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Last name: SLEZAK
First name: E.
Astronomy and Astrophysics, 472, pp. 29-49, http://dx.doi.org./10.1051/0004-6361:7150
Context: Galaxy clustering shows segregation effects with galaxy type, color and luminosity, which bring clues on the relationship with the underlying density field. Aims: We explore these effects among the populations of giant and dwarf galaxies detected in the ESO-Sculptor survey. Methods: We calculate the spatial two-point auto and...
We address the problem of joint signal restoration and parameter estimation in the context of the forthcoming MUSE instrument, which will provide spectroscopic measurements of light emitted by very distant galaxies. Restoration of spectra is formulated as a linear inverse problem, accounting for the instrument response and the noise spectral...
We address the problem of joint signal restoration and parameter estimation in the context of the forthcoming MUSE instrument, which will provide spectroscopic measurements of light emitted by very distant galaxies. Restoration of spectra is formulated as a linear inverse problem, accounting for the instrument response and the noise spectral...
Statistical Methodology, 5, pp. 361-372, http://dx.doi.org./10.1016/j.stamet..02.002
Astronomy and Astrophysics, 506, pp. 637-645 (2009)
Advances in Space Research, 36, pp. 650-655, http://dx.doi.org./10.1016/j.asr..01.104
We introduce a new multiscale restoration algorithm for images with few photons counts and its use for denoising XMM data. We use a thresholding of the wavelet space so as to remove the noise contribution at each scale while preserving the multiscale information of the signal. Contrary to other algorithms the signal restoration process is the...
International audience
In the framework of the hierarchical model of structure formation, galaxy clusters form through the accretion and merging of substructures of smaller mass. Our goal is to characterize the physics and dynamics of these processes through the study of merging clusters. For this purpose we have built a sample of 10 low--redshift clusters viewed at...
Accurate knowledge of the morphology of halos and its evolution are key constraints on the galaxy formation model as well as a determinant parameter of the strong-lensing phenomenon. Using the cosmological hydrodynamic simulation, the Evolution and Assembly of GaLaxies and their Environments (EAGLE), we aim to provide a comprehensive analysis...
We present the analysis and results of a new VRI photometric and spectroscopic survey of the central ∼1.8×1.2 Mpc 2 region of the galaxy cluster A3921 (z = 0.094). We detect the presence of two dominant clumps of galaxies with a mass ratio of ∼5: a main cluster centred on the Brightest Cluster Galaxy (BCG) (A3921-A), and an NW sub-cluster...
Started in 2005 in the frame of the french Action Spécifique Observatoire Virtuel, the aim of the Workflow Working Group is to provide Workflow use cases in several domains (image, spectrum, etc.) and to improve them with VO (or other) existing tools. Another important point is to develop collaborations with people from the IT community (links...
The French Action Spécifique Observatoires Virtuels has created the Workflow Working Group in 2005. Its aim is to explore the use of the Workflow paradigm in the astronomical domain. The first consensus was the definition of a Workflow as a sequence of tasks realized in a controlled context (at various levels: intelligence in the choice of the...
International audience
Astronomy and Astrophysics, 460, pp. 381-391, http://dx.doi.org./10.1051/0004-6361:20053970
Science, 326, Issue 5958, pp. 1379-1382 (2009)
Astronomy and Astrophysics, 478, pp. 93-94, http://dx.doi.org./10.1051/0004-6361:20066088e
Astronomy and Astrophysics, 478, pp. 93-94, http://dx.doi.org./10.1051/0004-6361:20066088e
Astronomy and Astrophysics, 461, pp. 81-93, http://dx.doi.org./10.1051/0004-6361:20066088
Context. Large numbers of deep optical images will be available in the near future, allowing statistically significant studies of low surface brightness structures such as intracluster light (ICL) in galaxy clusters. The detection of these structures requires efficient algorithms dedicated to this task, which traditional methods find difficult...
Astronomy and Astrophysics, 447, pp. 133-144, http://dx.doi.org./10.1051/0004-6361:20052838
We have obtained wide field images of the Coma cluster in the B, V, R and I bands with the CFH12K camera at CFHT. In order to search for large scale diffuse emission, we have applied to these images an iterative multi scale wavelet analysis and reconstruction technique which allowed to model all the sources (stars and galaxies) and subtract...
We have obtained wide field images of the Coma cluster in the B, V, R and I bands with the CFH12K camera at CFHT. To search for large scale diffuse emission, we have applied to these images an iterative multiscale wavelet analysis and reconstruction technique which made it possible to model all the sources (stars and galaxies) and subtract them...