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Sample records for glare survey ii

  1. Survey of discomfort glare from the headlamps of cars widely used in Iran.

    PubMed

    Mehri, Ahmad; Farhang Dehghan, Somayeh; Hajizadeh, Roohalah; Zakerian, Seyed Abolfazl; Mohammadi, Hamzeh; Abbasi, Milad

    2017-10-03

    On 2-lane roads, discomfort glare can cause annoyance, discomfort, inconvenience, stress, and fatigue to drivers, posing a risk of accidents. The aim of this study is to evaluate discomfort glare from the headlamps of cars widely used in Iran. The discomfort glare of new vehicles including Pride Saba model GTX, Pride Model 131SL, Samand Soren, Peugeot 405, Megane, and Peugeot Pars was examined at distances of 5 to 100 m at a background luminance of 50 cd/m(2) (late twilight/early dawn lighting) and 1 cd/m(2) (nighttime) using Schmidt-Clausen and Bindels model and de Boer's subjective scale. According to the de Boer scale, at a background luminance of 50 cd/m(2), the discomfort glare for all studied vehicles was between 1.98 and 4.05 in high-beam mode and between 3.5 and 5.4 in low-beam mode. At a background luminance of 1 cd/m(2), discomfort glare was between 0.41 and 2.48 in high-beam mode and between 1.93 and 3.84 in low-beam mode. In high-beam mode, the average levels of discomfort glare of these vehicles gradually increased when the distance between cars was reduced by up to about 20 m. In low-beam mode, there was no discomfort glare up to a vehicle distance of 40 m. In addition, at an angle of 1.15°-5.73° between the line of sight and light of vehicles in high-beam mode, the level of discomfort glare was increased, but at an angle of 5.73°-22.9° the level of discomfort glare was reduced. In low-beam mode at an angle of 2.86°-22.9°, the level of discomfort glare was almost identical. The results show that in high-beam mode and with a 100-m distance between vehicles as well as in low-beam mode at intervals of less than 40 m between cars, discomfort glare is created. It can be concluded that by providing solutions such as installing road lighting system, an increase in luminance of roads, separating or widening road lanes, increasing the lateral distance between vehicles, and increasing the angle between lighted vehicles and drivers can noticeably

  2. Anti-Glare Filters

    NASA Technical Reports Server (NTRS)

    1989-01-01

    Glare from CRT screens has been blamed for blurred vision, eyestrain, headaches, etc. Optical Coating Laboratory, Inc. (OCLI) manufactures a coating to reduce glare which was used to coat the windows on the Gemini and Apollo spacecraft. In addition, OCLI offers anti-glare filters (Glare Guard) utilizing the same thin film coating technology. The coating minimizes brightness, provides enhanced contrast and improves readability. The filters are OCLI's first consumer product.

  3. Glare in aviation.

    PubMed

    Brennan, D H

    1989-05-01

    The control of high-speed aircraft is a demanding task in which rapid decisions, based on visually acquired information, must frequently be made. Glare, both direct and veiling, is a prime cause of visual degradation in flight. The visual effects of glare are discussed together with means of reducing its consequences. In addition, the visual sequelae of looking at a nuclear fireball are discussed together with means of providing protection.

  4. How to Avoid Headlight Glare

    MedlinePlus

    ... how to handle nighttime glare with confidence. New Lights, Old Problems Drivers have been complaining about glare ... answer involves technology, automotive design, and demographics. Extra Lights Many vehicles now sport fog lamps or other ...

  5. Evaluation of glare at the Ivanpah Solar Electric Generating System

    DOE PAGES

    Ho, C. K.; Sims, C. A.; Christian, J. M.

    2015-06-05

    The Ivanpah Solar Electric Generating System (ISEGS), located on I-15 about 40 miles (60 km) south of Las Vegas, NV, consists of three power towers 459 ft (140 m) tall and over 170,000 reflective heliostats with a rated capacity of 390 MW. In addition, reports of glare from the plant have been submitted by pilots and air traffic controllers and recorded by the Aviation Safety Reporting System and the California Energy Commission since 2013. Aerial and ground-based surveys of the glare were conducted in April, 2014, to identify the cause and to quantify the irradiance and potential ocular impacts ofmore » the glare. Results showed that the intense glare viewed from the airspace above ISEGS was caused by heliostats in standby mode that were aimed to the side of the receiver. Evaluation of the glare showed that the retinal irradiance and subtended source angle of the glare from the heliostats in standby were sufficient to cause significant ocular impact (potential for after-image) up to a distance of ~6 miles (10 km), but the values were below the threshold for permanent eye damage. Glare from the receivers had a low potential for after-image at all ground-based monitoring locations outside of the site boundaries. A Letter to Airmen has been issued by the Federal Aviation Administration to notify pilots of the potential glare hazards. Additional measures to mitigate the potential impacts of glare from ISGES are also presented and discussed.« less

  6. Evaluation of glare at the Ivanpah Solar Electric Generating System

    SciTech Connect

    Ho, C. K.; Sims, C. A.; Christian, J. M.

    2015-06-05

    The Ivanpah Solar Electric Generating System (ISEGS), located on I-15 about 40 miles (60 km) south of Las Vegas, NV, consists of three power towers 459 ft (140 m) tall and over 170,000 reflective heliostats with a rated capacity of 390 MW. In addition, reports of glare from the plant have been submitted by pilots and air traffic controllers and recorded by the Aviation Safety Reporting System and the California Energy Commission since 2013. Aerial and ground-based surveys of the glare were conducted in April, 2014, to identify the cause and to quantify the irradiance and potential ocular impacts of the glare. Results showed that the intense glare viewed from the airspace above ISEGS was caused by heliostats in standby mode that were aimed to the side of the receiver. Evaluation of the glare showed that the retinal irradiance and subtended source angle of the glare from the heliostats in standby were sufficient to cause significant ocular impact (potential for after-image) up to a distance of ~6 miles (10 km), but the values were below the threshold for permanent eye damage. Glare from the receivers had a low potential for after-image at all ground-based monitoring locations outside of the site boundaries. A Letter to Airmen has been issued by the Federal Aviation Administration to notify pilots of the potential glare hazards. Additional measures to mitigate the potential impacts of glare from ISGES are also presented and discussed.

  7. Evaluation of Glare at the Ivanpah Solar Electric Generating System

    SciTech Connect

    Ho, Clifford K.; Sims, Cianan; Christian, Joshua Mark

    2014-07-01

    The Ivanpah Solar Electric Generating System (ISEGS), located on I - 15 about 40 miles (60 km) south of Las Vegas, NV, consists of three power towers 459 ft (140 m) tall and over 170,000 reflective heliostats with a rated capacity of 390 MW. Reports of glare from the plant have been submitted by pilots and air traffic controllers and recorded by the Aviation Safety Reporting System and the California Energy Commission since 2013. Aerial and ground - based surveys of the glare were conducted in April, 2014, to identify the cause and to quantify the irradiance and potential ocular impact s of the glare . Results showed that the intense glare viewed from the airspace above ISEGS was caused by he liostats in standby mode that were aimed to the side of the receiver. Evaluation of the glare showed that the retinal irradiance and subtended source angle of the glare from the heliostats in standby were sufficient to cause significant ocular impact (pot ential for after - image) up to a distance of %7E6 miles (10 km), but the values were below the threshold for permanent eye damage . Glare from the receivers had a low potential for after - image at all ground - based monitoring locations outside of the site bound aries. A Letter to Airmen has been issued by the Federal Aviation Administration to notify pilots of the potential glare hazards. Additional measures to mitigate the potential impacts of glare from ISGES are also presented and discussed. This page intentionally left blank

  8. Glare Design Aspects and Philosophies

    NASA Astrophysics Data System (ADS)

    Vermeeren, C. A. J. R.; Beumler, Th.; de Kanter, J. L. C. G.; van der Jagt, O. C.; Out, B. C. L.

    2003-07-01

    The very nature of Glare is its crack bridging mechanism, which provides superior damage tolerance properties. Depending on the property, Glare shows either monolithic metal or composite behaviour, which challenges the definition of strength justification and certification procedures. Airworthiness regulations have to be interpreted for Glare in order to guarantee the same level of safety as obtained for aircraft structures made of other materials and to take at the same time benefit of its particular properties. Cut-outs are highly fatigue sensitive due to the stress concentrations they cause. In aircraft fuselages these cut-outs are quite large in the case of the windows and doors. The stress level may be increased through the application of Glare in the doubler packages, due to the improved fatigue behaviour compared to conventional aluminium. Glare also presents the possibility of tailoring the material to the load, i.e. fibres aligned with the load, e.g., a 45 degree orientation. FE analysis defined the total doubler package and a test programme was run to confirm the behaviour of the material and to predict the crack behaviour of the Glare door corner. Some aspects of the detailed design of aircraft structures in Glare, the design of splices and riveted joints are discussed. In order to apply Glare in very large fuselage panels, a splice concept was developed, which allows a number of longitudinal splices to be cured in the same curing cycle as the basic material. Through the introduction of this splicing concept, the width of a panel is no longer limited to the maximum width of the aluminium sheet. Internal local reinforcements (doublers) can be integrated into the panel during lay-up. A discussion on the design of riveted joints in Glare is held.

  9. Rainbow glare by retinal imaging

    NASA Astrophysics Data System (ADS)

    Sun, Han-Ying; Chiang, Yao-Ting; Yeh, Shang-Min; Huang, Shuan-Yu; Horng, Chi-Ting; Wang, Hsiang-Chen

    2016-07-01

    This study aims to determine whether IntraLase surgery can cause rainbow glare. Monte-Carlo ray tracing method is used to study visual conditions of an ordered microstructure array on the cornea. A corneal flap in the simulated eye model can generate numerous microbubbles caused by IntraLase surgery. Moreover, this study evaluates the visual performance under different conditions such as the size and interval of the microbubble structure on the cornea with vary incident angles and diameters of light. The results of this study can help elucidate the real cause of rainbow glare as a side effect of IntraLase.

  10. Discomfort Glare: What Do We Actually Know?

    SciTech Connect

    Clear, Robert D.

    2012-04-19

    We reviewed glare models with an eye for missing conditions or inconsistencies. We found ambiguities as to when to use small source versus large source models, and as to what constitutes a glare source in a complex scene. We also found surprisingly little information validating the assumed independence of the factors driving glare. A barrier to progress in glare research is the lack of a standardized dependent measure of glare. We inverted the glare models to predict luminance, and compared model predictions against the 1949 Luckiesh and Guth data that form the basis of many of them. The models perform surprisingly poorly, particularly with regards to the luminance-size relationship and additivity. Evaluating glare in complex scenes may require fundamental changes to form of the glare models.

  11. Disability glare in soft multifocal contact lenses.

    PubMed

    Wahl, Siegfried; Fornoff, Luise; Ochakovski, G Alex; Ohlendorf, Arne

    2017-10-07

    The study investigated the effect of the design of multifocal contact lenses on the sensitivity to contrast and disability glare. Contrast sensitivity was measured in 16 young adults (mean age: 25.5±2.5years) at a distance of 2m under two conditions: no-glare and glare. Two designs (Center Near and Center Distance) of the Biofinity soft contact lens were used to simulate correction for presbyopes, while a correction with single vision trial lenses and contact lenses acted as controls. The design of the used multifocal contact lenses had a significant influence on the log area under the curve of the contrast sensitivity function (AUC-CSF). Compared to the spectacle lens correction, the AUC-CSF was significantly reduced, in case CS was measured with the Center Near design lens, under the no-glare (p<0.001) and the glare condition (p: p<0.001). In case of the Center Distance design contact lens, the AUC-CSF was significantly smaller in case CS was tested under glare (p=0.001). Disability glare (DG) was depending on the spatial frequency and the design of the multifocal lens, while the Center Distance design produced higher amounts of DG (p<0.001), compared to the other used corrections. The optical design of a multifocal contact lenses has a significant impact on the contrast sensitivity as well as the disability glare. In order to dispense the best correction in terms of contact lenses, the sensitivity to contrast under no-glare and glare conditions should be tested a medium spatial frequencies. Copyright © 2017. Published by Elsevier Ltd.

  12. The immediate effects of glare and electrochromic glare-reducing mirrors in simulated truck driving.

    PubMed

    Ranney, T A; Simmons, L A; Masalonis, A J

    2000-01-01

    In this experiment 12 experienced truck drivers drove a fixed-base driving simulator for three 8-h sessions under simulated nighttime driving conditions. Sessions included (a) no glare, (b) intermittent glare presented in the exterior rearview mirrors to simulate following vehicles, and (c) intermittent glare with electrochromic glare reduction. The driving task combined vehicle control on straight and curved road segments with detection of pedestrians appearing alongside the road and targets appearing in the rearview mirrors. The presence of glare slowed detection of pedestrians and, to a lesser extent, slowed the detection of targets appearing in mirrors. Glare was also associated with increased lane position variability, reduced speed on curves, and, most consistently, increased steering variability. We found only meager evidence that electrochromic glare reduction improved target detection performance and no evidence that glare reduction improved vehicle control, despite the fact that participants consistently voiced positive preferences for glare reduction. The results will aid decision making that requires incorporation of the benefits of electrochromic glare-reducing mirrors.

  13. Mitigating the Impacts of Glint and Glare

    SciTech Connect

    Hillesheim, Michael; Kandt, Alicen; Phillips, Steven

    2015-09-01

    The National Renewable Energy Laboratory, supporting the Department of the Navy Renewable Energy Program Office, has developed an innovative glint/glare analysis and visualization methodology to understand and mitigate the possible impacts of light reflecting off solar photovoltaic arrays.

  14. Glare suppression by coherence gated negation

    PubMed Central

    Zhou, Edward Haojiang; Shibukawa, Atsushi; Brake, Joshua; Ruan, Haowen; Yang, Changhuei

    2016-01-01

    Imaging of a weak target hidden behind a scattering medium can be significantly confounded by glare. We report a method, termed coherence gated negation (CGN), that uses destructive optical interference to suppress glare and allow improved imaging of a weak target. As a demonstration, we show that by permuting through a set range of amplitude and phase values for a reference beam interfering with the optical field from the glare and target reflection, we can suppress glare by an order of magnitude, even when the optical wavefront is highly disordered. This strategy significantly departs from conventional coherence gating methods in that CGN actively “gates out” the unwanted optical contributions while conventional methods “gate in” the target optical signal. We further show that the CGN method can outperform conventional coherence gating image quality in certain scenarios by more effectively rejecting unwanted optical contributions. PMID:28713849

  15. The Southern H ii Region Discovery Survey (SHRDS): Pilot Survey

    NASA Astrophysics Data System (ADS)

    Brown, C.; Jordan, C.; Dickey, John M.; Anderson, L. D.; Armentrout, W. P.; Balser, Dana S.; Bania, T. M.; Dawson, J. R.; McClure-Griffiths, N. M.; Wenger, Trey V.

    2017-07-01

    The Southern H ii Region Discovery Survey is a survey of the third and fourth quadrants of the Galactic plane that will detect radio recombination line (RRL) and continuum emission at cm-wavelengths from several hundred H ii region candidates using the Australia Telescope Compact Array. The targets for this survey come from the WISE Catalog of Galactic H ii Regions and were identified based on mid-infrared and radio continuum emission. In this pilot project, two different configurations of the Compact Array Broad Band receiver and spectrometer system were used for short test observations. The pilot surveys detected RRL emission from 36 of 53 H ii region candidates, as well as seven known H ii regions that were included for calibration. These 36 recombination line detections confirm that the candidates are true H ii regions and allow us to estimate their distances.

  16. Manufacturing of GLARE Parts and Structures

    NASA Astrophysics Data System (ADS)

    Sinke, J.

    2003-07-01

    GLARE is a hybrid material consisting of alternating layers of metal sheets and composite layers, requiring special attention when manufacturing of parts and structures is concerned. On one hand the applicable manufacturing processes for GLARE are limited, on the other hand, due to the constituents and composition of the laminate, it offers new opportunities for production. One of the opportunities is the manufacture of very large skin panels by lay-up techniques. Lay-up techniques are common for full composites, but uncommon for metallic structures. Nevertheless, large GLARE skin panels are made by lay-up processes. In addition, the sequences of forming and laminating processes, that can be selected, offer manufacturing options that are not applicable to metals or full composites. With respect to conventional manufacturing processes, the possibilities for Fibre Metal Laminates in general, are limited. The limits are partly due to the different failure modes, partly due to the properties of the constituents in the laminate. For machining processes: the wear of the cutting tools during machining operations of GLARE stems from the abrasive nature of the glass fibres. For the forming processes: the limited formability, expressed by a small failure strain, is related to the glass fibres. However, although these manufacturing issues may restrict the use of manufacturing processes for FMLs, application of these laminates in aircraft is not hindered.

  17. Controlling Glare Problems in the VDT Work Environment.

    ERIC Educational Resources Information Center

    Schleifer, Lawrence M.; Sauter, Steven L.

    1985-01-01

    The sources and characteristics (light measurement, direct and indirect or reflected glare) of glare problems in the video display terminal work environment are described. Glare control measures, including the location and design of lighting systems, managing outdoor light and using screen filters and hoods, are reviewed. Five sources are given.…

  18. The effect of glare on eye movements when reading.

    PubMed

    Glimne, S; Brautaset, R L; Seimyr, G Öqvist

    2015-01-01

    Glare is a very common source of image degradation when performing computer work. Since reading is a task that is very sensitive to image degradation induced disability glare affects reading performance. To assess the effect of different glare conditions on eye movements when reading on a computer screen. Glare conditions have an impact on reading. This observation is based on the results from a study where we investigated how reading eye movements were affected by glare. Sixteen subjects with normal vision participated in this study. In a balanced repeated-measurement study, all subjects performed equal near-vision reading tasks. In addition to the condition of no glare three controlled conditions of glare were used: direct light, indirect light, and desk luminary. The subjects read three texts under each condition: First a short standardized text (IReST), secondly a longer newspaper text, and finally an additional IReST text. The texts were read on a Tobii T120 eye tracker. The results show that glare does have a negative effect on reading performance. The more adverse the lighting condition was, the slower the reading speed became. The decrease was primarily a result of increased fixation durations. Both glare conditions of direct and indirect glare increased the fixation durations significantly (p < 0.05). This study shows that even moderate glare conditions can have an impact on reading. The results show that it is important to follow recommendations of lighting design in computer work environment in order to avoid disability glare.

  19. KENNEDY SPACE CENTER, FLA. - NASA launches its second Mars Exploration Rover, Opportunity, aboard a Delta II launch vehicle. The bright glare briefly illuminated Florida Space Coast beaches. Opportunity’s dash to Mars began with liftoff at 11:18:15 p.m. Eastern Daylight Time from Cape Canaveral Air Force Station, Fla. The spacecraft separated successfully from the Delta's third stage 83 minutes later, after it had been boosted out of Earth orbit and onto a course toward Mars.

    NASA Image and Video Library

    2003-07-07

    KENNEDY SPACE CENTER, FLA. - NASA launches its second Mars Exploration Rover, Opportunity, aboard a Delta II launch vehicle. The bright glare briefly illuminated Florida Space Coast beaches. Opportunity’s dash to Mars began with liftoff at 11:18:15 p.m. Eastern Daylight Time from Cape Canaveral Air Force Station, Fla. The spacecraft separated successfully from the Delta's third stage 83 minutes later, after it had been boosted out of Earth orbit and onto a course toward Mars.

  20. Full scale GLARE fuselage panel tests

    NASA Technical Reports Server (NTRS)

    Vercammen, Roland W. A.; Ottens, Harold H.

    1996-01-01

    A GLARE fuselage panel, representative of the crown section of the Fokker 100 fuselage in front of the wing, was tested. The panels were loaded by air pressure resulting in tangential stress in the panel by axial loading, representative of both the cabin pressure and the fuselage bending due to taxiing and gust loading. A fatigue test, simulating 180000 flights, followed by static tests were performed. The panel was loaded to failure at 1.32 ultimate load. The test set-up, the uniform strain distribution of the panel, and the fatigue loads applied at high test frequency are described. The use of GLARE leads to a substantial weight reduction without affecting the fatigue static strength.

  1. Measurement Of Transmittance And Veiling Glare Index

    NASA Astrophysics Data System (ADS)

    Barton, Norman P.

    1981-10-01

    Transmittance and Veiling Glare Index measurements in conjunction with the Optical Transfer Function can give a set of objective measurements for specifying and providing quantitative data on the performance of components and complete optical systems. The main application of the work described, is to directly viewed telescopic systems. Transmittance, the ratio of transmitted radiance to incident irradiance, of telescopic instruments is usually measured with a small diameter collimated beam, integrating sphere and photo multiplier detector. An alternative method in which the full aperture of the objective is filled by the incident beam will reveal any adverse effects of vignetting or variability of anti reflection coatings and is of importance in subjective/objective comparisons when the eye pupil is greater than the exit pupil of the telescopic system. The MVEE 'audit' and Standard telescopes which were developed for investigation of the application of OTF measurement to visual instruments were found to have markedly different Veiling Glare Index values when measured on a wide glare field apparatus. Subsequently a series of measurements of these telescopes, using several current techniques for the measurement of stray light, indicated the importance of unwanted radiation which came from outside the field of view and the inadequacy of routine VGI measurements with a glare field equal to the field of view of the specimen being tested. For a single measurement test it was concluded that a black spot on a wide field (>±45 degrees) was desirable; this is substantially test condition C2 of British Standard 4995. The Standard telescope, as tested above, had the lowest VGI and the Audit telescope the highest VGI of all systems tested, with a modern 10 x 60 sight having a VGI value close to the former. The final section of the paper discusses possible combined instruments for measuring all three parameters, to give the most effective utilization of apparatus.

  2. Evaluation of a New Controlled Point Source LED Glare Tester for Disability Glare Detection in Participants With and Without Cataracts.

    PubMed

    Epitropoulos, Alice T; Fram, Nicole R; Masket, Samuel; Price, Francis W; Snyder, Michael E; Stulting, R Doyle

    2015-03-01

    To determine glare-induced change during visual acuity testing in patients with and without cataract using the controlled point source light-emitting diode (LED) glare tester (EpiGlare Tester; Epico, LLC, Columbus, OH), a new medical device for identification of glare disability. This prospective, multicenter study enrolled 40 patients (80 eyes with cataracts) and 49 control subjects (98 eyes without cataracts). Corrected distance visual acuity (CDVA) was measured with and without glare using the EpiGlare Tester as a glare source. Functional visual ability was evaluated using driving and glare subscales from the Refractive Status Vision Profile questionnaire. The primary efficacy measure was change in CDVA measurement with and without glare in patients with senile cataract compared to participants without cataract. Secondary efficacy measures included correlation of the CDVA change caused by functional glare disability and subjective patient and investigator assessments. CDVA reduction was greater for patients with cataract, with a mean reduction of -0.49 ± 0.3 logMAR, than for participants without cataracts at -0.13 ± 0.2 logMAR (P < .001). This equates to a 5-line Snellen reduction (0.49 logMAR) in patients with cataracts and a 1-line reduction (-0.13 logMAR) in patients without cataracts. Among patients with cataracts, 83% stated the device accurately represented the difficulty experienced while driving at night (P < .001); among participants without cataracts, 71% reported being minimally affected by glare from the device (P = .003). A new controlled point source LED glare tester demonstrated the adverse effect on visual acuity due to glare in patients with cataract, accurately simulated night driving glare issues for patients with cataracts, and was rated as easy to use and useful by investigators. Copyright 2015, SLACK Incorporated.

  3. Graphics Education Survey. Part II.

    ERIC Educational Resources Information Center

    Ernst, Sandra B.

    After a 1977 survey reflected the importance of graphics education for news students, a study was developed to investigate the state of graphics education in the whole field of journalism. A questionnaire was sent to professors and administrators in four print-oriented professional fields of education: magazine, advertising, public relations, and…

  4. Eye movement and pupil size constriction under discomfort glare.

    PubMed

    Lin, Yandan; Fotios, Steve; Wei, Minchen; Liu, Yihong; Guo, Weihong; Sun, Yaojie

    2015-01-29

    Involuntary physiological responses offer an alternative means to psychophysical procedures for objectively evaluating discomfort glare. This study examined eye movement and pupil size responses to glare discomfort using new approaches to analysis: relative pupil size and speed of eye movement. Participants evaluated glare discomfort using the standard de Boer rating scale under various conditions manipulated to influence glare discomfort. Eye movement was recorded using an electro-oculogram (EOG), and pupil size was recorded using Tobii glasses. Ten young (mean age: 24.5 years old) and 10 senior (mean age: 61 years old) participants were recruited for this experiment. Subjective evaluation of glare discomfort was highly correlated with eye movement (multiple correlation coefficient [R(2)] of >0.94, P < 0.001) and pupil constriction (R(2) = 0.38, P < 0.001). Severe glare discomfort increased the speed of eye movement and caused larger pupil constriction. Larger variations of eye movement were found among seniors. The two physiological responses studied here to characterize discomfort glare under various lighting conditions had significant correlation with the subjective evaluation. The correlation between discomfort glare and physiological responses suggests an objective way to characterize and evaluate discomfort glare that may overcome the problems of conventional subjective evaluation. It also offers an explanation as to why long-term exposure to discomfort glare leads to visual fatigue and eyestrain. Copyright 2015 The Association for Research in Vision and Ophthalmology, Inc.

  5. Sloan Digital Sky Survey II (SDSS-II) Supernova Data

    DOE Data Explorer

    The Sloan Digital Sky Survey (SDSS) is a series of three interlocking imaging and spectroscopic surveys, carried out over an eight-year period with a dedicated 2.5m telescope located at Apache Point Observatory in Southern New Mexico. The SDSS Supernova Survey was one of those three components of SDSS and SDSS-II, a 3-year extension of the original SDSS that operated from July 2005 to July 2008. The Supernova Survey was a time-domain survey, involving repeat imaging of the same region of sky every other night, weather permitting. The primary scientific motivation was to detect and measure light curves for several hundred supernovae through repeat scans of the SDSS Southern equatorial stripe 82 (about 2.5? wide by ~120? long). Over the course of three 3-month campaigns SDSS-II SN discovered and measured multi-band lightcurves for ~500 spectroscopically confirmed Type Ia supernovae in the redshift range z=0.05-0.4. In addition, the project harvested a few hundred light curves for SNe Ia and discovered about 80 spectroscopically confirmed core-collapse supernovae (supernova types Ib/c and II).

  6. Veiling glare reduction methods compared for ophthalmic applications

    NASA Technical Reports Server (NTRS)

    Buchele, D. R.

    1981-01-01

    Veiling glare in ocular viewing was simulated by viewing the retina of an eye model through a sheet of light-scattering material lit from the front. Four methods of glare reduction were compared, namely, optical scanning, polarized light, viewing and illumination paths either coaxial or intersecting at the object, and closed circuit TV. Photographs show the effect of these methods on visibility. Polarized light was required to eliminate light specularly reflected from the instrument optics. The greatest glare reduction was obtained when the first three methods were utilized together. Glare reduction using TV was limited by nonuniform distribution of scattered light over the image.

  7. MMT Survey for Intervening Mg II Absorption

    NASA Astrophysics Data System (ADS)

    Nestor, Daniel B.; Turnshek, David A.; Rao, Sandhya M.

    2006-05-01

    We present the results from a spectroscopic survey for intervening Mg II absorption in the spectra of 381 background QSOs conducted at the MMT telescope. This survey complements our earlier SDSS EDR Mg II survey, extending our results to lower redshift (z~=0.15) and weaker Mg II λ2796 rest equivalent width (Wλ27960~=0.1 Å). We confirm two major results from that survey: the transition in the Wλ27960 distribution at Wλ27960~0.3 Å, and the Wλ27960-dependent evolution of the incidence of systems. The nature of ∂2N/∂z∂Wλ27960 is consistent with the idea that multiple physically distinct components/processes contribute to the incidence of Mg II absorption systems in a W0-dependent manner and evolve at different rates. A significant decrease in the total proper absorption cross section is detected in our MMT data for systems as weak as 1.0 Å<=Wλ27960<1.5 Å at z<~0.4. We discuss this W0-dependent evolution in the context of the evolution of galaxy structures, processes including superwinds and interactions, and damped-Lyα absorbers. We also consider the possibility that the observed redshift and Wλ27960 dependence of the incidence of absorption in spectroscopic surveys for low-ionization/neutral gas results from the effects of dust-induced extinction. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona.

  8. THE ARECIBO H II REGION DISCOVERY SURVEY

    SciTech Connect

    Bania, T. M.; Anderson, L. D.; Balser, Dana S.

    2012-11-10

    We report the detection of radio recombination line (RRL) emission using the Arecibo Observatory at X band (9 GHz, 3 cm) from 37 previously unknown H II regions in the Galactic zone 66 Degree-Sign {>=} l {>=} 31 Degree-Sign and | b | {<=} 1 Degree-Sign . This Arecibo H II Region Discovery Survey (Arecibo HRDS) is a continuation of the Green Bank Telescope (GBT) HRDS. The targets for the Arecibo HRDS have spatially coincident 24 {mu}m and 20 cm emission of a similar angular morphology and extent. To take advantage of Arecibo's sensitivity and small beam size, sources in this sample are fainter, smaller in angle, or in more crowded fields compared to those of the GBT HRDS. These Arecibo nebulae are some of the faintest H II regions ever detected in RRL emission. Our detection rate is 58%, which is low compared to the 95% detection rate for GBT HRDS targets. We derive kinematic distances to 23 of the Arecibo HRDS detections. Four nebulae have negative local standard of rest velocities and are thus unambiguously in the outer Galaxy. The remaining sources are at the tangent-point distance or farther. We identify a large, diffuse H II region complex that has an associated H I and {sup 13}CO shell. The {approx}90 pc diameter of the G52L nebula in this complex may be the largest Galactic H II region known, and yet it has escaped previous detection.

  9. The Arecibo H II Region Discovery Survey

    NASA Astrophysics Data System (ADS)

    Bania, Thomas M.; Anderson, L. D.; Balser, D. S.

    2013-01-01

    We report the detection of radio recombination line emission (RRL) using the Arecibo Observatory at X-band (9 GHz, 3 cm) from 37 previously unknown H II regions in the Galactic zone 66 deg > l_gal > 31 deg and | b | < 1 deg. This Arecibo H II Region Discovery Survey (Arecibo HRDS) is a continuation of the Green Bank Telescope (GBT) HRDS. The targets for the Arecibo HRDS have spatially coincident 24 micron and 20 cm emission of a similar angular morphology and extent. To take advantage of Arecibo's sensitivity and small beam size, sources in this sample are fainter, smaller in angle, or in more crowded fields compared to those of the GBT HRDS. These Arecibo nebulae are some of the faintest H II regions ever detected in RRL emission. Our detection rate is 58%, which is low compared to the 95% detection rate for GBT HRDS targets. We derive kinematic distances to 23 of the Arecibo HRDS detections. Four nebulae have negative LSR velocities and are thus unambiguously in the outer Galaxy. The remaining sources are at the tangent point distance or farther. We identify a large, diffuse H II region complex that has an associated HI and 13-CO shell. The ~90 pc diameter of the G52L nebula in this complex may be the largest Galactic H II region known, and yet it has escaped previous detection.

  10. Macular pigment spatial distribution effects on glare disability.

    PubMed

    Putnam, Christopher M; Bassi, Carl J

    2015-01-01

    This project explored the relationship of the macular pigment optical density (MPOD) spatial profile with measures of glare disability (GD) across the macula. A novel device was used to measure MPOD across the central 16° of retina along four radii using customized heterochromatic flicker photometry (cHFP)at eccentricities of 0°, 2°, 4°, 6° and 8°. MPOD was measured as discrete and integrated values at all measured retinal loci. GD was calculated as a difference in contrast sensitivity (CS) between no glare and glare conditions using identical stimuli presented at the same eccentricities. GD was defined as [(CSNo Glare-CSGlare)/CSNo Glare] in order to isolate the glare attenuation effects of MPOD by controlling for CS variability among the subject sample. Correlations of the discrete and integrated MPOD with GD were compared. The cHFP identified reliable MPOD spatial distribution maps demonstrating a 1st-order exponential decay as a function of increasing eccentricity. There was a significant negative correlation between both measures of foveal MPOD and GD using 6 cycles per degree (cpd) and 9 cpd stimuli. Significant correlations were found between corresponding parafoveal MPOD measures and GD at 2 and 4° of eccentricity using 9 cpd stimuli with greater MPOD associated with less glare disability. These results are consistent with the glare attenuation effects of MP at higher spatial frequencies and support the hypothesis that discrete and integrated measures of MPOD have similar correlations with glare attenuation effects across the macula. Additionally, peak foveal MPOD appears to influence GD across the macula. Copyright © 2014 Spanish General Council of Optometry. Published by Elsevier Espana. All rights reserved.

  11. Macular pigment spatial distribution effects on glare disability

    PubMed Central

    Putnam, Christopher M.; Bassi, Carl J.

    2015-01-01

    Purpose This project explored the relationship of the macular pigment optical density (MPOD) spatial profile with measures of glare disability (GD) across the macula. Methods A novel device was used to measure MPOD across the central 16° of retina along four radii using customized heterochromatic flicker photometry (cHFP)at eccentricities of 0°, 2°, 4°, 6° and 8°. MPOD was measured as discrete and integrated values at all measured retinal loci. GD was calculated as a difference in contrast sensitivity (CS) between no glare and glare conditions using identical stimuli presented at the same eccentricities. GD was defined as [(CSNo Glare − CSGlare)/CSNo Glare] in order to isolate the glare attenuation effects of MPOD by controlling for CS variability among the subject sample. Correlations of the discrete and integrated MPOD with GD were compared. Results The cHFP identified reliable MPOD spatial distribution maps demonstrating a 1st-order exponential decay as a function of increasing eccentricity. There was a significant negative correlation between both measures of foveal MPOD and GD using 6 cycles per degree (cpd) and 9 cpd stimuli. Significant correlations were found between corresponding parafoveal MPOD measures and GD at 2 and 4° of eccentricity using 9 cpd stimuli with greater MPOD associated with less glare disability. Conclusions These results are consistent with the glare attenuation effects of MP at higher spatial frequencies and support the hypothesis that discrete and integrated measures of MPOD have similar correlations with glare attenuation effects across the macula. Additionally, peak foveal MPOD appears to influence GD across the macula. PMID:25697374

  12. META-GLARE: a shell for CIG systems.

    PubMed

    Bottrighi, Alessio; Rubrichi, Stefania; Terenziani, Paolo

    2015-01-01

    In the last twenty years, many different approaches to deal with Computer-Interpretable clinical Guidelines (CIGs) have been developed, each one proposing its own representation formalism (mostly based on the Task-Network Model) execution engine. We propose META-GLARE a shell for easily defining new CIG systems. Using META-GLARE, CIG system designers can easily define their own systems (basically by defining their representation language), with a minimal programming effort. META-GLARE is thus a flexible and powerful vehicle for research about CIGs, since it supports easy and fast prototyping of new CIG systems.

  13. Solar glare hazard analysis tool on account of determined points of time

    SciTech Connect

    Ho, Clifford K; Sims, Cianan Alexander

    2014-09-23

    Technologies pertaining to determining when glare will be perceived by a hypothetical observer from a glare source and the intensity of glare that will be perceived by the hypothetical observer from the glare source are described herein. A first location of a potential source of solar glare is received, and a second location of the hypothetical observer is received. Based upon such locations, including respective elevations, and known positions of the sun over time, a determination as to when the hypothetical observer will perceive glare from the potential source of solar glare is made. Subsequently, an amount of irradiance entering the eye of the hypothetical observer is calculated to assess potential ocular hazards.

  14. The mechanical behavior of GLARE laminates for aircraft structures

    NASA Astrophysics Data System (ADS)

    Wu, Guocai; Yang, J.-M.

    2005-01-01

    GLARE (glass-reinforced aluminum laminate) is a new class of fiber metal laminates for advanced aerospace structural applications. It consists of thin aluminum sheets bonded together with unidirectional or biaxially reinforced adhesive prepreg of high-strength glass fibers. GLARE laminates offer a unique combination of properties such as outstanding fatigue resistance, high specific static properties, excellent impact resistance, good residual and blunt notch strength, flame resistance and corrosion properties, and ease of manufacture and repair. GLARE laminates can be tailored to suit a wide variety of applications by varying the fiber/resin system, the alloy type and thickness, stacking sequence, fiber orientation, surface pretreatment technique, etc. This article presents a comprehensive overview of the mechanical properties of various GLARE laminates under different loading conditions.

  15. Google Glass Glare: disability glare produced by a head-mounted visual display.

    PubMed

    Longley, Chris; Whitaker, David

    2016-03-01

    Head mounted displays are a type of wearable technology - a market that is projected to expand rapidly over the coming years. Probably the most well known example is the device Google Glass (or 'Glass'). Here we investigate the extent to which the device display can interfere with normal visual function by producing monocular disability glare. Contrast sensitivity was measured in two normally sighted participants, 32 and 52 years of age. Data were recorded for the right eye, the left eye and then again in a binocular condition. Measurements were taken both with and without the Glass in place, across a range of stimulus luminance levels using a two-alternative forced-choice methodology. The device produced a significant reduction in contrast sensitivity in the right eye (>0.5 log units). The level of disability glare increased as stimulus luminance was reduced in a manner consistent with intraocular light scatter, resulting in a veiling retinal illuminance. Sensitivity in the left eye was unaffected. A significant reduction in binocular contrast sensitivity occurred at lower luminance levels due to a loss of binocular summation, although binocular sensitivity was not found to fall below the sensitivity of the better monocular level (binocular inhibition). Head mounted displays such as Google Glass have the potential to cause significant disability glare in the eye exposed to the visual display, particularly under conditions of low luminance. They can also cause a more modest binocular reduction in sensitivity by eliminating the benefits of binocular summation. © 2015 The Authors Ophthalmic & Physiological Optics © 2015 The College of Optometrists.

  16. Rejection Of Scattered Radiation And Veiling Glare In A Large-Field Image-Intensifier System

    NASA Astrophysics Data System (ADS)

    Plenkovich, Dinko; Nayak, Chiraprakash

    1988-06-01

    A prototype system for digital fluorography of the chest is under development in our research laboratory. It consists of a special-procedures x-ray unit upgraded with a 40-cm image intensifier, a Compumotor driven multiple-slit assembly, and MicroVAX II based frame grabber and frame processor. Contrast in an image-intensifier x-ray system is degraded by scattered radiation and veiling glare. They both increase with the diameter of the image-intensifier input phosphor. Grids, air gaps, and paired scanning apertures are not effective against veiling glare. In our prototype system both scattered radiation and veiling glare are rejected using the electronic-collimation principle. A multiple-slit assembly is scanned between the x-ray tube and the patient. Images are recorded and digitized for each position of the slit assembly. The resultant image is reconstructed from a series of digitized slit images using an appropriate computer algorithm. Technologies for manufacturing the multiple-slit assembly and the image-reconstruction algorithms are discussed. The peak-detection algorithm does not require as accurate stepping of the slit assembly as the threshold-and-summation algorithm, but it wastes a portion of the radiation dose. Comparative single- and dual-energy images of a chest phantom are presented. Superior separation of bone and soft-tissue images was achieved when the electronic scanning slit was used because, of more efficient scatter rejection.

  17. META-GLARE: A meta-system for defining your own computer interpretable guideline system-Architecture and acquisition.

    PubMed

    Bottrighi, Alessio; Terenziani, Paolo

    2016-09-01

    Several different computer-assisted management systems of computer interpretable guidelines (CIGs) have been developed by the Artificial Intelligence in Medicine community. Each CIG system is characterized by a specific formalism to represent CIGs, and usually provides a manager to acquire, consult and execute them. Though there are several commonalities between most formalisms in the literature, each formalism has its own peculiarities. The goal of our work is to provide a flexible support to the extension or definition of CIGs formalisms, and of their acquisition and execution engines. Instead of defining "yet another CIG formalism and its manager", we propose META-GLARE (META Guideline Acquisition, Representation, and Execution), a "meta"-system to define new CIG systems. In this paper, META-GLARE, a meta-system to define new CIG systems, is presented. We try to capture the commonalities among current CIG approaches, by providing (i) a general manager for the acquisition, consultation and execution of hierarchical graphs (representing the control flow of actions in CIGs), parameterized over the types of nodes and of arcs constituting it, and (ii) a library of different elementary components of guidelines nodes (actions) and arcs, in which each type definition involves the specification of how objects of this type can be acquired, consulted and executed. We provide generality and flexibility, by allowing free aggregations of such elementary components to define new primitive node and arc types. We have drawn several experiments, in which we have used META-GLARE to build a CIG system (Experiment 1 in Section 8), or to extend it (Experiments 2 and 3). Such experiments show that META-GLARE provides a useful and easy-to-use support to such tasks. For instance, re-building the Guideline Acquisition, Representation, and Execution (GLARE) system using META-GLARE required less than one day (Experiment 1). META-GLARE is a meta-system for CIGs supporting fast prototyping

  18. Discomfort glare with complex fenestration systems and the impact on energy use when using daylighting control

    SciTech Connect

    Hoffmann, Sabine; McNeil, Andrew; Lee, Eleanor S.; Kalyanam, Raghuram

    2015-11-03

    Glare is a frequent issue in highly glazed buildings. A modelling approach is presented that uses discomfort glare probability and discomfort glare index as metrics to determine occupants’ behaviour. A glare control algorithm that actuated an interior shade for glare protection based on the predicted perception was implemented in a building simulation program. A reference case with a state-of-the-art base glazing was compared to the same glazing but with five different complex fenestration systems, i.e., exterior shades. The windows with exterior shades showed significant variations in glare frequencies. Energy use intensity in a prototypical office building with daylighting controls was greatly influenced for the systems with frequent glare occurrence. While the base glazing could benefit from glare control, some of the exterior shades showed significantly greater energy use when discomfort glare-based operation of interior shades was considered.

  19. A note on image degradation, disability glare, and binocular vision

    NASA Astrophysics Data System (ADS)

    Rajaram, Vandana; Lakshminarayanan, Vasudevan

    2013-08-01

    Disability glare due to scattering of light causes a reduction in visual performance due to a luminous veil over the scene. This causes problem such as contrast detection. In this note, we report a study of the effect of this veiling luminance on human stereoscopic vision. We measured the effect of glare on the horopter measured using the apparent fronto-parallel plane (AFPP) criterion. The empirical longitudinal horopter measured using the AFPP criterion was analyzed using the so-called analytic plot. The analytic plot parameters were used for quantitative measurement of binocular vision. Image degradation plays a major effect on binocular vision as measured by the horopter. Under the conditions tested, it appears that if vision is sufficiently degraded then the addition of disability glare does not seem to significantly cause any further compromise in depth perception as measured by the horopter.

  20. Glare-free optical system for fundus visualization

    NASA Astrophysics Data System (ADS)

    Salakhutdinov, Viktor K.; Smetanin, Yuriy G.; Doroshenko, Jasser; Sivachenko, Eugene A.

    2014-05-01

    The paper describes results of development of fundus-camera with non-glare optical scheme. The scheme is based on multiple lenses with a light gathering power (D/F <= 1) substantially less than one. Illumination of fundus can be provided through eye's pupil less than 3 mm. And much attention was directed to method of calculation of the no-glare optical scheme. The key idea is that geometry of optic elements of the system provides that glare in the form of ghost reflection from optical surface of one element focuses on a small-size absorbing screen located on another optical surface. Shows the possibility of implementation and the experimental results. During experiments with B/W camera we got Full HD color image of fundus having the eye's pupil diameter of 1.5 mm and illumination of fundus tissue in accordance with sanitary rules.

  1. A real-time monitoring system for night glare protection

    NASA Astrophysics Data System (ADS)

    Ma, Jun; Ni, Xuxiang

    2010-11-01

    When capturing a dark scene with a high bright object, the monitoring camera will be saturated in some regions and the details will be lost in and near these saturated regions because of the glare vision. This work aims at developing a real-time night monitoring system. The system can decrease the influence of the glare vision and gain more details from the ordinary camera when exposing a high-contrast scene like a car with its headlight on during night. The system is made up of spatial light modulator (The liquid crystal on silicon: LCoS), image sensor (CCD), imaging lens and DSP. LCoS, a reflective liquid crystal, can modular the intensity of reflective light at every pixel as a digital device. Through modulation function of LCoS, CCD is exposed with sub-region. With the control of DSP, the light intensity is decreased to minimum in the glare regions, and the light intensity is negative feedback modulated based on PID theory in other regions. So that more details of the object will be imaging on CCD and the glare protection of monitoring system is achieved. In experiments, the feedback is controlled by the embedded system based on TI DM642. Experiments shows: this feedback modulation method not only reduces the glare vision to improve image quality, but also enhances the dynamic range of image. The high-quality and high dynamic range image is real-time captured at 30hz. The modulation depth of LCoS determines how strong the glare can be removed.

  2. Computation of glint, glare, and solar irradiance distribution

    DOEpatents

    Ho, Clifford Kuofei; Khalsa, Siri Sahib Singh

    2015-08-11

    Described herein are technologies pertaining to computing the solar irradiance distribution on a surface of a receiver in a concentrating solar power system or glint/glare emitted from a reflective entity. At least one camera captures images of the Sun and the entity of interest, wherein the images have pluralities of pixels having respective pluralities of intensity values. Based upon the intensity values of the pixels in the respective images, the solar irradiance distribution on the surface of the entity or glint/glare corresponding to the entity is computed.

  3. Computation of glint, glare, and solar irradiance distribution

    DOEpatents

    Ho, Clifford Kuofei; Khalsa, Siri Sahib Singh

    2017-08-01

    Described herein are technologies pertaining to computing the solar irradiance distribution on a surface of a receiver in a concentrating solar power system or glint/glare emitted from a reflective entity. At least one camera captures images of the Sun and the entity of interest, wherein the images have pluralities of pixels having respective pluralities of intensity values. Based upon the intensity values of the pixels in the respective images, the solar irradiance distribution on the surface of the entity or glint/glare corresponding to the entity is computed.

  4. Optical design of low glare luminaire applied for tunnel light

    NASA Astrophysics Data System (ADS)

    Tsai, M. S.; Lee, X. H.; Lo, Y. C.; Sun, C. C.

    2014-09-01

    In this study, a low glare and high-efficient tunnel lighting design which consists of a cluster light-emitting diode and a free-form lens is presented. Most of the energy emitted from the proposed luminaire is transmitted onto the surface of the road in front of drivers, and the probability that the energy is emitted directly into drivers' eyes is low. Compared with traditional fluorescent lamps, the proposed luminaire, of which the optical utilization factor, optical efficiency, and uniformity are, respectively, 44%, 92.5%, and 0.72, performs favorably in traffic safety, energy saving, and glare reduction.

  5. PHLUX: Photographic Flux Tools for Solar Glare and Flux

    SciTech Connect

    2010-12-02

    A web-based tool to a) analytically and empirically quantify glare from reflected light and determine the potential impact (e.g., temporary flash blindness, retinal burn), and b) produce flux maps for central receivers. The tool accepts RAW digital photographs of the glare source (for hazard assessment) or the receiver (for flux mapping), as well as a photograph of the sun for intensity and size scaling. For glare hazard assessment, the tool determines the retinal irradiance (W/cm2) and subtended source angle for an observer and plots the glare source on a hazard spectrum (i.e., low-potential for flash blindness impact, potential for flash blindness impact, retinal burn). For flux mapping, the tool provides a colored map of the receiver scaled by incident solar flux (W/m2) and unwraps the physical dimensions of the receiver while accounting for the perspective of the photographer (e.g., for a flux map of a cylindrical receiver, the horizontal axis denotes receiver angle in degrees and the vertical axis denotes vertical position in meters; for a flat panel receiver, the horizontal axis denotes horizontal position in meters and the vertical axis denotes vertical position in meters). The flux mapping capability also allows the user to specify transects along which the program plots incident solar flux on the receiver.

  6. 77 FR 27118 - Safety Zone; Rocketts Red Glare Fireworks, Ancarrows Landing Park, James River, Richmond, VA

    Federal Register 2010, 2011, 2012, 2013, 2014

    2012-05-09

    ... SECURITY Coast Guard 33 CFR Part 165 RIN 1625-AA00 Safety Zone; Rocketts Red Glare Fireworks, Ancarrows... in Richmond, VA in support of the Rocketts Red Glare Fireworks event. This action is necessary to provide for the safety of life on navigable waters during the Rocketts Red Glare Fireworks show. This...

  7. 77 FR 13525 - Safety Zone; Rocketts Red Glare Fireworks, Ancarrows Landing Park, James River, Richmond, VA

    Federal Register 2010, 2011, 2012, 2013, 2014

    2012-03-07

    ... SECURITY Coast Guard 33 CFR Part 165 RIN 1625-AA00 Safety Zone; Rocketts Red Glare Fireworks, Ancarrows... safety of life on navigable waters during the Rocketts Red Glare Fireworks show. This action is intended....T05-0114 to read as follows: Sec. 165.T05-0114 Safety Zone; Rocketts Red Glare Fireworks, Ancarrows...

  8. 12. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    12. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  9. 22. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    22. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  10. 18. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    18. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  11. 13. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    13. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  12. 15. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    15. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  13. 8. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    8. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  14. 24. July 1971 AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    24. July 1971 AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  15. 20. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    20. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  16. 11. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    11. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  17. 9. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    9. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  18. 16. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    16. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  19. 7. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    7. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  20. 17. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    17. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  1. 19. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    19. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  2. 14. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    14. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  3. 10. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    10. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  4. 23. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    23. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  5. 21. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    21. July 1971. AERIAL RECONNAISSANCE II, ERIE RAILWAY SURVEY. - Erie Railway, Bradford Division, Bridge 27.66, Spanning Kinzua Creek Valley, 1.5 miles northeast of Kushequa, Mount Jewett, McKean County, PA

  6. The Extended Northern ROSAT Galaxy Cluster Survey (NORAS II). I. Survey Construction and First Results

    NASA Astrophysics Data System (ADS)

    Böhringer, Hans; Chon, Gayoung; Retzlaff, Jörg; Trümper, Joachim; Meisenheimer, Klaus; Schartel, Norbert

    2017-05-01

    As the largest, clearly defined building blocks of our universe, galaxy clusters are interesting astrophysical laboratories and important probes for cosmology. X-ray surveys for galaxy clusters provide one of the best ways to characterize the population of galaxy clusters. We provide a description of the construction of the NORAS II galaxy cluster survey based on X-ray data from the northern part of the ROSAT All-Sky Survey. NORAS II extends the NORAS survey down to a flux limit of 1.8 × 10-12 erg s-1 cm-2 (0.1-2.4 keV), increasing the sample size by about a factor of two. The NORAS II cluster survey now reaches the same quality and depth as its counterpart, the southern REFLEX II survey, allowing us to combine the two complementary surveys. The paper provides information on the determination of the cluster X-ray parameters, the identification process of the X-ray sources, the statistics of the survey, and the construction of the survey selection function, which we provide in numerical format. Currently NORAS II contains 860 clusters with a median redshift of z = 0.102. We provide a number of statistical functions, including the log N-log S and the X-ray luminosity function and compare these to the results from the complementary REFLEX II survey. Using the NORAS II sample to constrain the cosmological parameters, σ 8 and Ω m , yields results perfectly consistent with those of REFLEX II. Overall, the results show that the two hemisphere samples, NORAS II and REFLEX II, can be combined without problems into an all-sky sample, just excluding the zone of avoidance.

  7. KENNEDY SPACE CENTER, FLA. - From a burst of fire and smoke, the Delta II launch vehicle races into the sky carrying the second Mars Exploration Rover, Opportunity. The bright glare briefly illuminated Florida Space Coast beaches. Opportunity’s dash to Mars began with liftoff at 11:18:15 p.m. Eastern Daylight Time from Cape Canaveral Air Force Station, Fla. The spacecraft separated successfully from the Delta's third stage 83 minutes later, after it had been boosted out of Earth orbit and onto a course toward Mars.

    NASA Image and Video Library

    2003-07-07

    KENNEDY SPACE CENTER, FLA. - From a burst of fire and smoke, the Delta II launch vehicle races into the sky carrying the second Mars Exploration Rover, Opportunity. The bright glare briefly illuminated Florida Space Coast beaches. Opportunity’s dash to Mars began with liftoff at 11:18:15 p.m. Eastern Daylight Time from Cape Canaveral Air Force Station, Fla. The spacecraft separated successfully from the Delta's third stage 83 minutes later, after it had been boosted out of Earth orbit and onto a course toward Mars.

  8. KENNEDY SPACE CENTER, FLA. - NASA launches its second Mars Exploration Rover, Opportunity, aboard a Delta II launch vehicle. The bright glare briefly illuminated Florida Space Coast beaches. Opportunity’s dash to Mars began with liftoff at 11:18:15 p.m. Eastern Daylight Time from Cape Canaveral Air Force Station, Fla. The spacecraft separated successfully from the Delta's third stage 83 minutes later, after it had been boosted out of Earth orbit and onto a course toward Mars. [Photo courtesy of Ray Yost and Scott Andrews/NIKON

    NASA Image and Video Library

    2003-07-07

    KENNEDY SPACE CENTER, FLA. - NASA launches its second Mars Exploration Rover, Opportunity, aboard a Delta II launch vehicle. The bright glare briefly illuminated Florida Space Coast beaches. Opportunity’s dash to Mars began with liftoff at 11:18:15 p.m. Eastern Daylight Time from Cape Canaveral Air Force Station, Fla. The spacecraft separated successfully from the Delta's third stage 83 minutes later, after it had been boosted out of Earth orbit and onto a course toward Mars. [Photo courtesy of Ray Yost and Scott Andrews/NIKON

  9. Balancing solar shading, daylighting and glare with translucent louvers

    SciTech Connect

    Jackaway, A.; Davies, M.

    1997-12-31

    Successful design of comfortable low-energy office buildings implicitly requires careful consideration for solar shading, daylighting, and the control of glare. Yet these inherently intertwined issues often demand conflicting design responses that pose difficult challenges for designers who frequently discover that successfully addressing one issue means sacrificing the performance with another. This is most commonly observed when excessive shading and glare control strategies reduce interior daylighting so significantly that electric lighting is operated at full capacity directly adjacent to fully glazed facades. The new Phoenix office building at England`s Building Research Establishment (BRE) employs an operable external translucent louver system along its southern facade to achieve a reasonable balance of these issues without significantly sacrificing individual performance. This paper describes the configuration and developmental processes for this system.

  10. ARGOS - II. The Galactic bulge survey

    NASA Astrophysics Data System (ADS)

    Freeman, K.; Ness, M.; Wylie-de-Boer, E.; Athanassoula, E.; Bland-Hawthorn, J.; Asplund, M.; Lewis, G.; Yong, D.; Lane, R.; Kiss, L.; Ibata, R.

    2013-02-01

    We describe the motivation, field locations and stellar selection for the Abundances and Radial velocity Galactic Origins Survey (ARGOS) spectroscopic survey of 28 000 stars in the bulge and inner disc of the Milky Way galaxy across latitudes of b = -5° to -10°. The primary goal of this survey is to constrain the formation processes of the bulge and establish whether it is predominantly a merger or instability remnant. From the spectra (R = 11 000), we have measured radial velocities and determined stellar parameters, including metallicities and [α/Fe] ratios. Distances were estimated from the derived stellar parameters and about 14 000 stars are red giants within 3.5 kpc of the Galactic Centre. In this paper, we present the observations and analysis methods. Subsequent papers (III and IV) will discuss the stellar metallicity distribution and kinematics of the Galactic bulge and inner disc, and the implications for the formation of the bulge.

  11. University Benefits Survey. Part II (Pensions).

    ERIC Educational Resources Information Center

    University of Western Ontario, London.

    Results of a 1985 survey of pensions at 17 Ontario, Canada, universities are presented. Information is provided on: eligibility, types of plans, member contributions, university contributions, benefits on normal retirement (age 65) and on early retirement (age 55), benefits on termination and on death, indexing and annuities, trustee and…

  12. Status of the Transneptunian Automated Occultation Survey (TAOS II)

    NASA Astrophysics Data System (ADS)

    Lehner, Matthew; Wang, Shiang-Yu; Alcock, Charles; Reyes-Ruiz, Mauricio; Castro, Joel; Chen, Wen Ping; Chu, You-Hua; Cook, Kem H.; Geary, John C.; Huang, Chung-Kai; Kim, Dae-Won; Norton, Timothy; Szentgyorgyi, Andrew; Yen, WeiLing; Zhang, Zhi-Wei; Figueroa, Liliana

    2016-10-01

    The Transneptunian Automated Occultation Survey (TAOS II) will aim to detect occultations of stars by small (~1 km diameter) objects in the Kuiper Belt and beyond. Such events are very rare ($<0.001 events per star per year) and short in duration (~200 ms), so many stars must be monitored at a high readout cadence. TAOS II will operate three 1.3 meter telescopes at the Observatorio Astronomico Nacional at San Pedro Martir in Baja California, Mexico. With a 2.3 square degree field of view and a high speed camera comprising CMOS imagers, the survey will monitor 10,000 stars simultaneously with all three telescopes at a readout cadence of 20 Hz. Construction of the site began in the fall of 2013, and the survey will begin in the summer of 2017. This poster will provide an update on the status of the survey development and the schedule leading to the beginning of survey operations.

  13. Pajarito Plateau archaeological surveys and excavations. II

    SciTech Connect

    Steen, C R

    1982-04-01

    Los Alamos National Laboratory continues its archaeological program of data gathering and salvage excavations. Sites recently added to the archaeological survey are described, as well as the results of five excavations. Among the more interesting and important discoveries are (1) the apparently well-established local use of anhydrous lime, and (2) a late pre-Columbian use of earlier house sites and middens for garden plots. Evidence indicated that the local puebloan population was the result of an expansion of upper Rio Grande peoples, not an influx of migrants.

  14. Status of the Transneptunian Automated Occultation Survey (TAOS II)

    NASA Astrophysics Data System (ADS)

    Lehner, Matthew J.; Wang, Shiang Yu; Reyes-Ruiz, Mauricio; Chu, You Hua; Lee, William; Zhang, Zhi Wei; Cook, Kem H.; Norton, Timothy; Szentgyorgyi, Andrew; Alcock, Charles

    2015-11-01

    The Transneptunian Automated Occultation Survey (TAOS II) will aim to detect occultations of stars by small (~1 km diameter) objects in the Kuiper Belt and beyond. Such events are very rare (<10-3 events per star per year) and short in duration (~200 ms), so many stars must be monitored at a high readout cadence. TAOS II will operate three 1.3 meter telescopes at the Observatorio Astronómico Nacional at San Pedro Mártir in Baja California, México. With a 2.3 square degree field of view and a high speed camera comprising CMOS imagers, the survey will monitor 10,000 stars simultaneously with all three telescopes at a nominal readout cadence of 20 Hz. Construction of the site began in the fall of 2013. We present here an update on the status of the TAOS II survey, including the site development, camera fabrication, and project schedule.

  15. Glare Recovery of a Two Dimensional Tracking Task with Respect to Various Colors

    DTIC Science & Technology

    1976-04-01

    basically as shown in fi~’ure 8. When light enters the eye a photosensitive element (S) is decomposed and becomes opsin (0) and retinene (R . The...Comparator button 104 is then pressed high which activates the glare source which consists of two automotive type headlights. The glare source is...glare periods. Based on the results of this study it would appear that because the greatest portion of today’s aviation activities are using the

  16. Loading-unloading response of circular GLARE fiber-metal laminates under lateral indentation

    NASA Astrophysics Data System (ADS)

    Tsamasphyros, George J.; Bikakis, George S.

    2015-01-01

    GLARE is a Fiber-Metal laminated material used in aerospace structures which are frequently subjected to various impact damages. Hence, the response of GLARE plates subjected to lateral indentation is very important. In this paper, analytical expressions are derived and a non-linear finite element modeling procedure is proposed in order to predict the static load-indentation curves of circular GLARE plates during loading and unloading by a hemispherical indentor. We have recently published analytical formulas and a finite element procedure for the static indentation of circular GLARE plates which are now used during the loading stage. Here, considering that aluminum layers are in a state of membrane yield and employing energy balance during unloading, the unloading path is determined. Using this unloading path, an algebraic equation is derived for calculating the permanent dent depth of the GLARE plate after the indentor's withdrawal. Furthermore, our finite element procedure is modified in order to simulate the unloading stage as well. The derived formulas and the proposed finite element modeling procedure are applied successfully to GLARE 2-2/1-0.3 and to GLARE 3-3/2-0.4 circular plates. The analytical results are compared with corresponding FEM results and a good agreement is found. The analytically calculated permanent dent depth is within 6 % for the GLARE 2 plate, and within 7 % for the GLARE 3 plate, of the corresponding numerically calculated result. No other solution of this problem is known to the authors.

  17. European cardiac resynchronization therapy survey II: rationale and design.

    PubMed

    Dickstein, Kenneth; Normand, Camilla; Anker, Stefan D; Auricchio, Angelo; Blomström, Carina Lundqvist; Lundqvist, Carina Blomström; Bogale, Nigussie; Cleland, John; Filippatos, Gerasimos; Gasparini, Maurizio; Gitt, Anselm; Hindricks, Gerhard; Kuck, Karl-Heinz; Ponikowski, Piotr; Stellbrink, Christoph; Ruschitzka, Frank; Linde, Cecilia

    2015-01-01

    The Cardiac Resynchronization Therapy (CRT) Survey II is a 6 months snapshot survey initiated by two ESC Associations, the European Heart Rhythm Association and the Heart Failure Association, which is designed to describe clinical practice regarding implantation of CRT devices in a broad sample of hospitals in 47 ESC member countries. The large volume of clinical and demographic data collected should reflect current patient selection, implantation, and follow-up practice and provide information relevant for assessing healthcare resource utilization in connection with CRT. The findings of this survey should permit representative benchmarking both nationally and internationally across Europe.

  18. Ca II absorbers in the Sloan Digital Sky Survey: statistics

    NASA Astrophysics Data System (ADS)

    Sardane, Gendith M.; Turnshek, David A.; Rao, Sandhya M.

    2014-10-01

    We present the results of a survey for Ca II λλ3934, 3969 absorption-line systems culled from ˜95 000 Sloan Digital Sky Survey (SDSS) Data Release 7 and Data Release 9 quasar spectra. With 435 doublets identified in the catalogue, this list is the largest Ca II catalogue compiled to date, spanning redshifts z < 1.34, which corresponds to the most recent ˜8.9 Gyr of the history of the Universe. We derive statistics on the Ca II rest equivalent width distribution and incidence. We find that the λ3934 rest equivalent width (W0^{λ 3934}) distribution cannot be described by a single exponential function. A double exponential function is required to produce a satisfactory description. The function can be written as a sum of weak and strong components: {partial n}/{partial W0^{λ 3934}}= ({N_{wk}^{ast }}/{W_{wk}^{ast }}) exp ({ -{W0^{λ 3934}}/{W_{wk}^{ast } } }) + ({N_{str}^{ast }}/{W_{str}^{ast }}) exp ({ -{W0^{λ 3934}}/{W_{str}^{ast } } }). A maximum likelihood fit to the unbinned data indicates N_{wk}^{ast }=0.140± 0.029, W_{wk}^{ast }=0.165± 0.020 \\unicode{197}, N_{str}^{ast }=0.024± 0.020, and W_{str}^{ast }=0.427± 0.101 Å. This suggests that the Ca II absorbers are composed of at least two distinct populations. The incidence of the overall Ca II absorber population does not show evidence for evolution in the standard cosmology. The normalization of the no-evolution curve, i.e. the value of the Ca II incidence extrapolated to redshift z = 0, for W0^{λ 3934} ≥ 0.3 Å, is n0 = 0.017 ± 0.001. In comparison to Mg II surveys, we found that only 3 per cent of Mg II systems in the SDSS have Ca II, confirming that Ca II systems are rare. We also report on some preliminary investigations of the nature of the two populations of Ca II absorbers, and show that they can likely be distinguished using their Mg II properties.

