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La colitis eosinofílica es una patología gastrointestinal infrecuente que pertenece al grupo de las denominadas “enfermedades primarias eosinofílicas del tracto digestivo”. Existen 3 tipos: mucosa, transmural (muscular) y subserosa. Presentamos el caso de un paciente varón, de 23 años de edad, con cuadro clínico de dolor abdominal, náuseas, diarrea crónica y presentación de ascitis. Se descarta etiologías parasitarias y otras secundarias. La endoscopia digestiva alta no fue contributoria. Mediante colonoscopia se observa características de inflamación en el ileon distal y colon ascendente, cuyos hallazgos histológicos son compatibles con colitis eosinofílica. El estudio de líquido ascítico es sugestivo de ascitis eosinofílica. El paciente recibió tratamiento de inducción con prednisona a 40mg diarios por vía oral, lográndose remisión a las 2 semanas, continuando con terapia de mantenimiento a base de prednisona con retiro progresivo de la dosis. Se logra control de la enfermedad de manera exitosa.

Ferroelectric nanoparticles, due to their high non-linear optical response, are of considerable practical interest for their use as nanoprobes for the study of biological materials by multiphoton microscopy methods. To prevent toxic effects, it is necessary to modify the surface using biocompatible polymers. Here we report the results of the study on the effect of surface modification of BaTiO3 nanoparticles with hydrolyzed chitosan obtained from shrimp exoskeletons (Penaeus vannamei). It was found that increasing of the hydrolyzed chitosan concentration in the solution during surface modification from 1 to 3% leads to a significant reduction in nanoparticle agglomeration, while the intensity of the second harmonic generation changes insignificantly. Graphical abstract

Resumen Introduccion Los resultados de la reparacion de la hernia paraestomal (HP) basados en datos provenientes de registros son escasos. El objetivo del presente trabajo es analizar los datos recogidos sobre la HP en el Registro Nacional de Hernia Incisional (EVEREG) y asi evaluar las practicas actuales y resultados en la reparacion de una HP. Metodos Se analizan los datos de la cohorte de HP registradas en el periodo desde julio de 2012 hasta junio de 2018. Se analizan las complicaciones, recidivas y factores asociados a ellas de la cohorte completa de HP, independientemente del tipo de estoma al que se asocian. Posteriormente, se realiza el mismo analisis del grupo de HP con relacion a una colostomia (grupo mas numeroso). Resultados Se estudiaron 353 HP. De estas, 259 (73%) fueron HP en el contexto de una colostomia terminal, 74 (21%) en el de una ileostomia terminal y 20 (6%) en el de una ureteroileostomia (Bricker). La edad media global fue de 68,7 ± 11,1 anos y 135 (38%) pacientes fueron del sexo femenino. El abordaje abierto y la cirugia electiva fueron predominantes (78% y 92%, respectivamente). El 99% se reparo con una malla sintetica no absorbible. Las complicaciones postoperatorias globales fueron altas (30,6%), asi como la recurrencia global (27,5%) tras un seguimiento medio de 9,4 meses. Conclusiones La reparacion de la HP es poco frecuente comparada con el conjunto de reparaciones de la hernia incisional. La cirugia de la HP parece relacionarse con un porcentaje elevado de complicaciones postoperatorias y recidiva.

An upward transport of water via the Hadley cell has been suggested as one of the mechanisms to transport water vapor to the upper atmosphere [Shaposhnikov et al., 2019], which would enhance the hydrogen escape on Mars [cf. Chaffin et al., 2017]. Carbon monoxide is one of the tracers which can measure the dynamics in the Martian atmosphere because CO distribution is a combination of photochemistry and dynamics. Above ~60 km altitude, the CO mixing ratio increases with altitude due to the production from photodissociation of CO2 and is further enhanced around the polar regions because of downwelling from the thermosphere [Daerden et al., 2019; Holmes et al., 2019; Olsen et al., 2021; Yoshida et al., accepted]. In the lower atmosphere, CO is recycled to CO2 by the catalytic cycle by odd hydrogen. The photochemical lifetime of CO is too slow, and then its lifetime is ~6 years in the lower atmosphere [Krasnopolsky, 2007]. Thus, seasonal variation of CO in the lower atmosphere is a consequence of CO2 sublimation/condensation at the polar cap [Encrenaz et al., 2006; Smith et al., 2009, 2021]. In addition, transport of rich CO atmosphere from southern to northern hemispheres during Ls = 90 – 180 has been measured by Smith et al. (2008, 2018) as predicted due to the breaking of the polar vortex by the GCM model. Although the vertical distribution of CO VMR is an index to determine the condensation of CO2, photochemistry, and dynamics, there is no direct comparison between measurements and simulations because we did not obtain the CO vertical distribution before the Trace Gas Orbiter (TGO) ExoMars mission. To clarify the vertical and horizontal transport of CO in the Martian atmosphere, we investigate the CO VMR retrieved from the solar occultation (SO) channel of Nadir and Occultation for MArs Discovery (NOMAD) instrument aboard TGO [Vandaele et al., 2018].The SO channel operates at wavenumbers from 2325.6 to 4347.8 cm-1 with relatively high spectral resolution (R = 17,000). CO (2-0) band spectra features between 3970.7 and 4360.1 cm-1 are measured regularly in orders 186 to 191 of the instrument. We retrieved CO number densities using CO spectra features in orders 186 to 191 and radiative transfer code, ASIMUT [Vandaete et al., 2006], based on the Optimal Estimation Method [Rogers, 2006]. ASIMUT was performed for each spectrum at each tangential altitude independently [e.g., Aoki et al., 2019]. The latest updated instrument calibrations [Villanueva et al., submitted; Thomas et al., 2022] have been applied. We used the GEM-Mars model temperature and CO2 profiles [Neary et al., 2018; Daerden et al., 2019] to derive the CO VMR. The CO spectra were investigated from April 2018 to September 2021, corresponding from MY 34 Ls ~ 150 to MY 36 Ls ~ 105. The total number of dataset is 31,000.Firstly, we found that the retrieved CO VMR in orders 187 to 191 does not correspond to that in order 186 below ~60 km altitude. The CO VMR derived from orders 187 to 191 is underestimated. The strongest 2-0 band of CO is located at 4288.3cm-1, which corresponds to order 190, and it saturates around ~60 km. The saturation of CO lines would be related to the underestimation of CO VMR. When we tested the retrieval sensitivity of saturated lines in order 186, the underestimation of CO VMR also appears below 40 km altitude in the case that we perform the ASIMUT using the entire wavenumber range of order 186 (4179.0 – 4212.2 cm-1) compared with using a partial wavenumber range, 4189.0 – 4198.0 cm-1, of order 186. To avoid the underestimation of CO VMR, the retrieved CO VMR derived from CO spectra in the orders 187 – 191 is limited between 60 and ~110 km altitude, that from CO spectra in order 186 is limited between 40 and ~110 km, and that from CO spectra in 4189.0 – 4198.0 cm-1 is limited between the near-surface to 40 km altitude.The retrieved CO VMR distributes from 300 to ~5000 ppm. In the polar regions, the CO VMR increases above ~40 km and reaches 4000 ppm at 70 km, which is attributed to the production of CO from photodissociation of CO2 and transport of CO-enriched air via meridional circulation [Daerden et al., 2019]. That is consistent with the results measured by the Atmospheric Chemistry Suite aboard TGO [Olsen et al., 2021]. In the lower atmosphere, the enriched CO VMR up to ~3500 ppm appears from 90 to 200 in Ls in the southern hemisphere, which would be attributed to the CO2 condense in the southern winter season. We will report the CO distribution in more detail while distinguishing the dataset into season and latitude along with altitude.

