Summary of MASS method
Unmixing
Conclusion and future work
K-means method
Full Text
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