Astronomy & Astrophysics
 | | CubeCombinaisonFusion | Jan 2009-Jan 2013 | Hyperspectral data fusion Keywords: optimal data fusion, spatial and spectral super-resolution, model-based, recursive update, Bayesian inference Input image type: hyperspectral, multiple images
 Participants: C. Collet [P.I.], M. Petremand, A. Jalobeanu, F. Salzenstein, V. Mazet Collaborators: E. Anterrieu (LATT), H. Carfantan (LATT), A. Bijaoui (OCA), E. Slezak (OCA), P. Weilbacher (AIP) Funding: ANR Dahlia

This project aims at providing a method for the statistical fusion of hyperspectral datacubes acquired from MUSE instrument. Each acquisition session of the same astronomical scene leads to an hyperspectral observation (or image) whose size is about 301x301x3578 pixels. As the amount of data grows while the number of sessions increases, a robust fusion method must be developed in order to produce a reduced datacube including all the information contained within the original set of observations. Each hyperspectral image may be acquired from various observation conditions (seeing, spatial and spectral sampling, geometric distortions, shifts...) and the fusion algorithm we propose takes these constraints into account. Finally, the uncertainty related to the fusion process is available for each spatial location in the form of a covariance matrix. Post-treatments can then use these statistical data to improve their performances. |
|  | | CubeDeconvolution | Jan 2009-Jan 2013 | Deconvolution of hyperspectral observations with varying PSF Keywords: deconvolution, varying PSF, astronomical data cube Input image type: hyperspectral, single image
 Participants: V. Mazet, C. Collet Collaborators: H. Carfantan [P.I.] (LATT), E. Anterrieu (LATT), S. Roques (LATT), L. Jolissaint (Leiden) Funding: ANR Dahlia

We consider the problem of deconvolution of astronomical data cubes. This project is part of ANR Dahlia (2009-2013) which aims at developping new methods for image analysis applied to the new integral field unit MUSE. Because in this application the data are huge (300x300x4096) and the PSF varies spatially and spectrally, no existing method could succesfully be applied. Therefore, we propose to develop a new framework in which we model the PSF variations. We also need to propose new priors and models to take into account the complexity of the spectral information in the cube. In a second hand, we will tune the method to the particular use for MUSE. This model will be developed in partnership with LATT (Toulouse, France). |
|  | | CubeSourceSeparation | Jan 2009-Jan 2013 | Source separation in hyperspectral deep field observations Keywords: source separation, decomposition into elementary signals, astronomical data cube Input image type: hyperspectral, single image
 Participants: C. Collet, V. Mazet, F. Salzenstein, M. Louys Collaborators: Y. Deville [P.I.] (LATT), S. Hosseini (LATT) Funding: ANR Dahlia

When observing two close astronomical sources (for example in star formation regions or globular clusters), the star spectra can recover yielding a mixture of the information. This project aims at extracting the spectral information of each source. This is a difficult problem since we have to estimate the source number and to handle with huge dimension data. Thus, we need to consider all the prior information available (positivity of mixture coefficients, positivity of the spectra, parcimony of the signals, ...). For these reasons, we use non-negative matrix factorization. This project takes place in collaboration with LATT (Toulouse, France). |
|  | | CubeVisualization | Jan 2009-Jan 2013 | Development of a visualization tool enabling large IFU data cubes upload, navigation and interpretation Keywords: Visualization, massive data sets, hyperspectral data, IFU Input image type: hyperspectral, multiple images
 Participants: M. Louys [P.I.], M. Petremand, V. Mazet, C. Collet Collaborators: E. Slezak (OCA), R. Bacon (CRAL) Funding: ANR Dahlia