The D/H ratio is a key parameter to understand the atmospheric evolution of a planet. On Mars a D/H ~ 5 times larger than the ratio on Earth is measured. This large ratio can be explained by a preferential escape of the hydrogen compared to the deuterium due to its lower mass. However, while the thermal escape (Jeans escape) is strongly mass dependent other non-thermal processes are less mass dependent and would impact the time needed to fractionate the water from the terrestrial value to the current value. After the first detections of the deuterium Lyman-α emission from Earth (Bertaux et al. 1992, Krasnopolsky et al. 1998), the mission MAVEN performed the first systematic observations of the atomic deuterium Lyman-α emission around Mars showing a brightness of several hundreds of Rayleigh near Mars winter solstice (Clarke et al. 2017, Mayyasi et al. 2017), much larger than the Earth detections done near aphelion (~ 20 – 50 Rayleighs). This seasonal variation of the deuterium Lyman-α brightness is consistent with the variations of the hydrogen Lyman-α brightness observed from Mars Express (Chaffin et al. 2014, Chaufray et al. 2021), HST (Clarke et al. 2014), and MAVEN/IUVS (Clarke et al. 2017, Chaffin et al. 2018) and should result from the processes transporting the water vapor from the lower atmosphere to the upper atmosphere (Vals et al. 2022). In this work we will present preliminary simulations of the 3D deuterium abundance in the Martian upper atmosphere (Fig. 1) using a 3D time dependent global circulation model, including the chemical reactions between HD and HDO with the ions in the upper atmosphere, its extension in the exosphere, and a comparison of the simulated D Lyman-α brightness with the brightness measured by MAVEN/IUVS (Mayyasi et al. 2017) for the Martian year 33. Fig. 1 Simulated average dayside and nightside D density at different altitudes in the thermosphere and exosphere along one Martian year. We will also present first results of the simulated non-thermal escape of H and D produced by collisions between hot oxygen with H, D, H2 and HD as well as the escape of planetary H+ and D+ driven by the solar wind interaction. We will compare the D and H thermal escape rate with the non-thermal escape rates. References: Bertaux et al. (1992), in ESOC conference and workshop proceedings, 44, 459. Chaffin, M. et al. (2014), Geophys. Res. Lett., 41, 314-320 Chaffin, M. et al. (2018), J. Geophys. Res., 123, 2192-2210 Chaufray et al., (2021), Icarus, 353,113498 Clarke et al. (2014), Geophys. Res. Lett., 41, 8013-8020 Clarke et al. (2017), J. Geophys. Res., 122, 2336-2344 Krasnopolsky et al., (1998), Science, 280, 1576 Mayyasi et al., (2017), J. Geophys. Res., 122, 10811-10823 Vals et al. (2022), J. Geophys. Res., under revisions

Introduction The large enrichments of D/H currently measured in atmospheric water suggest that a large fraction, beyond 80%, of this water was lost over time1,2, and Ar and O isotopic ratios measured with MAVEN3 and TGO4 indicate Mars has lost a large fraction of its atmosphere. As we attempt to trace back the history of water on Mars, it is unknown how much water remains locked in non-labile/sub-surface reservoirs, and an important question is whether all current labile reservoirs have evolved in the same way and undergone extensive exchange. New measurements with TGOWe have analyzed data over the entirety a Martian year as measured with TGO/NOMAD, which probed the release of water from the two polar caps using the instrument’s solar occultation mode. Specifically, the measurements presented here have been collected by the NOMAD10 instrument suite onboard TGO. The data were collected employing the Solar Occultation (SO) channel/mode of the instrument. Interpretation and extraction of molecular abundances from the calibrated data is done by employing the Planetary Spectrum Generator (PSG, https://psg.gsfc.nasa.gov)11, and as reported in 12. The model employs a layer-by-layer line-by-line method in a spherical and refractive geometry. We employ the latest linelists for H2O, HDO, and CO2 as compiled in the HITRAN-2020 database13, which are complemented to include the latest H2O and HDO broadening coefficients for a CO2 atmosphere14,15. Probing the seasonal release from both capsDuring Martian Year 34, the planet was engulfed in a global dust storm (GDS) that greatly perturbed the temperature and vertical structure of the Martian atmosphere. In addition, the lingering effects of the GDS were joined by a large regional dust storm that started during late southern summer (LS 320). These two major events greatly affected the climate of Mars, primarily leading to a strong increase in atmospheric temperature, a substantial rise in altitude of the hygropause, and subsequent transport of water to unexpectedly high altitudes16–22. Interestingly, during the GDS when the northern hemisphere was in the winter season, the climate was substantially warmer there than normal23–25, leading to high-altitude water also in the northern hemisphere. Typically, the largest seasonal water columns are observed during summer in the northern hemisphere26, and that may be true in MY35, but the vertical profile of water is highly compact (confined to altitudes below 20 km), even at the peak of northern summer (LS 90-130). In all cases (all seasons and regions of the planet) the D/H declines quickly above the hygropause, from a nominal value above 5 VSMOW to a very low value near Discussions and conclusionsThe new results presented here, which probe the vertical profiles of water and D/H for both seasonal caps, together with previous ground-based and orbital measurements, suggest a common and highly enriched value for this labile reservoir of water. Atmospheric D/H behaves as an integrator of the differential individual atomic (H and D) escape rates, and therefore without any new supply of water into the system, the D/H of the labile sources will continue to increase. Among other phenomena, the chaotic changes in obliquity that Mars has experienced, and the corresponding impact on climate and regions of ice stability28,29, could lead to large exchanges between the reservoirs and further homogenization of the D/H across the planet. Thus, the D/H value of the polar caps could be similar to the modern labile D/H value observed in the seasonal releases. References1. Jakosky, B. M. Annual Review of Earth and Planetary Sciences 49, 71–93 (2021).2. Villanueva, G. L. et al.. Science 348, 218–221 (2015).3. Jakosky, B. M. et al. Science (2017) doi:10.1126/science.aai7721.4. Alday, J. et al. JGR: Planets 126, e2021JE006992 (2021).5. Scheller, E. L., et al. Science 372, 56–62 (2021).6. Plaut, J. J. et al. Science 316, 92 (2007).7. Zuber, M. T. et al. Science 282, 2053 (1998).8. Byrne, S. & Murray, B. C. JGR: Planets 107, 11-1-11–12 (2002).9. Fishbaugh, K. E. & Head, J. W. Icarus 174, 444–474 (2005).10. Vandaele, A. C. et al. Planetary and Space Science 119, 233–249 (2015).11. Villanueva, G. L., et al. JQSRT 217, 86–104 (2018).12. Villanueva, G. L. et al. Science Advances (2021) doi:10.1126/sciadv.abc8843.13. Gordon, I. E. et al. JQSRT 107949 (2022) doi:10.1016/j.jqsrt.2021.107949.14. Devi, V. M. et al. JQSRT 187, 472–488 (2017).15. Régalia, L. et al.JQSRT 231, 126–135 (2019).16. Aoki, S. et al. JGR: Planets 124, 3482–3497 (2019).17. Belyaev, D. A. et al. GRL 48, e2021GL093411 (2021).18. Chaffin, M. S. et al. Nat Astron 5, 1036–1042 (2021).19. Heavens, N. G. et al. Nature Astronomy 2, 126–132 (2018).20. Holmes, J. A. et al. Earth and Planetary Science Letters 571, 117109 (2021).21. Neary, L. et al. GRL 47, e2019GL084354 (2020).22. Stone, S. W. et al. Science (2020) doi:10.1126/science.aba5229.23. Daerden, F. et al. JGR: Planets n/a, e2021JE007079 (2022).24. Montabone, L. et al. JGR: Planets 125, e2019JE006111 (2020).25. Rossi, L. et al. GRL 48, e2020GL090962 (2021).26. Crismani, M. M. J. et al. JGR: Planets 126, e2021JE006878 (2021).27. Laskar, J. et al. Icarus 170, 343 (2004).28. Jakosky, B. M., Henderson, B. G. & Mellon, M. T. JGR: Planets 100, 1579–1584 (1995).29. Levrard, B., Forget, F., Montmessin, F. & Laskar, J. JGR: Planets 112, (2007).

The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) has been designed to investigate the composition of Mars' atmosphere, with a particular focus on trace gases, clouds, and dust. The instrument probes the ultraviolet and infrared regions covering large parts of the 0.2-4.3 µm spectral range [1,2], with 3 spectral channels: a solar occultation channel (SO – Solar Occultation; 2.3–4.3 μm), a second infrared channel capable of nadir, solar occultation, and limb sounding (LNO – Limb Nadir and solar Occultation; 2.3–3.8 μm), and an ultraviolet/visible channel (UVIS – Ultraviolet and Visible Spectrometer, 200–650 nm). NOMAD performs solar occultation, nadir and limb observations dedicated to the determination of the composition and the structure of the Martian atmosphere. TGO started its science phase in April 2018 and instruments have now been accumulating data for more than two Martian years. We will present selected results obtained by the NOMAD instrument covering the atmosphere composition with observations of several trace gases, dust, and clouds. We also report on the different discoveries highlighted by the instrument by pointing to a series of contributions to this conference that will present in detail several specific studies, like recent progress in the instrument calibration, the latest CO2 and temperature vertical profiles, studies of aerosol nature and distribution, water vapor profiles and variability, carbon monoxide vertical distribution, ozone vertical profiles, climatology and relation with water, airglow observations, detection of CO2 ice clouds, surface ices and in general advances in the analysis of the spectra recorded by the three channels of NOMAD. References [1] Vandaele, A.C., et al., 2015. Planet. Space Sci. 119, 233-249. [2] Vandaele et al., 2018. Space Sci. Rev., 214:80, doi.org/10.1007/s11214-11018-10517-11212.

