2,400 research outputs found
An atlas of emission line fluxes of planetary nebulae in the 1150-3200 A region
Emission line fluxes for 28 planetary nebulae are presented. The nebulae were chosen to cover a wide range of excitation classes, apparent diameters, location in the sky, and types of central stars. All objects were observed in the low dispersion mode of the IUE spectrographs, using the large entrance aperture
The spectrum of HM Sagittae: A planetary nebula excited by a Wolf-Rayet star
A total of image tube spectrograms of HM Sagittae were obtained. More than 70 emission lines, including several broad emission features, were identified. An analysis of the spectra indicates that HM Sagittae is a planetary nebula excited by a Wolf-Rayet star. The most conspicuous Wolf-Rayet feature is that attributed to a blend of C III at 4650 A and He II at 4686 A
Direct Measurements of Interplanetary Dust Particles in the Vicinity of Earth
The direct measurements made by the Explorer VIII satellite provide the first sound basis for analyzing all available direct measurements of the distribution of interplanetary dust particles. The model average distribution curve established by such an analysis departs significantly from that predicted by the (uncertain) extrapolation of results from meteor observations. A consequence of this difference is that the daily accretion of interplanetary particulate matter by the earth is now considered to be mainly dust particles of the direct measurements range of particle size. Almost all the available direct measurements obtained with microphone systems on rockets, satellites, and spacecraft fit directly on the distribution curve defined by Explorer VIII data. The lack of reliable datum points departing significantly from the model average distribution curve means that available direct measurements show no discernible evidence of an appreciable geocentric concentration of interplanetary dust particles
MAPIR: An Airborne Polarmetric Imaging Radiometer in Support of Hydrologic Satellite Observations
In this age of dwindling water resources and increasing demands, accurate estimation of water balance components at every scale is more critical to end users than ever before. Several near-term Earth science satellite missions are aimed at global hydrologic observations. The Marshall Airborne Polarimetric Imaging Radiometer (MAPIR) is a dual beam, dual angle polarimetric, scanning L band passive microwave radiometer system developed by the Observing Microwave Emissions for Geophysical Applications (OMEGA) team at MSFC to support algorithm development and validation efforts in support of these missions. MAPIR observes naturally-emitted radiation from the ground primarily for remote sensing of land surface brightness temperature from which we can retrieve soil moisture and possibly surface or water temperature and ocean salinity. MAPIR has achieved Technical Readiness Level 6 with flight heritage on two very different aircraft, the NASA P-3B, and a Piper Navajo
Nurses\u27 Alumnae Association Bulletin, June 1970
Alumnae President\u27s Message
Congratulations Alumni Association
Portrait of Samuel D. Gross
Officers and Chairmen of Committees
Financial Report
Progress of Jefferson 1969-1970
School of Nursing Annual Report
School of Practical Nursing Report
Emergency Department
Patient Services Department
Annual Luncheon Pictures
Committee Reports
Progress of the Alumnae Association
Crossword Puzzle
Missing Graduates
Resume of Alumnae Meetings Minutes
Class News
Student Nurses Section
Crossword Puzzle Answers
Notice
Nurses\u27 Alumnae Association Bulletin, June 1969
Alumnae President\u27s Message
Officers and Chairmen
Financial Report
Progressive Changes at Jefferson
School of Nursing Report
Student Activities
School of Practical Nursing Report
Jefferson Expansion Report
Clerk-Typist Report
Committee Reports
Resume of Alumnae Meetings
Class News
1969 CLINIC Correspondence
Notice
Are School Absences Correlated with Influenza Surveillance Data in England? Results from Decipher My Data-A Research Project Conducted through Scientific Engagement with Schools.
