Search

The mid-infrared channel of the Atmospheric Chemistry Suite (ACS MIR) onboard the ExoMars Trace Gas Orbiter is capable of observing the infrared absorption of ozone (O3) in the atmosphere of Mars. During solar occulations, the 003←000 band (3000-3060 cm-1) is observed with spectral sampling of ∼0.045 cm-1. Around the equinoxes in both hemispheres and over the southern winters, we regularly observe around 200-500 ppbv of O3 below 30 km. The warm southern summers, near perihelion, produce enough atmospheric moisture that O3 is not detectable at all, and observations are rare even at high northern latitudes. During the northern summers, water vapour is restricted to below 10 km, and an O3 layer (100-300 ppbv) is visible between 20-30 km. At this same time, the aphelion cloud belt forms, condensing water vapour and allowing O3 to build up between 30-40 km. A comparison to vertical profiles of water vapour and temperature in each season reveals that water vapour abundance is controlled by atmospheric temperature, and H2O and O3 are anti-correlated as expected. When the atmosphere cools, over time or over altitude, water vapour condenses (observed as a reduction in its mixing ratio) and the production of odd hydrogen species is reduced, which allows O3 to build up. Conversely, warmer temperatures lead to water vapour enhancements and ozone loss. The LMD Mars Global Climate Model is able to reproduce vertical structure and seasonal changes of temperature, H2O, and O3 that we observe. However, the observed O3 abundance is larger by factors between 2 and 6, indicating important differences in the rate of odd-hydrogen photochemistry.

The Emirates Mars Mission (EMM) was launched to Mars in the summer of 2020, and is the first interplanetary spacecraft mission undertaken by the United Arab Emirates (UAE). The mission has multiple programmatic and scientific objectives, including the return of scientifically useful information about Mars. Three science instruments on the mission’s Hope Probe will make global remote sensing measurements of the Martian atmosphere from a large low-inclination orbit that will advance our understanding of atmospheric variability on daily and seasonal timescales, as well as vertical atmospheric transport and escape. The mission was conceived and developed rapidly starting in 2014, and had aggressive schedule and cost constraints that drove the design and implementation of a new spacecraft bus. A team of Emirati and American engineers worked across two continents to complete a fully functional and tested spacecraft and bring it to the launchpad in the middle of a global pandemic. EMM is being operated from the UAE and the United States (U.S.), and will make its data freely available.

The Atmospheric Chemistry Suite (ACS) onboard the ExoMars Trace Gas Orbiter (TGO) monitors the Martian atmosphere through different spectral intervals in the infrared light. We present a retrieval algorithm tailored to the analysis of spectra acquired in nadir geometry by TIRVIM, the thermal infrared channel of ACS. Our algorithm simultaneously retrieves vertical profile of atmospheric temperature up to 50 km, surface temperature, and integrated optical depth of dust and water ice clouds. The specificity of the TIRVIM dataset lies in its capacity to resolve the diurnal cycle over a 54 sol period. However, it is uncertain to what extent can the desired atmospheric quantities be accurately estimated at different times of day. Here we first present an Observing System Simulation Experiment (OSSE). We produce synthetic observations at various latitudes, seasons and local times and run our retrieval algorithm on these synthetic data, to evaluate its robustness. Different sources of biases are documented, in particular regarding aerosol retrievals. Atmospheric temperature retrievals are found robust even when dust and/or water ice cloud opacities are not well estimated in our OSSE. We then apply our algorithm to TIRVIM observations in April-May, 2018 and perform a cross-validation of retrieved atmospheric temperature and dust integrated opacity by comparisons with thousands of co-located Mars Climate Sounder (MCS) retrievals. Most differences between TIRVIM and MCS atmospheric temperatures can be attributed to differences in vertical sensitivity. Daytime dust opacities agree well with each other, while biases are found in nighttime dust opacity retrieved from TIRVIM at this season., 51 pages, 29 figures. Accepted in Juanuary 2022 for publication in Journal of Geophysical Research (Planets)

Exposed scarps images and ice-penetrating radar measurements in the North Polar Layered Deposits (NPLD) of Mars show alternating layers that provide an archive of past climate oscillations, that are thought to be linked to orbital variations, akin to Milankovitch cycles on Earth. We use the Laboratoire de Meteorologie Dynamique (LMD) Martian Global Climate Model (GCM) to study paleoclimate states to enable a better interpretation of the NPLD physical and chemical stratigraphy. When a tropical ice reservoir is present, water vapor transport from the tropics to the poles at low obliquity is modulated by the intensity of summer. At times of low and relatively constant obliquity, the flux still varies due to other orbital elements, promoting polar layer formation. Ice migrates from the tropics towards the poles in two stages. First, when surface ice is present in the tropics, and second, when the equatorial deposit is exhausted, from ice that was previously deposited in mid-high latitudes. The polar accumulation rate is significantly higher when tropical ice is available, forming thicker layers per orbital cycle. However, the majority of the NPLD is sourced from ice that temporary resided in the mid-high latitudes and the layers become thinner as the source location moves poleward. The migration stages imprint different D/H ratios in different sections in the PLDs. The NPLD is isotopically depleted compared to the SPLD in all simulations. Thus we predict the D/H ratio of the atmosphere in contact with NPLD upper layers is biased relative to the average global ice reservoirs., Comment: 23 pages, 7 figures. JGR-planets (2022)