The effect of magnetic field of 0.3 T on the concentration, distribution of sizes in suspension and zeta potential of colloidal gold and colloidal silver nanoparticles, obtained by considering the pulsed laser ablation in double distilled water was studied. The magnetic field was transverse to the direction of incidence of the laser radiation and parallel to the surface of a submerged target. An Nd: YAG laser was used (1064 nm in wavelength, 10 ns in duration, repetition rate of 10 Hz and 37 mJ of energy) to ablate targets. The colloids were characterized by inductively coupled plasma optical emission spectroscopy, ultraviolet-visible spectroscopy, dynamic light scattering and zeta potential. Concentration analysis suggested that applying magnetic field of 0.3 T during nanoparticle synthesis leads to higher concentration. Applying magnetic field led to an eleven percent increase in the concentration of the colloid with gold nanoparticles and a five percent increase in the concentration of the colloidal silver nanoparticles. The absorption spectra suggested the presence of spherical nanoparticles. When analyzing the effect of the magnetic field on the hydrodynamic size distribution of the nanoparticles and the zeta potential of the colloids, no significant changes were evidenced. The magnetic confinement of the plasma induced by laser ablation caused changes in the characteristics of the colloids.

The prevalence of mental health problems during childhood and adolescence is on the rise. There is a growing interest in the examination of personal variables that may function as risk factors and that may be targeted for effective intervention. This study explores the relationships amongst different aspects of psychological inflexibility (one, typically studied, focusing on the individual’s responding to unwanted emotions and cognitions, and another, more recently explored, focusing on the individual’s responding to desired thoughts and affective states), emotional intelligence, and mental health symptoms. A total of 129 school-going children (mean age: 11.16 years old) completed a battery of instruments comprising the Avoidance and Fusion Questionnaire-Youth (AFQ-Y17), the Experiential Approach Scale (EAS), the Emotional Intelligence Quotient Inventory (EQi-YV), and the Revised Child Anxiety and Depression Scale (RCADS-30). Results showed that both the AFQ-Y17 score and an EAS subscale score (Anxious Clinging) were significant independent predictors of mental health symptoms in general. Emotional intelligence was predictive only for depression, and both the AFQ-Y17 and the Anxious Clinging EAS subscale significantly incremented the predictive power of a hierarchical linear regression model including all three variables. These results underscore the relevance of psychological inflexibility for child/adolescent mental health, and the need to further explore a specific aspect of inflexibility regarding positive emotions and other appetitive private events.

In response to the publication "Acute appendicitis, foreign bodies and COVID-19 vaccination: correspondence", we reviewed the association between acute surgical abdomen and COVID-19 vaccination.

Acceptance and commitment therapy (ACT) is an effective treatment for chronic pain conditions. ACT seeks to produce clinical change by enhancing Psychological Flexibility (PF). This exploratory (feasibility and preliminary effectiveness) study presents a pilot application of an online ACT group intervention for fibromyalgia (FM) with an extensive Experiential Sampling (ES) assessment of outcome and process variables via smartphone.5-weekly ACT online group sessions were applied to 9 female FM patients. Questionnaire-based assessments of several clinical outcomes and PF processes were conducted pre- and post-intervention, and at 6-month follow-up. Extensive (6 weeks pre- and 6 weeks post-intervention) smartphone-delivered ES was implemented to gather process and outcome data in the patients' usual contexts. Clinically significant change was evaluated both at the group level and individually.This treatment format appears to be feasible and acceptable to participants, with good adoption and completion rates (75 %) and excellent rates of treatment completion and clinical adherence (100 %). Participants showed significant reductions in affective pain, distress and biopsychosocial impact of FM both post-intervention and at 6-month follow-up (as measured with questionnaires), as well as significant improvements in satisfaction with actions and emotional discomfort (as measured through ES). Multilevel regression analyses indicated that PF-related processes assessed through ES had a significant impact on clinical outcomes and predicted the impact of FM at the 6-month follow-up.A brief online group ACT intervention for FM was both feasible and acceptable to participants. Also, there was preliminary evidence of effectiveness in enhancing pain-related PF and producing clinical benefits in FM.

Idiopathic myointimal hyperplasia of the mesenteric veins (IMHMV) is an uncommon cause of intestinal ischemia. It was firstly described by Genta and Haggit in 1991. Only a few cases have been reported and it is difficult to know the true incidence.

Background and purpose: The transient receptor potential vanilloid 4 (TRPV4) cation channel participates in multiple physiological processes and is also at the core of different diseases, making this channel an interesting pharmacological target with therapeutic potential. However, little is known about the structural elements governing its inhibition. Experimental approach: We have now combined in silico drug discovery and molecular dynamics simulation based on Xenopus tropicalis xTRPV4 structure with functional studies measuring cell Ca2+ influx mediated by human TRPV4 channel to characterize the binding site of known TRPV4 inhibitors and to identify novel small molecule channel modulators. Key results: We have found that the inhibitor HC067047 binds to a pocket conformed by residues from S2-S3 linker (xTRPV4-D542), S4 (xTRPV4-M583 and Y587 and S5 (xTRPV4-D609 and F613). This pocket was also used for structure-based virtual screening in the search of novel channel modulators. Forty potential hits were selected based on the lower docking scores (from ~250,000 compounds) and their effect upon TRPV4 functionally tested. Three were further analysed for stability using molecular dynamics simulation and functionally tested on TRPV4 channels carrying mutations in the binding pocket. Compound NSC151066, shown to require residue xTRPV4-M583 for its inhibitory effect, presented an IC50 of 145 nM and demonstrated to be an effective antiviral against Zika virus with a potency similar to HC067047. Conclusion and implications: Together, we propose structural insights into the inhibition of TRPV4 and how this information can be used for the design of novel channel modulators. We thank Dr. Andres Merits (University of Tartu, Estonia) for kindly providing the plasmid encoding the ZIKV with NanoLuc, Spanish Ministry of Economy and Competitiveness through grants RTI2018‐099718 (to M.A.V.) and BFU2016‐80039‐R (to J.D.), an institutional “Unidad de Excelencia María de Maeztu” CEX2018‐000792‐M and FEDER funds. F.G.‐N. thanks Fondecyt Regular projects 1170733, the US Army of USA, W911NF‐14‐1‐0520 and The Centro Interdisciplinario de Neurociencia de Valparaíso is a Millennium Institute supported by the Millennium Scientific Initiative of the Ministerio de Economía, Fomento y Turismo P029‐022‐F.

Data de publicació electrònica: 02-11-2022 Cells respond to physical stimuli, such as stiffness1, fluid shear stress2 and hydraulic pressure3,4. Extracellular fluid viscosity is a key physical cue that varies under physiological and pathological conditions, such as cancer5. However, its influence on cancer biology and the mechanism by which cells sense and respond to changes in viscosity are unknown. Here we demonstrate that elevated viscosity counterintuitively increases the motility of various cell types on two-dimensional surfaces and in confinement, and increases cell dissemination from three-dimensional tumour spheroids. Increased mechanical loading imposed by elevated viscosity induces an actin-related protein 2/3 (ARP2/3)-complex-dependent dense actin network, which enhances Na+/H+ exchanger 1 (NHE1) polarization through its actin-binding partner ezrin. NHE1 promotes cell swelling and increased membrane tension, which, in turn, activates transient receptor potential cation vanilloid 4 (TRPV4) and mediates calcium influx, leading to increased RHOA-dependent cell contractility. The coordinated action of actin remodelling/dynamics, NHE1-mediated swelling and RHOA-based contractility facilitates enhanced motility at elevated viscosities. Breast cancer cells pre-exposed to elevated viscosity acquire TRPV4-dependent mechanical memory through transcriptional control of the Hippo pathway, leading to increased migration in zebrafish, extravasation in chick embryos and lung colonization in mice. Cumulatively, extracellular viscosity is a physical cue that regulates both short- and long-term cellular processes with pathophysiological relevance to cancer biology. This work was supported in part by R01 CA257647 (to K.K. and D.M.G.), R01 GM134542 (to S.X.S. and K.K.), NSF 2045715 (to Y.L.), R01 AR071976 (to C.-M.F. and J.T.), R01 AR072644 (to C.-M.F. and J.T.) and R01 CA054358 (to A.P.F.), the Spanish Ministry of Science, Education and Universities through grants RTI2018 099718-B-100 (to M.A.V.) and an institutional “Maria de Maeztu” Programme for Units of Excellence in R&D and FEDER funds (to M.A.V.), and postdoctoral fellowships from the Fonds de recherche du Quebec—Nature et technologies and the Natural Sciences and Engineering Research Council of Canada (to A.K.). The opinions, findings and conclusions, or recommendations expressed are those of the authors and do not necessarily reflect the views of any of the funding agencies.

