Placental Uric Acid Transport System: Glucose Transporter 9 (SLC2A9)

Placental Uric Acid Transport System: Glucose Transporter 9 (SLC2A9). INTRODUCTION: Pre-eclampsia, a pregnancy-specific disease, contributes substantially to perinatal morbidity and mortality of both the mother and her child. Pre-eclampsia is often associated with high maternal urate serum levels, which in turn has been shown to play a role in the pathogenesis of this disease. The aim of this study was to investigate the glucose transporter GLUT9-mediated placental uric acid transport system. METHODS: In this study western blot, immunofluorescence techniques as well as a transepithelial transport (Transwell) model were used to assess GLUT9 protein expression and, respectively, uric acid transport activity. Electrophysiological techniques and transmission electron microscopy (TEM) were used to characterize the properties and the structure of GLUT9. RESULTS: Uric acid is transported across a BeWo choriocarcinoma cell monolayer with 530 pmol/min. We could successfully overexpress and for the first time purify the GLUT9b isoform using the Xenopus laevis oocytes expression system. Chloride seems to modulate the urate transport system. TEM revealed that GLUT9b isoform is present as monomer and dimmer in the Xenopus laevis overexpression model. A class average of all the particles allowed us to develop a first model of human GLUT9b structure, which was derived from the published crystal structure of the bacterial homologue of GLUT1-4. CONCLUSIONS: In vitro the “materno-fetal” transport of uric acid is slow indicating that in vivo the fetus might be protected from short-term fluctuations of maternal urate serum levels. The low-resolution structure obtained from TEM validates the proposed homology model regarding the structure of human GLUT9b. In ongoing studies this model is used to perform virtual screening to identify novel modulators of the urate transport system enabling the development of novel therapies in pregnancy complications.

The dust environment of comet 67P/Churyumov-Gerasimenko from Rosetta OSIRIS and VLT observations in the 4.5 to 2.9 AU heliocentric distance range inbound

Context. The ESA Rosetta spacecraft, currently orbiting around cornet 67P/Churyumov-Gerasimenko, has already provided in situ measurements of the dust grain properties from several instruments, particularly OSIRIS and GIADA. We propose adding value to those measurements by combining them with ground-based observations of the dust tail to monitor the overall, time-dependent dust-production rate and size distribution. Aims. To constrain the dust grain properties, we take Rosetta OSIRIS and GIADA results into account, and combine OSIRIS data during the approach phase (from late April to early June 2014) with a large data set of ground-based images that were acquired with the ESO Very Large Telescope (VLT) from February to November 2014. Methods. A Monte Carlo dust tail code, which has already been used to characterise the dust environments of several comets and active asteroids, has been applied to retrieve the dust parameters. Key properties of the grains (density, velocity, and size distribution) were obtained from. Rosetta observations: these parameters were used as input of the code to considerably reduce the number of free parameters. In this way, the overall dust mass-loss rate and its dependence on the heliocentric distance could be obtained accurately. Results. The dust parameters derived from the inner coma measurements by OSIRIS and GIADA and from distant imaging using VLT data are consistent, except for the power index of the size-distribution function, which is alpha = -3, instead of alpha = -2, for grains smaller than 1 mm. This is possibly linked to the presence of fluffy aggregates in the coma. The onset of cometary activity occurs at approximately 4.3 AU, with a dust production rate of 0.5 kg/s, increasing up to 15 kg/s at 2.9 AU. This implies a dust-to-gas mass ratio varying between 3.8 and 6.5 for the best-fit model when combined with water-production rates from the MIRO experiment.