WISE/NEOWISE observations of Active Bodies in the Main Belt

We report results based on mid-infrared photometry of 5 active main belt objects (AMBOs) detected by the Wide-field Infrared Survey Explorer (WISE) spacecraft. Four of these bodies, P/2010 R2 (La Sagra), 133P/Elst-Pizarro, (596) Scheila, and 176P/LINEAR, showed no signs of activity at the time of the observations, allowing the WISE detections to place firm constraints on their diameters and albedos. Geometric albedos were in the range of a few percent, and on the order of other measured comet nuclei. P/2010 A2 was observed on April 2-3, 2010, three months after its peak activity. Photometry of the coma at 12 and 22 {\mu}m combined with ground-based visible-wavelength measurements provides constraints on the dust particle mass distribution (PMD), dlogn/dlogm, yielding power-law slope values of {\alpha} = -0.5 +/- 0.1. This PMD is considerably more shallow than that found for other comets, in particular inbound particle fluence during the Stardust encounter of comet 81P/Wild 2. It is similar to the PMD seen for 9P/Tempel 1 in the immediate aftermath of the Deep Impact experiment. Upper limits for CO2 & CO production are also provided for each AMBO and compared with revised production numbers for WISE observations of 103P/Hartley 2.Comment: 32 Pages, including 5 Figure

ExoMars TGO/NOMAD‐UVIS vertical profiles of ozone: Part 2: The high‐altitude layers of atmospheric ozone

Solar occultations performed by the Nadir and Occultation for MArs Discovery (NOMAD) ultraviolet and visible spectrometer (UVIS) onboard the ExoMars Trace Gas Orbiter (TGO) have provided a comprehensive mapping of atmospheric ozone density. The observations here extend over a full Mars year (MY) between April 21, 2018 at the beginning of the TGO science operations during late northern summer on Mars (MY 34, Ls = 163°) and March 9, 2020 (MY 35). UVIS provided transmittance spectra of the Martian atmosphere allowing measurements of the vertical distribution of ozone density using its Hartley absorption band (200 – 300 nm). The overall comparison to water vapor is found in the companion paper to this work (Patel et al., 2021). Our findings indicate the presence of (1) a high-altitude peak of ozone between 40 and 60 km in altitude over the north polar latitudes for at least 45% of the Martian year during mid-northern spring, late northern summer-early southern spring, and late southern summer, and (2) a second, but more prominent, high-altitude ozone peak in the south polar latitudes, lasting for at least 60% of the year including the southern autumn and winter seasons. When present, both high-altitude peaks are observed in the sunrise and sunset occultations, suggesting that the layers could persist during the day. Results from the Mars general circulation models predict the general behavior of these peaks of ozone and are used in an attempt to further our understanding of the chemical processes controlling high-altitude ozone on Mars

Multi-Band Search for Volcanic Outgassing in the Tharsis and Syrtis Major Regions on Mars

Ph.D. University of Hawaii at Manoa 2015.Includes bibliographical references.We carried out the first and most comprehensive to date (2015), ground-based, semisimultaneous, multi-band and multi-species search for sulphuretted gases (SO2, H2S, OCS and SO) above the Tharsis and Syrtis volcanic regions on Mars. The submillimeter search extended between 23 November 2011 and 25 May 2014 which corresponded to Mars' mid Northern Spring and mid Northern Summer seasons (Ls = 34 - 135°). SO2, SO and H2S were targeted at their rotational transitions at 346.652 GHz, 304.078 GHz and 300.505 Ghz, respectively, using the high-resolution heterodyne receiver Barney on the 10.4 m single-dish antenna of the Caltech Submillimeter Observatory (CSO), and SO2 at HARP on the 15 m James Clerk Maxwell Telescope (JCMT) at Maunakea, Hawai'i. No sulphuretted gases were detected. We infer 2σ upper limits across the disk of the planet using the CSO of 1.1 ppb, 0.7 ppb and 1.3 ppb for SO2, SO and H2S, respectively, and 3.1 ppb on SO2 using the JCMT. The infrared search covered OCS in its combination band (v1+v3) at 3.42 μm (2924 cm-1), during Mars' late Northern Spring and mid Northern Summer seasons, spanning Ls= 43° and Ls= 145°, between 15 Dec. 2011 and 13 June 2014, using the high resolution infrared spectrometer CSHELL on the 3 m NASA Infrared Telescope Facility (IRTF). No absorption of atmospheric OCS has been detected, and we infer a 2σ upper limit of 0.8 ppb on OCS. Our current limit 1.1 ppb for SO2 yields an outgassing rate of less than 55 tons/day. Compared to two terrestrial analogs, we would have been able to detect any volcanic release that is more than 4% the size of Kilauea (Hawai`i) or one twentieth the size of the Masaya volcano (Nicaragua). The mass rate of magma that is able to degas 55 tons of SO2 per day is estimated as 37 kilotons of magma per day, or 12,000 m3 per day (0.14 m3/s). The non detection of any of the sulfur compounds in the atmosphere of Mars provides limits to the level of current volcanic activity in the crust of Mars