J.M.O. acknowledges financial support from the Portuguese Foundation for Science and Technology (FCT) and the European Social Fund (ESF) through the PhD grant SFRH/BD/131700/2017. The work leading to these results has received funding from the European Research Council under the European Community's H2020 2014-2021 ERC grant Agreement nffi 669416 "Lucky Star". We thank S. Para who supported some travels to observe the 5 October 2017 occultation. T.B. was supported for this research by an appointment to the National Aeronautics and Space Administration (NASA) Post-Doctoral Program at the Ames Research Center administered by Universities Space Research Association (USRA) through a contract with NASA. We acknowledge useful exchanges with Mark Gurwell on the ALMA CO observations. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. J.L.O., P.S.-S., N.M. and R.D. acknowledge financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709), they also acknowledge the financial support by the Spanish grant AYA-2017-84637-R and the Proyecto de Excelencia de la Junta de Andalucia J.A. 2012-FQM1776. The research leading to these results has received funding from the European Union's Horizon 2020 Research and Innovation Programme, under Grant Agreement no. 687378, as part of the project "Small Bodies Near and Far" (SBNAF). P.S.-S. acknowledges financial support by the Spanish grant AYA-RTI2018-098657-J-I00 "LEO-SBNAF". The work was partially based on observations made at the Laboratorio Nacional de Astrofisica (LNA), Itajuba-MG, Brazil. The following authors acknowledge the respective CNPq grants: F.B.-R. 309578/2017-5; R.V.-M. 304544/2017-5, 401903/2016-8; J.I.B.C. 308150/2016-3 and 305917/2019-6; M.A. 427700/20183, 310683/2017-3, 473002/2013-2. This study was financed in part by the Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior -Brasil (CAPES) -Finance Code 001 and the National Institute of Science and Technology of the e-Universe project (INCT do e-Universo, CNPq grant 465376/2014-2). G.B.R. acknowledges CAPES-FAPERJ/PAPDRJ grant E26/203.173/2016 and CAPES-PRINT/UNESP grant 88887.571156/2020-00, M.A. FAPERJ grant E26/111.488/2013 and A.R.G.Jr. FAPESP grant 2018/11239-8. B.E.M. thanks CNPq 150612/2020-6 and CAPES/Cofecub-394/2016-05 grants. Part of the photometric data used in this study were collected in the frame of the photometric observations with the robotic and remotely controlled telescope at the University of Athens Observatory (UOAO; Gazeas 2016). The 2.3 m Aristarchos telescope is operated on Helmos Observatory by the Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing of the National Observatory of Athens. Observations with the 2.3 m Aristarchos telescope were carried out under OPTICON programme. This project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 730890. This material reflects only the authors views and the Commission is not liable for any use that may be made of the information contained therein. The 1. 2m Kryoneri telescope is operated by the Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing of the National Observatory of Athens. The Astronomical Observatory of the Autonomous Region of the Aosta Valley (OAVdA) is managed by the Fondazione Clement Fillietroz-ONLUS, which is supported by the Regional Government of the Aosta Valley, the Town Municipality of Nus and the "Unite des Communes valdotaines Mont-Emilius". The 0.81 m Main Telescope at the OAVdA was upgraded thanks to a Shoemaker NEO Grant 2013 from The Planetary Society. D.C. and J.M.C. acknowledge funds from a 2017 'Research and Education' grant from Fondazione CRT-Cassa di Risparmio di Torino. P.M. acknowledges support from the Portuguese Fundacao para a Ciencia e a Tecnologia ref. PTDC/FISAST/29942/2017 through national funds and by FEDER through COMPETE 2020 (ref. POCI010145 FEDER007672). F.J. acknowledges Jean Luc Plouvier for his help. S.J.F. and C.A. would like to thank the UCL student support observers: Helen Dai, Elise Darragh-Ford, Ross Dobson, Max Hipperson, Edward Kerr-Dineen, Isaac Langley, Emese Meder, Roman Gerasimov, Javier Sanjuan, and Manasvee Saraf. We are grateful to the CAHA, OSN and La Hita Observatory staffs. This research is partially based on observations collected at Centro Astronomico HispanoAleman (CAHA) at Calar Alto, operated jointly by Junta de Andalucia and Consejo Superior de Investigaciones Cientificas (IAA-CSIC). This research was also partially based on observation carried out at the Observatorio de Sierra Nevada (OSN) operated by Instituto de Astrofisica de Andalucia (CSIC). This article is also based on observations made with the Liverpool Telescope operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. Partially based on observations made with the Tx40 and Excalibur telescopes at the Observatorio Astrofisico de Javalambre in Teruel, a Spanish Infraestructura Cientifico-Tecnica Singular (ICTS) owned, managed and operated by the Centro de Estudios de Fisica del Cosmos de Aragon (CEFCA). Tx40 and Excalibur are funded with the Fondos de Inversiones de Teruel (FITE). A.R.R. would like to thank Gustavo Roman for the mechanical adaptation of the camera to the telescope to allow for the observation to be recorded. R.H., J.F.R., S.P.H. and A.S.L. have been supported by the Spanish projects AYA2015-65041P and PID2019-109467GB-100 (MINECO/FEDER, UE) and Grupos Gobierno Vasco IT1366-19. Our great thanks to Omar Hila and their collaborators in Atlas Golf Marrakech Observatory for providing access to the T60cm telescope. TRAPPIST is a project funded by the Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) under grant PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liege, and performed in collaboration with Cadi Ayyad University of Marrakesh. E.J. is a FNRS Senior Research Associate., Context. A stellar occultation by Neptune's main satellite, Triton, was observed on 5 October 2017 from Europe, North Africa, and the USA. We derived 90 light curves from this event, 42 of which yielded a central flash detection. Aims. We aimed at constraining Triton's atmospheric structure and the seasonal variations of its atmospheric pressure since the Voyager 2 epoch (1989). We also derived the shape of the lower atmosphere from central flash analysis. Methods. We used Abel inversions and direct ray-tracing code to provide the density, pressure, and temperature profiles in the altitude range similar to 8 km to similar to 190 km, corresponding to pressure levels from 9 mu bar down to a few nanobars. Results. (i) A pressure of 1.18 +/- 0.03 mu bar is found at a reference radius of 1400 km (47 km altitude). (ii) A new analysis of the Voyager 2 radio science occultation shows that this is consistent with an extrapolation of pressure down to the surface pressure obtained in 1989. (iii) A survey of occultations obtained between 1989 and 2017 suggests that an enhancement in surface pressure as reported during the 1990s might be real, but debatable, due to very few high S/N light curves and data accessible for reanalysis. The volatile transport model analysed supports a moderate increase in surface pressure, with a maximum value around 2005-2015 no higher than 23 mu bar. The pressures observed in 1995-1997 and 2017 appear mutually inconsistent with the volatile transport model presented here. (iv) The central flash structure does not show evidence of an atmospheric distortion. We find an upper limit of 0.0011 for the apparent oblateness of the atmosphere near the 8 km altitude., Portuguese Foundation for Science and Technology SFRH/BD/131700/2017, European Social Fund (ESF) SFRH/BD/131700/2017, European Research Council under the European Community's H2020 2014-2021 ERC grant 669416, Spanish Government SEV-2017-0709 AYA-2017-84637-R AYA-RTI2018-098657-J-I00, Junta de Andalucia 2012-FQM1776, European Union's Horizon 2020 Research and Innovation Programme, as part of the project "Small Bodies Near and Far" (SBNAF) 687378, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ), Fundacao de Apoio a Pesquisa do Distrito Federal (FAPDF) 309578/2017-5 304544/2017-5 401903/2016-8 308150/2016-3 305917/2019-6 427700/2018-3 310683/2017-3 473002/2013-2, Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) 001, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ) 465376/2014-2 CAPES-FAPERJ/PAPDRJ grant E26/203.173/2016 CAPES-PRINT/UNESP grant 88887.571156/2020-00, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio De Janeiro (FAPERJ) E26/111.488/2013, Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) 2018/11239-8, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPQ) 150612/2020-6, European Union's Horizon 2020 research and innovation programme 730890, Regional Government of the Aosta Valley, Town Municipality of Nus, Unite des Communes valdotaines Mont-Emilius, Planetary Society, Fondazione CRT-Cassa di Risparmio di Torino, Portuguese Foundation for Science and Technology PTDC/FISAST/29942/2017, FEDER through COMPETE 2020 POCI010145 FEDER007672, UK Research & Innovation (UKRI), Science & Technology Facilities Council (STFC), Fondos de Inversiones de Teruel (FITE), Spanish Government AYA2015-65041P PID2019-109467GB-100, Grupos Gobierno Vasco IT1366-19, Fonds de la Recherche Scientifique - FNRS PDR T.0120.21, University of Liege, CAPES/Cofecub-394/2016-05

