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Exoplanets with cloud-free, haze-free atmospheres at the pressures probed by transmission spectroscopy represent a valuable opportunity for detailed atmospheric characterization and precise chemical abundance constraints. We present the first optical to infrared (0.3-5 microns) transmission spectrum of the hot Jupiter WASP-62b, measured with Hubble/STIS and Spitzer/IRAC. The spectrum is characterized by a 5.1-sigma detection of Na I absorption at 0.59 microns, in which the pressure-broadened wings of the Na D-lines are observed from space for the first time. A spectral feature at 0.4 microns is tentatively attributed to SiH at 2.1-sigma confidence. Our retrieval analyses are consistent with a cloud-free atmosphere without significant contamination from stellar heterogeneities. We simulate James Webb Space Telescope (JWST) observations, for a combination of instrument modes, to assess the atmospheric characterization potential of WASP-62b. We demonstrate that JWST can conclusively detect Na, H2O, FeH, and SiH within the scope of its Early Release Science (ERS) program. As the only transiting giant planet currently known in the JWST Continuous Viewing Zone, WASP-62b could prove a benchmark giant exoplanet for detailed atmospheric characterization in the James Webb era., Comment: 14 pages, 5 figures, accepted for publication in ApJL

We present Hubble Space Telescope (HST) near-ultraviolet (NUV) transits of the hot Jupiter WASP-121b, acquired as part of the PanCET program. Time-series spectra during two transit events were used to measure the transmission spectra between 2280 and 3070 Å at a resolution of 30,000. Using HST data from 61 Space Telescope Imaging Spectrograph visits, we show that data from HST's Pointing Control System can be used to decorrelate the instrument systematic errors (jitter decorrelation), which we used to fit the WASP-121b light curves. The NUV spectra show very strong absorption features, with the NUV white light curve found to be larger than the average optical and near-infrared value at 6σ confidence. We identify and spectrally resolve absorption from the Mg ii doublet in the planetary exosphere at a 5.9σ confidence level. The Mg ii doublet is observed to reach altitudes of R pl/R star = 0.284 ± 0.037 for the 2796 Å line and 0.242 ± 0.0431 for the 2804 Å line, which exceeds the Roche lobe size as viewed in transit geometry (R eqRL/R star = 0.158). We also detect and resolve strong features of the Fe ii UV1 and UV2 multiplets, and observe the lines reaching altitudes of R pl/R star ≈ 0.3. At these high altitudes, the atmospheric Mg ii and Fe ii gas is not gravitationally bound to the planet, and these ionized species may be hydrodynamically escaping or could be magnetically confined. Refractory Mg and Fe atoms at high altitudes also indicate that these species are not trapped into condensate clouds at depth, which places constraints on the deep interior temperature.

We present HST near-ultraviolet (NUV) transits of the hot Jupiter WASP-121b, acquired as part of the PanCET program. Time series spectra during two transit events were used to measure the transmission spectra between 2280 and 3070 Angstroms at a resolution of 30,000. Using HST data from 61 STIS visits, we show that data from HST's Pointing Control System can be used to decorrelate the instrument systematic errors (Jitter Decorrelation), which we used to fit the WASP-121b light curves. The NUV spectrum show very strong absorption features, with the NUV white light curve found to be larger than the average optical and near-infrared value at 6-$\sigma$ confidence. We identify and spectrally resolve absorption from the Mg ii doublet in the planetary exosphere at a 5.9-$\sigma$ confidence level. The Mg ii doublet is observed to reach altitudes of $R_{pl}/R_{star}=0.284\pm0.037$ for the 2796 Angstrom line and $0.242\pm0.0431$ in the 2804 Angstrom line, which exceeds the Roche lobe size as viewed in transit geometry ($R_{\rm eqRL}/R_{star}$ = 0.158). We also detect and resolve strong features of the Fe ii UV1 and UV2 multiplets, and observe the lines reaching altitudes of $R_{pl}/R_{star}\approx0.3$. At these high altitudes, the atmospheric Mg ii and Fe ii gas is not gravitationally bound to the planet, and these ionized species may be hydrodynamically escaping or could be magnetically confined. Refractory Mg and Fe atoms at high altitudes also indicates that these species are not trapped into condensate clouds at depth, which places constraints on the deep interior temperature., Comment: 22 pages, 16 figures, 2 Tables. Accepted for publication in AJ. Spectra available at https://pages.jh.edu/~dsing3

Biofouled vessels create novel, mobile habitats characterized by great abundances of opportunistic and non-native species. Vessel biofouling1 affects the environment as well as the economics of vessel management...

