Low anterior resection syndrome (LARS) is associated with a severe negative impact on patients’ quality of life (QOL). In a recent prospective randomized controlled trial (RCT) by our group, early (“prophylactic”) use of transanal irrigation (TAI) following rectal resection for rectal cancer was shown to improve symptoms associated with LARS significantly compared with a group under supportive therapy (ST) within 1 and 3 months following closure of the protective ileostomy. The aim of the present study was to evaluate the outcome after 12 months when patients had the option to choose between the two therapeutic options and/or modify the regimen of TAI (volume and time). In the RCT, 18 patients had been allocated to start with TAI following ileostomy closure, while 19 patients remained on ST only. Once the 3-month follow-up had been completed patients could choose between TAI or ST, respectively, and were invited for follow-up after 12 months. The maximum number of bowel movements during the day and the Wexner and LARS score as well as physical (PC) and mental (MC) component of the SF-36 questionnaire were evaluated. Furthermore, in patients who had changed their treatment arm, reasons for this decision were reported. Six patients were lost to follow-up (all in the ST group). One patient from the ST group started with TAI due to problems associated with LARS, bringing the total number of TAI patients to 19. Nine patients from the previous TAI arm changed to ST due to the long duration of the emptying process (n: 8) or pain during TAI (n: 1), respectively. After 12 months, the median volume of water used for irrigation was 600 ml (range 200–1000 ml). The ten patients who continued with TAI patients showed a lower number of defecation episodes per daytime (TAI median 3; 1–6, ST median 5; 2–10, p: 0.018) and per night (TAI median 0; 0–1, ST median 1; 0–5, p: 0.004) compared to the ST group. Although the LARS score was lower in patients who used TAI after 12 months (TAI median 18; 9–32, ST median 30; 3–39), this failed to reach the level of significance (p: 0.063). Evaluation of the Wexner score and the 36-item Short Form Health Survey as well as comparison of patients who remained on TAI (n: 9) versus those who had stopped TAI after 3 months (n: 9) failed to find any statistically significant difference between TAI and ST. This follow-up study revealed that a considerable number of patients decided to stop TAI within 12 months. However, the number of bowel movements during the day were still lower when TAI was used than when patients had ST only. Randomized trial. DRKS00011752, https://apps.who.int/trialsearch/.

We study the inclusive production of J/psi and psi(2S) mesons originating from the decays of bottom-flavored hadrons produced in p anti-p collisions at the Fermilab Tevatron and in pp collisions at the CERN LHC. We work at next-to-leading order in the general-mass variable-flavor-number scheme (GM-VFNS) implemented with nonperturbative fragmentation functions fitted to e^+e^- data of inclusive b-hadron production exploiting their universality. The three-momentum distributions of the charmonia used were extracted from B-decay data in the framework of nonrelativistic-QCD factorization. Comparing the theoretical predictions thus obtained with transverse-momentum distributions measured by the CDF II, ALICE, ATLAS, CMS, and LHCb Collaborations, we find excellent overall agreement as for both absolute normalization and lineshape, which provides a nontrivial test of the GM-VFNS over wide ranges of center-of-mass energy, transverse momentum, and rapidity.