The Climatology of Carbon Monoxide and Water Vapor on Mars as Observed by CRISM and Modeled by the GEM-Mars General Circulation Model

Radiative transfer modeling of near-infrared spectra taken by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instrument onboard Mars Reconnaissance Orbiter (MRO) enables the column-integrated abundance of carbon monoxide (CO) and water vapor (H 2 O) to be retrieved. These results provide a detailed global description of the seasonal and spatial distribution of CO in the Mars atmosphere and new information about the interannual variability of H2O. The CRISM retrievals show the seasonally and globally averaged carbon monoxide mixing ratio to be near 800 parts per million, but with strong seasonal variations, especially at high latitudes. At low latitudes, the carbon monoxide mixing ratio varies in response to the mean seasonal cycle of surface pressure and shows little variation with topography. At high latitudes, carbon monoxide is depleted in the summer hemisphere by a factor of two or more, while in the winter hemisphere there is relatively higher mixing ratio in regions with low-lying topography. Water vapor shows only modest interannual variations, with the largest observed difference being unusually dry conditions in the wake of the Mars Year 28 global dust storm. Modeling results from the GEM (Global Environmental Multiscale) - Mars general circulation model generally reproduce the observed seasonal and spatial trends and provide insight into the underlying physical processes

Prospective : comment traitera-t-on les tumeurs rénales et prostatiques et urothéliales dans 10 ans ?

International audienceForward thinking does not seek to predict the future, to unveil it as if it were already in existence, rather, its aim is to help us to construct it. Although today's epidemiological and therapeutic situations for urogenital tumours can evolve over the next 10~years, diagnostic and therapeutic methods, as well as the treatment and implementation of innovations, are already rapidly changing. Rather than reducing our prospective thinking to the therapeutic treatment of cancer only, we will aim at proposing a global sanitary vision that includes diagnosis, therapies, prevention, routine utilisation of technomedicine, genomics and even nanomedicine. This journey into the near future of tomorrow's cancerology holds the promise of being better adapted to the evolution of the medical thinking process. Imagining the way we will be treating renal, prostatic and urothelial tumours in 10~years' time is as much an introspection into our present day treatment system as a projection into its hoped for future evolution.La prospective n’a pas pour objet de prédire l’avenir, de nous le dévoiler, comme s’il s’agissait d’une chose déjà faite, mais de nous aider à le construire. Si le contexte épidémiologique et thérapeutique actuel de ces tumeurs urogénitales peut évoluer en 10 ans, les méthodes diagnostiques et thérapeutiques d’aujourd’hui, ainsi que les concepts de prise en charge et l’implémentation des innovations sont déjà en pleine mutation. Plutôt que de focaliser la prospective à 10 ans uniquement sur la thérapeutique des cancers, nous chercherons à proposer une vision globale sanitaire incluant diagnostics, thérapeutiques, préventions, et l’utilisation en routine de la technomédecine, la génômique ou encore la nanomédecine. Ce voyage, dans un futur proche dans la cancérologie de demain, promet d’être plus adapté à l’évolution du mode de penser la médecine. L’exercice d’imagination de la manière dont nous traiterons les tumeurs rénales, prostatiques et urothéliales dans 10 ans, est autant une introspection au sein de notre actuel système de soins, que la manière dont nous souhaitons et pouvons le voir évoluer

