“Probabilistic Analysis for Space & Earth Observations”
Multisource & Multispectral Image Processing via Bayesian Inference
MIV team ICUBE

CNRSUDS

Research Projects

Our application areas range from deep sky exploration (star fields, galaxies, nebulae) to planetary imaging (planets, small bodies) including Earth observation — using images at various resolutions and spectral depths. We aim at a better understanding of space imaging in order to provide new tools for astronomy and astrophysics, planetary sciences and remote sensing specialists.
Projects are organized by application area and starting date. All projects are displayed, including collaborative works and PhD theses.

Application areas

  • Astronomy & Astrophysics
  • Planetary Imaging
  • Remote Sensing (Earth)
  • Astronomy & Astrophysics

    CubeCombinaisonFusionJan 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.
    CubeDeconvolutionJan 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).
    CubeSourceSeparationJan 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).
    CubeVisualizationJan 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.
    GalaxyClassificationOct 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, ...
    AstroCubeSegmentationSep 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.
    DeepSkyFusionDec 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.
    LSBGalaxyDetectFeb 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.
    CopulaHMTSegmentOct 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.
    PNSpectrumJun 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.
    MultiColorVizOct 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.
    HyperGalaxyClassOct 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.
    QTreeRestoFusionOct 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.
    FuzzyMarkovSegmentJan 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.
    MissingMultiSegmentAOct 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.
    QTreeMultiSegmentOct 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.
    http://icube.unistra.fr/icube/index.php/Accueil

    Planetary Imaging (Small Bodies & Planets)

    3DSpaceFusionDec 2005-Nov 2008
    Multisource data fusion, 3D surface recovery and super-resolution
    Keywords: 3D surface recovery, reflectance estimation, data fusion, super-resolution, model-based, recursive update, Bayesian inference
    Input image type: multispectral, multiple images

    Participants: A. Jalobeanu [P.I.], C. Collet, M. Joshi, S. Sharma
    Collaborator: A. Bijaoui (OCA)
    Funding: ANR (SpaceFusion project)

    The originality of the project lies in considering data fusion as the estimation of a single model, of arbitrary spatial and spectral resolutions. The model is to be inferred from a number of observations, possibly from different sensors under various conditions. It is all about reconstructing a geometric and radiometric object that best relates to the observations and integrates all the useful information contained in the initial data.
    In planetary imaging, both terrain topography and camera parameters must be taken into account to efficiently combine several images. Therefore, the topography will explicitely be included in the model. It will be decoupled from the multispectral reflectance that relates to the texture and color of the terrain. The object provided by the fusion-reconstruction method will be a 3D surface, possibly super-resolved regarding both geometry and reflectance.
    We will start by defining a generative model, enabling us to describe the image formation from a single multiband (3D surface). The estimation of the model parameters and related uncertainties will be performed through hierarchical Bayesian inference. This will enable us to integrate the physics of the studied objects by including all available a priori knowledge. It will also involve observation models describing the data acquisition process (image formation and degradation). This approach will remain open since it will allow for model updating, in order to include new data into the model as soon as they become available.
    3DShapeInferenceJan 2004-Sep 2006
    3D shape recovery via Bayesian inference
    Keywords: DEM reconstruction, surface recovery, Bayesian inference, marginalization, rendering
    Input image type: single band, multiple images

    Participants: A. Jalobeanu [P.I.], S. Sharma
    Collaborator: J. Stutz (NASA)

    We aim at the recovery of the 3D geometry of small bodies or planetary surfaces, using multiple, single band images taken under similar lighting conditions. The new technique currently being developed is based on a fully Bayesian inference, involving prior modeling and marginalization. The shape is parametrized by a Spline height field, textured by a Spline reflected radiance field. We assume Gaussian Markovian priors for the surface model. The modeled observation process, equivalent to rendering, is modeled by a geometric transform followed by a convolution a PSF, and contamination by additive Gaussian noise.
    The major novelty of the proposed method consists of marginalizing out the reflected radiances considered as nuisance parameters, which is achieved by a hierarchy of approximations. This reduces the inference to minimizing an energy that only depends on the shape vertices, and therefore allows for an efficient Iterated Conditional Mode (ICM) optimization scheme to be implemented. A Gaussian approximation of the posterior shape density is computed, thus providing estimates of both the geometry and its uncertainty. The effectiveness of the new shape reconstruction method has been shown in 2D. A 3D method is currently under development and seeks to recover a surface from multiple observations, reconstructing the topography by marginalizing out both albedo and shading.
    The first stage of the algorithm, or initiaization, consists of Bayesian stereo vision: first infer a dense disparity map (project DispMapInference), then use it to calibrate the push-broom cameras (project BayesCameraCalibration), and finally convert the disparities into a height field.
    SurfaceModelRenderJan 2002-Sep 2005
    Accurate rendering and modeling of natural 3D surfaces
    Keywords: subdivision surfaces, wavelets on meshes, fractals, graphical models, object-based rendering, shadows, occlusions
    Input image type: single band, single image