Zusammenfassung Einleitung Während der letzten Jahrzehnte hat die Häufigkeit von Übergewicht und Adipositas dramatisch zugenommen. Für Beide Entitäten sind mit einem hohen Risiko für metabolische und kardiovaskuläre Folgeund Begleiterkrankungen assoziiert. Die vorliegende Studie untersuchte das metabolische und kardiovaskuläre Risikoprofil in einer Kohorte von Kindern und Jugendlichen mit Übergewicht und/oder Adipositas. Patienten und Methoden Alle 519 Kinder und Jugendlichen mit Übergewicht oder Adipositas (Alter 13,6 ± 2,6 Jahre, BMI 30,9 ± 5,2 kg/m2, BMI-SDS 2,44 ± 0,53), die sukzessive in die MEDIGREIF Inselklinik Heringsdorf zwischen dem 01.01.2006 und dem 31.07.2010 eingewiesen worden waren zur Teilnahme an einem strukturierten Behandlungs- und Schulungsprogramm zur Gewichtsreduktion, wurden in die Studie eingeschlossen. Ergebnisse Während einer stationären Behandlungsperiode von 36,2 ± 8,1 Tagen erzielten die Patienten signifikante Reduktionen des BMI (von 30,9 ± 5,2 auf 28,5 ± 4,8 kg/m2, p<0,05), des BMI-SDS (von 2,44 ± 0,53 auf 2,11 ± 0,62, p<0,05), der Fettmasse (von 32,1 ± 12,5 auf 26,9 ± 10,5 kg, p<0,05) und des prozentualen Körperfettanteils (von 37,3 ± 7,0 auf 34,0 ± 6,6 %, p<0,05). Zu Beginn der Untersuchung ergaben sich positive Korrelationen zwischen BMI-SDS und dem Gesamtcholesterin, dem LDL-Cholesterin und Triglyceriden (r=0,28, p<0,05, r=0,26, p<0,05, r=0,12, p<0.05), sowie eine negative Korrelation für HDL-Cholesterin (r=−0,24, p<0,05). 216/519 Patienten (42%) hatten eine mittlere Harnsäure-Konzentration oberhalb des Grenzwertes von 380,0 μmol/l. Es ergab sich eine positive Korrelation mit dem BMISDS (r=0,36, p<0,05). Während der 24-Stunden Blutdruck-Messung lagen der systolische Wert bei 123,1 ± 11,0, der diastolische bei 68,8 ± 7,5 mmHg. Auch der systolische und diastolische Blutdruck zeigten signifikante Korrelationen mit dem BMI und dem BMI-SDS (r=0,37, p<0,05, r=0,25, p<0,05). Die mittlere Carotis Intima-Media-Dicke betrug 0,49 ± 0,07 mm. 394/519 (76 %) Kinder hatten erhöhte Werte ≥0,45 mm, 296/519 (57 %) der Kinder und Jugendlichen hatten noch weit höhere Werte von ≥0,50 mm. Die Korrelation zwischen der Carotis Intima-Media-Dicke und dem BMI-SDS betrug r=0,39 (p<0,05). Das CRP betrug im Median <0,50 mg/dl (range, <0,5–6,80 mg/dl). Erhöhte Werte (oberhalb des Grenzwertes von 0,50 mg/dl) zeigten 127/519 Patienten (25 %). Auch hinsichtlich des C-reaktiven Proteins (CRP) ergab sich eine Korrelation mit dem BMI-SDS (r=0,17, p<0,05). Insgesamt zeigten ca. 78 % der Kinder und Jugendlichen mit Übergewicht und Adipositas, die eingewiesen wurden zur Teilnahme an einem stationären strukturierten Behandlungs- und Schulungsprogramm zur Gewichtsreduktion, mindestens einen metabolischen oder kardiovaskulären Risikofaktor. Schlussfolgerungen Bei Kindern und Jugendlichen mit Übergewicht und Adipositas ist die Prävalenz von metabolischen und kardiovaskulären Risikofaktoren sehr hoch. Konsequenterweise haben diese Patienten ein sehr hohes Risiko für eine erhöhte Morbidität. Eine frühe Identifikation und Intervention erscheinen auf diesem Hintergrund unbedingt notwendig.

[1] The NASA Discovery Moon Mineralogy Mapper imaging spectrometer was selected to pursue a wide range of science objectives requiring measurement of composition at fine spatial scales over the full lunar surface. To pursue these objectives, a broad spectral range imaging spectrometer with high uniformity and high signal-to-noise ratio capable of measuring compositionally diagnostic spectral absorption features from a wide variety of known and possible lunar materials was required. For this purpose the Moon Mineralogy Mapper imaging spectrometer was designed and developed that measures the spectral range from 430 to 3000 nm with 10 nm spectral sampling through a 24 degree field of view with 0.7 milliradian spatial sampling. The instrument has a signal-to-noise ratio of greater than 400 for the specified equatorial reference radiance and greater than 100 for the polar reference radiance. The spectral cross-track uniformity is >90% and spectral instantaneous field-of-view uniformity is >90%. The Moon Mineralogy Mapper was launched on Chandrayaan-1 on the 22nd of October. On the 18th of November 2008 the Moon Mineralogy Mapper was turned on and collected a first light data set within 24 h. During this early checkout period and throughout the mission the spacecraft thermal environment and orbital parameters varied more than expected and placed operational and data quality constraints on the measurements. On the 29th of August 2009, spacecraft communication was lost. Over the course of the flight mission 1542 downlinked data sets were acquired that provide coverage of more than 95% of the lunar surface. An end-to-end science data calibration system was developed and all measurements have been passed through this system and delivered to the Planetary Data System (PDS.NASA.GOV). An extensive effort has been undertaken by the science team to validate the Moon Mineralogy Mapper science measurements in the context of the mission objectives. A focused spectral, radiometric, spatial, and uniformity validation effort has been pursued with selected data sets including an Earth-view data set. With this effort an initial validation of the on-orbit performance of the imaging spectrometer has been achieved, including validation of the cross-track spectral uniformity and spectral instantaneous field of view uniformity. The Moon Mineralogy Mapper is the first imaging spectrometer to measure a data set of this kind at the Moon. These calibrated science measurements are being used to address the full set of science goals and objectives for this mission.