Surgical treatment of pulmonary aspergilloma: Current outcome

Objective: This retrospective study was designed to confirm that aggressive pulmonary resection can provide effective long-term palliation of disease for patients with pulmonary aspergilloma. Methods and results: From 1959 to 1998, 84 patients underwent a total of 90 operations for treatment of pulmonary aspergilloma in the Marie-Lannelongue Hospital. The mean follow-up period was 9 years, and 83% of the patients were followed up for 5 years or until death, if the latter occurred earlier. The median age was 44 years. The most common indications were hemoptysis (66%) and sputum production (15%). Fifteen patients (18%) had no symptoms. Tuberculosis and lung abscess were the most common underlying causes of lung disease (65%). The procedures were 70 lobar or segmental resections, 8 cavernostomies, and 7 pneumonectomies. Five thoracoplasties were required after lobectomy (3 patients) or pneumonectomy (2 patients). The operative mortality rate was 4%. The major complications were bleeding (23 patients), prolonged air leak (31 patients), respiratory failure (10 patients), and empyema (5 patients). The actuarial survival curve showed 84% survival at 5 years and 74% survival at 10 years. During the first 2 years, death was related to the surgical procedure and the underlying disease. In contrast, 85% of the survivors had a good late result. Conclusion: Lobar resection in both the symptomatic and the asymptomatic patients was conducted in low-risk settings. For patients whose condition is unfit for pulmonary resection, cavernostomy may need to be undertaken despite the high operative risk. The better survival rate in this study may have been due to the selection of patients with better lung function and localized pulmonary disease

A double-blind, randomised comparison of the anti-emetic efficacy of two intravenous doses of dolasetron mesilate and granisetron in patients receiving high dose cisplatin chemotherapy

This multicentre, double-blind, double-dummy, randomised trial was designed to compare the efficacy and safety of single intravenous doses of dolasetron mesilate and granisetron in the prevention of acute emesis and nausea due to high-dose (≥80 mg/m2) cisplatin. Single intravenous doses of 1.8 or 2.4 mg/kg of dolasetron mesilate or 3 mg of granisetron hydrochloride were administered in a volume of 50 ml over a 5-min period, beginning 30 min prior to cisplatin (≥80 mg/m2) administration. The number and timing of emetic episodes, time to administration of escape anti-emetic medication, severity of nausea by visual analogue scale (VAS), and safety were monitored for 24 h after the start of cisplatin-containing chemotherapy. Investigators' evaluations of overall efficacy and patients' satisfaction with therapy were recorded at the end of the 24-h study period. Of the 474 patients evaluable for efficacy, complete responses were achieved by 54, 47 and 48% of patients given dolasetron mesilate 1.8 mg/kg, dolasetron mesilate 2.4 mg/kg and granisetron, respectively. Statistically, treatment groups had comparable complete and complete plus major responses, times to first emesis, and use of escape medication; patient maximum nausea severity and treatment satisfaction ratings; and physician nausea severity and overall efficacy assessments. For the majority of efficacy endpoints, 1.8 mg/kg dolasetron mesilate produced numerically superior responses compared with the 2.4 mg/kg dose. Gender and prior chemotherapy were significant predictors of complete response; males and chemotherapy-naive patients had higher responses. The overall incidences of adverse events were comparable among the treatment groups; headache and diarrhoea were most common. In conclusion, 1.8 and 2.4 mg/kg of dolasetron mesilate and granisetron (3 mg) were equally effective in preventing nausea and vomiting induced by highly emetogenic cisplatin-containing chemotherapy. In addition, because no additional benefit was observed with 2.4 mg/kg of dolasetron mesilate and numerically greater responses were observed with the 1.8 mg/kg dose, the lower dose of 1.8 mg/kg is optimal for further clinical development. Copyright © 1996 Elsevier Science Ltd.SCOPUS: ar.jinfo:eu-repo/semantics/publishe

