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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.

[EN] This paper presents an innovative teaching experience carried out as part of a project in the Teaching Innovation Program at the University of Jaén (PIMED-UJA 2019-2023). The main goal of this project was the production of a series of brief training videos that modelled specific skills in assessment and intervention, in order to facilitate the acquisition of procedural skills specific to the degrees in Psychology and Nursing, as well as to the Health Psychology Masters degree. Faculty from different courses of these degrees (all of them registered healthcare psychologists with experience in their respective domains) scripted different therapy interactions that depicted specific therapeutic skills. The different roles (therapist and client) were played by professional actors that prepared the scripts and received specific feedback from the involved faculty, both before and during the recording sessions. The paper presents results regarding the use of these training videos in three different courses: Foundations of Psychological Assessment, Psychosocial Sciences in Healthcare, and Third Wave Behavioral Therapies in Healthcare Contexts. Students exposed to the training videos showed reductions in anticipatory anxiety, as well as increases in selfefficacy and the perceived utility of training for their future development as healthcare professionals., [ES] En este trabajo se presenta una experiencia de innovación docente realizada dentro del Plan de Innovación y Mejora Docente de la Universidad de Jaén (PIMED-UJA 2019-2023). El objetivo fundamental fue generar una serie de vídeos que modelaran habilidades de evaluación e intervención, a fin de facilitar la adquisición de competencias procedimentales específicas de los grados en Psicología, Enfermería y del máster en Psicología General Sanitaria. Para la elaboración de los vídeos, el profesorado de diferentes asignaturas, psicológos sanitarios con amplia experiencia, guionizaron situaciones de terapia donde se mostraban habilidades concretas. Los participantes de los vídeos fueron actores profesionales que recibieron los guiones así como feedback tanto antes como durante la grabación. En este trabajo se presentan los resultados de la utilización de estos vídeos en tres asignaturas: Fundamentos de Evaluación Psicológica, Ciencias Psicosociales Aplicadas a los Cuidados de la Salud y Terapias de Tercera Generación en el Ámbito de la Salud. El alumnado al que se presentó los vídeos mostró una reducción de la ansiedad para enfrentarse a situaciones de interacción terapéutica, y un incremento de la autoeficacia y de la utilidad percibida de las herramientas utilizadas en su formación como futuros profesionales de la salud.

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.

Background The discrepancy between actual and ideal body image is considered an index of body dissatisfaction and a risk factor for eating disorders. While discrepancy has been traditionally tested with figural drawing rating scales, in recent times the use of implicit measures has been explored. Methods This study employs the Implicit Relational Assessment Procedure (IRAP) to examine actual-ideal body-size discrepancy in a sample of 130 Spanish college students, as well as its utility to predict symptoms of eating disorders and other body-image relevant measures. Participants completed the Contour Drawing Rating Scale (CDRS). The three smallest and the three largest contour drawings of the CDRS were used as target stimuli in two different IRAP tasks: one in combination with the sample phrases “I am” and “I am not” (that assessed implicit actual body image), another in combination with the phrases “I want to be” and “I don’t want to be” (that assessed implicit ideal body image). After completing both IRAP tasks, participants completed explicit measures of body-image psychological inflexibility, body dissatisfaction, and symptoms of eating disorders. Results Results showed a small implicit bias towards thinness. Participants were faster in affirming than denying that they are thin and that they desire to be thin. They were also faster in affirming than denying that they are fat and that they want to be fat, but to a smaller extent than with thinness. Specifically, the implicit desire to be (or not be) fat emerged as an independent predictor of eating disorder symptoms, psychological inflexibility, and body dissatisfaction that significantly increased the predictive power of CDRS scores. Conclusions These findings underscore the need for further research on specific body image implicit beliefs towards fatness, both in subclinical and clinical populations, in order to examine whether willingness to accept the idea that one can have a larger body size can be a suitable target for prevention and intervention in eating disorders., Plain English summary Body dissatisfaction can be thought of as the discrepancy between actual and desired body size. This is typically measured with rating scales depicting a series of body silhouettes of increasing size, from extreme thinness to fatness. Respondents mark the points that match their current body size and the one they would ideally like to be (the more distance between both, the more body dissatisfaction). Like all self-reports, these scales are liable to self-presentation biases. Experimental procedures that require respondents to answer under time pressure (implicit measures) tap into more automatic reactions that are less amenable to deliberate manipulation. This study used one such procedure (the IRAP) to examine how rapidly participants identified themselves (or not) with pictures of underweight or overweight, and how rapidly they expressed a desire to be (or not) like such pictures. Participants did not show a clear discrepancy between their actual and their ideal body size with the IRAP. However, automatic reactions indicative of acceptance/rejection of the idea of becoming fatter, predicted the degree of body image distress as measured with different instruments. Unwillingness to accept this idea was associated with more severe symptoms of disordered eating.

