Gifted Education: A Multi-Case Study on the Identification Process of Historically Underrepresented Students in Gifted Programs in North Carolina

The purpose of this multiple case study was to explore how Newland, Big Hills, and Edison Elementary, which are public elementary schools in North Carolina, identify gifted students who are historically underrepresented for placement in academically gifted classes. Based on statistical data from the Department of Education and the North Carolina Department of Public Instruction, there is a disparity between the identification of Whites, Blacks, and Hispanics, especially in impoverished communities. The study sought to understand the process of identification of gifted students and how it contributes to under-representation of Black, Hispanic, and impoverished students. The study revealed what social characteristics and demographic data are prioritized in the process and what factors and values influence the process of identification in these schools by asking: what factors of identification procedures result in higher than average identification rates of historically underrepresented gifted students? The theory guiding this study is Social Dominance Theory by Sidanius and Pratto (1999), which holds that possible oppression and discrimination is subconscious and upheld by society as a whole, whether or not it works in favor of society. This study focused on 3 elementary schools that have data that supports a higher than average enrollment of gifted students that are historically underrepresented. At each school interviews were conducted with 10 – 15 participants who have direct contact with the gifted program: principals, assistant principals, gifted coordinators, psychologists, counselors, and lead teachers. Data from the interviews were analyzed for categories and themes to connect important in this manner, and adds to the growing empirical research. Specific documents were analyzed for additional data

Simultaneous Ka-Band Site Characterization: Goldstone, CA, White Sands, NM, and Guam, USA

To statistically characterize atmospheric effects on Ka-band links at NASA operational sites, NASA has constructed site test interferometers (STI s) which directly measure the tropospheric phase stability and rain attenuation. These instruments observe an unmodulated beacon signal broadcast from a geostationary satellite (e.g., Anik F2) and measure the phase difference between the signals received by the two antennas and its signal attenuation. Three STI s have been deployed so far: the first one at the NASA Deep Space Network Tracking Complex in Goldstone, California (May 2007); the second at the NASA White Sands Complex, in Las Cruses, New Mexico (February 2009); and the third at the NASA Tracking and Data Relay Satellite (TDRS) Remote Ground Terminal (GRGT) complex in Guam (May 2010). Two station-years of simultaneous atmospheric phase fluctuation data have been collected at Goldstone and White Sands, while one year of data has been collected in Guam. With identical instruments operating simultaneously, we can directly compare the phase stability and rain attenuation at the three sites. Phase stability is analyzed statistically in terms of the root-mean-square (rms) of the tropospheric induced time delay fluctuations over 10 minute blocks. For two years, the time delay fluctuations at the DSN site in Goldstone, CA, have been better than 2.5 picoseconds (ps) for 90% of the time (with reference to zenith), meanwhile at the White Sands, New Mexico site, the time delay fluctuations have been better than 2.2 ps with reference to zenith) for 90% of time. For Guam, the time delay fluctuations have been better than 12 ps (reference to zenith) at 90% of the time, the higher fluctuations are as expected from a high humidity tropical rain zone. This type of data analysis, as well as many other site quality characteristics (e.g., rain attenuation, infrastructure, etc.) will be used to determine the suitability of all the sites for NASA s future communication services at Ka-band

X-raying the Beating Heart of a Newborn Star: Rotational Modulation of High-energy Radiation from V1647 Ori

We report a periodicity of ~1 day in the highly elevated X-ray emission from the protostar V1647 Ori during its two recent multiple-year outbursts of mass accretion. This periodicity is indicative of protostellar rotation at near-breakup speed. Modeling of the phased X-ray light curve indicates the high-temperature (~50 MK), X-ray-emitting plasma, which is most likely heated by accretion-induced magnetic reconnection, resides in dense (>~5e10 cm-3), pancake-shaped magnetic footprints where the accretion stream feeds the newborn star. The sustained X-ray periodicity of V1647 Ori demonstrates that such protostellar magnetospheric accretion configurations can be stable over timescales of years.Comment: 26 pages, 10 figure

Salivary PYY: A Putative Bypass to Satiety

Peptide YY3-36 is a satiation hormone released postprandially into the bloodstream from L-endocrine cells in the gut epithelia. In the current report, we demonstrate PYY3-36 is also present in murine as well as in human saliva. In mice, salivary PYY3-36 derives from plasma and is also synthesized in the taste cells in taste buds of the tongue. Moreover, the cognate receptor Y2R is abundantly expressed in the basal layer of the progenitor cells of the tongue epithelia and von Ebner's gland. The acute augmentation of salivary PYY3-36 induced stronger satiation as demonstrated in feeding behavioral studies. The effect is mediated through the activation of the specific Y2 receptor expressed in the lingual epithelial cells. In a long-term study involving diet-induced obese (DIO) mice, a sustained increase in PYY3-36 was achieved using viral vector-mediated gene delivery targeting salivary glands. The chronic increase in salivary PYY3-36 resulted in a significant long-term reduction in food intake (FI) and body weight (BW). Thus this study provides evidence for new functions of the previously characterized gut peptide PYY3-36 suggesting a potential simple and efficient alternative therapeutic approach for the treatment of obesity