  19. Status of the Transneptunian Automated Occultation Survey (TAOS II)

    NASA Astrophysics Data System (ADS)

    Lehner, Matthew J.; Wang, Shiang-Yu; Reyes-Ruiz, Mauricio; Alcock, Charles; Castro, Joel; Chen, Wen-Ping; Chu, You-Hua; Cook, Kem H.; Figueroa, Liliana; Geary, John C.; Huang, Chung-Kai; Kim, Dae-Won; Norton, Timothy; Szentgyorgyi, Andrew; Yen, Wei-Ling; Zhang, Zhi-Wei

    2016-07-01

    The Transneptunian Automated Occultation Survey (TAOS II) will aim to detect occultations of stars by small ( 1 km diameter) objects in the Kuiper Belt and beyond. Such events are very rare (< 10-3 events per star per year) and short in duration ( 200 ms), so many stars must be monitored at a high readout cadence. TAOS II will operate three 1.3 meter telescopes at the Observatorio Astronómico Nacional at San Pedro Mártir in Baja California, México. With a 2.3 square degree field of view and a high speed camera comprising CMOS imagers, the survey will monitor 10,000 stars simultaneously with all three telescopes at a readout cadence of 20 Hz. Construction of the site began in the fall of 2013, and the survey will begin in the summer of 2017.

  20. Status of the Transneptunian Automated Occultation Survey (TAOS II)

    NASA Astrophysics Data System (ADS)

    Lehner, M.; Wang, S.; Zhang, Z.; Ho, P.; Yen, W.; Reyes-Ruiz, M.; Richer, M.; Cook, K.; Hsu, S.; Chen, H.; Chang, Y.; Hiriart, D.; Ricci, D.; Szentgyorgyi, A.; Norton, T.; Geary, J.; Furesz, G.; Alcock, C.; Byun, Y.

    2014-07-01

    The Transneptunian Automated Occultation Survey (TAOS II) will aim to detect occultations of stars by small (˜1 km diameter) objects in the Transneptunian region and beyond. Such events are very rare (<10^{-3} events per star per year) and short in duration (˜200 ms), so many stars must be monitored at a high readout cadence. TAOS II will operate three 1.3 meter telescopes at the Observatorio Astronómico Nacional at San Pedro Mártir in Baja California, México. With a 2.3 square degree field of view and high-speed cameras comprising arrays of custom CMOS imagers, the survey will monitor 10,000 stars simultaneously with all three telescopes at a readout cadence of 20 Hz. The survey will begin operation in 2016. This poster presents an update on the status of the site preparation and the technical development.

  1. THE GREEN BANK TELESCOPE H II REGION DISCOVERY SURVEY. II. THE SOURCE CATALOG

    SciTech Connect

    Anderson, L. D.; Bania, T. M.; Balser, Dana S.; Rood, Robert T.

    2011-06-01

    The Green Bank Telescope (GBT) H II Region Discovery Survey has doubled the number of known H II regions in the Galactic zone 343{sup 0} {<=} l {<=} 67{sup 0} with | b | {<=} 1{sup 0}. We detected 603 discrete hydrogen radio recombination line (RRL) components at 9 GHz (3 cm) from 448 targets. Our targets were selected based on spatially coincident mid-infrared and 20 cm radio continuum emission. Such sources are almost invariably H II regions; we detected hydrogen RRL emission from 95% of our target sample. The sensitivity of the GBT and the power of its spectrometer together made this survey possible. Here, we provide a catalog of the measured properties of the RRL and continuum emission from the survey nebulae. The derived survey completeness limit, 180 mJy at 9 GHz, is sufficient to detect all H II regions ionized by single O-stars to a distance of 12 kpc. These recently discovered nebulae share the same distribution on the sky as does the previously known census of Galactic H II regions. On average, however, the new nebulae have fainter continuum fluxes, smaller continuum angular sizes, fainter RRL intensities, and smaller RRL line widths. Though small in angular size, many of our new nebulae show little spatial correlation with tracers associated with extremely young H II regions, implying that our sample spans a range of evolutionary states. We discovered 34 first quadrant negative-velocity H II regions, which lie at extreme distances from the Sun and appear to be part of the Outer Arm. We found RRL emission from 208 Spitzer GLIMPSE 8.0 {mu}m 'bubble' sources, 65 of which have been cataloged previously. It thus appears that nearly all GLIMPSE bubbles are H II regions and that {approx}50% of all Galactic H II regions have a bubble morphology at 8.0 {mu}m.

  2. The Green Bank Telescope Galactic H II Region Discovery Survey

    NASA Astrophysics Data System (ADS)

    Bania, T. M.; Anderson, L. D.; Balser, Dana S.; Rood, R. T.

    2010-08-01

    We discovered a large population of previously unknown Galactic H II regions by using the Green Bank Telescope to detect their hydrogen radio recombination line emission. Since recombination lines are optically thin at 3 cm wavelength, we can detect H II regions across the entire Galactic disk. Our targets were selected based on spatially coincident 24 μm and 21 cm continuum emission. For the Galactic zone -16 ° <= ell <= 67° and |b| <= 1°, we detected 602 discrete recombination line components from 448 lines of sight, 95% of the sample targets, which more than doubles the number of known H II regions in this part of the Milky Way. We found 25 new first quadrant nebulae with negative LSR velocities, placing them beyond the solar orbit. Because we can detect all nebulae inside the solar orbit that are ionized by O-stars, the Discovery Survey targets, when combined with existing H II region catalogs, give a more accurate census of Galactic H II regions and their properties. The distribution of H II regions across the Galactic disk shows strong, narrow (~1 kpc wide) peaks at Galactic radii of 4.3 and 6.0 kpc. The longitude-velocity distribution of H II regions now gives unambiguous evidence for Galactic structure, including the kinematic signatures of the radial peaks in the spatial distribution, a concentration of nebulae at the end of the Galactic Bar, and nebulae located on the kinematic locus of the 3 Kpc Arm.

  3. THE GREEN BANK TELESCOPE GALACTIC H II REGION DISCOVERY SURVEY

    SciTech Connect

    Bania, T. M.; Anderson, L. D.; Balser, Dana S.; Rood, R. T.

    2010-08-01

    We discovered a large population of previously unknown Galactic H II regions by using the Green Bank Telescope to detect their hydrogen radio recombination line emission. Since recombination lines are optically thin at 3 cm wavelength, we can detect H II regions across the entire Galactic disk. Our targets were selected based on spatially coincident 24 {mu}m and 21 cm continuum emission. For the Galactic zone -16 {sup 0} {<=} l {<=} 67{sup 0} and |b| {<=} 1{sup 0}, we detected 602 discrete recombination line components from 448 lines of sight, 95% of the sample targets, which more than doubles the number of known H II regions in this part of the Milky Way. We found 25 new first quadrant nebulae with negative LSR velocities, placing them beyond the solar orbit. Because we can detect all nebulae inside the solar orbit that are ionized by O-stars, the Discovery Survey targets, when combined with existing H II region catalogs, give a more accurate census of Galactic H II regions and their properties. The distribution of H II regions across the Galactic disk shows strong, narrow ({approx}1 kpc wide) peaks at Galactic radii of 4.3 and 6.0 kpc. The longitude-velocity distribution of H II regions now gives unambiguous evidence for Galactic structure, including the kinematic signatures of the radial peaks in the spatial distribution, a concentration of nebulae at the end of the Galactic Bar, and nebulae located on the kinematic locus of the 3 Kpc Arm.

  4. A digital filtration technique for scatter-glare correction based on thickness estimation

    SciTech Connect

    Ersahin, A.; Molloi, S.; Qian, Y.J.

    1995-09-01

    In order to quantitate anatomical and physiological parameters such as vessel dimensions and volumetric blood flow, it is necessary to make corrections for scatter and veiling glare, which are the major sources of nonlinearities in video densitometric digital subtraction angiography (DSA). A convolution filtering technique has been investigated to estimate scatter-glare distribution in DSA images without the need to sample the scatter-glare intensity for each patient. This technique utilizes exposure parameters and image gray levels to assign equivalent Lucite thickness for every pixel in the image. The thickness information is then used to estimate scatter-glare intensity on a pixel-by-pixel basis. To test its ability to estimate scattering-glare intensity, the correction technique was applied to images of a Lucite step phantom, anthropomorphic chest phantom, head phantom, and animal models at different thicknesses, projections, and beam energies. The root-mean-square (rms) percentage error of these estimates was obtained by comparison with direct scatter-glare measurements made behind a lead strip. The average rms percentage errors in the scatter-glare estimate for the 25 phantom studies and the 17 animal studies were 6.44% and 7.96%, respectively. These results indicate that the scatter-glare intensity can be estimated with adequate accuracy for a wide range of thicknesses, projections, and beam energies using exposure parameters and gray level information.

  5. A General Quantitative Method for Evaluating the Visual Significance of Reflected Glare, Utilizing Visual Performance Data.

    ERIC Educational Resources Information Center

    Blackwell, H. Richard

    1963-01-01

    The results of all basic measurements and calculations of reflected glare for different lighting materials and conditions are presented in a series of tables and charts. All basic concepts of a quantitative method for evaluating the visual significance of reflected glare are identified in relationship to different types of visual performance. The…

  6. Dynamic illumination based system to remove the glare and improve the quality of medical images.

    PubMed

    Gupta, Vipin; Vajinepalli, Pallavi; Venkatesan, Shankar; Seth, Subhendu; Keswarpu, Payal; Nalam, Asish; Sathpathy, Akash

    2013-01-01

    Medical images taken from camera based devices (e.g. laparoscope, colposcope, retinoscope, etc) are greatly affected by numerous bright reflection spots (called glare or specular reflections). This may affect the visibility of the abnormal features (if present in the glare locations). We have developed a novel solution to overcome this problem by incorporating a multi-LED lighting solution. This will intelligently and rapidly switch on and off the LED's in a pattern that dynamically and geometrically shifts/shuffles these glare spots back and forth in the image such that every glare-affected area of a single image frame can be reconstructed from a few adjacent time-frame images. We have built the prototype that successfully demonstrates how the glare problem in the medical video/image can be satisfactorily solved, significantly enhancing the accuracy of this vital procedure in the diagnosis of diseases. We achieve 65-95% reduction in specularity on phantom model using the proposed approach.

  7. Pattern glare: the effects of contrast and color

    PubMed Central

    Monger, Laura J.; Wilkins, Arnold J.; Allen, Peter M.

    2015-01-01

    Aim: To test a theory of visual stress by investigating the inter-relationships between (1) the threshold contrast/saturation at which individuals first report discomfort when viewing colored gratings of progressively increasing contrast and decreasing saturation; (2) the choice of a colored overlay for reading; (3) any increase in reading speed when the overlay is used. Method: Ninety-five young adults, with normal color vision, reported illusions from square-wave gratings (Pattern Glare Test), chose any colored overlays that improved clarity (Intuitive Color Overlays) and read aloud randomly ordered common words (Wilkins Rate of Reading Test). This was followed by an automated choice of tints for text using various screen colors on a tablet, and a test of discomfort from patterns of progressively increasing contrast and decreasing saturation, using software developed for this study. All participants wore their optimal refractive correction throughout the procedure. Results: Fifty-eight participants chose a colored overlay and reported that it made text easier and more comfortable to read. On average, these individuals had a greater improvement in reading speed with their overlays (p = 0.003), a lower contrast threshold at which discomfort from achromatic gratings was first reported (p = 0.015), and a tendency to report more pattern glare (p = 0.052), compared to the other participants. Participants who chose both a most and least preferred tint for text using the automated procedure reported discomfort from colored gratings at a significantly higher contrast with their most preferred color compared to their least preferred color (p = 0.003). The choice of a colored tint was moderately consistent across tests. The most and least preferred colors tended to be complementary. Conclusion: Colored tints that improved reading speed reduced pattern glare both in terms of the illusion susceptibility and in terms of discomfort contrast threshold, supporting a theory of

  8. Spectral Confusion for Cosmological Surveys of Redshifted C II Emission

    NASA Technical Reports Server (NTRS)

    Kogut, A.; Dwek, E.; Moseley, S. H.

    2015-01-01

    Far-infrared cooling lines are ubiquitous features in the spectra of star-forming galaxies. Surveys of redshifted fine-structure lines provide a promising new tool to study structure formation and galactic evolution at redshifts including the epoch of reionization as well as the peak of star formation. Unlike neutral hydrogen surveys, where the 21 cm line is the only bright line, surveys of redshifted fine-structure lines suffer from confusion generated by line broadening, spectral overlap of different lines, and the crowding of sources with redshift. We use simulations to investigate the resulting spectral confusion and derive observing parameters to minimize these effects in pencilbeam surveys of redshifted far-IR line emission. We generate simulated spectra of the 17 brightest far-IR lines in galaxies, covering the 150-1300 µm wavelength region corresponding to redshifts 0 < z < 7, and develop a simple iterative algorithm that successfully identifies the 158 µm [C II] line and other lines. Although the [C II] line is a principal coolant for the interstellar medium, the assumption that the brightest observed lines in a given line of sight are always [C II] lines is a poor approximation to the simulated spectra once other lines are included. Blind line identification requires detection of fainter companion lines from the same host galaxies, driving survey sensitivity requirements. The observations require moderate spectral resolution 700 < R < 4000 with angular resolution between 20? and 10', sufficiently narrow to minimize confusion yet sufficiently large to include a statistically meaningful number of sources.

  9. SPECTRAL CONFUSION FOR COSMOLOGICAL SURVEYS OF REDSHIFTED C II EMISSION

    SciTech Connect

    Kogut, A.; Dwek, E.; Moseley, S. H.

    2015-06-20

    Far-infrared cooling lines are ubiquitous features in the spectra of star-forming galaxies. Surveys of redshifted fine-structure lines provide a promising new tool to study structure formation and galactic evolution at redshifts including the epoch of reionization as well as the peak of star formation. Unlike neutral hydrogen surveys, where the 21 cm line is the only bright line, surveys of redshifted fine-structure lines suffer from confusion generated by line broadening, spectral overlap of different lines, and the crowding of sources with redshift. We use simulations to investigate the resulting spectral confusion and derive observing parameters to minimize these effects in pencil-beam surveys of redshifted far-IR line emission. We generate simulated spectra of the 17 brightest far-IR lines in galaxies, covering the 150–1300 μm wavelength region corresponding to redshifts 0 < z < 7, and develop a simple iterative algorithm that successfully identifies the 158 μm [C ii] line and other lines. Although the [C ii] line is a principal coolant for the interstellar medium, the assumption that the brightest observed lines in a given line of sight are always [C ii] lines is a poor approximation to the simulated spectra once other lines are included. Blind line identification requires detection of fainter companion lines from the same host galaxies, driving survey sensitivity requirements. The observations require moderate spectral resolution 700 < R < 4000 with angular resolution between 20″ and 10′, sufficiently narrow to minimize confusion yet sufficiently large to include a statistically meaningful number of sources.

  10. Spectral Confusion for Cosmological Surveys of Redshifted C II Emission

    NASA Technical Reports Server (NTRS)

    Kogut, A.; Dwek, E.; Moseley, S. H.

    2015-01-01

    Far-infrared cooling lines are ubiquitous features in the spectra of star-forming galaxies. Surveys of redshifted fine-structure lines provide a promising new tool to study structure formation and galactic evolution at redshifts including the epoch of reionization as well as the peak of star formation. Unlike neutral hydrogen surveys, where the 21 cm line is the only bright line, surveys of redshifted fine-structure lines suffer from confusion generated by line broadening, spectral overlap of different lines, and the crowding of sources with redshift. We use simulations to investigate the resulting spectral confusion and derive observing parameters to minimize these effects in pencilbeam surveys of redshifted far-IR line emission. We generate simulated spectra of the 17 brightest far-IR lines in galaxies, covering the 150-1300 µm wavelength region corresponding to redshifts 0 < z < 7, and develop a simple iterative algorithm that successfully identifies the 158 µm [C II] line and other lines. Although the [C II] line is a principal coolant for the interstellar medium, the assumption that the brightest observed lines in a given line of sight are always [C II] lines is a poor approximation to the simulated spectra once other lines are included. Blind line identification requires detection of fainter companion lines from the same host galaxies, driving survey sensitivity requirements. The observations require moderate spectral resolution 700 < R < 4000 with angular resolution between 20? and 10', sufficiently narrow to minimize confusion yet sufficiently large to include a statistically meaningful number of sources.

  11. HERSCHEL GALACTIC PLANE SURVEY OF [N ii] FINE STRUCTURE EMISSION

    SciTech Connect

    Goldsmith, Paul F.; Yıldız, Umut A.; Langer, William D.; Pineda, Jorge L.

    2015-12-01

    We present the first large-scale high angular resolution survey of ionized nitrogen in the Galactic Plane through emission of its two fine structure transitions ([N ii]) at 122 and 205 μm. The observations were largely obtained with the PACS instrument onboard the Herschel Space Observatory. The lines of sight were in the Galactic plane, following those of the Herschel OTKP project GOT C+. Both lines are reliably detected at the 10{sup −8}–10{sup −7} Wm{sup −2} sr{sup −1} level over the range –60° ≤ l ≤ 60°. The rms of the intensity among the 25 PACS spaxels of a given pointing is typically less than one third of the mean intensity, showing that the emission is extended. [N ii] is produced in gas in which hydrogen is ionized, and collisional excitation is by electrons. The ratio of the two fine structure transitions provides a direct measurement of the electron density, yielding n(e) largely in the range 10–50 cm{sup −3} with an average value of 29 cm{sup −3} and N{sup +} column densities 10{sup 16}–10{sup 17} cm{sup −2}. [N ii] emission is highly correlated with that of [C ii], and we calculate that between 1/3 and 1/2 of the [C ii] emission is associated with the ionized gas. The relatively high electron densities indicate that the source of the [N ii] emission is not the warm ionized medium (WIM), which has electron densities more than 100 times smaller. Possible origins of the observed [N ii] include the ionized surfaces of dense atomic and molecular clouds, the extended low-density envelopes of H ii regions, and low-filling factor high-density fluctuations of the WIM.

  12. Observers' Judgments of the Effects of Glare on Their Visual Acuity for High and Low Contrast Stimuli.

    PubMed

    Sewall, Ashley A Stafford; Borzendowski, Stephanie A Whetsel; Tyrrell, Richard A; Stephens, Benjamin R; Rosopa, Patrick J

    2016-07-01

    Disability glare refers to a reduction in the ability to discern a stimulus that is positioned near another stimulus that has a much higher luminance. While it is common for drivers to report that they have been "blinded" by oncoming headlights, it is unclear whether observers can accurately judge when they are visually disabled by glare. This experiment sought to quantify the accuracy with which observers can judge when a glare source reduces their visual acuity. Seventeen observers estimated their disability glare threshold (DGT)-the luminance of a glare source that would be just sufficient to impair their ability to discern the orientation of a Landolt C that was surrounded by the glare source. These estimated DGTs were compared to the participant's actual DGTs. Participants consistently underestimated the intensity of glare that was required to impair their acuity. On average, estimates of glare threshold were 88% lower than actual glare threshold intensities. Participants' judgments were affected by stimulus size but not stimulus contrast. These results suggest that observers can exaggerate the debilitating effects of glare and that they can fail to appreciate that high contrast stimuli are more robust to glare. A driver who believes that even the lowest intensities of headlight glare can visually impair an oncoming driver may be reluctant to use high beam headlamps, despite their significant visibility advantages. © The Author(s) 2016.

  13. Status of the Transneptunian Automated Occultation Survey (TAOS II)

    NASA Astrophysics Data System (ADS)

    Reyes-Ruiz, Mauricio

    2014-11-01

    TAOS II is a next generation occultation survey with the goal of measuring the size distribution of the small objects (diameters between 0.5 and 30 km) in the Kuiper Belt. The project is a collaboration between the Academia Sinica Institute of Astronomy and Astrophysics, the Universidad Nacional Autonoma de Mexico, and the Harvard-Smithsonian Center for Astrophysics, The survey will operate three 1.3 m telescopes at San Pedro Martir Observatory in Baja California, Mexico. Each telescope will be equipped with a custom camera comprising a focal plane array of CMOS imagers. Each camera will be capable of reading out image data from 10,000 stars at a cadence of 20 Hz. All telescopes will monitor the same set of stars simultaneously to search for coincident occultation events while minimizing the false positive rate. This poster describes the project and reports on the progress of the development of the survey infrastructure.

  14. Development of a Headlight Glare Simulator for a Driving Simulator.

    PubMed

    Hwang, Alex D; Peli, Eli

    2013-07-01

    We describe the design and construction of a headlight glare simulator to be used with a driving simulator. The system combines a modified programmable off-the-shelf LED display board and a beamsplitter so that the LED lights, representing the headlights of oncoming cars, are superimposed over the driving simulator headlights image. Ideal spatial arrangement of optical components to avoid misalignments of the superimposed images is hard to achieve in practice and variations inevitably introduce some parallax. Furthermore, the driver's viewing position varies with driver's height and seating position preferences exacerbate such misalignment. We reduce the parallax errors using an intuitive calibration procedure (simple drag-and-drop alignment of nine LED positions with calibration dots on the screen). To simulate the dynamics of headlight brightness changes when two vehicles are approaching, LED intensity control algorithms based on both headlight and LED beam shapes were developed. The simulation errors were estimated and compared to real-world headlight brightness variability.

  15. Sloan Digital Sky Survey II (SDSS-II), Data Release 7, including the Legacy Survey

    DOE Data Explorer

    The Sloan Digital Sky Survey (SDSS) is a series of three interlocking imaging and spectroscopic surveys, carried out over an eight-year period with a dedicated 2.5m telescope located at Apache Point Observatory in Southern New Mexico. The seventh data release (DR7) from the SDSS represents a completion of the overall, original project, though SDSS-III began in 2008 and will build upon the knowledge gained already. The SDSS Legacy Survey provided a uniform, well-calibrated map of more than 7,500 square degrees of the North Galactic Cap, and three stripes in the South Galactic Cap totaling 740 square degrees. The central stripe in the South Galactic Gap, Stripe 82, was scanned multiple times to enable a deep co-addition of the data and to enable discovery of variable objects. Legacy data supported studies ranging from asteroids and nearby stars to the large-scale structure of the universe. All of the imaging data have been processed to yield calibrated astrometric and photometric parameters and classifications. These parameters are available in one or more tables in a database accessible via the Catalog Archive Server (CAS) at http://cas.sdss.org/astro. [taken and edited from the Legacy page at http://www.sdss.org/legacy/index.html] All three surveys summarized are: 1) Legacy: an imaging survey in five bands over a contiguous 7646 deg2 high-latitude elliptical region in the Northern Galactic Cap, plus an additional 750 deg2 in the Southern Galactic Cap, together with spectroscopy of complete samples of galaxies and quasars covering about 8200 square degrees. The total imaging area in the Legacy survey is 8423 square degrees; 2) SEGUE: (Sloan Extension for Galactic Understanding and Exploration): additional imaging of 3240 deg2 of sky at lower Galactic latitudes, together with spectroscopy of 240,000 stars towards 200 sight lines covering 1400 square degrees (spread throughout the Legacy and SEGUE imaging footprints), to study the structure of the Milky Way; 3

  16. Psychophysiologic sensitization to headlight glare among professional drivers with and without cardiovascular disease.

    PubMed

    Emdad, R; Belkic, K; Theorell, T; Cizinsky, S; Savic, C; Olsson, K

    1998-04-01

    Previous studies have shown that young, healthy professional drivers show heightened central nervous system arousal and cardiovascular hyperreactivity to simulated headlight glare. Electroencephalographic and cardiovascular response and recovery to simulated headlight glare (the glare pressor test) were examined in 4 groups of male professional drivers (age 25-52 years)--12 with ischemic heart disease (IHD), 12 with hypertension (HTN), 10 with borderline hypertension (BHTN), and 34 who were healthy--and in 23 non-professional driver controls--with the aim of assessing sensitization to this night driving stressor in relation to degree of cardiovascular disease severity. After glare exposure the IHD drivers showed the most pronounced alpha blockade, a rise in diastolic blood pressure (DBP; p < .05), and, unlike the other groups, a persistent fall in finger pulse volume (p < .02). The BHTN group reacted initially with DBP rise and finger pulse drop (ps < .05 and .02, respectively), mainly without central nervous system arousal. The DBP remained constant in normotensive professional drivers older than 40. The drivers' cardiovascular responses to glare were inversely related to reported stressors and subjective experience. Anxiety trait and long work hours were associated with heightened central arousal to glare in professional drivers. The results suggest that there may be progressive degrees of sensitization to glare exposure in these samples, with the least among normotensive professional drivers older than 40, moderate levels in borderline hypertensives, and the most severe in drivers with IHD.

  17. Type IA supernova spectroscopy analysis of Sloan Digital Sky Survey II - Supernova Survey

    NASA Astrophysics Data System (ADS)

    Zheng, Chen

    2009-06-01

    Supernovae (SNe) have played an important role in the recent dramatic development of observational cosmology. They possess homogeneous observable properties, and thus approximate "standard candles", allowing them to be precise, luminosity distance indicators. Over the last decade, the observed sample of supernovae (SNe) has increased by more than an order of magnitude. Further advances will no longer be limited by statistical errors, but rather by the control of systematic uncertainties, associated with source diversity and evolution. Over 500 SNe Ia have been discovered by the Sloan Digital Sky Survey (SDSS) -- II SN Survey during the three fall seasons from 2005 to 2007. We combine spectroscopic and photometric data to explore reducing these systematic errors. One challenge is to remove accurately the host galaxy light from the observed spectra. We have developed an effective host-subtraction tool using a composite color-constrained PCA+template-fitting program. We have applied this technique to more than 700 spectra from SNe with redshifts up to 0.4 obtained from the SDSS-II SN Survey and more than 200 spectra from low-z SNe at redshifts less than 0.01 obtained from the Center for Astrophysics (CfA) SN archive. We have also developed an automatic method to quantify spectral features of SNe Ia and applied it to the CfA and SDSS-II samples. By comparing the time series of the spectral features between these two samples, we have found no sign of cosmological evolution. We have, however, found evidence for luminosity-dependent differences in the Mg II 4300, Si II 4000, Si II 5800, and Si II 6150 lines. This should be useful for cosmological studies.

  18. Catalina Sky Survey II, a Next-Generation Survey with Small Binocular Telescopes

    NASA Astrophysics Data System (ADS)

    Larson, Stephen M.; Beshore, E. C.

    2010-10-01

    The Congress has directed NASA to develop a Near-Earth Object (NEO) survey program to detect, track, catalog, and characterize NEOs ≥ 140 meters in diameter by 2020. We are studying one possible approach, the Catalina Sky Survey II (CSS-II), a dedicated, low-cost, rapid-response, advanced survey that could be quickly deployed. CSS-II will dovetail with the planned capabilities of LSST and Pan-STARRS (PS), and add important new capabilities for NEO characterization and follow up that other surveys will not have. At the core of our proposal is three Small Binocular Telescopes (SBTs) using existing mirrors from the former Multiple Mirror Telescope. Working individually from a single observing site, each SBT will have the light grasp of a 2.4-meter telescope. Working together, they will be equivalent to a single telescope with a 4.2-meter mirror. Our approach has many advantages, including economy, 100 percent commitment to NEO search, low risk relative to other approaches, the ability to provide characterization of threatening objects, scalability, and the addition of significant new search capacity. The characterization potential of the mixed-use survey programs of LSST and PS will be valuable, but limited. Determining impact energy is vital to mitigation strategies. Impact energy follows from mass and velocity. Velocity is obtained from the orbital solution, but mass requires size and composition. Both size (through albedo) and composition can be significantly constrained with low-resolution spectroscopy covering the region from 0.35 to 2.4 microns. Shapes and rotation rates can best be obtained through time-series studies during close approaches. We will describe some preliminary designs for the CSS-II, the flexibility afforded by its multiple, independently-targeted mount design, freedom to adopt new observing strategies, and the potential for generating valuable science through a systematic spectrographic study of the asteroid population as part of its search

  19. NEWLY IDENTIFIED EXTENDED GREEN OBJECTS (EGOs) FROM THE SPITZER GLIMPSE II SURVEY. II. MOLECULAR CLOUD ENVIRONMENTS

    SciTech Connect

    Chen Xi; Gan Conggui; Shen Zhiqiang; Ellingsen, Simon P.; Titmarsh, Anita; He Jinhua

    2013-06-01

    We have undertaken a survey of molecular lines in the 3 mm band toward 57 young stellar objects using the Australia Telescope National Facility Mopra 22 m radio telescope. The target sources were young stellar objects with active outflows (extended green objects (EGOs)) newly identified from the GLIMPSE II survey. We observe a high detection rate (50%) of broad line wing emission in the HNC and CS thermal lines, which combined with the high detection rate of class I methanol masers toward these sources (reported in Paper I) further demonstrates that the GLIMPSE II EGOs are associated with outflows. The physical and kinematic characteristics derived from the 3 mm molecular lines for these newly identified EGOs are consistent with these sources being massive young stellar objects with ongoing outflow activity and rapid accretion. These findings support our previous investigations of the mid-infrared properties of these sources and their association with other star formation tracers (e.g., infrared dark clouds, methanol masers and millimeter dust sources) presented in Paper I. The high detection rate (64%) of the hot core tracer CH{sub 3}CN reveals that the majority of these new EGOs have evolved to the hot molecular core stage. Comparison of the observed molecular column densities with predictions from hot core chemistry models reveals that the newly identified EGOs from the GLIMPSE II survey are members of the youngest hot core population, with an evolutionary time scale of the order of 10{sup 3} yr.

  20. ColorChecker at the beach: dangers of sunburn and glare

    NASA Astrophysics Data System (ADS)

    McCann, John

    2014-01-01

    In High-Dynamic-Range (HDR) imaging, optical veiling glare sets the limits of accurate scene information recorded by a camera. But, what happens at the beach? Here we have a Low-Dynamic-Range (LDR) scene with maximal glare. Can we calibrate a camera at the beach and not be burnt? We know that we need sunscreen and sunglasses, but what about our cameras? The effect of veiling glare is scene-dependent. When we compare RAW camera digits with spotmeter measurements we find significant differences. As well, these differences vary, depending on where we aim the camera. When we calibrate our camera at the beach we get data that is valid for only that part of that scene. Camera veiling glare is an issue in LDR scenes in uniform illumination with a shaded lens.

  1. The accuracy of drivers' judgments of the effects of headlight glare on their own visual acuity.

    PubMed

    Stafford Sewall, Ashley A; Whetsel Borzendowski, Stephanie A; Tyrrell, Richard A

    2014-01-01

    Drivers' judgments of the magnitude of disability glare caused by high-beam headlights may not match actual declines in visual performance. This study investigated younger and older drivers' beliefs about their own visual performance in the presence of headlight glare. Eleven older drivers and seventeen younger drivers judged the distance at which they would just be able to recognize the orientation of a white Landolt C if it were present adjacent to the headlamps of a stationary opposing vehicle at night. The younger participants were generally accurate in their estimates of the recognition distance of the stimulus, while older participants significantly overestimated both their own acuity and the effect of glare on their vision. From this study, we see that older drivers' judgments about the disabling effects of oncoming headlights may be systematically inaccurate. These misperceptions about headlight glare may help explain why drivers tend to underuse high beams.

  2. Spatial Mapping of Macular Pigment Optical Density and Its Relationship to Contrast Sensitivity and Glare Disability

    NASA Astrophysics Data System (ADS)

    Putnam, Christopher

    This dissertation explored the relationship of the macular pigment optical density (MPOD) spatial profile with measures of contrast sensitivity (CS), glare disability (GD), relative glare disability (RGD) and intraocular light scatter. A novel device capable of measuring MPOD across the central 160 of retina along 8 principle meridians using customized heterochromatic flicker photometry (cHFP) at eccentricities of 00, 20, 40, 60 and 80 was built. MPOD was calculated as both discrete and integrated values at all measured retinal loci. CS was measured using vertical grating stimuli of 3, 6 and 9 cycles per degree (cpd) also presented at 00, 20, 4 0, 60 and 80 eccentricity. GD was calculated as a difference in CS between glare and no glare conditions (CSNo Glare - CSGlare) using the same vertical grating stimuli presented at the same eccentricities. RGD [(CSNo Glare - CSGlare) / CSNo Glare] was calculated to isolate the glare attenuation effects of MPOD by controlling for CS variability among the subject sample. Intraocular scatter was assessed through a direct compensation method using a commercially available device. Statistical analyses of the discrete and integrated MPOD associations with CS, GD, RGD and intraocular scatter were evaluated. The cHFP identified reliable MPOD spatial distribution maps demonstrating a 1 st order exponential decay curve as a function of increasing eccentricity. Foveal MPOD revealed the highest correlation coefficients with RGD using 9cpd stimuli. These results are consistent with the glare attenuation effects of MP at higher spatial frequencies. Further support may be seen from the significant correlations found between corresponding parafoveal MPOD measures and both GD and RGD at 20 and 40 of eccentricity using 9cpd stimuli with greater MPOD being associated with less glare disability. All calculated measures of foveal MPOD shared similar significant correlation coefficients with both GD and RGD using 6cpd and 9cpd stimuli. Discrete

  3. The Sloan Digital Sky Survey-II Supernova Survey: Technical Summary

    SciTech Connect

    Frieman, Joshua A.; Bassett, Bruce; Becker, Andrew; Choi, Changsu; Cinabro, David; DeJongh, Don Frederic; Depoy, Darren L.; Doi, Mamoru; Garnavich, Peter M.; Hogan, Craig J.; Holtzman, Jon; Im, Myungshin; Jha, Saurabh; Konishi, Kohki; Lampeitl, Hubert; Marriner, John; Marshall, Jennifer L.; McGinnis, David; Miknaitis, Gajus; Nichol, Robert C.; Prieto, Jose Luis; /Ohio State U. /Rochester Inst. Tech. /Stanford U., Phys. Dept. /Pennsylvania U. /Penn State U., Astron. Astrophys. /Portsmouth U. /Tokyo U. /Tokyo U. /South African Astron. Observ. /Tokyo U. /Stanford U., Phys. Dept. /Fermilab /Fermilab /Ohio State U. /Stanford U., Phys. Dept. /Fermilab /Bristol U. /Apache Point Observ. /Liverpool John Moores U., ARI /Columbia U., CBA /Apache Point Observ. /Ohio State U. /Durham U. /Portsmouth U. /South African Astron. Observ. /Naval Academy, Annapolis /UC, Berkeley /UC, Berkeley /Ohio State U. /Stockholm U. /New Mexico State U. /Princeton U. Observ. /Tokyo U. /Washington U., Seattle, Astron. Dept. /Stanford U., Phys. Dept. /Jefferson Lab /Apache Point Observ. /Gottingen U. /Chicago U. /San Francisco State U. /DARK Cosmology Ctr. /Fermilab /Apache Point Observ. /Durham U. /Princeton U. Observ. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ. /Barcelona U. /Stockholm U. /Apache Point Observ. /Lick Observ. /Sussex U. /Barcelona U. /Apache Point Observ. /Ohio State U. /Apache Point Observ. /Fermilab /DARK Cosmology Ctr. /Chicago U. /Fermilab /South African Astron. Observ. /Ohio State U. /Apache Point Observ. /Texas U., McDonald Observ. /Fermilab

    2007-09-14

    The Sloan Digital Sky Survey-II (SDSS-II) has embarked on a multi-year project to identify and measure light curves for intermediate-redshift (0.05 < z < 0.35) Type Ia supernovae (SNe Ia) using repeated five-band (ugriz) imaging over an area of 300 sq. deg. The survey region is a stripe 2.5 degrees wide centered on the celestial equator in the Southern Galactic Cap that has been imaged numerous times in earlier years, enabling construction of a deep reference image for discovery of new objects. Supernova imaging observations are being acquired between 1 September and 30 November of 2005-7. During the first two seasons, each region was imaged on average every five nights. Spectroscopic follow-up observations to determine supernova type and redshift are carried out on a large number of telescopes. In its first two three-month seasons, the survey has discovered and measured light curves for 327 spectroscopically confirmed SNe Ia, 30 probable SNe Ia, 14 confirmed SNe Ib/c, 32 confirmed SNe II, plus a large number of photometrically identified SNe Ia, 94 of which have host-galaxy spectra taken so far. This paper provides an overview of the project and briefly describes the observations completed during the first two seasons of operation.

  4. Evaluation of Anti-Glare Applications for a Tactical Helmet-Mounted Display

    DTIC Science & Technology

    2012-03-01

    simulated sunlight condition. 15. SUBJECT TERMS Helmet-Mounted Display, HMD, Glare, Anti-Reflective, Hood 16. SECURITY CLASSIFICATION OF: 17...legibility with each film and HMD hood covering under normal office lighting and under a simulated sunlight condition. In this test paradigm, participants had...impediment in the form of glare as sunlight is reflected into the user’s eye. Since operators can be expected to perform their missions at any time of

  5. The dark side of photovoltaic — 3D simulation of glare assessing risk and discomfort

    SciTech Connect

    Rose, Thomas; Wollert, Alexander

    2015-04-15

    Photovoltaic (PV) systems form an important force in the implementation of renewable energies, but as we all know, the force has always its dark side. Besides efficiency considerations and discussions about architectures of power distribution networks, the increasing numbers of installations of PV systems for implementing renewable energies have secondary effects. PV systems can generate glare due to optical reflections and hence might be a serious concern. On the one hand, glare could affect safety, e.g. regarding traffic. On the other hand, glare is a constant source of discomfort in vicinities of PV systems. Hence, assessment of glare is decisive for the success of renewable energies near municipalities and traffic zones for the success of solar power. Several courts decided on the change of PV systems and even on their de-installation because of glare effects. Thus, location-based assessments are required to limit potential reflections and to avoid risks for public infrastructure or discomfort of residents. The question arises on how to calculate reflections accurately according to the environment's topography. Our approach is founded in a 3D-based simulation methodology to calculate and visualize reflections based on the geometry of the environment of PV systems. This computational model is implemented by an interactive tool for simulation and visualization. Hence, project planners receive flexible assistance for adjusting the parameters of solar panels amid the planning process and in particular before the installation of a PV system. - Highlights: • Solar panels cause glare that impacts neighborhoods and traffic infrastructures. • Glare might cause disability and discomfort. • 3D environment for the calculation of glare • Interactive tool to simulate and visualize reflections • Impact assessment of solar power plant farms.

  6. Night Vision Performance in Detection and Identification of Moving Targets after Glare

    DTIC Science & Technology

    1979-07-01

    provided by the Institute. We are grateful to Noah Phyllis Levin , M.A., who provided adminis- trative and secretarial services essential to the conduct of...NIGHT VISION PERFORMANCE IN DETECTION AND IDENTIFICATION OF MOVING TARGETS AFTER GLARE Final Report July 1979 Anthony J. Adams , Ph.D. Gunilla...surprise, since our previous work (Brown, 1972; Adams et a], 1976) revealed significant velocity effects for resolution of ramp targets without glare. Brown

  7. Development of a Headlight Glare Simulator for a Driving Simulator

    PubMed Central

    Hwang, Alex D.; Peli, Eli

    2012-01-01

    We describe the design and construction of a headlight glare simulator to be used with a driving simulator. The system combines a modified programmable off–the-shelf LED display board and a beamsplitter so that the LED lights, representing the headlights of oncoming cars, are superimposed over the driving simulator headlights image. Ideal spatial arrangement of optical components to avoid misalignments of the superimposed images is hard to achieve in practice and variations inevitably introduce some parallax. Furthermore, the driver’s viewing position varies with driver’s height and seating position preferences exacerbate such misalignment. We reduce the parallax errors using an intuitive calibration procedure (simple drag-and-drop alignment of nine LED positions with calibration dots on the screen). To simulate the dynamics of headlight brightness changes when two vehicles are approaching, LED intensity control algorithms based on both headlight and LED beam shapes were developed. The simulation errors were estimated and compared to real-world headlight brightness variability. PMID:24443633

  8. Second Epoch VLBA Calibrator Survey Observations - VCS-II

    NASA Technical Reports Server (NTRS)

    Gordon, David; Jacobs, Christopher; Beasley, Anthony; Peck, Alison; Gaume, Ralph; Charlot, Patrick; Fey, Alan; Ma, Chopo; Titov, Oleg; Boboltz, David

    2016-01-01

    Six very successful VLBA calibrator survey campaigns were run between 1994 and 2007 to build up a large list of compact radio sources with positions precise enough for use as VLBI phase reference calibrators. We report on the results of a second epoch VLBA Calibrator Survey campaign (VCS-II) in which 2400 VCS sources were re-observed at X and S bands in order to improve the upcoming third realization of the International Celestial Reference Frame (ICRF3) as well as to improve their usefulness as VLBI phase reference calibrators. In this survey, some 2062 previously detected sources and 324 previously undetected sources were detected and revised positions are presented. Average position uncertainties for the reobserved sources were reduced from 1.14 and 1.98 mas to 0.24 and 0.41 mas in RA and Declination, respectively, or by nearly a factor of 5. Minimum detected flux values were approximately 15 and 28 mJy in X and S bands, respectively, and median total fluxes are approximately 230 and 280 mJy. The vast majority of these sources are flat-spectrum sources, with approximately 82% having spectral indices greater than -0.5.

  9. A portable inspection system to estimate direct glare of various LED modules

    NASA Astrophysics Data System (ADS)

    Chen, Po-Li; Liao, Chun-Hsiang; Li, Hung-Chung; Jou, Shyh-Jye; Chen, Han-Ting; Lin, Yu-Hsin; Tang, Yu-Hsiang; Peng, Wei-Jei; Kuo, Hui-Jean; Sun, Pei-Li; Lee, Tsung-Xian

    2015-07-01

    Glare is caused by both direct and indirect light sources and discomfort glare produces visual discomfort, annoyance, or loss in visual performance and visibility. Direct glare is caused by light sources in the field of view whereas reflected glare is caused by bright reflections from polished or glossy surfaces that are reflected toward an individual. To improve visual comfort of our living environment, a portable inspection system to estimate direct glare of various commercial LED modules with the range of color temperature from 3100 K to 5300 K was developed in this study. The system utilized HDR images to obtain the illumination distribution of LED modules and was first calibrated for brightness and chromaticity and corrected with flat field, dark-corner and curvature by the installed algorithm. The index of direct glare was then automatically estimated after image capturing, and the operator can recognize the performance of LED modules and the possible effects on human being once the index was out of expecting range. In the future, we expect that the quick-response smart inspection system can be applied in several new fields and market, such as home energy diagnostics, environmental lighting and UGR monitoring and popularize it in several new fields.

  10. The sloan digital sky Survey-II supernova survey: search algorithm and follow-up observations

    SciTech Connect

    Sako, Masao; Bassett, Bruce; Becker, Andrew; Hogan, Craig J.; Cinabro, David; DeJongh, Fritz; Frieman, Joshua A.; Marriner, John; Miknaitis, Gajus; Depoy, D. L.; Prieto, Jose Luis; Dilday, Ben; Kessler, Richard; Doi, Mamoru; Garnavich, Peter M.; Holtzman, Jon; Jha, Saurabh; Konishi, Kohki; Lampeitl, Hubert; Nichol, Robert C.; and others

    2008-01-01

    The Sloan Digital Sky Survey-II Supernova Survey has identified a large number of new transient sources in a 300 deg{sup 2} region along the celestial equator during its first two seasons of a three-season campaign. Multi-band (ugriz) light curves were measured for most of the sources, which include solar system objects, galactic variable stars, active galactic nuclei, supernovae (SNe), and other astronomical transients. The imaging survey is augmented by an extensive spectroscopic follow-up program to identify SNe, measure their redshifts, and study the physical conditions of the explosions and their environment through spectroscopic diagnostics. During the survey, light curves are rapidly evaluated to provide an initial photometric type of the SNe, and a selected sample of sources are targeted for spectroscopic observations. In the first two seasons, 476 sources were selected for spectroscopic observations, of which 403 were identified as SNe. For the type Ia SNe, the main driver for the survey, our photometric typing and targeting efficiency is 90%. Only 6% of the photometric SN Ia candidates were spectroscopically classified as non-SN Ia instead, and the remaining 4% resulted in low signal-to-noise, unclassified spectra. This paper describes the search algorithm and the software, and the real-time processing of the SDSS imaging data. We also present the details of the supernova candidate selection procedures and strategies for follow-up spectroscopic and imaging observations of the discovered sources.

  11. Psychophysical investigations of discomfort and disability glare from underground coal mine illumination systems. Open File Report, May 1980-July 1983

    SciTech Connect

    Whitehead, K.L.; Lindahl, P.; Vincent, R.; Crouch, C.

    1983-10-01

    A literature search was conducted to identify current light-control technology and hardware that may be applicable on underground lighting systems to minimize disability and discomfort glare. No research dealing specifically with mine lighting was found, but abstracts on research considered potentially applicable are included in the report. Information on several commercial light-control products for use in controlling glare are also included. Vision tests conducted on 137 mine personnel to determine their discomfort and disability glare sensitivity indicate their sensitivity to disability glare is about the same as the general population.

  12. Effect of Direct Glare on Orbicularis Oculi and Trapezius During Computer Reading.

    PubMed

    Mork, Randi; Bruenech, Jan Richard; Thorud, Hanne Mari Schiøtz

    2016-07-01

    Unfavorable visual conditions during computer work may affect development of both eyestrain and musculoskeletal pain in the neck and shoulder area. The aim of the study was to investigate how direct glare affects symptom development, muscle activity, and muscle blood flow in m. orbicularis oculi and m. trapezius during reading on a computer screen. Fifteen healthy young adults with normal binocular vision read text on a computer screen at an optimized computer workplace, 30 minutes with glare exposure and 30 minutes with appropriate lighting. Postural angles were continuously registered. Development of eye symptoms and musculoskeletal pain in the neck and shoulder area were recorded using VAS scales. Muscle activity and muscle blood flow were measured continuously using electromyography and photoplethysmography, respectively. Glare exposure resulted in significantly more pronounced eye pain, increased orbicularis muscle activity, and increased trapezius blood flow compared to reading with appropriate lighting. There were no significant differences in posture between the two light conditions. There were also significant associations between orbicularis oculi activity and both trapezius blood flow and neck pain during both conditions. Results from the current study show that direct glare conditions cause increased eyestrain and orbicularis oculi contraction during reading on a computer screen. This study also indicates that exposure to direct glare affects the trapezius muscle, possibly by an interaction between the visual system, sympathetic nervous system, and head-stabilizing muscles. In addition, there were associations between the use of orbicularis oculi, trapezius blood flow, and development of neck pain independent of the lighting.

  13. Large area glare sources and their effect on discomfort and visual performance at computer workstations

    SciTech Connect

    Osterhaus, W.K.E.; Bailey, I.L.

    1992-05-01

    This paper studies the effects of a large area light source of variable but uniform luminance surrounding a video display terminal (VDT) on the perceived glare discomfort and visual performance of computer operators. A set of criteria was established for rating the discomfort from glare as either ``intolerable,`` ``disturbing,`` ``noticeable,`` or ``imperceptible``. Source luminance adjustments by means of a variable transformer to match the subjective glare criteria, as well as ratings of preselected lighting conditions on a visual analog scale with the same criteria, were used to determine comfortable lighting conditions. Results from the experiment indicate that subjects reliably selected a preferred lighting condition at any time when asked to adjust the luminance to produce optimum visual comfort. There was considerable between-subject variation in the range of luminances over which the surround field was neither noticeably too dim nor noticeably too bright. Comfortable luminance ranges also varied with initial presentation luminances immediately preceding the adjustment. Subjects preferred higher luminances following high initial presentation luminances. Performance speed at a difficult letter-counting task suggests that visual performance was slightly impaired by the presence of glare discomfort. Counting errors also occurred slightly more frequently under higher surround source luminances. There was a tendency for subjects to become more susceptible to glare over the course of the experiment.

  14. The Data Release of the Sloan Digital Sky Survey-II Supernova Survey

    SciTech Connect

    Sako, Masao; et al.

    2014-01-14

    This paper describes the data release of the Sloan Digital Sky Survey-II (SDSS-II) Supernova Survey conducted between 2005 and 2007. Light curves, spectra, classifications, and ancillary data are presented for 10,258 variable and transient sources discovered through repeat ugriz imaging of SDSS Stripe 82, a 300 deg2 area along the celestial equator. This data release is comprised of all transient sources brighter than r~22.5 mag with no history of variability prior to 2004. Dedicated spectroscopic observations were performed on a subset of 889 transients, as well as spectra for thousands of transient host galaxies using the SDSS-III BOSS spectrographs. Photometric classifications are provided for the candidates with good multi-color light curves that were not observed spectroscopically. From these observations, 4607 transients are either spectroscopically confirmed, or likely to be, supernovae, making this the largest sample of supernova candidates ever compiled. We present a new method for SN host-galaxy identification and derive host-galaxy properties including stellar masses, star-formation rates, and the average stellar population ages from our SDSS multi-band photometry. We derive SALT2 distance moduli for a total of 1443 SN Ia with spectroscopic redshifts as well as photometric redshifts for a further 677 purely-photometric SN Ia candidates. Using the spectroscopically confirmed subset of the three-year SDSS-II SN Ia sample and assuming a flat Lambda-CDM cosmology, we determine Omega_M = 0.315 +/- 0.093 (statistical error only) and detect a non-zero cosmological constant at 5.7 sigmas.

  15. The method of estimation of background luminance in objective glare measurements

    NASA Astrophysics Data System (ADS)

    Blaszczak, Urszula J.

    2004-08-01

    Human eye is able to change its sensitivity to light in the process of adaptation. Still the process of vision can be accompanied by inconvenient phenomena, e.g. glare. The newest European norms recommended the CIE Unified Glare Rating method to estimate glare. A condition of practical realization of this method is the knowledge of the luminance distribution in the room. The best detection method is to use a CCD camera, which allows to evaluate all the quantities needed to calculate the UGR index: the background luminance, the luminance of the luminous parts of each luminaire at the observer's eye, the solid angle of the luminous parts of each luminaire and the position index for each luminaire. In the paper a definition of the background luminance Lb and the influence of the errors in Lb estimation on the value of the UGR index are presented. Two methods of the background luminance measurement are described and discussed.

  16. Design and demonstration of high efficiency anti-glare LED luminaires for indoor lighting.

    PubMed

    Chiang, Che-Wen; Hsu, Yu-Kai; Pan, Jui-Wen

    2015-02-09

    An anti-glare luminaire design is proposed to reduce the effect of glare and the multi-shadow while preserving high optical efficiency, high illumination uniformity and low unified glare rating (UGR). Comparison to the traditional direct light emitting diode (LED) luminaire in optical simulations showed an enhancement of the illumination uniformity from 64.9% to 80.0%. The optical efficiency was 79.5%, and the UGR value was controlled under 18.8. For the actual measurement, the finished product had an illumination uniformity of 77.0%, optical efficiency of 76.0%, UGR value of 19.0, and efficacy of 81.4 lm/w. Through this design, the lighting performance was greatly enhanced.

  17. Visual stimuli are common triggers of migraine and are associated with pattern glare.

    PubMed

    Harle, Deacon E; Shepherd, Alex J; Evans, Bruce J W

    2006-10-01

    To investigate the associations between interictal pattern glare, visual stress, and visual triggers of migraine. There has been relatively little research on the visual stimuli that can trigger migraine episodes. This is surprising, since if practitioners can obviate such triggers, then some attacks may be prevented. The existing literature suggests that patients who are prone to visually triggered migraines report more illusions on viewing striped patterns ("pattern glare") and that colored filters may be an effective intervention for these people. Headache symptoms and headache triggers were investigated in migraine and control groups in 2 separate experiments. In one experiment, we also determined, for each participant, pattern glare, whether it was reduced by colored filters and, if so, what the optimum color of filter was. Color vision was also assessed with the D15 test. People with migraine saw significantly more illusions on viewing each striped pattern and experienced greater pattern glare. They were also more likely to select a colored filter to aid visual comfort, particularly colors in the blue-to-green sector of the spectrum. Color vision was impaired subtly but significantly in migraine. Principal component analyses grouped common headache triggers into 5 broadly equal components: food, visual triggers, alcohol, stress and tiredness, and the environment. In a second analysis, the overall number of illusions seen in striped patterns was associated with visual triggers while pattern glare, use of colored filters, and interictal light sensitivity together formed a sixth component interpreted as visual stress. It is suggested that clinicians should ask migraine patients whether visual stimuli trigger their migraine, about interictal visual symptoms, and use the pattern glare test to ensure that those who may benefit from optometric interventions are appropriately managed.

  18. Mobile computing device configured to compute irradiance, glint, and glare of the sun

    DOEpatents

    Gupta, Vipin P; Ho, Clifford K; Khalsa, Siri Sahib

    2014-03-11

    Described herein are technologies pertaining to computing the solar irradiance distribution on a surface of a receiver in a concentrating solar power system or glint/glare emitted from a reflective entity. A mobile computing device includes at least one camera that captures images of the Sun and the entity of interest, wherein the images have pluralities of pixels having respective pluralities of intensity values. Based upon the intensity values of the pixels in the respective images, the solar irradiance distribution on the surface of the entity or glint/glare corresponding to the entity is computed by the mobile computing device.

  19. Corneal tattooing to reduce glare in cases of traumatic iris loss.

    PubMed

    Reed, J W

    1994-09-01

    The traumatic loss of iris is often associated with symptoms of glare, which can be debilitating. This symptom may be benefitted by wearing a contact lens with a clear, central optical zone and opacification of the remainder. The patient who is contact lens-intolerant may be helped by tattooing of all of the cornea except the central visual axis. Four patients who had traumatic iris loss and who were treated by this technique reported reduced glare as well as improvement in the cosmetic appearance of the eye. Although corneal tattooing is an ancient procedure, it continues to be of benefit for selected patients.

  20. The extended ROSAT-ESO flux limited X-ray galaxy cluster survey (REFLEX II) II. Construction and properties of the survey

    NASA Astrophysics Data System (ADS)

    Böhringer, H.; Chon, G.; Collins, C. A.; Guzzo, L.; Nowak, N.; Bobrovskyi, S.

    2013-07-01

    Context. Galaxy clusters provide unique laboratories to study astrophysical processes on large scales and are important probes for cosmology. X-ray observations are currently the best means of detecting and characterizing galaxy clusters. Therefore X-ray surveys for galaxy clusters are one of the best ways to obtain a statistical census of the galaxy cluster population. Aims: In this paper we describe the construction of the REFLEX II galaxy cluster survey based on the southern part of the ROSAT All-Sky Survey. REFLEX II extends the REFLEX I survey by a factor of about two down to a flux limit of 1.8 × 10-12 erg s cm (0.1-2.4 keV). Methods: We describe the determination of the X-ray parameters, the process of X-ray source identification, and the construction of the survey selection function. Results: The REFLEX II cluster sample comprises currently 915 objects. A standard selection function is derived for a lower source count limit of 20 photons in addition to the flux limit. The median redshift of the sample is z = 0.102. Internal consistency checks and the comparison to several other galaxy cluster surveys imply that REFLEX II is better than 90% complete with a contamination less than 10%. Conclusions: With this publication we give a comprehensive statistical description of the REFLEX II survey and provide all the complementary information necessary for a proper modeling of the survey for astrophysical and cosmological applications. Based on observations at the European Southern Observatory La Silla, ChileFull Tables 2 and 3 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/555/A30

  1. Drivers' judgments of the effect of headlight glare on their ability to see pedestrians at night.

    PubMed

    Whetsel Borzendowski, Stephanie A; Stafford Sewall, Ashley A; Rosopa, Patrick J; Tyrrell, Richard A

    2015-06-01

    Several studies have concluded that pedestrians typically overestimate their own conspicuity to approaching drivers at night. The present experiments extended this research by exploring the accuracy of drivers' judgments of pedestrian conspicuity while facing varying degrees of headlight glare. In Experiment 1, participants on an open road estimated their ability to see a roadside pedestrian in each of two clothing configurations and with each of three different glare intensities present. In Experiment 2, participants responded to a roadside pedestrian under the same open road conditions; the participants were naïve with regard to both the position of the pedestrian and to the clothing and glare manipulations. Consistent with earlier research, estimates of response distance were, on the average, over three times greater than actual recognition distance. The extent to which participants overestimated conspicuity was greater when the pedestrian wore a retroreflective vest, and participants incorrectly judged that headlight glare would not degrade drivers' ability to see a pedestrian wearing a retroreflective vest. These results confirm that road users' understanding of issues involving drivers' night vision is limited. These misunderstandings may result in road users behaving in ways that increase the risk of nighttime collisions with pedestrians. Copyright © 2015 Elsevier Ltd. All rights reserved.

  2. GLARE: a Domain-Independent System for Acquiring, Representing and Executing Clinical Guidelines

    PubMed Central

    Molino, Gianpaolo; Terenziani, Paolo; Montani, Stefania; Bottrighi, Alessio; Torchio, Mauro

    2006-01-01

    We briefly describe GLARE, a domain-independent system to acquire, represent and execute clinical guidelines, which as been developed since 1997 in a joint cooperation between Computer Sciences Departments and Az. Ospedaliera S.Giovanni Battista in Turin, one of the largest hospitals in Italy. A demo of the (prototypical) system is also available. PMID:17238656

  3. Test track evaluation of headlight glare associated with adaptive curve HID, fixed HID, and fixed halogen low beam headlights.

    PubMed

    Reagan, Ian J; Frischmann, Tim; Brumbelow, Matthew L

    2016-12-01

    Adaptive curve headlights swivel with steering input and are linked to reduced insurance claims and improved visual performance. This study assessed glare experienced from adaptive curve high-intensity discharge (HID), fixed (non-swiveling) HID and fixed halogen headlights - all tested in low beam mode. Twenty participants rated glare from vehicles' headlights using the DeBoer visual discomfort scale as a test driver drove towards them from five approaches on a test track. Participants rated the fixed halogen condition as less glaring than the adaptive curve and fixed HID conditions. There was no significant difference in ratings between the HID low-beam conditions. Collapsing across roadway approaches, the mean subjective ratings for the fixed halogen, adaptive curve HID and fixed HID low-beam conditions indicated 'satisfactory' levels of glare. Differences between subjective ratings were supported by illuminance data. Differences among the three low-beam systems appear minor, relative to their differences from a benchmark high-beam condition. Practitioner Summary: Insurance data indicates reduced claims associated with adaptive curve lighting. The current effort was to study how such lighting affects discomfort glare of oncoming drivers relative to conventional headlights. Participants rated halogen headlights as less glaring than fixed and adaptive curve HID low beams. Differences among systems were small and associated with acceptable levels of discomfort glare.

  4. Burrell-Optical-Kepler Survey (BOKS) II: Early Variability Results

    NASA Astrophysics Data System (ADS)

    Howell, Steve B.; Feldmeier, J.; von Braun, K.; Everett, M.; Mihos, C.; Harding, P.; Knox, C.; Sherry, W.; Lee, T.; Ciardi, D.; Rudick, C.; Proctor, M.; van Belle, G.

    2006-12-01

    We present preliminary results for the photometric time-series data obtained with the BOKS survey (see BOKS I poster Feldmeier et al.). The BOKS survey covers about 1 square degree in the constellation of Cygnus. We obtained nearly 2000 SDSS r-band images spanning a total time period of 39 days. Each point source in our BOKS survey is also present in the single epoch, 7-color photometric survey catalogue being produced by the NASA Discovery program Kepler mission. Light curves of approximately 60,000 point sources, spanning r=14 to 20, are examined and discussed. We will present variability demographics for the BOKS survey including characterization of the light curves into variable classes based on type, color, amplitude, and any extra-solar planet transit candidates.

  5. Sloan Digital Sky Survey II (SDSS-II), Data Release 6, including Extension for Galactic Understanding and Exploration (SEGUE)

    DOE Data Explorer

    Yanny, Brian; Rockosi, Constance; Newberg, Heidi Jo; Knapp, Gillian R.

    The Sloan Digital Sky Survey (see www.sdss.org for general information) will map one-quarter of the entire sky and perform a redshift survey of galaxies, quasars and stars. The DR6 is the sixth major data release and provides images, imaging catalogs, spectra, and redshifts for download. It is the first data release of SDSS-II, an extension of the original SDSS consisting of three subprojects: Legacy, SEGUE and a Supernova survey. Be sure to check out the separate page for SEGUE also at http://classic.sdss.org/dr6/start/aboutsegue.html.

  6. A Survey of Fertilizer Dealers: II. Sources of Agronomic Information.

    ERIC Educational Resources Information Center

    Schmitt, M. A.

    1988-01-01

    Reports on a survey of fertilizer dealers that was conducted to assess how the dealers were obtaining their agronomic information, aside from formal training sessions, and determine if these sources of information were satisfactory in fulfilling the dealers' needs. (TW)

  7. A Survey of Fertilizer Dealers: II. Sources of Agronomic Information.

    ERIC Educational Resources Information Center

    Schmitt, M. A.

    1988-01-01

    Reports on a survey of fertilizer dealers that was conducted to assess how the dealers were obtaining their agronomic information, aside from formal training sessions, and determine if these sources of information were satisfactory in fulfilling the dealers' needs. (TW)

  8. The China Mental Health Survey: II. Design and field procedures.

    PubMed

    Liu, Zhaorui; Huang, Yueqin; Lv, Ping; Zhang, Tingting; Wang, Hong; Li, Qiang; Yan, Jie; Yu, Yaqin; Kou, Changgui; Xu, Xiufeng; Lu, Jin; Wang, Zhizhong; Qiu, Hongyan; Xu, Yifeng; He, Yanling; Li, Tao; Guo, Wanjun; Tian, Hongjun; Xu, Guangming; Xu, Xiangdong; Ma, Yanjuan; Wang, Linhong; Wang, Limin; Yan, Yongping; Wang, Bo; Xiao, Shuiyuan; Zhou, Liang; Li, Lingjiang; Tan, Liwen; Chen, Hongguang; Ma, Chao

    2016-11-01

    China Mental Health Survey (CMHS), which was carried out from July 2013 to March 2015, was the first national representative community survey of mental disorders and mental health services in China using computer-assisted personal interview (CAPI). Face-to-face interviews were finished in the homes of respondents who were selected from a nationally representative multi-stage disproportionate stratified sampling procedure. Sample selection was integrated with the National Chronic Disease and Risk Factor Surveillance Survey administered by the National Centre for Chronic and Non-communicable Disease Control and Prevention in 2013, which made it possible to obtain both physical and mental health information of Chinese community population. One-stage design of data collection was used in the CMHS to obtain the information of mental disorders, including mood disorders, anxiety disorders, and substance use disorders, while two-stage design was applied for schizophrenia and other psychotic disorders, and dementia. A total of 28,140 respondents finished the survey with 72.9% of the overall response rate. This paper describes the survey mode, fieldwork organization, procedures, and the sample design and weighting of the CMHS. Detailed information is presented on the establishment of a new payment scheme for interviewers, results of the quality control in both stages, and evaluations to the weighting.

  9. SKA weak lensing- II. Simulated performance and survey design considerations

    NASA Astrophysics Data System (ADS)

    Bonaldi, Anna; Harrison, Ian; Camera, Stefano; Brown, Michael L.