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 this work, we studied the microfibers of a textile (T-shirt) of the Chimú culture. This culture developed on the northern coast of Peru. To determine the raw material and structural quality of the microfibers, the results of the Chimú textile were compared with the corresponding results for the microfibers of cotton from the northern coast of Peru (native cotton). Scanning electron microscopy images revealed that the Chimú textile yarns are composed of a set of interwoven microfibers. Energy-dispersive X-ray spectroscopy and pulsed laser-induced plasma spectroscopy techniques allowed the identification of characteristic cellulose atoms in the microfibers of Chimú textile and native cotton. Only for the Chimú textile, these spectroscopic techniques allowed the identification of atoms corresponding to natural dyes and powder residues. Attenuated total reflection Fourier transform infrared spectroscopy identified the same molecular bonds for the microfibers of Chimú textile and native cotton. For the microfibers of Chimú textile and native cotton, the X-ray diffractograms showed peaks characteristic of the cellulose Ig polymorphism of monoclinic P21 structure. The raw material of the Chimú textile is cotton and the microfibers of this material show significant structural stability. Resumen En este trabajo se estudiaron las microfibras de un textil (camiseta) de la cultura Chimú. Esta cultura se desarrolló en la costa norte del Perú. Para determinar la materia prima y calidad estructural de las microfibras, los resultados del textil Chimú fueron comparados con los correspondientes para las microfibras del algodón de la costa norte del Perú (algodón nativo). Las imágenes de microscopia electrónica de barrido revelaron que los hilos del textil Chimú están compuestos por un conjunto de microfibras entrelazadas. Las técnicas de espectroscopia de rayos X por energía dispersiva y de plasmas inducidos por laser permitieron identificar átomos característicos de la celulosa en las microfibras del textil Chimú y del algodón nativo. Únicamente para el textil Chimú, estas técnicas espectroscópicas permitieron identificar átomos que corresponderían a tintes naturales y a residuos de polvo. La espectroscopia de infrarrojo con transformada de Fourier por reflexión total permitió identificar los mismos enlaces moleculares para las microfibras del textil Chimú y del algodón nativo. Para las microfibras del textil Chimú y del algodón nativo, los difractogramas de rayos X mostraron picos característicos del polimorfismo de la celulosa Iß de estructura monoclínica P21. La materia prima del textil Chimú es el algodón y las microfibras del mismo presentan una significativa estabilidad estructural.

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.

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.

Description, Piezo1 transduces mechanical forces at the intercellular bridge to coordinate the machinery necessary to split dividing cells., Mechanical forces are exerted throughout cytokinesis, the final step of cell division. Yet, how forces are transduced and affect the signaling dynamics of cytokinetic proteins remains poorly characterized. We now show that the mechanosensitive Piezo1 channel is activated at the intercellular bridge (ICB) connecting daughter cells to regulate abscission. Inhibition of Piezo1 caused multinucleation both in vitro and in vivo. Piezo1 positioning at the ICB during cytokinesis depends on Pacsin3. Pharmacological and genetic inhibition of Piezo1 or Pacsin3 resulted in mislocation of Rab11-family-interacting protein 3 (Rab11-FIP3) endosomes, apoptosis-linked gene 2-interacting protein X (ALIX), and endosomal sorting complex required for transport III (ESCRT-III). Furthermore, we identified FIP3 as the link between Piezo1-generated Ca2+ signals and ALIX delivery to the ICB, where ALIX recruits the ESCRT-III component charged multivesicular body protein 4B, which promotes abscission. These results provide a different view of how mechanical forces participate in cytokinesis and identify Piezo1 as a key modulator of endosome trafficking.

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.

