We present the early UV and optical light curve of Type IIP supernova (SN) 2010aq at z = 0.0862, and compare it to analytical models for thermal emission following SN shock breakout in a red ...supergiant star. SN 2010aq was discovered in joint monitoring between the Galaxy Evolution Explorer (GALEX) Time Domain Survey (TDS) in the NUV and the Pan-STARRS1 Medium Deep Survey (PS1 MDS) in the g, r, i, and z bands. The GALEX and Pan-STARRS1 observations detect the SN less than 1 day after the shock breakout, measure a diluted blackbody temperature of 31, 000 {+-} 6000 K 1 day later, and follow the rise in the UV/optical light curve over the next 2 days caused by the expansion and cooling of the SN ejecta. The high signal-to-noise ratio of the simultaneous UV and optical photometry allows us to fit for a progenitor star radius of 700 {+-} 200R {sub sun}, the size of a red supergiant star. An excess in UV emission two weeks after shock breakout compared with SNe well fitted by model atmosphere-code synthetic spectra with solar metallicity is best explained by suppressed line blanketing due to a lower metallicity progenitor star in SN 2010aq. Continued monitoring of PS1 MDS fields by the GALEX TDS will increase the sample of early UV detections of Type II SNe by an order of magnitude and probe the diversity of SN progenitor star properties.
Obesity is highly prevalent and adds greatly to the risk of cardiovascular and metabolic diseases. However, a subset of the obese has been identified who do not appear to carry this risk. Some ...studies suggest that anthropomorphic correlates of risk, such as waist circumference, differ between African Americans and Whites and features of uncomplicated obesity have not been well characterized in this population. The goal of our study was to determine the prevalence and associated features of uncomplicated obesity, including relationships to waist circumference and the achievement of weight loss in primarily African American patients.
A retrospective chart review.
Outpatient medically supervised weight loss program located at a teaching hospital in Washington, DC.
Predominately adult African American females.
Thirty-one percent of our population had no documented metabolic or cardiovascular disease. This group was on average younger, but had similar waist circumference (44 +/- 13.8 vs 44 +/- 6.6 inches) and achieved similar mean weight loss at 3 months (9.9 +/- 10.4 vs 10.3 +/- 12.4 lbs.) as the group with comorbid conditions.
Waist circumference was not an indicator of risk among African American women and achieved weight loss did not depend on pre-existing comorbidities.
L Dwarfs and the Substellar Mass Function Reid, I. Neill; Kirkpatrick, J. Davy; Liebert, J ...
The Astrophysical journal,
08/1999, Letnik:
521, Številka:
2
Journal Article
We report the discovery of two binary M dwarf systems in the immediate solar neighbourhood using the Two Micron All Sky Survey (2MASS). The first is an M6.5 companion to the nearby G star HD 86728 ...(Gl 376). The known properties of HD 86728 indicate that the M dwarf (Gl 376B) is old, metal-rich and only 14.9 parsec away. The M dwarf is highly active, with both Hα and X-ray emission. Thus, Gl 376B offers the opportunity to study an old, bright, active M dwarf with known metallicity, age and luminosity. We show that it is probable that Gl 376B is itself an unresolved pair. The other system consists of an M6.5 and an M8 dwarf with 14.5 arcsec separation. We estimate a distance of ∼16 parsec for this very low-mass pair. Stronger activity is observed in the M6.5 dwarf, supporting evidence that chromospheric activity is weakening near the hydrogen-burning limit.
Results will be presented from a new NASA optical survey of objects at geosynchronous orbit (GEO). The goal is to determine the total population of debris objects at GEO to as small a limiting size ...as possible. This survey uses the University of Michigan's 0.6/0.9 m Schmidt telescope Michigan Orbital Debris Survey Telescope (MODEST). Located at Cerro Tololo Inter-American Observatory in Chile, the system is equipped with a scanning CCD with a field of view of 1.3°
×
1.3°, and can detect objects smaller than 20 cm diameter at GEO. Each night the telescope scans a strip of sky 100° long
×
1.3° high. Up to eight independent detections are made of each candidate GEO object in a 5 min time span, yielding measurements of brightness, position, and angular motion. Since February 2001, an extensive series of observations of the GEO regime has been carried out with this system, revealing a considerable population of objects smaller than 1 m in diameter.
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