We present HST near-ultraviolet (NUV) transits of the hot Jupiter WASP-121b, acquired as part of the PanCET program. Time series spectra during two transit events were used to measure the transmission spectra between 2280 and 3070 Angstroms at a resolution of 30,000. Using HST data from 61 STIS visits, we show that data from HST's Pointing Control System can be used to decorrelate the instrument systematic errors (Jitter Decorrelation), which we used to fit the WASP-121b light curves. The NUV spectrum show very strong absorption features, with the NUV white light curve found to be larger than the average optical and near-infrared value at 6-$\sigma$ confidence. We identify and spectrally resolve absorption from the Mg ii doublet in the planetary exosphere at a 5.9-$\sigma$ confidence level. The Mg ii doublet is observed to reach altitudes of $R_{pl}/R_{star}=0.284\pm0.037$ for the 2796 Angstrom line and $0.242\pm0.0431$ in the 2804 Angstrom line, which exceeds the Roche lobe size as viewed in transit geometry ($R_{\rm eqRL}/R_{star}$ = 0.158). We also detect and resolve strong features of the Fe ii UV1 and UV2 multiplets, and observe the lines reaching altitudes of $R_{pl}/R_{star}\approx0.3$. At these high altitudes, the atmospheric Mg ii and Fe ii gas is not gravitationally bound to the planet, and these ionized species may be hydrodynamically escaping or could be magnetically confined. Refractory Mg and Fe atoms at high altitudes also indicates that these species are not trapped into condensate clouds at depth, which places constraints on the deep interior temperature., Comment: 22 pages, 16 figures, 2 Tables. Accepted for publication in AJ. Spectra available at https://pages.jh.edu/~dsing3

Detergent extracts of Trypanosoma cruzi epimastigotes catalysed the hydrolysis of a range of amino-acyl and peptidyl p-nitro-anilides and aminomethylcoumarins. At least three enzymes were detected that cleave Z-Phe-Arg-MCA. Two of these were optimally active at alkaline pH, the other at pH 4·0. Of the two enzymes with alkaline pH optima, one was a cysteine peptidase and was unable to cleave Bz-Arg-MCA readily, whilst the other cleaved Bz-Arg-MCA and was inhibited by diisopropyl fluorophosphate. The acidic enzyme was similar to cathespin L of other eukayrotes with respect to its pH profile, substrate-specificity and inhibitor-sensitivity. Evidence was presented that epimastigotes contain a cysteine-type dipeptidyl aminopeptidase, one or more aminopeptidases, and a serine peptidase that cleaves Boc-Ala-Ala-pNA. Digitonin solubilization of the activities from cells supports the hypothesis that the cathespin L-like enzyme and the dipeptidyl aminopeptidase are lysosomal, whilst the Bz-Arg-MCA hydrolase, the aminopeptidases and the Boc-Ala-Ala-pNA serine peptidase are cytosolic

Non-PR, IFPRI5; CRP4, PHND; A4NH, CGIAR Research Program on Agriculture for Nutrition and Health (A4NH), This paper asserts that schools offer a unique platform from which to realize multiple benefits for children and their communities, while helping to achieve the SDGs. Furthermore, schools can exert influence beyond the student population, serving as a foundation for the involvement of teachers, parents and other community members. Intervention can catalyze community development, bring about social protection and economic empowerment, influence agricultural production systems to deliver diverse and nutritious foods, promote lifelong healthy-eating habits, and address basic health, hygiene, and sanitation issues that affect wellbeing. By providing a better health and living environment, schools have the potential to not only support education, but also underpin mainstream nutrition activities in communities and advance child development (Patton et al. 2016).