NGIMS data sets used in this paper are available on the Planetary Data System (http://pds-atmospheres.nmsu.edu/data_ and_services/atmospheres_data/MAVEN/ngims.html) as well as EUV data sets (https://pds-ppi.igpp.ucla.edu/search/view/?f=yes&id=pds://PPI/maven.euv.modelled). Data cubes containing M-GITM simulations used in this paper can be found on the University of Michigan Deep Blue repository (http://doi.org/10.7302/85qt-e980)., Using a new observational technique, the NGIMS (Neutral Gas and Ion Mass Spectrometer) instrument on the MAVEN (Mars Atmosphere and Volatile Evolution) spacecraft has the unique capability to measure horizontal thermospheric winds. Measured along the orbit track from periapsis (∼150 km) to ∼200 km, these are the first in situ observations of thermospheric winds at Mars. Significantly, this also means that simulated winds from a global circulation model can be compared to in situ observations from this part of the Martian atmosphere for the first time. In this study, observations from five NGIMS neutral wind campaigns have been compared to simulations from the Mars Global Ionosphere-Thermosphere Model (M-GITM), a ground to exosphere 3-D general circulation model. By comparing NGIMS neutral wind observations to model simulations, the processes driving the winds and their variations in the upper atmosphere are examined. These comparisons show that for certain observational periods, the M-GITM simulated winds can generally replicate the magnitude and/or direction of the NGIMS wind observations, while in others, significant differences occur. In general, wind observations from NGIMS campaigns with large orbit-to-orbit variability are not well replicated by M-GITM, while campaigns with higher observed wind speeds are better captured by the model. Additionally, using these data-model comparisons, the relative role of normal solar forcing and corresponding differential heating in driving thermospheric winds at Mars is found to be variable, likely acting as the primary driver under some conditions and secondary to other physical processes under others.©2019. American Geophysical Union. All Rights Reserved., Funding support for this research was provided by the MAVEN project, Grant NNH10CC04C. This work was also supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program - Grant 80NSSC18K1238. Funding for F. Gonzalez-Galindo and M. A. Lopez-Valverde was provided by the Spanish National Research Council under intramural project CSIC 201450E022

This is an open access article under the terms of the Creative Commons Attribution-NonCommercial-NoDerivs License, which permits use and distribution in any medium, provided the original work is properly cited, the use is non-commercial and no modifications or adaptations are made., We present observations of terminator CO2 ice clouds events in three groups: Equatorial dawn, Equatorial dusk (both between 20°S and 20°N) and Southern midlatitudes at dawn (45°S and 55°S east of Hellas Basin) with ESA ExoMars Trace Gas Orbiter's Nadir and Occultation for MArs Discovery instrument. CO2 ice abundance is retrieved simultaneously with water ice, dust, and particle sizes, and rotational temperature and CO2 column profiles in 16 of 26 cases. Small particles (, ExoMars is a space mission of the European Space Agency (ESA) and Roscosmos. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB-BIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with the financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493), by the Spanish MICINN through its Plan Nacional and by European funds under grants PGC2018-101836-B-I00 and ESP2017-87143-R (MINECO/FEDER), as well as by UK Space Agency through grants ST/V002295/1, ST/V005332/1, ST/R001405/1 and ST/S00145X/1 and Italian Space Agency through grant 2018-2-HH.0. The IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709). This work was supported by NASA's Mars Program Office under WBS 604796, “Participation in the TGO/NOMAD Investigation of Trace Gases on Mars” and by NASA's SEEC initiative under Grant Number NNX17AH81A, “Remote sensing of Planetary Atmospheres in the Solar System and Beyond”. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No. 101004052. U.S. investigators were supported by the National Aeronautics and Space Administration.

Psychological inflexibility is a transdiagnostic dimension associated to psychological distress and poor mental health and quality of life. While multiple instruments have been developed for the assessment of patterns of inflexible responding to aversive private events (e.g., unwanted cognitions and emotions), the Experiential Approach Scale (EAS) is the first instrument specifically designed to assess inflexible responding to appetitive private events (e.g., desired affective states). In this study, we explored the factor structure, internal consistency, and convergent validity of a Spanish adaptation of the EAS with a convenience sample of college students from Spain (n = 206; 79% female). A two-factor solution demonstrated very good fit to the data and was similar to the original two-subscale EAS structure: Anxious Clinging and Experience Prolonging. The scale showed adequate overall (α = 0.85) and subscale (αs: 0.90 and 0.89) internal consistency. Unlike the original instrument, both subscales were uncorrelated. Anxious Clinging correlated positively with experiential avoidance and with measures of negative affect and psychopathology, and negatively with positive affect, subjective happiness, and life satisfaction. In turn, Experience Prolonging correlated negatively with psychopathology and positively with positive affect, subjective happiness, and life satisfaction. Our results point to Anxious Clinging as the only EAS subscale contributing to psychological inflexibility.

The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter has been designed to investigate the composition of Mars' atmosphere, with a particular focus on trace gases, clouds and dust. The instrument probes the ultraviolet and infrared regions covering large parts of the 0.2-4.3 µm spectral range [1,2], with 3 spectral channels: a solar occultation channel (SO – Solar Occultation; 2.3–4.3 μm), a second infrared channel capable of nadir, solar occultation, and limb sounding (LNO – Limb Nadir and solar Occultation; 2.3–3.8 μm), and an ultraviolet/visible channel (UVIS – Ultraviolet and Visible Spectrometer, 200–650 nm). Since its arrival at Mars in April 2018, NOMAD performed solar occultation, nadir and limb observations dedicated to the determination of the composition and structure of the atmosphere.NOMAD has been accumulating data about the Martian atmosphere and its surface since its insertion. We will present some results covering the atmosphere composition including clouds and dust, climatologies of water, carbon monoxide and ozone. We also report on the different discoveries highlighted by the instrument by pointing to a series of contributions to this conference that will present in detail several specific studies, like recent progress in the instrument calibration, the latest CO2 and temperature vertical profiles, studies of aerosol nature and distribution, water vapor profiles and variability, carbon monoxide vertical distribution, dayglow observations; detection of HCl, its vertical profiles and in general advances in the analysis of the spectra recorded by the three channels of NOMAD.References[1] Vandaele, A.C., et al., 2015. Planet. Space Sci. 119, 233-249.[2] Vandaele et al., 2018. Space Sci. Rev., 214:80, doi.org/10.1007/s11214-11018-10517-11212.

Introduction NOMAD is a three-channel spectrometer on the ExoMars 2016 Trace Gas Orbiter. The NOMAD solar occultation (SO) channel has been operating around Mars since April 2018 [1]. In the past three years of science operations, we have performed many calibrations and have taken millions of spectra. This huge dataset allows us to continue to refine the calibration, through additional characterisation of the optical elements, detector performance and temperature-induced effects. SO channel By using an Acousto-Optic Tunable Filter (AOTF) in combination with an echelle grating spectrometer, the SO channel is able to operate at unprecedented spectral resolution – typically 0.15 to 0.25 cm-1 [2] – and is therefore able to measure trace gases and set stringent upper limits on the presence (or non-presence) of organic molecules in the Martian atmosphere [3]. In solar occultation mode, the Sun is used as the illumination source, meaning that very high Signal-to-Noise Ratios (SNRs) can be achieved, typically up to 2,000 for a single spectrum at the top of the atmosphere. The SO channel records 24 spectra per second in solar occultation mode, with a typical vertical sampling resolution (i.e. altitude difference between consecutive spectra) of around 50-150m [4]. Therefore, by binning multiple spectra together, the SNR can be increased significantly whilst still keeping a high vertical sampling resolution. Calibration However the AOTF-grating combination also presents additional challenges, as the optical properties of both elements must be independently characterised in order to correctly retrieve atmospheric gas concentrations. Analysis of the AOTF shape and sidelobes, and the Instrument Line Shape (ILS), are ongoing in several of the groups within the NOMAD team. Additional systematic effects have also been identified in the spectra e.g. [5] which hamper efforts to further increase SNR and thus reduce detection limits via binning. Whilst much calibration work on this has already been performed [2, 4], the calibration can still be improved and work is ongoing to understand these effects and how to remove them from the data. Applications Since the beginning of the mission, a particular emphasis has been placed on making observations of CH4 around Gale Crater, in both nadir and solar occultation modes. HCl detections observations are now also made regularly, following the discovery of HCl in the atmosphere [7, 8] and its isotopologue [5], which are close to the detection limit of the channel. Calibration improvements will allow us to further constrain the CH4 upper detection limit, observe lower concentrations of HCl, and further constrain the isotopic ratio. References [1] Vandaele, A. C. et al (2015) Planet. Space Sci., 119 ; [2] Liuzzi, G. et al. (2019) Icarus, 321 ; [3] Knutsen, E. W. et al. (2021), Icarus, 357 ; [4] Thomas, I. R. et al. (submitted 2021) “Calibration of NOMAD on ExoMars Trace Gas Orbiter: Part 1 – the SO channel”; [5] Liuzzi G. et al (2021) GRL 48(9); [6] Korablev, O. et al. (2021) Science Advances, 7(7); [8] Aoki, S. et al. (accepted 2021) “Annual appearance of hydrogen chloride on Mars and a striking similarity with the water vapor vertical distribution observed by TGO/NOMAD”, GRL.