    2016-12-01

    We construct a pipeline for simulating weak lensing cosmology surveys with the Square Kilometre Array (SKA), taking as inputs telescope sensitivity curves; correlated source flux, size and redshift distributions; a simple ionospheric model; source redshift and ellipticity measurement errors. We then use this simulation pipeline to optimize a 2-yr weak lensing survey performed with the first deployment of the SKA (SKA1). Our assessments are based on the total signal to noise of the recovered shear power spectra, a metric that we find to correlate very well with a standard dark energy figure of merit. We first consider the choice of frequency band, trading off increases in number counts at lower frequencies against poorer resolution; our analysis strongly prefers the higher frequency Band 2 (950-1760 MHz) channel of the SKA-MID telescope to the lower frequency Band 1 (350-1050 MHz). Best results would be obtained by allowing the centre of Band 2 to shift towards lower frequency, around 1.1 GHz. We then move on to consider survey size, finding that an area of 5000 deg2 is optimal for most SKA1 instrumental configurations. Finally, we forecast the performance of a weak lensing survey with the second deployment of the SKA. The increased survey size (3π steradian) and sensitivity improves both the signal to noise and the dark energy metrics by two orders of magnitude.

  10. The REFLEX II galaxy cluster survey: power spectrum analysis

    NASA Astrophysics Data System (ADS)

    Balaguera-Antolínez, A.; Sánchez, Ariel G.; Böhringer, H.; Collins, C.; Guzzo, L.; Phleps, S.

    2011-05-01

    We present the power spectrum of galaxy clusters measured from the new ROSAT-ESO Flux-Limited X-Ray (REFLEX II) galaxy cluster catalogue. This new sample extends the flux limit of the original REFLEX catalogue to 1.8 × 10-12 erg s-1 cm-2, yielding a total of 911 clusters with ≥94 per cent completeness in redshift follow-up. The analysis of the data is improved by creating a set of 100 REFLEX II-catalogue-like mock galaxy cluster catalogues built from a suite of large-volume Λ cold dark matter (ΛCDM) N-body simulations (L-BASICC II). The measured power spectrum is in agreement with the predictions from a ΛCDM cosmological model. The measurements show the expected increase in the amplitude of the power spectrum with increasing X-ray luminosity. On large scales, we show that the shape of the measured power spectrum is compatible with a scale-independent bias and provide a model for the amplitude that allows us to connect our measurements with a cosmological model. By implementing a luminosity-dependent power-spectrum estimator, we observe that the power spectrum measured from the REFLEX II sample is weakly affected by flux-selection effects. The shape of the measured power spectrum is compatible with a featureless power spectrum on scales k > 0.01 h Mpc-1 and hence no statistically significant signal of baryonic acoustic oscillations can be detected. We show that the measured REFLEX II power spectrum displays signatures of non-linear evolution.

  11. GlaRe, a GIS tool to reconstruct the 3D surface of palaeoglaciers

    NASA Astrophysics Data System (ADS)

    Pellitero, Ramón; Rea, Brice R.; Spagnolo, Matteo; Bakke, Jostein; Ivy-Ochs, Susan; Frew, Craig R.; Hughes, Philip; Ribolini, Adriano; Lukas, Sven; Renssen, Hans

    2016-09-01

    Glacier reconstructions are widely used in palaeoclimatic studies and this paper presents a new semi-automated method for generating glacier reconstructions: GlaRe, is a toolbox coded in Python and operating in ArcGIS. This toolbox provides tools to generate the ice thickness from the bed topography along a palaeoglacier flowline applying the standard flow law for ice, and generates the 3D surface of the palaeoglacier using multiple interpolation methods. The toolbox performance has been evaluated using two extant glaciers, an icefield and a cirque/valley glacier from which the subglacial topography is known, using the basic reconstruction routine in GlaRe. Results in terms of ice surface, ice extent and equilibrium line altitude show excellent agreement that confirms the robustness of this procedure in the reconstruction of palaeoglaciers from glacial landforms such as frontal moraines.

  12. Anthropometric Survey (ANSUR) II Pilot Study: Methods and Summary Statistics

    DTIC Science & Technology

    2009-04-01

    SIZES( DIMENSIONS ) ARMY NATIONAL GUARD COMPARISON MEASUREMENTS WHOLE BODY SCAN ANTHROPOMETRIC MEASUREMENT TOOL INFORMATION RETRIEVAL...1 1.1 SELECTION OF SURVEY DIMENSIONS ........................................................................ 3 1.2 THE SAMPLE...to what extent, this epidemic has influenced body dimensions in the Army —active duty, National Guard, or Reserves. The A2P consisted of 3462

  13. MMT HYPERVELOCITY STAR SURVEY. II. FIVE NEW UNBOUND STARS

    SciTech Connect

    Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J. E-mail: mgeller@cfa.harvard.edu

    2012-05-20

    We present the discovery of five new unbound hypervelocity stars (HVSs) in the outer Milky Way halo. Using a conservative estimate of Galactic escape velocity, our targeted spectroscopic survey has now identified 16 unbound HVSs as well as a comparable number of HVSs ejected on bound trajectories. A Galactic center origin for the HVSs is supported by their unbound velocities, the observed number of unbound stars, their stellar nature, their ejection time distribution, and their Galactic latitude and longitude distribution. Other proposed origins for the unbound HVSs, such as runaway ejections from the disk or dwarf galaxy tidal debris, cannot be reconciled with the observations. An intriguing result is the spatial anisotropy of HVSs on the sky, which possibly reflects an anisotropic potential in the central 10-100 pc region of the Galaxy. Further progress requires measurement of the spatial distribution of HVSs over the southern sky. Our survey also identifies seven B supergiants associated with known star-forming galaxies; the absence of B supergiants elsewhere in the survey implies there are no new star-forming galaxies in our survey footprint to a depth of 1-2 Mpc.

  14. Ontario University Benefits Survey. Part II (Pensions). December 1, 1979.

    ERIC Educational Resources Information Center

    University of Western Ontario, London.

    Results of a survey of pension plans in Ontario universities are summarized according to type of plan, eligibility, member and university contributions, and benefits. Benefits for normal retirment, early retirement, termination, and death are presented. Death benefits are outlined for before retirement, after retirement, and by model pension…

  15. Delphi Survey: A Report of Rounds I and II.

    ERIC Educational Resources Information Center

    Reynolds, Maynard C.

    This DELPHI survey, undertaken as a part of the Council for Exceptional Children project on professional standards and guidelines, was intended to provide input to the project staff, feedback to the respondents, and information to all interested persons in the field on trends and issues in the field of special education. The query domains included…

  16. Comparison of glare in YAG-damaged intraocular lenses: injection-molded versus lathe-cut.

    PubMed

    Bath, P E; Dang, Y; Martin, W H

    1986-11-01

    A comparative analysis of YAG laser intraocular lens (IOL) damage was undertaken on injection-molded and lathe-cut IOLs. Damage sites were evaluated with polarized light. A consistent positive polarization was observed in the damage sites of lathe-cut IOLs. A consistent negative polarization was observed in the damage sites of injection-molded IOLs. The presence of positive polarization in IOL damage sites may be correlated with increased potential for glare. Results and clinical implications are discussed.

  17. Delays in Laser Glare Onset Differentially Affect Target-Location Performance in a Visual Search Task.

    DTIC Science & Technology

    1991-06-01

    incandescent central glare, lens opacity (Interzeag, Opacity Lensmeter), and color sensitivity (Farnsworth- Munsell 100- Hue Test , Kollmorgen Corp...Baltimore, MD). PROCEDURES Subjects were tested separately. Each subject sat in the cockpit-familiarization trainer in a completely darkened room for the...accuracy of target-location responses. All post-hoc pairwise comparisons among means were carried out using Tukey’s HSD test at the 0.05 probability level

  18. Supporting physicians in taking decisions in clinical guidelines: the GLARE "what if" facility.

    PubMed

    Terenziani, Paolo; Montani, Stefania; Bottrighi, Alesio; Torchio, Mauro; Molino, Gianpaolo

    2002-01-01

    GLARE (GuideLine Acquisition, Representation and Execution) is a domain-independent system for the acquisition, representation and execution of clinical guidelines. GLARE is unique in its approach to supporting the decision-making process of users/physicians faced with various alternatives in the guidelines. In many cases, the best alternative cannot be determined on the basis of "local information" alone (i.e., by considering just the selection criteria associated with the decision at hand), but must also take into account information stemming from relevant alternative pathways. Exploitation of "global information" available in the various pathways is made possible by GLARE through the "what if" facility, a form of hypothetical reasoning which allows users to gather relevant decision parameters (e.g., costs, resources, times) from selected parts of the guideline in a semi-automatic fashion. In particular, the extremely complex task of coping with temporal information involves the extension and adaptation of various techniques developed by the Artificial Intelligence (AI) community.

  19. Field Surveys, IOC Valleys. Volume II, Part II. Biological Resources Survey, Pine and Wah Wah Valleys, Utah.

    DTIC Science & Technology

    1981-08-01

    contained two or more species of cactus on each site. Grasses included Aristida purpurea, Bromus tectorum, Hilaria jamesii, Oryzopsis hymen - oides, and...TR-48-II-Il 260 tolerances to salinity: Atriplex canescens and Atriplex hymen - elytra can survive very high salinity conditions; Ambrosia dumosa

  20. Characterising our Universe with the REFLEX II cluster survey

    NASA Astrophysics Data System (ADS)

    Chon, G.; Boehringer, H.

    2014-07-01

    Galaxy clusters are important cosmological probes and they are in particular useful to constrain the parameters for the matter density and the density fluctuation amplitude in the Universe. The currently largest uncertainties in using galaxy clusters for cosmological tests originate in our imperfect knowledge of scaling relations between cluster observables and the masses of galaxy clusters. Using well defined statistical samples constructed from our REFLEX and NORAS survey of X-ray luminous clusters in the ROSAT All-Sky Survey, we aim for a comprehensive characterization of the statistical properties of the structure of galaxy clusters in the nearby Universe. We will discuss scaling relations, morphological distributions and the effect of the enviroment on these properties. For the first time we compare such results for flux- and volume-limted samples of galaxy clusters.

  1. The M33 Synoptic Stellar Survey. II. Mira Variables

    NASA Astrophysics Data System (ADS)

    Yuan, Wenlong; He, Shiyuan; Macri, Lucas M.; Long, James; Huang, Jianhua Z.

    2017-04-01

    We present the discovery of 1847 Mira candidates in the Local Group galaxy M33 using a novel semi-parametric periodogram technique coupled with a random forest classifier. The algorithms were applied to ∼2.4 × 105 I-band light curves previously obtained by the M33 Synoptic Stellar Survey. We derive preliminary period–luminosity relations at optical, near-infrared, and mid-infrared wavelengths and compare them to the corresponding relations in the Large Magellanic Cloud.

  2. VizieR Online Data Catalog: Newly EGOs from GLIMPSE II survey. II. MoC (Chen+, 2013)

    NASA Astrophysics Data System (ADS)

    Chen, X.; Gan, C.-G.; Ellingsen, S. P.; He, J.-H.; Shen, Z.-Q.; Titmarsh, A.

    2013-10-01

    A survey for molecular lines in the 3mm band toward ~60% of the GLIMPSE II EGO catalog (Paper I, Cat. J/ApJS/206/9) was performed with the Australia Telescope National Facility (ATNF) Mopra 22m radio telescope in 2009 august 9-20. Fifty-five sites, which include fifty-seven of the GLIMPSE II EGOs were observed in the survey (the two EGO-pairs G352.52+0.76(a)/G352.52+0.76(b) and G358.46-0.39(a)/G358.46-0.39(b) were covered simultaneously within a single Mopra observation). (11 data files).

  3. A Type II Supernova Hubble Diagram from the CSP-I, SDSS-II, and SNLS Surveys

    NASA Astrophysics Data System (ADS)

    de Jaeger, T.; González-Gaitán, S.; Hamuy, M.; Galbany, L.; Anderson, J. P.; Phillips, M. M.; Stritzinger, M. D.; Carlberg, R. G.; Sullivan, M.; Gutiérrez, C. P.; Hook, I. M.; Howell, D. Andrew; Hsiao, E. Y.; Kuncarayakti, H.; Ruhlmann-Kleider, V.; Folatelli, G.; Pritchet, C.; Basa, S.

    2017-02-01

    The coming era of large photometric wide-field surveys will increase the detection rate of supernovae by orders of magnitude. Such numbers will restrict spectroscopic follow-up in the vast majority of cases, and hence new methods based solely on photometric data must be developed. Here, we construct a complete Hubble diagram of Type II supernovae (SNe II) combining data from three different samples: the Carnegie Supernova Project-I, the Sloan Digital Sky Survey II SN, and the Supernova Legacy Survey. Applying the Photometric Color Method (PCM) to 73 SNe II with a redshift range of 0.01–0.5 and with no spectral information, we derive an intrinsic dispersion of 0.35 mag. A comparison with the Standard Candle Method (SCM) using 61 SNe II is also performed and an intrinsic dispersion in the Hubble diagram of 0.27 mag, i.e., 13% in distance uncertainties, is derived. Due to the lack of good statistics at higher redshifts for both methods, only weak constraints on the cosmological parameters are obtained. However, assuming a flat universe and using the PCM, we derive the universe’s matter density: {{{Ω }}}m={0.32}-0.21+0.30 providing a new independent evidence for dark energy at the level of two sigma. This paper includes data gathered with the 6.5 m Magellan Telescopes, with the du Pont and Swope telescopes located at Las Campanas Observatory, Chile; and the Gemini Observatory, Cerro Pachon, Chile (Gemini Program N-2005A-Q-11, GN-2005B-Q-7, GN-2006A-Q-7, GS-2005A-Q-11, GS-2005B-Q-6, and GS-2008B-Q-56). Based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere, Chile (ESO Programmes 076.A-0156,078.D-0048, 080.A-0516, and 082.A-0526).

  4. A new method of glare protection on highway real-time monitoring during nighttime

    NASA Astrophysics Data System (ADS)

    Xu, Jin; Chen, Zhebo; Ni, Xuxiang; Lu, Zukang

    2007-01-01

    When car run in highway during night, need switch on its headlight, for intensity of the light is very high, it will cause glare vision, the camera of monitoring system will be saturation, and all the other detail (For example: License plate) can't be shown on the screen except headlight and its glare. In this paper, introduce a new system and method of glare protection on highway nighttime monitoring, it can decrease the intensity of headlight and the glare vision in real-time, so the monitoring system could gain more details of highway from camera. The whole system's hardware is made up of outer camera-lens, inner camera-lens, spatial light modulator array and image sensor. The outer camera-lens images the objects (cars on highway) on the plane of the spatial light modulator array's panel. So, the spatial light modulator array can modulate part of the image on its panel, such as decrease or increase transmission ratio (or reflect ratio). The inner camera-lens images the spatial light modulator array's panel to the image sensor. So, the image on the image sensor is the image of object image after modulated. After the image sensor gained the image, we will use our software to analyze the image, use real-time processing to get the saturation and glared region. Firstly, we use threshold arithmetic to get the saturation and high intensive pixels of the image; secondly, we use filter to get ride of the noise made from threshold arithmetic, so we can get the region of saturation and glare region of the original image; thirdly, we do expand arithmetic at the direction of car's moving, and feedback the image to spatial light modulator. If we don't use expand arithmetic at the direction of car's moving, and feedback the image gained after step 2, for the car in highway is moving very fast, after the time of image processing, the car has moved to a new location with it's direction, so the feedback image will not decrease the light intensity of the car's headlight and it

  5. U.S. Air Force Turbine Engine Emission Survey. Volume II. Individual Engine Test Reports.

    DTIC Science & Technology

    1978-08-01

    1» I MI HU III.I11M1,|IHIIPH|I»^^—»^ II 111.11 l|. I I | mi | . I I. I.,.L ENGINE J85 -5 17 ^ ^_._. rr •Wl...AD-AÜbl 665 UNCLASSIFIED SCOTT ENVIRONMENTAL TECHNOLOGY INC PLUMSTEAOVILLE PA F/G 21/5 U.S. AIR FORCE TURBINE ENGINE EMISSION SURVEY...i run’ LEVEL CEEDOTR-7834 U.S. AIR FORCE TURBINE ENGINE EMISSION SURVEY VOL II INDIVIDUAL ENGINE TEST REPORTS v o-< 3 „ fi-^\\^92 ANTHONY F

  6. The Core Collapse Supernova Rate from the SDSS-II Supernova Survey

    SciTech Connect

    Taylor, Matt; Cinabro, David; Dilday, Ben; Galbany, Lluis; Gupta, Ravi R.; Kessler, R.; Marriner, John; Nichol, Robert C.; Richmond, Michael; Schneider, Donald P.; Sollerman, Jesper

    2014-08-26

    We use the Sloan Digital Sky Survey II Supernova Survey (SDSS-II SNS) data to measure the volumetric core collapse supernova (CCSN) rate in the redshift range (0.03 < z < 0.09). Using a sample of 89 CCSN, we find a volume-averaged rate of 1.06 ± 0.19 × 10(–)(4)((h/0.7)(3)/(yr Mpc(3))) at a mean redshift of 0.072 ± 0.009. We measure the CCSN luminosity function from the data and consider the implications on the star formation history.

  7. The core collapse supernova rate from the SDSS-II supernova survey

    SciTech Connect

    Taylor, Matt; Cinabro, David; Dilday, Ben; Galbany, Lluis; Gupta, Ravi R.; Kessler, R.; Marriner, John; Nichol, Robert C.; Richmond, Michael; Schneider, Donald P.; Sollerman, Jesper

    2014-09-10

    We use the Sloan Digital Sky Survey II Supernova Survey (SDSS-II SNS) data to measure the volumetric core collapse supernova (CCSN) rate in the redshift range (0.03 < z < 0.09). Using a sample of 89 CCSN, we find a volume-averaged rate of 1.06 ± 0.19 × 10{sup –4}((h/0.7){sup 3}/(yr Mpc{sup 3})) at a mean redshift of 0.072 ± 0.009. We measure the CCSN luminosity function from the data and consider the implications on the star formation history.

  8. The Chandra Fornax Survey. II. The Source Catalog

    NASA Astrophysics Data System (ADS)

    Williamson, Karen; Zurek, D.; Scharf, C.

    2010-01-01

    The Fornax cluster of galaxies lies in the southern hemisphere and is second only to the richer and more well-studied Virgo cluster in its accessibility for high resolution multi-wavelength data collection. A deep \\emph{Chandra} survey of the inner one degree of this cluster was performed in 2003, with first results published in 2005 identifying 771 X-ray point sources. We present a catalog of these X-ray point sources. Possible and likely optical candidates were identified from ground-based, HST and GALEX images. This catalog will facilitate future investigations by enhancing our understanding of a cluster's fainter and smaller objects, calibrating distance rulers, and constraining cosmological models. This work was conducted by a Research Experience for Undergraduates (REU) position at the American Museum of Natural History and funded by the NSF.

  9. A Combined MG II/CA II Survey of Stellar Magnetic Activity in the Solar Neighborhood

    NASA Technical Reports Server (NTRS)

    Wicklund, B. M.; Donahue, R. A.; Dobson, A. K.; Baliunas, Sallie L.

    1997-01-01

    We use nearly contemporaneus low-resolution IUE observations of Mg II h + k emission and Mount Wilson Observatory Ca II H + K S indices for 33 pairs of observations of lower main sequence stars to formulate a relationship that will permit accurate predictions of S values as a function of (B - V) color and Mg II h + k flux. The resulting relationship is useful because it will extend the set of solar neighborhood stars for which a uniform estimate of chromospheric activity is available to include stars that are not observable from Mount Wilson as well as providing additional estimates of activity levels for stars that are on the Mount Wilson HK Project observing list.

  10. Hα kinematics of the Spitzer Infrared Nearby Galaxies Survey - II

    NASA Astrophysics Data System (ADS)

    Dicaire, I.; Carignan, C.; Amram, P.; Hernandez, O.; Chemin, L.; Daigle, O.; de Denus-Baillargeon, M.-M.; Balkowski, C.; Boselli, A.; Fathi, K.; Kennicutt, R. C.

    2008-04-01

    This is the second part of an Hα kinematics follow-up survey of the Spitzer Infrared Nearby Galaxies Survey (SINGS) sample. The aim of this paper is to shed new light on the role of baryons and their kinematics and on the dark/luminous matter relation in the star-forming regions of galaxies, in relation with studies at other wavelengths. The data for 37 galaxies are presented. The observations were made using Fabry-Perot interferometry with the photon-counting camera FaNTOmM on four different telescopes, namely the Canada-France-Hawaii 3.6-m, the ESO La Silla 3.6-m, the William Herschel 4.2-m and the Observatoire du mont Mégantic 1.6-m telescopes. The velocity fields are computed using custom IDL routines designed for an optimal use of the data. The kinematical parameters and rotation curves are derived using the GIPSY software. It is shown that non-circular motions associated with galactic bars affect the kinematical parameters fitting and the velocity gradient of the rotation curves. This leads to incorrect determinations of the baryonic and dark matter distributions in the mass models derived from those rotation curves. Based on observations made with the ESO 3.60-m telescope at La Silla Observatories under programme ID 076.B-0859 and on observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France and the University of Hawaii. E-mail: isabelle@astro.umontreal.ca (ID);claude.carignan@umontreal.ca (CC) ‡ Visiting Astronomer, Canada-France-Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France and the University of Hawaii.

  11. The Green Bank Telescope Galactic H II Region Discovery Survey

    NASA Astrophysics Data System (ADS)

    Bania, Thomas M.; Anderson, L. D.; Balser, D. S.; Rood, R. T.

    2010-05-01

    We discovered a large population of previously unknown Galactic HII regions by using the NRAO Green Bank Telescope to detect hydrogen radio recombination line (RRL) emission from these nebulae. Since recombination lines are optically thin at 3 cm wavelength, we can detect HII regions across the entire Galactic disk. Our targets were selected based on spatially coincident 24µm (Spitzer/MIPSGAL) and 21 cm (either from the VLA Galactic Plane Survey or the NRAO NVSS) continuum emission. For the Galactic zone, -16° < Lgal < 67° and |Bgal|<1°, we detected 602 discrete RRL components from 95% of the sample targets, which more than doubles the number of known HII regions in this part of the Milky Way. We found 25 new first quadrant nebulae with negative RRL velocities, placing them beyond the Solar orbit in the Perseus arm. We plan to determine the distance to over 90% of our sources (for the region Lgal>18°) by using HI emission/absorption experiments to resolve the kinematic distance ambiguity. Because we can detect all nebulae inside the Solar orbit that are ionized by O-stars, the Discovery Survey targets, when combined with existing HII region catalogs, will give a more accurate census of Galactic HII regions and their properties. The distribution of HII regions across the Galactic disk shows strong, narrow ( 1 kpc wide) peaks at Galactic radii of 4.3 and 6.0 kpc. There is still an overall dearth of HII regions within 4 kpc radius. For the first time the longitude-velocity distribution of HII regions gives unambiguous evidence for Galactic structure, including the kinematic signatures of the radial peaks in the spatial distribution, a concentration of nebulae at the end of the Galactic Bar, and nebulae located in kinematic locus of the 3 kpc Arm.

  12. VizieR Online Data Catalog: REFLEX II. Properties of the survey (Boehringer+ 2013)

    NASA Astrophysics Data System (ADS)

    Boehringer, H.; Chon, G.; Collins, C. A.; Guzzo, L.; Nowak, N.; Bobrovskyi, S.

    2013-06-01

    Like REFLEX I, the extended survey covers the southern sky outside the band of the Milky Way (|bII|>=20°) with regions around the Magellanic clouds excised (3 in LMC, 3 in SMC). The total survey area after this excision amounts to 4.24 steradian (or 13924°2) which corresponds to 33.75% of the sky. Different from REFLEX I, we use the refined RASS product RASS III (Voges et al. 1999, Cat. IX/10). (2 data files).

  13. Effects of planar and non-planar driver-side mirrors on age-related discomfort-glare responses

    PubMed Central

    Lockhart, Thurmon E.; Atsumi, Bunji; Ghosh, Arka; Mekaroonreung, Haruetai; Spaulding, Jeremy

    2010-01-01

    In this study, we evaluated subjective nighttime discomfort-glare responses on three different types of planar and non-planar driver-side mirrors on two age groups. Fifty-six individuals (28 young [18–35 years] and 28 old [65 years and over]) participated in this experiment. Subjective discomfort-glare rating scores on three different types of driver-side mirrors were assessed utilizing De Boer's rating scale in a controlled nighttime driving environment (laboratory ambient illuminant level—l lux with headlight turned off). Three driver-side mirrors included planar “flat mirror”: radius of curvature 242650.92 mm, reflectivity 0.60114, and surface reflectance 0.60568; “curved mirror”: radius of curvature 1433.3 mm, reflectivity 0.21652, and surface reflectance 0.58092; “blue mirror”: radius of curvature 1957.1 mm, reflectivity 0.25356, and surface reflectance 0.54585. The results indicated that with the same glare level (as measured by angle of incidence and illuminance in front of the eyes), older adults reported worse feelings of glare than their younger counterparts. Furthermore, the results indicated that both young and older adults reported worse feelings of glare for planar driver-side mirror than non-planar driver-side mirrors. These results suggest that older adults' criterion of discomfort-glare is more sensitive than their younger counterparts, and importantly, the non-planar driver-side mirrors can be beneficial in terms of reducing nighttime discomfort-glare for both the young and the elderly. PMID:20582252

  14. Effects of planar and non-planar driver-side mirrors on age-related discomfort-glare responses.

    PubMed

    Lockhart, Thurmon E; Atsumi, Bunji; Ghosh, Arka; Mekaroonreung, Haruetai; Spaulding, Jeremy

    2006-03-01

    In this study, we evaluated subjective nighttime discomfort-glare responses on three different types of planar and non-planar driver-side mirrors on two age groups. Fifty-six individuals (28 young [18-35 years] and 28 old [65 years and over]) participated in this experiment. Subjective discomfort-glare rating scores on three different types of driver-side mirrors were assessed utilizing De Boer's rating scale in a controlled nighttime driving environment (laboratory ambient illuminant level-l lux with headlight turned off). Three driver-side mirrors included planar "flat mirror": radius of curvature 242650.92 mm, reflectivity 0.60114, and surface reflectance 0.60568; "curved mirror": radius of curvature 1433.3 mm, reflectivity 0.21652, and surface reflectance 0.58092; "blue mirror": radius of curvature 1957.1 mm, reflectivity 0.25356, and surface reflectance 0.54585. The results indicated that with the same glare level (as measured by angle of incidence and illuminance in front of the eyes), older adults reported worse feelings of glare than their younger counterparts. Furthermore, the results indicated that both young and older adults reported worse feelings of glare for planar driver-side mirror than non-planar driver-side mirrors. These results suggest that older adults' criterion of discomfort-glare is more sensitive than their younger counterparts, and importantly, the non-planar driver-side mirrors can be beneficial in terms of reducing nighttime discomfort-glare for both the young and the elderly.

  15. A survey of recent EBR-II passive safety testing

    SciTech Connect

    Planchon, H.P.; Golden, G.H.; Sackett, J.I.; Singer, R.M.; Mohr, D.; Chang, L.K.; Feldman, E.E.; Sevy, R.H.

    1987-01-01

    During the last two years, the testing program at EBR-II has investigated the capabilities of liquid metal reactors (LMRs) to perform vital safety functions passively. In particular the tests have examined post shutdown decay heat removal by natural circulation and passive shutdown of the reactor after accidents which lead to undercooling. The undercooling accidents have been divided into two categories - the loss of flow without scram (LOFWS) (a family of events involving a loss of forced flow through the reactor), and the loss of heat sink without scram (LOHSWS) (a family of events involving a loss of the ability to transfer reactor heat to down stream components which generate steam and electricity.) The type of ''passive shutdown'' that has been examined is caused by natural processes - principally thermal expansion of the reactor structures, fuel and coolant. As used in this paper the term excludes automatic control of power, operator intervention or negative reactivity generated by special in-core devices. 18 refs., 7 figs., 1 tab.

  16. Seroepidemiologic studies in Oaxaca, Mexico. II. Survey for arbovirus antibody.

    PubMed

    Goldsmith, R S; Zarate, M L; Cedeño-Ferreira, J; Antonio Paz, E

    1979-01-01

    A serologic survey was conducted in south-western Mexico to obtain information on human experience with arbovirus infections. Sera were collected from two semitropical areas along the Pacific coast of Oaxaca State, two mountain areas above 1,700 meters and the interior valley at 1,500 meters. Of the 610 sera tested for group A antibody, 4.9 per cent were positive in the hemagglutination-inhibition (HI) test to Venezuelan (VE), 11 per cent to Eastern, and none to Western encephalitis viruses. In neutralization tests the antibody was shown to be probably due to VE virus infections. When sera were screened for group B antibodies in the HI test, 32 per cent were positive with St. Louis encephalitis (SLE), 19 per cent with Ilhéus, and 4 per cent with yellow fever viruses. The pattern of reactions suggested that SLE or an antigenically related virus was responsible for the antibody detected. An unusually high rate was found in a mountain area at 2,000 meters: 41 per cent of 113 persons tested were seropositive to SLE. Of 493 sera screened by complement-fixation test, 6 per cent were positive to Nepuyo, 4 per cent to Patois, and 3 per cent to Tlacotalpan viruses.

  17. THE CARNEGIE-IRVINE GALAXY SURVEY. II. ISOPHOTAL ANALYSIS

    SciTech Connect

    Li Zhaoyu; Ho, Luis C.; Barth, Aaron J.; Peng, Chien Y.

    2011-12-01

    The Carnegie-Irvine Galaxy Survey (CGS) is a comprehensive investigation of the physical properties of a complete, representative sample of 605 bright (B{sub T} {<=} 12.9 mag) galaxies in the southern hemisphere. This contribution describes the isophotal analysis of the broadband (BVRI) optical imaging component of the project. We pay close attention to sky subtraction, which is particularly challenging for some of the large galaxies in our sample. Extensive crosschecks with internal and external data confirm that our calibration and sky subtraction techniques are robust with respect to the quoted measurement uncertainties. We present a uniform catalog of one-dimensional radial profiles of surface brightness and geometric parameters, as well as integrated colors and color gradients. Composite profiles highlight the tremendous diversity of brightness distributions found in disk galaxies and their dependence on Hubble type. A significant fraction of S0 and spiral galaxies exhibit non-exponential profiles in their outer regions. We perform Fourier decomposition of the isophotes to quantify non-axisymmetric deviations in the light distribution. We use the geometric parameters, in conjunction with the amplitude and phase of the m = 2 Fourier mode, to identify bars and quantify their size and strength. Spiral arm strengths are characterized using the m = 2 Fourier profiles and structure maps. Finally, we utilize the information encoded in the m = 1 Fourier profiles to measure disk lopsidedness. The databases assembled here and in Paper I lay the foundation for forthcoming scientific applications of CGS.

  18. MX Siting Investigation. Mineral Resources Survey, Seven Additional Valleys, Nevada/Utah Siting Area. Volume II.

    DTIC Science & Technology

    1981-06-23

    AO-AI13 14𔃾 ERTEC WESTERN INC LONG BEACH CA F/6 7/4 MX SITING INVESTIGATION. MINERAL RESOURCES SURVEY, SEVEN ADDITI-ETC(U) JUN Al F04704-80-C-OGO6...DTIC-DDA-2 FORM DOCUMENT PROCESSING SHEET DTIC ocT :g 70A -- ~’ .9 ’I K ii I / "~1 - i~ / . . ..1’ ~ ~- .. ~ ~1 I E-TR-50 MINERAL RESOURCES SURVEY...144 ERTEC WESTERN INC. LONG BEACH CA F/6 7/4 MX SITING INVESTIGATION. MINERAL RESOURCES SURVEY. SEVEN AOOITI-ETCIU) JUN 81 FON7O-80-C-0006

  19. THE SURVEY OF LINES IN M31 (SLIM): INVESTIGATING THE ORIGINS OF [C II] EMISSION

    SciTech Connect

    Kapala, M. J.; Sandstrom, K.; Groves, B.; Kreckel, K.; Schinnerer, E.; Walter, F.; Fouesneau, M.; Croxall, K.; Dalcanton, J.; Leroy, A.

    2015-01-01

    The [C II] 158 μm line is one of the strongest emission lines observed in star-forming galaxies and has been empirically measured to correlate with the star-formation rate (SFR) globally and on kiloparsec scales. However, because of the multiphase origins of [C II], one might expect this relation to break down at small scales. We investigate the origins of [C II] emission by examining high spatial resolution observations of [C II] in M31 with the Survey of Lines in M31. We present five ∼700 × 700 pc (3' × 3') fields mapping the [C II] emission, Hα emission, and the ancillary infrared (IR) data. We spatially separate star-forming regions from diffuse gas and dust emission on ∼50 pc scales. We find that the [C II]-SFR correlation holds even at these scales, although the relation typically has a flatter slope than found at larger (kiloparsec) scales. While the Hα emission in M31 is concentrated in the SFR regions, we find that a significant amount (∼20%-90%) of the [C II] emission comes from outside star-forming regions and that the total IR emission (TIR) has the highest diffuse fraction of all SFR tracers. We find a weak correlation of the [C II]/TIR to dust color in each field and find a large-scale trend of increasing [C II]/TIR with galactocentric radius. The differences in the relative diffuse fractions of [C II], Hα, and IR tracers are likely caused by a combination of energetic photon leakage from H II regions and heating by the diffuse radiation field arising from older (B-star) stellar populations. However, we find that by averaging our measurements over kiloparsec scales, these effects are minimized, and the relation between [C II] and SFR found in other nearby galaxy studies is retrieved.

  20. Biennial Survey of Education, 1916-18. Volume II. Bulletin, 1919, No. 89

    ERIC Educational Resources Information Center

    Bureau of Education, Department of the Interior, 1921

    1921-01-01

    Volume II of the Biennial Survey of Education, 1916-1918 includes the following chapters: (1) Education in Great Britain and Ireland (I. L. Kandel); (2) Education in parts of the British Empire: Educational Developments in the Dominion of Canada (Walter A. Montgomery), Public School System of Jamaica (Charles A. Asbury), Recent Progress of…

  1. Ontario Universities Benefits Survey, 1991-92. Part I: Benefits Excluding Pensions [and] Part II: Pensions.

    ERIC Educational Resources Information Center

    Council of Senior Administrative Officers--Universities of Ontario, Toronto.

    This report, which combined Part I and Part II of a benefit study, presents data from a survey of Ontario universities concerning fringe benefits offered in 1991-92. Part I is made up of a series of tables displaying the information on particular benefits institution-by-institution. The first five tables cover general aspects of benefits,…

  2. Potential energy savings with exterior shades in large office buildings and the impact of discomfort glare

    SciTech Connect

    Hoffmann, Sabine; Lee, Eleanor

    2015-04-01

    Exterior shades are highly efficient for reducing solar load in commercial buildings. Their impact on net energy use depends on the annual energy balance of heating, cooling, fan and lighting energy. This paper discusses the overall energy use intensity of various external shading systems for a prototypical large office building split into the different types of energy use and for different orientations and window sizes. Lighting energy was calculated for a constant lighting power as well as for dimmed lighting fixtures (daylighting control). In Section 3, slat angles and solar cut-off angles were varied for fixed exterior slat shading systems. While the most light-blocking shades performed best for the case without daylighting controls, the optimum cut-off angle with daylighting controls was found to be 30 deg for the office building prototype used in Chicago and Houston. For large window-to-wall (WWR) ratios, window related annual energy use could be reduced by at least 70 % without daylighting control and by a minimum of 86 % with daylighting control in average over all orientations. The occurrence of discomfort glare was is considered in Section 4 of the paper, which looks at the performance of commercially available exterior shading systems when an interior shade is used in addition to the exterior shade during hours when occupants would experience discomfort glare. Glare control impacts overall energy use intensity significantly for exterior shades with high transmittance, especially when daylighting controls are used. In these cases, exterior shades are only beneficial for window-to-wall areas ≥ 45% in the hot Houston climate. For smaller windows and in a heating/cooling climate like Chicago, exterior shades can increase energy consumption

  3. Glare disability and spherical aberration with five foldable intraocular lenses: a prospective randomized study.

    PubMed

    Casprini, Fabrizio; Balestrazzi, Angelo; Tosi, Gian Marco; Miracco, Flavia; Martone, Gianluca; Cevenini, Gabriele; Caporossi, Aldo

    2005-02-01

    To compare differences in subjective glare and spherical aberration between five foldable intraocular lenses (IOLs) made of different materials and to different designs. This prospective study comprised 175 cataract patients who underwent phacoemulsification and were randomized to receive one of five types of foldable IOL (AcrySof MA30BA, Alcon; Sensar AR40, AMO; AcrySof SA30AL, Alcon; Sensar AR40e, AMO, and Tecnis Z9000, Pharmacia & Upjohn). All patients received a questionnaire investigating the incidence of subjective photic phenomena. Two months postoperatively, we collected data regarding subjective glare and evaluated pupil size, visual acuity and wavefront aberration of the cornea and eye. With regard to difficulty in performing ordinary activities under different light conditions and light and dark adaptation, the difference between the groups was not significant (p > 0.05, chi-squared test). With respect to difficulty in driving at night, the MA30BA group had a significant higher incidence of photic phenomena than the SA30AL, AR40e and Z9000 groups (p < 0.05, chi-squared test). Wavefront measurements revealed a significant difference between the Z9000, AR40e and SA30AL groups, which showed the lowest values, and the MA30BA group, which showed the highest value (p < 0.05, anova with Tamhane posthoc test). New generation IOLs such as the Pharmacia Z9000, AMO AR40e and AcrySof SA30AL have a lower incidence of glare and spherical aberrations; however, their impact on future IOL design should be conditioned by further data, especially regarding posterior capsule opacification.

  4. Evaluation of anti-glare applications for a tactical helmet-mounted display

    NASA Astrophysics Data System (ADS)

    Roll, Jason L.; Trew, Noel J. M.; Geis, Matthew R.; Havig, Paul R.

    2011-06-01

    Non see-through, monocular helmet mounted displays (HMDs) provide warfighters with unprecedented amounts of information at a glance. The US Air Force recognizes their usefulness, and has included such an HMD as part of a kit for ground-based, Battlefield Airmen. Despite their many advantages, non see-through HMDs occlude a large portion of the visual field when worn as designed, directly in front of the eye. To address this limitation, operators have chosen to wear it just above the cheek, angled up toward the eye. However, wearing the HMD in this position exposes the display to glare, causing a potential viewing problem. In order to address this problem, we tested several film and HMD hood applications for their effect on glare. The first experiment objectively examined the amount of light reflected off the display with each application in a controlled environment. The second experiment used human participants to subjectively evaluate display readability/legibility with each film and HMD hood covering under normal office lighting and under a simulated sunlight condition. In this test paradigm, participants had to correctly identify different icons on a map and different words on a white background. Our results indicate that though some applications do reduce glare, they do not significantly improve the HMD's readability/legibility compared with an uncovered screen. This suggests that these post-production modifications will not completely solve this problem and underscores the importance of employing a user-centered approach early in the design cycle to determine an operator's use-case before manufacturing an HMD for a particular user community.

  5. TYPE II CEPHEID CANDIDATES. IV. OBJECTS FROM THE NORTHERN SKY VARIABILITY SURVEY

    SciTech Connect

    Schmidt, Edward G.

    2013-09-15

    We have obtained VR photometry of 447 Cepheid variable star candidates with declinations north of -14 Degree-Sign 30', most of which were identified using the Northern Sky Variability Survey (NSVS) data archive. Periods and other photometric properties were derived from the combination of our data with the NSVS data. Atmospheric parameters were determined for 81 of these stars from low-resolution spectra. The identification of type II Cepheids based on the data presented in all four papers in this series is discussed. On the basis of spectra, 30 type II Cepheids were identified while 53 variables were identified as cool, main sequence stars and 283 as red giants following the definitions in Paper III. An additional 30 type II Cepheids were identified on the basis of light curves. The present classifications are compared with those from the Machine-learned All Sky Automated Survey Classification Catalog for 174 stars in common.

  6. VizieR Online Data Catalog: New EGOs from Spitzer GLIMPSE II survey. I. (Chen+, 2013)

    NASA Astrophysics Data System (ADS)

    Chen, X.; Gan, C.-G.; Ellingsen, S. P.; He, J.-H.; Shen, Z.-Q.; Titmarsh, A.

    2013-10-01

    We have adopted methods similar to those used by Cyganowski et al. (2008, Cat. J/AJ/136/2391) to compile a catalog of EGOs in the GLIMPSE II survey region. We displayed the archived GLIMPSE II Image Atlas mosaics (Version 3.5). We have constructed images in each of the IRAC bands (3.6, 4.5, 5.8, and 8.0um), as well as for the Spitzer Multiband Imaging Photometer (MIPS) 24um band (from the MIPS Galactic Plane Survey (MIPSGAL survey; Carey et al. 2009PASP..121...76C), and a three-color composite (3.6um-blue, 4.5um-green, and 8.0-m-red) for each of the 98 newly identified EGOs. To investigate the nature of the newly cataloged EGO sample from the GLIMPSE II survey region, we have performed a survey for molecular lines in the 3mm band toward ~60% of the sources with the ATNF Mopra 22m radio telescope. The Mopra observations consisted of a single pointing for each source and were undertaken in the period 2009 August 9-20. (5 data files).

  7. Design of asymmetric freeform lens for low glared LED street light with total internal reflection.

    PubMed

    Lai, Min-Feng; Chen, Yi-Chian; Anh, Nguyen Doan Quoc; Chen, Tsai-Yu; Ma, Hsin-Yi; Lee, Hsiao-Yi

    2016-01-25

    The study is focused on the asymmetric secondary freeform lens (ASFL) design for creating a low glared light-emitting diode (LED) street light. The lens is mounted on a chip on board (COB) LED as the new LED street light module to perform a non-axial symmetric light intensity distribution. The experimental results show that the street light can work without inclining lamps and reach Chinese National Standards (CNS) and Illuminating Engineering Society of North America (IESNA) standards at the same time.

  8. Flicker-glare and visual-comfort assessments of light emitting diode billboards.

    PubMed

    Lin, Meng-Wei; Hsieh, Pin-Hsuan; Chang, Erik C; Chen, Yi-Chun

    2014-08-01

    This study investigated the discomfort glare produced by the high-brightness LED billboards in relation to four factors: flicker frequency, panel luminance, viewing angular sub-tense, and ambient illuminance. The results showed that visual comfort is not affected by ambient illuminance but by the other three factors. Also, interaction was found between luminance and viewing angle. The experimental data were curve fitted to construct visual comfort models of LED billboard displays. By modulating the operating conditions, comfort display with LED billboards can be achieved.

  9. The Sloan Digital Sky Survey-II Supernova Survey:Search Algorithm and Follow-up Observations

    SciTech Connect

    Sako, Masao; Bassett, Bruce; Becker, Andrew; Cinabro, David; DeJongh, Don Frederic; Depoy, D.L.; Doi, Mamoru; Garnavich, Peter M.; Craig, Hogan, J.; Holtzman, Jon; Jha, Saurabh; Konishi, Kohki; Lampeitl, Hubert; Marriner, John; Miknaitis, Gajus; Nichol, Robert C.; Prieto, Jose Luis; Richmond, Michael W.; Schneider, Donald P.; Smith, Mathew; SubbaRao, Mark; /Chicago U. /Tokyo U. /Tokyo U. /South African Astron. Observ. /Tokyo U. /Apache Point Observ. /Seoul Natl. U. /Apache Point Observ. /Apache Point Observ. /Tokyo U. /Seoul Natl. U. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ.

    2007-09-14

    The Sloan Digital Sky Survey-II Supernova Survey has identified a large number of new transient sources in a 300 deg2 region along the celestial equator during its first two seasons of a three-season campaign. Multi-band (ugriz) light curves were measured for most of the sources, which include solar system objects, Galactic variable stars, active galactic nuclei, supernovae (SNe), and other astronomical transients. The imaging survey is augmented by an extensive spectroscopic follow-up program to identify SNe, measure their redshifts, and study the physical conditions of the explosions and their environment through spectroscopic diagnostics. During the survey, light curves are rapidly evaluated to provide an initial photometric type of the SNe, and a selected sample of sources are targeted for spectroscopic observations. In the first two seasons, 476 sources were selected for spectroscopic observations, of which 403 were identified as SNe. For the Type Ia SNe, the main driver for the Survey, our photometric typing and targeting efficiency is 90%. Only 6% of the photometric SN Ia candidates were spectroscopically classified as non-SN Ia instead, and the remaining 4% resulted in low signal-to-noise, unclassified spectra. This paper describes the search algorithm and the software, and the real-time processing of the SDSS imaging data. We also present the details of the supernova candidate selection procedures and strategies for follow-up spectroscopic and imaging observations of the discovered sources.

  10. PHOTOMETRY OF TYPE II CEPHEID CANDIDATES FROM THE NORTHERN PART OF THE ALL SKY AUTOMATED SURVEY

    SciTech Connect

    Schmidt, Edward G.; Hemen, Brian; Rogalla, Danielle; Thacker-Lynn, Lauren E-mail: bhemen1@bigred.unl.edu E-mail: lthacke1@bigred.unl.edu

    2009-06-15

    We have obtained VR photometry of 282 Cepheid variable star candidates from the northern part of the All Sky Automated Survey (ASAS). These together with data from the ASAS and the Northern Sky Variability Survey (NSVS) were used to redetermine the periods of the stars. We divided the stars into four groups based on location in a plot of mean color, (V-R), versus period. Two of the groups fell within the region of the diagram containing known type II Cepheids and yielded 14 new highly probable type II Cepheids. The properties of the remaining stars in these two groups are discussed but their nature remains uncertain. Unexplained differences exist between the sample of stars studied here and a previous sample drawn from the NSVS by Akerlof et al. This suggests serious biases in the identification of variables in different surveys.

  11. The WIRCam Deep Survey. II. Mass selected clustering

    NASA Astrophysics Data System (ADS)

    Bielby, R. M.; Gonzalez-Perez, V.; McCracken, H. J.; Ilbert, O.; Daddi, E.; Le Fèvre, O.; Hudelot, P.; Kneib, J.-P.; Mellier, Y.; Willott, C.

    2014-08-01

    We present an analysis of the clustering of galaxies from z ≈ 2 to the present day using the WIRCam Deep Survey (WIRDS). WIRDS combines deep optical data from the CFHTLS Deep fields with its own deep near-infrared data, providing a photometric data-set over an effective area of 2.4 deg2, from which accurate photometric redshifts and stellar masses can be estimated. We use the data to calculate the angular correlation function for galaxy samples split by star-formation activity, stellar mass and redshift. Using WIRDS with its large total area and multiple fields gives a low cosmic variance contribution to the error, which we estimate to be less than ~2.8%. Based on power-law fits, we estimate the real-space clustering for each sample, determining clustering lengths and power-law slopes. For galaxies selected by constant mass, we find that the clustering scale shows no evolution up to z ≈ 2. Splitting the galaxy sample by mass, we see a consistent trend for higher mass galaxies to have larger clustering scales at all redshifts considered. We use our results to test the galform semi-analytical model of galaxy formation and evolution. The observed trends are well matched by the model galaxies for both the redshift evolution and the mass dependence of the galaxy clustering. We split the galaxy population into passive and star-forming populations based on rest-frame dust-corrected NUV-r colours. We find that the passive galaxy populations show a significantly larger clustering scale at all redshifts than the star-forming population below masses of M⋆ ~ 1011 h-1 M⊙, showing that even at z ≈ 2 passive galaxies exist in denser environments than the bulk of the star-forming galaxy population. For star-forming galaxies with stellar masses of M⋆ ≳ 1011 h-1 M⊙, we find a clustering strength of ~8 h-1 Mpc across all redshifts, comparable to the measurements for the passive population. Additionally, for star-forming galaxies we see that clustering strength

  12. PHYSICAL AND MORPHOLOGICAL PROPERTIES OF [O II] EMITTING GALAXIES IN THE HETDEX PILOT SURVEY

    SciTech Connect

    Bridge, Joanna S.; Gronwall, Caryl; Ciardullo, Robin; Hagen, Alex; Zeimann, Greg; Malz, A. I.; Schneider, Donald P. E-mail: caryl@astro.psu.edu E-mail: hagen@psu.edu E-mail: aimalz@psu.edu; and others

    2015-02-01

    The Hobby-Eberly Dark Energy Experiment pilot survey identified 284 [O II] λ3727 emitting galaxies in a 169 arcmin{sup 2} field of sky in the redshift range 0 < z < 0.57. This line flux limited sample provides a bridge between studies in the local universe and higher-redshift [O II] surveys. We present an analysis of the star formation rates (SFRs) of these galaxies as a function of stellar mass as determined via spectral energy distribution fitting. The [O II] emitters fall on the ''main sequence'' of star-forming galaxies with SFR decreasing at lower masses and redshifts. However, the slope of our relation is flatter than that found for most other samples, a result of the metallicity dependence of the [O II] star formation rate indicator. The mass-specific SFR is higher for lower mass objects, supporting the idea that massive galaxies formed more quickly and efficiently than their lower mass counterparts. This is confirmed by the fact that the equivalent widths of the [O II] emission lines trend smaller with larger stellar mass. Examination of the morphologies of the [O II] emitters reveals that their star formation is not a result of mergers, and the galaxies' half-light radii do not indicate evolution of physical sizes.

  13. A very deep IRAS survey at l(II) = 97 deg, b(II) = +30 deg

    NASA Astrophysics Data System (ADS)

    Hacking, Perry; Houck, James R.

    1987-05-01

    A deep far-infrared survey is presented using over 1000 scans made of a 4 to 6 sq. deg. field at the north ecliptic pole by the IRAS. Point sources from this survey are up to 100 times fainter than the IRAS point source catalog at 12 and 25 micrometers, and up to 10 times fainter at 60 and 100 micrometers. The 12 and 25 micrometer maps are instrumental noise-limited, and the 60 and 100 micrometer maps are confusion noise-limited. The majority of the 12 micrometer point sources are stars within the Milky Way. The 25 micrometer sources are composed almost equally of stars and galaxies. About 80% of the 60 micrometer sources correspond to galaxies on Palomar Observatory Sky Survey (POSS) enlargements. The remaining 20% are probably galaxies below the POSS detection limit. The differential source counts are presented and compared with what is predicted by the Bahcall and Soneira Standard Galaxy Model using the B-V-12 micrometer colors of stars without circumstellar dust shells given by Waters, Cote and Aumann. The 60 micrometer source counts are inconsistent with those predicted for a uniformly distributed, nonevolving universe. The implications are briefly discussed.

  14. A very deep IRAS survey at l(II) = 97 deg, b(II) = +30 deg

    NASA Technical Reports Server (NTRS)

    Hacking, Perry; Houck, James R.

    1987-01-01

    A deep far-infrared survey is presented using over 1000 scans made of a 4 to 6 sq. deg. field at the north ecliptic pole by the IRAS. Point sources from this survey are up to 100 times fainter than the IRAS point source catalog at 12 and 25 micrometers, and up to 10 times fainter at 60 and 100 micrometers. The 12 and 25 micrometer maps are instrumental noise-limited, and the 60 and 100 micrometer maps are confusion noise-limited. The majority of the 12 micrometer point sources are stars within the Milky Way. The 25 micrometer sources are composed almost equally of stars and galaxies. About 80% of the 60 micrometer sources correspond to galaxies on Palomar Observatory Sky Survey (POSS) enlargements. The remaining 20% are probably galaxies below the POSS detection limit. The differential source counts are presented and compared with what is predicted by the Bahcall and Soneira Standard Galaxy Model using the B-V-12 micrometer colors of stars without circumstellar dust shells given by Waters, Cote and Aumann. The 60 micrometer source counts are inconsistent with those predicted for a uniformly distributed, nonevolving universe. The implications are briefly discussed.

  15. Photometric properties of intermediate-redshift Type Ia supernovae observed by the Sloan Digital Sky Survey-II Supernova Survey

    SciTech Connect

    Takanashi, N.; Doi, M.; Yasuda, N.; Kuncarayakti, H.; Konishi, K.; Schneider, D. P.; Cinabro, D.; Marriner, J.

    2016-12-06

    We have analyzed multi-band light curves of 328 intermediate redshift (0.05 <= z < 0.24) type Ia supernovae (SNe Ia) observed by the Sloan Digital Sky Survey-II Supernova Survey (SDSS-II SN Survey). The multi-band light curves were parameterized by using the Multi-band Stretch Method, which can simply parameterize light curve shapes and peak brightness without dust extinction models. We found that most of the SNe Ia which appeared in red host galaxies (u - r > 2.5) don't have a broad light curve width and the SNe Ia which appeared in blue host galaxies (u - r < 2.0) have a variety of light curve widths. The Kolmogorov-Smirnov test shows that the colour distribution of SNe Ia appeared in red / blue host galaxies is different (significance level of 99.9%). We also investigate the extinction law of host galaxy dust. As a result, we find the value of Rv derived from SNe Ia with medium light curve width is consistent with the standard Galactic value. On the other hand, the value of Rv derived from SNe Ia that appeared in red host galaxies becomes significantly smaller. Furthermore, these results indicate that there may be two types of SNe Ia with different intrinsic colours, and they are obscured by host galaxy dust with two different properties.

  16. Photometric properties of intermediate-redshift Type Ia supernovae observed by the Sloan Digital Sky Survey-II Supernova Survey

    DOE PAGES

    Takanashi, N.; Doi, M.; Yasuda, N.; ...

    2016-12-06

    We have analyzed multi-band light curves of 328 intermediate redshift (0.05 <= z < 0.24) type Ia supernovae (SNe Ia) observed by the Sloan Digital Sky Survey-II Supernova Survey (SDSS-II SN Survey). The multi-band light curves were parameterized by using the Multi-band Stretch Method, which can simply parameterize light curve shapes and peak brightness without dust extinction models. We found that most of the SNe Ia which appeared in red host galaxies (u - r > 2.5) don't have a broad light curve width and the SNe Ia which appeared in blue host galaxies (u - r < 2.0) havemore » a variety of light curve widths. The Kolmogorov-Smirnov test shows that the colour distribution of SNe Ia appeared in red / blue host galaxies is different (significance level of 99.9%). We also investigate the extinction law of host galaxy dust. As a result, we find the value of Rv derived from SNe Ia with medium light curve width is consistent with the standard Galactic value. On the other hand, the value of Rv derived from SNe Ia that appeared in red host galaxies becomes significantly smaller. Furthermore, these results indicate that there may be two types of SNe Ia with different intrinsic colours, and they are obscured by host galaxy dust with two different properties.« less

  17. A CLASS I AND CLASS II CH{sub 3}OH MASER SURVEY OF EGOs FROM THE GLIMPSE SURVEY

    SciTech Connect

    Cyganowski, C. J.; Churchwell, E.; Brogan, C. L.; Hunter, T. R.

    2009-09-10

    We present the results of a high angular resolution Very Large Array (VLA) Class I 44 GHz and Class II 6.7 GHz CH{sub 3}OH maser survey of a sample of {approx}20 massive young stellar object (MYSO) outflow candidates selected on the basis of extended 4.5 {mu}m emission in Spitzer Galactic Legacy Infrared Mid-Plane Survey Extraordinaire images. These 4.5 {mu}m selected candidates are referred to as extended green objects (EGOs), for the common coding of this band as green in three-color Infrared Array Camera images. The detection rate of 6.7 GHz Class II CH{sub 3}OH masers, which are associated exclusively with massive YSOs, toward EGOs is {approx}>64%-nearly double the detection rate of surveys using other MYSO selection criteria. The detection rate of Class I 44 GHz CH{sub 3}OH masers, which trace molecular outflows, is {approx}89% toward EGOs associated with 6.7 GHz CH{sub 3}OH masers. The two types of CH{sub 3}OH masers exhibit different spatial distributions: 6.7 GHz masers are centrally concentrated and usually coincide with 24 {mu}m emission, while 44 GHz masers are widely distributed and generally trace diffuse 4.5 {mu}m features. We also present results of a complementary James Clerk Maxwell Telescope (JCMT) single-pointing molecular line survey of EGOs in the outflow tracers HCO{sup +}(3-2) and SiO(5-4). The HCO{sup +} line profiles and high SiO detection rate (90%) are indicative of the presence of active outflows. No 44 GHz continuum emission is detected at the 5 mJy beam{sup -1} (5{sigma}) level toward 95% of EGOs surveyed, excluding bright ultracompact H II regions as powering sources for the 4.5 {mu}m outflows. The results of our surveys constitute strong evidence that EGOs are young, massive YSOs, with active outflows, presumably powered by ongoing accretion.

  18. RESIS-II: An Updated Version of the Original Reservoir Sedimentation Survey Information System (RESIS) Database

    USGS Publications Warehouse

    Ackerman, Katherine V.; Mixon, David M.; Sundquist, Eric T.; Stallard, Robert F.; Schwarz, Gregory E.; Stewart, David W.

    2009-01-01

    The Reservoir Sedimentation Survey Information System (RESIS) database, originally compiled by the Soil Conservation Service (now the Natural Resources Conservation Service) in collaboration with the Texas Agricultural Experiment Station, is the most comprehensive compilation of data from reservoir sedimentation surveys throughout the conterminous United States (U.S.). The database is a cumulative historical archive that includes data from as early as 1755 and as late as 1993. The 1,823 reservoirs included in the database range in size from farm ponds to the largest U.S. reservoirs (such as Lake Mead). Results from 6,617 bathymetric surveys are available in the database. This Data Series provides an improved version of the original RESIS database, termed RESIS-II, and a report describing RESIS-II. The RESIS-II relational database is stored in Microsoft Access and includes more precise location coordinates for most of the reservoirs than the original database but excludes information on reservoir ownership. RESIS-II is anticipated to be a template for further improvements in the database.

  19. The HIFI spectral survey of AFGL 2591 (CHESS). II. Summary of the survey

    NASA Astrophysics Data System (ADS)

    Kaźmierczak-Barthel, M.; van der Tak, F. F. S.; Helmich, F. P.; Chavarría, L.; Wang, K.-S.; Ceccarelli, C.

    2014-07-01

    Aims: This paper presents the richness of submillimeter spectral features in the high-mass star forming region AFGL 2591. Methods: As part of the Chemical Herschel Survey of Star Forming Regions (CHESS) key programme, AFGL 2591 was observed by the Herschel (HIFI) instrument. The spectral survey covered a frequency range from 480 to 1240 GHz as well as single lines from 1267 to 1901 GHz (i.e. CO, HCl, NH3, OH, and [CII]). Rotational and population diagram methods were used to calculate column densities, excitation temperatures, and the emission extents of the observed molecules associated with AFGL 2591. The analysis was supplemented with several lines from ground-based JCMT spectra. Results: From the HIFI spectral survey analysis a total of 32 species were identified (including isotopologues). Although the lines are mostly quite weak (∫TmbdV ~ few K km s-1), 268 emission and 16 absorption lines were found (excluding blends). Molecular column densities range from 6 × 1011 to 1 × 1019 cm-2 and excitation temperatures from 19 to 175 K. Cold (e.g. HCN, H2S, and NH3 with temperatures below 70 K) and warm species (e.g. CH3OH, SO2) in the protostellar envelope can be distinguished. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Appendix A is available in electronic form at http://www.aanda.org

  20. Color and contrast sensitivity after glare from high-brightness LEDs

    NASA Astrophysics Data System (ADS)

    Reidenbach, H.-D.

    2008-02-01

    The color contrast capability was investigated for 3 volunteers with 7 specially developed test charts in red, green, blue, cyan, magenta, yellow and black as a reference, namely without and after glare from 4 colored high-brightness LEDs. Each subject completed 56 tests in order to check especially the ability to discriminate low contrast. It was found that a contrast decrease of one level is equivalent to an increase of about 4 s in the required identification time and in addition a delay time between about 14 s and 16 s has been measured at the beginning of the respective test as a result of the dazzling glare from an LED. In addition trials have been performed with 4 different pseudoisochromatic color plates designed by Ishihara for color vision. These plates have been used to determine temporary color deficiencies after an exposure from a high-brightness LED. For this purpose 40 volunteers have been included in a laboratory test. Color vision was impaired for periods between 27 s and 186 s depending on the applied color plate and respective LED color.

  1. Normal values for the size of a halo produced by a glare source.

    PubMed

    Puell, María C; Pérez-Carrasco, María J; Barrio, Ana; Antona, Beatriz; Palomo-Alvarez, Catalina

    2013-09-01

    To determine the size of a halo in the visual field induced by bright light in healthy eyes of all ages using the Vision Monitor (MonCv3; Metrovision, Pérenchies, France) and to assess the repeatability of the method. Measurements were made in the right eyes of 147 healthy subjects (mean age: 48.2 ± 16.2 years) who were classified into six age groups. Using the Vision Monitor, optotypes of low luminance were presented at a distance of 2.5 m. The visual angle subtended by the radius of the halo was calculated in minutes of arc (arc min). The repeatability of the method was determined in a subset of 37 subjects older than 50 years by calculating the Bland-Altman coefficient of repeatability. The mean radius of the halo was 111.6 ± 39.8 arc min. Halo radius started to increase significantly from the age of 50 to 59 years. The relationship between halo radius and age (r = 0.65; P < .0001) was described by fitting a power function to the data. Halo size was independent of gender. The coefficient of repeatability of the method was ±44 arc min. Halo size increases with age following a power model. The normal halo size values provided could help clinicians distinguish between normal or abnormal glare problems. The intersession repeatability observed for halo size measurement indicates this method could be useful for assessing visual impairment caused by glare. Copyright 2013, SLACK Incorporated.

  2. Dazzling glare: Protection criteria versus visual performance. Interim report, September 1985-August 1990

    SciTech Connect

    Sheehy, J.B.

    1989-06-07

    Laser eye protection was first introduced into the U.S. Fleet when the need arose to protect aviators and aircrew from our own neodymium systems. This protection was designed to reduce the incidence energy below the maximum permissible exposure level established by the American National Standards Institute. Since range finders used an infrared wavelength, as defined and therefore not visible to the eye, there was no possibility of glare. With time more systems were developed employing lasers in both the visible and infrared portion of the spectrum. When the lasing of the police helicopter in Los Angeles was first reported in 1981 it immediately became apparent that for wavelengths in the visible portion of the spectrum substantial losses in visual performance could be encountered at safe exposure levels. The incident emphasized the need to develop laser eye protection based on criteria that encompassed both transient (glare) and permanent (burns, hemorraghic lesions) effects. The goal of this research project has been to establish protection levels based on performance rather than damage criteria.

  3. Visual ergonomic aspects of glare on computer displays: glossy screens and angular dependence

    NASA Astrophysics Data System (ADS)

    Brunnström, Kjell; Andrén, Börje; Konstantinides, Zacharias; Nordström, Lukas

    2007-02-01

    Recently flat panel computer displays and notebook computer are designed with a so called glare panel i.e. highly glossy screens, have emerged on the market. The shiny look of the display appeals to the costumers, also there are arguments that the contrast, colour saturation etc improves by using a glare panel. LCD displays suffer often from angular dependent picture quality. This has been even more pronounced by the introduction of Prism Light Guide plates into displays for notebook computers. The TCO label is the leading labelling system for computer displays. Currently about 50% of all computer displays on the market are certified according to the TCO requirements. The requirements are periodically updated to keep up with the technical development and the latest research in e.g. visual ergonomics. The gloss level of the screen and the angular dependence has recently been investigated by conducting user studies. A study of the effect of highly glossy screens compared to matt screens has been performed. The results show a slight advantage for the glossy screen when no disturbing reflexes are present, however the difference was not statistically significant. When disturbing reflexes are present the advantage is changed into a larger disadvantage and this difference is statistically significant. Another study of angular dependence has also been performed. The results indicates a linear relationship between the picture quality and the centre luminance of the screen.