We have implemented full CO ice cloud microphysics into the LMD Mars Global Climate Model (MGCM) and we have conducted the first global simulations. The microphysical model implementation follows the modal scheme used for water ice cloud microphysics in the MGCM, but includes specific aspects that need to be accounted for when dealing with CO ice clouds. These include nucleation of CO on water ice crystals and CO condensation theory adapted for the Martian conditions. The model results are compared to available observations globally, and separately for polar regions and equatorial mesosphere. The observed seasonal and latitudinal variability of the CO ice clouds is in general reproduced. The polar regions are covered by CO ice clouds during the winter as observed. Instead of forming only in the lowest 10–15 km of the atmosphere, they extend up to several tens of kilometers above the surface in the model, dictated by the modeled temperature structure. We have also quantified the contribution of the cloud microphysics to the surface CO ice deposits. Snowfall from these clouds contributes up to 10% of the atmosphere–surface ice flux in the polar regions in our simulations, in the range that has been indirectly deduced from observations. In the mesosphere, notable amounts of CO ice clouds form only when water ice crystals are used as condensation nuclei in addition to dust particles, and their spatial distribution is in agreement with observations. The mesospheric temperature structure, dominated by tides, dictates the longitudinal and seasonal distribution of these clouds. The seasonal and local time variations of the clouds are not fully reproduced by the model. There is a long pause in CO ice cloud formation in the model around the aphelion season, but clouds have been observed during this period, although with a lower apparition frequency. Modeled mesospheric clouds form mainly during the night and in the morning, whereas during the daytime, when most of the cloud observations have been made, the model rarely predicts clouds. These discrepancies could be explained by the strong dependence of the cloud formation process on mesospheric temperatures that are themselves challenging to reproduce and sensitive to the MGCM processes and parameters. The rare possibilities for nighttime observations might also bias the observational climatologies towards daytime detections. Future developments of the model consist in the inclusion of a possible exogenous condensation nucleus source in the mesosphere and the radiative effect of CO ice clouds. © 2022 Elsevier Inc. All rights reserved., This paper presents the results of ten years of development that has been supported by funding from several sources. We thank the Agence National de la Recherche for funding (project MECCOM, ANR-18-CE31-0013). We are also grateful for the financial support by the LabEx (Laboratoire d’Excellence) ESEP, by the French space agency CNES and the European Space Agency ESA. We acknowledge the support of the French national planetology programme (PNP) as well. F.G.-G. is funded by the Spanish Ministerio de Ciencia, Innovación y Universidades, the Agencia Estatal de Investigación and EC FEDER funds under project RTI2018-100920-J-I00, and acknowledges financial support from the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). This work was performed using HPC computing resources from GENCI-CINES (Grant 2021-A0100110391), and resources at the ESPRI mesocentre of the IPSL institute .