This is an open-access article distributed under the terms of the Creative Commons Attribution-NonCommercial license, which permits use, distribution, and reproduction in any medium, so long as the resultant use is not for commercial advantage and provided the original work is properly cited., Isotopic ratios and, in particular, the water D/H ratio are powerful tracers of the evolution and transport of water on Mars. From measurements performed with ExoMars/NOMAD, we observe marked and rapid variability of the D/H along altitude on Mars and across the whole planet. The observations (from April 2018 to April 2019) sample a broad range of events on Mars, including a global dust storm, the evolution of water released from the southern polar cap during southern summer, the equinox phases, and a short but intense regional dust storm. In three instances, we observe water at very high altitudes (>80 km), the prime region where water is photodissociated and starts its escape to space. Rayleigh distillation appears the be the driving force affecting the D/H in many cases, yet in some instances, the exchange of water reservoirs with distinctive D/H could be responsible. © 2021 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science., This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with the financial and contractual coordination by the ESA Prodex Office (PEA 4000103401 and 4000121493), by the Spanish MICINN through its Plan Nacional, by European funds under grants PGC2018-101836-B-I00 and ESP2017-87143-R (MINECO/FEDER), and by the Spanish Science Ministry Centro de Excelencia Severo Ochoa Program under grant SEV-2017-0709, as well as by the U.K. Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1, and ST/S00145X/1 and the Italian Space Agency through grant 2018-2-HH.0. This work was supported by NASA’s Mars Program Office under WBS 604796, “Participation in the TGO/NOMAD investigation of trace gases on Mars” and by NASA’s SEEC initiative under grant number NNX17AH81A, “Remote sensing of planetary atmospheres in the solar system and beyond.” M.J.C. was supported by the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by Universities Space Research Association (USRA) under contract with NASA. S.A. is postdoctoral researcher of the Belgian Fund for Scientific Research (FNRS).

Invadosomes support cell invasion by coupling both acto-adhesive and extracellular matrix degradative functions, which are apparently antagonistic. β1-integrin dynamics regulate this coupling, but the actual sensing mechanism and effectors involved have not yet been elucidated. Using genetic and reverse genetic approaches combined with biochemical and imaging techniques, we now show that the calcium channel TRPV4 colocalizes with β1-integrins at the invadosome periphery and regulates its activation and the coupling of acto-adhesive and degradative functions. TRPV4-mediated regulation of podosome function depends on its ability to sense reactive oxygen species (ROS) in invadosomes' microenvironment and involves activation of the ROS/calcium-sensitive kinase Ask1 and binding of the motor MYO1C. Furthermore, disease-associated TRPV4 gain-of-function mutations that modulate ECM degradation are also implicated in the ROS response, which provides new perspectives in our understanding of the pathophysiology of TRPV4 channelopathies. This work was funded by the Agence Nationale de la Recherche (ANR; invadocontrol; ANR-13-JSV2-0003-01) program and Ligue Contre le Cancer as “Equipe labellisée Ligue 2014” (EL2014.LNCC/CAR), the Spanish Ministry of Economy, Industry, and Competitiveness through grant RTI2018-099718, the institutional “Maria de Maeztu” Program for Units of Excellence in Research and Development, and FEDER funds. S. Vellino was funded by the European Marie-Sklodowska-Curie funding program. Proteomic experiments were partly supported by the Proteomics French Infrastructure (grant ANR-10-INBS-08-01) and Labex GRAL (grant ANR-10-LABX-49-01)

Petersen's space hernia is the most frequent location of internal hernia after a laparoscopic gastric bypass. The diagnosis or a high suspicion of internal herniation are indications for urgent surgery. We present the case of a patient who required an exploratory laparoscopy. He had a computed tomography compatible with internal herniation. We found a Petersen's space hernia and a jejunojenustomy defect. We reduced the protruded loops and we closed both mesenteric defects. The closure of mesenteric defects in primary surgery is a controversial matter. Overall, it is recommended to close them.Las hernias del espacio de Petersen son la localización más frecuente de las hernias internas tras un bypass gástrico laparoscópico. Su diagnóstico, e incluso su sospecha, son indicación de cirugía urgente. Presentamos el caso de un paciente que requirió una laparotomía exploradora en la que se halló una hernia del espacio de Petersen tras presentar en la tomografía computarizada el signo del «remolino». Se realizó la reducción de las asas intestinales herniadas junto al cierre del defecto mesentérico de dicho espacio. El cierre de los defectos mesentéricos en la cirugía primaria continúa generando controversia, pero como norma general se recomienda su cierre.

Incisional hernia (HI), in open and laparoscopic surgery, is a very frequent complication. HI located in the umbilical region are called M3. The main aim of this study is to compare HI produced by the placement of an umbilical laparoscopic trocar (M3T) with those located in M3 in open surgery (M3O) in terms of basal characteristics, complications and recurrences; and secondarily the identification of risk factors.Cross-sectional observational study based on the national prospective registry EVEREG during the period of July 2012-June 2018. The main variables were recurrences and postoperative complications. Both groups (M3T and M3O) were compared. Multiple logistic regression was performed to identify the risk factors of the entire cohort.882 had a follow-up time longer than 12 months. M3O group presented superior ASA-Class, more complex HI and previous repair. It also presented a higher recurrence rate at 12 and 24 months (8.6% vs. 2.5%; P0,0001 and 9.3% vs. 2.9%; P0.0001) and higher postoperative complications rate (21.9% vs. 14.6 %; P = 0.02). Previous repair, intervention length and associated procedures requirement were identified as risk factors for postoperative complications. Absence of a specialist present during surgery, previous repair, and the absence of complications were identified as risk factors for recurrence. In the PSM analysis no differences were detected in of complications and recurrences.HI M3O is more complex than M3T. The complexity is not related to the origin of the hernia but to its characteristics and those of the patient.

Polymer-gold nanoparticle nanocomposites based on POSS polymer with a thiol group was obtained by laser ablation in liquids (LAL). Laser ablation of a gold target in a solution of ethanol and POSS-thiol produced high purity nanocomposites of POSS decorated with gold nanoparticles (Au NPs) in colloidal suspension. TEM characterization showed spherical geometry of the Au NPs, mainly smaller than 60 nm. The UV–Vis-NIR spectroscopy exhibited the typical absorbance spectra for spherical Au NPs in the visible range (520–550 nm) related to plasmonic behavior. POSS-Au NPs nanocomposites exhibited an improvement in the colloid stability, absorbance peak and reproducibility, compared to the NPs without POSS-thiol. The optimal values were found for Au NPs synthesized in a POSS-thiol ethanol solution at 0.0168 mM. The low cytotoxic activity in human gingival fibroblasts (HGF) suggest the biocompatibility of the nanocomposite. The optical properties and biocompatibility of the nanocomposite shows its use viability for applications as biosensors based in optical response.