  4. Effect of yellow filter on visual acuity and contrast sensitivity under glare condition among different age groups.

    PubMed

    Mahjoob, Monireh; Heydarian, Samira; Koochi, Somayyeh

    2016-08-01

    The aim of this study is to investigate the effect of yellow filter on visual acuity and contrast sensitivity under glare condition for various ages. A total of 60 subjects, aged 5-60 years, with no ocular pathology and no previous surgery were assessed in this cross-sectional study. We divided subjects into six subgroups according to their ages, and the number of subjects in each group was 10: group 1, aged 5-10 years; group 2, aged 11-20 years; group 3, aged 21-30 years; group 4, aged 31-40 years; group 5, aged 41-50 years; and group 6, aged 51-60 years. Snellen visual acuity and Pelli Robson contrast sensitivity with and without glare and with the use of yellow filter under glare condition were determined. Data analysis was carried out using SPSS, version 20. Our results showed a significant reduction in contrast sensitivity under glare condition in all age groups (p = 0.000), which improved significantly with the use of yellow filter (p = 0.000). Although when data in different age groups were analyzed separately, this improvement was only significant in older subjects, aged 51-60 years (p = 0.007). No significant difference was found between Snellen visual acuity with and without glare (p = 0.083), and also we found no yellow filter effect on visual acuity under glare condition. We conclude that yellow filter, which absorbs short wavelength, may provide significant contrast sensitivity benefits for individuals and influences older subjects more than younger ones.

  5. THE GREEN BANK TELESCOPE H II REGION DISCOVERY SURVEY. III. KINEMATIC DISTANCES

    SciTech Connect

    Anderson, L. D.; Bania, T. M.; Balser, Dana S.; Rood, Robert T.

    2012-07-20

    Using the H I emission/absorption method, we resolve the kinematic distance ambiguity and derive distances for 149 of 182 (82%) H II regions discovered by the Green Bank Telescope H II Region Discovery Survey (GBT HRDS). The HRDS is an X-band (9 GHz, 3 cm) GBT survey of 448 previously unknown H II regions in radio recombination line and radio continuum emission. Here, we focus on HRDS sources from 67 Degree-Sign {>=} l {>=} 18 Degree-Sign , where kinematic distances are more reliable. The 25 HRDS sources in this zone that have negative recombination line velocities are unambiguously beyond the orbit of the Sun, up to 20 kpc distant. They are the most distant H II regions yet discovered. We find that 61% of HRDS sources are located at the far distance, 31% at the tangent-point distance, and only 7% at the near distance. 'Bubble' H II regions are not preferentially located at the near distance (as was assumed previously) but average 10 kpc from the Sun. The HRDS nebulae, when combined with a large sample of H II regions with previously known distances, show evidence of spiral structure in two circular arc segments of mean Galactocentric radii of 4.25 and 6.0 kpc. We perform a thorough uncertainty analysis to analyze the effect of using different rotation curves, streaming motions, and a change to the solar circular rotation speed. The median distance uncertainty for our sample of H II regions is only 0.5 kpc, or 5%. This is significantly less than the median difference between the near and far kinematic distances, 6 kpc. The basic Galactic structure results are unchanged after considering these sources of uncertainty.

  6. Changes of Multiple Metal Accumulation (MMA) in New Orleans Soil: Preliminary Evaluation of Differences between Survey I (1992) and Survey II (2000)

    PubMed Central

    Mielke, Howard W.; Gonzales, Christopher; Powell, Eric; MielkeJr, Paul W.

    2005-01-01

    Soil metal surveys were conducted in Baltimore, MD (1976–1979), Minnesota (1981–1988) and most recently, New Orleans, LA (1989-present). The unique characteristic of New Orleans is that it has two surveys; Survey I was completed in 1992 and Survey II was completed in 2000. This paper seeks to determine if there is a perceptible change in the amount of metals during less than a decade that separated these surveys. The Survey I collection was 4,026 samples stratified by 283 census tracts. All samples were collected in residential neighborhoods at least one block from a busy street. The Survey II collection was 5,467 samples stratified by 286 census tracts (plus City Park). The Survey II collection included busy streets as a category of samples. For comparison, the busy street category of 1,078 samples was excluded from Survey II for a total of 4,388 samples. The extraction methods of the two surveys used the same protocol for strength of acid (1 M HNO3), shaker-time (2 hours), and room temperature (~22ºC). However, Survey II differed in amount of sample used in extraction. For Surveys I and II, 4.0g and 0.4g were used respectively. The same ICP-AES was used to measure 8 metals in both surveys. To evaluate the analytical results of the two methods, reference soil samples (n=36) from the Wageningen Evaluating Programs for Analytical Laboratories, International Soil-analytical Exchange (WEPAL; ISE) were used. The relationship between the 4.0 and 0.4 g results were linear and the Survey I results were adjusted for sample:acid ratio. Further evaluation was done by creating interpolated Multiple Metal Accumulation (MMA) maps based on the median MMA for each census tract. A new map was created by dividing Survey II MMA by Survey I MMA. The ratio indicates increases of soil metals in the inner city and decreases of soil metals in the outlying areas of Metropolitan New Orleans. Comparing fresh parent alluvium from the Mississippi River with urban soil metal quantities

  7. Spectroscopic CCD surveys for quasars at large redshift. II - A Pfuei transit survey

    NASA Technical Reports Server (NTRS)

    Schmidt, Maarten; Schneider, Donald P.; Gunn, James E.

    1986-01-01

    A CCD transit survey has been carried out with the 200 in. telescope of a strip of sky 5 arcmin wide and 9 hr long. Direct images and slitless spectra of over 43,000 objects were obtained on two successive nights. An automatic search for emission lines of given minimum equivalent width and signal-to-noise ratio yielded 52 candidate sources. Slit spectra revealed that 24 were emission-line galaxies with z less than 0.4 and eight were quasars with 2 between 1.00 and 2.76. The number of quasars detect agrees with that predicted from luminosity function models for z less than 2.9. The models also indicate that between 30 and 62 quasars with z less than 2.9 should have been found in this survey, but none were detected. This result reconfirms that there is a redshift cutoff near or below redshift three. The apparent conflict of this measurement with the known existence of dozens of quasars with redshifts larger than three is discussed.

  8. Psychometric Properties of the Hypoglycemia Fear Survey-II for Adults With Type 1 Diabetes

    PubMed Central

    Gonder-Frederick, Linda A.; Schmidt, Karen M.; Vajda, Karen A.; Greear, Megan L.; Singh, Harsimran; Shepard, Jaclyn A.; Cox, Daniel J.

    2011-01-01

    OBJECTIVE To perform the first comprehensive psychometric evaluation of the Hypoglycemia Fear Survey-II (HFS-II), a measure of the behavioral and affective dimensions of fear of hypoglycemia, using modern test-theory methods, including item-response theory (IRT). RESEARCH DESIGN AND METHODS Surveys completed in four previous studies by 777 adults with type 1 diabetes were aggregated for analysis, with 289 subjects completing both subscales of the HFS-II and 488 subjects completing only the Worry subscale. The aggregated sample (53.3% female, 44.4% using insulin pumps) had a mean age of 41.9 years, diabetes duration of 23.8 years, HbA1c value of 7.7%, and 1.4 severe hypoglycemic episodes in the past year. Data analysis included exploratory factor analysis using polychoric correlations and IRT. Factors were analyzed for fit, trait-level locations, point-measure correlations, and separation values. RESULTS Internal and test-retest reliability was good, as well as convergent validity, as demonstrated by significant correlations with other measures of psychological distress. Scores were significantly higher in subjects who had experienced severe hypoglycemia in the past year. Factor analyses validated the two subscales of the HFS-II. Item analyses showed that 12 of 15 items on the Behavior subscale, and all of the items on the Worry subscale had good-fit statistics. CONCLUSIONS The HFS-II is a reliable and valid measure of the fear of hypoglycemia in adults with type 1 diabetes, and factor analyses and IRT support the two separate subscales of the survey. PMID:21346182

  9. Testing supernova cosmology and progenitor effects with the SDSS-II supernova survey

    NASA Astrophysics Data System (ADS)

    D'Andrea, Christopher Brian

    The study of Type Ia Supernovae, the brilliant explosions of White Dwarfs, has ushered in a new era of observational Cosmology, one in which we have learned that the Universe is not only expanding, but accelerating in its expansion. For further advances to be made in the the field of Supernova Cosmology, future planned surveys will have to understand the systematic differences in these explosions. We use the full 3-year observational data from the Sloan Digital Sky Survey - II Supernova Survey to explore this field. First, we show that the environment a Type Ia Supernova occurs in biases the distance modulus at which current algorithms place them, resulting in a systematic error in derived cosmological parameters. We then investigate the ability Type II-P Supernovae to be used as complements to their brighter cousins as cosmological distance indicators, subject to different progenitor effects and thus different sources of uncertainty. Finally we quantify the diversity in Type II-P Supernovae themselves and the relationship the environment has on their observational properties, and the propensity this might have for biasing distance measurements with these objects.

  10. Psychometric properties of the School Fears Survey Scale for preadolescents (SFSS-II).

    PubMed

    García-Fernández, José Manuel; Espada Sánchez, José Pedro; Orgilés Amorós, Mireia; Méndez Carrillo, Xavier

    2010-08-01

    This paper describes the psychometric properties of a new children's self-report measure. The School Fears Survey Scale, Form II (SFSS-II) assesses school fears in children from ages 8 to 11. The factor solution with a Spanish sample of 3,665 children isolated four factors: Fear of academic failure and punishment, fear of physical discomfort, fear of social and school assessment and anticipatory and separation anxiety. The questionnaire was tested by confirmatory factor analysis, which accounted for 55.80% of the total variance. Results indicated that the SFSS-II has a high internal consistency (alpha= .89). The results revealed high test-retest reliability and appropriate relationship with other scales. The age by gender interaction was significant. Two-way analysis of variance found that older children and girls had higher anxiety. The instrument shows adequate psychometric guarantees and can be used for the multidimensional assessment of anxiety in clinical and educational settings.

  11. Anniston Community Health Survey: Follow-Up and Dioxin Analyses (ACHS-II) - Methods

    PubMed Central

    Birnbaum, L.S.; Dutton, N.D.; Cusack, C.; Mennemeyer, S.T.; Pavuk, M.

    2015-01-01

    High serum concentrations of polychlorinated biphenyls (PCBs) have been reported previously among residents of Anniston, Alabama, where a PCB production facility was located in the past. As the second of two cross-sectional studies of these Anniston residents, the Anniston Community Health Survey: Follow-Up and Dioxin Analyses (ACHS-II) will yield repeated measurements to be used to evaluate changes over time in ortho-PCB concentrations and selected health indicators in study participants. Dioxins, non-ortho PCBs, other chemicals, heavy metals, and a variety of additional clinical tests not previously measured in the original ACHS cohort will be examined in ACHS-II. The follow-up study also incorporates a questionnaire with extended sections on diet and occupational history for a more comprehensive assessment of possible exposure sources. Data collection for ACHS-II from 359 eligible participants took place in 2014, seven to nine years after ACHS. PMID:25982988

  12. Anniston community health survey: Follow-up and dioxin analyses (ACHS-II)--methods.

    PubMed

    Birnbaum, Linda S; Dutton, N D; Cusack, C; Mennemeyer, S T; Pavuk, M

    2016-02-01

    High serum concentrations of polychlorinated biphenyls (PCBs) have been reported previously among residents of Anniston, Alabama, where a PCB production facility was located in the past. As the second of two cross-sectional studies of these Anniston residents, the Anniston Community Health Survey: Follow-Up and Dioxin Analyses (ACHS-II) will yield repeated measurements to be used to evaluate changes over time in ortho-PCB concentrations and selected health indicators in study participants. Dioxins, non-ortho PCBs, other chemicals, heavy metals, and a variety of additional clinical tests not previously measured in the original ACHS cohort will be examined in ACHS-II. The follow-up study also incorporates a questionnaire with extended sections on diet and occupational history for a more comprehensive assessment of possible exposure sources. Data collection for ACHS-II from 359 eligible participants took place in 2014, 7 to 9 years after ACHS.

  13. PLANETARY NEBULAE DETECTED IN THE SPITZER SPACE TELESCOPE GLIMPSE II LEGACY SURVEY

    SciTech Connect

    Zhang Yong; Sun Kwok E-mail: sunkwok@hku.h

    2009-11-20

    We report the result of a search for the infrared counterparts of 37 planetary nebulae (PNs) and PN candidates in the Spitzer Galactic Legacy Infrared Mid-Plane Survey Extraordinaire II (GLIMPSE II) survey. The photometry and images of these PNs at 3.6, 4.5, 5.8, 8.0, and 24 mum, taken through the Infrared Array Camera (IRAC) and the Multiband Imaging Photometer for Spitzer (MIPS), are presented. Most of these nebulae are very red and compact in the IRAC bands, and are found to be bright and extended in the 24 mum band. The infrared morphology of these objects are compared with Halpha images of the Macquarie-AAO-Strasbourg (MASH) and MASH II PNs. The implications for morphological difference in different wavelengths are discussed. The IRAC data allow us to differentiate between PNs and H II regions and be able to reject non-PNs from the optical catalog (e.g., PNG 352.1 - 00.0). Spectral energy distributions are constructed by combing the IRAC and MIPS data with existing near-, mid-, and far-IR photometry measurements. The anomalous colors of some objects allow us to infer the presence of aromatic emission bands. These multi-wavelength data provide useful insights into the nature of different nebular components contributing to the infrared emission of PNs.

  14. Orthopedic manifestations in patients with mucopolysaccharidosis type II (Hunter syndrome) enrolled in the Hunter Outcome Survey

    PubMed Central

    Link, Bianca; de Camargo Pinto, Louise Lapagesse; Giugliani, Roberto; Wraith, James Edmond; Guffon, Nathalie; Eich, Elke; Beck, Michael

    2010-01-01

    Mucopolysaccharidosis type II (MPS II or Hunter syndrome) is a rare, inherited disorder caused by deficiency of the lysosomal enzyme iduronate-2-sulfatase. As a result of this deficiency, glycosaminoglycans accumulate in lysosomes in many tissues, leading to progressive multisystemic disease. The cardiopulmonary and neurological problems associated with MPS II have received considerable attention. Orthopedic manifestations are common but not as well characterized. This study aimed to characterize the prevalence and severity of orthopedic manifestations of MPS II and to determine the relationship of these signs and symptoms with cardiovascular, pulmonary and central nervous system involvement. Orthopedic manifestations of MPS II were studied using cross-sectional data from the Hunter Outcome Survey (HOS). The HOS is a global, physician-led, multicenter observational database that collects information on the natural history of MPS II and the long-term safety and effectiveness of enzyme replacement therapy. As of January 2009, the HOS contained baseline data on joint range of motion in 124 males with MPS II. In total, 79% of patients had skeletal manifestations (median onset, 3.5 years) and 25% had abnormal gait (median onset, 5.4 years). Joint range of motion was restricted for all joints assessed (elbow, shoulder, hip, knee and ankle). Extension was the most severely affected movement: the exception to this was the shoulder. Surgery for orthopedic problems was rare. The presence of orthopedic manifestations was associated with the presence of central nervous system and pulmonary involvement, but not so clearly with cardiovascular involvement. Orthopedic interventions should be considered on an individual-patient basis. Although some orthopedic manifestations associated with MPS II may be managed routinely, a good knowledge of other concurrent organ system involvement is essential. A multidisciplinary approach is required. PMID:21808707

  15. Observations of Mg II Absorption near z ~ 1 Galaxies Selected from the DEEP2 Redshift Survey

    NASA Astrophysics Data System (ADS)

    Lovegrove, Elizabeth; Simcoe, Robert A.

    2011-10-01

    We study the frequency of Mg II absorption in the outer halos of galaxies at z = 0.6-1.4 (with median z = 0.87), using new spectra obtained of 10 background quasars with galaxy impact parameters of b < 100 kpc. The quasar sight lines were selected from the Sloan Digital Sky Survey DR6 QSO catalog based on proximity to galaxies in the DEEP2 redshift survey. In addition to the 10 small impact systems, we examine 40 additional galaxies at 100 kpc < b < 500 kpc serendipitously located in the same fields. We detect Mg II absorbers with equivalent width Wr = 0.15-1.0 Å, though not all absorbers correlate with DEEP galaxies. We find five unique absorbers within Δv = 500 km s-1 and b < 100 kpc of a DEEP galaxy; this small sample contains both early- and late-type galaxies and has no obvious trends with star formation rate. No Mg II is detected more than 100 kpc from galaxies; inside this radius the covering fraction scales with impact parameter and galaxy luminosity in a very similar fashion to samples studied at lower redshift. In all but one case, when Mg II is detected without a spectroscopically confirmed galaxy, there exists a plausible photometric candidate which was excluded because of slit collision or apparent magnitude. We do not detect any strong absorbers with Wr > 1.0 Å, consistent with other samples of galaxy-selected Mg II systems. We speculate that Mg II systems with 0.3 < Wr < 1.0 trace old relic material from galactic outflows and/or the halo assembly process, and that in contrast, systems with large Wr are more likely to reflect the more recent star-forming history of their associated galaxies. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.

  16. NEWLY IDENTIFIED EXTENDED GREEN OBJECTS (EGOs) FROM THE SPITZER GLIMPSE II SURVEY. I. CATALOG

    SciTech Connect

    Chen, Xi; Gan, Cong-Gui; Shen, Zhi-Qiang; Ellingsen, Simon P.; Titmarsh, Anita; He, Jin-Hua

    2013-05-01

    We have produced a catalog containing 98 newly identified massive young stellar object (MYSO) candidates associated with ongoing outflows (known as extended green objects, or EGOs). These have been identified from the Spitzer Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE) II data set and our new identifications increase the number of known EGOs to {approx}400 in our Galaxy, adding to the {approx}300 previously identified EGOs reported by Cyganowski et al. from the GLIMPSE I survey. The high detection rate ({approx}70%) of 95 GHz class I methanol masers achieved in a survey toward 57 of these new EGOs with the Mopra 22 m radio telescope demonstrates that the new EGOs are associated with outflows. Investigations of the mid-infrared properties and physical associations with other star formation tracers (e.g., infrared dark clouds, class I and II methanol masers, and millimeter Bolocam Galactic Plane Survey sources) reveal that the newly identified EGOs are very similar in nature to those in the sample of Cyganowski et al. All of the observational evidence supports the hypothesis that EGOs correspond to MYSOs at the earliest evolutionary stage, with ongoing outflow activity, and active rapid accretion.

  17. Attenuating Photostress and Glare Disability in Pseudophakic Patients through the Addition of a Short-Wave Absorbing Filter

    PubMed Central

    Hammond, Billy R.

    2015-01-01

    To evaluate the effects of filtering short wavelength light on visual performance under intense light conditions among pseudophakic patients previously implanted with a clear intraocular lens (IOL). This was a patient-masked, randomized crossover study conducted at 6 clinical sites in the United States between September 2013 and January 2014. One hundred fifty-four bilaterally pseudophakic patients were recruited. Photostress recovery time and glare disability thresholds were measured with clip-on blue-light-filtering and placebo (clear; no blue-light filtration) glasses worn over patients' habitual correction. Photostress recovery time was quantified as the time necessary to regain sight of a grating target after intense light exposure. Glare disability threshold was assessed as the intensity of a white-light annulus necessary to obscure a central target. The order of filter used and test eye were randomized across patients. Photostress recovery time and glare disability thresholds were significantly improved (both P < 0.0001) when patients used blue-light-filtering glasses compared with clear, nonfiltering glasses. Compared with a nonfiltering placebo, adding a clip-on blue-absorbing filter to the glasses of pseudophakic patients implanted with clear IOLs significantly increased their ability to cope with glare and to recover normal viewing after an intensive photostress. This result implies that IOL designs with blue-light-filtering characteristics may be beneficial under intense light conditions. PMID:25838942

  18. The HK-II Survey: Kinematics of Metal-Poor Stars in the Galaxy

    NASA Astrophysics Data System (ADS)

    Rhee, J.; Beers, T. C.

    2003-12-01

    The digitized HK-II survey (Rhee 2000, Ph.D. thesis, MSU) was originated as a follow-on to the HK-I survey of Beers and colleagues (e.g., Beers et al. 1992, AJ, 103, 1987). HK-I was based on visually-selected candidate metal-poor stars from objective-prism plates. Unfortunately, in the absence of color information, this selection technique introduced a rather severe temperature-related bias. As a result, the HK-I candidates do not include large numbers of metal-deficient giants. In HK-II, candidate metal-poor stars are quantitatively selected from digitized objective-prism spectra with JHK color information from the recently completeted 2MASS catalog. This approach eliminates much of the temperature bias. We have begun to survey candidate very metal-poor ([Fe/H] ≤ -2.0) giants from HK-II, over the magnitude range 11.0 ≤ B ≤ 16.0, covering some ˜7000 deg2 of intermediate to high Galactic-latitudes. Ongoing medium-resolution ( ˜ 1-2Å ) spectroscopic follow-up using NOAO observing facilities has allowed us to obtain, to date, some 1000 spectra (400, 450, and 150 spectra for red giants, subgiants near the main-sequence turnoff, and FHB/A stars, respectively) for the HK-II metal-poor star candidates. In particular, the detection rate of bona fide very metal-poor giants is about 45 %, which is quite encouraging. Most of the "mistakes" are slightly more metal-rich giants, with -2.0 < [Fe/H] < -1.0. Metallicities and radial velocities are determined from our spectroscopy, and proper motions for most of the program stars are obtained from the recently released UCAC2 astrometric survey catalog. Here we present an analysis of the full space motions for numerous metal-poor stars from the HK-II survey. A comparision of the chemical and kinematic properties between high- and low-halo populations (that is, giants vs. sub-giants) will aid us in understanding the formation history of the Milky Way. J.R. acknowledges partial support for this work by NASA through the AAS

  19. Glare-Tunable Transparent Electrochemical Smart Window Coupled with Transparent Organic Light-Emitting Diode

    NASA Astrophysics Data System (ADS)

    Uchida, Takayuki; Shibasaki, Masaaki; Matsuzaki, Tatsuya; Nagata, Yujiro

    2013-04-01

    We fabricated a novel device assembled by coupling a transparent organic light-emitting diode (TOLED) and a glare-tunable transparent electrochemical device. This device could be operated in six different states, namely, (1) transparent, (2) mirror, (3) black, (4) dual emission, (5) single-side emission with mirror, and (6) single-side emission with black. Switching between each of these states could be tuned by varying/selecting the applied DC bias voltage. The device showed 63.8% transmittance in the transparent state, and 42.1% reflectance in the mirror state at 700 nm. Transmittance in both the mirror and black states was less than 0.1% in the visible range.

  20. FIRST-YEAR SLOAN DIGITAL SKY SURVEY-II SUPERNOVA RESULTS: HUBBLE DIAGRAM AND COSMOLOGICAL PARAMETERS

    SciTech Connect

    Kessler, Richard; Frieman, Joshua A.; Becker, Andrew C.; Vanderplas, Jake; Cinabro, David; Marriner, John; Davis, Tamara M.; Dilday, Benjamin; Jha, Saurabh W.; Holtzman, Jon; Lampeitl, Hubert; Smith, Mathew; Nichol, Robert C.; Sako, Masao; Zheng Chen; Bassett, Bruce; Elson, Ed; Bender, Ralf; Depoy, Darren L.; Doi, Mamoru

    2009-11-01

    We present measurements of the Hubble diagram for 103 Type Ia supernovae (SNe) with redshifts 0.04 < z < 0.42, discovered during the first season (Fall 2005) of the Sloan Digital Sky Survey-II (SDSS-II) Supernova Survey. These data fill in the redshift 'desert' between low- and high-redshift SN Ia surveys. Within the framework of the MLCS2K2 light-curve fitting method, we use the SDSS-II SN sample to infer the mean reddening parameter for host galaxies, R{sub V} = 2.18 {+-} 0.14{sub stat} {+-} 0.48{sub syst}, and find that the intrinsic distribution of host-galaxy extinction is well fitted by an exponential function, P(A{sub V} ) = exp(-A{sub V} /{tau}{sub V}), with {tau}{sub V} = 0.334 {+-} 0.088 mag. We combine the SDSS-II measurements with new distance estimates for published SN data from the ESSENCE survey, the Supernova Legacy Survey (SNLS), the Hubble Space Telescope (HST), and a compilation of Nearby SN Ia measurements. A new feature in our analysis is the use of detailed Monte Carlo simulations of all surveys to account for selection biases, including those from spectroscopic targeting. Combining the SN Hubble diagram with measurements of baryon acoustic oscillations from the SDSS Luminous Red Galaxy sample and with cosmic microwave background temperature anisotropy measurements from the Wilkinson Microwave Anisotropy Probe, we estimate the cosmological parameters w and {omega}{sub M}, assuming a spatially flat cosmological model (FwCDM) with constant dark energy equation of state parameter, w. We also consider constraints upon {omega}{sub M} and {omega}{sub {lambda}} for a cosmological constant model ({lambda}CDM) with w = -1 and non-zero spatial curvature. For the FwCDM model and the combined sample of 288 SNe Ia, we find w = -0.76 {+-} 0.07(stat) {+-} 0.11(syst), {omega}{sub M} = 0.307 {+-} 0.019(stat) {+-} 0.023(syst) using MLCS2K2 and w = -0.96 {+-} 0.06(stat) {+-} 0.12(syst), {omega}{sub M} = 0.265 {+-} 0.016(stat) {+-} 0.025(syst) using the SALT-II

  1. A cross-polarized freeform illumination design for glare reduction in fruit quality inspection

    NASA Astrophysics Data System (ADS)

    Keresztes, Janos C.; Koshel, R. John; Chipman, Russel; Stover, John C.; Saeys, Wouter

    2015-09-01

    Common illumination systems in short wave infrared (SWIR) hyperspectral imaging (HSI) include direct or indirect tungsten halogen lights. While direct lights provide more radiation onto the samples than dome setups, thus being more energy efficient, the acquired images often suffer from specular reflections and gloss. Glare artifacts in images increase variability in the data limiting the accuracy of machine vision algorithms for defect detection and quality inspection, or even providing false positives. Although domes are known to provide a near Lambertian illumination and glare free images, glossy regions and heterogeneities may remain in the data in practice. More particularly, in the field of fruit and vegetable quality inspection, due to their waxy surface, it remains challenging to design an efficient realistic lighting system. This paper suggests a new approach to optimize the illumination of fruit and vegetables based on measurements of the bidirectional reflectance distribution function (BRDF), shape and Stokes parameters. From these measured values, a BRDF model is loaded into ray-tracing software for realistic illumination engineering in order to determine the most suitable illumination scheme. This concept is applied to apples and a cross polarizer (CP) with freeform optics (FO) optical configuration is proposed, which allows the FO to be optimized to maximize uniformity in the field of view of the imager and removes the parallel polarized gloss on the apples. The performance of this CP illumination system was determined experimentally for a set of apples. This cross polarized (CP) illumination system provided a uniformity (U) of 92% and an efficiency (ν) of 90%, while U = 87% and ν = 14% for an ideal dome configuration when illuminating a rectangular target. The simulated imaged apples with assigned optical properties performed better with CP (U=80%) than when using a dome (U=73%) by 7%. Finally, the sensitivity of the design for the light

  2. The VMC Survey - XIII. Type II Cepheids in the Large Magellanic Cloud

    NASA Astrophysics Data System (ADS)

    Ripepi, V.; Moretti, M. I.; Marconi, M.; Clementini, G.; Cioni, M.-R. L.; de Grijs, R.; Emerson, J. P.; Groenewegen, M. A. T.; Ivanov, V. D.; Muraveva, T.; Piatti, A. E.; Subramanian, S.

    2015-01-01

    The VISTA (Visible and Infrared Survey Telescope for Astronomy) survey of the Magellanic Clouds System (VMC) is collecting deep Ks-band time-series photometry of the pulsating variable stars hosted in the system formed by the two Magellanic Clouds and the Bridge connecting them. In this paper, we have analysed a sample of 130 Large Magellanic Cloud (LMC) Type II Cepheids (T2CEPs) found in tiles with complete or near-complete VMC observations for which identification and optical magnitudes were obtained from the OGLE III (Optical Gravitational Lensing Experiment) survey. We present J and Ks light curves for all 130 pulsators, including 41 BL Her, 62 W Vir (12 pW Vir) and 27 RV Tau variables. We complement our near-infrared photometry with the V magnitudes from the OGLE III survey, allowing us to build a variety of period-luminosity (PL), period-luminosity-colour (PLC) and period-Wesenheit (PW) relationships, including any combination of the V, J, Ks filters and valid for BL Her and W Vir classes. These relationships were calibrated in terms of the LMC distance modulus, while an independent absolute calibration of the PL(Ks) and the PW(Ks, V) was derived on the basis of distances obtained from Hubble Space Telescope parallaxes and Baade-Wesselink technique. When applied to the LMC and to the Galactic globular clusters hosting T2CEPs, these relations seem to show that (1) the two Population II standard candles RR Lyrae and T2CEPs give results in excellent agreement with each other; (2) there is a discrepancy of ˜0.1 mag between Population II standard candles and classical Cepheids when the distances are gauged in a similar way for all the quoted pulsators. However, given the uncertainties, this discrepancy is within the formal 1σ uncertainties.

  3. Cosmology with Photometrically Classified Type Ia Supernovae from the SDSS-II Supernova Survey

    NASA Astrophysics Data System (ADS)

    Campbell, Heather; D'Andrea, Chris B.; Nichol, Robert C.; Sako, Masao; Smith, Mathew; Lampeitl, Hubert; Olmstead, Matthew D.; Bassett, Bruce; Biswas, Rahul; Brown, Peter; Cinabro, David; Dawson, Kyle S.; Dilday, Ben; Foley, Ryan J.; Frieman, Joshua A.; Garnavich, Peter; Hlozek, Renee; Jha, Saurabh W.; Kuhlmann, Steve; Kunz, Martin; Marriner, John; Miquel, Ramon; Richmond, Michael; Riess, Adam; Schneider, Donald P.; Sollerman, Jesper; Taylor, Matt; Zhao, Gong-Bo

    2013-02-01

    We present the cosmological analysis of 752 photometrically classified Type Ia Supernovae (SNe Ia) obtained from the full Sloan Digital Sky Survey II (SDSS-II) Supernova (SN) Survey, supplemented with host-galaxy spectroscopy from the SDSS-III Baryon Oscillation Spectroscopic Survey. Our photometric-classification method is based on the SN classification technique of Sako et al., aided by host-galaxy redshifts (0.05 < z < 0.55). SuperNova ANAlysis simulations of our methodology estimate that we have an SN Ia classification efficiency of 70.8%, with only 3.9% contamination from core-collapse (non-Ia) SNe. We demonstrate that this level of contamination has no effect on our cosmological constraints. We quantify and correct for our selection effects (e.g., Malmquist bias) using simulations. When fitting to a flat ΛCDM cosmological model, we find that our photometric sample alone gives Ω m = 0.24+0.07 -0.05 (statistical errors only). If we relax the constraint on flatness, then our sample provides competitive joint statistical constraints on Ω m and ΩΛ, comparable to those derived from the spectroscopically confirmed Three-year Supernova Legacy Survey (SNLS3). Using only our data, the statistics-only result favors an accelerating universe at 99.96% confidence. Assuming a constant wCDM cosmological model, and combining with H 0, cosmic microwave background, and luminous red galaxy data, we obtain w = -0.96+0.10 -0.10, Ω m = 0.29+0.02 -0.02, and Ω k = 0.00+0.03 -0.02 (statistical errors only), which is competitive with similar spectroscopically confirmed SNe Ia analyses. Overall this comparison is reassuring, considering the lower redshift leverage of the SDSS-II SN sample (z < 0.55) and the lack of spectroscopic confirmation used herein. These results demonstrate the potential of photometrically classified SN Ia samples in improving cosmological constraints.

  4. Photometric properties of intermediate-redshift Type Ia supernovae observed by the Sloan Digital Sky Survey-II Supernova Survey

    NASA Astrophysics Data System (ADS)

    Takanashi, N.; Doi, M.; Yasuda, N.; Kuncarayakti, H.; Konishi, K.; Schneider, D. P.; Cinabro, D.; Marriner, J.

    2017-02-01

    We have analysed multiband light curves of 328 intermediate-redshift (0.05 ≤ z < 0.24) Type Ia supernovae (SNe Ia) observed by the Sloan Digital Sky Survey-II Supernova Survey. The multiband light curves were parametrized by using the multiband stretch method, which can simply parametrize light-curve shapes and peak brightness without dust extinction models. We found that most of the SNe Ia that appeared in red host galaxies (u - r > 2.5) do not have a broad light-curve width and the SNe Ia that appeared in blue host galaxies (u - r < 2.0) have a variety of light-curve widths. The Kolmogorov-Smirnov test shows that the colour distribution of SNe Ia appearing in red/blue host galaxies is different (a significance level of 99.9 per cent). We also investigate the extinction law of host galaxy dust. As a result, we find that the value of Rv derived from SNe Ia with medium light-curve widths is consistent with the standard Galactic value, whereas the value of Rv derived from SNe Ia that appear in red host galaxies becomes significantly smaller. These results indicate that there may be two types of SNe Ia with different intrinsic colours, and that they are obscured by host galaxy dust with two different properties.

  5. Influence of the Metal Volume Fraction on the permanent dent depth and energy absorption of GLARE plates subjected to low velocity impact

    NASA Astrophysics Data System (ADS)

    Bikakis, GSE; Savaidis, A.; Zalimidis, P.; Tsitos, S.

    2016-11-01

    Fiber-metal laminates are hybrid composite materials, consisting of alternating metal layers bonded to fiber-reinforced prepreg layers. GLARE (GLAss REinforced) belongs to this new family of materials. GLARE is the most successful fiber-metal laminate up to now and is currently being used for the construction of primary aerospace structures, such as the fuselage of the Airbus A380 air plane. Impact properties are very important in aerospace structures, since impact damage is caused by various sources, such as maintenance damage from dropped tools, collision between service cars or cargo and the structure, bird strikes and hail. The principal objective of this article is to evaluate the influence of the Metal Volume Fraction (MVF) on the low velocity impact response of GLARE fiber-metal laminates. Previously published differential equations of motion are employed for this purpose. The low velocity impact behavior of various circular GLARE plates is predicted and characteristic values of impact variables, which represent the impact phenomenon, are evaluated versus the corresponding MVF of the examined GLARE material grades. The considered GLARE plates are subjected to low velocity impact under identical impact conditions. A strong effect of the MVF on the maximum impact load and a significant effect on the maximum plate deflection of GLARE plates has been found.

  6. Influence of the Metal Volume Fraction on the maximum deflection and impact load of GLARE plates subjected to low velocity impact

    NASA Astrophysics Data System (ADS)

    Bikakis, GSE; Savaidis, A.; Zalimidis, P.; Tsitos, S.

    2016-11-01

    Fiber-metal laminates are hybrid composite materials, consisting of alternating metal layers bonded to fiber-reinforced prepreg layers. GLARE (GLAss REinforced) belongs to this new family of materials. GLARE is the most successful fiber-metal laminate up to now and is currently being used for the construction of primary aerospace structures, such as the fuselage of the Airbus A380 air plane. Impact properties are very important in aerospace structures, since impact damage is caused by various sources, such as maintenance damage from dropped tools, collision between service cars or cargo and the structure, bird strikes and hail. The principal objective of this article is to evaluate the influence of the Metal Volume Fraction (MVF) on the low velocity impact response of GLARE fiber-metal laminates. Previously published differential equations of motion are employed for this purpose. The low velocity impact behavior of various circular GLARE plates is predicted and characteristic values of impact variables, which represent the impact phenomenon, are evaluated versus the corresponding MVF of the examined GLARE material grades. The considered GLARE plates are subjected to low velocity impact under identical impact conditions. A strong effect of the MVF on the maximum impact load and a significant effect on the maximum plate deflection of GLARE plates has been found.

  7. First-Year Spectroscopy for the SDSS-II Supernova Survey

    SciTech Connect

    Zheng, Chen; Romani, Roger W.; Sako, Masao; Marriner, John; Bassett, Bruce; Becker, Andrew; Choi, Changsu; Cinabro, David; DeJongh, Fritz; Depoy, Darren L.; Dilday, Ben; Doi, Mamoru; Frieman, Joshua A.; Garnavich, Peter M.; Hogan, Craig J.; Holtzman, Jon; Im, Myungshin; Jha, Saurabh; Kessler, Richard; Konishi, Kohki; Lampeitl, Hubert

    2008-03-25

    This paper presents spectroscopy of supernovae discovered in the first season of the Sloan Digital Sky Survey-II Supernova Survey. This program searches for and measures multi-band light curves of supernovae in the redshift range z = 0.05-0.4, complementing existing surveys at lower and higher redshifts. Our goal is to better characterize the supernova population, with a particular focus on SNe Ia, improving their utility as cosmological distance indicators and as probes of dark energy. Our supernova spectroscopy program features rapid-response observations using telescopes of a range of apertures, and provides confirmation of the supernova and host-galaxy types as well as precise redshifts. We describe here the target identification and prioritization, data reduction, redshift measurement, and classification of 129 SNe Ia, 16 spectroscopically probable SNe Ia, 7 SNe Ib/c, and 11 SNe II from the first season. We also describe our efforts to measure and remove the substantial host galaxy contamination existing in the majority of our SN spectra.

  8. A Large-Scale, Low-Frequency Murchison Widefield Array Survey of Galactic H ii Regions between 260 < l < 340

    NASA Astrophysics Data System (ADS)

    Hindson, L.; Johnston-Hollitt, M.; Hurley-Walker, N.; Callingham, J. R.; Su, H.; Morgan, J.; Bell, M.; Bernardi, G.; Bowman, J. D.; Briggs, F.; Cappallo, R. J.; Deshpande, A. A.; Dwarakanath, K. S.; For, B.-Q.; Gaensler, B. M.; Greenhill, L. J.; Hancock, P.; Hazelton, B. J.; Kapińska, A. D.; Kaplan, D. L.; Lenc, E.; Lonsdale, C. J.; Mckinley, B.; McWhirter, S. R.; Mitchell, D. A.; Morales, M. F.; Morgan, E.; Oberoi, D.; Offringa, A.; Ord, S. M.; Procopio, P.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Staveley-Smith, L.; Subrahmanyan, R.; Tingay, S. J.; Wayth, R. B.; Webster, R. L.; Williams, A.; Williams, C. L.; Wu, C.; Zheng, Q.

    2016-05-01

    We have compiled a catalogue of H ii regions detected with the Murchison Widefield Array between 72 and 231 MHz. The multiple frequency bands provided by the Murchison Widefield Array allow us identify the characteristic spectrum generated by the thermal Bremsstrahlung process in H ii regions. We detect 306 H ii regions between 260° < l < 340° and report on the positions, sizes, peak, integrated flux density, and spectral indices of these H ii regions. By identifying the point at which H ii regions transition from the optically thin to thick regime, we derive the physical properties including the electron density, ionised gas mass, and ionising photon flux, towards 61 H ii regions. This catalogue of H ii regions represents the most extensive and uniform low frequency survey of H ii regions in the Galaxy to date.

  9. THE GREEN BANK TELESCOPE H II REGION DISCOVERY SURVEY. IV. HELIUM AND CARBON RECOMBINATION LINES

    SciTech Connect

    Wenger, Trey V.; Bania, T. M.; Balser, Dana S.; Anderson, L. D.

    2013-02-10

    The Green Bank Telescope H II Region Discovery Survey (GBT HRDS) found hundreds of previously unknown Galactic regions of massive star formation by detecting hydrogen radio recombination line (RRL) emission from candidate H II region targets. Since the HRDS nebulae lie at large distances from the Sun, they are located in previously unprobed zones of the Galactic disk. Here, we derive the properties of helium and carbon RRL emission from HRDS nebulae. Our target sample is the subset of the HRDS that has visible helium or carbon RRLs. This criterion gives a total of 84 velocity components (14% of the HRDS) with helium emission and 52 (9%) with carbon emission. For our highest quality sources, the average {sup 4}He{sup +}/H{sup +} abundance ratio by number, (y {sup +}), is 0.068 {+-} 0.023(1{sigma}). This is the same ratio as that measured for the sample of previously known Galactic H II regions. Nebulae without detected helium emission give robust y {sup +} upper limits. There are 5 RRL emission components with y {sup +} less than 0.04 and another 12 with upper limits below this value. These H II regions must have either a very low {sup 4}He abundance or contain a significant amount of neutral helium. The HRDS has 20 nebulae with carbon RRL emission but no helium emission at its sensitivity level. There is no correlation between the carbon RRL parameters and the 8 {mu}m mid-infrared morphology of these nebulae.

  10. Large Magellanic Cloud Near-infrared Synoptic Survey. IV. Leavitt Laws for Type II Cepheid Variables

    NASA Astrophysics Data System (ADS)

    Bhardwaj, Anupam; Macri, Lucas M.; Rejkuba, Marina; Kanbur, Shashi M.; Ngeow, Chow-Choong; Singh, Harinder P.

    2017-04-01

    We present time-series observations of Population II Cepheids in the Large Magellanic Cloud at near-infrared (JHK s ) wavelengths. Our sample consists of 81 variables with accurate periods and optical (VI) magnitudes from the OGLE survey, covering various subtypes of pulsators (BL Herculis, W Virginis, and RV Tauri). We generate light-curve templates using high-quality I-band data in the LMC from OGLE and K s -band data in the Galactic bulge from VISTA Variables in Via Láctea survey and use them to obtain robust mean magnitudes. We derive period–luminosity (P–L) relations in the near-infrared and Period–Wesenheit (P–W) relations by combining optical and near-infrared data. Our P–L and P–W relations are consistent with published work when excluding long-period RV Tauris. We find that Pop II Cepheids and RR Lyraes follow the same P–L relations in the LMC. Therefore, we use trigonometric parallax from the Gaia DR1 for VY Pyx and the Hubble Space Telescope parallaxes for k Pav and 5 RR Lyrae variables to obtain an absolute calibration of the Galactic K s -band P–L relation, resulting in a distance modulus to the LMC of {μ }{LMC}=18.54+/- 0.08 mag. We update the mean magnitudes of Pop II Cepheids in Galactic globular clusters using our light-curve templates and obtain distance estimates to those systems, anchored to a precise late-type eclipsing binary distance to the LMC. We find that the distances to these globular clusters based on Pop II Cepheids are consistent (within 2σ ) with estimates based on the {M}V-[{Fe}/{{H}}] relation for horizontal branch stars.

  11. Comparing acquired angioedema with hereditary angioedema (types I/II): findings from the Icatibant Outcome Survey

    PubMed Central

    Zanichelli, A.; Caballero, T.; Bouillet, L.; Aberer, W.; Maurer, M.; Fain, O.; Fabien, V.; Andresen, I.

    2017-01-01

    Summary Icatibant is used to treat acute hereditary angioedema with C1 inhibitor deficiency types I/II (C1‐INH‐HAE types I/II) and has shown promise in angioedema due to acquired C1 inhibitor deficiency (C1‐INH‐AAE). Data from the Icatibant Outcome Survey (IOS) were analysed to evaluate the effectiveness of icatibant in the treatment of patients with C1‐INH‐AAE and compare disease characteristics with those with C1‐INH‐HAE types I/II. Key medical history (including prior occurrence of attacks) was recorded upon IOS enrolment. Thereafter, data were recorded retrospectively at approximately 6‐month intervals during patient follow‐up visits. In the icatibant‐treated population, 16 patients with C1‐INH‐AAE had 287 attacks and 415 patients with C1‐INH‐HAE types I/II had 2245 attacks. Patients with C1‐INH‐AAE versus C1‐INH‐HAE types I/II were more often male (69 versus 42%; P = 0·035) and had a significantly later mean (95% confidence interval) age of symptom onset [57·9 (51·33–64·53) versus 14·0 (12·70–15·26) years]. Time from symptom onset to diagnosis was significantly shorter in patients with C1‐INH‐AAE versus C1‐INH‐HAE types I/II (mean 12·3 months versus 118·1 months; P = 0·006). Patients with C1‐INH‐AAE showed a trend for higher occurrence of attacks involving the face (35 versus 21% of attacks; P = 0·064). Overall, angioedema attacks were more severe in patients with C1‐INH‐HAE types I/II versus C1‐INH‐AAE (61 versus 40% of attacks were classified as severe to very severe; P < 0·001). Median total attack duration was 5·0 h and 9·0 h for patients with C1‐INH‐AAE versus C1‐INH‐HAE types I/II, respectively. PMID:27936514

  12. Comparing acquired angioedema with hereditary angioedema (types I/II): findings from the Icatibant Outcome Survey.

    PubMed

    Longhurst, H J; Zanichelli, A; Caballero, T; Bouillet, L; Aberer, W; Maurer, M; Fain, O; Fabien, V; Andresen, I

    2017-04-01

    Icatibant is used to treat acute hereditary angioedema with C1 inhibitor deficiency types I/II (C1-INH-HAE types I/II) and has shown promise in angioedema due to acquired C1 inhibitor deficiency (C1-INH-AAE). Data from the Icatibant Outcome Survey (IOS) were analysed to evaluate the effectiveness of icatibant in the treatment of patients with C1-INH-AAE and compare disease characteristics with those with C1-INH-HAE types I/II. Key medical history (including prior occurrence of attacks) was recorded upon IOS enrolment. Thereafter, data were recorded retrospectively at approximately 6-month intervals during patient follow-up visits. In the icatibant-treated population, 16 patients with C1-INH-AAE had 287 attacks and 415 patients with C1-INH-HAE types I/II had 2245 attacks. Patients with C1-INH-AAE versus C1-INH-HAE types I/II were more often male (69 versus 42%; P = 0·035) and had a significantly later mean (95% confidence interval) age of symptom onset [57·9 (51·33-64·53) versus 14·0 (12·70-15·26) years]. Time from symptom onset to diagnosis was significantly shorter in patients with C1-INH-AAE versus C1-INH-HAE types I/II (mean 12·3 months versus 118·1 months; P = 0·006). Patients with C1-INH-AAE showed a trend for higher occurrence of attacks involving the face (35 versus 21% of attacks; P = 0·064). Overall, angioedema attacks were more severe in patients with C1-INH-HAE types I/II versus C1-INH-AAE (61 versus 40% of attacks were classified as severe to very severe; P < 0·001). Median total attack duration was 5·0 h and 9·0 h for patients with C1-INH-AAE versus C1-INH-HAE types I/II, respectively. © 2016 British Society for Immunology.

  13. Alchemical poetry in medieval and early modern Europe: a preliminary survey and synthesis. Part II - Synthesis.

    PubMed

    Kahn, Didier

    2011-03-01

    This article provides a preliminary description of medieval and early modern alchemical poetry composed in Latin and in the principal vernacular languages of western Europe. It aims to distinguish the various genres in which this poetry flourished, and to identify the most representative aspects of each cultural epoch by considering the medieval and early modern periods in turn. Such a distinction (always somewhat artificial) between two broad historical periods may be justified by the appearance of new cultural phenomena that profoundly modified the character of early modern alchemical poetry: the ever-increasing importance of the prisca theologia, the alchemical interpretation of ancient mythology, and the rise of neo-Latin humanist poetry. Although early modern alchemy was marked by the appearance of new doctrines (notably the alchemical spiritus mundi and Paracelsianism), alchemical poetry was only superficially modified by criteria of a scientific nature, which therefore appear to be of lesser importance. This study falls into two parts. Part I provides a descriptive survey of extant poetry, and in Part II the results of the survey are analysed in order to highlight such distinctive features as the function of alchemical poetry, the influence of the book market on its evolution, its doctrinal content, and the question of whether any theory of alchemical poetry ever emerged. Part II is accompanied by an index of the authors and works cited in both parts.

  14. VizieR Online Data Catalog: Second epoch VLBA Calibrator Survey (VCS-II) (Gordon+, 2016)

    NASA Astrophysics Data System (ADS)

    Gordon, D.; Jacobs, C.; Beasley, A.; Peck, A.; Gaume, R.; Charlot, P.; Fey, A.; Ma, C.; Titov, O.; Boboltz, D.

    2016-07-01

    Six Very Long Baseline Array (VLBA) calibrator survey campaigns were run between 1994 and 2007 (VCS1, Beasley et al. 2002, cat. J/ApJS/141/13; VCS2, Fomalont et al. 2003, cat. J/AJ/126/2562; VCS3, Petrov et al. 2005, cat. J/AJ/129/1163; VCS4, Petrov et al. 2006, cat. J/AJ/131/1872; VCS5, Kovalev et al. 2007, cat. J/AJ/133/1236; VCS6, Petrov et al. 2008, cat. J/AJ/136/580) We report on the results of a second epoch VLBA Calibrator Survey campaign (VCS-II) in which 2400 VCS sources were re-observed in the X and S bands. The VLBA S/X (S band~2.3GHz and X band~8.6GHz) dual frequency system was used. We used the VLBA RDBE/Mark5C system, which has 16 32MHz channels and records 2 Gbits/s using 2 bit sampling. Due to S-band filters below 2200MHz and above 2400MHz at most of the VLBA antennas, and a broad area of RFI from SiriusXM satellites (2320-2345MHz), only four channels could be deployed in the S band (2220.0, 2252.0, 2284.0, and 2348.0MHz). The other 12 channels were deployed in the X band (8460.0, 8492.0, 8524.0, 8556.0, 8620.0, 8652.0, 8716.0, 8748.0, 8812.0, 8844.0, 8876.0, and 8908.0MHz). We set a target of 300 sources per session, or 2400 total sources for the 8 VLBA sessions. We selected all sources from the Goddard Space Flight Center (GSFC) S/X astrometric/geodetic catalog (available at http://gemini.gsfc.nasa.gov/solutions/ or by following the links at http://lupus.gsfc.nasa.gov/) between -50° and +90° decl. that had been observed in only 1 or 2 sessions as of mid 2013. This amounted to ~2060 sources. To fill out the list, we added ~340 additional sources that had been observed but not detected in the original VCS1-6 analysis. The eight schedules were run between 2014 January and 2015 March (VCS-II-A/BG219A on 2014 01/04 10:04-01/05 10:02; VCS-II-B/BG219B1 on 2014 05/31 17:12-06/01 17:05; VCS-II-D/BG219D on 2014 06/09 09:13-06/10 09:10; VCS-II-C/BG219C on 2014 08/05 13:03-08/06 13:00; VCS-II-E/BG219E on 2014 08/09 00:00-08/09 23:55; VCS-II-F/BG219F on 2014

  15. COSMOLOGY WITH PHOTOMETRICALLY CLASSIFIED TYPE Ia SUPERNOVAE FROM THE SDSS-II SUPERNOVA SURVEY

    SciTech Connect

    Campbell, Heather; D'Andrea, Chris B; Nichol, Robert C.; Smith, Mathew; Lampeitl, Hubert; Sako, Masao; Olmstead, Matthew D.; Brown, Peter; Dawson, Kyle S.; Bassett, Bruce; Biswas, Rahul; Kuhlmann, Steve; Cinabro, David; Dilday, Ben; Foley, Ryan J.; Frieman, Joshua A.; Garnavich, Peter; Hlozek, Renee; Jha, Saurabh W.; Kunz, Martin; and others

    2013-02-15

    We present the cosmological analysis of 752 photometrically classified Type Ia Supernovae (SNe Ia) obtained from the full Sloan Digital Sky Survey II (SDSS-II) Supernova (SN) Survey, supplemented with host-galaxy spectroscopy from the SDSS-III Baryon Oscillation Spectroscopic Survey. Our photometric-classification method is based on the SN classification technique of Sako et al., aided by host-galaxy redshifts (0.05 < z < 0.55). SuperNova ANAlysis simulations of our methodology estimate that we have an SN Ia classification efficiency of 70.8%, with only 3.9% contamination from core-collapse (non-Ia) SNe. We demonstrate that this level of contamination has no effect on our cosmological constraints. We quantify and correct for our selection effects (e.g., Malmquist bias) using simulations. When fitting to a flat {Lambda}CDM cosmological model, we find that our photometric sample alone gives {Omega} {sub m} = 0.24{sup +0.07} {sub -0.05} (statistical errors only). If we relax the constraint on flatness, then our sample provides competitive joint statistical constraints on {Omega} {sub m} and {Omega}{sub {Lambda}}, comparable to those derived from the spectroscopically confirmed Three-year Supernova Legacy Survey (SNLS3). Using only our data, the statistics-only result favors an accelerating universe at 99.96% confidence. Assuming a constant wCDM cosmological model, and combining with H {sub 0}, cosmic microwave background, and luminous red galaxy data, we obtain w = -0.96{sup +0.10} {sub -0.10}, {Omega} {sub m} = 0.29{sup +0.02} {sub -0.02}, and {Omega} {sub k} = 0.00{sup +0.03} {sub -0.02} (statistical errors only), which is competitive with similar spectroscopically confirmed SNe Ia analyses. Overall this comparison is reassuring, considering the lower redshift leverage of the SDSS-II SN sample (z < 0.55) and the lack of spectroscopic confirmation used herein. These results demonstrate the potential of photometrically classified SN Ia samples in improving

  16. Methodology to assess potential glint and glare hazards from concentrating solar power plants : analytical models and experimental validation.

    SciTech Connect

    Diver, Richard B., Jr.; Ghanbari, Cheryl M.; Ho, Clifford Kuofei

    2010-04-01

    With growing numbers of concentrating solar power systems being designed and developed, glint and glare from concentrating solar collectors and receivers is receiving increased attention as a potential hazard or distraction for motorists, pilots, and pedestrians. This paper provides analytical methods to evaluate the irradiance originating from specularly and diffusely reflecting sources as a function of distance and characteristics of the source. Sample problems are provided for both specular and diffuse sources, and validation of the models is performed via testing. In addition, a summary of safety metrics is compiled from the literature to evaluate the potential hazards of calculated irradiances from glint and glare. Previous safety metrics have focused on prevention of permanent eye damage (e.g., retinal burn). New metrics used in this paper account for temporary flash blindness, which can occur at irradiance values several orders of magnitude lower than the irradiance values required for irreversible eye damage.

  17. Measurement of the droplets sizes of a flash boiling spray using an improved extended glare point velocimetry and sizing

    NASA Astrophysics Data System (ADS)

    Shen, Shiquan; Jia, Ming; Wang, Tianyou; Lü, Qieni; Sun, Kai

    2016-04-01

    An improved extended glare point velocimetry and sizing (EGPVS) is proposed to investigate the droplets sizes of a flash boiling spray. When a spherical droplet with a relative refractive index from 1.16 to 1.41 is illuminated by two opposite laser sheets and a charge-coupled device camera is used to collect the s-polarization light at an observation angle of 90°, the intensities of the reflected lights are much stronger than the other order scattering lights. If the intensity of incident laser is controlled appropriately, two glare points from the reflected lights for the droplet are formed at the focused plane, while the intensities of the other order scattering lights are too weak to form any glare points. Then, the droplet diameter can be derived from the distance between the two glare points. In addition, the focused image is relative small, making it possible to measure dense spray. First, the characteristics of the improved EGPVS are discussed, and a series of standard particles are measured for validating this technique. Then, the technique is applied to investigate the droplets sizes of flash boiling spray. It is found that the minimum measurable diameter of droplets is 7.1 μm, and the relative error is less than 4.7 %. The droplet size distributions of spray are different at different stages. The Sauter mean diameter (SMD) of gasoline spray decreases gradually as the fuel temperature increases, which is different from that of a single-component fuel with a sharp decrease in SMD at the flash boiling stage.

  18. Mechanical Properties Characterization and Business Case Analysis of the Fiber Metal Laminate GLARE-3 for Use as Secondary Aircraft Structure

    DTIC Science & Technology

    2010-03-01

    static four-point bending and tensile testing and dynamic impact testing. Aggregate behavior of the constituent materials was predicted using a model...these second generation materials have been required to operate well beyond their initial design lifetimes . The number of critical cracks that have...theoretical model to be able to accurately predict how other GLARE lay-ups would perform under the same given loading and bending conditions. The material

  19. Investigation into the Fiber Orientation Effect on the Formability of GLARE Materials in the Stamp Forming Process

    NASA Astrophysics Data System (ADS)

    Liu, Shichen; Lang, Lihui; Sherkatghanad, Ehsan; Wang, Yao; Xu, Wencai

    2017-07-01

    Glass-reinforced aluminum laminate (GLARE) is a new class of fiber metal laminates (FMLs) which has the advantages such as high tensile strength, outstanding fatigue, impact resistance, and excellent corrosion properties. GLARE has been extensively applied in advanced aerospace and automobile industries. However, the deformation behavior of the glass fiber during forming must be studied to the benefits of the good-quality part we form. In this research, we focus on the effect of fiber layer orientation on the GLARE laminate formability in stamp forming process. Experimental and numerical analysis of stamping a hemisphere part in different fiber orientation is investigated. The results indicate that unidirectional and multi-directional fiber in the middle layer make a significant effect on the thinning and also surface forming quality of the three layer sheet. Furthermore, the stress-strain distribution of the aluminum alloy and the unique anisotropic property of the fiber layer exhibit that fiber layer orientation can also affect the forming depths as well as the fracture modes of the laminate. According to the obtained results, it is revealed that multi-directional fiber layers are a good alternative compared to the unidirectional fibers especially when a better formability is the purpose.

  20. The Coordinated Radio and Infrared Survey for High-mass Star Formation. II. Source Catalog

    NASA Astrophysics Data System (ADS)

    Purcell, C. R.; Hoare, M. G.; Cotton, W. D.; Lumsden, S. L.; Urquhart, J. S.; Chandler, C.; Churchwell, E. B.; Diamond, P.; Dougherty, S. M.; Fender, R. P.; Fuller, G.; Garrington, S. T.; Gledhill, T. M.; Goldsmith, P. F.; Hindson, L.; Jackson, J. M.; Kurtz, S. E.; Martí, J.; Moore, T. J. T.; Mundy, L. G.; Muxlow, T. W. B.; Oudmaijer, R. D.; Pandian, J. D.; Paredes, J. M.; Shepherd, D. S.; Smethurst, S.; Spencer, R. E.; Thompson, M. A.; Umana, G.; Zijlstra, A. A.

    2013-03-01

    The CORNISH project is the highest resolution radio continuum survey of the Galactic plane to date. It is the 5 GHz radio continuum part of a series of multi-wavelength surveys that focus on the northern GLIMPSE region (10° < l < 65°), observed by the Spitzer satellite in the mid-infrared. Observations with the Very Large Array in B and BnA configurations have yielded a 1.''5 resolution Stokes I map with a root mean square noise level better than 0.4 mJy beam-1. Here we describe the data-processing methods and data characteristics, and present a new, uniform catalog of compact radio emission. This includes an implementation of automatic deconvolution that provides much more reliable imaging than standard CLEANing. A rigorous investigation of the noise characteristics and reliability of source detection has been carried out. We show that the survey is optimized to detect emission on size scales up to 14'' and for unresolved sources the catalog is more than 90% complete at a flux density of 3.9 mJy. We have detected 3062 sources above a 7σ detection limit and present their ensemble properties. The catalog is highly reliable away from regions containing poorly sampled extended emission, which comprise less than 2% of the survey area. Imaging problems have been mitigated by down-weighting the shortest spacings and potential artifacts flagged via a rigorous manual inspection with reference to the Spitzer infrared data. We present images of the most common source types found: H II regions, planetary nebulae, and radio galaxies. The CORNISH data and catalog are available online at http://cornish.leeds.ac.uk.

  1. THE COORDINATED RADIO AND INFRARED SURVEY FOR HIGH-MASS STAR FORMATION. II. SOURCE CATALOG

    SciTech Connect

    Purcell, C. R.; Hoare, M. G.; Lumsden, S. L.; Urquhart, J. S.; Cotton, W. D.; Chandler, C.; Churchwell, E. B.; Diamond, P.; Fuller, G.; Garrington, S. T.; Dougherty, S. M.; Fender, R. P.; Gledhill, T. M.; Goldsmith, P. F.; Hindson, L.; Jackson, J. M.; Kurtz, S. E.; Marti, J. [Departamento de Fisica, EPSJ, Universidad de Jaen, Campus Las Lagunillas s and others

    2013-03-01

    The CORNISH project is the highest resolution radio continuum survey of the Galactic plane to date. It is the 5 GHz radio continuum part of a series of multi-wavelength surveys that focus on the northern GLIMPSE region (10 Degree-Sign < l < 65 Degree-Sign ), observed by the Spitzer satellite in the mid-infrared. Observations with the Very Large Array in B and BnA configurations have yielded a 1.''5 resolution Stokes I map with a root mean square noise level better than 0.4 mJy beam{sup -1}. Here we describe the data-processing methods and data characteristics, and present a new, uniform catalog of compact radio emission. This includes an implementation of automatic deconvolution that provides much more reliable imaging than standard CLEANing. A rigorous investigation of the noise characteristics and reliability of source detection has been carried out. We show that the survey is optimized to detect emission on size scales up to 14'' and for unresolved sources the catalog is more than 90% complete at a flux density of 3.9 mJy. We have detected 3062 sources above a 7{sigma} detection limit and present their ensemble properties. The catalog is highly reliable away from regions containing poorly sampled extended emission, which comprise less than 2% of the survey area. Imaging problems have been mitigated by down-weighting the shortest spacings and potential artifacts flagged via a rigorous manual inspection with reference to the Spitzer infrared data. We present images of the most common source types found: H II regions, planetary nebulae, and radio galaxies. The CORNISH data and catalog are available online at http://cornish.leeds.ac.uk.

  2. Multi-centre National Population Health Examination Survey (WOBASZ II study): assumptions, methods, and implementation.