Background: TAK-228 is an investigational, oral and highly selective ATP-competitive inhibitor of TORC1/2. Targeting the PI3K/AKT/mTOR pathway with the dual TORC1/2 inhibitor TAK-228 may restore sensitivity to endocrine therapies in patients (pts) with breast cancer who have progressed on the combination of an endocrine agent plus a TORC1 inhibitor. Here we report data from the phase 2 portion of a phase 1b/2 study of TAK-228 plus exemestane (E) or fulvestrant (F). Methods: Postmenopausal women with ER+ and HER2-, inoperable or metastatic breast cancer (MBC) following everolimus (EVE) plus E or F after progression, received oral TAK-228 (4 mg QD) plus E (25 mg QD) or F (500 mg monthly) for 28-day cycles until progressive disease (PD) or unacceptable toxicity (NCT02049957). Pts were enrolled into parallel cohorts based on prior response to EVE plus E or F and were given the same prior therapy (E or F) at their established dose: EVE-sensitive, defined as disease progression after complete response (CR), partial response (PR), or ≥6 mos stable disease (SD); or EVE-resistant, defined as disease progression without a CR or PR, or after Results: From Oct 2015 to Dec 2017, 94 pts were enrolled. Median age was 58 y (range 32–83). At baseline, most pts (67%) had stage IV disease and others were stage IA–IIIC (24%), other (3%) or unknown (5%); 94% of EVE-sensitive (93% E vs 100% F) and 88% of EVE-resistant pts (91% E vs 75% F) had received ≥4 prior lines of therapy. Pts received a median of 3 cycles (1–15) of TAK-228. At data cutoff (24 Apr 2018), 98% of pts had discontinued treatment, mainly due to PD (76%) or adverse events (AEs; 14%). CBR-16 was 41% (n=21) in EVE-sensitive and 26% (n=11) in EVE-resistant pts (table). CBR-24 was 24% in EVE-sensitive (19% E vs 50% F) and 23% in EVE-resistant (23% E vs 25% F) pts. Eleven of 21 pts who achieved CBR-16 also achieved CBR-24 (6 SD, 5 PR) in the EVE-sensitive cohort and 8 of 11 pts in the EVE-resistant cohort (6 SD, 2 PR). The ORR was 12% in EVE-sensitive pts and 9% in EVE-resistant pts (table). Median PFS (95% CI) was 4.1 mos (2.2–5.5) and 3.4 mos (1.9–5.4), and median OS (95% CI) was 15.9 mos (14.1–19.5) and 14.0 mos (13.0–16.0) in the EVE-sensitive and -resistant cohorts, respectively. Drug-related any grade and grade ≥3 AEs were seen in 90% and 29% of pts, respectively. Most common drug-related any grade AEs were nausea (50%), fatigue (38%), hyperglycemia and diarrhea (each 29%); 22% of pts reported a serious AE. No deaths were reported. Treatment is ongoing in two pts. Conclusion: TAK-228 plus E or F showed modest clinical benefit in pts with previously treated, EVE-sensitive or -resistant MBC, with an acceptable safety profile. EVE-sensitive (N=51)EVE-resistant (N=43) TAK-228+TAK-228+Best response, n (%)E (n=43)F (n=8)E (n=35)F (n=8)ORR=CR+PR4 (9)2 (25)3 (9)1 (13)CR001 (3)0PR4 (9)2 (25)2 (6)1 (13)CBR-1617 (40)4 (50)9 (26)2 (25) Citation Format: Diamond JR, Potter D, Salkeni M, Silverman P, Haddad T, Forget F, Awada A, Canon J-L, Danso M, Lortholary A, Bourgeois H, Tan-Chiu E, Patel C, Neuwirth R, Leonard EJ, Lim B. Phase 2 safety and efficacy results of TAK-228 in combination with exemestane or fulvestrant in postmenopausal women with ER-positive/HER2-negative metastatic breast cancer previously treated with everolimus [abstract]. In: Proceedings of the 2018 San Antonio Breast Cancer Symposium; 2018 Dec 4-8; San Antonio, TX. Philadelphia (PA): AACR; Cancer Res 2019;79(4 Suppl):Abstract nr PD1-09.

WOS:000558450600011; International audience; Owing to difficulties in accessing the vast open ocean, the beta (β) diversity of pelagic fish assemblages remains poorly studied. We investigated the relationship between assemblage similarity and geographical distance between anchored fish aggregating devices (FADs), sampled by standardised underwater visual censuses in three anchored FAD arrays in the Indian Ocean—at the Maldives, the Seychelles and Mauritius. The use of two complementary indices of β-diversity, based on presence/absence data (Jaccard similarity coefficient) and abundance data (Bray–Curtis index), revealed that geographical distance between sampling sites (from 4 to 257 km) appeared to have no effect on the similarity of fish assemblages associated with FADs within each array. The results of this preliminary study question the generalisation of the paradigm of an increase in β-diversity with geographic distance to the open-ocean fish community. Large-scale studies using a variety of datasets should be conducted to further investigate patterns of β-diversity in the open ocean.