Metodología ABP para el Estudio de la Física

Hoy en día nos encontramos en una sociedad que emplea tecnología en su día a día, pero aún hay un sitio que la tecnología no ha podido conquistar del todo, la educación. Al revisar un aula evidenciamos que no ha tenido cambios significativos en muchos años lo cual genera un desinterés en los estudiantes y no los motiva a la investigación ni a la apropiación del conocimiento. Como solución se plantea una nueva estrategia didáctica usando las TIC y soportada por un Aprendizaje Basado en Proyectos el cual motiva al estudiante a la apropiación delconocimiento y despierta un espíritu científico. Para esto se implementó el diseño y elaboración de prototipos físicos soportados en dispositivos mecánicos y electrónicos, para facilitar la conceptualización de las variables que determinan el movimiento ondulatorio, heredadas del movimiento circular y M.A.S y la comprensión de sus respectivas modelaciones matemáticas. De esta manera, se describe una experiencia educativa realizada con un grupo de estudiantes de ingeniería de sistemas de la Universidad Cooperativa de Colombia, sede Ibagué, con quienes se lleva a cabo una investigación-acción, en la que se hace un análisis profundo de su desempeño en el proceso de diseño, elaboración e implementación del prototipo.Se evidencio en el 77% de los estudiantes participantes en esta acción de formación, el desarrollo de ciertas actitudes que identificaron un espíritu científico, como son: habilidades para la comunicación, el trabajo en equipo, la evaluación crítica y la adquisición de nuevos conocimientoscientíficos que les indujo a un constante cuestionamiento

Resistance to autosomal dominant Alzheimer's disease in an APOE3 Christchurch homozygote: a case report.

We identified a PSEN1 (presenilin 1) mutation carrier from the world's largest autosomal dominant Alzheimer's disease kindred, who did not develop mild cognitive impairment until her seventies, three decades after the expected age of clinical onset. The individual had two copies of the APOE3 Christchurch (R136S) mutation, unusually high brain amyloid levels and limited tau and neurodegenerative measurements. Our findings have implications for the role of APOE in the pathogenesis, treatment and prevention of Alzheimer's disease

Science opportunities enabled by the era of Visible Band Stellar Imaging with sub-100 μarc-sec angular resolution

This white paper briefly summarizes stellar science opportunities enabled by ultra-high resolution (sub-100 μarc-sec) astronomical imaging in the visible (U/V) wavebands. We describe the science impact of imaging of several thousand bright (m < 6), hot (O/B/A) stars using a modern implementation of Stellar Intensity Interferometry (SII)

LSST: from Science Drivers to Reference Design and Anticipated Data Products

(Abridged) We describe here the most ambitious survey currently planned in the optical, the Large Synoptic Survey Telescope (LSST). A vast array of science will be enabled by a single wide-deep-fast sky survey, and LSST will have unique survey capability in the faint time domain. The LSST design is driven by four main science themes: probing dark energy and dark matter, taking an inventory of the Solar System, exploring the transient optical sky, and mapping the Milky Way. LSST will be a wide-field ground-based system sited at Cerro Pach\'{o}n in northern Chile. The telescope will have an 8.4 m (6.5 m effective) primary mirror, a 9.6 deg$^2$ field of view, and a 3.2 Gigapixel camera. The standard observing sequence will consist of pairs of 15-second exposures in a given field, with two such visits in each pointing in a given night. With these repeats, the LSST system is capable of imaging about 10,000 square degrees of sky in a single filter in three nights. The typical 5$\sigma$ point-source depth in a single visit in $r$ will be $\sim 24.5$ (AB). The project is in the construction phase and will begin regular survey operations by 2022. The survey area will be contained within 30,000 deg$^2$ with $\delta<+34.5^\circ$, and will be imaged multiple times in six bands, $ugrizy$, covering the wavelength range 320--1050 nm. About 90\% of the observing time will be devoted to a deep-wide-fast survey mode which will uniformly observe a 18,000 deg$^2$ region about 800 times (summed over all six bands) during the anticipated 10 years of operations, and yield a coadded map to $r\sim27.5$. The remaining 10\% of the observing time will be allocated to projects such as a Very Deep and Fast time domain survey. The goal is to make LSST data products, including a relational database of about 32 trillion observations of 40 billion objects, available to the public and scientists around the world.Comment: 57 pages, 32 color figures, version with high-resolution figures available from https://www.lsst.org/overvie