    PubMed

    Drygas, Wojciech; Niklas, Arkadiusz A; Piwońska, Aleksandra; Piotrowski, Walerian; Flotyńska, Anna; Kwaśniewska, Magdalena; Nadrowski, Paweł; Puch-Walczak, Aleksandra; Szafraniec, Krystyna; Bielecki, Wojciech; Kozakiewicz, Krystyna; Pająk, Andrzej; Tykarski, Andrzej; Zdrojewski, Tomasz

    Cardiovascular diseases (CVDs) are the main cause of morbidity and mortality in developed countries. Despite the progress in diagnostics and treatment, it is expected that CVD will still be the main cause of death worldwide until at least 2030. From 1991 CVD mortality in Poland systematically decreased, but it is still higher than the average in Western Europe. In 2013 CVDs were the cause of 46% of all deaths in Poland (40.9% in men and 51.1% in women) and 26.9% of deaths among persons under 65 years of age. The epidemiologic assessment of prevalence, control and treatment of CVD risk factors, and monitoring of healthy behaviour and morbidity due to diseases like coronary artery disease, hypertension and diabetes is very important for health policy planning. The WOBASZ II is the newest Polish population based survey, performed in 2013-2014 to evaluate prevalence, control, treatment, and morbidity. The study was the continuation of WOBASZ (2003-2005). To describe the goals and methods of the WOBASZ II study and to present the results of the recruitment. The WOBASZ II study was planned as a cross-sectional survey of a random sample of Polish residents aged over 20 years. The selection, using the National Identity Card Registry of the Ministry of Internal Affairs, was made as a three-stage sampling, stratified according to administrative units (voivodeships), type of urbanisation (commune), and gender. The study protocol consisted of a questionnaire used in face-to-face interviews, physical examination, and blood samples. WOBASZ II was coordinated by the Department of Epidemiology, Cardiovascular Diseases Prevention and Health Promotion of the Institute of Cardiology in Warsaw in cooperation with medical universities in Gdansk, Katowice, Krakow, Lodz, and Poznan. Out of 15,120 persons, 1557 persons were not eligible. Out of eligible persons, 6170 (2760 men and 3410 women) were examined (the response rate 45.5%). The highest response rates were observed in Warminsko

  3. From bed topography to ice thickness: GlaRe, a GIS tool to reconstruct the surface of palaeoglaciers

    NASA Astrophysics Data System (ADS)

    Pellitero, Ramon; Rea, Brice; Spagnolo, Matteo; Bakke, Jostein; Ivy-Ochs, Susan; Frew, Craig; Hughes, Philip; Ribolini, Adriano; Renssen, Hans; Lukas, Sven

    2016-04-01

    We present GlaRe, A GIS tool that automatically reconstructs the 3D geometry for palaeoglaciers given the bed topography. This tool utilises a numerical approach and can work using a minimum of morphological evidence i.e. the position of the palaeoglacier front. The numerical approach is based on an iterative solution to the perfect plasticity assumption for ice rheology, explained in Benn and Hulton (2010). The tool can be run in ArcGIS 10.1 (ArcInfo license) and later updates and the toolset is written in Python code. The GlaRe toolbox presented in this paper implements a well-established approach for the determination of palaeoglacier equilibrium profiles. Significantly it permits users to quickly run multiple glacier reconstructions which were previously very laborious and time consuming (typically days for a single valley glacier). The implementation of GlaRe will facilitate the reconstruction of large numbers of palaeoglaciers which will provide opportunities for such research addressing at least two fundamental problems: 1. Investigation of the dynamics of palaeoglaciers. Glacier reconstructions are often based on a rigorous interpretation of glacial landforms but not always sufficient attention and/or time has been given to the actual reconstruction of the glacier surface, which is crucial for the calculation of palaeoglacier ELAs and subsequent derivation of quantitative palaeoclimatic data. 2. the ability to run large numbers of reconstructions and over much larger spatial areas provides an opportunity to undertake palaeoglaciers reconstructions across entire mountain, ranges, regions or even continents, allowing climatic gradients and atmospheric circulation patterns to be elucidated. The tool performance has been evaluated by comparing two extant glaciers, an icefield and a cirque/valley glacier from which the subglacial topography is known with a basic reconstruction using GlaRe. Results from the comparisons between extant glacier surfaces and modelled

  4. The Norris Survey of the Corona Borealis Supercluster. II. Galaxy Evolution with Redshift and Environment

    NASA Astrophysics Data System (ADS)

    Small, Todd A.; Sargent, Wallace L. W.; Hamilton, Donald

    1997-10-01

    We measure the field galaxy luminosity function (LF) as a function of color and redshift from z = 0 to z = 0.5 using galaxies from the Norris Survey of the Corona Borealis Supercluster. The data set consists of 603 field galaxies with 0 < z <= 0.5 and spans a wide range in apparent magnitude (14.0 <~ r <~ 21.5), although our field galaxy LF analysis is limited to 493 galaxies with r <= 20.0 mag. We use the observed g-r colors of the galaxies to compute accurate corrections to the rest BAB and r bands. We find that our local r-band LF, when normalized to counts in high galactic latitude fields, agrees well with the local LF measured in the Las Campanas Redshift Survey. Our BAB-band local LF, however, does not match the bj-band LF from the Stromlo/APM survey, having a normalization 1.6 times higher. We see compelling evidence that the BAB-band field galaxy LF evolves with redshift. The evolution is strongest for the population of star-forming galaxies with [O II] λ3727 rest-frame equivalent widths greater than 10 Å. The population of red, quiescent galaxies shows no sign of evolution to z = 0.5. The evolution of the LF that we observe is consistent with the findings of other faint galaxy redshift surveys. The fraction of galaxies with [O II] emission increases rapidly with redshift, but the fraction of galaxies with strong Hδ absorption, a signature of a burst of star formation, does not. We thus conclude that the star formation in distant galaxies is primarily long-lived. We also compute the LFs of the Corona Borealis supercluster (z ~ 0.07, 419 galaxies with 14.1 <= r <= 20.0 mag) and the Abell 2069 supercluster (z ~ 0.11, 318 galaxies with 15.1 <= r <= 20.0 mag). The shapes of the two supercluster luminosity functions are broadly similar to the shape of the local luminosity function. However, there are important differences. Both supercluster LFs have an excess of very bright galaxies. In addition, the characteristic magnitude of the Corona Borealis

  5. The Vulture Survey: Analyzing the Evolution of MgII and CIV Absorbers

    NASA Astrophysics Data System (ADS)

    Mathes, Nigel; Churchill, Christopher W.; Murphy, Michael

    2017-01-01

    We present the results of an archival VLT/UVES and Keck/HIRES quasar absorption line survey. We examine over 600 quasar lines of sight in order to inventory the cosmic properties of MgII and CIV absorbers. We employ an accurate, automated approach to line detection which consistently detects absorption lines with rest-frame equivalent widths less than 0.02 Å in S/N > 40 spectra. We determine redshift path densities, equivalent width and column density distributions, and cosmic mass densities as a function of redshift. We find that the evolution in the universal distribution of this metal absorbing gas correlates strongly with the cosmic star formation history of galaxies. We measure a significant enhancement in the comoving opacity of strong MgII and CIV absorbers around z=2. We also measure the pixel two-point velocity correlation function and find broader, higher velocity signatures around z=2. We examine possible causes for these trends, and determine that at z=2 galaxies transport significantly higher quantities of metal enriched gas into and out of their halos through star formation than at other times.

  6. Host galaxies of luminous type II AGN: Winds, shocks, and comparisons to The SAMI Galaxy Survey

    NASA Astrophysics Data System (ADS)

    McElroy, Rebecca; Croom, Scott; Pracy, Michael; SAMI Galaxy Survey Team

    2016-01-01

    We present IFS observations of luminous (log(L[O III]/L⊙) > 8.7) local (z < 0.11) type II AGN, and demonstrate that winds are ubiquitous within this sample and have a direct influence on the ISM of the host galaxies. We use both non-parametric (e.g. line width and asymmetry) and multi-Gaussian fitting to decompose the complex emission profiles close to the AGN. We find line widths containing 80% flux in the range 400 - 1600 km/s with a mean of 790 ± 90 km/s, such high velocities are strongly suggestive that these AGN are driving ionized outflows. Additionally, multi-Gaussian fitting reveals that 14/17 of our targets require 3 separate kinematic components in the ionized gas in their central regions. The broadest components of these fits have FWHM = 530 - 2520 km/s, with a mean value of 920 ± 50 km/s. By simultaneously fitting both the Hβ/[O III] and Hα/[N II] complexes we construct ionization diagnostic diagrams for each component. 13/17 of our galaxies show a significant (> 95 %) correlation between the [N II]/Hα ratio and the velocity dispersion of the gas. Such a correlation is the natural consequence of a contribution to the ionization from shock excitation and we argue that this demonstrates that the outflows from these AGN are directly impacting the surrounding ISM within the galaxies. In addition, we use stellar absorption features to measure kinematics for these AGN host galaxies and those of a control sample selected from the SAMI Galaxy Survey to search for evidence of these luminous AGN being preferentially hosted by disturbed or merging systems.

  7. A Herschel [C ii] Galactic plane survey. I. The global distribution of ISM gas components

    NASA Astrophysics Data System (ADS)

    Pineda, J. L.; Langer, W. D.; Velusamy, T.; Goldsmith, P. F.

    2013-06-01

    Context. The [C ii] 158 μm line is an important tool for understanding the life cycle of interstellar matter. Ionized carbon is present in a variety of phases of the interstellar medium (ISM), including the diffuse ionized medium, warm and cold atomic clouds, clouds in transition from atomic to molecular, and dense and warm photon dominated regions. Aims: Velocity-resolved observations of [C ii] are the most powerful technique available to disentangle the emission produced by these components. These observations can also be used to trace CO-dark H2 gas and determine the total mass of the ISM. Methods: The Galactic Observations of Terahertz C+ (GOT C+) project surveys the [C ii] 158 μm line over the entire Galactic disk with velocity-resolved observations using the Herschel/HIFI instrument. We present the first longitude-velocity maps of the [C ii] emission for Galactic latitudes b = 0°, ±0.5°, and ±1.0°. We combine these maps with those of H i, 12CO, and 13CO to separate the different phases of the ISM and study their properties and distribution in the Galactic plane. Results: [C ii] emission is mostly associated with spiral arms, mainly emerging from Galactocentric distances between 4 and 10 kpc. It traces the envelopes of evolved clouds as well as clouds that are in the transition between atomic and molecular. We estimate that most of the observed [C ii] emission is produced by dense photon dominated regions (~47%), with smaller contributions from CO-dark H2 gas (~28%), cold atomic gas (~21%), and ionized gas (~4%). Atomic gas inside the Solar radius is mostly in the form of cold neutral medium (CNM), while the warm neutral medium gas dominates the outer galaxy. The average fraction of CNM relative to total atomic gas is ~43%. We find that the warm and diffuse CO-dark H2 is distributed over a larger range of Galactocentric distances (4-11 kpc) than the cold and dense H2 gas traced by 12CO and 13CO (4-8 kpc). The fraction of CO-dark H2 to total H2 increases

  8. Characteristics and verification of a car-borne survey system for dose rates in air: KURAMA-II.

    PubMed

    Tsuda, S; Yoshida, T; Tsutsumi, M; Saito, K

    2015-01-01

    The car-borne survey system KURAMA-II, developed by the Kyoto University Research Reactor Institute, has been used for air dose rate mapping after the Fukushima Dai-ichi Nuclear Power Plant accident. KURAMA-II consists of a CsI(Tl) scintillation detector, a GPS device, and a control device for data processing. The dose rates monitored by KURAMA-II are based on the G(E) function (spectrum-dose conversion operator), which can precisely calculate dose rates from measured pulse-height distribution even if the energy spectrum changes significantly. The characteristics of KURAMA-II have been investigated with particular consideration to the reliability of the calculated G(E) function, dose rate dependence, statistical fluctuation, angular dependence, and energy dependence. The results indicate that 100 units of KURAMA-II systems have acceptable quality for mass monitoring of dose rates in the environment.

  9. The International Deep Planet Survey. II. The frequency of directly imaged giant exoplanets with stellar mass

    NASA Astrophysics Data System (ADS)

    Galicher, R.; Marois, C.; Macintosh, B.; Zuckerman, B.; Barman, T.; Konopacky, Q.; Song, I.; Patience, J.; Lafrenière, D.; Doyon, R.; Nielsen, E. L.

    2016-10-01

    Context. Radial velocity and transit methods are effective for the study of short orbital period exoplanets but they hardly probe objects at large separations for which direct imaging can be used. Aims: We carried out the international deep planet survey of 292 young nearby stars to search for giant exoplanets and determine their frequency. Methods: We developed a pipeline for a uniform processing of all the data that we have recorded with NIRC2/Keck II, NIRI/Gemini North, NICI/Gemini South, and NACO/VLT for 14 yr. The pipeline first applies cosmetic corrections and then reduces the speckle intensity to enhance the contrast in the images. Results: The main result of the international deep planet survey is the discovery of the HR 8799 exoplanets. We also detected 59 visual multiple systems including 16 new binary stars and 2 new triple stellar systems, as well as 2279 point-like sources. We used Monte Carlo simulations and the Bayesian theorem to determine that 1.05+2.80-0.70% of stars harbor at least one giant planet between 0.5 and 14 MJ and between 20 and 300 AU. This result is obtained assuming uniform distributions of planet masses and semi-major axes. If we consider power law distributions as measured for close-in planets instead, the derived frequency is 2.30+5.95-1.55%, recalling the strong impact of assumptions on Monte Carlo output distributions. We also find no evidence that the derived frequency depends on the mass of the hosting star, whereas it does for close-in planets. Conclusions: The international deep planet survey provides a database of confirmed background sources that may be useful for other exoplanet direct imaging surveys. It also puts new constraints on the number of stars with at least one giant planet reducing by a factor of two the frequencies derived by almost all previous works. Tables 11-15 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc

  10. VizieR Online Data Catalog: 2XMMi/SDSS Galaxy Cluster Survey. II. (Takey+, 2013)

    NASA Astrophysics Data System (ADS)

    Takey, A.; Schwope, A.; Lamer, G.

    2013-08-01

    We compile a sample of X-ray-selected galaxy groups and clusters from the XMM-Newton serendipitous source catalogue (2XMMi-DR3) with optical confirmation and redshift measurement from the Sloan Digital Sky Survey (SDSS). The X-ray cluster candidates were selected from the 2XMMi-DR3 catalogue in the footprint of the SDSS-DR7. We developed a finding algorithm to search for overdensities of galaxies at the positions of the X-ray cluster candidates in the photometric redshift space and to measure the redshifts of the clusters from the SDSS data. The detection algorithm provides the photometric redshift of 530 galaxy clusters. Of these, 310 clusters have a spectroscopic redshift for at least one member galaxy. About 75 percent of the optically confirmed cluster sample are newly discovered X-ray clusters. Moreover, 301 systems are known as optically selected clusters in the literature while the remainder are new discoveries in X-ray and optical bands. The optically confirmed cluster sample spans a wide redshift range 0.03-0.70 (median z=0.32). In this paper, we present the catalogue of X-ray-selected galaxy groups and clusters from the 2XMMi/SDSS galaxy cluster survey. The catalogue has two subsamples: (i) a cluster sample comprising 345 objects with their X-ray spectroscopic temperature and flux from the spectral fitting, and (ii) a cluster sample consisting of 185 systems with their X-ray flux from the 2XMMi-DR3 catalogue, because their X-ray data are insufficient for spectral fitting. The updated LX-T relation of the current sample with X-ray spectroscopic parameters is presented. We see no evidence for evolution in the slope and intrinsic scatter of the LX-T relation with redshift when excluding the low-luminosity groups (5 data files).

  11. The Unique Optical Design of the CTI-II Survey Telescope

    NASA Astrophysics Data System (ADS)

    Ackermann, Mark R.; McGraw, J. T.; MacFarlane, M.

    2006-12-01

    The CCD/Transit Instrument with Innovative Instrumentation (CTI-II) is being developed for precision ground-based astrometric and photometric astronomical observations. The 1.8m telescope will be stationary, near-zenith pointing and will feature a CCD-mosaic array operated in time-delay and integrate (TDI) mode to image a continuous strip of the sky in five bands. The heart of the telescope is a Nasmyth-like bent-Cassegrain optical system optimized to produce near diffraction-limited images with near zero distortion over a circular1.42 deg field. The optical design includes an f/2.2 parabolic ULE primary with no central hole salvaged from the original CTI telescope and adds the requisite hyperbolic secondary, a folding flat and a highly innovative all-spherical, five lens corrector which includes three plano surfaces. The reflective and refractive portions of the design have been optimized as individual but interdependent systems so that the same reflective system can be used with slightly different refractive correctors. At present, two nearly identical corrector designs are being evaluated, one fabricated from BK-7 glass and the other of fused silica. The five lens corrector consists of an air-spaced triplet separated from follow-on air-spaced doublet. Either design produces 0.25 arcsecond images at 83% encircled energy with a maximum of 0.0005% distortion. The innovative five lens corrector design has been applied to other current and planned Cassegrain, RC and super RC optical systems requiring correctors. The basic five lens approach always results in improved performance compared to the original designs. In some cases, the improvement in image quality is small but includes substantial reductions in distortion. In other cases, the improvement in image quality is substantial. Because the CTI-II corrector is designed for a parabolic primary, it might be especially useful for liquid mirror telescopes. We describe and discuss the CTI-II optical design with respect

  12. Urinary cadmium and blood pressure: results from the NHANES II survey.

    PubMed Central

    Whittemore, A S; DiCiccio, Y; Provenzano, G

    1991-01-01

    Relationships between urinary cadmium levels and blood pressure were examined in a sample of 951 adult men and women who participated in the Second National Health and Nutritional Examination Survey (NHANES II). Among all participants, positive relationships were seen between urinary cadmium levels and both systolic and diastolic blood pressure (p less than 0.05 and p less than 0.01, respectively), after adjusting for age, sex, race, relative body weight, smoking status, and hypertensive medication use. However, analyses for subgroups determined by sex and smoking status were inconsistent. Among current smokers, urinary cadmium levels were significantly positively associated with both systolic and diastolic blood pressure for women, and with diastolic blood pressure for men. Yet among former smokers and lifelong nonsmokers of both sexes, urinary cadmium was not significantly associated with either systolic or diastolic blood pressure. Evidence that some hypertensive medications increase urinary cadmium excretion suggests that the positive associations seen among current smokers may reflect high urinary cadmium levels among hypertensives induced by hypertensive treatment. After treated hypertensives were removed from the analysis, regression coefficients relating blood pressure to cadmium dropped by a factor of two and lost statistical significance. We conclude that the present data provide little support for a causal association between systemic cadmium and hypertension at nonoccupational exposure levels. Further, conflicting results of previous studies may reflect failure to control adequately for age, smoking status, and hypertensive treatment. PMID:2040243

  13. A Deep Multicolor Survey. II. Initial Spectroscopy and Comparison with Expected Quasar Number Counts: Erratum

    NASA Astrophysics Data System (ADS)

    Hall, Patrick B.; Osmer, Patrick S.; Green, Richard F.; Porter, Alain C.; Warren, Stephen J.

    1996-11-01

    In the paper "A Deep Multicolor Survey. II. Initial Spectroscopy and Comparison with Expected Quasar Number Counts" by Patrick B. Hall, Patrick S. Osmer, Richard F. Green, Alain C. Porter, and Stephen J. Warren (ApJ, 462,614 [1996]), some of the figures were inadvertently printed with poor resolution. The full information conveyed in the images is thus difficult to perceive. Here we present high-resolution versions of the affected figures (Fig. 1 and Figs. 10-15). In all diagrams, objects from the catalog are plotted as error bars, with only half the full error bars plotted, for clarity. Error ban extending off the diagram indicate upper limits. Spectroscopically confirmed quasars, compact narrow emission-line galaxies (CNELGs), and stars are plotted as filled boxes, open boxes, and inverted triangles, respectively. Spectroscopically observed but unidentified candidates are plotted as crosses and simulated quasar colors as dots. The line of simulated quasar points at U- V = 3.0 in Figure 11a and the similar lines in other color-color diagrams indicate that the simulated colors are lower limits. The reader should also note that Figures 16b and 16c were incorrectly switched with each other in the paper.

  14. Thermal and optical design analyses, optimizations, and experimental verification for a novel glare-free LED lamp for household applications.

    PubMed

    Khan, M Nisa

    2015-07-20

    Light-emitting diode (LED) technologies are undergoing very fast developments to enable household lamp products with improved energy efficiency and lighting properties at lower cost. Although many LED replacement lamps are claimed to provide similar or better lighting quality at lower electrical wattage compared with general-purpose incumbent lamps, certain lighting characteristics important to human vision are neglected in this comparison, which include glare-free illumination and omnidirectional or sufficiently broad light distribution with adequate homogeneity. In this paper, we comprehensively investigate the thermal and lighting performance and trade-offs for several commercial LED replacement lamps for the most popular Edison incandescent bulb. We present simulations and analyses for thermal and optical performance trade-offs for various LED lamps at the chip and module granularity levels. In addition, we present a novel, glare-free, and production-friendly LED lamp design optimized to produce very desirable light distribution properties as demonstrated by our simulation results, some of which are verified by experiments.

  15. A Survey of Optometry Graduates to Determine Practice Patterns: Part II: Licensure and Practice Establishment Experiences.

    ERIC Educational Resources Information Center

    Bleimann, Robert L.; Smith, Lee W.

    1985-01-01

    A summary of Part II of a two-volume study of optometry graduates conducted by the Association of Schools and Colleges of Optometry is presented. Part II includes the analysis of the graduates' licensure and practice establishment experiences. (MLW)

  16. The New Zealand workforce survey II: occupational risk factors for asthma.

    PubMed

    Eng, Amanda; 'T Mannetje, Andrea; Douwes, Jeroen; Cheng, Soo; McLean, Dave; Ellison-Loschmann, Lis; Pearce, Neil

    2010-03-01

    We conducted a cross-sectional population-based survey in New Zealand that collected information on work history, current workplace exposures, and selected health outcomes. We report here the findings on occupational risk factors for asthma symptoms. A random sample of men and women aged 20-64 years were selected from the New Zealand Electoral Roll and invited to take part in a telephone survey. Current asthma was defined as: (i) woken up by shortness of breath in the past 12 months; or (ii) an attack of asthma in the past 12 months; or (iii) currently taking asthma medication. Adult-onset asthma was defined as first attack of asthma at age 18 or over. Prevalence odds ratios (ORs) for all occupations were calculated using logistic regression adjusting for sex, age, smoking, and deprivation. Totally, 2903 participants were included in the analyses. The prevalence of current asthma was 17% and the prevalence of adult-onset asthma was 9%. Prevalence ORs for current asthma were elevated for ever working as a printer [OR = 2.26; 95% confidence interval (CI) = 1.09-4.66], baker (OR = 1.98; 95% CI = 1.02-3.85), sawmill labourer (OR = 3.26; 95% CI = 1.05-10.16), metal processing plant operator (OR = 2.48; 95% CI = 1.22-5.05), and cleaner (OR = 1.60; 95% CI = 1.09-2.35). Excess risks of adult-onset asthma were also found for ever working as a printer, baker, and sawmill labourer as well as ever-working as a market-oriented animal producer (OR = 1.66; 95% CI = 1.14-2.41), and other agricultural worker (OR = 2.08; 95% CI = 1.03-4.20). A number of occupations not previously considered at high risk for asthma were also identified, including teachers and certain sales professionals. This population-based study has confirmed findings of previous international studies showing elevated risks in a number of high-risk occupations. The strongest risks were consistently observed for printers, bakers, and sawmill labourers. Several occupations were also identified that have not been

  17. Survey of non-linear hydrodynamic models of type-II Cepheids

    NASA Astrophysics Data System (ADS)

    Smolec, R.

    2016-03-01

    We present a grid of non-linear convective type-II Cepheid models. The dense model grids are computed for 0.6 M⊙ and a range of metallicities ([Fe/H] = -2.0, -1.5, -1.0), and for 0.8 M⊙ ([Fe/H] = -1.5). Two sets of convective parameters are considered. The models cover the full temperature extent of the classical instability strip, but are limited in luminosity; for the most luminous models, violent pulsation leads to the decoupling of the outermost model shell. Hence, our survey reaches only the shortest period RV Tau domain. In the Hertzsprung-Russell diagram, we detect two domains in which period-doubled pulsation is possible. The first extends through the BL Her domain and low-luminosity W Vir domain (pulsation periods ˜2-6.5 d). The second domain extends at higher luminosities (W Vir domain; periods >9.5 d). Some models within these domains display period-4 pulsation. We also detect very narrow domains (˜10 K wide) in which modulation of pulsation is possible. Another interesting phenomenon we detect is double-mode pulsation in the fundamental mode and in the fourth radial overtone. Fourth overtone is a surface mode, trapped in the outer model layers. Single-mode pulsation in the fourth overtone is also possible on the hot side of the classical instability strip. The origin of the above phenomena is discussed. In particular, the role of resonances in driving different pulsation dynamics as well as in shaping the morphology of the radius variation curves is analysed.

  18. The IMACS Cluster Building Survey. II. Spectral Evolution of Galaxies in the Epoch of Cluster Assembly

    NASA Astrophysics Data System (ADS)

    Dressler, Alan; Oemler, Augustus, Jr.; Poggianti, Bianca M.; Gladders, Michael D.; Abramson, Louis; Vulcani, Benedetta

    2013-06-01

    The IMACS Cluster Building Survey (ICBS) provides spectra of ~2200 galaxies 0.31 < z < 0.54 in five rich clusters (R <~ 5 Mpc) and the field. Infalling, dynamically cold groups with tens of members account for approximately half of the supercluster population, contributing to a growth in cluster mass of ~100% by the present day. The ICBS spectra distinguish non-star-forming (PAS) and poststarburst (PSB) from star-forming galaxies—continuously star-forming (CSF) or starbursts (SBH or SBO), identified by anomalously strong Hδ absorption or [O II] emission. For the infalling cluster groups and similar field groups, we find a correlation between PAS+PSB fraction and group mass, indicating substantial "preprocessing" through quenching mechanisms that can turn star-forming galaxies into passive galaxies without the unique environment of rich clusters. SBH + SBO starburst galaxies are common, and they maintain an approximately constant ratio (SBH+SBO)/CSF ≈ 25% in all environments—from field, to groups, to rich clusters. Similarly, while PSB galaxies strongly favor denser environments, PSB/PAS ≈ 10%-20% for all environments. This result, and their timescale τ ~ 500 Myr, indicates that starbursts are not signatures of a quenching mechanism that produces the majority of passive galaxies. We suggest instead that starbursts and poststarbursts signal minor mergers and accretions, in star-forming and passive galaxies, respectively, and that the principal mechanisms for producing passive systems are (1) early major mergers, for elliptical galaxies, and (2) later, less violent processes—such as starvation and tidal stripping, for S0 galaxies. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.

  19. THE IMACS CLUSTER BUILDING SURVEY. II. SPECTRAL EVOLUTION OF GALAXIES IN THE EPOCH OF CLUSTER ASSEMBLY

    SciTech Connect

    Dressler, Alan; Oemler, Augustus Jr.; Poggianti, Bianca M.; Vulcani, Benedetta; Gladders, Michael D.; Abramson, Louis

    2013-06-10

    The IMACS Cluster Building Survey (ICBS) provides spectra of {approx}2200 galaxies 0.31 < z < 0.54 in five rich clusters (R {approx}< 5 Mpc) and the field. Infalling, dynamically cold groups with tens of members account for approximately half of the supercluster population, contributing to a growth in cluster mass of {approx}100% by the present day. The ICBS spectra distinguish non-star-forming (PAS) and poststarburst (PSB) from star-forming galaxies-continuously star-forming (CSF) or starbursts (SBH or SBO), identified by anomalously strong H{delta} absorption or [O II] emission. For the infalling cluster groups and similar field groups, we find a correlation between PAS+PSB fraction and group mass, indicating substantial ''preprocessing'' through quenching mechanisms that can turn star-forming galaxies into passive galaxies without the unique environment of rich clusters. SBH + SBO starburst galaxies are common, and they maintain an approximately constant ratio (SBH+SBO)/CSF Almost-Equal-To 25% in all environments-from field, to groups, to rich clusters. Similarly, while PSB galaxies strongly favor denser environments, PSB/PAS Almost-Equal-To 10%-20% for all environments. This result, and their timescale {tau} {approx} 500 Myr, indicates that starbursts are not signatures of a quenching mechanism that produces the majority of passive galaxies. We suggest instead that starbursts and poststarbursts signal minor mergers and accretions, in star-forming and passive galaxies, respectively, and that the principal mechanisms for producing passive systems are (1) early major mergers, for elliptical galaxies, and (2) later, less violent processes-such as starvation and tidal stripping, for S0 galaxies.

  20. The Effect of Host Galaxies on Type Ia Supernovae in the SDSS-II Supernova Survey

    SciTech Connect

    Lampeitl, Hubert; Smith, Mathew; Nichol, Robert C.; Bassett, Bruce; Cinabro, David; Dilday, Benjamin; Foley, Ryan J.; Frieman, Joshua A.; Garnavich, Peter M.; Goobar, Ariel; Im, Myungshin; /Seoul Natl. U. /Rutgers U., Piscataway

    2010-05-01

    We present an analysis of the host galaxy dependencies of Type Ia Supernovae (SNe Ia) from the full three year sample of the SDSS-II Supernova Survey. We re-discover, to high significance, the strong correlation between host galaxy type and the width of the observed SN light curve, i.e., fainter, quickly declining SNe Ia favor passive host galaxies, while brighter, slowly declining Ia's favor star-forming galaxies. We also find evidence (at between 2 to 3{sigma}) that SNe Ia are {approx_equal} 0.1 magnitudes brighter in passive host galaxies, than in star-forming hosts, after the SN Ia light curves have been standardized using the light curve shape and color variations: This difference in brightness is present in both the SALT2 and MCLS2k2 light curve fitting methodologies. We see evidence for differences in the SN Ia color relationship between passive and star-forming host galaxies, e.g., for the MLCS2k2 technique, we see that SNe Ia in passive hosts favor a dust law of R{sub V} {approx_equal} 1, while SNe Ia in star-forming hosts require R{sub V} {approx} 2. The significance of these trends depends on the range of SN colors considered. We demonstrate that these effects can be parameterized using the stellar mass of the host galaxy (with a confidence of > 4{sigma}) and including this extra parameter provides a better statistical fit to our data. Our results suggest that future cosmological analyses of SN Ia samples should include host galaxy information.

  1. A COMPLETE ATLAS OF H I ABSORPTION TOWARD H II REGIONS IN THE SOUTHERN GALACTIC PLANE SURVEY (SGPS I)

    SciTech Connect

    Brown, C.; Dickey, J. M.; Dawson, J. R.; McClure-Griffiths, N. M.

    2014-04-01

    We present a complete catalog of H I emission and absorption spectrum pairs, toward H II regions, detectable within the boundaries of the Southern Galactic Plane Survey (SGPS I), a total of 252 regions. The catalog is presented in graphical, numerical, and summary formats. We demonstrate an application of this new data set through an investigation of the locus of the Near 3 kpc Arm.

  2. Field Surveys, IOC Valleys. Volume III, Part II. Cultural Resources Survey, Pine and Wah Wah Valleys, Utah.

    DTIC Science & Technology

    1981-08-01

    including horse, camel, mammoth, Ertm E-TR-48-III-II 20 musk ox, and certain species of bison, goat, and bear, which had previously inhabited the marsh and...34 - - -9,$.. 𔄃 Im I I I Si to * Location lype/Contents Affiliation 42B@644 rid e over cr ek - P/J depression, cleared areas, Fr elon (f4-5-18-92) ground

  3. The Alabama Adolescent Health Survey: Health Knowledge and Behaviors. Summary Report II.

    ERIC Educational Resources Information Center

    Nagy, Stephen; Adcock, Anthony

    This survey is a follow-up to a comprehensive survey of eighth- and tenth-grade public school students conducted in 1988. The 1990 sample includes over 3,400 students from rural, metropolitan, and mixed school districts. Data were collected using a 120-item questionnaire and compared to available information from the 1988 survey. The study…

  4. National databases and rheumatology research II: the National Health and Nutrition Examination Surveys.

    PubMed

    Sokka, Tuulikki; Krishnan, Eswar

    2004-11-01

    Three National Health and Nutrition Examination Surveys were conducted in the United States between 1971 and 1994 to provide data on the nutritional and health status of the population and on specific target conditions. This article describes features of the surveys and provides examples of research on musculoskeletal disorders that used the survey data.

  5. Preliminary evaluation of discomfort glare from organic light-emitting diode and edge-lit light-emitting diode lighting panels

    NASA Astrophysics Data System (ADS)

    Mou, Xi; Freyssinier, Jean Paul; Narendran, Nadarajah; Bullough, John D.

    2017-05-01

    The organic light-emitting diode (OLED) is an area light source, and its primary competing technology is the edge-lit light-emitting diode (LED) panel. Both technologies are similar in shape and appearance, but there is little understanding of how people perceive discomfort glare (DG) from area sources. The objective of this study was to evaluate the DG of these two technologies under similar operating conditions. Additionally, two existing DG models were compared to evaluate the correlation between predicted values and observed values. In an earlier study, we found no statistically significant difference in human response in terms of DG between OLED and edge-lit LED panels when the two sources produced the same luminous stimulus. The range of testing stimulus was expanded to test different panel luminances at three background illuminations. The results showed no difference in perceived glare between the panels, and, as the background illumination increased, the perceived glare decreased. In other words, both appeared equally glary beyond a certain luminance and background illumination. We then compared two existing glare models with the observed values and found that one model showed a good estimation of how humans perceive DG. That model was further modified to increase its power.

  6. CALIFA, the Calar Alto Legacy Integral Field Area survey. II. First public data release

    NASA Astrophysics Data System (ADS)

    Husemann, B.; Jahnke, K.; Sánchez, S. F.; Barrado, D.; Bekerait*error*ė, S.; Bomans, D. J.; Castillo-Morales, A.; Catalán-Torrecilla, C.; Cid Fernandes, R.; Falcón-Barroso, J.; García-Benito, R.; González Delgado, R. M.; Iglesias-Páramo, J.; Johnson, B. D.; Kupko, D.; López-Fernandez, R.; Lyubenova, M.; Marino, R. A.; Mast, D.; Miskolczi, A.; Monreal-Ibero, A.; Gil de Paz, A.; Pérez, E.; Pérez, I.; Rosales-Ortega, F. F.; Ruiz-Lara, T.; Schilling, U.; van de Ven, G.; Walcher, J.; Alves, J.; de Amorim, A. L.; Backsmann, N.; Barrera-Ballesteros, J. K.; Bland-Hawthorn, J.; Cortijo, C.; Dettmar, R.-J.; Demleitner, M.; Díaz, A. I.; Enke, H.; Florido, E.; Flores, H.; Galbany, L.; Gallazzi, A.; García-Lorenzo, B.; Gomes, J. M.; Gruel, N.; Haines, T.; Holmes, L.; Jungwiert, B.; Kalinova, V.; Kehrig, C.; Kennicutt, R. C.; Klar, J.; Lehnert, M. D.; López-Sánchez, Á. R.; de Lorenzo-Cáceres, A.; Mármol-Queraltó, E.; Márquez, I.; Mendez-Abreu, J.; Mollá, M.; del Olmo, A.; Meidt, S. E.; Papaderos, P.; Puschnig, J.; Quirrenbach, A.; Roth, M. M.; Sánchez-Blázquez, P.; Spekkens, K.; Singh, R.; Stanishev, V.; Trager, S. C.; Vilchez, J. M.; Wild, V.; Wisotzki, L.; Zibetti, S.; Ziegler, B.

    2013-01-01

    We present the first public data release (DR1) of the Calar Alto Legacy Integral Field Area (CALIFA) survey. It consists of science-grade optical datacubes for the first 100 of eventually 600 nearby (0.005 < z < 0.03) galaxies, obtained with the integral-field spectrograph PMAS/PPak mounted on the 3.5 m telescope at the Calar Alto observatory. The galaxies in DR1 already cover a wide range of properties in color-magnitude space, morphological type, stellar mass, and gas ionization conditions. This offers the potential to tackle a variety of open questions in galaxy evolution using spatially resolved spectroscopy. Two different spectral setups are available for each galaxy, (i) a low-resolution V500 setup covering the nominal wavelength range 3745-7500 Å with a spectral resolution of 6.0 Å (FWHM), and (ii) a medium-resolution V1200 setup covering the nominal wavelength range 3650-4840 Å with a spectral resolution of 2.3 Å (FWHM). We present the characteristics and data structure of the CALIFA datasets that should be taken into account for scientific exploitation of the data, in particular the effects of vignetting, bad pixels and spatially correlated noise. The data quality test for all 100 galaxies showed that we reach a median limiting continuum sensitivity of 1.0 × 10-18 erg s-1 cm-2 Å-1 arcsec-2 at 5635 Å and 2.2 × 10-18 erg s-1 cm-2 Å-1 arcsec-2 at 4500 Å for the V500 and V1200 setup respectively, which corresponds to limiting r and g band surface brightnesses of 23.6 mag arcsec-2 and 23.4 mag arcsec-2, or an unresolved emission-line flux detection limit of roughly 1 × 10-17 erg s-1 cm-2 arcsec-2 and 0.6 × 10-17 erg s-1 cm-2 arcsec-2, respectively. The median spatial resolution is 3farcs7, and the absolute spectrophotometric calibration is better than 15% (1σ). We also describe the available interfaces and tools that allow easy access to this first publicCALIFA data at http://califa.caha.es/DR1 Based on observations collected at the Centro Astron

  7. A facile fabrication of light diffusing film with LDP/polyacrylates composites coating for anti-glare LED application

    NASA Astrophysics Data System (ADS)

    Song, Shisen; Sun, Yaojie; Lin, Yandan; You, Bo

    2013-05-01

    In this paper, we present a facile coating technique to fabricate the light diffusing film with hemispherical surface convex micro-structure. The coating was prepared by different ratio of light-diffusing particles (LDP)/polyacrylates composites via in situ radical polymerization, with the H2SO4 and vinyl triethoxysilane (A-151) pretreatment made the LDP better dispersed and incorporated with polyacrylate polymer chains. When the mass ratio (LDP/polyacrylate) was 0.5, the film obtained the highest light-diffusing effect and more than 90% transmittance due to the formation of hemispherical surface convex micro-structure. The light diffusing films have excellent anti-glare property if applied to LED light system.

  8. Candidate type II quasars at 2 < z < 4.3 in the Sloan Digital Sky Survey III

    NASA Astrophysics Data System (ADS)

    Alexandroff, Rachael; Strauss, Michael A.; Greene, Jenny E.; Zakamska, Nadia L.; Ross, Nicholas P.; Brandt, W. N.; Liu, Guilin; Smith, Paul S.; Ge, Jian; Hamann, Fred; Myers, Adam D.; Petitjean, Patrick; Schneider, Donald P.; Yesuf, Hassen; York, Donald G.

    2013-11-01

    At low redshifts, dust-obscured quasars often have strong yet narrow permitted lines in the rest-frame optical and ultraviolet, excited by the central active nucleus, earning the designation type II quasars. We present a sample of 145 candidate type II quasars at redshifts between 2 and 4.3, encompassing the epoch at which quasar activity peaked in the universe. These objects, selected from the quasar sample of the Baryon Oscillation Spectroscopic Survey of the Sloan Digital Sky Survey III, are characterized by weak continuum in the rest-frame ultraviolet (typical continuum magnitude of i ≈ 22) and strong lines of C IV and Lyα, with full width at half-maximum less than 2000 km s-1. The continuum magnitudes correspond to an absolute magnitude of -23 or brighter at redshift 3, too bright to be due exclusively to the host galaxies of these objects. Roughly one third of the objects are detected in the shorter wavelength bands of the Wide-Field Infrared Survey Explorer survey; the spectral energy distributions of these objects appear to be intermediate between classic type I and type II quasars seen at lower redshift. Five objects are detected at rest frame 6 μm by Spitzer, implying bolometric luminosities of several times 1046 erg s-1. We have obtained polarization measurements for two objects; they are roughly 3 per cent polarized. We suggest that these objects are luminous quasars, with modest dust extinction (AV ˜ 0.5 mag), whose ultraviolet continuum also includes a substantial scattering contribution. Alternatively, the line of sight to the central engines of these objects may be obscured by optically thick material whose covering fraction is less than unity.

  9. Differentiating between Bipolar Disorder types I and II: results from the National Epidemiologic Survey on Alcohol and Related Conditions (NESARC).

    PubMed

    Bega, Sivan; Schaffer, Ayal; Goldstein, Benjamin; Levitt, Anthony

    2012-04-01

    Bipolar Disorder I (BD I) and Bipolar Disorder II (BD II) vary considerably, with differences in symptomatology, management and prognosis. For patients with depression, the distinction between BD I and BD II is not always apparent, and hinges on the differentiation between manic/mixed and hypomanic episodes. Other putative differences between patients with BD I and II exist and may assist in distinguishing between these two conditions. Data were obtained from the National Epidemiological Survey on Alcohol and Related Conditions. A total of 1429 subjects were included in our analysis based on DSM-IV criteria, 935 with BD I and 494 with BD II. We examined for differences in a number of variables including demographics, clinical features, depressive symptoms, and co-morbid conditions using t-tests and chi-square analyses for a comparison of means as well as a logistic regression for variables found to be significant. Key differences between BD I and BD II were identified in all categories in our comparison of means. In the regression analysis, a number of variables were determined to be predictors of BD I, including unemployment (OR=0.6), taking medications for depression (OR=1.7), a history of a suicide attempt (OR=1.8), depressive symptoms such as weight gain (OR=1.7), fidgeting (OR=1.5), feelings of worthlessness (OR=1.6) and difficulties with responsibilities (OR=2.2), as well as the presence of specific phobias (OR=1.8) and Cluster C traits (OR=1.4). Our results indicate that in addition to the differences between manic/mixed and hypomanic episodes, other significant differences exist that may be used to help differentiate BD I from BD II. Copyright © 2011 Elsevier B.V. All rights reserved.

  10. The Isan Culture Maintenance and Revitalisation Programme's Multilingual Signage Attitude Survey: Phase II

    ERIC Educational Resources Information Center

    Draper, John

    2016-01-01

    This article contextualises and presents to the academic community the full dataset of the Isan Culture Maintenance and Revitalisation Programme's (ICMRP) multilingual signage survey. The ICMRP is a four-year European Union co-sponsored project in Northeast Thailand. This article focuses on one aspect of the project, four surveys each of 1,500…

  11. What's for Lunch? II. A 1990 Survey of Options in the School Lunch Program.

    ERIC Educational Resources Information Center

    Morris, Patricia McGrath; And Others

    This report provides information on the content of school lunches offered to middle school children in the public schools. A total of 163 middle schools in 42 states responded to the school lunch survey. Survey findings are given on: (1) the contents of the main course, vegetable and fruit offerings, desserts, and beverages; and (2) lunches…

  12. The Isan Culture Maintenance and Revitalisation Programme's Multilingual Signage Attitude Survey: Phase II

    ERIC Educational Resources Information Center

    Draper, John

    2016-01-01

    This article contextualises and presents to the academic community the full dataset of the Isan Culture Maintenance and Revitalisation Programme's (ICMRP) multilingual signage survey. The ICMRP is a four-year European Union co-sponsored project in Northeast Thailand. This article focuses on one aspect of the project, four surveys each of 1,500…

  13. Waves Forecasters in World War II (with a Brief Survey of Other Women Meteorologists in World War II).

    NASA Astrophysics Data System (ADS)

    Lewis, J. M.

    1995-11-01

    Out of the nearly 6000 U.S. military officers who were trained to be weather forecasters during World War II, there wore approximately 100 women. They were recruited into the Women Accepted for Volunteer Emergency Service (WAVES) by the U.S. Navy and underwent training with the military men in the so-called cadet program. Letters of reminiscence from six WAVES forecasters are combined with official navy correspondence, archival information from universities, and newspaper articles of the period to reconstruct the recruitment, training, duty assignments, and postwar careers of these women.With limited information, an effort has also been made to document the training of civilian women in the cadet program, and to estimate the number of women who served as forecasters in foreign countries during the war. The status of women in meteorology prior to the United States' entry into the war is examined as a backdrop to the study. Principal results of the study are as follows:1) The recruitment of WAVES forecasters was in response to extreme shortages of weather officers at the Naval Air Stations (NAS) in early 1943 as the war escalated.2) Those recruited to be WAVES forecasters had previous experience as math/science teachers and had a lower than average attrition rate in the demanding cadet program.3) The WAVES were assigned as NAS forecasters stateside, and there is some evidence that they were differentially treated in comparison to the male naval forecasters.4) In addition to the women forecasters in the WAVES, approximately 50 civilian women were trained in the cadet program under the sponsorship of the Civilian Aeronautics Administration and the U.S. Weather Bureau; England also recruited an estimated 50 women into weather forecasting during the latter stages of WWII.5) Of the 200 women who were trained to be forecasters, it is estimated that less than 10% remained in meteorology.

  14. Type-II AGN population from the zCOSMOS survey

    NASA Astrophysics Data System (ADS)

    Bongiorno, A.; Mignoli, M.; Zamorani, G.; Zcosmos Team

    2008-10-01

    I'll present the first results on the type-II AGN population isolated from the zCOSMOS bright sample which consists of 10k sources, purely magnitude selected at I=22.5. The selected type-II AGN sample consists of about 200 AGN, selected using the diagnostic diagrams up to redshift ~1.0. I'll present the properties of this sample (i.e. SED and morphology) and some preliminary results on the evolution of type-II AGN, as well as on the evolution of their fraction with respect to the total AGN population (Type-I + Type-II), as a function of both luminosity and redshift.

  15. VizieR Online Data Catalog: VVV survey Galactic Bulge Pop. II Cepheids (Bhardwaj+, 2017)

    NASA Astrophysics Data System (ADS)

    Bhardwaj, A.; Rejkuba, M.; Minniti, D.; Surot, F.; Valenti, E.; Zoccali, M.; Gonzalez, O. A.; Romaniello, M.; Kanbur, S. M.; Singh, H. P.

    2017-07-01

    We present a combined OGLE-III and VVV catalogue with periods, classification, mean magnitudes and extinction for 264 Galactic bulge population II Cepheids having good-quality Ks-band light curves. (1 data file).

  16. Aerial radiometric and magnetic survey: Marysvale detail survey, Richfield National Topographic Map sheet, Utah. Volume II. Radiometric multi-variable stacked profile data. Final report

    SciTech Connect

    Not Available

    1982-01-01

    The results of the analyses of a systematic airborne gamma radiation and total magnetic survey for the area identified as Marysvale, located in southwestern Utah, is presented in Volumes I-IV of this report. The airborne data gathered is reduced by ground computer facilities to yield profile plots of the equivalent uranium, thorium and potassium gamma radiation intensities, the ratios of these intensities, the total gamma radiation counting rate and the earth's residual magnetic field intensity. Profile plots of the aircraft's altitude above the earth's surface, the ambient temperature and pressure, and the magnetic field data measured by a base station magnetometer is presented also. An evaluation of the distribution of the radiometric data in terms of its established geochemical map units, which were derived via geochemical analysis methods, for the entire survey area has been prepared and is included. The determination of the geochemical units presented has been established principally from the analysis of the radiometric and magnetic contour maps and, more importantly, the multi-variate analysis map. A general description of the area, including descriptions of the various geologic and geochemical units, is included within the text. Volume II contains the 10-variable radiometric stacked profile data for the entire survey area.

  17. The Diesel Exhaust in Miners Study: II. Exposure Monitoring Surveys and Development of Exposure Groups

    PubMed Central

    Coble, Joseph B.; Stewart, Patricia A.; Vermeulen, Roel; Yereb, Daniel; Stanevich, Rebecca; Blair, Aaron; Silverman, Debra T.; Attfield, Michael

    2010-01-01

    Air monitoring surveys were conducted between 1998 and 2001 at seven non-metal mining facilities to assess exposure to respirable elemental carbon (REC), a component of diesel exhaust (DE), for an epidemiologic study of miners exposed to DE. Personal exposure measurements were taken on workers in a cross-section of jobs located underground and on the surface. Air samples taken to measure REC were also analyzed for respirable organic carbon (ROC). Concurrent measurements to assess exposure to nitric oxide (NO) and nitrogen dioxide (NO2), two gaseous components of DE, were also taken. The REC measurements were used to develop quantitative estimates of average exposure levels by facility, department, and job title for the epidemiologic analysis. Each underground job was assigned to one of three sets of exposure groups from specific to general: (i) standardized job titles, (ii) groups of standardized job titles combined based on the percentage of time in the major underground areas, and (iii) larger groups based on similar area carbon monoxide (CO) air concentrations. Surface jobs were categorized based on their use of diesel equipment and proximity to DE. A total of 779 full-shift personal measurements were taken underground. The average REC exposure levels for underground jobs with five or more measurements ranged from 31 to 58 μg m−3 at the facility with the lowest average exposure levels and from 313 to 488 μg m−3 at the facility with the highest average exposure levels. The average REC exposure levels for surface workers ranged from 2 to 6 μg m−3 across the seven facilities. There was much less contrast in the ROC compared with REC exposure levels measured between surface and underground workers within each facility, as well as across the facilities. The average ROC levels underground ranged from 64 to 195 μg m−3, while on the surface, the average ROC levels ranged from 38 to 71 μg m−3 by facility, an ∼2- to 3-fold difference. The average NO and

  18. Predictors of BMI Vary along the BMI Range of German Adults - Results of the German National Nutrition Survey II.

    PubMed

    Moon, Kilson; Krems, Carolin; Heuer, Thorsten; Roth, Alexander; Hoffmann, Ingrid

    2017-01-01

    The objective of the study was to identify predictors of BMI in German adults by considering the BMI distribution and to determine whether the association between BMI and its predictors varies along the BMI distribution. The sample included 9,214 adults aged 18-80 years from the German National Nutrition Survey II (NVS II). Quantile regression analyses were conducted to examine the association between BMI and the following predictors: age, sports activities, socio-economic status (SES), healthy eating index-NVS II (HEI-NVS II), dietary knowledge, sleeping duration and energy intake as well as status of smoking, partner relationship and self-reported health. Age, SES, self-reported health status, sports activities and energy intake were the strongest predictors of BMI. The important outcome of this study is that the association between BMI and its predictors varies along the BMI distribution. Especially, energy intake, health status and SES were marginally associated with BMI in normal-weight subjects; this relationships became stronger in the range of overweight, and were strongest in the range of obesity. Predictors of BMI and the strength of these associations vary across the BMI distribution in German adults. Consequently, to identify predictors of BMI, the entire BMI distribution should be considered. © 2017 The Author(s) Published by S. Karger GmbH, Freiburg.

  19. Molecular clouds and star formation in the inner galaxy - A comparison of CO, H II, and far-infrared surveys

    NASA Technical Reports Server (NTRS)

    Myers, P. C.; Dame, T. M.; Thaddeus, P.; Cohen, R. S.; Silverberg, R. F.; Dwek, E.; Hauser, M. G.

    1986-01-01

    Surveys of the galactic plane over galactic latitudes from -1 degree to +1 degree and galactic longitudes from 12 degrees to 60 degrees are compared in the CO line at 2.6 mm, in the far-infrared (FIR) continuum at 150 micrometers and 250 micrometers, and in the radio continuum and H 110-alpha recombination line at 6 cm. The main purposes are to determine the degree of association between FIR sources, H II regions, and molecular clouds in the first quadrant and to describe and analyze the stellar content of these molecular clouds. Among the conclusions it is noted that most FIR sources coincide with HII regions, and nearly all H II regions coincide with molecular clouds, and that clouds in the inner galaxy are probably several tens of millions of years old and may have been producing O stars for only about the most recent 20 percent of their lives.

  20. Garrison-Taft 500 KV Transmission Project : Phase II Hunter Survey Final Report.

    SciTech Connect

    Allen, Steward D.

    1989-07-01

    This report presents the results of the Phase 2 survey of hunters conducted to assess the impacts of Bonneville Power Administration's 500-kV transmission line on elk hunting opportunities in western Montana. The survey is the second in a series of three; a baseline study was conducted in 1983 before the line was constructed and a mail survey will be conducted in 1987. The three surveys form the social component of the Elk Monitoring and Mitigation Project being conducted by several state and federal agencies. A report prepared by the Montana Department of Fish, Wildlife and Parks contains background information on the transmission line and entire monitoring effort, a description of the two primary study areas, and progress on the biological component of the study. 2 refs., 4 tabs.

  1. Galactic bulge population II Cepheids in the VVV survey: period-luminosity relations and a distance to the Galactic centre

    NASA Astrophysics Data System (ADS)

    Bhardwaj, A.; Rejkuba, M.; Minniti, D.; Surot, F.; Valenti, E.; Zoccali, M.; Gonzalez, O. A.; Romaniello, M.; Kanbur, S. M.; Singh, H. P.

    2017-09-01

    Context. Multiple stellar populations of different ages and metallicities reside in the Galactic bulge that trace its structure and provide clues to its formation and evolution. Aims: We present the near-infrared observations of population II Cepheids in the Galactic bulge from VISTA Variables in the Vía Láctea (VVV) survey. The JHKs photometry together with optical data from Optical Gravitational Lensing Experiment (OGLE) survey provide an independent estimate of the distance to the Galactic centre. The old, metal-poor and low-mass population II Cepheids are also investigated as useful tracers for the structure of the Galactic bulge. Methods: We identify 340 population II Cepheids in the VVV survey Galactic bulge catalogue based on their match with the OGLE-III Catalogue. The single-epoch JH and multi-epoch Ks observations complement the accurate periods and optical (VI) mean-magnitudes from OGLE. The sample consisting of BL Herculis and W Virginis subtypes is used to derive period-luminosity relations after correcting mean-magnitudes for the extinction. Our Ks-band period-luminosity relation, Ks = -2.189(0.056) [log (P)-1] + 11.187(0.032), is consistent with published work for BL Herculis and W Virginis variables in the Large Magellanic Cloud. Results: We present a combined OGLE-III and VVV catalogue with periods, classification, mean magnitudes, and extinction for 264 Galactic bulge population II Cepheids that have good-quality Ks-band light curves. The absolute magnitudes for population II Cepheids and RR Lyraes calibrated using Gaia and Hubble Space Telescope parallaxes, together with calibrated magnitudes for Large Magellanic Cloud population II Cepheids, are used to obtain a distance to the Galactic centre, R0 = 8.34 ± 0.03(stat.) ± 0.41(syst.), which changes by with different extinction laws. While noting the limitation of small number statistics, we find that the present sample of population II Cepheids in the Galactic bulge shows a nearly spheroidal

  2. Snapshots of America's Families II: A View of the Nation and 13 States from the National Survey of America's Families, 1997-1999.

    ERIC Educational Resources Information Center

    Koppelman, Jane, Ed.

    This collection of snapshots examines the well-being of America's children and adults through the lens of the 1999 National Survey of America's Families. Snapshots include: "Foreword: Snapshots of America's Families II: A View of the Nation and 13 States from the National Survey of America's Families" (Alyssa Wigton and Alan Weil);…

  3. VizieR Online Data Catalog: The HII Region Discovery Survey (HRDS). II. (Anderson+, 2011)

    NASA Astrophysics Data System (ADS)

    Anderson, L. D.; Bania, T. M.; Balser, D. S.; Rood, R. T.

    2011-08-01

    Our observations were made with the Green Bank Telescope (GBT) 100m telescope from 2008 June through 2010 October. We assembled our target list from the following multi-frequency, large solid angle Galactic surveys: the NRAO Very Large Array (VLA) Galactic Plane Survey at 21cm HI and continuum (VGPS: Stil et al. 2006AJ....132.1158S), the NRAO VLA Sky Survey at 20cm continuum (NVSS: Condon et al. 1998, Cat. VIII/65), the Southern Galactic Plane Survey at 21cm HI and continuum (SGPS: Haverkorn et al. 2006ApJS..167..230H), the VLA MAGPIS at 20cm continuum (Helfand et al. 2006, Cat. J/AJ/131/2525), and the Spitzer 24um MIPSGAL survey (Carey et al. 2009PASP..121...76C). Our analysis here also uses 8.0um data from the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE: Benjamin et al. 2003PASP..115..953B), which were obtained with the Infrared Array Camera (IRAC) on the Spitzer Space Telescope. (4 data files).

  4. A survey of the Large Magellanic Cloud in the (C II) 158 micron line

    NASA Technical Reports Server (NTRS)

    Mochizuki, Kenji; Nakagawa, Takao; Doi, Yasuo; Yui, Yukari Y.; Okuda, Haruyuki; Shibai, Hiroshi; Yui, Masao; Nishimura, Tetsuo; Low, Frank J.

    1994-01-01

    We have mapped the Large Magellanic Cloud (the LMC) in the (C II) 158 microns fine-structure line with the Balloon-borne Infrared Carbon Explorer (BICE) system. The (C II) line emission was detected over most of the LMC. The mean (C II)/CO (J = 1-0) line intensity ratio was 23,000 18 times larger than the typical value observed in the Galactic plane (1300). This result implies that each clump of the molecular clouds in the LMC has a larger C(+) envelope relative to its CO core than those in our Galaxy. Lower dust abundance due to its lower metallicity allows UV photons, which convert CO molecules into C(+) ions, to penetrate deeper into the clumps in the LMC than in our Galaxy.

  5. A Copernicus survey of Mg II emission in late-type stars

    NASA Technical Reports Server (NTRS)

    Weiler, E. J.; Oegerle, W. R.

    1979-01-01

    The behavior of Mg II emission in late-type stars is examined using scan data obtained with the Copernicus satellite. The luminosity in the Mg II k emission line was found to be closely related to stellar absolute magnitude, leading to the suggestion that such correlation may be very useful for future UV observations. The stellar surface flux in the k line was observed to be roughly constant or to decrease slowly with later spectral type, a finding which is then used to show that the pressure at the top of the chromosphere decreases with later spectral type, in agreement with the conclusions by McClintock et al. (1975). An asymmetry in the Mg II k line was noticed to be present in the available data for the stars later than K2-K5.

  6. THE PRISM MULTI-OBJECT SURVEY (PRIMUS). II. DATA REDUCTION AND REDSHIFT FITTING

    SciTech Connect

    Cool, Richard J.; Moustakas, John; Blanton, Michael R.; Hogg, David W.; Burles, Scott M.; Coil, Alison L.; Aird, James; Mendez, Alexander J.; Eisenstein, Daniel J.; Wong, Kenneth C.; Zhu, Guangtun; Bernstein, Rebecca A.

    2013-04-20

    The PRIsm MUlti-object Survey (PRIMUS) is a spectroscopic galaxy redshift survey to z {approx} 1 completed with a low-dispersion prism and slitmasks allowing for simultaneous observations of {approx}2500 objects over 0.18 deg{sup 2}. The final PRIMUS catalog includes {approx}130,000 robust redshifts over 9.1 deg{sup 2}. In this paper, we summarize the PRIMUS observational strategy and present the data reduction details used to measure redshifts, redshift precision, and survey completeness. The survey motivation, observational techniques, fields, target selection, slitmask design, and observations are presented in Coil et al. Comparisons to existing higher-resolution spectroscopic measurements show a typical precision of {sigma}{sub z}/(1 + z) = 0.005. PRIMUS, both in area and number of redshifts, is the largest faint galaxy redshift survey completed to date and is allowing for precise measurements of the relationship between active galactic nuclei and their hosts, the effects of environment on galaxy evolution, and the build up of galactic systems over the latter half of cosmic history.

  7. THE WIRED SURVEY. II. INFRARED EXCESSES IN THE SDSS DR7 WHITE DWARF CATALOG

    SciTech Connect

    Debes, John H.; Leisawitz, David T.; Hoard, D. W.; Wachter, Stefanie; Cohen, Martin

    2011-12-01

    With the launch of the Wide-field Infrared Survey Explorer (WISE), a new era of detecting planetary debris and brown dwarfs (BDs) around white dwarfs (WDs) has begun with the WISE InfraRed Excesses around Degenerates (WIRED) Survey. The WIRED Survey is sensitive to substellar objects and dusty debris around WDs out to distances exceeding 100 pc, well beyond the completeness level of local WDs. In this paper, we present a cross-correlation of the preliminary Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7) WD catalog between the WISE, Two-Micron All Sky Survey (2MASS), UKIRT Infrared Deep Sky Survey (UKIDSS), and SDSS DR7 photometric catalogs. From {approx}18,000 input targets, there are WISE detections comprising 344 'naked' WDs (detection of the WD photosphere only), 1020 candidate WD+M dwarf binaries, 42 candidate WD+BD systems, 52 candidate WD+dust disk systems, and 69 targets with indeterminate infrared excess. We classified all of the detected targets through spectral energy distribution model fitting of the merged optical, near-IR, and WISE photometry. Some of these detections could be the result of contaminating sources within the large ( Almost-Equal-To 6'') WISE point-spread function; we make a preliminary estimate for the rates of contamination for our WD+BD and WD+disk candidates and provide notes for each target of interest. Each candidate presented here should be confirmed with higher angular resolution infrared imaging or infrared spectroscopy. We also present an overview of the observational characteristics of the detected WDs in the WISE photometric bands, including the relative frequencies of candidate WD+M, WD+BD, and WD+disk systems.

  8. VizieR Online Data Catalog: Spitzer/IRS survey of Class II objects in Orion A. I. (Kim+, 2016)

    NASA Astrophysics Data System (ADS)

    Kim, K. H.; Watson, D. M.; Manoj, P.; Forrest, W. J.; Furlan, E.; Najita, J.; Sargent, B.; Hernandez, J.; Calvet, N.; Adame, L.; Espaillat, C.; Megeath, S. T.; Muzerolle, J.; McClure, M. K.

    2016-10-01

    We present 319 Class II disks observed with Spitzer/IRS in the Orion A star-forming region. We described the Spitzer/IRS and IRTF/SpeX observations and data reduction process in Kim+ (2013, J/ApJ/769/149). The Orion A objects in this paper were selected based on the identification of young stars with disks by IRAC/Two Micron All Sky Survey (2MASS) color-color diagrams (Megeath+ 2012, J/AJ/144/192). We observed them using Spitzer/IRS during campaigns 36, 39, 40, and 44 between 2006 November and 2007 October. To this group we added 16 additional objects (5 in the ONC; 11 in L1641) that were reclassified as Class II from Class 0/I sources observed in the Orion A protostar survey by C. Poteet et al. (2016, in preparation); 14 of these 16 were observed during campaigns 39 and 40, but 2 sources were observed in campaign 56 (see table 1). Of our IRS targets observed in both SL and LL modules in Orion A with Spitzer/IRS, we observed 120 at near-IR (0.8-2.4um) wavelengths with the medium-resolution spectrograph SpeX, on the NASA IRTF on Mauna Kea during the 2010A, 2011A, and 2011B semesters (see table 3). (9 data files).

  9. Ontario Universities Benefits Survey 1994-96. Part I: Benefits Excluding Pensions [and] Part II: Pensions.

    ERIC Educational Resources Information Center

    Council of Ontario Universities, Toronto.

    This report presents data from a survey of Ontario (Canada) universities concerning employment benefits offered in 1994-96. Part 1 covers benefits other than pensions. Tables display the information on particular benefits institution-by-institution including: administration and insurance plans, communication of benefits, proposed changes, life and…

  10. Linking a Medical User Survey to Management for Library Effectiveness: II, A Checkland Soft Systems Study.

    ERIC Educational Resources Information Center

    Brember, V. L.

    1985-01-01

    Presents Checkland's soft systems methodology, discusses it in terms of the systems approach, and illustrates how it was used to relate evidence of user survey to practical problems of library management. Difficulties in using methodology are described and implications for library management and information science research are presented. (8…

  11. Ontario Universities Benefits Survey, 1993-94, Part I, Benefits Excluding Pensions [and] Part II: Pensions.

    ERIC Educational Resources Information Center

    Council of Senior Administrative Officers--Universities of Ontario, Toronto.

    This report presents data from a survey of Ontario (Canada) universities concerning employment benefits offered in 1993-94. Part I covers benefits other than pensions. Tables display the information on particular benefits institution-by-institution including: administration and insurance plans, communication of benefits, proposed changes,…

  12. Ontario Universities Benefits Survey 1994-96. Part I: Benefits Excluding Pensions [and] Part II: Pensions.

    ERIC Educational Resources Information Center

    Council of Ontario Universities, Toronto.