Introduction The southern spring and summer on Mars in the 34th Martian Year (MY34, Ls 180o-360o) was decorated by two dust storms: the global one (GDS) at Ls 190o-240o, and the regional one at Ls 320o-330o. Just before the onset of the GDS, the nominal ExoMars Trace Gas Orbiter mission began (April 2018) with an onboard solar occultation experiment by the spectrometric Atmospheric Chemistry Suite (ACS) [1]. The first ACS-NIR retrievals of the temperature and water mixing ratio revealed an increase the H2O abundance up to altitudes of 80-100 km not only in the stormy events but also at the perihelion in the southern hemisphere (around Ls~270o) [2]. Moreover, as it was shown, the water supersaturation occurs even in presence of the ice clouds, while the stormy warm atmosphere rises the hygropause level [2, 3]. This phenomenon increases a capability of water escape from Mars. Simultaneous investigation from the NOMAD/TGO solar occultations demonstrated analogue results for the H2O enhancement up to 80 km in the stormy seasons, but without the saturation estimations [4]. In this paper, we present results from more sensitive solar occultation measurements in the 2.65-2.7 μm spectral range by the middle infrared channel of ACS (ACS-MIR). The channel allows mesospheric and thermospheric retrievals of temperature and CO2 density in parallel with the mesospheric water abundance. Our results confirm the ACS-NIR and NOMAD conclusions concerning the H2O vapour behaviour in the second half of the MY34. We report the most humid mesosphere occurred in the perihelion season where the water enrichment was established about 5-10 ppbv at altitudes of 110-120 km. We also present the temperature and CO2 density seasonal distribution covering the troposphere, the mesosphere and the thermosphere of Mars. Measurements The ACS-MIR channel is a cross-dispersion echelle spectrometer dedicated to solar occultation measurements in the 2.3–4.3 μm wavelength range [1]. The instrumental resolving power λ/Δλ reaches ~30 000, while the altitude resolution is 1-2 km and the signal/noise ratio is about ~1000. Each occultation session covers a spectral interval with one or a few CO2 absorption bands appropriate for the atmospheric density and temperature retrievals. In this work, we perform data analysis in the 2.65-2.7 μm spectral range, which occupies echelle diffraction orders from 221 to 224, observed simultaneously. This spectral region hosts strong CO2 and H2O absorption bands that are sensitive to detections of CO2 density up to 180-190 km and H2O density up to 120-130 km. For the MY34 the MIR dataset in the considered spectral range is made of ~100 occultation profiles in the Northern hemisphere and of ~90 in the Southern one encompassing seasonal period from Ls 165o to 355o. Retrieval concept The temperature and densities retrieval scheme consists of several iterations with a fitting of a forwardly modelled transmission spectrum to a measured one at each observed altitude. The model includes line-by-line calculations CO2 and H2O absorption cross sections depending on specified temperature and pressure. The fitting procedure is based on Jacobian matrix containing transmission derivatives on free parameters: temperature, CO2 density and H2O density. The clue contribution to an optimal estimation comes from the molecular cross sections derivatives on temperature; they differ significantly from line to line in the considered spectral range. Thanks to that, an independent and simultaneous retrieval of temperature and density is possible. Once the altitude profiles of these parameters are estimated at the first iteration, we calculate the atmospheric pressure profile assuming the hydrostatic equilibrium. This assumption was successfully tested by other vertical profile retrievals from the ACS data [1, 5]. The uncertainty of the retrievals is determined by the transmission errors and the Jacobian matrix for each of free parameters. This estimation allows establishing maximal altitudes with a positive detection of CO2 and H2O densities. Results ACS-MIR solar occultations in the 2.65-2.7 μm spectral range provide us with unprecedented capability to profile CO2 density and temperature from 20 to 180 km, covering the troposphere, the mesosphere and the thermosphere of Mars. The homopause varies around ~130 km and CO2 mixing ratio decreases from 96% to 20-40% at 180 km due to photolysis and molecular diffusion. In parallel with the same dataset, we report very high altitude water abundance, at 110-120 km, that occurred in the southern spring and summer including the GDS and the perihelion in the 34th Martian Year. However, our measurements in the northern hemisphere revealed such a high H2O enrichment only at the stormy events. Comparison of our climatology with some improvements in the Global Circulation Model for the MY34 is in progress. Acknowledgements The retrievals of density/temperature profiles in IKI are funded by the RSF grant #20-42-09035. References [1] Korablev O. et al., 2018. The Atmospheric Chemistry Suite (ACS) of three spectrometers for the ExoMars 2016 Trace Gas Orbiter. Space Sci. Rev., 214:7. DOI 10.1007/s11214-017-0437-6. [2] Fedorova A. et al., 2020. Stormy water on Mars: The distribution and saturation of atmospheric water during the dusty season. Science, eaay9522. DOI: 10.1126/science.aay9522. [3] Fedorova A. et al., 2018. Water vapor in the middle atmosphere of Mars during the 2007 global dust storm. Icarus 300: 440-457. [4] Aoki S. et al., 2019. Water vapor vertical profiles on Mars in dust storms observed by TGO/NOMAD. JGR Planets, 124, 3482-3497. https://doi.org/10.1029/2019JE006109. [5] Alday J. et al., 2019. Oxygen isotopic ratios in Martian water vapour observed by ACS MIR on board the ExoMars Trace Gas Orbiter. A&A, 630, A91. DOI: 10.1051/0004-6361/201936234.

We present simultaneous retrievals of vertical profiles of CO2 and temperature obtained from a small sample of solar occultation scans by the NOMAD-SO [1] and ACS-MIR [2] instruments on board the ExoMars Trace Gas Orbiter (TGO). The orbits or scans selected from each instrument's observations are sufficiently close in time and space so that the atmospheric variability plays a minor role and a meaningful comparison of the performance of both instrument channels is possible. This is an on-going work devoted to a proper validation of both instruments. We will present a small selection of retrievals than can be used for a critical analysis of the results obtained and as a first step into the mutual validation of NOMAD-SO and ACS-MIR.1. Instruments and observationsOur work is focussed in the NOMAD-SO and the ACS-MIR channels, those specifically devoted to operational observations in solar occultation. Several groups in the NOMAD and ACS teams are performing retrievals of species abundances from these signals and some are reported in this conference [3,4]. We focus on the retrieval of CO2 and temperature in the 2.7 µm range, the strongest IR bands by this gas in the spectra region coverd by SO and ACS [5]. The spectra correspond to calibrated transmittances derived from SO difraction orders 164 and 165 and from MIR position 4 spectra. About a dozen strong CO2 lines are observed in these spectra up to very high tangent altitudes, around 170-180 km. The present study targets at both solar occultation signals, NOMAD-SO and ACS-MIR, but unfortunately, due to some unexpected miss-alignments among the different channels in each instrument and between NOMAD and ACS, an entirely simultaneous observation of the solar disc as it emerges or hides behind the atmosphere is not possible with both SO and MIR channels. Instead this work study the inversions from the two channels in nearly coincident solar occultations, with small changes in latitude, longitude, solar longitude and time.2. Retrieval Scheme We have performed the present retrievals using an inversion code previously used in the Earth upper atmosphere for routine operations of the MIPAS instrument on board the Envisat mission [6]. The inversion scheme, which has been recently adapted to Mars for limb sounding in emission from the OMEGA spectrometer on board the Mars Express spacecraft [7], is adapted here for occultation observations. At the core of the inversion scheme is the forward model KOPRA (Karlsruhe Optimized and Precise Radiative transfer Algorithm [8] ) and the inversion processor (RCP), jointly developed by the Institute for Meteorology and Climate Research (IMK) and the IAA [9].As mentioned above we used here CO2 calibrated transmittances obtained from routine processing by the PI teams. But before injection into the inversion algorithm, a pre-processing of every orbit or scan is performed in order to correct every spectrum of spurious effects. These are essentially two: residual spectral shifts and artificial bending in single spectra. The magnitude of these two effects changes from order to order and between SO and ACS. In spite of these differences, the pre-processing is conceptually similar to both signals, and is actually performed with the same Python code. Further, the ILS associated to each of the signals is best reproduced by a double gaussian, whose detailed description (parameters describing their FWHM and peak ratios, for example) requires also a precise determination by the user, as apparently it slightly varies with time and observing conditions.It is specially useful to obtain both density and temperature information from a single scan, and this is the purpose of the present study. The simultaneous retrieval from a given scan actually derives a CO2 density profile, and after an iterative process, a temperature profile assuming hydrostatic equilibrium. An adjustment for the pointing is also intruduced, and the aerosol extinction and possible interference from species like H2O are also considered during the inversion to obtain the best fits.3. Results We will discuss the fist comparisons of CO2 and temperatures from NOMAD-SO and ACS-MIR, using a common pre-processing and inversion code. The retrievals perform in a similar manner, as in both cases the number of lines, the ro-vibrational bands and the spectral region are similar. Small differences in noise and spectral resolution have some impact but overall both channels permit sounding the Mars atmosphere up to the upper thermosphere with just one single scan. Averaging kernels indicate effective vertical resolutions around 4-6 km in the middle atmosphere (50-100 km), both in CO2 and temperature. The inversion is affected by heavy dust loading and in general degrades below about 30 km and above 150 km due to saturation and noise, respectively. AcknowledgementsThe IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCIU through the ‘Center of Excellence Severo Ochoa’ award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709). MALV was funded by grant PGC2018-101836-B-100 (MCIU/AEI/FEDER, EU). ExoMars is a space mission of the European Space Agency (ESA) and Roscosmos. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB-BIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). US investigators were supported by the National Aeronautics and Space Administration. References[1] Vandaele et al., Space Science Reviews 214 (5), 2018 [2] Korablev et al., Space. Sci. Rev. 214, 7 (2018). [3] Loic et al., Update on CO2 and temperature profiles retrievals from NOMAD-SO on board ExoMars TGO, contribution to this conference, 2020. [4] Shohei et al., Water vapor vertical profiles on Mars: Results from the first full Mars Year of TGO/NOMAD science operations, contribution to this conference, 2020. [5] Lopez-Valverde et al., Space Sci Rev (2018) 214:29 [6] Funke, B., et al. , Atmos. Chem. Phys., 9(7), 2387–2411, 2009.Funke et al., ACP, 9, 2387–2411, 2009. [7] Jimenez-Monferrer, Icarus in press, 2020 [8] Stiller et al., JQSRT, 72, 249–280, 2002 [9] von Clarmann et al., J. Geophys. Res. 108, 4746, 2003 How to cite: Lopez-Valverde, M. A., Funke, B., Hill, B., Gonzalez-Galindo, F., Aoki, S., Trompet, L., Thomas, I., Villanueva, G., Erwin, J., Olsen, K., Belyaev, D., Trokhimovskiy, A., Alday Parejo, J., Lopez-Puertas, M., Lopez-Moreno, J. J., Montmessin, F., Patel, M., Bellucci, G., Vandele, A. C., and Korablev, O.: CO2 and temperature retrievals in the Mars atmosphere from solar occultation by NOMAD-SO and ACS-MIR: performance and cross validation., Europlanet Science Congress 2020, online, 21 September–9 Oct 2020, EPSC2020-924, 2020