Objectives: Niraparib is a poly(ADP-ribose) polymerase (PARP) inhibitor approved as maintenance treatment for patients (pts) with newly diagnosed advanced or recurrent ovarian cancer following a response to platinum-based chemotherapy (CT) doublet. The PRIMA/ENGOT-OV26/GOG-3012 (NCT02655016) study showed that niraparib following first-line treatment improved progression-free survival (PFS) in the overall intention-to-treat (ITT) population (hazard ratio [HR] 0.62; 95% CI 0.50-0.76). Methods: This double-blind, placebo (PBO)-controlled, phase 3 trial evaluated niraparib in pts with newly diagnosed, advanced, high-grade serous or endometrioid ovarian, primary peritoneal, or fallopian tube cancer with a complete or partial response to first-line CT. Pts were considered to be at a high risk for disease progression based on their clinical characteristics. This post-hoc analysis presents the efficacy of niraparib, measured by PFS, based on time of surgery and residual disease status, and was not powered to determine differences among the subgroups. Results: Data cutoff was May 2019. In total, 733 pts were randomized in the PRIMA study. Efficacy outcomes by surgical timing, either primary debulking surgery (PDS) or interval debulking surgery (IDS), and postoperative residual disease status, either no visible residual disease (NVRD) or visible residual disease (VRD), are shown in Table. Pts who underwent PDS or IDS had similar efficacy with niraparib maintenance treatment versus PBO in the ITT population (PFS HRs were 0.67 and 0.57, respectively). Niraparib treatment reduced risk of progression by 42% in pts who received PDS and had VRD, 35% in those with IDS and NVRD, and 59% in those with IDS and VRD. Efficacy was not evaluable for pts with PDS and NVRD due to low sample size. Download : Download high-res image (142KB) Download : Download full-size image Conclusions: In this post-hoc analysis, the impact of residual disease after PDS or IDS on the efficacy of niraparib was comparable across subgroups. Pts with IDS and VRD had the highest reduction in the risk of progression

International audience; Pneumatic actuators have inherent compliance and hence they are very interesting for applications involving interaction with environment or human. But controlling such kind of actuators is not trivial. The paper presents an implementation of iterative Linear Quadratic regulator (iLQR) based optimal control framework to control an anthropomorphic arm with each joint actuated by an agonist-antagonistic pair of Mckibben artificial muscles. The method is applied to positioning tasks and generation of explosive movements by maximizing the link speed. It is then compared to traditional control strategies to justify that optimal control is effective in controlling the position in highly non-linear pneumatic systems. Also the importance of varying compliance is highlighted by repeating the tasks at different compliance level. The algorithm validation is reported here by several simulations and hardware experiments in which the shoulder and elbow flexion are controlled simultaneously.

Objectif de l’etude Notre etude vise a mesurer l’impact de campagnes d’information sur le bon usage du medicament destinees aux professionnels de sante en analysant l’evolution des prescriptions medicales collectees en vie reelle. Objectif de l’etude L’etude porte sur des medicaments dont un mauvais usage en prescription fait courir soit par sa frequence, soit par sa gravite, des risques inacceptables pour la sante des patients. Elle consiste dans un premier temps a observer en vie reelle les prescriptions de ces medicaments sur un echantillon representatif d’ordonnances, pendant une duree suffisante pour objectiver l’ampleur et la constance du mesusage initial, puis a realiser une campagne d’information aupres des prescripteurs tout en poursuivant l’observation, afin de mesurer l’evolution quantitative du mesusage par comparaison avec les observations initiales. Cette campagne est constituee de messages de bon usage, diffuses par des canaux multiples : courriel, site web, logiciels de prescription. Une attention particuliere est apportee a la contextualisation des messages vis-a-vis de la prescription en cause, autrement dit a la pertinence des notifications delivrees. La maniere dont ces messages sont visualises ou au contraire ignores par les professionnels est egalement analysee. Dans le strict respect de la confidentialite des patients et des professionnels de sante, l’observation des pratiques de prescription en vie reelle dans ces situations a risque a ete realisee grâce a une brique logicielle specialisee qui extrait du dossier medical et de l’ordonnance informatisee les informations permettant de detecter les contre-indications, les erreurs de posologie et les interactions medicamenteuses. Resultats L’etude, qui s’est deroulee a partir de mars 2017, a porte sur plus de 20 000 medecins liberaux utilisant la brique logicielle embarquee localement, soit environ 1 200 000 ordonnances par semaine. Pour chaque situation de prescription a risque etudiee, l’observation qui precede la campagne d’information sur le bon usage met en evidence un pourcentage relativement faible des cas de mesusage detectes (de 0,5 a 6,5 % des medicaments concernes, selon la situation en cause) et le caractere constant de ce pourcentage au cours du temps. Pendant la campagne d’information, nous constatons que les messages sont tres rarement debranches par le prescripteur, ce qui signifie qu’il les considere generalement comme utiles. Au cours du premier mois qui suit le debut de cette campagne, le pourcentage de mesusage detecte se reduit dans tous les cas de maniere statistiquement significative. Conclusion Cette etude demontre que des messages de bon usage a destination du prescripteur peuvent, si la campagne est bien realisee, avoir un impact favorable sur les pratiques. Elle demontre d’autre part qu’il est possible de mesurer en temps reel l’impact de ces campagnes grâce a l’usage de donnees de vie reelle dans le respect strict de la confidentialite des personnes.