    This report presents data from a survey of Ontario (Canada) universities concerning employment benefits offered in 1994-96. Part 1 covers benefits other than pensions. Tables display the information on particular benefits institution-by-institution including: administration and insurance plans, communication of benefits, proposed changes, life and…

  13. The Peat Marwick/AS&U Compensation Survey. Part II: For College and University Executives.

    ERIC Educational Resources Information Center

    American School and University, 1986

    1986-01-01

    A total of 375 responses were received from two- and four-year colleges nationwide to a survey of compensation packages for the following positions: president; professor; and chief officers for academic concerns, business, facilities, purchasing, and computer services. Tables display data sorted by two- and four-year institutions and enrollment…

  14. VizieR Online Data Catalog: The Bolocam Galactic Plane Survey. II. (Rosolowsky+, 2010)

    NASA Astrophysics Data System (ADS)

    Rosolowsky, E.; Dunham, M. K.; Ginsburg, A.; Bradley, E. T.; Aguirre, J.; Bally, J.; Battersby, C.; Cyganowski, C.; Dowell, D.; Drosback, M.; Evans, N. J.; Glenn, J.; Harvey, P.; Stringfellow, G. S.; Walawender, J.; Williams, J. P.

    2010-09-01

    The BGPS is described in full detail in Paper I, Aguirre et al., 2010, submitted. The survey uses the 144-element Bolocam array on the Caltech Submillimeter Observatory, which observes in a band centered at 268GHz (1.1mm) and a width of 46GHz. (1 data file).

  15. The Sub-Kilometer Asteroid Diameter Survey II: The debiased size distribution of main belt asteroids

    NASA Astrophysics Data System (ADS)

    Jedicke, R.; Gladman, B.; Davis, D.; Petit, J.-M.

    2011-10-01

    The Sub-Kilometer Asteroid Diameter Survey (SKADS, [1]) imaged ˜8.6 square degrees of sky and detected 1277 main belt asteroids to a limiting magnitude of R˜23 (at which the efficiency is 50%). SKADS was performed in both V and R filters and allows a probabilistic assignment of an albedo, and therefore diameter, to each object. By planting synthetic objects directly into the images we have determined the moving object detection efficiency as a function of their rate and direction of motion and their apparent magnitude on each of the six survey nights. The surveying pattern was designed to provide recovery of the asteroids over intervals of >6 days and therefore provides a good orbit, distance and absolute magnitude for each of the objects. We have performed a high-resolution, high-accuracy simulation of the multi-night surveying procedure to compute the observational selection effects as a function of semi-major axis, eccentricity, inclination and absolute magnitude (see Figure 1). We will present the results of this simulation and provide the observationally corrected distributions of main belt objects as a function of their orbital parameters, absolute magnitude and diameter.

  16. The Peat Marwick/AS&U Compensation Survey. Part II: For College and University Executives.

    ERIC Educational Resources Information Center

    American School and University, 1986

    1986-01-01

    A total of 375 responses were received from two- and four-year colleges nationwide to a survey of compensation packages for the following positions: president; professor; and chief officers for academic concerns, business, facilities, purchasing, and computer services. Tables display data sorted by two- and four-year institutions and enrollment…

  17. A Survey of the Contemporary Indians of Canada: Economic, Political, Educational Needs and Policies. Volume II.

    ERIC Educational Resources Information Center

    Tremblay, M. A.; And Others

    Two sets of issues are discussed in this volume of the survey. These issues are related to the provision and adequacy of schools for the Indian child and adult, and to leadership, organization and direction of reserves. Although mindful of the wider setting of culture and community in which these issues find their definition, they are abstracted…

  18. AKARI INFRARED CAMERA SURVEY OF THE LARGE MAGELLANIC CLOUD. II. THE NEAR-INFRARED SPECTROSCOPIC CATALOG

    SciTech Connect

    Shimonishi, Takashi; Onaka, Takashi; Kato, Daisuke; Sakon, Itsuki; Ita, Yoshifusa; Kawamura, Akiko; Kaneda, Hidehiro

    2013-02-01

    We performed a near-infrared spectroscopic survey toward an area of {approx}10 deg{sup 2} of the Large Magellanic Cloud (LMC) with the infrared satellite AKARI. Observations were carried out as part of the AKARI Large-area Survey of the Large Magellanic Cloud (LSLMC). The slitless multi-object spectroscopic capability of the AKARI/IRC enabled us to obtain low-resolution (R {approx} 20) spectra in 2-5 {mu}m for a large number of point sources in the LMC. As a result of the survey, we extracted about 2000 infrared spectra of point sources. The data are organized as a near-infrared spectroscopic catalog. The catalog includes various infrared objects such as young stellar objects (YSOs), asymptotic giant branch (AGB) stars, supergiants, and so on. It is shown that 97% of the catalog sources have corresponding photometric data in the wavelength range from 1.2 to 11 {mu}m, and 67% of the sources also have photometric data up to 24 {mu}m. The catalog allows us to investigate near-infrared spectral features of sources by comparison with their infrared spectral energy distributions. In addition, it is estimated that about 10% of the catalog sources are observed at more than two different epochs. This enables us to study a spectroscopic variability of sources by using the present catalog. Initial results of source classifications for the LSLMC samples are presented. We classified 659 LSLMC spectra based on their near-infrared spectral features by visual inspection. As a result, it is shown that the present catalog includes 7 YSOs, 160 C-rich AGBs, 8 C-rich AGB candidates, 85 O-rich AGBs, 122 blue and yellow supergiants, 150 red super giants, and 128 unclassified sources. Distributions of the classified sources on the color-color and color-magnitude diagrams are discussed in the text. Continuous wavelength coverage and high spectroscopic sensitivity in 2-5 {mu}m can only be achieved by space observations. This is an unprecedented large-scale spectroscopic survey toward the

  19. Evaluation of Workpiece Temperature during Drilling of GLARE Fiber Metal Laminates Using Infrared Techniques: Effect of Cutting Parameters, Fiber Orientation and Spray Mist Application

    PubMed Central

    Giasin, Khaled; Ayvar-Soberanis, Sabino

    2016-01-01

    The rise in cutting temperatures during the machining process can influence the final quality of the machined part. The impact of cutting temperatures is more critical when machining composite-metal stacks and fiber metal laminates due to the stacking nature of those hybrids which subjects the composite to heat from direct contact with metallic part of the stack and the evacuated hot chips. In this paper, the workpiece surface temperature of two grades of fiber metal laminates commercially know as GLARE is investigated. An experimental study was carried out using thermocouples and infrared thermography to determine the emissivity of the upper, lower and side surfaces of GLARE laminates. In addition, infrared thermography was used to determine the maximum temperature of the bottom surface of machined holes during drilling GLARE under dry and minimum quantity lubrication (MQL) cooling conditions under different cutting parameters. The results showed that during the machining process, the workpiece surface temperature increased with the increase in feed rate and fiber orientation influenced the developed temperature in the laminate. PMID:28773757

  20. The Three-mm Ultimate Mopra Milky way Survey (MALT110): Completion of Phase II

    NASA Astrophysics Data System (ADS)

    Barnes, Peter; Lo, Nadia; Jones, Paul; Muller, Erik; Cunningham, Maria; Fuller, Gary; Longmore, Steven; Whitney, Barbara; Mizuno, Norikazu; Schuller, Frederic; Brogan, Crystal; Benjamin, Bob; Indermuehle, Balthasar; Caselli, Paola; Molinari, Sergio; Hernandez, Audra; Lowe, Vicki; Nguyen-Luong, Quang; Crutcher, Richard; Wakker, Bart; Goodman, Alyssa; Chibueze, James Okwe; Umemoto, Tomofumi; Nakanishi, Hiroyuki; O'Dougherty, Stefan; Sharpe, Margaret; Pitts, Rebecca

    2014-04-01

    We propose to combine Mopra's very fast mapping and robotic observing capabilities to complete the expanded latitude coverage for a long-overdue (but previously technically forbidding) comprehensive survey, begun in 2011, of the southern Milky Way's molecular Interstellar Medium. ThrUMMS' goal is to obtain arcminute-resolution, 0.7 K sensitivity maps of 12CO, 13CO, C18O, and CN over most of the 4th quadrant, quickly and publicly. Together with other ongoing or planned surveys of the Milky Way's cold ISM, ThrUMMS' parsec-resolution maps will revolutionise our understanding of molecular cloud and star formation, the total ecology of the ISM and its relationship with our Galaxy's stars, and the dynamics, chemistry, structure and evolution of the Milky Way itself.

  1. Visual servoing in medical robotics: a survey. Part II: tomographic imaging modalities--techniques and applications.

    PubMed

    Azizian, Mahdi; Najmaei, Nima; Khoshnam, Mahta; Patel, Rajni

    2015-03-01

    Intraoperative application of tomographic imaging techniques provides a means of visual servoing for objects beneath the surface of organs. The focus of this survey is on therapeutic and diagnostic medical applications where tomographic imaging is used in visual servoing. To this end, a comprehensive search of the electronic databases was completed for the period 2000-2013. Existing techniques and products are categorized and studied, based on the imaging modality and their medical applications. This part complements Part I of the survey, which covers visual servoing techniques using endoscopic imaging and direct vision. The main challenges in using visual servoing based on tomographic images have been identified. 'Supervised automation of medical robotics' is found to be a major trend in this field and ultrasound is the most commonly used tomographic modality for visual servoing. Copyright © 2014 John Wiley & Sons, Ltd.

  2. Cosmic shear results from the deep lens survey. II. Full cosmological parameter constraints from tomography

    SciTech Connect

    Jee, M. James; Tyson, J. Anthony; Hilbert, Stefan; Schneider, Michael D.; Schmidt, Samuel; Wittman, David

    2016-06-15

    Here, we present a tomographic cosmic shear study from the Deep Lens Survey (DLS), which, providing a limiting magnitude ${r}_{\\mathrm{lim}}\\sim 27$ ($5\\sigma $), is designed as a precursor Large Synoptic Survey Telescope (LSST) survey with an emphasis on depth. Using five tomographic redshift bins, we study their auto- and cross-correlations to constrain cosmological parameters. We use a luminosity-dependent nonlinear model to account for the astrophysical systematics originating from intrinsic alignments of galaxy shapes. We find that the cosmological leverage of the DLS is among the highest among existing $\\gt 10$ deg2 cosmic shear surveys. Combining the DLS tomography with the 9 yr results of the Wilkinson Microwave Anisotropy Probe (WMAP9) gives ${{\\rm{\\Omega }}}_{m}={0.293}_{-0.014}^{+0.012}$, ${\\sigma }_{8}={0.833}_{-0.018}^{+0.011}$, ${H}_{0}={68.6}_{-1.2}^{+1.4}\\;{\\text{km s}}^{-1}\\;{{\\rm{Mpc}}}^{-1}$, and ${{\\rm{\\Omega }}}_{b}=0.0475\\pm 0.0012$ for ΛCDM, reducing the uncertainties of the WMAP9-only constraints by ~50%. When we do not assume flatness for ΛCDM, we obtain the curvature constraint ${{\\rm{\\Omega }}}_{k}=-{0.010}_{-0.015}^{+0.013}$ from the DLS+WMAP9 combination, which, however, is not well constrained when WMAP9 is used alone. The dark energy equation-of-state parameter w is tightly constrained when baryonic acoustic oscillation (BAO) data are added, yielding $w=-{1.02}_{-0.09}^{+0.10}$ with the DLS+WMAP9+BAO joint probe. The addition of supernova constraints further tightens the parameter to $w=-1.03\\pm 0.03$. Our joint constraints are fully consistent with the final Planck results and also with the predictions of a ΛCDM universe.

  3. Cosmic shear results from the deep lens survey. II. Full cosmological parameter constraints from tomography

    SciTech Connect

    Jee, M. James; Tyson, J. Anthony; Hilbert, Stefan; Schneider, Michael D.; Schmidt, Samuel; Wittman, David

    2016-06-15

    Here, we present a tomographic cosmic shear study from the Deep Lens Survey (DLS), which, providing a limiting magnitude ${r}_{\\mathrm{lim}}\\sim 27$ ($5\\sigma $), is designed as a precursor Large Synoptic Survey Telescope (LSST) survey with an emphasis on depth. Using five tomographic redshift bins, we study their auto- and cross-correlations to constrain cosmological parameters. We use a luminosity-dependent nonlinear model to account for the astrophysical systematics originating from intrinsic alignments of galaxy shapes. We find that the cosmological leverage of the DLS is among the highest among existing $\\gt 10$ deg2 cosmic shear surveys. Combining the DLS tomography with the 9 yr results of the Wilkinson Microwave Anisotropy Probe (WMAP9) gives ${{\\rm{\\Omega }}}_{m}={0.293}_{-0.014}^{+0.012}$, ${\\sigma }_{8}={0.833}_{-0.018}^{+0.011}$, ${H}_{0}={68.6}_{-1.2}^{+1.4}\\;{\\text{km s}}^{-1}\\;{{\\rm{Mpc}}}^{-1}$, and ${{\\rm{\\Omega }}}_{b}=0.0475\\pm 0.0012$ for ΛCDM, reducing the uncertainties of the WMAP9-only constraints by ~50%. When we do not assume flatness for ΛCDM, we obtain the curvature constraint ${{\\rm{\\Omega }}}_{k}=-{0.010}_{-0.015}^{+0.013}$ from the DLS+WMAP9 combination, which, however, is not well constrained when WMAP9 is used alone. The dark energy equation-of-state parameter w is tightly constrained when baryonic acoustic oscillation (BAO) data are added, yielding $w=-{1.02}_{-0.09}^{+0.10}$ with the DLS+WMAP9+BAO joint probe. The addition of supernova constraints further tightens the parameter to $w=-1.03\\pm 0.03$. Our joint constraints are fully consistent with the final Planck results and also with the predictions of a ΛCDM universe.

  4. Cosmic shear results from the deep lens survey. II. Full cosmological parameter constraints from tomography

    DOE PAGES

    Jee, M. James; Tyson, J. Anthony; Hilbert, Stefan; ...

    2016-06-15

    Here, we present a tomographic cosmic shear study from the Deep Lens Survey (DLS), which, providing a limiting magnitudemore » $${r}_{\\mathrm{lim}}\\sim 27$$ ($$5\\sigma $$), is designed as a precursor Large Synoptic Survey Telescope (LSST) survey with an emphasis on depth. Using five tomographic redshift bins, we study their auto- and cross-correlations to constrain cosmological parameters. We use a luminosity-dependent nonlinear model to account for the astrophysical systematics originating from intrinsic alignments of galaxy shapes. We find that the cosmological leverage of the DLS is among the highest among existing $$\\gt 10$$ deg2 cosmic shear surveys. Combining the DLS tomography with the 9 yr results of the Wilkinson Microwave Anisotropy Probe (WMAP9) gives $${{\\rm{\\Omega }}}_{m}={0.293}_{-0.014}^{+0.012}$$, $${\\sigma }_{8}={0.833}_{-0.018}^{+0.011}$$, $${H}_{0}={68.6}_{-1.2}^{+1.4}\\;{\\text{km s}}^{-1}\\;{{\\rm{Mpc}}}^{-1}$$, and $${{\\rm{\\Omega }}}_{b}=0.0475\\pm 0.0012$$ for ΛCDM, reducing the uncertainties of the WMAP9-only constraints by ~50%. When we do not assume flatness for ΛCDM, we obtain the curvature constraint $${{\\rm{\\Omega }}}_{k}=-{0.010}_{-0.015}^{+0.013}$$ from the DLS+WMAP9 combination, which, however, is not well constrained when WMAP9 is used alone. The dark energy equation-of-state parameter w is tightly constrained when baryonic acoustic oscillation (BAO) data are added, yielding $$w=-{1.02}_{-0.09}^{+0.10}$$ with the DLS+WMAP9+BAO joint probe. The addition of supernova constraints further tightens the parameter to $$w=-1.03\\pm 0.03$$. Our joint constraints are fully consistent with the final Planck results and also with the predictions of a ΛCDM universe.« less

  5. Physicians' attitudes toward homosexuality and HIV: survey of a California Medical Society- revisited (PATHH-II).

    PubMed

    Smith, Davey M; Mathews, Wm Christopher

    2007-01-01

    In 1982, Mathews et al. surveyed San Diego County Medical Society's (SDCMS) physicians about their attitudes toward homosexuality. They found significant differences in prevalence of homophobic attitudes by gender, year of medical school graduation, specialty, and practice setting. To assess current physicians' attitudes toward homosexuality and persons with HIV infection, an anonymous, self-administered, 17-item survey was mailed to all 4,385 members of the SDCMS and 1,271 UCSD physicians. The survey included items measuring attitudes toward homosexuality and toward entry to medical school and referral patterns, conditional on sexual orientation and HIV status of hypothetical referents. Only 3% of respondents would not admit a highly qualified homosexual applicant to medical school compared with 30% in 1982. Similarly, 9% would discontinue referrals to a gay pediatrician compared with 46% of respondents in 1982. Forty-two percent would not admit a "highly qualified but asymptomatic HIV-infected applicant with excellent response to antiretroviral therapy to medical school" and 66% would discontinue referral to a general surgeon known to be HIV infected. In multiple logistic regression analyses controlling for sex and medical school affiliation, significant (p < 0.05) independent predictors of being in the highest 10% on an HIV-phobia scale were year of graduation from medical school and degree of homophobia (model ROC = 0.77). This survey suggests a substantial reduction in homophobia since 1982. However, attitudes toward homosexuals and year of graduation from medical school appear to be significant predictors of attitudes toward persons with HIV infection.

  6. Test program element II blanket and shield thermal-hydraulic and thermomechanical testing, experimental facility survey

    SciTech Connect

    Ware, A.G.; Longhurst, G.R.

    1981-12-01

    This report presents results of a survey conducted by EG and G Idaho to determine facilities available to conduct thermal-hydraulic and thermomechanical testing for the Department of Energy Office of Fusion Energy First Wall/Blanket/Shield Engineering Test Program. In response to EG and G queries, twelve organizations (in addition to EG and G and General Atomic) expressed interest in providing experimental facilities. A variety of methods of supplying heat is available.

  7. Cosmic Shear Results from the Deep Lens Survey. II. Full Cosmological Parameter Constraints from Tomography

    NASA Astrophysics Data System (ADS)

    Jee, M. James; Tyson, J. Anthony; Hilbert, Stefan; Schneider, Michael D.; Schmidt, Samuel; Wittman, David

    2016-06-01

    We present a tomographic cosmic shear study from the Deep Lens Survey (DLS), which, providing a limiting magnitude {r}{lim}˜ 27 (5σ ), is designed as a precursor Large Synoptic Survey Telescope (LSST) survey with an emphasis on depth. Using five tomographic redshift bins, we study their auto- and cross-correlations to constrain cosmological parameters. We use a luminosity-dependent nonlinear model to account for the astrophysical systematics originating from intrinsic alignments of galaxy shapes. We find that the cosmological leverage of the DLS is among the highest among existing \\gt 10 deg2 cosmic shear surveys. Combining the DLS tomography with the 9 yr results of the Wilkinson Microwave Anisotropy Probe (WMAP9) gives {{{Ω }}}m={0.293}-0.014+0.012, {σ }8={0.833}-0.018+0.011, {H}0={68.6}-1.2+1.4 {\\text{km s}}-1 {{{Mpc}}}-1, and {{{Ω }}}b=0.0475+/- 0.0012 for ΛCDM, reducing the uncertainties of the WMAP9-only constraints by ˜50%. When we do not assume flatness for ΛCDM, we obtain the curvature constraint {{{Ω }}}k=-{0.010}-0.015+0.013 from the DLS+WMAP9 combination, which, however, is not well constrained when WMAP9 is used alone. The dark energy equation-of-state parameter w is tightly constrained when baryonic acoustic oscillation (BAO) data are added, yielding w=-{1.02}-0.09+0.10 with the DLS+WMAP9+BAO joint probe. The addition of supernova constraints further tightens the parameter to w=-1.03+/- 0.03. Our joint constraints are fully consistent with the final Planck results and also with the predictions of a ΛCDM universe.

  8. Apples to apples A2 - II. Cluster selection functions for next-generation surveys

    NASA Astrophysics Data System (ADS)

    Ascaso, B.; Mei, S.; Bartlett, J. G.; Benítez, N.

    2017-01-01

    We present the cluster selection function for three of the largest next-generation stage-IV surveys in the optical and infrared: Euclid-Optimistic, Euclid-Pessimistic and the Large Synoptic Survey Telescope (LSST). To simulate these surveys, we use the realistic mock catalogues introduced in the first paper of this series. We detected galaxy clusters using the Bayesian Cluster Finder in the mock catalogues. We then modelled and calibrated the total cluster stellar mass observable-theoretical mass (M^{*}_CL-M_h) relation using a power-law model, including a possible redshift evolution term. We find a moderate scatter of σ _{M^{*}_CL | M_h} of 0.124, 0.135 and 0.136 dex for Euclid-Optimistic, Euclid-Pessimistic and LSST, respectively, comparable to other work over more limited ranges of redshift. Moreover, the three data sets are consistent with negligible evolution with redshift, in agreement with observational and simulation results in the literature. We find that Euclid-Optimistic will be able to detect clusters with >80 per cent completeness and purity down to 8 × 1013 h-1 M⊙ up to z < 1. At higher redshifts, the same completeness and purity are obtained with the larger mass threshold of 2 × 1014 h-1 M⊙ up to z = 2. The Euclid-Pessimistic selection function has a similar shape with ˜10 per cent higher mass limit. LSST shows ˜5 per cent higher mass limit than Euclid-Optimistic up to z < 0.7 and increases afterwards, reaching a value of 2 × 1014 h-1 M⊙ at z = 1.4. Similar selection functions with only 80 per cent completeness threshold have also been computed. The complementarity of these results with selection functions for surveys in other bands is discussed.

  9. The infrared medium-deep survey. II. How to trigger radio AGNs? Hints from their environments

    SciTech Connect

    Karouzos, Marios; Im, Myungshin; Kim, Jae-Woo; Lee, Seong-Kook; Jeon, Yiseul; Choi, Changsu; Hong, Jueun; Hyun, Minhee; Jun, Hyunsung David; Kim, Dohyeong; Kim, Yongjung; Kim, Ji Hoon; Kim, Duho; Park, Won-Kee; Taak, Yoon Chan; Yoon, Yongmin; Chapman, Scott; Pak, Soojong; Edge, Alastair

    2014-12-10

    Activity at the centers of galaxies, during which the central supermassive black hole is accreting material, is nowadays accepted to be rather ubiquitous and most probably a phase of every galaxy's evolution. It has been suggested that galactic mergers and interactions may be the culprits behind the triggering of nuclear activity. We use near-infrared data from the new Infrared Medium-Deep Survey and the Deep eXtragalactic Survey of the VIMOS-SA22 field and radio data at 1.4 GHz from the FIRST survey and a deep Very Large Array survey to study the environments of radio active galactic nuclei (AGNs) over an area of ∼25 deg{sup 2} and down to a radio flux limit of 0.1 mJy and a J-band magnitude of 23 mag AB. Radio AGNs are predominantly found in environments similar to those of control galaxies at similar redshift, J-band magnitude, and (M{sub u} – M{sub r} ) rest-frame color. However, a subpopulation of radio AGNs is found in environments up to 100 times denser than their control sources. We thus preclude merging as the dominant triggering mechanism of radio AGNs. By fitting the broadband spectral energy distribution of radio AGNs in the least and most dense environments, we find that those in the least dense environments show higher radio-loudness, higher star formation efficiencies, and higher accretion rates, typical of the so-called high-excitation radio AGNs. These differences tend to disappear at z > 1. We interpret our results in terms of a different triggering mechanism for these sources that is driven by mass loss through winds of young stars created during the observed ongoing star formation.

  10. A Successful Broadband Survey for Giant Lyα Nebulae. II. Spectroscopic Confirmation

    NASA Astrophysics Data System (ADS)

    Prescott, Moire K. M.; Dey, Arjun; Jannuzi, Buell T.

    2013-01-01

    Using a systematic broadband search technique, we have carried out a survey for large Lyα nebulae (or Lyα "blobs") at 2 <~ z <~ 3 within 8.5 deg2 of the NOAO Deep Wide-Field Survey Boötes field, corresponding to a total survey comoving volume of ≈108 h -3 70 Mpc3. Here, we present our spectroscopic observations of candidate giant Lyα nebulae. Of 26 candidates targeted, 5 were confirmed to have Lyα emission at 1.7 <~ z <~ 2.7, 4 of which were new discoveries. The confirmed Lyα nebulae span a range of Lyα equivalent widths, colors, sizes, and line ratios, and most show spatially extended continuum emission. The remaining candidates did not reveal any strong emission lines, but instead exhibit featureless, diffuse, blue continuum spectra. Their nature remains mysterious, but we speculate that some of these might be Lyα nebulae lying within the redshift desert (i.e., 1.2 <~ z <~ 1.6). Our spectroscopic follow-up confirms the power of using deep broadband imaging to search for the bright end of the Lyα nebula population across enormous comoving volumes.

  11. A SUCCESSFUL BROADBAND SURVEY FOR GIANT Ly{alpha} NEBULAE. II. SPECTROSCOPIC CONFIRMATION

    SciTech Connect

    Prescott, Moire K. M.; Dey, Arjun; Jannuzi, Buell T.

    2013-01-01

    Using a systematic broadband search technique, we have carried out a survey for large Ly{alpha} nebulae (or Ly{alpha} {sup b}lobs{sup )} at 2 {approx}< z {approx}< 3 within 8.5 deg{sup 2} of the NOAO Deep Wide-Field Survey Booetes field, corresponding to a total survey comoving volume of Almost-Equal-To 10{sup 8} h {sup -3} {sub 70} Mpc{sup 3}. Here, we present our spectroscopic observations of candidate giant Ly{alpha} nebulae. Of 26 candidates targeted, 5 were confirmed to have Ly{alpha} emission at 1.7 {approx}< z {approx}< 2.7, 4 of which were new discoveries. The confirmed Ly{alpha} nebulae span a range of Ly{alpha} equivalent widths, colors, sizes, and line ratios, and most show spatially extended continuum emission. The remaining candidates did not reveal any strong emission lines, but instead exhibit featureless, diffuse, blue continuum spectra. Their nature remains mysterious, but we speculate that some of these might be Ly{alpha} nebulae lying within the redshift desert (i.e., 1.2 {approx}< z {approx}< 1.6). Our spectroscopic follow-up confirms the power of using deep broadband imaging to search for the bright end of the Ly{alpha} nebula population across enormous comoving volumes.

  12. New active galactic nuclei detected in ROSAT All Sky Survey galaxies. II. The complete dataset

    NASA Astrophysics Data System (ADS)

    Kollatschny, W.; Kotulla, R.; Pietsch, W.; Bischoff, K.; Zetzl, M.

    2008-06-01

    Aims: The ROSAT ALL Sky Survey Bright Source Catalogue (RASS-BSC) has been correlated with the Catalogue of Principal Galaxies (PGC) to identify new extragalactic counterparts. 550 reliable optical counterparts have been detected. However there existed no optical spectra for about 200 Active Galactic Nuclei (AGN) candidates before the ROSAT ALL Sky Survey (RASS) was completed. Methods: We took optical spectra of 176 X-ray candidates and companions at ESO, Calar Alto observatory and McDonald observatory. When necessary we used a line profile decomposition to measure line fluxes, widths and centers to classify their type of activity. Results: We discuss the redshift-, linewidth-, as well as optical and X-ray luminosity distribution of our ROSAT selected sample. 139 galaxies of our 166 X-ray counterparts have been identified as AGN with 93 being Seyfert 1 galaxies (61%). Eighteen of them (20%) are Narrow Line Seyfert 1 galaxies. 34 X-ray candidates (21%) are LINERs and only eight candidates (5%) are Seyfert 2. The ratio of the number of Seyfert 1 galaxies to Seyfert 2 galaxies is about 11/1. Optical surveys result in ratios of 1/1.4. The high fraction of detected Seyfert 1 galaxies is explained by the sensitivity of the ROSAT to soft X-rays which are heavily absorbed in type 2 AGN. Two X-ray candidates are HII-galaxies and 25 candidates (15%) show no signs of spectral activity. The AGN in our RASS selected sample exhibit slightly higher optical luminosities (MB = (-20.71 ± 1.75) mag) and similar X-ray luminosities (log(LX [ erg s-1] ) = 42.9 ± 1.7) compared to other AGN surveys. The Hα line width distribution (FWHM) of our newly identified ROSAT AGN sample is similar to the line widths distribution based on SDSS AGN. However, our newly identified RASS AGN have rather reddish colors explaining why they have not been detected before in ultraviolet or blue excess surveys.

  13. A survey for PAH emission in H II regions, planetary and proto-planetary nebulae

    NASA Technical Reports Server (NTRS)

    Demuizon, M.; Cox, P.; Lequeux, J.

    1989-01-01

    The results of a systematic investigation of polycyclic aromatic hydrocarbon (PAH) emission in H II regions, planetary nebulae (PN), and proto-planetary nebulae (PNN), are reported. Data is obtained from the low resolution spectra (LRS) of IRAS. The results show that: PAHs are formed in carbon rich objects; and PAH emission is ubiquitous in general interstellar medium and requires the presence of ultraviolet photons, in planetary and proto-planetary nebulae, PAH emission is seen only where an ionizing flux is present and in carbon rich objects.

  14. Cardiovascular health knowledge of the Polish population. Comparison of two national multi-centre health surveys: WOBASZ and WOBASZ II.

    PubMed

    Piwońska, Aleksandra; Piotrowski, Walerian; Piwoński, Jerzy; Kozela, Magdalena; Nadrowski, Paweł; Bielecki, Wojciech; Kozakiewicz, Krystyna; Pająk, Andrzej; Tykarski, Andrzej; Zdrojewski, Tomasz; Drygas, Wojciech

    2017-01-01

    To compare the cardiovascular health knowledge (CHK) of the adult Polish population in the years 2003-2005 and 2013-2014, and to evaluate the CHK determinants in the Polish adult population. Data came from the two random samples of the Polish population, screened in 2003-2005 in the WOBASZ health survey (6392 men and 7153 women, aged 20-74 years) and in 2013-2014 in the WOBASZ II health survey (2751 men and 3418 women, aged 20+ years). For the present analysis, the population of WOBASZ II was limited to persons aged 20-74 years. A CHK score (CHKs) was constructed based on questionnaire answers of responders, and the results of physical examination and ranged from -1 (lowest knowledge) to +6 (highest knowledge). Women had greater CHK than men. In both studies, about 30% of women and 40% of men did not know their blood pressure (BP). About 20% of men and women that declared their BP awareness was not able to classify it correctly to the normal or high category. Most persons that declared body weight awareness could give their body weight to within 2 kg and could correctly classify it as normal or overweight/obesity. The mean CHKs raised in men from 1.74 in WOBASZ to 1.93 in WOBASZ II (in women, respectively, from 2.10 to 2.23). The chance of having CHK greater than mean value of CHKs increased in men by 31% and in women by 27% in WOBASZ II compared to WOBASZ (ORCHK = 1.31, p < 0.0001 in men; ORCHK = 1.27, p < 0.0001 in women). Younger, better educated persons and men with coronary artery disease history and persons with familial history of death from myocardial infarction or stroke had greater health knowledge. Since 2003 Polish adults significantly advanced their knowledge and awareness of cardiovascular risk factors. Gender, age, education level, coronary artery disease history, and family history of cardiovascular disease death are significant determinants of CHK. From 20% to 30% of studied persons who declared their awareness, were shown to be unaware of their

  15. The Rise and Fall of Type Ia Supernova Light Curves in the SDSS-II Supernova Survey

    SciTech Connect

    Hayden, Brian T.; Garnavich, Peter M.; Kessler, Richard; Frieman, Joshua A.; Jha, Saurabh W.; Bassett, Bruce; Cinabro, David; Dilday, Benjamin; Kasen, Daniel; Marriner, John; Nichol, Robert C.; /Portsmouth U., ICG /Baltimore, Space Telescope Sci. /Johns Hopkins U.

    2010-01-01

    We analyze the rise and fall times of Type Ia supernova (SN Ia) light curves discovered by the Sloan Digital Sky Survey-II (SDSS-II) Supernova Survey. From a set of 391 light curves k-corrected to the rest-frame B and V bands, we find a smaller dispersion in the rising portion of the light curve compared to the decline. This is in qualitative agreement with computer models which predict that variations in radioactive nickel yield have less impact on the rise than on the spread of the decline rates. The differences we find in the rise and fall properties suggest that a single 'stretch' correction to the light curve phase does not properly model the range of SN Ia light curve shapes. We select a subset of 105 light curves well observed in both rise and fall portions of the light curves and develop a '2-stretch' fit algorithm which estimates the rise and fall times independently. We find the average time from explosion to B-band peak brightness is 17.38 {+-} 0.17 days, but with a spread of rise times which range from 13 days to 23 days. Our average rise time is shorter than the 19.5 days found in previous studies; this reflects both the different light curve template used and the application of the 2-stretch algorithm. The SDSS-II supernova set and the local SNe Ia with well-observed early light curves show no significant differences in their average rise-time properties. We find that slow-declining events tend to have fast rise times, but that the distribution of rise minus fall time is broad and single peaked. This distribution is in contrast to the bimodality in this parameter that was first suggested by Strovink (2007) from an analysis of a small set of local SNe Ia. We divide the SDSS-II sample in half based on the rise minus fall value, t{sub r} - t{sub f} {approx}< 2 days and t{sub r} - t{sub f} > 2 days, to search for differences in their host galaxy properties and Hubble residuals; we find no difference in host galaxy properties or Hubble residuals in our

  16. Characterising the local void with the X-ray cluster survey REFLEX II

    NASA Astrophysics Data System (ADS)

    Collins, Chris A.; Böhringer, Hans; Bristow, Martyn; Chon, Gayoung

    2016-10-01

    Claims of a significant underdensity or void in the density distribution on scales out to ~= 300 Mpc have recently been made using samples of galaxies. We present the results of an alternative test of the matter distribution on these scales using clusters of galaxies, which provide an independent and powerful probe of large-scale structure. We study the density distribution of X-ray clusters from the ROSAT-based REFLEX II catalogue, which covers a contiguous area of 4.24 steradians in the southern hempsphere (34% of the entire sky). Using the normalised comoving number density of clusters we find evidence for an underdensity (30-40%), out to z~ 0.04, equivalent to ~=170 Mpc and with a significance of 3.4σ. On scales between 300 Mpc and 1 Gpc the distribution of REFLEX II clusters is consistent with being uniform. We also confirm recent results that the underdensity has a large contribution from the direction of the South Galactic Cap region, but is not significant in the direction of the Northern Galactic Cap as viewed from the southern sky. Both the limited size of the detected underdensity and its lack of isotropy, argue against the idea that the Type Ia supernovae data can be explained without the need for dark energy.

  17. The ESO Slice Project (ESP) galaxy redshift survey. II. The luminosity function and mean galaxy density.

    NASA Astrophysics Data System (ADS)

    Zucca, E.; Zamorani, G.; Vettolani, G.; Cappi, A.; Merighi, R.; Mignoli, M.; Stirpe, G. M.; MacGillivray, H.; Collins, C.; Balkowski, C.; Cayatte, V.; Maurogordato, S.; Proust, D.; Chincarini, G.; Guzzo, L.; Maccagni, D.; Scaramella, R.; Blanchard, A.; Ramella, M.

    1997-10-01

    The ESO Slice Project (ESP) is a galaxy redshift survey we have recently completed as an ESO Key-Project over about 23 square degrees, in a region near the South Galactic Pole. The survey is nearly complete to the limiting magnitude b_J_=19.4 and consists of 3342 galaxies with reliable redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one-dimensional pencil beams: spanning a volume of ~5x10^4^h^-3^Mpc^3^ at the sensitivity peak (z~0.1), it provides an accurate determination of the "local" luminosity function and the mean galaxy density. We find that, although a Schechter function (with α=-1.22, M^*^_bJ_=-19.61+5logh and φ^*^=0.020h^3^/Mpc^3^) is an acceptable representation of the luminosity function over the entire range of magnitudes (M_bJ_<=-12.4+5logh), our data suggest the presence of a steepening of the luminosity function for M_bJ_>=-17+5logh. Such a steepening at the faint end of the luminosity function, well fitted by a power law with slope β~-1.6, is almost completely due to galaxies with emission lines: in fact, dividing our galaxies into two samples, i.e. galaxies with and without emission lines, we find significant differences in their luminosity functions. In particular, galaxies with emission lines show a significantly steeper slope and a fainter M^*^. The amplitude and the α and M^*^ parameters of our luminosity function are in good agreement with those of the AUTOFIB redshift survey (Ellis et al. 1996). Vice-versa, our amplitude is significantly higher, by a factor ~1.6 at M~M^*^, than that found for both the Stromlo-APM (Loveday et al. 1992) and the Las Campanas (Lin et al. 1996) redshift surveys. Also the faint end slope of our luminosity function is significantly steeper than that found in these two surveys. The galaxy number density for M_bJ_<=-16+5logh is well determined (n{bar}=0.08+/-0.015h^3^/Mpc^3^). Its estimate for M_bJ_<=-12.4+5logh is more uncertain, ranging from n{bar}=0.28h

  18. THE GALACTIC O-STAR SPECTROSCOPIC SURVEY (GOSSS). II. BRIGHT SOUTHERN STARS

    SciTech Connect

    Sota, A.; Apellániz, J. Maíz; Alfaro, E. J.; Barbá, R. H.; Arias, J. I.; Walborn, N. R.; Gamen, R. C.

    2014-03-01

    We present the second installment of GOSSS, a massive spectroscopic survey of Galactic O stars, based on new homogeneous, high signal-to-noise ratio, R ∼ 2500 digital observations from both hemispheres selected from the Galactic O-Star Catalog (GOSC). In this paper we include bright stars and other objects drawn mostly from the first version of GOSC, all of them south of δ = –20°, for a total number of 258 O stars. We also revise the northern sample of Paper I to provide the full list of spectroscopically classified Galactic O stars complete to B = 8, bringing the total number of published GOSSS stars to 448. Extensive sequences of exceptional objects are given, including the early Of/WN, O Iafpe, Ofc, ON/OC, Onfp, Of?p, and Oe types, as well as double/triple-lined spectroscopic binaries. The new spectral subtype O9.2 is also discussed. The magnitude and spatial distributions of the observed sample are analyzed. We also present new results from OWN, a multi-epoch high-resolution spectroscopic survey coordinated with GOSSS that is assembling the largest sample of Galactic spectroscopic massive binaries ever attained. The OWN data combined with additional information on spectroscopic and visual binaries from the literature indicate that only a very small fraction (if any) of the stars with masses above 15-20 M {sub ☉} are born as single systems. In the future we will publish the rest of the GOSSS survey, which is expected to include over 1000 Galactic O stars.

  19. Deep Chandra Survey of the Small Magellanic Cloud. II. Timing Analysis of X-Ray Pulsars

    NASA Astrophysics Data System (ADS)

    Hong, JaeSub; Antoniou, Vallia; Zezas, Andreas; Haberl, Frank; Sasaki, Manami; Drake, Jeremy J.; Plucinsky, Paul P.; Laycock, Silas

    2017-09-01

    We report the timing analysis results of X-ray pulsars from a recent deep Chandra survey of the Small Magellanic Cloud (SMC). We analyzed a total exposure of 1.4 Ms from 31 observations over a 1.2 deg2 region in the SMC under a Chandra X-ray Visionary Program. Using the Lomb–Scargle and epoch-folding techniques, we detected periodic modulations from 20 pulsars and a new candidate pulsar. The survey also covered 11 other pulsars with no clear sign of periodic modulation. The 0.5–8 keV X-ray luminosity (L X ) of the pulsars ranges from 1034 to 1037 erg s‑1 at 60 kpc. All of the Chandra sources with L X ≳ 4 × 1035 erg s‑1 exhibit X-ray pulsations. The X-ray spectra of the SMC pulsars (and high-mass X-ray binaries) are in general harder than those of the SMC field population. All but SXP 8.02 can be fitted by an absorbed power-law model with a photon index of Γ ≲ 1.5. The X-ray spectrum of the known magnetar SXP 8.02 is better fitted with a two-temperature blackbody model. Newly measured pulsation periods of SXP 51.0, SXP 214, and SXP 701, are significantly different from the previous XMM-Newton and RXTE measurements. This survey provides a rich data set for energy-dependent pulse profile modeling. Six pulsars show an almost eclipse-like dip in the pulse profile. Phase-resolved spectral analysis reveals diverse spectral variations during pulsation cycles: e.g., for an absorbed power-law model, some exhibit an (anti)-correlation between absorption and X-ray flux, while others show more intrinsic spectral variation (i.e., changes in photon indices).

  20. Intrinsic galaxy shapes and alignments - II. Modelling the intrinsic alignment contamination of weak lensing surveys

    NASA Astrophysics Data System (ADS)

    Joachimi, B.; Semboloni, E.; Hilbert, S.; Bett, P. E.; Hartlap, J.; Hoekstra, H.; Schneider, P.

    2013-11-01

    Intrinsic galaxy alignments constitute the major astrophysical systematic of forthcoming weak gravitational lensing surveys but also yield unique insights into galaxy formation and evolution. We build analytic models for the distribution of galaxy shapes based on halo properties extracted from the Millennium Simulation, differentiating between early- and late-type galaxies as well as central galaxies and satellites. The resulting ellipticity correlations are investigated for their physical properties and compared to a suite of current observations. The best-faring model is then used to predict the intrinsic alignment contamination of planned weak lensing surveys. We find that late-type galaxy models generally have weak intrinsic ellipticity correlations, marginally increasing towards smaller galaxy separation and higher redshift. The signal for early-type models at fixed halo mass strongly increases by three orders of magnitude over two decades in galaxy separation, and by one order of magnitude from z = 0 to z = 2. The intrinsic alignment strength also depends strongly on halo mass, but not on galaxy luminosity at fixed mass, or galaxy number density in the environment. We identify models that are in good agreement with all observational data, except that all models overpredict alignments of faint early-type galaxies. The best model yields an intrinsic alignment contamination of a Euclid-like survey between 0.5 and 10 per cent at z > 0.6 and on angular scales larger than a few arcminutes. Cutting 20 per cent of red foreground galaxies using observer-frame colours can suppress this contamination by up to a factor of 2.

  1. The Chandra planetary nebula survey (CHANPLANS). II. X-ray emission from compact planetary nebulae

    SciTech Connect

    Freeman, M.; Kastner, J. H.; Montez, R. Jr.; Balick, B.; Frew, D. J.; De Marco, O.; Parker, Q. A.; Jones, D.; Miszalski, B.; Sahai, R.; Blackman, E.; Frank, A.; Chu, Y.-H.; Guerrero, M. A.; Zijlstra, A.; Bujarrabal, V.; Corradi, R. L. M.; Nordhaus, J.; and others

    2014-10-20

    We present results from the most recent set of observations obtained as part of the Chandra X-ray observatory Planetary Nebula Survey (CHANPLANS), the first comprehensive X-ray survey of planetary nebulae (PNe) in the solar neighborhood (i.e., within ∼1.5 kpc of the Sun). The survey is designed to place constraints on the frequency of appearance and range of X-ray spectral characteristics of X-ray-emitting PN central stars and the evolutionary timescales of wind-shock-heated bubbles within PNe. CHANPLANS began with a combined Cycle 12 and archive Chandra survey of 35 PNe. CHANPLANS continued via a Chandra Cycle 14 Large Program which targeted all (24) remaining known compact (R {sub neb} ≲ 0.4 pc), young PNe that lie within ∼1.5 kpc. Results from these Cycle 14 observations include first-time X-ray detections of hot bubbles within NGC 1501, 3918, 6153, and 6369, and point sources in HbDs 1, NGC 6337, and Sp 1. The addition of the Cycle 14 results brings the overall CHANPLANS diffuse X-ray detection rate to ∼27% and the point source detection rate to ∼36%. It has become clearer that diffuse X-ray emission is associated with young (≲ 5 × 10{sup 3} yr), and likewise compact (R {sub neb} ≲ 0.15 pc), PNe with closed structures and high central electron densities (n{sub e} ≳ 1000 cm{sup –3}), and is rarely associated with PNe that show H{sub 2} emission and/or pronounced butterfly structures. Hb 5 is one such exception of a PN with a butterfly structure that hosts diffuse X-ray emission. Additionally, two of the five new diffuse X-ray detections (NGC 1501 and NGC 6369) host [WR]-type central stars, supporting the hypothesis that PNe with central stars of [WR]-type are likely to display diffuse X-ray emission.

  2. The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars

    NASA Astrophysics Data System (ADS)

    Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J.

    2014-03-01

    We present the second installment of GOSSS, a massive spectroscopic survey of Galactic O stars, based on new homogeneous, high signal-to-noise ratio, R ~ 2500 digital observations from both hemispheres selected from the Galactic O-Star Catalog (GOSC). In this paper we include bright stars and other objects drawn mostly from the first version of GOSC, all of them south of δ = -20°, for a total number of 258 O stars. We also revise the northern sample of Paper I to provide the full list of spectroscopically classified Galactic O stars complete to B = 8, bringing the total number of published GOSSS stars to 448. Extensive sequences of exceptional objects are given, including the early Of/WN, O Iafpe, Ofc, ON/OC, Onfp, Of?p, and Oe types, as well as double/triple-lined spectroscopic binaries. The new spectral subtype O9.2 is also discussed. The magnitude and spatial distributions of the observed sample are analyzed. We also present new results from OWN, a multi-epoch high-resolution spectroscopic survey coordinated with GOSSS that is assembling the largest sample of Galactic spectroscopic massive binaries ever attained. The OWN data combined with additional information on spectroscopic and visual binaries from the literature indicate that only a very small fraction (if any) of the stars with masses above 15-20 M ⊙ are born as single systems. In the future we will publish the rest of the GOSSS survey, which is expected to include over 1000 Galactic O stars. The GOSSS spectroscopic data in this article were gathered with one primary facility, the 2.5 m du Pont Telescope at Las Campanas Observatory (LCO), and three auxiliary ones, the 1.5 m Telescope at the Observatorio de Sierra Nevada (OSN), the 3.5 m Telescope at Calar Alto Observatory (CAHA), and the 4.2 m William Hershel Telescope at Observatorio del Roque de los Muchachos (ORM). The OWN spectroscopic data were gathered at LCO, La Silla Observatory, and CASLEO. Some of the supporting imaging data were obtained by

  3. The Extended GMRT Radio Halo Survey. II. Further results and analysis of the full sample

    NASA Astrophysics Data System (ADS)

    Kale, R.; Venturi, T.; Giacintucci, S.; Dallacasa, D.; Cassano, R.; Brunetti, G.; Cuciti, V.; Macario, G.; Athreya, R.

    2015-07-01

    The intra-cluster medium contains cosmic rays and magnetic fields that are manifested through the large scale synchrotron sources, termed radio haloes, relics, and mini-haloes. The Extended Giant Metrewave Radio Telescope (GMRT) Radio Halo Survey (EGRHS) is an extension of the GMRT Radio Halo Survey (GRHS) designed to search for radio haloes using GMRT 610/235 MHz observations. The GRHS and EGRHS consists of 64 clusters in the redshift range 0.2-0.4 that have an X-ray luminosity larger than 5 × 1044 erg s-1 in the 0.1-2.4 keV band and declination, δ > -31° in the REFLEX and eBCS X-ray cluster catalogues. In this second paper in the series, GMRT 610/235 MHz data on the last batch of 11 galaxy clusters and the statistical analysis of the full sample are presented. A new mini-halo in RX J2129.6+0005 and candidate diffuse sources in Z5247, A2552, and Z1953 have been discovered. A unique feature of this survey are the upper limits on the detections of 1 Mpc sized radio haloes; 4 new are presented here, making a total of 31 in the survey. Of the sample, 58 clusters with adequately sensitive radio information were used to obtain the most accurate occurrence fractions so far. The occurrence fractions of radio haloes, mini-haloes and relics in our sample are ~22%, ~16% and ~5%, respectively. The P1.4 GHz-LX diagrams for the radio haloes and mini-haloes are presented. The morphological estimators - centroid shift (w), concentration parameter (c), and power ratios (P3/P0) derived from the Chandra X-ray images - are used as proxies for the dynamical states of the GRHS and EGRHS clusters. The clusters with radio haloes and mini-haloes occupy distinct quadrants in the c-w, c-P3/P0 and w-P3/P0 planes, corresponding to the more and less morphological disturbance, respectively. The non-detections span both the quadrants. Appendices are available in electronic form at http://www.aanda.org

  4. Characterising large-scale structure with the REFLEX II cluster survey

    NASA Astrophysics Data System (ADS)

    Chon, Gayoung

    2016-10-01

    We study the large-scale structure with superclusters from the REFLEX X-ray cluster survey together with cosmological N-body simulations. It is important to construct superclusters with criteria such that they are homogeneous in their properties. We lay out our theoretical concept considering future evolution of superclusters in their definition, and show that the X-ray luminosity and halo mass functions of clusters in superclusters are found to be top-heavy, different from those of clusters in the field. We also show a promising aspect of using superclusters to study the local cluster bias and mass scaling relation with simulations.

  5. The Sloan Digital Sky Survey-II: Photometry and Supernova Ia Light Curves from the 2005 Data

    SciTech Connect

    Holtzman, Jon A.; Marriner, John; Kessler, Richard; Sako, Masao; Dilday, Ben; Frieman, Joshua A.; Schneider, Donald P.; Bassett, Bruce; Becker, Andrew; Cinabro, David; DeJongh, Fritz; Depoy, Darren L.; Doi, Mamoru; Garnavich, Peter M.; Hogan, Craig J.; Jha, Saurabh; Konishi, Kohki; Lampeitl, Hubert; Marshall, Jennifer L.; McGinnis, David; Miknaitis, Gajus; /KICP, Chicago /Portsmouth U., ICG /Ohio State U., Dept. Astron. /Baltimore, Space Telescope Sci. /Johns Hopkins U. /Rochester Inst. Tech. /KIPAC, Menlo Park /Portsmouth U., ICG /Tokyo U., Inst. Astron. /South African Astron. Observ. /Cape Town U. /Tokyo U., ICRR /KIPAC, Menlo Park

    2010-08-26

    We present ugriz light curves for 146 spectroscopically confirmed or spectroscopically probable Type Ia supernovae from the 2005 season of the SDSS-II Supernova survey. The light curves have been constructed using a photometric technique that we call scene modeling, which is described in detail here; the major feature is that supernova brightnesses are extracted from a stack of images without spatial resampling or convolution of the image data. This procedure produces accurate photometry along with accurate estimates of the statistical uncertainty, and can be used to derive photometry taken with multiple telescopes. We discuss various tests of this technique that demonstrate its capabilities. We also describe the methodology used for the calibration of the photometry, and present calibrated magnitudes and fluxes for all of the spectroscopic SNe Ia from the 2005 season.

  6. Preliminary Results of Detailed Chemical Abundance Analysis of Milky Way Satellite Galaxy Reticulum II Discovered in the Dark Energy Survey

    NASA Astrophysics Data System (ADS)

    Nagasawa, Daniel; Marshall, Jennifer L.; Li, Ting; Dark Energy Survey Milky Way Science Group

    2016-01-01

    We present preliminary results from abundance analysis of stars in Milky Way satellite galaxies found in the Dark Energy Survey (DES). DES has discovered 16 candidate satellite galaxies of the Milky Way in its first two years of operation. Since January 2015, three candidates have subsequently been revealed to be dark matter-dominated by spectroscopic follow-up studies of their kinematics, confirming their status as satellite galaxies. Spectroscopic follow-up of the remaining 13 candidates is underway. We have analyzed high resolution VLT/GIRAFFE spectra of member stars in one of these satellite galaxies, Reticulum II. Using equivalent width measurement and spectral synthesis methods, we measure the abundances of Iron and other species in order to begin to understand the chemical content of these Milky Way satellites.

  7. A Redshift Survey of IRAS Galaxies. II. Methods for Determining Self-consistent Velocity and Density Fields: Erratum

    NASA Astrophysics Data System (ADS)

    Yahil, Amos; Strauss, Michael A.; Davis, Marc; Huchra, John P.

    1991-11-01

    In the paper, "A Redshift Survey of IRAS Galaxies. II. Methods for Determining Self-consistent Velocity and Density Fields" by Amos Yahil, Michael A. Strauss, Marc Davis, and John P. Huchra (ApJ, 372,380 [1991]), Figures 14 and 15 were presented out of order, with their legends reversed. Thus, the figure at the bottom of page 391 is Figure 15, and should have the legend: "Fig. 15.-As in Fig. 13, for the method 3 results." The figure at the top of page 392 is Figure 14, and should have the legend: "Fig. 14.-Plot in Galactic coordinates of the quantity V_diff_ for galaxies within 3000 km s^-1^ of the LG. The symbol size is proportional to V_diff_ - 400 km s^-1^, which measures the deviation of the redshift- distance relation along the line of sight to that galaxy from pure Hubble flow."

  8. THE CHANDRA SURVEY OF THE COSMOS FIELD. II. SOURCE DETECTION AND PHOTOMETRY

    SciTech Connect

    Puccetti, S.; Vignali, C.; Cappelluti, N.; Brunner, H.; Brusa, M.; Fruscione, A.; Finoguenov, A.; Fiore, F.; Zamorani, G.; Gilli, R.; Comastri, A.; Aldcroft, T. L.; Elvis, M.; Civano, F.; Miyaji, T.; Damiani, F.; Koekemoer, A. M.; Mainieri, V.

    2009-12-01

    The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8 Ms, Chandra program that covers the central contiguous {approx}0.92 deg{sup 2} of the COSMOS field. C-COSMOS is the result of a complex tiling, with every position being observed in up to six overlapping pointings (four overlapping pointings in most of the central {approx}0.45 deg{sup 2} area with the best exposure, and two overlapping pointings in most of the surrounding area, covering an additional {approx}0.47 deg{sup 2}). Therefore, the full exploitation of the C-COSMOS data requires a dedicated and accurate analysis focused on three main issues: (1) maximizing the sensitivity when the point-spread function (PSF) changes strongly among different observations of the same source (from {approx}1 arcsec up to {approx}10 arcsec half-power radius); (2) resolving close pairs; and (3) obtaining the best source localization and count rate. We present here our treatment of four key analysis items: source detection, localization, photometry, and survey sensitivity. Our final procedure consists of a two step procedure: (1) a wavelet detection algorithm to find source candidates and (2) a maximum likelihood PSF fitting algorithm to evaluate the source count rates and the probability that each source candidate is a fluctuation of the background. We discuss the main characteristics of this procedure, which was the result of detailed comparisons between different detection algorithms and photometry tools, calibrated with extensive and dedicated simulations.

  9. THE TAIWANESE-AMERICAN OCCULTATION SURVEY PROJECT STELLAR VARIABILITY. II. DETECTION OF 15 VARIABLE STARS

    SciTech Connect

    Mondal, S.; Lin, C. C.; Chen, W. P.; Zhang, Z.-W.; Lin, H.-C.; Alcock, C.; Bianco, F. B.; Lehner, M. J.; Protopapas, P.; Axelrod, T.; Byun, Y.-I.; Kim, D.-W.; Coehlo, N. K.; Rice, J. A.; Cook, K. H.; Marshall, S. L.; Dave, R.; King, S.-K.; Lee, T.; Schwamb, M. E.

    2010-05-15

    The Taiwanese-American Occultation Survey (TAOS) project has collected more than a billion photometric measurements since 2005 January. These sky survey data-covering timescales from a fraction of a second to a few hundred days-are a useful source to study stellar variability. A total of 167 star fields, mostly along the ecliptic plane, have been selected for photometric monitoring with the TAOS telescopes. This paper presents our initial analysis of a search for periodic variable stars from the time-series TAOS data on one particular TAOS field, No. 151 (R.A. = 17{sup h}30{sup m}6.{sup s}7, decl. = 27{sup 0}17'30'', J2000), which had been observed over 47 epochs in 2005. A total of 81 candidate variables are identified in the 3 deg{sup 2} field, with magnitudes in the range 8 < R < 16. On the basis of the periodicity and shape of the light curves, 29 variables, 15 of which were previously unknown, are classified as RR Lyrae, Cepheid, {delta} Scuti, SX Phonencis, semi-regular, and eclipsing binaries.

  10. Emission Line Galaxies in the STIS Parallel Survey II: Star Formation Density

    NASA Technical Reports Server (NTRS)

    Teplitz, Harry I.; Collins, Nicholas R.; Gardner, Jonathan P.; Hill, Robert S.; Rhodes, Jason

    2002-01-01

    We present the luminosity function of [OII]-emitting galaxies at a median redshift of z = 0.9, as measured in the deep spectroscopic data in the STIS Parallel Survey (SPS). The luminosity function shows strong evolution from the local value, as expected. By using random lines of sight, the SPS measurement complements previous deep single field studies. We calculate the density of inferred star formation at this redshift by converting from [OII] to H(alpha) line flux as a function of absolute magnitude and find rho = 0.052 +/- 0.017 Solar mass/yr Mpc(sup -3) at a median redshift z approx. 0.9 within the range 0.46 less than z less than 1.415 (H(sub 0) = 50 km/s Mpc(sup -l), Omega(sub M) = 1.0, Omega(sub lambda) = 0.0). This density is consistent with a (1 + z)(sup )4 evolution in global star formation since z approx. 1. To reconcile the density with similar measurements made by surveys targeting H(alpha) may require substantial extinction correction.

  11. THE SWIFT UVOT STARS SURVEY. II. RR LYRAE STARS IN M3 AND M15

    SciTech Connect

    Siegel, Michael H.; Porterfield, Blair L.; Balzer, Benjamin G.; Hagen, Lea M. Z. E-mail: blp14@psu.edu E-mail: lea.zernow.hagen@gmail.com

    2015-10-15

    We present the first results of a near-ultraviolet (NUV) survey of RR Lyrae stars from the Ultraviolet Optical Telescope (UVOT) on board the Swift Gamma-ray Burst Mission. It is well-established that RR Lyrae stars have large amplitudes in the far- and near-ultraviolet. We have used UVOT’s unique wide-field NUV imaging capability to perform the first systematic NUV survey of variable stars in the Galactic globular clusters M3 and M15. We identify 280 variable stars, comprised of 275 RR Lyrae, 2 anomalous Cepheids, 1 classical Cepheid, 1 SX Phoenicis star, and 1 possible long-period or irregular variable. Only two of these are new discoveries. We compare our results to previous investigations and find excellent agreement in the periods with significantly larger amplitudes in the NUV. We map out, for the first time, an NUV Bailey diagram from globular clusters, showing the usual loci for fundamental mode RRab and first overtone RRc pulsators. We show the unique sensitivity of NUV photometry to both the temperatures and the surface gravities of RR Lyrae stars. Finally, we show evidence of an NUV period–metallicity–luminosity relationship. Future investigations will further examine the dependence of NUV pulsation parameters on metallicity and Oosterhoff classification.

  12. A Spectroscopic Survey of the ClassII YSO Population in the LkH(alpha)101 Region

    NASA Astrophysics Data System (ADS)

    Fleming, Scott; Lada, Elizabeth; Marinas, Naibi; Ybarra, Jason

    2010-08-01

    We propose to use the FLAMINGOS multi-object, near-IR spectrograph on the KPNO 4-m telescope to conduct a spectroscopic survey of previously-identified ClassII (``T Tauri'') YSO's in the LkH(alpha)101 star forming region. LkH(alpha)101 is a Herbig star with an associated population of ~ 150 YSOs. It is a member of the California Nebula, recently determined to be of comparable distance and size to the Orion Nebula, yet with significantly less star formation. We will use pre- existing FLAMINGOS photometry, combined with these spectra, to determine effective temperatures and luminosities for 72 ClassII YSO's. We will search for any age or mass distributions amongst the YSOs using theoretical tracks on the HR diagram. Finally, we will use these spectroscopic observations to constrain the effective temperatures and luminosities of the central sources when performing SED analysis to derive disk properties. The spatial distribution and environmental dependence of T Tauri disk properties in LkH(alpha)101 will then be explored. Additional targets on each multi-object mask will be used to search for substellar objects in the region to explore the low-end of the mass function.

  13. THE HST/ACS COMA CLUSTER SURVEY. II. DATA DESCRIPTION AND SOURCE CATALOGS

    SciTech Connect

    Hammer, Derek; Verdoes Kleijn, Gijs; Den Brok, Mark; Peletier, Reynier F.; Hoyos, Carlos; Balcells, Marc; Aguerri, Alfonso L.; Ferguson, Henry C.; Goudfrooij, Paul; Carter, David; Guzman, Rafael; Smith, Russell J.; Lucey, John R.; Graham, Alister W.; Trentham, Neil; Peng, Eric; Puzia, Thomas H.; Jogee, Shardha; Batcheldor, Dan; Bridges, Terry J.

    2010-11-15

    The Coma cluster, Abell 1656, was the target of an HST-ACS Treasury program designed for deep imaging in the F475W and F814W passbands. Although our survey was interrupted by the ACS instrument failure in early 2007, the partially completed survey still covers {approx}50% of the core high-density region in Coma. Observations were performed for 25 fields that extend over a wide range of cluster-centric radii ({approx}1.75 Mpc or 1{sup 0}) with a total coverage area of 274 arcmin{sup 2}. The majority of the fields are located near the core region of Coma (19/25 pointings) with six additional fields in the southwest region of the cluster. In this paper, we present reprocessed images and SEXTRACTOR source catalogs for our survey fields, including a detailed description of the methodology used for object detection and photometry, the subtraction of bright galaxies to measure faint underlying objects, and the use of simulations to assess the photometric accuracy and completeness of our catalogs. We also use simulations to perform aperture corrections for the SEXTRACTOR Kron magnitudes based only on the measured source flux and its half-light radius. We have performed photometry for {approx}73,000 unique objects; approximately one-half of our detections are brighter than the 10{sigma} point-source detection limit at F814W = 25.8 mag (AB). The slight majority of objects (60%) are unresolved or only marginally resolved by ACS. We estimate that Coma members are 5%-10% of all source detections, which consist of a large population of unresolved compact sources (primarily globular clusters but also ultra-compact dwarf galaxies) and a wide variety of extended galaxies from a cD galaxy to dwarf low surface brightness galaxies. The red sequence of Coma member galaxies has a color-magnitude relation with a constant slope and dispersion over 9 mag (-21 < M {sub F814W} < -13). The initial data release for the HST-ACS Coma Treasury program was made available to the public in 2008

  14. The HST/ACS Coma Cluster Survey. II. Data Description and Source Catalogs

    NASA Astrophysics Data System (ADS)

    Hammer, Derek; Verdoes Kleijn, Gijs; Hoyos, Carlos; den Brok, Mark; Balcells, Marc; Ferguson, Henry C.; Goudfrooij, Paul; Carter, David; Guzmán, Rafael; Peletier, Reynier F.; Smith, Russell J.; Graham, Alister W.; Trentham, Neil; Peng, Eric; Puzia, Thomas H.; Lucey, John R.; Jogee, Shardha; Aguerri, Alfonso L.; Batcheldor, Dan; Bridges, Terry J.; Chiboucas, Kristin; Davies, Jonathan I.; del Burgo, Carlos; Erwin, Peter; Hornschemeier, Ann; Hudson, Michael J.; Huxor, Avon; Jenkins, Leigh; Karick, Arna; Khosroshahi, Habib; Kourkchi, Ehsan; Komiyama, Yutaka; Lotz, Jennifer; Marzke, Ronald O.; Marinova, Irina; Matkovic, Ana; Merritt, David; Miller, Bryan W.; Miller, Neal A.; Mobasher, Bahram; Mouhcine, Mustapha; Okamura, Sadanori; Percival, Sue; Phillipps, Steven; Poggianti, Bianca M.; Price, James; Sharples, Ray M.; Tully, R. Brent; Valentijn, Edwin

    2010-11-01

    The Coma cluster, Abell 1656, was the target of an HST-ACS Treasury program designed for deep imaging in the F475W and F814W passbands. Although our survey was interrupted by the ACS instrument failure in early 2007, the partially completed survey still covers ~50% of the core high-density region in Coma. Observations were performed for 25 fields that extend over a wide range of cluster-centric radii (~1.75 Mpc or 1°) with a total coverage area of 274 arcmin2. The majority of the fields are located near the core region of Coma (19/25 pointings) with six additional fields in the southwest region of the cluster. In this paper, we present reprocessed images and SEXTRACTOR source catalogs for our survey fields, including a detailed description of the methodology used for object detection and photometry, the subtraction of bright galaxies to measure faint underlying objects, and the use of simulations to assess the photometric accuracy and completeness of our catalogs. We also use simulations to perform aperture corrections for the SEXTRACTOR Kron magnitudes based only on the measured source flux and its half-light radius. We have performed photometry for ~73,000 unique objects; approximately one-half of our detections are brighter than the 10σ point-source detection limit at F814W = 25.8 mag (AB). The slight majority of objects (60%) are unresolved or only marginally resolved by ACS. We estimate that Coma members are 5%-10% of all source detections, which consist of a large population of unresolved compact sources (primarily globular clusters but also ultra-compact dwarf galaxies) and a wide variety of extended galaxies from a cD galaxy to dwarf low surface brightness galaxies. The red sequence of Coma member galaxies has a color-magnitude relation with a constant slope and dispersion over 9 mag (-21 < M F814W < -13). The initial data release for the HST-ACS Coma Treasury program was made available to the public in 2008 August. The images and catalogs described in

  15. The XXL Survey. II. The bright cluster sample: catalogue and luminosity function

    NASA Astrophysics Data System (ADS)

    Pacaud, F.; Clerc, N.; Giles, P. A.; Adami, C.; Sadibekova, T.; Pierre, M.; Maughan, B. J.; Lieu, M.; Le Fèvre, J. P.; Alis, S.; Altieri, B.; Ardila, F.; Baldry, I.; Benoist, C.; Birkinshaw, M.; Chiappetti, L.; Démoclès, J.; Eckert, D.; Evrard, A. E.; Faccioli, L.; Gastaldello, F.; Guennou, L.; Horellou, C.; Iovino, A.; Koulouridis, E.; Le Brun, V.; Lidman, C.; Liske, J.; Maurogordato, S.; Menanteau, F.; Owers, M.; Poggianti, B.; Pomarède, D.; Pompei, E.; Ponman, T. J.; Rapetti, D.; Reiprich, T. H.; Smith, G. P.; Tuffs, R.; Valageas, P.; Valtchanov, I.; Willis, J. P.; Ziparo, F.