Visualizing multi-dimensional observation data sets is a common challenge for observational sciences and crucial for Integral Field Spectroscopy (IFS) in astronomy. For the specific case of IFS data cubes, like MUSE, the size of the observation requires ad-hoc tools to be able to upload, visualize and navigate inside the 2D+lambda cube. This work package aims at :
- providing a viewer that enables to see the IFU data cube and
navigate along the observational axes: position (x,y) and wavelength
lambda;
- allowing for intelligent browsing by linking to observational
metadata, provided along with the data cube, e.g. variation of the Line
Spread Function (LSF) along the wavelength axis, variance data corresponding to the observed data, etc...
- allowing for comparison of original data with analysis results,
available in heterogeneous formats: extracted sources lists, sky
background statistical features along position and wavelength axis,
fusion-combined data;
- comparing visually several data cubes with each other.
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|  | | GalaxyClassification | Oct 2007-Oct 2010 | Galaxy classification using both spatial (morphological) and spectral aspects Keywords: galaxy classification, multivariate cube, decomposition into structures, Bayesian inference, mathematical morphology Input image type: multispectral, single image
 Participants: C. Collet [P.I.], V. Mazet, B. Perret Collaborators: S. Lefèvre (LSIIT), E. Slezak (OCA), E. Bertin (IAP), F. Bonnarel (CDS) Funding: MENRT

At present, the galaxies are classified using their morphological visual appearance (e.g. Hubble sequence). However, studying the galaxies at several wavelength is very useful to understand their dynamics, their evolution, and, consequently, the universe history. Therefore, the goal of the project is to propose a classification method using both the spatial and spectral informations. We propose to use two complementary approaches in image processing: Bayesian inference and mathematical morphology. The first one considers a marked point process model set in a Bayesian framework, from which a posterior distribution is optimized using MCMC method to estimate the major geometrical parameters of the galaxy (center, size, presence of a bar, etc.). Then mathematical morphology provides informations about spiral arms, distribution of stars, ... |
|  | | AstroCubeSegmentation | Sep 2006-Dec 2009 | Hyperspectral data cube segmentation of astronomical images Keywords: Data cube, spectral line estimation, mixture of Gaussians, decomposition into elementary patterns, MCMC Input image type: hyperspectral, single image
 Participants: V. Mazet [P.I.], C. Collet, F. Flitti Collaborators: B. Vollmer (CDS), F. Bonnarel (CDS) Funding: ACI Grid (IDHA) + ACI MDA

This project aims at helping astronomers to handle complex spectroscopic line data cubes, where the inspection of the channel and moment maps is difficult. The goal is to provide a tool that is able to differentiate between kinematic zones in galaxies by segmenting the multispectral or hyperspectral image in homogeneous spectral areas. The kinematic zones are characterized by their own spectrum, which may be shifted due to the Doppler effect. Two approaches have been proposed.
In the first approach, the spectrum of each pixel is fitted to a combination of a limited number of Gaussian functions with fixed mean values and variances. This is needed because the number of input images for the segmentation process is limited (due to the Hughes phenomenon). The spatial distribution of the Gaussian weights is the input of a Markovian segmentation algorithm.
The final segmentation map contains classes of pixels with similar spectral line profiles.The application of our method to the HI data cube of the Virgo spiral galaxy NGC 4254 shows that regions of kinematic interest can be detected (Doppler effect).
The second (and current) approach consists in decomposing each pixel (i.e. each spectrum) into peaks whose number, position, amplitude and widths are estimated. For that purpose, an MCMC algorithm is used. Then, a second step consists of "tracking" the estimated peaks, from a pixel to another, finally providing 3D spectral homogeneous clouds. This approach is currently studied. |
|  | | DeepSkyFusion | Dec 2005-Dec 2008 | Multisource data fusion and 2D super-resolution Keywords: data fusion, spatial and spectral super-resolution, model-based, recursive update, Bayesian inference Input image type: multispectral, multiple images
 Participants: A. Jalobeanu [P.I.], C. Collet, F. Salzenstein, M. Louys, J. Gutiérrez, K. Quach Collaborators: A. Bijaoui (OCA), E. Slezak (OCA) Funding: ANR (SpaceFusion project)

The goal is to perform multi-source data fusion from multispectral images, possibly achieving spatial and spectral super-resolution. Our approach is to combine all (or almost all) the information into a single model. In this case, the model is a 2D image having an arbitrary resolution and number of spectral bands. In practice, this depends on the amount of available data, thus leading to super-resolved results when many input images are used.
We propose to use a Bayesian inference method, based on the inversion of a forward model. The forward model describes the image formation process for each observation, and takes into account some a priori knowledge (e.g. fractal structure and multiscale properties, image roughness). Thus, understanding the image formation process is an essential step.
The originality of the work is in devising and implementing new methods to perform multi-image data fusion (e.g. multiband images at various resolutions and orientations) through Bayesian inference, with the ability to address both spectral and spatial super-resolution when needed, and to perform model selection in order to automatically determine the resolution needed. This involves both automatic registration and spatial-spectral resampling, which are ill-posed inverse problems that are addressed within a rigorous, probabilistic framework. |
|  | | LSBGalaxyDetect | Feb 2005-Dec 2008 | LSB galaxy detection using a Markov quadtree Keywords: detection, Markov quadtree, low surface brightness galaxies Input image type: multispectral, single image
 Participants: C. Collet [P.I.], M. Louys, M. Petremand, B. Perret, F. Lavigne, D. Ballu Collaborators: W. Van Driel (Meudon Obs.), B. Vollmer (CDS), F. Bonnarel (CDS), S. Sabatini (Obs. Rome) Funding: ACI MD (MDA project)