International audience; With the rapid evolution of robotic technology, robots are expected to perform various complicated task. Explosive motions like throwing, kicking or jumping are some of the ambitious tasks interesting for researchers. In the present paper, we would like to present a ball throwing task performed by an anthropomorphic arm with each joint actuated by an agonist-antagonistic pair of Mckibben artificial muscles. Pneumatic actuators have inherent compliance and hence they are very interesting for applications involving interaction with environment or human. But controlling such kind of actuators is not trivial. The paper presents an implementation of iterative Linear Quadratic regulator (iLQR) based optimal control framework to control such actuators. The method is applied to positioning tasks and generation of explosive movements by throwing a ball to a maximum distance. It is then compared to traditional control strategies to justify that optimal control is effective in controlling the position in highly non-linear pneumatic systems. Also the importance of varying compliance is highlighted by repeating the tasks at different compliance level. The algorithm validation is reported here by several simulations and hardware experiments in which the shoulder and elbow flexion are controlled simultaneously.

Objective AGO-OVAR 16 demonstrated that pazopanib maintenance therapy significantly increased progression-free survival (PFS) in patients with ovarian cancer whose disease had not progressed after first-line therapy. In a sub-study, we evaluated the effect of clinically important germline BRCA1 and BRCA2 mutations on PFS. Methods Of 940 AGO-OVAR 16 participants, 664 had BRCA1 / 2 exon sequencing data (pazopanib, n =335; placebo, n =329). A Cox model was used to test the association between genetic variants and PFS. Results Ninety-seven of 664 patients (15%) carried clinically important BRCA1 / 2 mutations ( BRCA1 / 2 carriers: pazopanib 14%, placebo 16%). Median PFS was longer in BRCA1 / 2 mutation carriers than in BRCA1 / 2 non-carriers in the placebo arm (30.3 vs 14.1months, hazard ratio, 0.48; 95% confidence interval [CI]: 0.29–0.78; P =0.0031); a similar non-significant trend was noted with pazopanib (30.2 vs 17.7months, hazard ratio, 0.64; 95% CI: 0.40–1.03; P =0.069). Among BRCA1 / 2 non-carriers, PFS was longer for pazopanib-treated patients than placebo-treated patients (17.7 vs 14.1months, hazard ratio, 0.77; 95% CI: 0.62–0.97; P =0.024). Among BRCA1 / 2 carriers, there was no significant PFS difference between treatments, although numbers were small (pazopanib, 46; placebo, 51), resulting in a wide CI (hazard ratio, 1.36; 95% CI: 0.66–2.82). Conclusions Patients with clinically important BRCA1 / 2 mutations had better prognosis. BRCA1 / 2 mutation status might be added as strata in future trials in primary ovarian cancer.

Summary The concept of economic defendability states that individuals will only defend resources when the benefits outweigh the costs. Competitor density is one factor that influences resource defence among fishes, resource defence being predicted to be highest at intermediate competitor densities and reduced at higher and lower densities, producing a dome shaped relationship. We investigated the effects of competitor density using male swordtails, which form dominance hierarchies and have already been demonstrated to defend a food resource. We found that both aggression (F2,32 = 5.392; P = 0.010) and time at a food resource (F2,32 = 3.574; P = 0.040) vary with differences in competitor density, and that the frequency of aggression significantly predicts time at the food resource only at an intermediate density (P = 0.033; r2adj = 0.219). The ability to vary the level of defence with respect to the immediate environment may result in fitness benefits to male swordtails. Further studies examining changes in behaviour over time and examining interacting influencing factors would be beneficial.

Mars is a small planet with a thin atmosphere of almost pure carbon dioxide. To first order, the Martian meteorology can be compared with what one would expect on a cold, dry desert-like Earth. However, several phenomena make the Martian climate system more complex than it appears. First, as much as 30% of the carbon dioxide atmosphere condenses every winter at high latitude to form CO 2 ice polar caps, inducing large surface pressure variations all over the planet and an atmospheric circulation without equivalent on Earth. Second, a highly variable amount of suspended dust lifted by the winds modifies the radiative properties of the atmosphere, with sometime global dust storms able to totally shroud the planet. Last, a peculiar water cycle occurs on Mars, with water vapor transported by the atmosphere between the polar caps and possibly subsurface reservoirs, allowing the formation of clouds, hazes and frost. Telescopic and spacecraft observations have shown us that this complex climate system is highly variable, seasonally and from year to year, but these variations remain poorly understood. In fact, the Martian climate system has probably experienced large variations related to the oscillations in the parameters of the orbit and rotation of Mars (obliquity) a few millions or even thousand of years ago. These oscillations affected surface temperatures and the water cycle, inducing the mobilization and accumulation of large ice deposits in various locations on the planets. In a much distant past, it is also likely that Mars may have been a completely different planet. The observations of the geology (dry riverbeds and deltas, lacustrine sediments) and mineralogy (clay, sulfate) of the oldest surface on Mars dating back to more than 3 billions years ago provide evidence that liquid water was then abundant on the surface, at least episodically. Mars may have been warmed by a thicker atmosphere containing greenhouse gas and clouds, high geothermal fluxes, or episodically by large asteroid impacts.