    2016-06-01

    Context. The XXL Survey is the largest survey carried out by the XMM-Newton satellite and covers a total area of 50 square degrees distributed over two fields. It primarily aims at investigating the large-scale structures of the Universe using the distribution of galaxy clusters and active galactic nuclei as tracers of the matter distribution. The survey will ultimately uncover several hundreds of galaxy clusters out to a redshift of ~2 at a sensitivity of ~10-14 erg s-1 cm-2 in the [0.5-2] keV band. Aims: This article presents the XXL bright cluster sample, a subsample of 100 galaxy clusters selected from the full XXL catalogue by setting a lower limit of 3 × 10-14 erg s-1 cm-2 on the source flux within a 1' aperture. Methods: The selection function was estimated using a mixture of Monte Carlo simulations and analytical recipes that closely reproduce the source selection process. An extensive spectroscopic follow-up provided redshifts for 97 of the 100 clusters. We derived accurate X-ray parameters for all the sources. Scaling relations were self-consistently derived from the same sample in other publications of the series. On this basis, we study the number density, luminosity function, and spatial distribution of the sample. Results: The bright cluster sample consists of systems with masses between M500 = 7 × 1013 and 3 × 1014 M⊙, mostly located between z = 0.1 and 0.5. The observed sky density of clusters is slightly below the predictions from the WMAP9 model, and significantly below the prediction from the Planck 2015 cosmology. In general, within the current uncertainties of the cluster mass calibration, models with higher values of σ8 and/or ΩM appear more difficult to accommodate. We provide tight constraints on the cluster differential luminosity function and find no hint of evolution out to z ~ 1. We also find strong evidence for the presence of large-scale structures in the XXL bright cluster sample and identify five new superclusters. Based on

  16. Halo WD Local Space Density from the GSC-II-based Survey

    NASA Astrophysics Data System (ADS)

    Carollo, D.; Bucciarelli, B.; Hodgkin, S. T.; Lattanzi, M. G.; McLean, B.; Smart, R. L.; Spagna, A.

    2007-09-01

    Microlensing experiments (Alcock et al. 2000) have suggested that a significant part of the dark halo of the Milky Way could be composed of matter in the form of massive compact halo objects (MACHOs). Cool ancient white dwarfs (WDs) are the natural candidates. Here we present the results of the GSC2 survey of halo WDs, including a description of the WD sample, and a derivation of the local space density of halo WDs by means of an accurate kinematic analysis. The local space density of these objects is shown to be only about ˜ 10-5M⊙pc-3, corresponding to 0.1%--0.2% of the local dark matter.

  17. Redshifts for fainter galaxies in the first CfA survey slice. II

    NASA Technical Reports Server (NTRS)

    Wegner, Gary; Thorstensen, John R.; Kurtz, Michael J.; Geller, Margaret J.; Huchra, John P.

    1990-01-01

    Redshifts were measured for 96 galaxies in right ascension alpha between 8h and 17h declination delta between 30 and 31 deg, and with m(Zwicky) in the range 15.6-15.7. These correspond to 94 of the 96 entries in the Zwicky-Nilson merged catalog. The declination range delta between 29 deg and 31 deg is now complete to m(Zwicky) = 15.7. The structures in the first 6-deg-wide slice of the Center for Astrophysics redshift survey slice (delta between 26.5 and 32.5 deg are clearly defined in the 2-deg-wide slightly deeper sample; the fainter galaxies trace the structures defined by the brighter ones.

  18. The Herschel Virgo Cluster Survey . II. Truncated dust disks in H I-deficient spirals

    NASA Astrophysics Data System (ADS)

    Cortese, L.; Davies, J. I.; Pohlen, M.; Baes, M.; Bendo, G. J.; Bianchi, S.; Boselli, A.; De Looze, I.; Fritz, J.; Verstappen, J.; Bomans, D. J.; Clemens, M.; Corbelli, E.; Dariush, A.; di Serego Alighieri, S.; Fadda, D.; Garcia-Appadoo, D. A.; Gavazzi, G.; Giovanardi, C.; Grossi, M.; Hughes, T. M.; Hunt, L. K.; Jones, A. P.; Madden, S.; Pierini, D.; Sabatini, S.; Smith, M. W. L.; Vlahakis, C.; Xilouris, E. M.; Zibetti, S.

    2010-07-01

    By combining Herschel-SPIRE observations obtained as part of the Herschel Virgo Cluster Survey with 21 cm Hi data from the literature, we investigate the role of the cluster environment on the dust content of Virgo spiral galaxies. We show for the first time that the extent of the dust disk is significantly reduced in Hi-deficient galaxies, following remarkably well the observed “truncation” of the Hi disk. The ratio of the submillimetre-to-optical diameter correlates with the Hi-deficiency, suggesting that the cluster environment is able to strip dust as well as gas. These results provide important insights not only into the evolution of cluster galaxies but also into the metal enrichment of the intra-cluster medium. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.

  19. Superclusters of galaxies from the 2dF redshift survey. II. Comparison with simulations

    NASA Astrophysics Data System (ADS)

    Einasto, J.; Einasto, M.; Saar, E.; Tago, E.; Liivamägi, L. J.; Jõeveer, M.; Suhhonenko, I.; Hütsi, G.; Jaaniste, J.; Heinämäki, P.; Müller, V.; Knebe, A.; Tucker, D.

    2007-02-01

    Aims:We investigate properties of superclusters of galaxies found in of the 2dF Galaxy Redshift Survey, and compare them with properties of superclusters from the Millennium Simulation. Methods: We study the dependence of various characteristics of superclusters on their distance from the observer, on their total luminosity, and on their multiplicity. The multiplicity is defined by the number of Density Field (DF) clusters in superclusters. Using the multiplicity we divide superclusters into four richness classes: poor, medium, rich and extremely rich. Results: We show that superclusters are asymmetrical and have a multi-branching filamentary structure, with the degree of asymmetry and filamentarity being higher for the more luminous and richer superclusters. The comparison of real superclusters with Millennium superclusters shows that most properties of simulated superclusters agree very well with real data, the main differences being in the luminosity and multiplicity distributions.

  20. THE SWIFT AGN AND CLUSTER SURVEY. II. CLUSTER CONFIRMATION WITH SDSS DATA

    SciTech Connect

    Griffin, Rhiannon D.; Dai, Xinyu; Kochanek, Christopher S.; Bregman, Joel N. E-mail: xdai@ou.edu E-mail: jbregman@umich.edu

    2016-01-15

    We study 203 (of 442) Swift AGN and Cluster Survey extended X-ray sources located in the SDSS DR8 footprint to search for galaxy over-densities in three-dimensional space using SDSS galaxy photometric redshifts and positions near the Swift cluster candidates. We find 104 Swift clusters with a >3σ galaxy over-density. The remaining targets are potentially located at higher redshifts and require deeper optical follow-up observations for confirmation as galaxy clusters. We present a series of cluster properties including the redshift, brightest cluster galaxy (BCG) magnitude, BCG-to-X-ray center offset, optical richness, and X-ray luminosity. We also detect red sequences in ∼85% of the 104 confirmed clusters. The X-ray luminosity and optical richness for the SDSS confirmed Swift clusters are correlated and follow previously established relations. The distribution of the separations between the X-ray centroids and the most likely BCG is also consistent with expectation. We compare the observed redshift distribution of the sample with a theoretical model, and find that our sample is complete for z ≲ 0.3 and is still 80% complete up to z ≃ 0.4, consistent with the SDSS survey depth. These analysis results suggest that our Swift cluster selection algorithm has yielded a statistically well-defined cluster sample for further study of cluster evolution and cosmology. We also match our SDSS confirmed Swift clusters to existing cluster catalogs, and find 42, 23, and 1 matches in optical, X-ray, and Sunyaev–Zel’dovich catalogs, respectively, and so the majority of these clusters are new detections.

  1. A Deep Multicolor Survey. II. Initial Spectroscopy and Comparison with Expected Quasar Number Counts

    NASA Astrophysics Data System (ADS)

    Hall, Patrick B.; Osmer, Patrick S.; Green, Richard F.; Porter, Alain C.; Warren, Stephen J.

    1996-05-01

    We have used the KPNO 4 m Mayall telescope to image 0.83 deg^2^ of sky in six fields at high Galactic latitude in six filters spanning 3000- 10000 A to magnitude limits ranging from 22.1 to 23.8. As a first use of this database, we have conducted a multicolor survey for quasars. We discuss various methods of selecting outliers in different color-color diagrams and multicolor space that have been used to identify quasars at all redshifts from their colors alone. We discuss the initial results of our program of spectroscopic identification which has so far resulted in the identification of over 40 faint quasars, including one at z > 4, a similar number of compact narrow emission-line galaxies, and a number of unusual and potentially interesting stars. We use these spectroscopic results, along with extensive simulations of quasar spectra, to study the efficiency of our candidate selection procedures. Finally, we compare the number counts of our quasars and quasar candidates to the expected numbers based on previous studies of the quasar luminosity function. The agreement of our observations with these expectations is good in most cases. However, we do estimate that our survey contains more quasars with B < 21 and z < 2.3 than expected from the results published by Koo & Kron in 1988 and more z > 3 quasars than expected from the results published by Warren, Hewett, & Osmer in 1994, both at the 3 σ level. Additional spectroscopic observations will be required to confirm or refute these excesses.

  2. The High Time Resolution Universe Pulsar Survey - II. Discovery of five millisecond pulsars

    NASA Astrophysics Data System (ADS)

    Bates, S. D.; Bailes, M.; Bhat, N. D. R.; Burgay, M.; Burke-Spolaor, S.; D'Amico, N.; Jameson, A.; Johnston, S.; Keith, M. J.; Kramer, M.; Levin, L.; Lyne, A.; Milia, S.; Possenti, A.; Stappers, B.; van Straten, W.

    2011-10-01

    We present the discovery of five millisecond pulsars found in the mid-Galactic latitude portion of the High Time Resolution Universe (HTRU) survey. The pulsars have rotational periods from ˜2.3 ms to ˜7.5 ms, and all are in binary systems with orbital periods ranging from ˜0.3 to ˜150 d. In four of these systems, the most likely companion is a white dwarf, with minimum masses of ˜0.2 M⊙. The other pulsar, J1731-1847, has a very low mass companion and exhibits eclipses and is thus a member of the 'black widow' class of pulsar binaries. These eclipses have been observed in bands centred near frequencies of 700, 1400 and 3000 MHz, from which measurements have been made of the electron density in the eclipse region. These measurements have been used to examine some possible eclipse mechanisms. The eclipse and other properties of this source are used to perform a comparison with the other known eclipsing and 'black widow' pulsars. These new discoveries occupy a short-period and high-dispersion measure (DM) region of parameter space, which we demonstrate is a direct consequence of the high time and frequency resolution of the HTRU survey. The large implied distances to our new discoveries make observation of their companions unlikely with both current optical telescopes and the Fermi Gamma-ray Space Telescope. The extremely circular orbits make any advance of periastron measurements highly unlikely. No relativistic Shapiro delays are obvious in any of the systems although the low flux densities would make their detection difficult unless the orbits were fortuitously edge-on.

  3. Shocked POststarburst Galaxy Survey. II. The Molecular Gas Content and Properties of a Subset of SPOGs

    NASA Astrophysics Data System (ADS)

    Alatalo, Katherine; Lisenfeld, Ute; Lanz, Lauranne; Appleton, Philip N.; Ardila, Felipe; Cales, Sabrina L.; Kewley, Lisa J.; Lacy, Mark; Medling, Anne M.; Nyland, Kristina; Rich, Jeffrey A.; Urry, C. Meg

    2016-08-01

    We present CO(1-0) observations of objects within the Shocked POststarburst Galaxy Survey taken with the Institut de Radioastronomie Millimétrique 30 m single dish and the Combined Array for Research for Millimeter Astronomy interferometer. Shocked poststarburst galaxies (SPOGs) represent a transitioning population of galaxies, with deep Balmer absorption ({{EW}}{{H}δ }\\gt 5 {\\mathring{{A}}} ), consistent with an intermediate-age (A-star) stellar population, and ionized gas line ratios inconsistent with pure star formation. The CO(1-0) subsample was selected from SPOGs detected by the Wide-field Infrared Survey Explorer with 22 μm flux detected at a signal-to-noise ratio (S/N) > 3. Of the 52 objects observed in CO(1-0), 47 are detected with S/N > 3. A large fraction (37%-46% ± 7%) of our CO-SPOG sample were visually classified as morphologically disrupted. The H2 masses detected were between {10}8.7-10.8 {M}⊙ , consistent with the gas masses found in normal galaxies, though approximately an order of magnitude larger than the range seen in poststarburst galaxies. When comparing the 22 μm and CO(1-0) fluxes, SPOGs diverge from the normal star-forming relation, having 22 μm fluxes in excess of the relation by a factor of < {ɛ }{{MIR}}> ={4.91}-0.39+0.42, suggestive of the presence of active galactic nuclei (AGNs). The Na i D characteristics of CO-SPOGs show that it is likely that many of these objects host interstellar winds. Objects with large Na i D enhancements also tend to emit in the radio, suggesting possible AGN driving of neutral winds.

  4. ExploreNEOs. II. THE ACCURACY OF THE WARM SPITZER NEAR-EARTH OBJECT SURVEY

    SciTech Connect

    Harris, A. W.; Mommert, M.; Hora, J. L.; Fazio, G.; Smith, H. A.; Spahr, T. B.; Mueller, M.; Delbo, M.; Trilling, D. E.; Thomas, C. A.; Bhattacharya, B.; Chesley, S.; Mainzer, A.; Emery, J. P.; Penprase, B.; Stansberry, J. A.

    2011-03-15

    We report on results of observations of near-Earth objects (NEOs) performed with the NASA Spitzer Space Telescope as part of our ongoing (2009-2011) Warm Spitzer NEO survey ('ExploreNEOs'), the primary aim of which is to provide sizes and albedos of some 700 NEOs. The emphasis of the work described here is an assessment of the overall accuracy of our survey results, which are based on a semi-empirical generalized model of asteroid thermal emission. The NASA Spitzer Space Telescope has been operated in the so-called Warm Spitzer mission phase since the cryogen was depleted in 2009 May, with the two shortest-wavelength channels, centered at 3.6 {mu}m and 4.5 {mu}m, of the Infrared Array Camera continuing to provide valuable data. The set of some 170 NEOs in our current Warm Spitzer results catalog contains 28 for which published taxonomic classifications are available, and 14 for which relatively reliable published diameters and albedos are available. A comparison of the Warm Spitzer results with previously published results ('ground truth'), complemented by a Monte Carlo error analysis, indicates that the rms Warm Spitzer diameter and albedo errors are {+-}20% and {+-}50%, respectively. Cases in which agreement with results from the literature is worse than expected are highlighted and discussed; these include the potential spacecraft target 138911 2001 AE{sub 2}. We confirm that 1.4 appears to be an appropriate overall default value for the relative reflectance between the V band and the Warm Spitzer wavelengths, for use in correction of the Warm Spitzer fluxes for reflected solar radiation.

  5. The HST/ACS+WFC3 Survey for Lyman Limit Systems. II. Science

    NASA Astrophysics Data System (ADS)

    O'Meara, John M.; Prochaska, J. Xavier; Worseck, Gabor; Chen, Hsiao-Wen; Madau, Piero

    2013-03-01

    We present the first science results from our Hubble Space Telescope survey for Lyman limit absorption systems (LLS) using the low dispersion spectroscopic modes of the Advanced Camera for Surveys and the Wide Field Camera 3. Through an analysis of 71 quasars, we determine the incidence frequency of LLS per unit redshift and per unit path length, l(z) and l(X), respectively, over the redshift range 1 < z < 2.6, and find a weighted mean of l(X) =0.29 ± 0.05 for 2.0 < z < 2.5 through a joint analysis of our sample and that of Ribaudo et al. Through stacked spectrum analysis, we determine a median (mean) value of the mean free path to ionizing radiation at z = 2.4 of λ912 mfp = 243(252) h -1 72 Mpc, with an error on the mean value of ±43 h -1 72 Mpc. We also re-evaluate the estimates of λ912 mfp from Prochaska et al. and place constraints on the evolution of λ912 mfp with redshift, including an estimate of the "breakthrough" redshift of z = 1.6. Consistent with results at higher z, we find that a significant fraction of the opacity for absorption of ionizing photons comes from systems with N H I <=1017.5 cm-2 with a value for the total Lyman opacity of τLyman eff = 0.40 ± 0.15. Finally, we determine that at minimum, a 5-parameter (4 power law) model is needed to describe the column density distribution function f(N H I , X) at z ~ 2.4, find that f(N H I , X) undergoes no significant change in shape between z ~ 2.4 and z ~ 3.7, and provide our best fit model for f(N H I , X).

  6. The Swift AGN and Cluster Survey. II. Cluster Confirmation with SDSS Data

    NASA Astrophysics Data System (ADS)

    Griffin, Rhiannon D.; Dai, Xinyu; Kochanek, Christopher S.; Bregman, Joel N.

    2016-01-01

    We study 203 (of 442) Swift AGN and Cluster Survey extended X-ray sources located in the SDSS DR8 footprint to search for galaxy over-densities in three-dimensional space using SDSS galaxy photometric redshifts and positions near the Swift cluster candidates. We find 104 Swift clusters with a >3σ galaxy over-density. The remaining targets are potentially located at higher redshifts and require deeper optical follow-up observations for confirmation as galaxy clusters. We present a series of cluster properties including the redshift, brightest cluster galaxy (BCG) magnitude, BCG-to-X-ray center offset, optical richness, and X-ray luminosity. We also detect red sequences in ˜85% of the 104 confirmed clusters. The X-ray luminosity and optical richness for the SDSS confirmed Swift clusters are correlated and follow previously established relations. The distribution of the separations between the X-ray centroids and the most likely BCG is also consistent with expectation. We compare the observed redshift distribution of the sample with a theoretical model, and find that our sample is complete for z ≲ 0.3 and is still 80% complete up to z ≃ 0.4, consistent with the SDSS survey depth. These analysis results suggest that our Swift cluster selection algorithm has yielded a statistically well-defined cluster sample for further study of cluster evolution and cosmology. We also match our SDSS confirmed Swift clusters to existing cluster catalogs, and find 42, 23, and 1 matches in optical, X-ray, and Sunyaev-Zel’dovich catalogs, respectively, and so the majority of these clusters are new detections.

  7. Spectroscopy of supernova host galaxies from the SDSS-II SN survey with the SDSS and BOSS spectrographs

    NASA Astrophysics Data System (ADS)

    Olmstead, Matthew Dwaune

    Type Ia supernovae (SNeIa) have been used as standard candles to measure cosmological distances. The initial discovery of the accelerated expansion of the universe was performed using ~50 SNe Ia. Large SNe surveys have increased the number of spectroscopically-confirmed SNe Ia to over a thousand with redshift coverage beyond z = 1. We are now in the age of abundant photometry without the ability for full follow-up spectroscopy of all SN candidates. SN cosmology using these large samples will increasingly rely on robust photometric classification of SN candidates. Photometric classification will increase the sample by including faint SNe as these are preferentially not observed with follow-up spectroscopy. The primary concern with using photometrically classified SNe Ia in cosmology is when a core-collapse SNe is incorrectly classified as an SN Ia. This can be mitigated by obtaining the host galaxy redshift of each SN candidate and using this information as a prior in the photometric classification, removing one degree of freedom. To test the impact of redshift on photometric classification, I have performed an assessment on photometric classification of candidates from the Sloan Digital Sky Survey-II (SDSS-II) SN Survey. I have tested the classification with and without redshift priors by looking at the change of photometric classification, the effect of data quality on photometric classification, and the effect of SN light curve properties on photometric classification. Following our suggested classification scheme, there are a total of 1038 photometrically classified SNe Ia when using a flat redshift prior and 1002 SNe~Ia with the spectroscopic redshift. For 912 (91.0%) candidates classified as likely SNe Ia without redshift information, the classification is unchanged when adding the host galaxy redshift. Finally, I investigate the differences in the interpretation of the light curve properties with and without knowledge of the redshift. When using the SALT2

  8. A seroepidemiological survey of HTLV-I/II carriers in the Puna Jujeña.

    PubMed

    Dipierri, J E; Tajima, K; Cartier Robirosa, L; Sonoda, S

    1999-01-01

    Human T-cell leukemia virus type I (HTLV-I) carriers are clustered in limited groups in the world. One of these groups is the Andean native population of South America. As part of an international collaborative study devoted to explore the clustering of HTVL-I carriers in different countries, the aim of this paper was to evaluate the seroprevalence of HTLV-I/II virus in the native population of Puna Argentina in Jujuy. Blood samples of individuals of three populations of Puna Jujeña (Susques, Rinconada, Cochinoca) were screened with particle agglutination (PA), immunofluorescence (IF) and western immunoblotting analysis (WB) tests. Two out 86 (2.32%) individuals examined in the Puna Jujeña showed positive results for HTLV-I antibodies. It is concluded that the Province of Jujuy, in particular its less miscegenated highest altitude areas, constitute the northern and southern Andean natural geographical clustering of HTLV-I. This distribution is probably linked both to a history of prehistoric human dispersal in the Andes and to high mother- to-child transmission of the virus under close conditions of each group.

  9. The COSMOS-[O II] survey: evolution of electron density with star formation rate

    NASA Astrophysics Data System (ADS)

    Kaasinen, Melanie; Bian, Fuyan; Groves, Brent; Kewley, Lisa J.; Gupta, Anshu

    2017-03-01

    Star-forming galaxies at z > 1 exhibit significantly different properties to local galaxies of equivalent stellar mass. Not only are high-redshift star-forming galaxies characterized by higher star formation rates and gas fractions than their local counterparts, they also appear to host star-forming regions with significantly different physical conditions, including greater electron densities. To understand what physical mechanisms are responsible for the observed evolution of the star-forming conditions, we have assembled the largest sample of star-forming galaxies at z ∼ 1.5 with emission-line measurements of the {[O II]}λ λ 3726,3729 doublet. By comparing our z ∼ 1.5 sample to local galaxy samples with equivalent distributions of stellar mass, star formation rate and specific star formation rate we investigate the proposed evolution in electron density and its dependence on global properties. We measure an average electron density of 114_{-27}^{+28} cm^{-3} for our z ∼ 1.5 sample, a factor of 5 greater than the typical electron density of local star-forming galaxies. However, we find no offset between the typical electron densities of local and high-redshift galaxies with equivalent star formation rates. Our work indicates that the average electron density of a sample is highly sensitive to the star formation rates, implying that the previously observed evolution is mainly the result of selection effects.

  10. THE HST/ACS+WFC3 SURVEY FOR LYMAN LIMIT SYSTEMS. II. SCIENCE

    SciTech Connect

    O'Meara, John M.; Prochaska, J. Xavier; Worseck, Gabor; Madau, Piero

    2013-03-10

    We present the first science results from our Hubble Space Telescope survey for Lyman limit absorption systems (LLS) using the low dispersion spectroscopic modes of the Advanced Camera for Surveys and the Wide Field Camera 3. Through an analysis of 71 quasars, we determine the incidence frequency of LLS per unit redshift and per unit path length, l(z) and l(X), respectively, over the redshift range 1 < z < 2.6, and find a weighted mean of l(X) =0.29 {+-} 0.05 for 2.0 < z < 2.5 through a joint analysis of our sample and that of Ribaudo et al. Through stacked spectrum analysis, we determine a median (mean) value of the mean free path to ionizing radiation at z = 2.4 of {lambda}{sup 912}{sub mfp} = 243(252) h {sup -1}{sub 72} Mpc, with an error on the mean value of {+-}43 h {sup -1}{sub 72} Mpc. We also re-evaluate the estimates of {lambda}{sup 912}{sub mfp} from Prochaska et al. and place constraints on the evolution of {lambda}{sup 912}{sub mfp} with redshift, including an estimate of the ''breakthrough'' redshift of z = 1.6. Consistent with results at higher z, we find that a significant fraction of the opacity for absorption of ionizing photons comes from systems with N{sub H{sub I}} {<=}10{sup 17.5} cm{sup -2} with a value for the total Lyman opacity of {tau}{sup Lyman}{sub eff} = 0.40 {+-} 0.15. Finally, we determine that at minimum, a 5-parameter (4 power law) model is needed to describe the column density distribution function f(N{sub H{sub I}}, X) at z {approx} 2.4, find that f(N{sub H{sub I}}, X) undergoes no significant change in shape between z {approx} 2.4 and z {approx} 3.7, and provide our best fit model for f(N{sub H{sub I}}, X).

  11. The HST/ACS Coma Cluster Survey. II. Data Description and Source Catalogs

    NASA Technical Reports Server (NTRS)

    Hammer, Derek; Kleijn, Gijs Verdoes; Hoyos, Carlos; Den Brok, Mark; Balcells, Marc; Ferguson, Henry C.; Goudfrooij, Paul; Carter, David; Guzman, Rafael; Peletier, Reynier F.; Smith, Russell J.; Graham, Alister W.; Trentham, Neil; Peng, Eric; Puzia, Thomas H.; Lucey, John R.; Jogee, Shardha; Aguerri, Alfonso L.; Batcheldor, Dan; Bridges, Terry J.; Davies, Jonathan I.; Del Burgo, Carlos; Erwin, Peter; Hornschemeier, Ann; Hudson, Michael J.

    2010-01-01

    The Coma cluster, Abell 1656, was the target of a HST-ACS Treasury program designed for deep imaging in the F475W and F814W passbands. Although our survey was interrupted by the ACS instrument failure in early 2007, the partially-completed survey still covers approximately 50% of the core high density region in Coma. Observations were performed for twenty-five fields with a total coverage area of 274 aremin(sup 2), and extend over a wide range of cluster-centric radii (approximately 1.75 Mpe or 1 deg). The majority of the fields are located near the core region of Coma (19/25 pointings) with six additional fields in the south-west region of the cluster. In this paper we present SEXTRACTOR source catalogs generated from the processed images, including a detailed description of the methodology used for object detection and photometry, the subtraction of bright galaxies to measure faint underlying objects, and the use of simulations to assess the photometric accuracy and completeness of our catalogs. We also use simulations to perform aperture corrections for the SEXTRACTOR Kron magnitudes based only on the measured source flux and its half-light radius. We have performed photometry for 76,000 objects that consist of roughly equal numbers of extended galaxies and unresolved objects. Approximately two-thirds of all detections are brighter than F814W=26.5 mag (AB), which corresponds to the 10sigma, point-source detection limit. We estimate that Coma members are 5-10% of the source detections, including a large population of compact objects (primarily GCs, but also cEs and UCDs), and a wide variety of extended galaxies from cD galaxies to dwarf low surface brightness galaxies. The initial data release for the HST-ACS Coma Treasury program was made available to the public in August 2008. The images and catalogs described in this study relate to our second data release.

  12. THE SLOAN DIGITAL SKY SURVEY DATA RELEASE 7 SPECTROSCOPIC M DWARF CATALOG. II. STATISTICAL PARALLAX ANALYSIS

    SciTech Connect

    Bochanski, John J.; Hawley, Suzanne L.; West, Andrew A.

    2011-03-15

    We present a statistical parallax analysis of low-mass dwarfs from the Sloan Digital Sky Survey. We calculate absolute r-band magnitudes (M{sub r} ) as a function of color and spectral type and investigate changes in M{sub r} with location in the Milky Way. We find that magnetically active M dwarfs are intrinsically brighter in M{sub r} than their inactive counterparts at the same color or spectral type. Metallicity, as traced by the proxy {zeta}, also affects M{sub r} , with metal-poor stars having fainter absolute magnitudes than higher metallicity M dwarfs at the same color or spectral type. Additionally, we measure the velocity ellipsoid and solar reflex motion for each subsample of M dwarfs. We find good agreement between our measured solar peculiar motion and previous results for similar populations, as well as some evidence for differing motions of early and late M-type populations in U and W velocities that cannot be attributed to asymmetric drift. The reflex solar motion and the velocity dispersions both show that younger populations, as traced by magnetic activity and location near the Galactic plane, have experienced less dynamical heating. We introduce a new parameter, the independent position altitude (IPA), to investigate populations as a function of vertical height from the Galactic plane. M dwarfs at all types exhibit an increase in velocity dispersion when analyzed in comparable IPA subgroups.

  13. Red giant stars from the Sloan digital sky survey. II. Distances

    SciTech Connect

    Tan, Kefeng; Chen, Yuqin; Carrell, Kenneth; Zhao, Jingkun; Zhao, Gang

    2014-10-10

    We present distance determinations for a large and clean sample of red giant branch stars selected from the ninth data release of the Sloan Digital Sky Survey. The distances are calculated based on both observational cluster fiducials and theoretical isochrones. Distributions of distances from the two methods are very similar with peaks at about 10 kpc and tails extending to more than 70 kpc. We find that distances from the two methods agree well for the majority of the sample stars; though, on average, distances based on isochrones are 10% higher than those based on fiducials. We test the accuracy of our distance determinations using 332 stars from 10 Galactic globular and open clusters. The average relative deviation from the literature cluster distances is 4% for the fiducial-based distances and 8% for the isochrone-based distances, both of which are within the uncertainties. We find that the effective temperature and surface gravity derived from low-resolution spectra are not accurate enough to essentially improve the performance of distance determinations. However, for stars with significant extinction, effective temperature may help to better constrain their distances to some extent. We make our sample stars and their distances available from an online catalog. The catalog comprises 17,941 stars with reasonable distance estimations reaching to more than 70 kpc, which is suitable for the investigation of the formation and evolution of the Galaxy, especially the Galactic halo.

  14. Far-infrared data for symbiotic stars. II - The IRAS survey observations

    NASA Technical Reports Server (NTRS)

    Kenyon, S. J.; Fernandez-Castro, T.; Stencel, R. E.

    1988-01-01

    IRAS survey data for all known symbiotic binaries are reported. S type systems have 25 micron excesses much larger than those of single red giant stars, suggesting that these objects lose mass more rapidly than do normal giants. D type objects have far-IR colors similar to those of Mira variables, implying mass-loss rate of about 10 to the -6th solar masses/yr. The near-IR extinctions of the D types indicate that their Mira components are enshrouded in optically thick dust shells, while their hot companions lie outside the shells. If this interpretation of the data is correct, then the very red near-IR colors of D type symbiotic stars are caused by extreme amounts of dust absorption rather than dust emission. The small group of D prime objects possesses far-IR colors resembling those of compact planetary nebulae or extreme OH/IR stars. It is speculated that these binaries are not symbiotic stars at all, but contain a hot compact star and an exasymptotic branch giant which is in the process of ejecting a planetary nebula shell.

  15. Far-infrared data for symbiotic stars. II - The IRAS survey observations

    NASA Astrophysics Data System (ADS)

    Kenyon, S. J.; Fernandez-Castro, T.; Stencel, R. E.

    1988-06-01

    IRAS survey data for all known symbiotic binaries are reported. S type systems have 25 micron excesses much larger than those of single red giant stars, suggesting that these objects lose mass more rapidly than do normal giants. D type objects have far-IR colors similar to those of Mira variables, implying mass-loss rate of about 10 to the -6th solar masses/yr. The near-IR extinctions of the D types indicate that their Mira components are enshrouded in optically thick dust shells, while their hot companions lie outside the shells. If this interpretation of the data is correct, then the very red near-IR colors of D type symbiotic stars are caused by extreme amounts of dust absorption rather than dust emission. The small group of D prime objects possesses far-IR colors resembling those of compact planetary nebulae or extreme OH/IR stars. It is speculated that these binaries are not symbiotic stars at all, but contain a hot compact star and an exasymptotic branch giant which is in the process of ejecting a planetary nebula shell.

  16. DEEP NEAR-INFRARED SURVEY OF THE PIPE NEBULA. II. DATA, METHODS, AND DUST EXTINCTION MAPS

    SciTech Connect

    Roman-Zuniga, Carlos G.; Lada, Charles J.; Lombardi, Marco

    2010-12-20

    We present a new set of high-resolution dust extinction maps of the nearby and essentially starless Pipe Nebula molecular cloud. The maps were constructed from a concerted deep near-infrared imaging survey with the ESO-VLT, ESO-NTT, CAHA 3.5 m telescopes, and 2MASS data. The new maps have a resolution three times higher than the previous extinction map of this cloud by Lombardi et al. and are able to resolve structures down to 2600 AU. We detect 244 significant extinction peaks across the cloud. These peaks have masses between 0.1 and 18.4 M{sub sun}, diameters between 1.2 and 5.7 x 10{sup 4} AU (0.06 and 0.28 pc), and mean densities of about 10{sup 4} cm{sup -3}, all in good agreement with previous results. From the analysis of the mean surface density of companions we find a well-defined scale near 1.4 x 10{sup 4} AU below which we detect a significant decrease in structure of the cloud. This scale is smaller than the Jeans length calculated from the mean density of the peaks. The surface density of peaks is not uniform but instead it displays clustering. Extinction peaks in the Pipe Nebula appear to have a spatial distribution similar to the stars in Taurus, suggesting that the spatial distribution of stars evolves directly from the primordial spatial distribution of high-density material.

  17. THE SLOAN DIGITAL SKY SURVEY QUASAR LENS SEARCH. II. STATISTICAL LENS SAMPLE FROM THETHIRD DATA RELEASE

    SciTech Connect

    Inada, N; Oguri, M; Becker, R H; Shin, M; Richards, G T; Hennawi, J F; White, R L; Pindor, B; Strauss, M A; Kochanek, C S; Johnston, D E; Gregg, M D; Kayo, I; Eisenstein, D; Hall, P B; Castander, F J; Clocchiatti, A; Chiu, K; Kawano, Y; Scranton, R; Frieman, J; Keeton, C R; Morokuma, T; Rix, H; Turner, E L; Burless, S; Brunner, R J; Sheldon, E S; Bahcall, N A; Fukugita, M

    2007-09-13

    We report the first results of our systematic search for strongly lensed quasars using the spectroscopically confirmed quasars in the Sloan Digital Sky Survey (SDSS). Among 46,420 quasars from the SDSS Data Release 3 ({approx}4188 deg{sup 2}), we select a subsample of 22,683 quasars that are located at redshifts between 0.6 and 2.2 and are brighter than the Galactic extinction corrected i-band magnitude of 19.1. We identify 220 lens candidates from the quasar subsample, for which we conduct extensive and systematic follow-up observations in optical and near-infrared wavebands, in order to construct a complete lensed quasar sample at image separations between 1-inch and 20-inch and flux ratios of faint to bright lensed images larger than 10{sup -0.5}. We construct a statistical sample of 11 lensed quasars. Ten of these are galaxy-scale lenses with small image separations ({approx} 1-inch - 2-inch) and one is a large separation (15-inch) system which is produced by a massive cluster of galaxies, representing the first statistical sample of lensed quasars including both galaxy- and cluster-scale lenses. The Data Release 3 spectroscopic quasars contain an additional 11 lensed quasars outside the statistical sample.

  18. Ototoxic occupational exposures for a stock car racing team: II. chemical surveys.

    PubMed

    Gwin, Kristin K; Wallingford, Kenneth M; Morata, Thais C; Van Campen, Luann E; Dallaire, Jacques; Alvarez, Frank J

    2005-08-01

    The National Institute for Occupational Safety and Health (NIOSH) conducted a series of surveys to evaluate occupational exposure to noise and potentially ototoxic chemical agents among members of a professional stock car racing team. Exposure assessments included site visits to the team's race shop and a worst-case scenario racetrack. During site visits to the race team's shop, area samples were collected to measure exposures to potentially ototoxic chemicals, including, organic compounds (typical of solvents), metals, and carbon monoxide (CO). Exposures to these chemicals were all below their corresponding Occupational Safety and Health Administration (OSHA) permissible exposure limits (PELs), NIOSH recommended exposure limits (RELs), and American Conference of Governmental Industrial Hygienists (ACGIH) threshold limit values (TLVs). During site visits to the racetrack, area and personal samples were collected for organic compounds, lead, and CO in and around the "pit" area where the cars undergo race preparation and service during the race. Exposures to organic compounds and lead were either nondetectable or too low to quantify. Twenty-five percent of the CO time-weighted average concentrations exceeded the OSHA PEL, NIOSH REL, and ACGIH TLV after being adjusted for a 10-hour workday. Peak CO measurements exceeded the NIOSH recommended ceiling limit of 200 ppm. Based on these data, exposures to potentially ototoxic chemicals are probably not high enough to produce an adverse effect greater than that produced by the high sound pressure levels alone. However, carbon monoxide levels occasionally exceeded all evaluation criteria at the racetrack.

  19. The Sloan Digital Sky Survey Data Release 7 Spectroscopic M Dwarf Catalog. II. Statistical Parallax Analysis

    NASA Astrophysics Data System (ADS)

    Bochanski, John J.; Hawley, Suzanne L.; West, Andrew A.

    2011-03-01

    We present a statistical parallax analysis of low-mass dwarfs from the Sloan Digital Sky Survey. We calculate absolute r-band magnitudes (Mr ) as a function of color and spectral type and investigate changes in Mr with location in the Milky Way. We find that magnetically active M dwarfs are intrinsically brighter in Mr than their inactive counterparts at the same color or spectral type. Metallicity, as traced by the proxy ζ, also affects Mr , with metal-poor stars having fainter absolute magnitudes than higher metallicity M dwarfs at the same color or spectral type. Additionally, we measure the velocity ellipsoid and solar reflex motion for each subsample of M dwarfs. We find good agreement between our measured solar peculiar motion and previous results for similar populations, as well as some evidence for differing motions of early and late M-type populations in U and W velocities that cannot be attributed to asymmetric drift. The reflex solar motion and the velocity dispersions both show that younger populations, as traced by magnetic activity and location near the Galactic plane, have experienced less dynamical heating. We introduce a new parameter, the independent position altitude (IPA), to investigate populations as a function of vertical height from the Galactic plane. M dwarfs at all types exhibit an increase in velocity dispersion when analyzed in comparable IPA subgroups.

  20. The Gaia spectrophotometric standard stars survey: II. Instrumental effects of six ground-based observing campaigns

    NASA Astrophysics Data System (ADS)

    Altavilla, G.; Marinoni, S.; Pancino, E.; Galleti, S.; Ragaini, S.; Bellazzini, M.; Cocozza, G.; Bragaglia, A.; Carrasco, J. M.; Castro, A.; Di Fabrizio, L.; Federici, L.; Figueras, F.; Gebran, M.; Jordi, C.; Masana, E.; Schuster, W.; Valentini, G.; Voss, H.

    2015-08-01

    The Gaia SpectroPhotometric Standard Stars (SPSS) survey started in 2006, was awarded almost 450 observing nights and accumulated almost 100 000 raw data frames with both photometric and spectroscopic observations. Such large observational effort requires careful, homogeneous, and automatic data reduction and quality control procedures. In this paper, we quantitatively evaluate instrumental effects that might have a significant (i.e., ≥ 1 %) impact on the Gaia SPSS flux calibration. The measurements involve six different instruments, monitored over the eight years of observations dedicated to the Gaia flux standards campaigns: DOLORES@TNG in La Palma, EFOSC2@NTT and ROSS@REM in La Silla, CAFOS@2.2 m in Calar Alto, BFOSC@Cassini in Loiano, and LaRuca@1.5 m in San Pedro Mártir. We examine and quantitatively evaluate the following effects: CCD linearity and shutter times, calibration frames stability, lamp flexures, second order contamination, light polarization, and fringing. We present methods to correct for the relevant effects which can be applied to a wide range of observational projects at similar instruments. Based on data obtained with BFOSC@Cassini in Loiano, Italy; EFOSC2@NTT in La Silla, Chile; DOLORES@TNG in La Palma, Spain; CAFOS@2.2 m in Calar Alto, Spain; LaRuca@1.5 m in San Pedro Mártir, Mexico (see acknowledgements for more details).

  1. Urinary cadmium and blood pressure: Results from the NHANES II survey

    SciTech Connect

    Whittemore, A.S.; DiCiccio, Y. ); Provenzano, G. )

    1991-02-01

    Relationships between urinary cadmium levels and blood pressure were examined in a sample of 951 adult men and women who participated in the Second National Health and Nutritional Examination Survey (NHANES 2). Among all participants, positive relationships were seen between urinary cadmium levels and both systolic and diastolic blood pressure after adjusting for age, sex, race, relative body weight, smoking status, and hypertensive medication use. However, analyses for subgroups determined by sex and smoking status were inconsistent. Among current smokers, urinary cadmium levels were significantly positively associated with both systolic and diastolic blood pressure for women, and with diastolic blood pressure for men. Yet among former smokers and lifelong nonsmokers of both sexes, urinary cadmium was not significantly associated with either systolic or diastolic blood pressure. Evidence that some hypertensive medications increase urinary cadmium excretion suggests that the positive associations seen among current smokers may reflect high urinary cadium levels among hypertensives induced by hypertensive treatment. After treated hypertensives were removed from the analysis, regression coefficients relating blood pressure to cadmium dropped by a factor of two and lost statistical significance. The authors conclude that the present data provide little support for a causal association between systemic cadmium and hypertension at nonoccupational exposure levels. Further, conflicting results of previous studies may reflect failure to control adequately for age, smoking status, and hypertensive treatment.

  2. Fuel Quality/Processing Study. Volume II. Appendix, Task I, literature survey

    SciTech Connect

    O'Hara, J B; Bela, A; Jentz, N E; Klumpe, H W; Kessler, R E; Kotzot, H T; Loran, B I

    1981-04-01

    This activity was begun with the assembly of information from Parsons' files and from contacts in the development and commercial fields. A further more extensive literature search was carried out using the Energy Data Base and the American Petroleum Institute Data Base. These are part of the DOE/RECON system. Approximately 6000 references and abstracts were obtained from the EDB search. These were reviewed and the especially pertinent documents, approximately 300, were acquired in the form of paper copy or microfiche. A Fuel Properties form was developed for listing information pertinent to gas turbine liquid fuel properties specifications. Fuel properties data for liquid fuels from selected synfuel processes, deemed to be successful candidates for near future commercial plants were tabulated on the forms. The processes selected consisted of H-Coal, SRC-II and Exxon Donor Solvent (EDS) coal liquefaction processes plus Paraho and Tosco shale oil processes. Fuel properties analyses for crude and distillate syncrude process products are contained in Section 2. Analyses representing synthetic fuels given refinery treatments, mostly bench scale hydrotreating, are contained in Section 3. Section 4 discusses gas turbine fuel specifications based on petroleum source fuels as developed by the major gas turbine manufacturers. Section 5 presents the on-site gas turbine fuel treatments applicable to petroleum base fuels impurities content in order to prevent adverse contaminant effects. Section 7 relates the environmental aspects of gas turbine fuel usage and combustion performance. It appears that the near future stationary industrial gas turbine fuel market will require that some of the synthetic fuels be refined to the point that they resemble petroleum based fuels.

  3. VizieR Online Data Catalog: Robo-AO Kepler planetary candidate survey. II. (Baranec+, 2016)

    NASA Astrophysics Data System (ADS)

    Baranec, C.; Ziegler, C.; Law, N. M.; Morton, T.; Riddle, R.; Atkinson, D.; Schonhut, J.; Crepp, J.

    2016-10-01

    We selected targets that we had not previously observed from the KOI Catalog based on the Q1-Q12 Kepler data (Rowe et al. 2015, Cat. J/ApJS/217/16). These targets were added to the Robo-AO intelligent observing queue and observed during the summer of 2013. We obtained high angular resolution images of 956 Kepler planet candidate host stars with the Robo-AO robotic laser AOs system over the course of 19 nights between 2013 July 21 and 2013 October 25, detailed in Table5. We also include 13 images from 2012 (2012 July 16-September 13) that required additional confirmation of the KOI position in the Robo-AO field of view. All the observations were performed in a queue-scheduled mode in combination with other science programs using the Robo-AO autonomous laser AO system mounted on the robotic 1.5m telescope at Palomar Observatory (exposure time: 90s; observation wavelengths: 600-950nm; FWHM resolution: 0.12''-0.15''; field of view: 44''*44''; pixel scale: 43.1mas/pix; detector format: 10242 pixels; targets observed/hour: 20). We obtained images of 50 KOIs with the NIRC2 instrument behind the Keck II AO system that were previously observed with Robo-AO and had evidence of a companion. Observations were conducted on 2013 June 25, 2013 August 24 and 25, 2014 August 17, and 2015 July 25 in the K, Ks, or Kp filters, and in the narrow mode of NIRC2 (9.952mas/pixel). (4 data files).

  4. An updated survey of globular clusters in M 31. II. Newly discovered bright and remote clusters

    NASA Astrophysics Data System (ADS)

    Galleti, S.; Bellazzini, M.; Federici, L.; Buzzoni, A.; Fusi Pecci, F.

    2007-08-01

    Aims:We present the first results of a large spectroscopic survey of candidate globular clusters located in the extreme outskirts of the nearby M 31 galaxy. The survey is aimed at ascertaining the nature of the selected candidates to increase the sample of confirmed M 31 clusters lying more that 2° away from the center of the galaxy. Methods: We obtained low resolution spectra (λ/Δλ ≃ 800-1300) of 48 targets selected from the Extended Source Catalogue of 2MASS, as in Galleti et al. (2005, A&A, 436, 535). The observed candidates have been robustly classified according to their radial velocity and by verifying their extended/point-source nature from ground-based optical images. We have also obtained a spectrum and a radial velocity estimate for the remote M 31 globular discovered by Martin et al. (2006b, MNRAS, 371, 1983). Results: Among the 48 observed candidates clusters we found: 35 background galaxies, 8 foreground Galactic stars, and 5 genuine remote globular clusters. One of them has been already identified independently by Mackey et al. (2007, ApJ, 655, L85), their GC1; the other four are completely new discoveries: B516, B517, B518, B519. The newly discovered clusters lie at projected distance 40 kpc ≲ R_p≲ 100 kpc from the center of M 31, and have absolute integrated magnitude -9.5 ≲ MV ≲ -7.5. For all the observed clusters we have measured the strongest Lick indices and we have obtained spectroscopic metallicity estimates. Mackey-GC1, Martin-GC1, B517 and B518 have spectra typical of old and metal poor globular clusters ([Fe/H] ≲ -1.3); B519 appears old but quite metal-rich ([Fe/H]~≃ -0.5); B516 presents very strong Balmer absorption lines: if this is indeed a cluster it should have a relatively young age (likely < 2 Gyr). Conclusions: The present analysis nearly doubles the number of M 31 globulars at R_p≥ 40 kpc. At odds with the Milky Way, M 31 appears to have a significant population of very bright globular clusters in its extreme

  5. WEATHER ON OTHER WORLDS. II. SURVEY RESULTS: SPOTS ARE UBIQUITOUS ON L AND T DWARFS

    SciTech Connect

    Metchev, Stanimir A.; Heinze, Aren; Apai, Dániel; Flateau, Davin; Radigan, Jacqueline; Burgasser, Adam; Marley, Mark S.; Artigau, Étienne; Plavchan, Peter; Goldman, Bertrand

    2015-02-01

    We present results from the Weather on Other Worlds Spitzer Exploration Science program to investigate photometric variability in L and T dwarfs, usually attributed to patchy clouds. We surveyed 44 L3-T8 dwarfs, spanning a range of J – K{sub s} colors and surface gravities. We find that 14/23 (61%{sub −20%}{sup +17%}, 95% confidence) of our single L3-L9.5 dwarfs are variable with peak-to-peak amplitudes between 0.2% and 1.5%, and 5/16 (31%{sub −17%}{sup +25%}) of our single T0-T8 dwarfs are variable with amplitudes between 0.8% and 4.6%. After correcting for sensitivity, we find that 80%{sub −27%}{sup +20%} of L dwarfs vary by ≥0.2%, and 36%{sub −17%}{sup +26%} of T dwarfs vary by ≥0.4%. Given viewing geometry considerations, we conclude that photospheric heterogeneities causing >0.2% 3-5 μm flux variations are present on virtually all L dwarfs, and probably on most T dwarfs. A third of L dwarf variables show irregular light curves, indicating that L dwarfs may have multiple spots that evolve over a single rotation. Also, approximately a third of the periodicities are on timescales >10 hr, suggesting that slowly rotating brown dwarfs may be common. We observe an increase in the maximum amplitudes over the entire spectral type range, revealing a potential for greater temperature contrasts in T dwarfs than in L dwarfs. We find a tentative association (92% confidence) between low surface gravity and high-amplitude variability among L3-L5.5 dwarfs. Although we can not confirm whether lower gravity is also correlated with a higher incidence of variables, the result is promising for the characterization of directly imaged young extrasolar planets through variability.

  6. Galaxy pairs in the Sloan Digital Sky Survey - II. The effect of environment on interactions

    NASA Astrophysics Data System (ADS)

    Ellison, Sara L.; Patton, David R.; Simard, Luc; McConnachie, Alan W.; Baldry, Ivan K.; Mendel, J. Trevor

    2010-09-01

    We use a sample of close galaxy pairs selected from the Sloan Digital Sky Survey Data Release 4 (SDSS DR4) to investigate in what environments galaxy mergers occur and how the results of these mergers depend on differences in local galaxy density. The galaxies are quantified morphologically using two-dimensional bulge-plus-disc decompositions and compared to a control sample matched in stellar mass, redshift and local projected density. Lower density environments have fractionally more galaxy pairs with small projected separations (rp) and relative velocities (Δv), but even high-density environments contain significant populations of pairs with parameters that should be conducive to interactions. The connection between environment and Δv also implies that the velocity selection of a pairs sample affects (biases) the environment from which the pairs are selected. Metrics of asymmetry and colour are used to identify merger activity and triggered star formation. The location of star formation is inferred by distinguishing bulge and disc colours and calculating bulge fractions from the SDSS images. Galaxies in the lowest density environments show the largest changes in star formation rate, asymmetry and bulge-to-total fractions at small separations, accompanied by bluer bulge colours. At the highest local densities, the only galaxy property to show an enhancement in the closest pairs is asymmetry. We interpret these results as evidence that whilst interactions (leading to tidal distortions) occur at all densities, triggered star formation is seen only in low-to-intermediate density environments. We suggest that this is likely due to the typically higher gas fractions of galaxies in low-density environments. Finally, by cross-correlating our sample of galaxy pairs with a cluster catalogue, we investigate the dependence of interactions on clustercentric distance. It is found that for close pairs the fraction of asymmetric galaxies is highest in the cluster centres.

  7. Chromospherically Active Stars in the RAVE Survey. II. Young Dwarfs in the Solar Neighborhood

    NASA Astrophysics Data System (ADS)

    Žerjal, M.; Zwitter, T.; Matijevič, G.; Grebel, E. K.; Kordopatis, G.; Munari, U.; Seabroke, G.; Steinmetz, M.; Wojno, J.; Bienaymé, O.; Bland-Hawthorn, J.; Conrad, C.; Freeman, K. C.; Gibson, B. K.; Gilmore, G.; Kunder, A.; Navarro, J.; Parker, Q. A.; Reid, W.; Siviero, A.; Watson, F. G.; Wyse, R. F. G.

    2017-01-01

    A large sample of over 38,000 chromospherically active candidate solar-like stars and cooler dwarfs from the RAVE survey is addressed in this paper. An improved activity identification with respect to the previous study was introduced to build a catalog of field stars in the solar neighborhood with an excess emission flux in the calcium infrared triplet wavelength region. The central result of this work is the calibration of the age–activity relation for main-sequence dwarfs in a range from a few 10 {Myr} up to a few Gyr. It enabled an order of magnitude age estimation of the entire active sample. Almost 15,000 stars are shown to be younger than 1 {Gyr} and ∼2000 younger than 100 {Myr}. The young age of the most active stars is confirmed by their position off the main sequence in the J ‑ K versus {N}{UV}-V diagram showing strong ultraviolet excess, mid-infrared excess in the J ‑ K versus {W}1-{W}2 diagram, and very cool temperatures (J-K> 0.7). They overlap with the reference pre-main-sequence RAVE stars often displaying X-ray emission. The activity level increasing with the color reveals their different nature from the solar-like stars and probably represents an underlying dynamo-generating magnetic fields in cool stars. Of the RAVE objects from DR5, 50% are found in the TGAS catalog and supplemented with accurate parallaxes and proper motions by Gaia. This makes the database of a large number of young stars in a combination with RAVE’s radial velocities directly useful as a tracer of the very recent large-scale star formation history in the solar neighborhood. The data are available online in the Vizier database.

  8. Occupational exposures and uncontrolled adult-onset asthma in the European Community Respiratory Health Survey II.

    PubMed

    Le Moual, Nicole; Carsin, Anne-Elie; Siroux, Valérie; Radon, Katja; Norback, Dan; Torén, Kjell; Olivieri, Mario; Urrutia, Isabel; Cazzoletti, Lucia; Jacquemin, Bénédicte; Benke, Geza; Kromhout, Hans; Mirabelli, Maria C; Mehta, Amar J; Schlünssen, Vivi; Sigsgaard, Torben; Blanc, Paul D; Kogevinas, Manolis; Antó, Josep M; Zock, Jan-Paul

    2014-02-01

    Occupational exposure is a well-recognised modifiable risk factor for asthma, but the relationship between occupational exposure and asthma control has not been studied. We aimed to study this association among working-age adults from the European Community Respiratory Health Survey (ECRHS). Data were available for 7077 participants (mean age 43 years, 45% never-smokers, 5867 without asthma and 1210 with current asthma). Associations between occupational exposure to specific asthmagens and asthma control status (33% with uncontrolled asthma, based on the Global Initiative for Asthma guidelines) were evaluated using logistic and multinomial regressions, adjusted for age, sex and smoking status, with study areas included as a random effect. Statistically significant positive associations were observed between uncontrolled adult-onset asthma and both past 12-month and 10-year exposure to any occupational asthmagens (OR (95% CI) 1.6 (1.0-2.40) and 1.7 (1.2-2.5), respectively); high (1.7 (1.0-2.8) and 1.9 (1.3-2.9), respectively) and low (1.6 (1.0-2.7) and 1.8 (1.2-2.7), respectively) molecular weight agents; and cleaning agents (2.0 (1.1-3.6) and 2.3 (1.4-3.6), respectively), with stronger associations for long-term exposures. These associations were mainly explained by the exacerbation domain of asthma control and no associations were observed between asthmagens and partly controlled asthma. These findings suggest that occupational exposure to asthmagens is associated with uncontrolled adult-onset asthma. Occupational risk factors should be quickly identified to prevent uncontrolled asthma.

  9. Bright Metal-Poor Stars from the Hamburg/ESO Survey. II. A Chemodynamical Analysis

    NASA Astrophysics Data System (ADS)

    Beers, Timothy C.; Placco, Vinicius M.; Carollo, Daniela; Rossi, Silvia; Lee, Young Sun; Frebel, Anna; Norris, John E.; Dietz, Sarah; Masseron, Thomas

    2017-01-01

    We obtain estimates of stellar atmospheric parameters for a previously published sample of 1777 relatively bright (9< B< 14) metal-poor candidates from the Hamburg/ESO Survey. The original Frebel et al. analysis of these stars was able to derive estimates of [Fe/H] and [C/Fe] only for a subset of the sample, due to limitations in the methodology then available. A new spectroscopic analysis pipeline has been used to obtain estimates of {T}{eff}, {log} g, [Fe/H], and [C/Fe] for almost the entire data set. This sample is very local—about 90% of the stars are located within 0.5 kpc of the Sun. We consider the chemodynamical properties of these stars in concert with a similarly local sample of stars from a recent analysis of the Bidelman and MacConnell “weak metal” candidates by Beers et al. We use this combined sample to identify possible members of the halo stream of stars suggested by Helmi et al. and Chiba & Beers, as well as stars that may be associated with stripped debris from the putative parent dwarf of the globular cluster Omega Centauri, suggested to exist by previous authors. We identify a clear increase in the cumulative frequency of carbon-enhanced metal-poor (CEMP) stars with declining metallicity, as well as an increase in the fraction of CEMP stars with distance from the Galactic plane, consistent with previous results. We also identify a relatively large number of CEMP stars with kinematics consistent with the metal-weak thick-disk population, with possible implications for its origin.

  10. The SAMI Galaxy Survey: the discovery of a luminous, low-metallicity H II complex in the dwarf galaxy GAMA J141103.98-003242.3

    NASA Astrophysics Data System (ADS)

    Richards, S. N.; Schaefer, A. L.; López-Sánchez, Á. R.; Croom, S. M.; Bryant, J. J.; Sweet, S. M.; Konstantopoulos, I. S.; Allen, J. T.; Bland-Hawthorn, J.; Bloom, J. V.; Brough, S.; Fogarty, L. M. R.; Goodwin, M.; Green, A. W.; Ho, I.-T.; Kewley, L. J.; Koribalski, B. S.; Lawrence, J. S.; Owers, M. S.; Sadler, E. M.; Sharp, R.

    2014-12-01

    We present the discovery of a luminous unresolved H II complex on the edge of dwarf galaxy GAMA J141103.98-003242.3 using data from the Sydney-AAO Multi-object Integral field spectrograph (SAMI) Galaxy Survey. This dwarf galaxy is situated at a distance of ˜100 Mpc and contains an unresolved region of H II emission that contributes ˜70 per cent of the galaxy's Hα luminosity, located at the top end of established H II region luminosity functions. For the H II complex, we measure a star formation rate of 0.147 ± 0.041 M⊙ yr-1and a metallicity of 12+log(O/H) = 8.01 ± 0.05 that is lower than the rest of the galaxy by ˜0.2 dex. Data from the H I Parkes All-Sky Survey (HIPASS) indicate the likely presence of neutral hydrogen in the galaxy to potentially fuel ongoing and future star-forming events. We discuss various triggering mechanisms for the intense star formation activity of this H II complex, where the kinematics of the ionized gas are well described by a rotating disc and do not show any features indicative of interactions. We show that SAMI is an ideal instrument to identify similar systems to GAMA J141103.98-003242.3, and the SAMI Galaxy Survey is likely to find many more of these systems to aid in the understanding of their formation and evolution.

  11. Phase II of the Small Main-Belt Asteroid Spectroscopic Survey. A Feature-Based Taxonomy

    NASA Astrophysics Data System (ADS)

    Bus, Schelte J.; Binzel, Richard P.

    2002-07-01

    The second phase of the Small Main-belt Asteroid Spectroscopic Survey (SMASSII) produced an internally consistent set of visible-wavelength charge-coupled device (CCD) spectra for 1447 asteroids (Bus and Binzel 2002, Icarus, ). These data provide a basis for developing a new asteroid taxonomy that utilizes more of the information contained in CCD spectra. Here we construct a classification system that builds on the robust framework provided by existing asteroid taxonomies. In particular, we define three major groupings (the S-, C-, and X-complexes) that adhere to the classical definitions of the S-, C-, and X-type asteroids. A total of 26 classes are defined, based on the presence or absence of specific spectral features. Definitions and boundary parameters are provided for each class, allowing new spectral observations to be placed in this system. Of these 26 classes, 12 bear familiar single-letter designations that follow previous conventions: A, B, C, D, K, O, Q, R, S, T, V, and X. A new L-class is introduced to describe 35 objects with spectra having a steep UV slope shortward of 0.75 μm, but which are relatively flat longward of 0.75 μm. Asteroids with intermediate spectral characteristics are assigned multiletter designations: Cb, Cg, Cgh, Ch, Ld, Sa, Sk, Sl, Sq, Sr, Xc, Xe, and Xk. Members of the Cgh- and Ch-classes have spectra containing a 0.7-μm feature that is generally attributed to hydration. Although previously considered featureless, CCD observations reveal distinct features of varying strengths in the spectra of asteroids in the X-complex, thus allowing the Xc-, Xe-, and Xk-classes to be established. Most notably, the spectra of Xe-type asteroids contain an absorption feature centered near 0.49 μm that may be associated with troilite. Several new members are identified for previously unique or sparsely populated classes: 12 A-types, 3 O-types, and 3 R-types. Q-types are common within the near-Earth asteroid population but remain unobserved in

  12. SDSS-II Supernova survey. An analysis of the largest sample of type IA supernovae and correlations with host-galaxy spectral properties

    SciTech Connect

    Wolf, Rachel C.; D’Andrea, Chris B.; Gupta, Ravi R.; Sako, Masao; Fischer, John A.; Kessler, Rick; Jha, Saurabh W.; March, Marisa C.; Scolnic, Daniel M.; Fischer, Johanna-Laina; Campbell, Heather; Nichol, Robert C.; Olmstead, Matthew D.; Richmond, Michael; Schneider, Donald P.; Smith, Mathew

    2016-04-20

    Using the largest single-survey sample of Type Ia supernovae (SNe Ia) to date, we study the relationship between properties of SNe Ia and those of their host galaxies, focusing primarily on correlations with Hubble residuals (HR). Our sample consists of 345 photometrically-classified or spectroscopicallyconfirmed SNe Ia discovered as part of the SDSS-II Supernova Survey (SDSS-SNS). This analysis utilizes host-galaxy spectroscopy obtained during the SDSS-I/II spectroscopic survey and from an ancillary program on the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS) that obtained spectra for nearly all host galaxies of SDSS-II SN candidates. In addition, we use photometric hostgalaxy properties from the SDSS-SNS data release (Sako et al. 2014) such as host stellar mass and star-formation rate. We confirm the well-known relation between HR and host-galaxy mass and find a 3.6σ significance of a non-zero linear slope. We also recover correlations between HR and hostgalaxy gas-phase metallicity and specific star-formation rate as they are reported in the literature. With our large dataset, we examine correlations between HR and multiple host-galaxy properties simultaneously and find no evidence of a significant correlation. We also independently analyze our spectroscopically-confirmed and photometrically-classified SNe Ia and comment on the significance of similar combined datasets for future surveys.