Galaxies are diffuse objects which must be detected against a background of finite brightness with noise. Galaxies having the highest contrast with respect to this background are the most easily dectected. Low surface brightness (LSB) galaxies are those in which the contrast with respect to the background sky brightness is very low. As such they are difficult to discover. In some cases, small galaxies, which were classified as dwarf galaxies, turned out to be the center of a much larger disk LSB galaxy. [ see examples]
These low surface brightness galaxies were discovered only about 20 years ago. Their evolution must be different from 'normal' high surface brightness galaxies. Since they are difficult to detect, the number of known LSBs is very limited. They represent a galaxy class which is still not well understood.
We propose to take advantage of the redundancy in multispectral images to improve the detection, and to use a Markov tree-based prior model to help separate such large scale objects from the background, high frequency noise.
DetectLSB, coupled with LSBExplorer and MARSIAA, has been developed to ease the automatic detection and analysis of such faint objects. |
|  | | CopulaHMTSegment | Oct 2004-Dec 2005 | Copulas theory and pairwise quadtree Keywords: Copula theory, Markov pairwise quadtree Input image type: multispectral, single image
 Participants: F. Flitti [P.I.], C. Collet Collaborators: A. Joannic-Chardin (INT), W. Pieczynski (INT) Funding: ACI Grid (IDHA project)

The Hidden Markov Quadtree model is a very useful tool for multiband image segmentation. Nevertheless, this task, which requires multivariate probability density computations for the data likelihood term, has to cope with the lack of analytical multidimensional expressions in the non-Gaussian case. Thus, the multidimensional Gaussian distribution is usually used for its simplicity, even if the Gaussian assumption is not always verified. In this work, we propose a new approach based on copula theory to compute multivariate density on a pairwise Markov quadtree. |
|  | | PNSpectrum | Jun 2004-Dec 2005 | Planetary nebula long-slit spectrum rendering for inference purposes Keywords: volume rendering, planetary nebula modeling, long-slit spectrum, accurate sampling Input image type: single band, single image
 Participant: A. Jalobeanu [P.I.] Collaborators: K. Knuth (Univ. Albany), K. Huyser (NASA)

We are inferring three-dimensional planetary nebula (PN) models - including the size, shape, expansion rate, orientation, nebular mass distribution, and distance from Earth - using data consisting of images obtained over time from the Hubble Space Telescope (HST) and long-slit spectra obtained from Kitt Peak National Observatory and Cerro Tololo Inter-American Observatory. These images are taken from a single viewpoint in space, which creates a very challenging tomographic reconstruction.
We employ Bayesian model estimation using a parameterized physical model of the nebula, which incorporates much prior information about the known physics of how the PN is illuminated by the ionizing radiation from the central star. The model is used to make a prediction, which is then compared with the real data to determine how to improve the model. This methodology is extremely powerful and allows us to incorporate multiple disparate data types.
In this work, we focus on how to render a long-slit spectrum, given a parametrized physical model of the nebula. It involves an accurate sampling scheme in order to avoid artifacts due to discretization. Given the model of the gas density in the 3D space, this density is integrated along the line of sight for each pixel of the spectrum image. By comparing synthetic and real spectra, we can infer parameters that can not be inferred from images only, due to indeterminations in the tomographic reconstruction problem. |
|  | | MultiColorViz | Oct 2003-Jun 2006 | Color visualization of hyperspectral images Keywords: Multispectral, color display, HSV space, Fisher analysis, PCA, Markovian segmentation Input image type: hyperspectral, single image
 Participants: M. Petremand [P.I.], C. Collet, M. Louys, F. Flitti Collaborators: F. Bonnarel (CDS), L. Cambrésy (CDS), F. Genova (CDS) Funding: ACI MD (MDA Project)