Slope streaks are gravity-driven albedo features observed on martian slopes since the Viking missions. The debated mechanism of formation could involve alternatively dry granular flow or wet mass wasting. A systematic mapping of slope streaks from the High Resolution Stereo Camera is presented in this paper. Two regions known for their slope streaks activity have been studied, the first one is located close to Cerberus lava flow, and the second one is inside the Olympus Mons Aureole. The statistics of slope streaks shapes measured from orthorectified images confirm previous results from Mars Orbiter Camera surveys. Preferential orientations of slope streaks are reported. Slope streaks occur preferentially on west facing slopes at latitudes lower than 30° N for Olympus and on south–west facing slopes for Cerberus. Wind directions derived from a General Circulation Model during the dusty season correlate with these orientations. Furthermore, west facing slopes at Olympus have a thicker dust cover. These observations indicate that slope streaks are dust avalanches controlled by the preferential accumulation of dust in the downstream side of the wind flow. The paucity of slope streaks at high latitudes and their preferential orientation on south-facing slopes have been presented as an evidence for a potential role of H 2 O phase transition in triggering or flow. The potential role of H 2 O cannot be ruled out from our observations but the dust avalanche model together with the atmospheric circulation could potentially explain all observations. The role of H 2 O might be limited to a stabilizing effect of dust deposits on northward facing slopes at intermediate latitudes (30° N–33° N) and on all slopes further north.

The recent identification of large deposits of sulphates by remote sensing and in situ observations has been considered evidence of the past presence of liquid water on Mars. Here we report the unambiguous detection of diverse phyllosilicates, a family of aqueous alteration products, on the basis of observations by the OMEGA imaging spectrometer on board the Mars Express spacecraft. These minerals are mainly associated with Noachian outcrops, which is consistent with an early active hydrological system, sustaining the long-term contact of igneous minerals with liquid water. We infer that the two main families of hydrated alteration products detected-phyllosilicates and sulphates--result from different formation processes. These occurred during two distinct climatic episodes: an early Noachian Mars, resulting in the formation of hydrated silicates, followed by a more acidic environment, in which sulphates formed.

MafB oncoprotein detected by immunohistochemistry as a highly sensitive and specific marker for the prognostic unfavorable t(14;20) (q32;q12) in multiple myeloma patients

A dedicated mission to investigate exoplanetary atmospheres represents a major milestone in our quest to understand our place in the universe by placing our Solar System in context and by addressing the suitability of planets for the presence of life. EChO -the Exoplanet Characterisation Observatory- is a mission concept specifically geared for this purpose. EChO will provide simultaneous, multi-wavelength spectroscopic observations on a stable platform that will allow very long exposures. EChO will build on observations by Hubble, Spitzer and groundbased telescopes, which discovered the first molecules and atoms in exoplanetary atmospheres. EChO will simultaneously observe a broad enough spectral region -from the visible to the mid-IR- to constrain from one single spectrum the temperature structure of the atmosphere and the abundances of the major molecular species. The spectral range and resolution are tailored to separate bands belonging to up to 30 molecules to retrieve the composition and temperature structure of planetary atmospheres. The target list for EChO includes planets ranging from Jupiter-sized with equilibrium temperatures Teq up to 2000 K, to those of a few Earth masses, with Teq ~300 K. We have baselined a dispersive spectrograph design covering continuously the 0.4-16 micron spectral range in 6 channels (1 in the VIS, 5 in the IR), which allows the spectral resolution to be adapted from several tens to several hundreds, depending on the target brightness. The instrument will be mounted behind a 1.5 m class telescope, passively cooled to 50 K, with the instrument structure and optics passively cooled to ~45 K. EChO will be placed in a grand halo orbit around L2. We have also undertaken a first-order cost and development plan analysis and find that EChO is easily compatible with the ESA M-class mission framework., Comment: Accepted for publication in Experimental Astronomy, 23 pages, 15 figures

ESA's Venus Express probe has been in orbit since April 2006. Eight research papers in this issue present new results from the mission, covering the atmosphere, polar features, interactions with the solar wind and the controversial matter of venusian lightning. Hakan Svedham et al. open the section with a review of the similarities and (mostly) differences between Venus and its 'twin', the Earth. Andrew Ingersoll considers the latest results, and also how the project teams plan to make the most of the probe's remaining six years of life. Venus' mesosphere is a transition region between the retrograde super rotation at the top of the thick clouds and the solar-antisolar circulation in the thermosphere. The mesospheric distributions of HF, HCl, H2O and HDO are reported, and an unexpected extensive layer of warm air at altitudes 90–120 km on the nightside is found. Venus has thick clouds of H2SO4 aerosol particles extending from altitudes of 40 to 60 km. The 60–100 km region (the mesosphere) is a transition region between the 4 day retrograde superrotation at the top of the thick clouds and the solar–antisolar circulation in the thermosphere (above 100 km), which has upwelling over the subsolar point and transport to the nightside1,2. The mesosphere has a light haze of variable optical thickness, with CO, SO2, HCl, HF, H2O and HDO as the most important minor gaseous constituents, but the vertical distribution of the haze and molecules is poorly known because previous descent probes began their measurements at or below 60 km. Here we report the detection of an extensive layer of warm air at altitudes 90–120 km on the night side that we interpret as the result of adiabatic heating during air subsidence. Such a strong temperature inversion was not expected, because the night side of Venus was otherwise so cold that it was named the ‘cryosphere’ above 100 km. We also measured the mesospheric distributions of HF, HCl, H2O and HDO. HCl is less abundant than reported 40 years ago3. HDO/H2O is enhanced by a factor of ∼2.5 with respect to the lower atmosphere, and there is a general depletion of H2O around 80–90 km for which we have no explanation.

