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Maria Vanrell, & Jordi Vitria. (1997). Optimal 3x3 decomposable disks for morphological transformations. Image and Vision Computing, 15(2): 845–854.
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Xavier Otazu, M. Gonzalez-Audicana, O. Fors, & J. Nuñez. (2005). Introduction of Sensor Spectral Response Into Image Fusion Methods. Application to Wavelet-Based Methods. IEEE Transactions on Geoscience and Remote Sensing, 43(10): 2376–2385 (IF: 1.627).
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Xavier Otazu, & Maria Vanrell. (2005). A surround-induction function to unify assimilation and contrast in a computational model of color apearance.
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Susana Alvarez, Xavier Otazu, & Maria Vanrell. (2005). Image Segmentation Based on Inter-Feature Distance Maps. In Frontiers in Artificial Intelligence and Applications, IOS Press, 131: 75–82.
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A. Richichi, O. Fors, M.T. Merino, Xavier Otazu, J. Nuñez, A. Prades, et al. (2006). The Calar Alto lunar occultation program: update and new results. Astronomy and Astrophysics (Section ’Stellar structure and evolution’), 445:1081–1088.
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Robert Benavente, Maria Vanrell, & Ramon Baldrich. (2006). A data set for fuzzy colour naming. Color Research & Application, 31(1):48–56.
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J. Nuñez, Xavier Otazu, & M.T. Merino. (2005). A Multiresolution-Based Method for the Determination of the Relative Resolution between Images. First Application to Remote Sensing and Medical Images. International Journal of Imaging Systems and Technology, 15(5): 225–235 (IF: 0.439).
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Xavier Otazu, & Oriol Pujol. (2006). Wavelet based approach to cluster analysis. Application on low dimensional data sets. PRL - Pattern Recognition Letters, 27(14), 1590–1605.
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J. Nuñez, O. Fors, Xavier Otazu, Vicenç Pala, Roman Arbiol, & M.T. Merino. (2006). A Wavelet-Based Method for the Determination of the Relative Resolution Between Remotely Sensed Images. IEEE Transactions on Geoscience and Remote Sensing, 44(9): 2539–2548.
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Javier Vazquez, Maria Vanrell, Anna Salvatella, & Eduard Vazquez. (2007). A colour space based on the image content. In Artificial Intelligence Research and Development, C. Angulo and L. Godo, pp 205–212 IOS Press.
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Xavier Otazu, Maria Vanrell, & C. Alejandro Parraga. (2007). Mutiresolution Wavelet Framework Reproduces Induction Effects. Perception 36:167–167, supp.
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C. Alejandro Parraga, Robert Benavente, & Maria Vanrell. (2007). Modeling Colour-Naming Space with Fuzzy Sets. Perception 36:198–198, supp.
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Xavier Otazu, Maria Vanrell, & C. Alejandro Parraga. (2008). Multiresolution Wavelet Framework Models Brightness Induction Effects. VR - Vision Research, 733–751.
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O. Fors, A. Richichi, Xavier Otazu, & J. Nuñez. (2008). A new wavelet-based approach for the automated treatment of large sets of lunar occultation data. Astronomy and Astrohysics, 297–304.
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Robert Benavente, Maria Vanrell, & Ramon Baldrich. (2008). Parametric Fuzzy Sets for Automatic Color Naming. Journal of the Optical Society of America A, 2582–2593.
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Partha Pratim Roy, Eduard Vazquez, Josep Llados, Ramon Baldrich, & Umapada Pal. (2008). A System to Segment Text and Symbols from Color Maps. In Graphics Recognition. Recent Advances and New Opportunities (Vol. 5046, pp. 245–256). LNCS.
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T. Widemann, & Xavier Otazu. (2009). Titanias radius and an upper limit on its atmosphere from the September 8, 2001 stellar occultation. International Journal of Solar System Studies, 199(2), 458–476.
Abstract: On September 8, 2001 around 2 h UT, the largest uranian moon, Titania, occulted Hipparcos star 106829 (alias SAO 164538, a V=7.2, K0 III star). This was the first-ever observed occultation by this satellite, a rare event as Titania subtends only 0.11 arcsec on the sky. The star's unusual brightness allowed many observers, both amateurs or professionals, to monitor this unique event, providing fifty-seven occultations chords over three continents, all reported here. Selecting the best 27 occultation chords, and assuming a circular limb, we derive Titania's radius: View the MathML source (1-σ error bar). This implies a density of View the MathML source using the value View the MathML source derived by Taylor [Taylor, D.B., 1998. Astron. Astrophys. 330, 362–374]. We do not detect any significant difference between equatorial and polar radii, in the limit View the MathML source, in agreement with Voyager limb image retrieval during the 1986 flyby. Titania's offset with respect to the DE405 + URA027 (based on GUST86 theory) ephemeris is derived: ΔαTcos(δT)=−108±13 mas and ΔδT=−62±7 mas (ICRF J2000.0 system). Most of this offset is attributable to a Uranus' barycentric offset with respect to DE405, that we estimate to be: View the MathML source and ΔδU=−85±25 mas at the moment of occultation. This offset is confirmed by another Titania stellar occultation observed on August 1st, 2003, which provides an offset of ΔαTcos(δT)=−127±20 mas and ΔδT=−97±13 mas for the satellite. The combined ingress and egress data do not show any significant hint for atmospheric refraction, allowing us to set surface pressure limits at the level of 10–20 nbar. More specifically, we find an upper limit of 13 nbar (1-σ level) at 70 K and 17 nbar at 80 K, for a putative isothermal CO2 atmosphere. We also provide an upper limit of 8 nbar for a possible CH4 atmosphere, and 22 nbar for pure N2, again at the 1-σ level. We finally constrain the stellar size using the time-resolved star disappearance and reappearance at ingress and egress. We find an angular diameter of 0.54±0.03 mas (corresponding to View the MathML source projected at Titania). With a distance of 170±25 parsecs, this corresponds to a radius of 9.8±0.2 solar radii for HIP 106829, typical of a K0 III giant.
Keywords: Occultations; Uranus, satellites; Satellites, shapes; Satellites, dynamics; Ices; Satellites, atmospheres
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Xavier Otazu, Maria Vanrell, & C. Alejandro Parraga. (2008). Colour induction effects are modelled by a low-level multiresolution wavelet framework. Perception 37(Suppl.): 107.
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