This new approach is used for the color display of multispectral and hyperspectral images. The color representation of such data becomes problematic when the number of bands is higher than three, i.e. the basic RGB. Here we use a technique that uses a segmentation map as an a priori information, and then compute a Factorial Discriminant Analysis (Fisher analysis) in order to allow, at best, a distribution of the information in the HSV color space (Hue, Saturation, Value). The information collected from the segmentation map (where each pixel is associated with a class) has been shown to be beneficial to the representation of the images. Indeed, good results were obtained on large size image collections in the framework of astronomical images. This method can easily be applied to other domains such as polarimetric imaging or remote sensing. |
|  | | HyperGalaxyClass | Oct 2003-Nov 2006 | Hyperspectral data cube analysis for galaxy classification Keywords: hyperspectral, galaxy classification, meanshift, projection, segmentation, reduction Input image type: hyperspectral, single image
 Participants: C. Collet [P.I.], B. Perret, M. Petremand, M. Louys, O. Marchal Collaborators: F. Bonnarel (CDS), E. Slezak (OCA), J. Blaizot (CRAL), B. Guiderdoni (CRAL), F. Genova (CDS) Funding: ACI MD (MDA project)

This new approach is used for galaxy classification. The galaxies can be found by searching through hyperspectral data cubes. The high spatial and spectral resolution for such data cubes (the size can reach 1000x1000x1000 pixels) give both physical (spectral) and morphological (spatial) information. The goal is to associate a galaxy type from the morphological Hubble's classification to each galaxy using a both spectral and spatial method. First, spectra are projected onto a reference basis, given a set of projection weights. Second, the meanshift algorithm finds the modes of the projection weights distribution. These modes lead to a new projection basis and the projection and meanshift steps are repeated until convergence. These steps are used in order to find the main spectral behaviors in the data cube. This is the spectral part of the approach. Then, the LBG algorithm (spatial clustering) is used in the projection space to get a segmentation map where each galaxy is regarded as a set of classes. The class distribution in galaxies is representative of their type. Tests on synthetic data use galaxy fields resulting from GALICS, a galaxy field simulation software. |
|  | | QTreeRestoFusion | Oct 2002-Jun 2005 | Fusion/denoising in wavelet space using a Markov quadtree Keywords: Multispectral image fusion, denoising, Markov, quadtree, wavelets Input image type: multispectral, single image
 Participants: F. Flitti [P.I.], C. Collet Collaborators: E. Slezak (OCA), F. Bonnarel (CDS) Funding: ACI Grid (IDHA project)

This research deals with astronomical multiband image fusion and denoising. The wavelet domain is well adapted to such tasks. In fact, intensity fluctuations corresponding to the noise are most important at the finest resolution and related detail coefficients decrease quickly as the scale increases. Real structures in the image will therefore lead to larger detail coefficient values. This information can be suitably combined to detect and fuse real structures in all bands. In this work, we present a new fusion-restoration scheme for astronomical multispectral data, operating in four steps. First, a pyramidal algorithm with one wavelet analyzes all spectral bands, leading to a pyramid of detail coefficients for each band. Second, the detail information for all bands are combined into a single multiband and multiresolution pyramid. Fed into a hierarchical, quadtree-based Markovian classifier, it provides a multiscale binary segmentation map that acts as a mask for 'small enough' coefficients at each scale. Third, the selected (i.e., non-masked) coefficients are merged into a single pyramidal structure of detail coefficients. Finally, this resulting structure is used within an iterative reconstruction procedure to recover the denoised, fused image. The Markovian quadtree models spatial, interscale and interband correlations at once, allowing for information fusion from a whole data cube. |
|  | | FuzzyMarkovSegment | Jan 2002-Dec 2010 | Non-Stationary Fuzzy Markov Chain/Field Segmentation Keywords: Markov field, Markov chain, fuzzy models, fuzzy triplet Markov chain, non-stationary Markov chain Input image type: multispectral, single image
 Participants: F. Salzenstein [P.I.], C. Collet, M. Petremand, M. Hatt, G. Multon, S. Le Cam Collaborator: G. Lagache (IAS) Funding: ACI Grid (IDHA), ACI MD (MDA Project), MENRT