High spectral and spatial resolution data from the Moon Mineralogy Mapper (M3) instrument on Chandrayaan‐1 are used to investigate in detail changes in the optical properties of lunar materials accompanying space weathering. Three spectral parameters were developed and used to quantify spectral effects commonly thought to be associated with increasing optical maturity: an increase in spectral slope (“reddening”), a decrease in albedo (“darkening”), and loss of spectral contrast (decrease in absorption band depth). Small regions of study were defined that sample the ejecta deposits of small fresh craters that contain relatively crystalline (immature) material that grade into local background (mature) soils. Selected craters are small enough that they can be assumed to be of constant composition and thus are useful for evaluating trends in optical maturity. Color composites were also used to identify the most immature material in a region and show that maturity trends can also be identified using regional soil trends. The high resolution M3 data are well suited to quantifying the spectral changes that accompany space weathering and are able to capture subtle spectral variations in maturity trends. However, the spectral changes that occur as a function of maturity were observed to be dependent on local composition. Given the complexity of space weathering processes, this was not unexpected but poses challenges for absolute measures of optical maturity across diverse lunar terrains.

MAPPER DATA: FIRST RESULTS. P. J. Isaacson, J. Nettles, S. Besse, J. Boardman, L. Cheek, R. Clark, D. Dhingra, K. Donaldson Hanna, J. Head, R. Klima, G. Kramer, U. Mall, D. Moriarty, J. Mustard, N. Petro, C. Pieters, J. Sunshine, L. Taylor, S. Tompkins, J. Whitten, Dept. Geol. Sci., Brown Univ., [Peter_Isaacson@Brown.edu], Univ. of MD, AIG, USGS Denver, JHU/APL, LPI, Max Planck Inst., NASA GSFC, Univ. of TN, DARPA.

Introduction and Background: The history of volcanism on the western near side of the Moon is unique in both its duration and the basaltic compositions it left behind on the lunar surface. Together, Oceanus Procellarum and Mare Imbrium compose the largest expanse of the lunar maria with deposits ranging from the early history of lunar volcanism through its last major phases. Various techniques have dated many of these flows as younger than 3.0 Ga [1] with some areas having erupted as recently as ~1.2 Ga [2, 3], or almost two billion years after the youngest basalts collected by sample return missions. These last major phases of lunar volcanism produced spectrally unique, high-titanium basalts that cover large areas of Procellarum and Imbrium as well as smaller regions within several surrounding maria. The reflectance properties of soils and craters within these deposits display a relatively strong 1 μm feature and a weaker 2 μm absorption, suggesting the presence of abundant olivine [4, 5, 6]. However, previous telescopic and orbital measurements lack the combined spectral and spatial resolutions necessary for detailed mineralogical characterizations of these basalts. In the current study, visible to near-infrared reflectance data acquired by the Moon Mineralogy Mapper (M) on Chandrayaan-1 are used to investigate the mineralogy of these late-stage basalts and implications for the heterogeneity and evolution of their source regions. M Data Analysis: The M imaging spectrometer was a guest instrument on India’s Chandrayaan-1 mission which launched on October 22, 2008 and mapped the lunar surface from a polar orbit through August of 2009. M acquired visible to infrared reflectance data at spatial and spectral resolutions capable of measuring discrete basaltic flows within the lunar maria. This global data covers the wavelength range of ~430 to 3000 nm in 85 spectral bands at 140 to 280 m/pixel. Small amounts of data were also acquired of targeted regions in 259 spectral bands and at higher spatial resolutions. To perform preliminary compositional assessments, global mosaics were created by reducing the spatial resolution of the M data by a factor of 10 [7]. After calibration of the data to apparent reflectance and the application of thermal corrections [8, 9], a range of spectral parameters were calculated to explore broad mineralogical differences across the Moon. Figure 1 provides an example of a hemispheric color composite image that distinguishes several near side mare regions based on their 1 and 2 μm integrated band depths (IBD) and near infrared albedo. The latestage western maria are unique within this color composite due to their relatively weak 2 μm absorptions and strong 1 μm ferrous bands (distinguished by red hues in this color composite image).