Latest results from ChemCam Passive Sky Spectroscopy at Gale Crater, Mars

International audienceThe Mars Science Laboratory's (MSL) ChemCam spectrometer measures atmospheric aerosol properties as well as O2 and H2O gas abundances by operating in passive mode and observing scattered sky light at two different elevation angles [e.g. 1,2]. The most important ChemCam passive sky results reported to date include: evidence (via comparisons with MSL's REMS humidity sensor) for strong diurnal surface-atmosphere exchange of water vapor [3]; dust aerosol particle size patterns, in good agreement with other instruments, which include a seasonally repeating pattern of dust particle size ranging from typically 0.7 (in the clear season) to 1.7 (in the dusty season) microns effective radius along with very large dust particle sizes in a global dust storm [4, 5, 6]; O2 column-averaged volume mixing ratio results that are unexpectedly high with variability well beyond expectations for a non-condensable trace gas [2], but which are affected by not yet fully quantified measurement uncertainties. The ChemCam passive sky results now span about 3000 sols, and we will present new results and model comparisons based on that extended data set with improved methodology and with new comparisons to other instruments. Among the interesting new results in the extended data set is the return of water vapor and O2 seasonal patterns to more normal behavior after significant deviations from typical behavior in the vicinity of the 2018 global dust storm. One important comparison that we will report on is with new high spatial resolution water vapor retrievals from CRISM (on Mars Reconnaissance Orbiter) -- these comparisons have implications for the vertical profile of water vapor and for interpreting discrepancies among the various orbit-derived data sets. The other comparison that we will focus on is with newly reported solar-occulation-derived O2 measurements from ACS on Trace Gas Orbiter[7] along with previously reported in-situ O2 results from MSL's SAM-GCMS[8]. [1]McConnochie, et al. (2018), Icarus, 307. [2] McConnochie, et al. (2019) AGU Fall Meeting. [3]Savijarvi et al. (2019) Icarus 319. [4]Lemmon et al. (2019) GRL. [5]Lemmon et al. (2019) 9th Int. Conf. on Mars #6298. [6]Vicente-Retortillo et al. (2017), GRL, 44. [7] Fedorova et al. (2021) EGU Meeting EGU21-14406. [8] Trainer, et al. (2019), JGR, 124

Gravity Wave Observations by the Mars Science Laboratory REMS Pressure Sensor and Comparison With Mesoscale Atmospheric Modeling With MarsWRF

Funding Information: Guzewich, Smith, and Khayat were supported by the MSL Participating Scientist program. de la Torre Juarez, Newman, Kahanp??, Vi?dez-Moreiras, and Richardson were supported by the Mars Science Laboratory mission. Mason was supported by the NASA Postdoctoral Program, administered by the Universities Space Research Association. A portion of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). Funding Information: Guzewich, Smith, and Khayat were supported by the MSL Participating Scientist program. de la Torre Juarez, Newman, Kahanpää, Viúdez‐Moreiras, and Richardson were supported by the Mars Science Laboratory mission. Mason was supported by the NASA Postdoctoral Program, administered by the Universities Space Research Association. A portion of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). Publisher Copyright: © 2021. American Geophysical Union. All Rights Reserved.Surface pressure measurements on Mars have revealed a wide variety of atmospheric phenomena. The Mars Science Laboratory Rover Environmental Monitoring Station pressure sensor data set is now the longest duration record of surface pressure on Mars. We use the first 2580 Martian sols, nearly 4 Mars years, of measurements to identify atmospheric pressure waves with periods of tens of minutes to hours using wavelet analysis on residual pressure after the tidal harmonics are removed. We find these waves have a clear diurnal cycle with strongest activity in the early morning and late evening and a seasonal cycle with the strongest waves in the second half of the martian year (Ls = 180–360°). The strongest such waves of the entire mission occurred during the Mars Year 34 global dust storm. Comparable atmospheric waves are identified using atmospheric modeling with the MarsWRF general circulation model in a “nested” high spatial resolution mode. With the support of the modeling, we find these waves best fit the expected properties of inertia-gravity waves with horizontal wavelengths of O(100s) of km.Peer reviewe