The OI 557.7 nm green line has been measured in the Martian dayglow for the first time with the UVIS visible-ultraviolet spectrograph on board ESA’s Trace Gas Orbiter (Gérard et al., 2020). The first observations started in April 2019 in a special mode where the spacecraft is tilted to observe the limb with the UVIS nadir channel (Vandaele et al., 2015, Patel et al., 2017). The instrument detected the presence of bright green dayglow emission on every of those observations. The main peak altitude is located near 80 km, and its intensity varies as a result of the changing distance from sun, the local time and latitude of the observations. A second, less pronounced, emission peak is observed near 110 km. Photochemical model simulations (Gkouvelis et al., 2018) used the MCD density distribution (Forget et al., 1999) have been made to understand the sources of this airglow emission. It is able to reproduce the altitude and the brightness of the airglow layer. It indicates that the green line dayglow on Mars is essentially produced by photodissociation of CO2 molecules by solar far ultraviolet radiation (Fox & Dalgarno, 1979). A fraction of the oxygen atoms is formed in the 1S metastable state that produces the green emission. In this presentation, we describe additional dayside observations obtained since December 2019. For this purpose, the spacecraft has been used in a special mode where it is re-oriented so that the UVIS channel observed the sunlit limb (Lopez-Valverde et al., 2018). We analyse the observed limb profile variations and the changing altitude of the peak emission resulting from the variations of the pressure levels in the mesosphere (Gkouvelis et al., 2020). The measured intensities are compared with model calculations of the O(1S) density in the conditions of the observations. The ratio of ultraviolet spectral features relative to the oxygen emission also observed with UVIS will also be analysed. REFERENCES Forget, F. et al., J. Geophys. Res. 104(E10), 24155-24175 (1999). Fox, J.L. & Dalgarno, J. Geophys. Res. 84(A12), 7315-7333 (1979). Gérard, J.C. et al., Nature Astronomy, 1-4 (2020), https://doi.org/10.1038/s41550-020-1123-2 Gkouvelis, L. et al., J. Geophys.Res., 123(12), 3119-3132. (2018). Gkouvelis, L. et al., Icarus, 341, 113666 (2020). López-Valverde M. et al., Space Science Reviews, 214(1), 29 (2018). Patel, M. R. et al., Applied optics, 56(10), 2771-2782 (2017). Vandaele, A. C. et al., Optics Express, 23(23), 30028-30042 (2015).

A reversal design was employed for the analysis of transfer of fear and avoidance through equivalence classes. Two 5-member equivalence classes (A1-B1-C1-D1-E1 and A2-B2-C2-D2-E2) were established. Then B1 and C1 were paired with shock (CS+) and served as SD s in avoidance training (B2 and C2 were trained as CS-/S∆ s for avoidance). Further avoidance training followed with D1 and E1 (as SD s) and D2 and E2 (as S∆ s), with the first presentation of each of these stimuli serving as the first transfer test. Afterwards, aversive conditioning contingencies were reversed: B2 and D2 were paired with shock and trained as SD s for avoidance, B1 and D1 were presented without shock (CS-/S∆ s). Transfer was tested again with C1, E1, C2 and E2. This reversal was implemented to allow for the within-subject replication of transfer effects upon changes in the function of only a subset of each class's elements. Avoidance (key presses) and conditioned fear (skin conductance and heart rate) were simultaneously measured. Results show a clear transfer effect for avoidance, with between- and within-subject replications. For physiological measures, transfer effects in the first test could only be imputed on the basis of group-based inferential statistical analysis. Evidence for between-subject replication was weaker, with only a limited proportion of participants meeting the individual criterion for transfer.

The mid-infrared channel of the Atmospheric Chemistry Suite (ACS-MIR) is a cross-dispersion echelle spectrometer dedicated to solar occultation measurements in the 2.3–4.3 μm wavelength range [1]. The instrumental resolving power λ/Δλ reaches ~30 000, while the altitude resolution is ~1 km. ACS-MIR began regular science operations in April 2018 on board the ExoMars Trace Gas Orbiter (TGO). Each occultation session covers a spectral interval with one or a few CO2 absorption bands appropriate for the atmospheric density and temperature retrievals.In this paper, we present results from data analysis in the 2.65-2.7 μm spectral range hosting strong CO2 absorption bands detectable up to 180 km. It provides us with unprecedented capability to profile CO2 from 20 to 180 km, covering the troposphere, the mesosphere and the thermosphere of Mars. The homopause is found around ~130 km and CO2 mixing ratio decreases from 96% to 20-40% at 180 km due to photolysis and molecular diffusion. A multiple iteration scheme was applied to retrieve CO2 density and temperature from the rotational absorption lines, while pressure was estimated assuming hydrostatic equilibrium. The vertical profiles coincide well with the simultaneous occultations performed below 100 km by the near-infrared channel ACS-NIR [2]. At the moment, our MIR channel dataset is made of >100 profiles encompassing the second half of MY34 and the beginning of MY35 in both martian hemispheres. The retrievals of density/temperature profiles in IKI are funded by the RSF grant #20-42-09035.REFERENCES[1] Korablev O. et al., 2018. The Atmospheric Chemistry Suite (ACS) of three spectrometers for the ExoMars 2016 Trace Gas Orbiter. Space Sci. Rev., 214:7. DOI 10.1007/s11214-017-0437-6.[2] Fedorova A. et al., 2020. Stormy water on Mars: The distribution and saturation of atmospheric water during the dusty season. Science, eaay9522. DOI: 10.1126/science.aay9522.

Context. In February 2018, the international community working on the investigation and exploration of the atmosphere and surface of Mars met at ESAC near Madrid for a few days conference, organized and funded by the project UPWARDS (“Understanding Planet Mars With Advanced Remote- ensing Datasets and Synergistic Studies”, www.upwards-mars.eu) of the EU Horizon 2020 program. This project, and that conference, were devoted to promote the scientific exploitation of Mars Express data and to revisiting and sharing results from this mission, in preparation for the upcoming new European mission to Mars, the ExoMars-2016. The meeting approximately coincided in time with the end of the aerobraking phase of the Trace Gas Orbiter (TGO), which is the orbital element of ExoMars-2016. The TGO science phase started on 21 April 2018. This special issue of Icarus contains eleven papers which report original research results presented at the meeting or based on those presentations. This is obviously not an exhaustive representation of what was presented in Madrid, as other results have been published elsewhere. But they all share the motto of the meeting - from MEX to TGO - by presenting highlights of almost 15 years of Mars EXpress science legacy and new tools and methods for data analysis, thus paving the way for TGO observations and collaboration between two spacecraft. We think this is a valuable approach which, if properly and timely coordinated, can be very fruitful and should be promoted on every new space mission. The UPWARDS project could be considered as a bridge facilitating transition between two ESA missions, building team connections and enhancing science return from both missions. The second goal of the UPWARDS project, now more in the scientific than in the programmatic realm, was to exploit synergies between different teams in a cross-disciplinary approach, looking for an integral vision of the planet in an attempt to unveil couplings between different regions. In the meeting mentioned above, there were investigations from the subsoil and the surface, to the lower atmosphere's composition and dust, to the water cycle and up to the thermospheric structure and escape to space. In this framework, this issue presents its 11 contributions ordered in this bottom-to-top vision of the atmosphere., We want to acknowledge ESA for successful operations of the Mars Express and the TGO spacecrafts. The project UPWARDS-633127 was funded by the European Union's Horizon 2020 research and innovation Programme.