The segmentation process on multicomponent images requires a non-trivial modeling step, in order to affect a label for different sets of pixels exhibiting similar behaviors. On one hand, observations between bands are dependent and require an adapted multivariate model. On the other hand, the fuzzy statistical classification algorithms have not yet been used in astronomical imaging: as the observations are intrinsically inaccurate, a 'hard' classification which labels the data into finite discrete sets artificially eliminates the inaccuracy. Yet, many deep sky observations such as far galaxies or dust/gas clouds have such intrinsic fuzzy properties. Fuzzy schemes, taking into account discrete and continuous classes, are able to model the imprecision of the hidden data. We developed new fuzzy Markovian models (chain and field) assuming inter-band dependencies. The segmentation is performed in an unsupervised way, dealing with hyperparameter estimation. In particular, we apply such fuzzy-based procedures to astronomical observations where patterns exhibit diffuse structures. Moreover, these approaches allow us to account for missing data in one or several spectral bands as is often needed in Astronomy. |
|  | | MissingMultiSegmentA | Oct 2001-Jun 2003 | Noise modeling, outliers and missing data management for segmentation tasks with multiwavelength images Keywords: outliers, missing data, quadtree, unsupervised segmentation Input image type: multispectral, single image
 Participants: C. Collet [P.I.], M. Louys, A. Moktari, K-P. Maalej Collaborators: C. Bot (CDS), A. Lançon (CDS), A. Oberto (CDS), F. Bonnarel (CDS) Funding: ACI Grid (IDHA project)

This project deals with the unsupervised segmentation of astronomical multiband images. Most of these images have the particularity to be quantized on floating-point numbers with large luminance range, on different wavelengths, with missing data in several bands. These characteristics necessitate the manipulation of large amounts of accurate data on each spectral band, which is very different from the case of 8-bit integer pixels. We present some results obtained on multiwavelength images of the Small Magellanic Cloud, by using the Marginal Posterior Mode (MPM) estimator on a quadtree structure under Markovian assumptions. The estimation of the model parameters is then addressed with Expectation-Maximization (EM)-type algorithms, allowing for an unsupervised hyperparameter estimation. The main interest of this modeling effort lies in its generality: the algorithm handles multiwavelength floating-point data in a single upward and downward scan on the quadtree. A new aspect deals with the noise statistics that are supposed to be lognormal or Generalized Gaussian for each class. Another new aspect is the in-scale-coding of the label map. |
|  | | QTreeMultiSegment | Oct 1999-Jun 2004 | Multiresolution Markov Modeling for Multichannel Segmentation Keywords: Unsupervised segmentation, Markovian quadtree, Generalized Gaussian model, multispectral data Input image type: multispectral, single image
 Participants: C. Collet [P.I.], M. Louys, F. Flitti, M. Petremand Collaborators: J-N. Provost (INSA), P. Pérez (IRISA), P. Bouthemy (IRISA), F. Murtagh (Univ. London), A. Oberto (CDS), C. Bot (CDS), A. Lançon (CDS), F. Bonnarel (CDS) Funding: ACI Grid (IDHA project)

We have developed an unsupervised method to segment multispectral images corrupted by non-Gaussian noise. The efficiency of the proposed Markovian quadtree-based method has been illustrated on multichannel astronomical image segmentation tasks.
The proposed method relies on a hierarchical Markovian modeling and includes the estimation of all involved parameters. The parameters of the prior model are automatically calibrated while the estimation of the noise parameters is solved by identifying generalized distribution mixtures, by means of an Iterative Conditional Estimation procedure. Generalized Gaussian, Weibull or Rayleigh distributions are purported to model various intensity distributions of the multispectral images. They are indeed well suited to a large variety of correlated multispectral data. |
|  | | CubeExtract | - | Cube Extraction Keywords: cube preview, hyperspectral, adaptive binning Input image type: hyperspectral, single image
 Participants: M. Louys [P.I.], C. Collet, K. Hett Collaborator: F. Bonnarel (CDS) Funding: ICUBE/ Intern

We develop various methods for cut-out extraction in hyperspectral data cubes.
Preview products such as mean average image on a sub-band , average spectrum on a region of interest, are proposed .
Adaptive binning is examined in order to support adequate data selection in the data cube. |
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