School health and nutrition (SHN) programs are critical for achieving education for all (EFA) as research has shown that improvements in health status contribute to improvements in learning and academic outcomes. Through programs targeted to address major health conditions that are highly prevalent among poor schoolchildren, (for example, iron deficiency anemia, hunger, worm infections, diarrheal disease, and malaria) SHN programs can have a large impact on children’s education, increasing the time that they spend at school and their ability to learn while at school. SHN programs are recognized as important educational policy initiatives to improve education outcomes. Furthermore, schools provide an excellent platform for the delivery of child health and nutrition services, where they can strengthen the cost-effectiveness of health interventions and deliver gains in participation and learning. In this paper, the policy platform is documented as well as the type, coverage, and the effect of the SHN interventions, followed by the key areas identified for development and learning of the school health promotion program (SHPP).

School health and nutrition (SHN) programs are critical for achieving education for all (EFA) as research has shown that improvements in health status contribute to improvements in learning and academic outcomes. Through programs targeted to address major health conditions that are highly prevalent among poor schoolchildren, (for example, iron deficiency anemia, hunger, worm infections, diarrheal disease, and malaria) SHN programs can have a large impact on children’s education, increasing the time that they spend at school and their ability to learn while at school. SHN programs are recognized as important educational policy initiatives to improve education outcomes. Furthermore, schools provide an excellent platform for the delivery of child health and nutrition services, where they can strengthen the cost-effectiveness of health interventions and deliver gains in participation and learning. In this paper, the policy platform is documented as well as the type, coverage, and the effect of the SHN interventions, followed by the key areas identified for development and learning of the school health promotion program (SHPP).

School health and nutrition (SHN) programs are critical for achieving education for all (EFA) as research has shown that improvements in health status contribute to improvements in learning and academic outcomes. Through programs targeted to address major health conditions that are highly prevalent among poor schoolchildren, (for example, iron deficiency anemia, hunger, worm infections, diarrheal disease, and malaria) SHN programs can have a large impact on children’s education, increasing the time that they spend at school and their ability to learn while at school. SHN programs are recognized as important educational policy initiatives to improve education outcomes. Furthermore, schools provide an excellent platform for the delivery of child health and nutrition services, where they can strengthen the cost-effectiveness of health interventions and deliver gains in participation and learning. In this paper, the policy platform is documented as well as the type, coverage, and the effect of the SHN interventions, followed by the key areas identified for development and learning of the school health promotion program (SHPP).

We determined the flux ratios of the heavy and eccentric planet XO-3b to its parent star in the four IRAC bands of the Spitzer Space Telescope: 0.101% +- 0.004% at 3.6 micron; 0.143% +- 0.006% at 4.5 micron; 0.134% +- 0.049% at 5.8 micron and 0.150% +- 0.036% at 8.0 micron. The flux ratios are within [-2.2,0.3, -0.8, -1.7]-sigma of the model of XO-3b with a thermally inverted stratosphere in the 3.6 micron, 4.5 micron, 5.8 micron and 8.0 micron channels, respectively. XO-3b has a high illumination from its parent star (Fp ~(1.9 - 4.2) x 10^9 ergs cm^-2 s^-1) and is thus expected to have a thermal inversion, which we indeed observe. When combined with existing data for other planets, the correlation between the presence of an atmospheric temperature inversion and the substellar flux is insufficient to explain why some high insolation planets like TrES-3 do not have stratospheric inversions and some low insolation planets like XO-1b do have inversions. Secondary factors such as sulfur chemistry, atmospheric metallicity, amounts of macroscopic mixing in the stratosphere or even dynamical weather effects likely play a role. Using the secondary eclipse timing centroids we determined the orbital eccentricity of XO-3b as e = 0.277 +- 0.009. The model radius-age trajectories for XO-3b imply that at least some amount of tidal-heating is required to inflate the radius of XO-3b, and the tidal heating parameter of the planet is constrained to Qp < 10^6 ., Comment: Accepted for publications in The Astrophysical Journal