    Participant: A. Jalobeanu [P.I.]
    Collaborators: J. Stutz (NASA), F. Kuehnel (RIACS)
    Funding: INRIA, RIACS (NASA Ames)

    Models of natural images have long been used in computer vision. However, since they only describe the statistics of 2D scenes, they fail to capture all the properties of the underlying 3D world. Even though such models are sufficient for many vision tasks, a 3D scene model is needed when it comes to inferring a 3D object or its properties.
    We have developed both a multiscale surface prior model for the surface geometry, and an image formation model based on accurate and realistic rendering, that accounts for the physics of image generation. A graphical model is used to describe the hierarchical modeling process, from the actual surface to the final, blurred and noisy image.
    Geometric modeling is achieved through a fractal approach involving wavelets on subdivided meshes. We also addressed the problems of hidden surface removal, shadow casting and sampling, which are among the critical aspects of the rendering. Our original visibility determination technique is object-based, since it computes polygon intersections at the object (i.e. surface mesh) precision, whereas most methods are image-based (e.g. the z-buffer).
    There are a few promising potential applications, such as asteroid modeling, reflectance function generation for rough surfaces and planetary topography recovery.

    Remote Sensing (Earth Observation)

    BayesCameraCalibrationJun 2007-Dec 2008
    Absolute Push-Broom camera calibration with uncertainties
    Keywords: DEM matching, affine camera calibration, Bayesian inference
    Input image type: single band, single image

    Participants: A. Jalobeanu [P.I.], S. Sharma
    Funding: ANR SpaceFusion

    A precise camera model is required in order to derive accurate topography from dense disparity maps computed from a stereo pair. In remote sensing, push-broom cameras are widely used, however they are far more complex than rigid cameras based on 2D sensors, commonly used in computer vision. The absolute camera calibration problem amounts to estimating the trajectory and attitude for both images, as well as some internal parameters in some cases. The major difficulty comes from the high number of parameters involved, as the attitude can vary rapidely due to oscillations; indeed, there might be an independent set of parameters every 10 to 100 rows (and images typically have 10k rows). Therefore, performing an absolute calibration (with respect to a reference ellipsoid for instance) requires a large number of ground control points (GCP). Conversely, only a few points are required when the camera model is rigid.
    We propose to address this problem by locally approximating the imaging geometry by an affine model, whose parameters are inferred within a Bayesian framework, thus allowing for error estimation. We assume that a minimum number of GCPs is provided for each patch of the image where the affine model is valid. Existing elevation models (SRTM for Earth, MOLA for Mars) can be used as large sets of GCPs. The proposed technique actually performs a registration between the high resolution reconstructed elevation model and the lower resolution, existing set of GCPs, using a height field parametrization. Finally, the global camera model will be obtained by interpolating the set of local models, thus avoiding the complex task of trajectory computation by restricting to linear geometric transforms. As the number of estimated variables is much smaller than the number of data points (since there are many points for each row), the accuracy of the reconstructed topography should be significantly higher with respect to the existing model.
    DispMapInferenceJun 2006-Dec 2008
    Robust dense disparity map estimation with uncertainties
    Keywords: dense disparity map, deformation field, warping, B-Spline interpolation, radiometric changes, spatially adaptive
    Input image type: single band, single image

    Participant: A. Jalobeanu [P.I.]
    Collaborator: D. Fitzenz (CGE)
    Funding: ANR SpaceFusion, INSU (PNTS)

    Disparity maps estimated using computer vision-derived algorithms usually lack quantitative error estimates. This can be a major issue when the result is used to measure reliable physical parameters, such as topography for instance. Thus, we propose to develop a new method to infer the dense disparity map from two images. We use a probabilistic approach in order to compute uncertainties as well. Within this framework, parameters are described in terms of random variables. We start by defining a generative model for both raw observed images given all model variables, including disparities. The forward model mainly consists of warping the scene using B-Splines and using a spatially adaptive, semi-parametric radiometric change map. Then we use Bayesian inference to invert and recover the a posteriori probability density function (pdf) of the disparity map.
    The main contributions are: The design of an efficient model to take into account radiometric changes between images; A multigrid processing so as to speed up the optimization process; The use of raw data instead of orthorectified imagery; Efficient approximation schemes to integrate out unwanted parameters and compute uncertainties on the result. Three applications could benefit from this disparity inference method: DEM generation from a stereo pair (along or across track), automatic calibration of pushbroom cameras, and ground deformation estimation from two images at different dates.
    ReflectanceFusionDec 2005-Nov 2008
    Multisource, multispectral data fusion and super-resolution
    Keywords: Data fusion, super-resolution, pan-sharpening, model-based, Bayesian inference
    Input image type: multispectral, multiple images

    Participants: A. Jalobeanu [P.I.], C. Collet, M. Joshi
    Funding: ANR (SpaceFusion project)