The oxygen emission at 557.7 nm is a ubiquitous component of the spectrum of the terrestrial polar aurora and the reason for its usual green colour(1). It is also observed as a thin layer of glow surrounding the Earth near 90 km altitude in the dayside atmosphere(2,3)but it has so far eluded detection in other planets. Here we report dayglow observations of the green line outside the Earth. They have been performed with the Nadir and Occultation for Mars Discovery ultraviolet and visible spectrometer instrument on board the European Space Agency's ExoMars Trace Gas Orbiter. Using a special observation mode, scans of the dayside limb provide the altitude distribution of the intensity of the 557.7 nm line and its variability. Two intensity peaks are observed near 80 and 120 km altitude, corresponding to photodissociation of CO(2)by solar Lyman alpha and extreme ultraviolet radiation, respectively. A weaker emission, originating from the same upper level of the oxygen atom, is observed in the near ultraviolet at 297.2 nm. These simultaneous measurements of both oxygen lines make it possible to directly derive a ratio of 16.5 between the visible and ultraviolet emissions, and thereby clarify a controversy between discordant ab initio calculations and atmospheric measurements that has persisted despite multiple efforts. This ratio is considered a standard for measurements connecting the ultraviolet and visible spectral regions. This result has consequences for the study of auroral and airglow processes and for spectral calibration. The oxygen emission at 557.7 nm, responsible for the green colour of auroras on Earth, is present in two layers at 80 and 120 km altitude on the dayside atmosphere of Mars. Simultaneous observations of the oxygen both in this visible line and in the ultraviolet could also constrain the elusive visible/ultraviolet intensity ratio of the auroral emission to a value of 16.5., B.H. is research associate and S.A. is postdoctoral researcher of the Belgian Fund for Scientific Research (FNRS). ExoMars is a space mission of the ESA and Roscosmos. The NOMAD experiment is led by the IASB-BIRA, assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS) and the United Kingdom (The Open University). This project acknowledges funding from BELSPO, with the financial and contractual coordination by the ESA Prodex Office (PEA grant numbers 4000103401 and 4000121493). M.A.L.-V. and J.-J.L.-M. were supported by grant number PGC2018-101836-B-100 (MCIU/AEI/FEDER, EU) and by the Spanish Science Ministry Centro de Excelencia Severo Ochoa Program under grant number SEV-2017-0709. We also acknowledge support from the UK Space Agency through grant numbers ST/R005761/1, ST/P001262/1 and ST/S00145X/1 and the Italian Space Agency through grant number 2018-2-HH.0. We thank the ESA TGO team and its project scientist H. Svedhem for supporting observations in this special mode.

Introduction Our objective is to evaluate the safety of deep sedation with Propofol administered by endoscopists or trained nurses . Material and methods Retrospective study conducted in all patients undergoing colonoscopy for colorectal cancer (CRC) screening, sedated with Propofol controlled by the endoscopy team (ET) during a period of 8 months. Different variables were recorded: sex, anesthetic risk (ASA), dose of Propofol, duration of the exploration and presence of desaturation, bradycardia or hypotension. Results 277 colonoscopies were performed (53.4% male), with 25 (8.9%) complications related to sedation. The most frequent were cardiovascular complications (21 cases, 84%), including 15 cases of hypotension, 3 cases of bradycardia, and 3 of both at the same time. Four (1.4%) desaturations were recorded. In these cases, the mean dose of propofol (251mg), as well as the time of exploration (36±8 min) and the ASA classification were higher than in those patients without complications, or with cardiovascular events (no statistically significant difference). Discussion Deep sedation with propofol controlled by traide ET in our screening colonoscopy program is a safe procedure. .

Resumen Objetivo La estenosis de la anastomosis uretrovesical (EAU-V) afecta al 8,4% de pacientes intervenidos de prostatectomía radical retropúbica por cáncer. Nuestro propósito fue estudiar los factores de riesgo de estenosis de cuello vesical asociada a prostatectomía radical por carcinoma prostático en nuestro centro. Material y Métodos Estudio de casos-controles en una cohorte constituida por 120 pacientes intervenidos por adenocarcinoma prostático entre 2005 y 2012. Realizamos un análisis descriptivo de la muestra y el cálculo de la incidencia de EAU-V, un análisis univariante de los factores asociados mediante la t de Student y la chi cuadrado de Pearson, un análisis del tiempo transcurrido hasta la aparición de estenosis y una predicción del riesgo de EAU-V. Resultados La incidencia de EAU-V tras prostatectomía radical en nuestro servicio fue del 22,5%. Encontramos mayor riesgo en aquellos pacientes con débito por drenaje Jackson-Pratt (J-P) mayor de 500cc, drenaje J-P retirado después del tercer día, estancia superior a 8 días, hemoglobina postoperatoria baja, PSA preoperatorio bajo, densidad de PSA elevada o que fueron intervenidos por el cirujano 1 o 5. Todas las estenosis se produjeron en los 3 primeros años tras la cirugía. Los pacientes con un débito del drenaje por encima de 500cc y en los que el drenaje se retiró después del tercer día tienen 7,7 y 3,2 veces, respectivamente, más riesgo de padecer una EAU-V. Conclusiones Nuestra incidencia de EAU-V y sus factores asociados coinciden con los publicados. El modelo predictivo desarrollado tiene utilidad meramente teórica ya que no abarca la totalidad de los factores que pueden influir en la aparición de la estenosis.

Actin polymerization and assembly into stress fibers (SFs) is central to many cellular processes. However, how SFs form in response to the mechanical interaction of cells with their environment is not fully understood. Here we have identified Piezo2 mechanosensitive cationic channel as a transducer of environmental physical cues into mechanobiological responses. Piezo2 is needed by brain metastatic cells from breast cancer (MDA-MB-231-BrM2) to probe their physical environment as they anchor and pull on their surroundings or when confronted with confined migration through narrow pores. Piezo2-mediated Ca2+ influx activates RhoA to control the formation and orientation of SFs and focal adhesions (FAs). A possible mechanism for the Piezo2-mediated activation of RhoA involves the recruitment of the Fyn kinase to the cell leading edge as well as calpain activation. Knockdown of Piezo2 in BrM2 cells alters SFs, FAs, and nuclear translocation of YAP; a phenotype rescued by overexpression of dominant-positive RhoA or its downstream effector, mDia1. Consequently, hallmarks of cancer invasion and metastasis related to RhoA, actin cytoskeleton, and/or force transmission, such as migration, extracellular matrix degradation, and Serpin B2 secretion, were reduced in cells lacking Piezo2.

Krasnopolsky (2017) makes a careful review of our recent results about the Martian hydrogen content of the Martian upper atmosphere (Chaufray et al., 2015). We comment here on his two major points. First, he suggests that the non-thermal escape of H, and particularly collisions with hot oxygen, not taken into account in our general circulation model (GCM), should modify our reported H and H density profiles. This is an important issue; we acknowledge that future effective coupling of our GCM with comprehensive models of the Martian solar wind interaction, ideally after being validated with the latest plasma observations of H , would allow for better estimations of the relative importance of the H non-thermal and thermal escape processes. For the time being we need assumptions in the GCM, with proper and regular updates. According to a recent and detailed study of the anisotropic elastic and inelastic collision cross sections between O and H (Gacesa et al., 2012), the escape rates used by Krasnopolsky (2010) for this process might be overestimated. We therefore do not include non thermal escape of H in the model. And secondly, in response to Krasnopolsky's comment on the H escape variability with the solar cycle, we revised our calculations and found a small bug in the computation of the Jeans effusion velocity. Our revised computed H escape rates are included here. They have a small impact on our key conclusions: similar seasonal variations, a reduced variation with the solar cycle but still larger than Krasnopolsky (2017), and again a hydrogen scape systematically lower than the diffusion-limited flux. This bug does not affect the latest Mars Climate Database v5.2. © 2017 Elsevier Inc., This work has been partially funded by the European Union Horizon 2020 Programme (H2020 Compet -08-2014) under grant agreement UPWARDS-633127. We thank Programme National de Planetologie (PNP) and Programme National Soleil-Terre (PNST) for their support.

Objetivo: Analizar la eficacia diagnostica e incidencia de complicaciones de la puncion aspiracion con aguja fina (PAAF) guiada por tomografia computarizada (TC) del nodulo/masa pulmonar realizada por residentes de radiodiagnostico. Material y metodo: Estudio descriptivo-retrospectivo entre Enero-2011 y Junio-2016 de PAAF transtoracicas guiadas por TC para el estudio de un nodulo/masa pulmonar efectuada por un residente de radiodiagnostico. Los residentes realizaron esta tecnica de forma consecutiva segun la programacion del servicio, siguiendo el protocolo establecido y supervisados por un radiologo especializado. Para evaluar la eficacia, se incluyeron las PAAF con resultado especifico y para el calculo de las complicaciones, todas las PAAF realizadas. Se usaron la prueba Chi-cuadrado de Pearson o exacta de Fisher, T de Student o Mann-Whitney y los paquetes informaticos SPSS 15.0 y EPIDAT 3.1. Resultados: Se registraron 131 pacientes, realizandose en total 144 PAAF. La eficacia de la prueba diagnostica fue alta (cociente de probabilidad (CP): 7,35), destacando la diferencia entre el pulmon derecho (CP: 15,1) y el izquierdo (CP: 4,27). La sensibilidad y especificidad fueron mayores al 85%. Tuvimos 62 complicaciones (43,1%): 50 (34,7%) neumotorax con una mediana de 10,5mm (4,3-23,7) de diametro maximo y ninguno a tension; y 20 casos (13,9%) de hemorragia pulmonar diagnosticados unicamente por imagen. Conclusion: La PAAF guiada por TC es una herramienta diagnostica de alta precision y baja incidencia de complicaciones graves, que puede ser realizada por un residente de radiodiagnostico bajo supervision sin detrimento de la rentabilidad diagnostica o seguridad de la prueba. Palabras clave: nodulo/masa pulmonar, Tomografia computerizada, Puncion aspiracion con aguja fina guiada por TC, Citologia, Sensibilidad, Especificidad