The last major phases of lunar volcanism produced spectrally unique high-titanium basalts on the western nearside of the Moon. The Moon Mineralogy Mapper (M-3) on Chandrayaan-1 has provided detailed measurements of these basalts at spatial and spectral resolutions necessary for mineralogical interpretation and mapping of distinct compositional units. The M-3 imaging spectrometer acquired data in 85 spectral bands from similar to 430 to 3000 nm at 140 to 280 m/pixel in its global mapping mode during the first half of 2009. Reflectance data of several key sites in the western maria were also acquired at higher spatial and spectral resolutions using M-3's target mode, prior to the end of the Chandrayaan-1 mission. These new observations confirm that both fresh craters and mare soils within the western high-Ti basalts display strong 1 mm and weak 2 mm absorptions consistent with olivine-rich basaltic compositions. The inferred abundance of olivine is observed to correlate with stratigraphic sequence across different mare regions and absolute ages. The apparent stratigraphic evolution and Fe-rich compositions of these basalts as a whole suggest an origin from evolved residual melts rather than through the assimilation of more primitive olivine-rich sources. Mare deposits with spectral properties similar to these late stage high-Ti basalts appear to be very limited outside the Procellarum-Imbrium region of the Moon and, where present, appear to occur as small areas of late stage regional volcanism. Detailed analyses of these new data and supporting measurements are in progress to provide further constraints on the mineralogy, olivine abundance, and compositions of these final products of lunar volcanism and the nature and evolution of their source regions.

The search for water on the surface of the anhydrous Moon had remained an unfulfilled quest for 40 years. However, the Moon Mineralogy Mapper (M-3) on Chandrayaan-1 has recently detected absorption features near 2.8 to 3.0 micrometers on the surface of the Moon. For silicate bodies, such features are typically attributed to hydroxyl- and/or water-bearing materials. On the Moon, the feature is seen as a widely distributed absorption that appears strongest at cooler high latitudes and at several fresh feldspathic craters. The general lack of correlation of this feature in sunlit M-3 data with neutron spectrometer hydrogen abundance data suggests that the formation and retention of hydroxyl and water are ongoing surficial processes. Hydroxyl/water production processes may feed polar cold traps and make the lunar regolith a candidate source of volatiles for human exploration.

Introduction The Moon Mineralogy Mapper (M), which flew on India’s Chandrayaan-1 has provided the lunar science community with a richest view of our Moon to date. Information of the lunar surface returned by M provided the first conclusive evidence of the presence of OH, and possibly H2O at the poles, and in isolated locations as far down as the equator [1]. The coming discoveries and new views of our moon [see related abstracts within this conference] we owe to the vastly improved spectral resolution of the M instrument over previous lunar orbiters in particular the reining standard, Clementine’s ultravioletvisible (UVVIS) camera [2]. M’s spectral range is 4 times that of Clementine UVVIS, M’s spectral resolution (85 channels) is improved over Clementine UVVIS (5 channels), and M’s spatial resolution (∼150 m/pixel over all channels) is improved over Clementine’s (higher end at ∼125 m/pixel for the 750 nm channel and lower end at ∼250 m/pixel for the 415 nm channel). How does this improvement manifest in the data? How do M spectra compare with those from Clementine? Is it simply a matter of more detail in a spectrum? In an effort to answer some of these questions we focused on Mare Nectaris a region previously studied in detail by [3]. We used the same technique of Small Crater Rim and Ejecta Probing (SCREP) [4] to extract “fresh” spectral information from pixels that depict the rims and proximal ejecta of small, immature craters (0.5-5 km in diameter) that impacted into the mare basalt. These small craters act as windows through the ubiquitous, obscuring regolith, exposing the underlying, uncontaminated mare basalt [5, 6, 3]. Impact cratering studies and analysis of impact ejecta mechanics demonstrate that near the crater rim the original stratigraphy of the impact target is inverted [e.g., 7]. Therefore collecting data from this region provides the best approach to deriving the composition of the underlying basaltic unit [8].