Hydrogen chloride (HCl) was recently discovered in the atmosphere of Mars by two spectrometers onboard the ExoMars Trace Gas Orbiter. The reported detection made in Martian Year 34 was transient, present several months after the global dust storm during the southern summer season. Here, we present the full data set of vertically resolved HCl detections obtained by the NOMAD instrument, which covers also Martian year 35. We show that the particular increase of HCl abundances in the southern summer season is annually repeated, and that the formation of HCl is independent from a global dust storm event. We also find that the vertical distribution of HCl is strikingly similar to that of water vapor, which suggests that the uptake by water ice clouds plays an important role. The observed rapid decrease of HCl abundances at the end of the southern summer would require a strong sink independent of photochemical loss. © 2021. American Geophysical Union., ExoMars is a space mission of the European Space Agency 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, with the financial and contractual coordination by the European Space Agency Prodex Office (PEA 4000103401 and 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/S00145X/1 ST/S00145X/1 and ST/T002069/1, and 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." 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 Astrofisica de Andalucia (SEV-2017-0709). This work was supported by the Belgian Fonds de la Recherche Scientifique-FNRS under grant numbers 30442502 (ET_HOME) and T.0171.16 (CRAMIC) and Belgian Science Policy Office BrainBe SCOOP and MICROBE Projects. S. A. is "Charge de Recherches" at the F.R.S.-FNRS. U.S. investigators were supported by the National Aeronautics and Space Administration. We acknowledge support from the Institut National des Sciences de l'Univers" (INSU), the "Centre National de la Recherche Scientifique" (CNRS) and "Centre National d'Etudes Spatiales" (CNES) through the "Programme National de Planetologie".

The Cameron bands and the UV doublet are two of the most prominent emission systems in the UV in Mars dayside. Their altitude variation has been exploited in the past to derive thermospheric temperatures from measurements obtained by the Mariner 6, 7, and 9 missions, the SPICAM instrument on board Mars Express, and the IUVS instrument on board MAVEN. Here we identify and quantify possible biases in these temperature determinations. For this purpose, we use a global model able to simulate these two emission systems, and we compare the temperature derived from the simulated emission with that predicted by the model at the same location and time. We find that an exponential fit to the scale height of the UV doublet can be used to derive temperatures with an error less than 10 K at altitudes above about 170 km and for low and moderate values of the Solar Zenith Angle. The temperature derived from the Cameron bands is biased towards higher values due to the non-negligible contribution of CO to the emission. We find that, at 170 km, the difference between the temperature derived from the Cameron bands and the UV doublet can be related to the CO abundance. Our results have implications for previous temperature determinations from the Mariners, SPICAM/MEx and IUVS/MAVEN, some of them being biased by about 25 K. © 2021 Elsevier Inc. All rights reserved., The IAA team acknowledges financial support from the Agencia Estatal de Investigacion (AEI) of the Spanish Ministerio de Ciencia, Innovacion y Universidades (MCIU) through the "Center of Excellence Severo Ochoa'' award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709). FG-G and MALV are funded by the Spanish MCIU, the AEI, and EU FEDER funds under projects RTI2018-100920-J-I00 and PGC2018-101836-B-100, respectively.

Methane (CH4) on Mars has attracted a great deal of attention since it was first detected in January 2003. As methane is considered a potential marker for past/present biological or geological activity, any possible detection would require evidence with strong statistical significance. Ethane (C2H6) and ethylene (C2H4) are also relevant chemical species as their shorter lifetimes in the Martian atmosphere make them excellent tracers for recent and ongoing releases. If detected, a CH4/C2Hn ratio could aid in constraining the potential source of organic production. Here we present the results of an extensive search for hydrocarbons in the Martian atmosphere in 240,000 solar occultation measurements performed by the ExoMars Trace Gas Orbiter/NOMAD instrument from April 2018 to April 2019. The observations are global, covering all longitudes and latitudes from 85°N to 85°S, and sampled from 6 to 100 km altitude with a typical vertical resolution of 2 km. There were no statistically significant detections of organics and new stringent upper limits for global ethane and ethylene were set at 0.1 ppbv and 0.7 ppbv, respectively. No global background level of methane was observed, obtaining an upper limit of 0.06 ppbv, in agreement with early results from ExoMars (Korablev et al., 2019). Dedicated searches for localized plumes at more than 2000 locations provided no positive detections, implying that if methane were released in strong and rapid events, the process would have to be sporadic. © 2020 Elsevier Inc. All rights reserved., The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB-BIRA), assisted by Co-PI teams from Spain (IAACSIC), 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 Spanish Ministry of Science and Innovation (MCIU) 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 and ST/S00145X/1 and Italian Space Agency through grant 2018-2-HH.0. This work was supported by the Belgian Fonds de la Recherche Scientifique -FNRS under grant number 30442502 (ET_HOME). 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 Astrofisica de Andalucia (SEV-2017-0709). Canadian investigators were supported by the Canadian Space Agency. This work was supported by NASA's Mars Program Office under WBS 604796, "Participation in the TGO/NOMAD Investigation of Trace Gases on Mars". MC is 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 "Charge de Recherches" at the F.R.S.-FNRS. We would also like to thank Dr. Sara Faggi for valuable advice, expertise and continuous support during this study.

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).