BACKGROUND: School aged children are a key link in the transmission of influenza. Most cases have little or no interaction with health services and are therefore missed by the majority of existing surveillance systems. As part of a public engagement with science project, this study aimed to establish a web-based system for the collection of routine school absence data and determine if school absence prevalence was correlated with established surveillance measures for circulating influenza. METHODS: We collected data for two influenza seasons (2011/12 and 2012/13). The primary outcome was daily school absence prevalence (weighted to make it nationally representative) for children aged 11 to 16. School absence prevalence was triangulated graphically and through univariable linear regression to Royal College of General Practitioners (RCGP) influenza like illness (ILI) episode incidence rate, national microbiological surveillance data on the proportion of samples positive for influenza (A+B) and with Rhinovirus, RSV and laboratory confirmed cases of Norovirus. RESULTS: 27 schools submitted data over two respiratory seasons. During the first season, levels of influenza measured by school absence prevalence and established surveillance were low. In the 2012/13 season, a peak of school absence prevalence occurred in week 51, and week 1 in RCGP ILI surveillance data. Linear regression showed a strong association between the school absence prevalence and RCGP ILI (All ages, and 5-14 year olds), laboratory confirmed cases of influenza A & B, and weak evidence for a linear association with Rhinovirus and Norovirus. INTERPRETATION: This study provides initial evidence for using routine school illness absence prevalence as a novel tool for influenza surveillance. The network of web-based data collection platforms we established through active engagement provides an innovative model of conducting scientific research and could be used for a wide range of infectious disease studies in the future
The First Release COSMOS Optical and Near-IR Data and Catalog
We present imaging data and photometry for the COSMOS survey in 15
photometric bands between 0.3um and 2.4um. These include data taken on the
Subaru 8.3m telescope, the KPNO and CTIO 4m telescopes, and the CFHT 3.6m
telescope. Special techniques are used to ensure that the relative photometric
calibration is better than 1% across the field of view. The absolute
photometric accuracy from standard star measurements is found to be 6%. The
absolute calibration is corrected using galaxy spectra, providing colors
accurate to 2% or better. Stellar and galaxy colors and counts agree well with
the expected values. Finally, as the first step in the scientific analysis of
these data we construct panchromatic number counts which confirm that both the
geometry of the universe and the galaxy population are evolving.Comment: 19 pages, 13 figures, 14 tables, Accepted to ApJS for COSMOS speciall
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The Calar Alto Deep Imaging Survey: K-band Galaxy Number Counts
We present K-band number counts for the faint galaxies in the Calar Alto Deep
Imaging Survey (CADIS). We covered 4 CADIS fields, a total area of 0.2deg^2, in
the broad band filters B, R and K. We detect about 4000 galaxies in the K-band
images, with a completeness limit of K=19.75mag, and derive the K-band galaxy
number counts in the range of 14.25 < K < 19.75mag. This is the largest medium
deep K-band survey to date in this magnitude range. The B- and R-band number
counts are also derived, down to completeness limits of B=24.75mag and
R=23.25mag. The K-selected galaxies in this magnitude range are of particular
interest, since some medium deep near-infrared surveys have identified breaks
of both the slope of the K-band number counts and the mean B-K color at
K=17\sim18mag. There is, however, a significant disagreement in the K-band
number counts among the existing surveys. Our large near-infrared selected
galaxy sample allows us to establish the presence of a clear break in the slope
at K=17.0mag from dlogN/dm = 0.64 at brighter magnitudes to dlogN/dm = 0.36 at
the fainter end. We construct no-evolution and passive evolution models, and
find that the passive evolution model can simultaneously fit the B-, R- and
K-band number counts well. The B-K colors show a clear trend to bluer colors
for K > 18mag. We also find that most of the K=18-20mag galaxies have a B-K
color bluer than the prediction of a no-evolution model for an L_* Sbc galaxy,
implying either significant evolution, even for massive galaxies, or the
existence of an extra population of small galaxies.Comment: Accepted for A&A, 10 pages, 7 figure
Estimating the frequency of extremely energetic solar events, based on solar, stellar, lunar, and terrestrial records
The most powerful explosions on the Sun [...] drive the most severe
space-weather storms. Proxy records of flare energies based on SEPs in
principle may offer the longest time base to study infrequent large events. We
conclude that one suggested proxy, nitrate concentrations in polar ice cores,
does not map reliably to SEP events. Concentrations of select radionuclides
measured in natural archives may prove useful in extending the time interval of
direct observations up to ten millennia, but as their calibration to solar
flare fluences depends on multiple poorly known properties and processes, these
proxies cannot presently be used to help determine the flare energy frequency
distribution. Being thus limited to the use of direct flare observations, we
evaluate the probabilities of large-energy solar explosions by combining solar
flare observations with an ensemble of stellar flare observations. We conclude
that solar flare energies form a relatively smooth distribution from small
events to large flares, while flares on magnetically-active, young Sun-like
stars have energies and frequencies markedly in excess of strong solar flares,
even after an empirical scaling with the mean activity level of these stars. In
order to empirically quantify the frequency of uncommonly large solar flares
extensive surveys of stars of near-solar age need to be obtained, such as is
feasible with the Kepler satellite. Because the likelihood of flares larger
than approximately X30 remains empirically unconstrained, we present indirect
arguments, based on records of sunspots and on statistical arguments, that
solar flares in the past four centuries have likely not substantially exceeded
the level of the largest flares observed in the space era, and that there is at
most about a 10% chance of a flare larger than about X30 in the next 30 years.Comment: 14 pages, 3 figures (in press as of 2012/06/18); Journal of
Geophysical Research (Space Physics), 201
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