    We propose to develop new data fusion and reconstruction methods. The originality of the project lies in considering data fusion as the estimation of a single model, of arbitrary spatial and spectral resolutions. The model is to be inferred from a number of inhomogeneous observations, possibly from different sensors under various viewing conditions. It is all about reconstructing a multispectral radiometric object that best relates to the observations and integrates all the useful information contained in the initial data.
    The goal is to reconstruct a multispectral reflectance map that relates to the texture and color properties of the terrain. The object provided by the fusion-reconstruction method will be a well-sampled reflectance map, possibly super-resolved regarding both spatial and spectral sampling. Pan-sharpening is a special case where the goal is to infer a color image from a high-resolution panchromatic image and lower resolution color bands.
    We will start by modeling the multiband image formation from a single reflectance map. The estimation of the model parameters and related uncertainties will be performed through hierarchical Bayesian inference. This allows to integrate the physics of the Earth terrains by including available a priori knowledge. It also involves observation models describing the onboard data acquisition process (image formation and degradation from the satellites sensor to the ground reception).
    ImPolarJan 2003-Jul 2004
    Segmentation of Multicomponent Mueller Images
    Keywords: Multidimensional polarization encoded images, Mueller matrix, Bayesian segmentation
    Input image type: multispectral, single image

    Participants: C. Collet, R. Roux
    Collaborator: J. Zallat [P.I.] (LSIIT)
    Funding: CNRS (EPML8 - RTP26)

    We address the clustering of multidimensional polarization encoded images. The bi-dimensional coherence of the polarization information is considered. Two analysis ways are proposed: polarization contrast enhancement and a more sophisticated image processing algorithm based on a Markovian model.
    The proposed algorithms are applied to two different Mueller images acquired by a fully polarimetric imaging system. Polarimetric imaging can be used effectively to characterize objects even under low radiance conditions. It is particularly useful in determining target shapes and compositions. This work investigates the usefulness of coupling polarization information with image processing techniques as opposed to pixel-based processing usually employed. Taking into account the bidimensional consistency of polarization information proves to be very efficient. Indeed, good results were obtained by using a simple polarization contrast enhancement algorithm. On the other hand, only the Hierarchical Hidden Markov Model was able to segment properly the man-made object at very low signal level.
    MTFInferFractalJan 2001-Mar 2006
    Bayesian inference of parametric MTF using fractal priors
    Keywords: self-similarity, fractals, MTF estimation, uncertainties, marginalization
    Input image type: single band, single image

    Participant: A. Jalobeanu [P.I.]
    Collaborators: J. Zerubia (INRIA), L. Blanc-Féraud (INRIA)

    We develop a Bayesian approach to infer the parameters of both blur and noise from remote sensing images. The modulation transfer function (MTF) of the imaging system is modeled by a parametric function with a small number of parameters. The noise is assumed to be white, additive and Gaussian. Both blur and noise processes are supposed to be stationary. To constrain this ill-posed inverse problem, the unknown scene is modeled by a scale-invariant stochastic process governed by a fractal exponent and a global energy term.
    The main novelty consists of treating all parameters as random variables whose probability density function is inferred within a fully Bayesian framework. Thus, their uncertainties are provided as well as their optimal values. The chosen approach can be summarized as the computation of marginal distributions related to the useful parameters only. This requires integrating the joint pdf with respect to all the nuisance parameters, which is achieved through Laplace approximations.
    In addition, we investigate several schemes for model assessment and comparison, in order to validate this approach on real images and to propose further improvements.
    CorrNoiseWaterSegmentOct 1999-Jun 2003
    Multiscale Markov Modeling for Segmentation and Nautical Chart Update
    Keywords: Unsupervised segmentation, Markovian quadtree, Generalized Gaussian model, SPOT, multispectral data, bathymetry
    Input image type: multispectral, single image

    Participant: C. Collet [P.I.]
    Collaborators: J-N. Provost (INSA), P. Pérez (IRISA), P. Rostaing (UBO), P. Bouthemy (IRISA)
    Funding: EPSHOM

    We have developed an unsupervised method to segment multispectral images corrupted by a correlated non-Gaussian noise. The efficiency of the proposed Markovian quadtree-based method has been illustrated on satellite image segmentation tasks with multispectral observations, in order to update nautical charts.
    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 (ICE) procedure. Generalized Gaussian (GG) 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.
    Our segmentation method has been successfully applied to SPOT multispectral images. Within each segmented region, a bathymetric inversion model is then estimated to recover the water depth map. Experiments on several real images have demonstrated the efficiency of the whole process and the accuracy of the obtained results has been assessed using ground truth data.
    MissingMultiSegmentEOct 1998-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

    Participant: C. Collet [P.I.]
    Collaborators: J-N. Provost (INSA), P. Rostaing (UBO), P. Pérez (IRISA), P. Bouthemy (IRISA)
    Funding: EPSHOM

    This project deals with the unsupervised segmentation of multiband satellite 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 SPOT multispectral images, 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.

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