The Planetary Laboratory for Image Analysis (PLIA)

Hueso, R.; Legarreta, J.; Rojas, J. F.; Peralta, Javier; Pérez‐Hoyos, S.; Río‐Gaztelurrutia, T. del; Sánchez‐Lavega, A.

doi:10.1016/j.asr.2010.05.016

Cited by 40 publications

(21 citation statements)

References 39 publications

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“…After the contrast enhancement implied by the convolution kernel the images were mapped into cylindrical or polar projections depending on the geometry of the observation. For image processing and projection we used the software PLIA (Hueso et al, 2010). Fig.…”

Section: Methodsmentioning

confidence: 99%

Six years of Venus winds at the upper cloud level from UV, visible and near infrared observations from VIRTIS on Venus Express

Hueso

Peralta

Garate-Lopez

et al. 2015

Planetary and Space Science

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Section: Methodsmentioning

confidence: 99%

Six years of Venus winds at the upper cloud level from UV, visible and near infrared observations from VIRTIS on Venus Express

Hueso

Peralta

Garate-Lopez

et al. 2015

Planetary and Space Science

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“…Ground-based observations and HST and Cassini ISS images were navigated for limb position and features location with software LAIA and PLIA5960. We used three different techniques to retrieve wind speeds: Cloud-tracking of individual features; Latitudinal correlation of longitudinal brightness patterns; Supervised two-dimensional brightness correlation6162.…”

Section: Methodsmentioning

confidence: 99%

An enduring rapidly moving storm as a guide to Saturn’s Equatorial jet’s complex structure

et al. 2016

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Saturn has an intense and broad eastward equatorial jet with a complex three-dimensional structure mixed with time variability. The equatorial region experiences strong seasonal insolation variations enhanced by ring shadowing, and three of the six known giant planetary-scale storms have developed in it. These factors make Saturn's equator a natural laboratory to test models of jets in giant planets. Here we report on a bright equatorial atmospheric feature imaged in 2015 that moved steadily at a high speed of 450 ms−1 not measured since 1980–1981 with other equatorial clouds moving within an ample range of velocities. Radiative transfer models show that these motions occur at three altitude levels within the upper haze and clouds. We find that the peak of the jet (latitudes 10° N to 10° S) suffers intense vertical shears reaching +2.5 ms−1 km−1, two orders of magnitude higher than meridional shears, and temporal variability above 1 bar altitude level.

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“…All images were navigated and processed using the software PLIA (Hueso et al, 2010). The software uses the approximate predicted pointing extracted from the SPICE C-kernels (Acton, 1995) to navigate the images.…”

Section: Image Calibration Navigation and Measurement Errorsmentioning

confidence: 99%