We determined the flux ratios of the heavy and eccentric planet XO-3b to its parent star in the four IRAC bands of the Spitzer Space Telescope: 0.101% +- 0.004% at 3.6 micron; 0.143% +- 0.006% at 4.5 micron; 0.134% +- 0.049% at 5.8 micron and 0.150% +- 0.036% at 8.0 micron. The flux ratios are within [-2.2,0.3, -0.8, -1.7]-sigma of the model of XO-3b with a thermally inverted stratosphere in the 3.6 micron, 4.5 micron, 5.8 micron and 8.0 micron channels, respectively. XO-3b has a high illumination from its parent star (Fp ~(1.9 - 4.2) x 10^9 ergs cm^-2 s^-1) and is thus expected to have a thermal inversion, which we indeed observe. When combined with existing data for other planets, the correlation between the presence of an atmospheric temperature inversion and the substellar flux is insufficient to explain why some high insolation planets like TrES-3 do not have stratospheric inversions and some low insolation planets like XO-1b do have inversions. Secondary factors such as sulfur chemistry, atmospheric metallicity, amounts of macroscopic mixing in the stratosphere or even dynamical weather effects likely play a role. Using the secondary eclipse timing centroids we determined the orbital eccentricity of XO-3b as e = 0.277 +- 0.009. The model radius-age trajectories for XO-3b imply that at least some amount of tidal-heating is required to inflate the radius of XO-3b, and the tidal heating parameter of the planet is constrained to Qp < 10^6 ., Comment: Accepted for publications in The Astrophysical Journal

A workshop was held 6-16 January 2008 to evaluate the ability of various analysis methods to detect, enumerate, and determine the viability of phytoplankton at concentrations to be expected after treatment by successful ballast water treatment systems. Researchers from Woods Hole Oceanographic Institute, Moss Landing Marine Laboratory, Naval Research Laboratory, and Fluid Imaging Technologies were provided with six samples with known concentrations of live and dead Tetraselmis species in prepared seawater. A seventh sample contained live Tetraselmis plus dissolved organic matter and mineral matter to better mimic actual ballast water samples. Methods investigated included manual microscopy with vital stains, microscopy of concentrated samples stained with different stains, flow cytometry of stained organisms, pulsed amplitude modulated (PAM) fluorometry, and an enhanced flow-through system with imaging capability. Statistical analyses were performed on the results. Overall the methods were all self-consistent. Although there were differences from sample to sample, comparisons showed no real differences could be established indicating one method is better than others. Advantages and disadvantages of each analytical method for routine use are provided., The original document contains color images. All DTIC reproductions will be in black and white. Prepared in cooperation with U.S. Coast Guard Research and Development Center, Groton, CT.

Onychomycosis is a widespread refractory disease deleteriously affecting quality of life via social stigma and disrupting daily activities. Many physicians perceive onychomycosis as a cosmetic rather than a medical problem., Journal Article, Research Support, Non-U.S. Gov't, info:eu-repo/semantics/published

Onychomycosis is a widespread refractory disease deleteriously affecting quality of life via social stigma and disrupting daily activities. Many physicians perceive onychomycosis as a cosmetic rather than a medical problem., Journal Article, Research Support, Non-U.S. Gov't, info:eu-repo/semantics/published

Detergent extracts of Trypanosoma cruzi epimastigotes catalysed the hydrolysis of a range of amino-acyl and peptidyl p-nitro-anilides and aminomethylcoumarins. At least three enzymes were detected that cleave Z-Phe-Arg-MCA. Two of these were optimally active at alkaline pH, the other at pH 4·0. Of the two enzymes with alkaline pH optima, one was a cysteine peptidase and was unable to cleave Bz-Arg-MCA readily, whilst the other cleaved Bz-Arg-MCA and was inhibited by diisopropyl fluorophosphate. The acidic enzyme was similar to cathespin L of other eukayrotes with respect to its pH profile, substrate-specificity and inhibitor-sensitivity. Evidence was presented that epimastigotes contain a cysteine-type dipeptidyl aminopeptidase, one or more aminopeptidases, and a serine peptidase that cleaves Boc-Ala-Ala-pNA. Digitonin solubilization of the activities from cells supports the hypothesis that the cathespin L-like enzyme and the dipeptidyl aminopeptidase are lysosomal, whilst the Bz-Arg-MCA hydrolase, the aminopeptidases and the Boc-Ala-Ala-pNA serine peptidase are cytosolic