International audience; Global mineralogical mapping of Mars by the Observatoire pour la Mineralogie, l'Eau, les Glaces et l'Activite (OMEGA) instrument on the European Space Agency's Mars Express spacecraft provides new information on Mars' geological and climatic history. Phyllosilicates formed by aqueous alteration very early in the planet's history (the "phyllocian" era) are found in the oldest terrains; sulfates were formed in a second era (the "theiikian" era) in an acidic environment. Beginning about 3.5 billion years ago, the last era (the "siderikian") is dominated by the formation of anhydrous ferric oxides in a slow superficial weathering, without liquid water playing a major role across the planet.

Aim: Weekly paclitaxel (60mg/m2) and carboplatin (AUC 2.7) (TCw) has been shown to be an effective treatment in patients with recurrent or advanced gynaecological cancer (Vandenput Int J Gyn Cancer 2012; Torfs Eur J Cancer 2012; Cadron Gynecol Oncol, 2013). The main toxicity of the regimen has been neutropenia grade (G) 3-4 and or neutropenic fever. Methods: In this prospective study 108 patients were needed to detect a 15% reduction in the occurrence of G3-4 neutropenia (a: 0.05; b: 0.95) compared with the historical incidence of 84%, by using prophylactic filgrastim on day 5 of each of the 18 weekly planned courses. The main inclusion criteria were: measurable disease, platin-resistant or refractory epithelial ovarian carcinoma (OC), or recurrent or advanced endometrial (EC) or cervical cancer (CC), and no prior weekly or dose-dense TC. Results: 108 (3 cohorts of ovarian, endometrial and cervical cancer of each 36 patients) were included by 12 BGOG centers between February 20, 2012 and March 14, 2013. The median number of prior chemotherapy lines was 3 for OC, 2 for EC and 1 for CC, respectively. The percentage of G3-4 neutropenia was 34% (CI: 26%-44%; p Conclusions: TCw with G-CSF support is feasible with an acceptable toxicity in patients with platin-resistant or –refractory OC, and advanced or recurrent EC or CC. The incidence of G3-4neutropenia is lower with the addition of weekly G-CSF compared with earlier studies without the addition of prophylactic G-CSF. Disclosure: All authors have declared no conflicts of interest.

In patients with non-colon digestive carcinomas, various schedules and doses of 5-fluorouracil (5-FU) and leucovorin combined with cisplatin (CDDP) have been used extensively. The present study explored the toxicity and activity of a weekly 24-h infusion of high dose 5-FU modulated by high dose leucovorin with bi-weekly CDDP. 59 patients with measurable disease were treated with a weekly infusion of high dose 5-FU (2 or 2.6 g/m2)+leucovorin 500 mg/m2 for 6 weeks and a bi-weekly dose of CDDP (50 mg/m2). All patients had metastatic or locoregionally advanced disease and had a performance status < or =3. All patients were evaluable for toxicity and 58 for response. Toxicity was different according to the schedule of 5-FU. Serious adverse events occurred most frequently when 5-FU was given at a dose of 2.6 g/m2 with a high incidence of grade 3/4 neutropenia (16%) and febrile neutropenia (13%), and led to dose reductions in both CDDP and 5-FU in 13 patients (34%). For patients who started 5-FU at a dose of 2 g/m2, no reduction in 5-FU was required, and only 4 patients required a dose reduction of CDDP (19%). Grade 3/4 neutropenia was seen in 10% of patients of this group and only 1 patient required hospitalisation for febrile neutropenia. Other grade 3/4 toxicities were rare in both groups. Renal toxicity was infrequent and mild and did not require dose adjustments. The overall response rate was 33%; 19 patients achieved a partial responses (PR). No patient had a complete response (CR). The median duration of response was 5.7 months (range 2-24 months) and the median survival was 7.9 months ( range: 1-30, 95% confidence interval (CI): 7-9). The combination of weekly 24-h infusion of high dose 5-FU with leucovorin and bi-weekly cisplatin seems a well-tolerated and active treatment in non-colon digestive carcinomas. A dose of 2 g/m2 of 5-FU seems to be recommended.

3162 Background: 15 Belgian oncology centers are participating in an open-label Phase II trial of gefitinib (IRESSA) 500 mg/day in patients (pts) with advanced epidermal growth factor receptor-positive solid tumors who had failed ≥1 previous chemotherapy regimen and had no further chemotherapy treatment options. Here we report interim data. Methods: Pts received gefitinib 500 mg/day until disease progression. Objective tumor assessments, by RECIST, were made every 8 weeks and confirmed by repeat assessments ≥4 weeks later. Disease control rate (DCR) was defined as objective response (confirmed complete response or partial response [PR]) plus stable disease (SD) for ≥8 weeks. All adverse events (AEs) were reported and assessed by NCI-CTC version 2.0. Results: 193 pts have been enrolled with pancreatic cancer [21%], cervical cancer (CC) [19%], ovarian cancer (OC) [17%], sarcoma (S) [12%], cancer of unknown primary origin (U) [10%], hepatocellular carcinoma (HC) [9%], bladder cancer (BC) [7%], and endometria...