  13. Properties of galaxy groups in the Sloan Digital Sky Survey - II. Active galactic nucleus feedback and star formation truncation

    NASA Astrophysics Data System (ADS)

    Weinmann, Simone M.; van den Bosch, Frank C.; Yang, Xiaohu; Mo, H. J.; Croton, Darren J.; Moore, Ben

    2006-11-01

    Successfully reproducing the galaxy luminosity function (LF) and the bimodality in the galaxy distribution requires a mechanism that can truncate star formation in massive haloes. Current models of galaxy formation consider two such truncation mechanisms: strangulation, which acts on satellite galaxies, and active galactic nucleus (AGN) feedback, which predominantly affects central galaxies. The efficiencies of these processes set the blue fraction of galaxies, fblue(L, M), as a function of galaxy luminosity, L, and halo mass, M. In this paper, we use a galaxy group catalogue extracted from the Sloan Digital Sky Survey (SDSS) to determine fblue(L, M). To demonstrate the potential power of these data as a benchmark for galaxy formation models, we compare the results to the semi-analytical model for galaxy formation of Croton et al. Although this model accurately fits the global statistics of the galaxy population, as well as the shape of the conditional LF, there are significant discrepancies when the blue fraction of galaxies as a function of mass and luminosity is compared between the observations and the model. In particular, the model predicts (i) too many faint satellites in massive haloes, (ii) a blue fraction of satellites that is much too low, and (iii) a blue fraction of centrals that is too high and with an inverted luminosity dependence. In the same order, we argue that these discrepancies owe to (i) the neglect of tidal stripping in the semi-analytical model, (ii) the oversimplified treatment of strangulation, and (iii) improper modelling of dust extinction and/or AGN feedback. The data presented here will prove useful to test and calibrate future models of galaxy formation and, in particular, to discriminate between various models for AGN feedback and other star formation truncation mechanisms.

  14. The MUSCLES Treasury Survey. IV. Scaling Relations for Ultraviolet, Ca ii K, and Energetic Particle Fluxes from M Dwarfs

    NASA Astrophysics Data System (ADS)

    Youngblood, Allison; France, Kevin; Parke Loyd, R. O.; Brown, Alexander; Mason, James P.; Schneider, P. Christian; Tilley, Matt A.; Berta-Thompson, Zachory K.; Buccino, Andrea; Froning, Cynthia S.; Hawley, Suzanne L.; Linsky, Jeffrey; Mauas, Pablo J. D.; Redfield, Seth; Kowalski, Adam; Miguel, Yamila; Newton, Elisabeth R.; Rugheimer, Sarah; Segura, Antígona; Roberge, Aki; Vieytes, Mariela

    2017-07-01

    Characterizing the UV spectral energy distribution (SED) of an exoplanet host star is critically important for assessing its planet’s potential habitability, particularly for M dwarfs, as they are prime targets for current and near-term exoplanet characterization efforts and atmospheric models predict that their UV radiation can produce photochemistry on habitable zone planets different from that on Earth. To derive ground-based proxies for UV emission for use when Hubble Space Telescope (HST) observations are unavailable, we have assembled a sample of 15 early to mid-M dwarfs observed by HST and compared their nonsimultaneous UV and optical spectra. We find that the equivalent width of the chromospheric Ca ii K line at 3933 Å, when corrected for spectral type, can be used to estimate the stellar surface flux in ultraviolet emission lines, including H i Lyα. In addition, we address another potential driver of habitability: energetic particle fluxes associated with flares. We present a new technique for estimating soft X-ray and >10 MeV proton flux during far-UV emission line flares (Si iv and He ii) by assuming solar-like energy partitions. We analyze several flares from the M4 dwarf GJ 876 observed with HST and Chandra as part of the MUSCLES Treasury Survey and find that habitable zone planets orbiting GJ 876 are impacted by large Carrington-like flares with peak soft X-ray fluxes ≥10-3 W m-2 and possible proton fluxes ˜102-103 pfu, approximately four orders of magnitude more frequently than modern-day Earth.

  15. Food consumption of adults in Germany: results of the German National Nutrition Survey II based on diet history interviews.

    PubMed

    Heuer, Thorsten; Krems, Carolin; Moon, Kilson; Brombach, Christine; Hoffmann, Ingrid

    2015-05-28

    The second German National Nutrition Survey (NVS II) aimed to evaluate food consumption and other aspects of nutritional behaviour of a representative sample of the German population, using a modular design with three different dietary assessment methods. To assess usual food consumption, 15,371 German speaking subjects 14-80 years of age completed a diet history interview between November 2005 and November 2006. With reference to the guidelines of the German Nutrition Society (DGE), NVS II observed that the German population did not eat enough foods of plant origin, especially vegetables and consumed too much of meat and meat products. While generally similar food consumption is observed in other European countries, consumption of bread, fruit juices/nectars and beer is higher in Germany. On average, men consumed two times more meat and soft drinks as well as six times more beer than women did, whereas the consumption of vegetables, fruit as well as herbal/fruit tea was higher in women. Older participants showed a lower consumption of meat, fruit juice/nectars, soft drinks and spirits as well as a higher consumption of fish, vegetables, fruit, and herbal/fruit tea than adolescents and younger adults did. There are also differences in food consumption with regard to socio-economic status (SES). Persons with higher SES consumed more vegetables, fruit, fish, water, coffee/tea and wine, while persons with lower SES consumed more meat and meat products, soft drinks and beer. In general, the food consumption of women, the elderly and the higher SES group tends to be closer to the official dietary guidelines in Germany.

  16. The Swift X-ray Telescope Cluster Survey. II. X-ray spectral analysis

    NASA Astrophysics Data System (ADS)

    Tozzi, P.; Moretti, A.; Tundo, E.; Liu, T.; Rosati, P.; Borgani, S.; Tagliaferri, G.; Campana, S.; Fugazza, D.; D'Avanzo, P.

    2014-07-01

    < 0.4. We derive the luminosity-temperature relation for these 46 sources, finding good agreement with previous studies. Conclusions: Thanks to the good X-ray spectral quality and the low background of Swift/XRT, we are able to measure ICM temperatures and X-ray luminosities for the 46 sources with redshifts. Once redshifts are available for the remaining 26 sources, this sample will constitute a well-characterized, flux-limited catalog of clusters distributed over a broad redshift range (0.1 ≤ z ≤ 1.0) providing a statistically complete view of the cluster population with a selection function that allows a proper treatment of any measurement bias. The quality of the SWXCS sample is comparable to other samples available in the literature and obtained with much larger X-ray telescopes. Our results have interesting implications for the design of future X-ray survey telescopes, characterized by good-quality PSF over the entire field of view and low background. Tables 1 and 2 and Appendix A are available in electronic form at http://www.aanda.orgCatalog and data products of SWXCS, constantly updated, are made available to the public through the websites http://www.arcetri.astro.it/SWXCS/ and http://swxcs.ustc.edu.cn/

  17. Impact of flat panel-imager veiling glare on scatter-estimation accuracy and image quality of a commercial on-board cone-beam CT imaging system.

    PubMed

    Lazos, Dimitrios; Williamson, Jeffrey F

    2012-09-01

    The purposes of this study is to measure the low frequency drop (LFD) of the modulation transfer function (MTF), associated with the long tails of the detector point spread function (PSF) of an on-board flat panel imager and study its impact on cone-beam CT (CBCT) image quality and scatter measurement accuracy. Two different experimental methods were used to characterize LFD and its associated PSF of a Varian OBI flat-panel detector system: the edge response function (ERF) method and the disk transfer function (DTF) method. PSF was estimated by fitting parametric models to these measurements for four values of the applied voltage (kVp). The resultant PSF was used to demonstrate the effect of LFD on image contrast and CT number accuracy in CBCT images reconstructed from synthetic datasets, as well as, accuracy of scatter measurements with the beam-stop method. The MTFs derived from the measured ERF data revealed LFDs varying from 8% (at 60 kVp) to 10.5% (at 120 kVp), while the intensity of the long PSF tails was found to increase with increasing kVp. The veiling glare line spread functions derived from the ERF and DTF methods were in excellent agreement. Uncorrected veiling glare reduced contrast and the image intensity in CBCT reconstruction, near the phantom periphery (by 67 Hounsfield units in a 20 cm-in-diameter water phantom) and (to a smaller degree) near inhomogeneities. Use of the bow-tie filter mitigated these effects. Veiling glare also resulted in about 10%-15% overestimation of the scatter-to-primary ratio when measured with the beam-stop or beam-stop array method. The long tails of the detector PSF were found to have a modest dependence of beam spectrum, which is reflected on the MTF curve LFD. Our findings show that uncorrected veiling glare can affect quantitative accuracy and contrast in CBCT imaging, based on flat panel imager. In addition, it results in overestimation of the scatter-to-primary ratio, measured with the beam-stop methods.

  18. The Effect of Three Levels of Laser Glare on the Speed and Accuracy of Target Location Performance When Viewing a Briefly Presented Visual Array.

    DTIC Science & Technology

    1990-11-01

    glare, lens opacity (Interzeag, Opacity Lensmeter), and color sensitivity (Farnsworth- Munsell 100- Hue Test , Kollmorgen Corp., Baltimore, MD). TABLE 2...this project including subject scheduling, administration of vision aspessment tests , and data collection. In addition, LCDR Larry Schoenberg is r...1.50 (0.05) 2.47 (0.06) 4 2ý06 (0.12) 1.36 (0.10) 2.26 (0.18) 5 1.72 (0.14) 1.20 (0.09) 1.92 (0.15) 7 PROCEDURES Subjects were tested separately. They

  19. Impact of flat panel-imager veiling glare on scatter-estimation accuracy and image quality of a commercial on-board cone-beam CT imaging system

    SciTech Connect

    Lazos, Dimitrios; Williamson, Jeffrey F.

    2012-09-15

    Purpose: The purposes of this study is to measure the low frequency drop (LFD) of the modulation transfer function (MTF), associated with the long tails of the detector point spread function (PSF) of an on-board flat panel imager and study its impact on cone-beam CT (CBCT) image quality and scatter measurement accuracy. Methods: Two different experimental methods were used to characterize LFD and its associated PSF of a Varian OBI flat-panel detector system: the edge response function (ERF) method and the disk transfer function (DTF) method. PSF was estimated by fitting parametric models to these measurements for four values of the applied voltage (kVp). The resultant PSF was used to demonstrate the effect of LFD on image contrast and CT number accuracy in CBCT images reconstructed from synthetic datasets, as well as, accuracy of scatter measurements with the beam-stop method. Results: The MTFs derived from the measured ERF data revealed LFDs varying from 8% (at 60 kVp) to 10.5% (at 120 kVp), while the intensity of the long PSF tails was found to increase with increasing kVp. The veiling glare line spread functions derived from the ERF and DTF methods were in excellent agreement. Uncorrected veiling glare reduced contrast and the image intensity in CBCT reconstruction, near the phantom periphery (by 67 Hounsfield units in a 20 cm-in-diameter water phantom) and (to a smaller degree) near inhomogeneities. Use of the bow-tie filter mitigated these effects. Veiling glare also resulted in about 10%-15% overestimation of the scatter-to-primary ratio when measured with the beam-stop or beam-stop array method. Conclusions: The long tails of the detector PSF were found to have a modest dependence of beam spectrum, which is reflected on the MTF curve LFD. Our findings show that uncorrected veiling glare can affect quantitative accuracy and contrast in CBCT imaging, based on flat panel imager. In addition, it results in overestimation of the scatter-to-primary ratio, measured

  20. An X-ray survey of the 2 Jy sample - II. X-ray emission from extended structures

    NASA Astrophysics Data System (ADS)

    Mingo, B.; Hardcastle, M. J.; Ineson, J.; Mahatma, V.; Croston, J. H.; Dicken, D.; Evans, D. A.; Morganti, R.; Tadhunter, C.

    2017-09-01

    The 2 Jy sample is a survey of radio galaxies with flux densities above 2 Jy at 2.7 GHz. As part of our ongoing work on the southern subset of 2 Jy sources, in paper I of this series we analysed the X-ray cores of the complete 2 Jy sample with redshifts 0.05 < z < 0.7. For this work we focus on the X-ray emission associated with the extended structures (jets, lobes, and environments) of the complete subset of 2 Jy sources with 0.05 < z < 0.2 that we have observed with Chandra. We find that hotspots and jet knots are ubiquitous in Fanaroff-Riley class II (FRII) sources, which also inhabit systematically poorer environments than the Fanaroff-Riley class I (FRI) sources in our sample. Spectral fits of the hotspots with good X-ray statistics invariably show properties consistent with synchrotron emission, and we show that inverse-Compton mechanisms underpredict the X-ray emission we observe by 1-2 orders of magnitude. Inverse-Compton emission is detected from many of the lobes in our sample, and we find that the lobes of the FRII sources show magnetic fields lower by up to an order of magnitude than expected from equipartition extrapolations. This is consistent with previous results, which show that most FRII sources have electron energy densities higher than minimum energy requirements.

  1. Mechanistic study of the hydrodesulfurization of methanethiol over tungsten disulfide. II. A survey of rare earth sulfides for hydrodesulfurization activity

    SciTech Connect

    Dowd, D.Q.

    1985-01-01

    I. Hydrodesulfurization is a process whereby sulfur bound in organic compounds is removed as hydrogen sulfide, and is important to the control of sulfur dioxide emissions in the combustion of petroleum and coal fuels. It involves the cleavage of carbon sulfur bonds, and is catalyzed by layered disulfides such as molybdenum and tungsten disulfide. The simplest example is the reaction CH/sub 3/SH + H/sub 2/ ..-->.. CH/sub 4/ + H/sub 2/S. The mechanism of even this prototypical reaction is unclear. In an effort to clarify it, the kinetics of methanethiol hydro desulfurization over tungsten disulfide at low pressures was established, with partial pressures of methanethiol and hydrogen varied over a hundred fold. The kinetic order in each reactant was positive when its partial pressure was low, negative when its partial pressure was high. The negative order in hydrogen had not been previously seen. The product gases, methane and hydrogen sulfide, each exhibited negative kinetic orders at high partial pressures, zero kinetic orders at low partial pressures. A dual site Langmuir-Hinshelwood type mechanism, which defines one active site as two adjacent edge sulfur vacancies and the second as a neighboring sulfur atom, describes these results quite well. II. Seventeen rare earth sulfides were surveyed for catalytic activity toward methanethiol hydrodesulfurization. These sulfides included both stoichiometric and nonstoichiometric compositions and four different morphologies. In general, nonconductors were inactive and conductors were active. This correlation extended to the nonstoichiometric ..gamma..-phase sesquisulfides which exhibit both insulating and conducting properties.

  2. Lost in the Glare

    NASA Image and Video Library

    Within our own solar system we can observe planetary transits of Mercury and Venus when they pass in front of the Sun as viewed from Earth. Kepler will observe the same phenomena in order to detect...

  3. An Evaluative Survey Report on ESEA Title II: Fiscal Years 1966-1968. Part I, Analysis and Interpretation. Part II, Tables.

    ERIC Educational Resources Information Center

    Office of Education (DHEW), Washington, DC.

    This report provides benchmark data on the effects that the provision of school library resources, textbooks, and other instructional materials under Title II of the Elementary and Secondary Education Act (ESEA) has had on education in the nation's public and private elementary and secondary schools. The passage of Title II of ESEA set the stage…

  4. Investigations in Time and of Space Using the FIRST Survey: Radio Source Variability and the Evolution of FR II Quasars

    NASA Astrophysics Data System (ADS)

    Thyagarajan, Nithyanandan

    The FIRST survey covered ∼10,000 deg2 of the sky over a decade, providing unprecedented levels of flux density sensitivity (∼ 1 mJy) at 1.4 GHz, uniformity to within 15% (at ∼0.15 mJy rms), 5.4" angular resolution, astrometric accuracy to better than 1" and has cataloged ≳ 800,000 sources. It has made enormous contributions to diverse scientific ends including such subjects as radio source populations, quasars, large-scale structure and clustering of radio sources, gravitational lensing, cosmology, etc. I present the motivation, analysis and results of two projects also intended to demonstrate the power and expand the scope of the FIRST survey's scientific reach. A comprehensive search for variable and transient radio sources has been conducted using the ∼55,000 snapshot images of the FIRST survey. An analysis leading to the discovery of 1,651 variable and transient objects down to mJy levels over a wide range of timescales (few minutes to years) is presented. The multi-wavelength matching for counterparts reveals the diverse classes of objects exhibiting variability. Interestingly, ∼ 60% of the objects in the sample have either no classified counterparts or no corresponding sources at any other wavelength and require multi-wavelength follow-up observations. I discuss these classes of variables and speculate on the identity of objects that lack multi-wavelength counterparts. Thus, the FIRST survey has yielded the largest sample by far of radio variables and transients to date to unprecedented levels of sensitivity and sky coverage and demonstrates the promise of future radio instruments which have transient-detection as one of their key science projects. For decades, radio astronomers have attempted to use double-lobed radio sources to constrain the angular size-redshift (θ - z ) relation and to derive cosmological parameters therefrom. Most of the early attempts have, embarrassingly, shown general consistency with a static Euclidean universe rather

  5. Objectives and methodology of Romanian SEPHAR II Survey. Project for comparing the prevalence and control of cardiovascular risk factors in two East-European countries: Romania and Poland

    PubMed Central

    Dorobantu, Maria; Tautu, Oana-Florentina; Ghiorghe, Silviu; Badila, Elisabeta; Dana, Minca; Dobreanu, Minodora; Baila, Ilarie; Rutkowski, Marcin; Zdrojewski, Tomasz

    2015-01-01

    Introduction Comparing results of representative surveys conducted in different East-European countries could contribute to a better understanding and management of cardiovascular risk factors, offering grounds for the development of health policies addressing the special needs of this high cardiovascular risk region of Europe. The aim of this paper was to describe the methodology on which the comparison between the Romanian survey SEPHAR II and the Polish survey NATPOL 2011 results is based. Material and methods SEPHAR II, like NATPOL 2011, is a cross-sectional survey conducted on a representative sample of the adult Romanian population (18 to 80 years) and encompasses two visits with the following components: completing the study questionnaire, blood pressure and anthropometric measurements, and collection of blood and urine samples. Results From a total of 2223 subjects found at 2860 visited addresses, 2044 subjects gave written consent but only 1975 subjects had eligible data for the analysis, accounting for a response rate of 69.06%. Additionally we excluded 11 subjects who were 80 years of age (NATPOL 2011 included adult subjects up to 79 years). Therefore, the sample size included in the statistical analysis is 1964. It has similar age groups and gender structure as the Romanian population aged 18–79 years from the last census available at the moment of conducting the survey (weight adjustments for epidemiological analyses range from 0.48 to 8.7). Conclusions Sharing many similarities, the results of SEPHAR II and NATPOL 2011 surveys can be compared by a proper statistical method offering crucial information regarding cardiovascular risk factors in a high-cardiovascular risk European region. PMID:26322082

  6. Objectives and methodology of Romanian SEPHAR II Survey. Project for comparing the prevalence and control of cardiovascular risk factors in two East-European countries: Romania and Poland.

    PubMed

    Dorobantu, Maria; Tautu, Oana-Florentina; Darabont, Roxana; Ghiorghe, Silviu; Badila, Elisabeta; Dana, Minca; Dobreanu, Minodora; Baila, Ilarie; Rutkowski, Marcin; Zdrojewski, Tomasz

    2015-08-12

    Comparing results of representative surveys conducted in different East-European countries could contribute to a better understanding and management of cardiovascular risk factors, offering grounds for the development of health policies addressing the special needs of this high cardiovascular risk region of Europe. The aim of this paper was to describe the methodology on which the comparison between the Romanian survey SEPHAR II and the Polish survey NATPOL 2011 results is based. SEPHAR II, like NATPOL 2011, is a cross-sectional survey conducted on a representative sample of the adult Romanian population (18 to 80 years) and encompasses two visits with the following components: completing the study questionnaire, blood pressure and anthropometric measurements, and collection of blood and urine samples. From a total of 2223 subjects found at 2860 visited addresses, 2044 subjects gave written consent but only 1975 subjects had eligible data for the analysis, accounting for a response rate of 69.06%. Additionally we excluded 11 subjects who were 80 years of age (NATPOL 2011 included adult subjects up to 79 years). Therefore, the sample size included in the statistical analysis is 1964. It has similar age groups and gender structure as the Romanian population aged 18-79 years from the last census available at the moment of conducting the survey (weight adjustments for epidemiological analyses range from 0.48 to 8.7). Sharing many similarities, the results of SEPHAR II and NATPOL 2011 surveys can be compared by a proper statistical method offering crucial information regarding cardiovascular risk factors in a high-cardiovascular risk European region.

  7. Evolution of the cosmological mass density of neutral gas from Sloan Digital Sky Survey II - Data Release 7

    NASA Astrophysics Data System (ADS)

    Noterdaeme, P.; Petitjean, P.; Ledoux, C.; Srianand, R.

    2009-10-01

    We present the results of a search for damped Lyman-α (DLA) systems in the Sloan Digital Sky Survey II (SDSS), Data Release 7. We use a fully automatic procedure to identify DLAs and derive their column densities. The procedure is checked against the results of previous searches for DLAs in SDSS. We discuss the agreements and differences and show the robustness of our procedure. For each system, we obtain an accurate measurement of the absorber's redshift, the H I column density and the equivalent width of associated metal absorption lines, without any human intervention. We find 1426 absorbers with 2.15 < z < 5.2 with log N(H I) ≥ 20, out of which 937 systems have log N(H I) ≥ 20.3. This is the largest DLA sample ever built, made available to the scientific community through the electronic version of this paper. In the course of the survey, we discovered the intervening DLA with highest H I column density known to date with log N(H I) = 22.0±0.1. This single system provides a strong constraint on the high-end of the N(H I) frequency distribution now measured with high accuracy. We show that the presence of a DLA at the blue end of a QSO spectrum can lead to important systematic errors and propose a method to avoid them. This has important consequences for the measurement of the cosmological mass density of neutral gas at z ~ 2.2 and therefore on our understanding of galaxy evolution over the past 10 billion years. We find a significant decrease of the cosmological mass density of neutral gas in DLAs, Ω_g^DLA, from z = 4 to z = 2.2, consistent with the result of previous SDSS studies. However, and contrary to other SDSS studies, we find that Ω_g^DLA(z = 2.2) is about twice the value at z = 0. This implies that Ω_g^DLA keeps decreasing at z < 2.2. Catalog is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/505/1087

  8. A Measurement of the Rate of Type Ia Supernovae in Galaxy Clusters from the SDSS-II Supernova Survey

    SciTech Connect

    Dilday, Benjamin; Bassett, Bruce; Becker, Andrew; Bender, Ralf; Castander, Francisco; Cinabro, David; Frieman, Joshua A.; Galbany, Lluis; Garnavich, Peter; Goobar, Ariel; Hopp, Ulrich; /Munich, Tech. U. /Munich U. Observ. /Tokyo U.

    2010-03-01

    We present measurements of the Type Ia supernova (SN) rate in galaxy clusters based on data from the Sloan Digital Sky Survey-II (SDSS-II) Supernova Survey. The cluster SN Ia rate is determined from 9 SN events in a set of 71 C4 clusters at z {le} 0.17 and 27 SN events in 492 maxBCG clusters at 0.1 {le} z {le} 0.3. We find values for the cluster SN Ia rate of (0.37{sub -0.12-0.01}{sup +0.17+0.01}) SNur h{sup 2} and (0.55{sub -0.11-0.01}{sup +0.13+0.02}) SNur h{sup 2} (SNux = 10{sup -12}L{sub x{circle_dot}}{sup -1} yr{sup -1}) in C4 and maxBCG clusters, respectively, where the quoted errors are statistical and systematic, respectively. The SN rate for early-type galaxies is found to be (0.31{sub -0.12-0.01}{sup +0.18+0.01}) SNur h{sup 2} and (0.49{sub -0.11-0.01}{sup +0.15+0.02}) SNur h{sup 2} in C4 and maxBCG clusters, respectively. The SN rate for the brightest cluster galaxies (BCG) is found to be (2.04{sub -1.11-0.04}{sup +1.99+0.07}) SNur h{sup 2} and (0.36{sub -0.30-0.01}{sup +0.84+0.01}) SNur h{sup 2} in C4 and maxBCG clusters, respectively. The ratio of the SN Ia rate in cluster early-type galaxies to that of the SN Ia rate in field early-type galaxies is 1.94{sub -0.91-0.015}{sup +1.31+0.043} and 3.02{sub -1.03-0.048}{sup +1.31+0.062}, for C4 and maxBCG clusters, respectively. The SN rate in galaxy clusters as a function of redshift, which probes the late time SN Ia delay distribution, shows only weak dependence on redshift. Combining our current measurements with previous measurements, we fit the cluster SN Ia rate data to a linear function of redshift, and find r{sub L} = [(0.49{sub -0.14}{sup +0.15}) + (0.91{sub -0.81}{sup +0.85}) x z] SNuB h{sup 2}. A comparison of the radial distribution of SNe in cluster to field early-type galaxies shows possible evidence for an enhancement of the SN rate in the cores of cluster early-type galaxies. With an observation of at most 3 hostless, intra-cluster SNe Ia, we estimate the fraction of cluster SNe that are

  9. A MEASUREMENT OF THE RATE OF TYPE Ia SUPERNOVAE IN GALAXY CLUSTERS FROM THE SDSS-II SUPERNOVA SURVEY

    SciTech Connect

    Dilday, Benjamin; Jha, Saurabh W.; Bassett, Bruce; Becker, Andrew; Bender, Ralf; Hopp, Ulrich; Castander, Francisco; Cinabro, David; Frieman, Joshua A.; Galbany, LluIs; Miquel, Ramon; Garnavich, Peter; Goobar, Ariel; Ihara, Yutaka; Kessler, Richard; Lampeitl, Hubert; Nichol, Robert C.; Marriner, John; Molla, Mercedes

    2010-06-01

    We present measurements of the Type Ia supernova (SN) rate in galaxy clusters based on data from the Sloan Digital Sky Survey-II (SDSS-II) Supernova Survey. The cluster SN Ia rate is determined from 9 SN events in a set of 71 C4 clusters at z {<=} 0.17 and 27 SN events in 492 maxBCG clusters at 0.1 {<=} z {<=} 0.3. We find values for the cluster SN Ia rate of (0.37{sup +0.17+0.01} {sub -0.12-0.01}) SNur h {sup 2} and (0.55{sup +0.13+0.02} {sub -0.11-0.01}) SNur h {sup 2} (SNux = 10{sup -12} L {sup -1} {sub xsun} yr{sup -1}) in C4 and maxBCG clusters, respectively, where the quoted errors are statistical and systematic, respectively. The SN rate for early-type galaxies is found to be (0.31{sup +0.18+0.01} {sub -0.12-0.01}) SNur h {sup 2} and (0.49{sup +0.15+0.02} {sub -0.11-0.01}) SNur h {sup 2} in C4 and maxBCG clusters, respectively. The SN rate for the brightest cluster galaxies (BCG) is found to be (2.04{sup +1.99+0.07} {sub -1.11-0.04}) SNur h {sup 2} and (0.36{sup +0.84+0.01} {sub -0.30-0.01}) SNur h {sup 2} in C4 and maxBCG clusters, respectively. The ratio of the SN Ia rate in cluster early-type galaxies to that of the SN Ia rate in field early-type galaxies is 1.94{sup +1.31+0.043} {sub -0.91-0.015} and 3.02{sup +1.31+0.062} {sub -1.03-0.048}, for C4 and maxBCG clusters, respectively. The SN rate in galaxy clusters as a function of redshift, which probes the late time SN Ia delay distribution, shows only weak dependence on redshift. Combining our current measurements with previous measurements, we fit the cluster SN Ia rate data to a linear function of redshift, and find r{sub L} = [(0.49{sup +0.15} {sub -0.14})+(0.91{sup +0.85} {sub -0.81}) x z] SNuB h {sup 2}. A comparison of the radial distribution of SNe in cluster to field early-type galaxies shows possible evidence for an enhancement of the SN rate in the cores of cluster early-type galaxies. With an observation of at most three hostless, intra-cluster SNe Ia, we estimate the fraction of cluster SNe

  10. Comparison of two dietary assessment methods by food consumption: results of the German National Nutrition Survey II.

    PubMed

    Eisinger-Watzl, Marianne; Straßburg, Andrea; Ramünke, Josa; Krems, Carolin; Heuer, Thorsten; Hoffmann, Ingrid

    2015-04-01

    To further characterise the performance of the diet history method and the 24-h recalls method, both in an updated version, a comparison was conducted. The National Nutrition Survey II, representative for Germany, assessed food consumption with both methods. The comparison was conducted in a sample of 9,968 participants aged 14-80. Besides calculating mean differences, statistical agreement measurements encompass Spearman and intraclass correlation coefficients, ranking participants in quartiles and the Bland-Altman method. Mean consumption of 12 out of 18 food groups was higher assessed with the diet history method. Three of these 12 food groups had a medium to large effect size (e.g., raw vegetables) and seven showed at least a small strength while there was basically no difference for coffee/tea or ice cream. Intraclass correlations were strong only for beverages (>0.50) and revealed the least correlation for vegetables (<0.20). Quartile classification of participants exhibited more than two-thirds being ranked in the same or adjacent quartile assessed by both methods. For every food group, Bland-Altman plots showed that the agreement of both methods weakened with increasing consumption. The cognitive effort essential for the diet history method to remember consumption of the past 4 weeks may be a source of inaccurateness, especially for inhomogeneous food groups. Additionally, social desirability gains significance. There is no assessment method without errors and attention to specific food groups is a critical issue with every method. Altogether, the 24-h recalls method applied in the presented study, offers advantages approximating food consumption as compared to the diet history method.

  11. Energy Savings Opportunity Survey Energy Engineering Analysis Program (EEAP) Fort Campbell, Kentucky, Phase II. Volume 1, Section 1-3.

    DTIC Science & Technology

    1993-11-01

    includes an exterior lighting survey of five locations around the facility, a comprehensive survey of two generators at the Water Treatment Plant and Boiling Springs Pump House, and four chillers serving four buildings.

  12. Constraining Stellar Properties of Intervening Damped Lyα and Mg II Absorbing Galaxies toward GRB 050730

    NASA Astrophysics Data System (ADS)

    Minowa, Y.; Okoshi, K.; Kobayashi, N.; Takami, H.

    2012-09-01

    We performed multiband deep imaging of the field around GRB 050730 to identify the host galaxies of intervening absorbers, which consist of a damped Lyα absorption (DLA) system at z abs = 3.564, a sub-DLA system at z abs = 3.022, and strong Mg II absorption systems at z abs = 1.773 and 2.253. Our observations were performed after the gamma-ray burst afterglow had disappeared. Thus, our imaging survey has a higher sensitivity to the host galaxies of the intervening absorbers than the normal imaging surveys in the direction of QSOs, for which the QSO glare tends to hide the foreground galaxies. In this deep imaging survey, we could not detect any unambiguous candidates for the host galaxies of the intervening absorbers. Using the 3σ upper limit of the flux in the optical to mid-infrared observing bands, which corresponds to the UV to optical bands in the rest frame of the intervening absorbers, we constrained the star formation rates and stellar masses of the hosts. We estimated the star formation rates for the intervening absorbers to be <~ 2.5 M ⊙ yr-1 for z > 3 DLAs and <~ 1.0 M ⊙ yr-1 for z ~ 2 Mg II systems. Their stellar masses are estimated to be several times 109 M ⊙ or smaller for all intervening galaxies. These properties are comparable to dwarf galaxies, rather than the massive star-forming galaxies commonly seen in the z > 2 galaxy surveys based on emission-line selection or color selection.

  13. Measurements of the Rate of Type Ia Supernovae at Redshift z < ~0.3 from the SDSS-II Supernova Survey

    SciTech Connect

    Dilday, Benjamin; Smith, Mathew; Bassett, Bruce; Becker, Andrew; Bender, Ralf; Castander, Francisco; Cinabro, David; Filippenko, Alexei V.; Frieman, Joshua A.; Galbany, Lluis; Garnavich, Peter M.; /Notre Dame U. /Stockholm U., OKC /Stockholm U.

    2010-01-01

    We present a measurement of the volumetric Type Ia supernova (SN Ia) rate based on data from the Sloan Digital Sky Survey II (SDSS-II) Supernova Survey. The adopted sample of supernovae (SNe) includes 516 SNe Ia at redshift z {approx}< 0.3, of which 270 (52%) are spectroscopically identified as SNe Ia. The remaining 246 SNe Ia were identified through their light curves; 113 of these objects have spectroscopic redshifts from spectra of their host galaxy, and 133 have photometric redshifts estimated from the SN light curves. Based on consideration of 87 spectroscopically confirmed non-Ia SNe discovered by the SDSS-II SN Survey, we estimate that 2.04{sub -0.95}{sup +1.61}% of the photometric SNe Ia may be misidentified. The sample of SNe Ia used in this measurement represents an order of magnitude increase in the statistics for SN Ia rate measurements in the redshift range covered by the SDSS-II Supernova Survey. If we assume a SN Ia rate that is constant at low redshift (z < 0.15), then the SN observations can be used to infer a value of the SN rate of r{sub V} = (2.69{sub -0.30-0.01}{sup +0.34+0.21}) x 10{sup -5} SNe yr{sup -1} Mpc{sup -3} (H{sub 0}/(70 km s{sup -1} Mpc{sup -1})){sup 3} at a mean redshift of {approx} 0.12, based on 79 SNe Ia of which 72 are spectroscopically confirmed. However, the large sample of SNe Ia included in this study allows us to place constraints on the redshift dependence of the SN Ia rate based on the SDSS-II Supernova Survey data alone. Fitting a power-law model of the SN rate evolution, r{sub V} (z) = A{sub p} x ((1+z)/(1+z{sub 0})){sup {nu}}, over the redshift range 0.0 < z < 0.3 with z{sub 0} = 0.21, results in A{sub p} = (3.43{sub -0.15}{sup +0.15}) x 10{sup -5} SNe yr{sup -1} Mpc{sup -3} (H{sub 0}/(70 km s{sup -1} Mpc{sup -1})){sup 3} and {nu} = 2.04{sub -0.89}{sup +0.90}.

  14. The MUSCLES Treasury Survey. II. Intrinsic LYα and Extreme Ultraviolet Spectra of K and M Dwarfs with Exoplanets*

    NASA Astrophysics Data System (ADS)

    Youngblood, Allison; France, Kevin; Parke Loyd, R. O.; Linsky, Jeffrey L.; Redfield, Seth; Schneider, P. Christian; Wood, Brian E.; Brown, Alexander; Froning, Cynthia; Miguel, Yamila; Rugheimer, Sarah; Walkowicz, Lucianne

    2016-06-01

    The ultraviolet (UV) spectral energy distributions (SEDs) of low-mass (K- and M-type) stars play a critical role in the heating and chemistry of exoplanet atmospheres, but are not observationally well-constrained. Direct observations of the intrinsic flux of the Lyα line (the dominant source of UV photons from low-mass stars) are challenging, as interstellar H i absorbs the entire line core for even the closest stars. To address the existing gap in empirical constraints on the UV flux of K and M dwarfs, the MUSCLES Hubble Space Telescope Treasury Survey has obtained UV observations of 11 nearby M and K dwarfs hosting exoplanets. This paper presents the Lyα and extreme-UV spectral reconstructions for the MUSCLES targets. Most targets are optically inactive, but all exhibit significant UV activity. We use a Markov Chain Monte Carlo technique to correct the observed Lyα profiles for interstellar absorption, and we employ empirical relations to compute the extreme-UV SED from the intrinsic Lyα flux in ˜100 Å bins from 100-1170 Å. The reconstructed Lyα profiles have 300 km s-1 broad cores, while >1% of the total intrinsic Lyα flux is measured in extended wings between 300 and 1200 km s-1. The Lyα surface flux positively correlates with the Mg ii surface flux and negatively correlates with the stellar rotation period. Stars with larger Lyα surface flux also tend to have larger surface flux in ions formed at higher temperatures, but these correlations remain statistically insignificant in our sample of 11 stars. We also present H i column density measurements for 10 new sightlines through the local interstellar medium. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555.

  15. The 2XMMi/SDSS Galaxy Cluster Survey. II. The optically confirmed cluster sample and the LX - T relation

    NASA Astrophysics Data System (ADS)

    Takey, A.; Schwope, A.; Lamer, G.

    2013-10-01

    Aims: We compile a sample of X-ray-selected galaxy groups and clusters from the XMM-Newton serendipitous source catalogue (2XMMi-DR3) with optical confirmation and redshift measurement from the Sloan Digital Sky Survey (SDSS). We present an analysis of the X-ray properties of this new sample with particular emphasis on the X-ray luminosity-temperature (LX - T) relation. Methods: The X-ray cluster candidates were selected from the 2XMMi-DR3 catalogue in the footprint of the SDSS-DR7. We developed a finding algorithm to search for overdensities of galaxies at the positions of the X-ray cluster candidates in the photometric redshift space and to measure the redshifts of the clusters from the SDSS data. For optically confirmed clusters with good quality X-ray data we derived the X-ray flux, luminosity, and temperature from proper spectral fits, while the X-ray flux for clusters with low-quality X-ray data was obtained from the 2XMMi-DR3 catalogue. Results: The detection algorithm provides the photometric redshift of 530 galaxy clusters. Of these, 310 clusters have a spectroscopic redshift for at least one member galaxy. About 75 percent of the optically confirmed cluster sample are newly discovered X-ray clusters. Moreover, 301 systems are known as optically selected clusters in the literature while the remainder are new discoveries in X-ray and optical bands. The optically confirmed cluster sample spans a wide redshift range 0.03-0.70 (median z = 0.32). In this paper, we present the catalogue of X-ray-selected galaxy groups and clusters from the 2XMMi/SDSS galaxy cluster survey. The catalogue has two subsamples: (i) a cluster sample comprising 345 objects with their X-ray spectroscopic temperature and flux from the spectral fitting; and (ii) a cluster sample consisting of 185 systems with their X-ray flux from the 2XMMi-DR3 catalogue, because their X-ray data are insufficient for spectral fitting. For each cluster, the catalogue also provides the X-ray bolometric

  16. Early-time light curves of Type Ib/c supernovae from the SDSS-II Supernova Survey

    NASA Astrophysics Data System (ADS)

    Taddia, F.; Sollerman, J.; Leloudas, G.; Stritzinger, M. D.; Valenti, S.; Galbany, L.; Kessler, R.; Schneider, D. P.; Wheeler, J. C.

    2015-02-01

    Context. Type Ib/c supernovae (SNe Ib/c) have been investigated in several single-object studies; however, there is still a paucity of works concerning larger, homogeneous samples of these hydrogen-poor transients, in particular regarding the premaximum phase of their light curves. Aims: In this paper we present and analyze the early-time optical light curves (LCs, ugriz) of 20 SNe Ib/c from the Sloan Digital Sky Survey (SDSS) SN survey II, aiming to study their observational and physical properties, as well as to derive their progenitor parameters. Methods: High-cadence, multiband LCs are fitted with a functional model and the best-fit parameters are compared among the SN types. Bolometric LCs (BLCs) are constructed for the entire sample. We also computed the black-body (BB) temperature (TBB) and photospheric radius (Rph) evolution for each SN via BB fits on the spectral energy distributions. In addition, the bolometric properties are compared to both hydrodynamical and analytical model expectations. Results: Complementing our sample with literature data, we find that SNe Ic and Ic-BL (broad-line) have shorter rise times than those of SNe Ib and IIb. The decline rate parameter, Δm15, is similar among the different subtypes. SNe Ic appear brighter and bluer than SNe Ib, but this difference vanishes if we consider host galaxy extinction corrections based on colors. Templates for SN Ib/c LCs are presented. Our SNe have typical TBB of ~10 000 K at the peak and Rph of ~1015 cm. Analysis of the BLCs of SNe Ib and Ic gives typical ejecta masses Mej≈ 3.6-5.7 M⊙, energies EK≈ 1.5-1.7×1051 erg, and M(56Ni) ≈ 0.3 M⊙. Higher values for EK and M(56Ni) are estimated for SNe Ic-BL (Mej≈ 5.4 M⊙, EK≈ 10.7×1051 erg, M(56Ni) ≈ 1.1 M⊙). For the majority of SNe Ic and Ic-BL, we can put strong limits (<2-4 days) on the duration of the expected early-time plateau. Less stringent limits can be placed on the duration of the plateau for the sample of SNe Ib. In the

  17. A SURVEY OF z {approx} 6 QUASARS IN THE SLOAN DIGITAL SKY SURVEY DEEP STRIPE. II. DISCOVERY OF SIX QUASARS AT z {sub AB}>21

    SciTech Connect

    Jiang Linhua; Fan Xiaohui; Bian Fuyan; Annis, James; Lin Huan; Chiu, Kuenley; Jester, Sebastian; Lupton, Robert H.; Strauss, Michael A.; Richards, Gordon T.; Malanushenko, Viktor; Malanushenko, Elena; Schneider, Donald P.

    2009-07-15

    We present the discovery of six new quasars at z {approx} 6 selected from the Sloan Digital Sky Survey (SDSS) southern survey, a deep imaging survey obtained by repeatedly scanning a stripe along the celestial equator. The six quasars are about 2 mag fainter than the luminous z {approx} 6 quasars found in the SDSS main survey and 1 mag fainter than the quasars reported in Paper I. Four of them comprise a complete flux-limited sample at 21 < z {sub AB} < 21.8 over an effective area of 195 deg{sup 2}. The other two quasars are fainter than z {sub AB} = 22 and are not part of the complete sample. The quasar luminosity function at z {approx} 6 is well described as a single power law {phi}(L {sub 1450}) {proportional_to} L {sup {beta}} {sub 1450} over the luminosity range -28 < M {sub 1450} < -25. The best-fitting slope {beta} varies from -2.6 to -3.1, depending on the quasar samples used, with a statistical error of 0.3-0.4. About 40% of the quasars discovered in the SDSS southern survey have very narrow Ly{alpha} emission lines, which may indicate small black hole masses and high Eddington luminosity ratios, and therefore short black hole growth timescales for these faint quasars at early epochs.

  18. He II emitters in the VIMOS VLT Deep Survey: Population III star formation or peculiar stellar populations in galaxies at 2 < z < 4.6?

    NASA Astrophysics Data System (ADS)

    Cassata, P.; Le Fèvre, O.; Charlot, S.; Contini, T.; Cucciati, O.; Garilli, B.; Zamorani, G.; Adami, C.; Bardelli, S.; Le Brun, V.; Lemaux, B.; Maccagni, D.; Pollo, A.; Pozzetti, L.; Tresse, L.; Vergani, D.; Zanichelli, A.; Zucca, E.

    2013-08-01

    Aims: The aim of this work is to identify He II emitters at 2 < z < 4.6 and to constrain the source of the hard ionizing continuum that powers the He II emission. Methods: We assembled a sample of 277 galaxies with a highly reliable spectroscopic redshift at 2 < z < 4.6 from the VIMOS-VLT Deep Survey (VVDS) Deep and Ultra-Deep data, and we identified 39 He II λ1640 emitters. We studied their spectral properties, measuring the fluxes, equivalent widths (EW), and full width at half maximum (FWHM) for most relevant lines, including He II λ1640, Lyα line, Si II λ1527, and C IV λ1549. Results: About 10% of galaxies at z ~ 3 and iAB ≤ 24.75 show He II in emission, with rest frame equivalent widths EW0 ~ 1-7 Å, equally distributed between galaxies with Lyα in emission or in absorption. We find 11 (3.9% of the global population) reliable He II emitters with unresolved He II lines (FWHM0 < 1200 km s-1), 13 (4.6% of the global population) reliable emitters with broad He II emission (FWHM0 > 1200 km s-1), 3 active galactic nuclei (AGN), and an additional 12 possible He II emitters. The properties of the individual broad emitters are in agreement with expectations from a Wolf-Rayet (W-R) model. Instead, the properties of the narrow emitters are not compatible with this model, nor with predictions of gravitational cooling radiation produced by gas accretion, unless this is severely underestimated by current models by more than two orders of magnitude. Rather, we find that the EW of the narrow He II line emitters are in agreement with expectations for a Population III (PopIII) star formation, if the episode of star formation is continuous, and we calculate that a PopIII star formation rate (SFR) of 0.1-10 M⊙ yr-1 alone is enough to sustain the observed He II flux. Conclusions: We conclude that narrow He II emitters are powered either by the ionizing flux from a stellar population rare at z ~ 0 but much more common at z ~ 3, or by PopIII star formation. As proposed by

  19. A 158 μm [C II] Line Survey of Galaxies at z ~ 1-2: An Indicator of Star Formation in the Early Universe

    NASA Astrophysics Data System (ADS)

    Stacey, G. J.; Hailey-Dunsheath, S.; Ferkinhoff, C.; Nikola, T.; Parshley, S. C.; Benford, D. J.; Staguhn, J. G.; Fiolet, N.

    2010-12-01

    We have detected the 158 μm [C II] line from 12 galaxies at z ~ 1-2. This is the first survey of this important star formation tracer at redshifts covering the epoch of maximum star formation in the universe and quadruples the number of reported high-z [C II] detections. The line is very luminous, between <0.024% and 0.65% of the far-infrared (FIR) continuum luminosity of our sources, and arises from photodissociation regions on molecular cloud surfaces. An exception is PKS 0215+015, where half of the [C II] emission could arise from X-ray-dominated regions near the central active galactic nucleus (AGN). The L [C II]/L FIR ratio in our star formation-dominated systems is ~8 times larger than that of our AGN-dominated systems. Therefore this ratio selects for star formation-dominated systems. Furthermore, the L [C II]/L FIR and L [C II]/L (CO(1-0)) ratios in our star-forming galaxies and nearby starburst galaxies are the same, so that luminous star-forming galaxies at earlier epochs (z ~ 1-2) appear to be scaled-up versions of local starbursts entailing kiloparsec-scale starbursts. Most of the FIR and [C II] radiation from our AGN-dominated sample (excepting PKS 0215+015) also arises from kiloparsec-scale star formation, but with far-UV radiation fields ~8 times more intense than in our star formation-dominated sample. We speculate that the onset of AGN activity stimulates large-scale star formation activity within AGN-dominated systems. This idea is supported by the relatively strong [O III] line emission, indicating very young stars, that was recently observed in high-z composite AGN/starburst systems. Our results confirm the utility of the [C II] line, and in particular, the L [C II]/L (FIR) and L [C II]/L CO(1-0) ratios as tracers of star formation in galaxies at high redshifts.

  20. A 158 {mu}m [C II] LINE SURVEY OF GALAXIES AT z {approx} 1-2: AN INDICATOR OF STAR FORMATION IN THE EARLY UNIVERSE

    SciTech Connect

    Stacey, G. J.; Hailey-Dunsheath, S.; Ferkinhoff, C.; Nikola, T.; Parshley, S. C.; Benford, D. J.; Staguhn, J. G.; Fiolet, N. E-mail: steve@mpe.mpg.d

    2010-12-01

    We have detected the 158 {mu}m [C II] line from 12 galaxies at z {approx} 1-2. This is the first survey of this important star formation tracer at redshifts covering the epoch of maximum star formation in the universe and quadruples the number of reported high-z [C II] detections. The line is very luminous, between <0.024% and 0.65% of the far-infrared (FIR) continuum luminosity of our sources, and arises from photodissociation regions on molecular cloud surfaces. An exception is PKS 0215+015, where half of the [C II] emission could arise from X-ray-dominated regions near the central active galactic nucleus (AGN). The L{sub [C{sub II}]}/L{sub FIR} ratio in our star formation-dominated systems is {approx}8 times larger than that of our AGN-dominated systems. Therefore this ratio selects for star formation-dominated systems. Furthermore, the L{sub [C{sub II}]}/L{sub FIR} and L{sub [C{sub II}]}/L{sub (CO(1-0))} ratios in our star-forming galaxies and nearby starburst galaxies are the same, so that luminous star-forming galaxies at earlier epochs (z {approx} 1-2) appear to be scaled-up versions of local starbursts entailing kiloparsec-scale starbursts. Most of the FIR and [C II] radiation from our AGN-dominated sample (excepting PKS 0215+015) also arises from kiloparsec-scale star formation, but with far-UV radiation fields {approx}8 times more intense than in our star formation-dominated sample. We speculate that the onset of AGN activity stimulates large-scale star formation activity within AGN-dominated systems. This idea is supported by the relatively strong [O III] line emission, indicating very young stars, that was recently observed in high-z composite AGN/starburst systems. Our results confirm the utility of the [C II] line, and in particular, the L{sub [C{sub II}]}/L{sub (FIR)} and L{sub [C{sub II}]}/L{sub CO(1-0)} ratios as tracers of star formation in galaxies at high redshifts.

  1. Survey II of Public and Leadership Attitudes Toward Nuclear Power Development in the United States. Study No. 2628.

    ERIC Educational Resources Information Center

    Harris (Louis) and Associates, Inc., New York, NY.

    This publication details a national survey done by Louis Harris and Associates, similar to one done in 1975, to assess attitudes toward nuclear power in the United States. The survey consisted of three parts. The first part was in-person, door-to-door interviews with 1,597 randomly selected households nationwide. The second part was 309…

  2. A Survey of College Reading Programs in New York State, Part II: Diagnosis, Placement and Program Components.

    ERIC Educational Resources Information Center

    Malinowski, Patricia A.

    During spring 1988, an initial survey was conducted among two- and four-year colleges in New York State to identify the primary reading test used for diagnosis and placement. In order to address several questions raised by the study, a follow-up survey of participating two-year colleges was conducted during fall 1989. Of the 28 two-year colleges…

  3. Survey II of Public and Leadership Attitudes Toward Nuclear Power Development in the United States. Study No. 2628.

    ERIC Educational Resources Information Center

    Harris (Louis) and Associates, Inc., New York, NY.

    This publication details a national survey done by Louis Harris and Associates, similar to one done in 1975, to assess attitudes toward nuclear power in the United States. The survey consisted of three parts. The first part was in-person, door-to-door interviews with 1,597 randomly selected households nationwide. The second part was 309…

  4. Survey Instrument Validity Part II: Validation of a Survey Instrument Examining Athletic Trainers' Knowledge and Practice Beliefs Regarding Exertional Heat Stroke

    ERIC Educational Resources Information Center

    Burton, Laura J.; Mazerolle, Stephanie M.

    2011-01-01

    Objective: The purpose of this article is to discuss the process of developing and validating an instrument to investigate an athletic trainer's attitudes and behaviors regarding the recognition and treatment of exertional heat stroke. Background: Following up from our initial paper, which discussed the process of survey instrument design and…

  5. Survey Instrument Validity Part II: Validation of a Survey Instrument Examining Athletic Trainers' Knowledge and Practice Beliefs Regarding Exertional Heat Stroke

    ERIC Educational Resources Information Center

    Burton, Laura J.; Mazerolle, Stephanie M.

    2011-01-01

    Objective: The purpose of this article is to discuss the process of developing and validating an instrument to investigate an athletic trainer's attitudes and behaviors regarding the recognition and treatment of exertional heat stroke. Background: Following up from our initial paper, which discussed the process of survey instrument design and…

  6. The Exoplanet Mass-Ratio Function From the MOA-II Survey: Discovery of a Break and Likely Peak at a Neptune Mass

    NASA Technical Reports Server (NTRS)

    Suzuki, D.; Bennett, D. P.; Sumi, T.; Bond, I. A.; Rogers, L. A.; Abe, F.; Asakura, Y.; Bhattacharya, A.; Donachie, M.; Freeman, M.; hide

    2016-01-01

    We report the results of the statistical analysis of planetary signals discovered in MOA-II microlensing survey alert system events from 2007 to 2012. We determine the survey sensitivity as a function of planet star mass ratio, q, and projected planet star separation, s, in Einstein radius units. We find that the mass-ratio function is not a single power law, but has a change in slope at q approx.10(exp -4), corresponding to approx. 20 Stellar Mass for the median host-star mass of approx. 0.6 M. We find significant planetary signals in 23 of the 1474 alert events that are well-characterized by the MOA-II survey data alone. Data from other groups are used only to characterize planetary signals that have been identified in the MOA data alone. The distribution of mass ratios and separations of the planets found in our sample are well fit by a broken power-law model. We also combine this analysis with the previous analyses of Gould et al. and Cassan et al., bringing the total sample to 30 planets. The unbroken power-law model is disfavored with a p-value of 0.0022, which corresponds to a Bayes factor of 27 favoring the broken power-law model. These results imply that cold Neptunes are likely to be the most common type of planets beyond the snow line.

  7. POISSON project. II. A multi-wavelength spectroscopic and photometric survey of young protostars in L 1641

    NASA Astrophysics Data System (ADS)

    Caratti o Garatti, A.; Garcia Lopez, R.; Antoniucci, S.; Nisini, B.; Giannini, T.; Eislöffel, J.; Ray, T. P.; Lorenzetti, D.; Cabrit, S.

    2012-02-01

    Context. Characterising stellar and circumstellar properties of embedded young stellar objects (YSOs) is mandatory for understanding the early stages of the stellar evolution. This task requires the combination of both spectroscopy and photometry, covering the widest possible wavelength range, to disentangle the various protostellar components and activities. Aims: As part of the POISSON project (Protostellar Optical-Infrared Spectral Survey On NTT), we present a multi-wavelength spectroscopic and photometric investigation of embedded YSOs in L 1641, aimed to derive the stellar parameters and evolutionary stages and to infer their accretion properties. Methods: Our multi-wavelength database includes low-resolution optical-IR spectra from the NTT and Spitzer (0.6-40 μm) and photometric data covering a spectral range from 0.4 to 1100 μm, which allow us to construct the YSOs spectral energy distributions (SEDs) and to infer the main stellar parameters (visual extinction, spectral type, accretion, stellar, bolometric luminosity, mass accretion, and ejection rates). Results: The NTT optical-NIR spectra are rich in emission lines, which are mostly associated with YSO accretion, ejection, and chromospheric activities. A few emission lines, prominent ice (H2O and CO2), and amorphous silicate absorption features have also been detected in the Spitzer spectra. The SED analysis allows us to group our 27 YSOs into nine Class I, eleven Flat, and seven Class II objects. However, on the basis of the derived stellar properties, only six Class I YSOs have an age of ~105 yr, while the others are older (5 × 105-106 yr), and, among the Flat sources, three out of eleven are more evolved objects (5 × 106-107 yr), indicating that geometrical effects can significantly modify the SED shapes. Inferred mass accretion rates (Ṁacc) show a wide range of values (3.6 × 10-9 to 1.2 × 10-5 M⊙ yr-1), which reflects the age spread observed in our sample well. Average values of mass

  8. The Survey of Lines in M31 (SLIM): The Drivers of the [C ii]/TIR Variation

    NASA Astrophysics Data System (ADS)

    Kapala, Maria J.; Groves, Brent; Sandstrom, Karin; Jarrett, Thomas; da Cunha, Elisabete; Croxall, Kevin; Dalcanton, Julianne; Draine, Bruce; Glover, Simon; Schinnerer, Eva

    2017-06-01

    The ratio of the [C ii] 158 μ {{m}} emission line over the total infrared emission (TIR) is often used as a proxy for the photoelectric (PE) heating efficiency ({ε }{PE}) of the far-ultraviolet (FUV) photons absorbed by dust in the interstellar medium. In the nearby galaxy M31, we measure a strong radial variation of [C ii]/TIR that we rule out as being due to an intrinsic variation in {ε }{PE}. [C ii]/TIR fails as a proxy for {ε }{PE}, because the TIR measures all dust heating, not just the contribution from FUV photons capable of ejecting electrons from dust grains. Using extensive multi-wavelength coverage from the FUV to far-infrared, we infer the attenuated FUV emission ({{UV}}{att}), and the total attenuated flux ({{TOT}}{att}). We find [C ii]/TIR to be strongly correlated with {{UV}}{att}/{{TOT}}{att}, indicating that, in M31 at least, one of the dominant drivers for [C ii]/TIR variation is the relative hardness of the absorbed stellar radiation field. We define {ε }{PE}{UV}, [C ii]/{{UV}}{att} which should be more closely related to the actual PE efficiency, which we find to be essentially constant (1.85+/- 0.8 % ) in all explored fields in M31. This suggests that part of the observed variation of [C ii]/TIR in other galaxies is likely due to a change in the relative hardness of the absorbed stellar radiation field, caused by a combination of variations in the stellar population, dust opacity, and galaxy metallicity, though PE efficiency may also vary across a wider range of environments.

  9. Approach to the non-operative management of patients with stage II non-small cell lung cancer (NSCLC): A survey of Canadian medical and radiation oncologists.

    PubMed

    Dudani, Shaan; Leighl, Natasha B; Ho, Cheryl; Pantarotto, Jason R; Zhu, Xiaofu; Zhang, Tinghua; Wheatley-Price, Paul

    2016-04-01

    Standard management of stage II non-small cell lung cancer (NSCLC) is surgery, often followed by adjuvant chemotherapy. However, some patients do not undergo surgery for various reasons. The optimal non-surgical management of stage II NSCLC is undefined. We surveyed Canadian oncologists to understand current practices. Canadian oncologists specializing in the management of lung cancer were invited by email to complete an anonymous, online survey developed by the research team. Physician demographics were recorded. Physicians were asked to comment on their practice and make treatment choices in eight clinical scenarios of inoperable stage II NSCLC. Responses were received from 81/194 physicians (42% response rate), 57% medical and 42% radiation oncologists. Most physicians (90%) had a practice with at least 25% lung cancer patients and 85% were based at an academic institution. Across eight clinical patient scenarios, radical therapy was selected 79-98% of the time. Radical radiotherapy alone and concurrent chemoradiotherapy were the preferred options for these patients, while sequential chemoradiation was less favoured. Nodal status (N0 vs N1) did not influence choice of therapy (p 0.31), but the reason for patient inoperability did (p<0.0001). There was no significant difference in choice of therapy when comparing responses between medical vs radiation oncologists, academic vs community physicians, and physicians with high vs low proportion of lung cancer patients. Most lung cancer physicians manage inoperable stage II NSCLC patients with curative intent, but consensus on how to optimally employ radiotherapy and/or chemotherapy is lacking. Future prospective, randomized trials are warranted. Copyright © 2016 Elsevier Ireland Ltd. All rights reserved.

  10. Phase II. Environmental baseline survey of McCormick Ranch, Kirtland Air Force Base, New Mexico. Part 2. Final report, October 1993-January 1995

    SciTech Connect

    Hagaraty, G.; Johnson, J.; Middlebrooks, P.

    1996-01-31

    The Phase II EBS results document the extent of environmental contamination believed to be present on McCormick Ranch. Explosive test areas having the greatest potential for containing soil contaminants were identified using several geophysical survey methods: EM 31 terrain conductivity meter, magnetometer/gradiometer, and ground penetrating radar. From the geophysical surveys, five areas were selected to conduct further environmental analysis. A total of 310 soil samples were collected from the five areas and 13 specific high explosive test sites. The samples were screened for semi-volatile organic compounds, PETN, TNT, TNT-degradation products, nitrates and radioactivity. Laboratory analyses were performed and no explosives or degradation products were identified. Semi-volatile organic compounds were found in 2 samples, manganese was detected in 3 samples, nitrates were discovered below soil action levels, and radiation levels were below background. Consequently, it is unlikely that significant contamination exists.

  11. Phase II. Environmental baseline survey of McCormick Ranch, Kirtland Air Force Base, New Mexico. Part 1. Final report, October 1993-January 1995

    SciTech Connect

    Hagaraty, G.; Johnson, J.; Middlebrooks, P.

    1996-01-31

    The Phase II EBS results document the extent of environmental contamination believed to be present on McCormick Ranch. Explosive test areas having the greatest potential for containing soil contaminants were identified using several geophysical survey methods: EM 31 terrain conductivity meter, magnetometer/gradiometer, and ground penetrating radar. From the geophysical surveys, five areas were selected to conduct further environmental analysis. A total of 310 soil samples were collected from the and 13 specific high explosive test sites. The samples were screened for semi-volatile organic PETN, TNT, TNT-degradation products, nitrates and radioactivity. Laboratory analyses were and no explosives or degradation products were identified. Semi-volatile organic compounds were in 2 samples, manganese was detected in 3 samples, nitrates were discovered below soil action levels, and radiation levels were below background. Consequently, it is unlikely that significant contamination exists.

  12. Phase II. Environmental baseline survey of McCormick Ranch, Kirtland Air Force Base, New Mexico. Part 3. Final report, October 1993-January 1995

    SciTech Connect

    Hagaraty, G.; Johnson, J.; Middlebrooks, P.

    1996-01-31

    The Phase II EBS results document the extent of environmental contamination believed to be present on McCormick Ranch. Explosive test areas having the greatest potential for containing soil contaminants were identified using several geophysical survey methods: EM 31 terrain conductivity meter, magnetometer/gradiometer, and ground penetrating radar. From the geophysical surveys, five areas were selected to conduct further environmental analysis. A total of 310 soil samples were collected from the five areas and 13 specific high explosive test sites. The samples were screened for semi-volatile organic compounds, PETN, TNT, TNT-degradation products, nitrates and radioactivity. Laboratory analyses were and no explosives or degradation products were identified. Semi-volatile organic compounds were in 2 samples, manganese was detected in 3 samples, nitrates were discovered below soil action levels, and radiation levels were below background. Consequently, it is unlikely that significant contamination exists.

  13. Phase II. Environmental baseline survey of McCormick Ranch, Kirtland Air Force Base, New Mexico. Part 5. Final report, October 1993-January 1995

    SciTech Connect

    Hagaraty, G.; Johnson, J.; Middlebrooks, P.

    1996-01-31

    The Phase II EBS results document the extent of environmental contamination believed to be present on McCormick Ranch. Explosive test areas having the greatest potential for containing soil contaminants were identified using several geophysical survey methods: EM 31 terrain conductivity meter, magnetometer/gradiometer, and ground penetrating radar. From the geophysical surveys, five areas were selected to conduct further environmental analysis. A total of 310 soil samples were collected from the areas and 13 specific high explosive test sites. The samples were screened for semi-volatile organic compounds, PETN, TNT, TNT-degradation products, nitrates and radioactivity. Laboratory analyses were performed and no explosives or degradation products were identified. Semi-volatile organic compounds were in 2 samples, manganese was detected in 3 samples, nitrates were discovered below soil action levels and radiation levels were below background. Consequently, it is unlikely that significant contamination exists.

  14. Phase II. Environmental baseline survey of McCormick Ranch, Kirtland Air Force Base, New Mexico. Part 4. Final report, October 1993-January 1995

    SciTech Connect

    Hagaraty, G.; Johnson, J.; Middlebrooks, P.

    1996-01-31

    The Phase II EBS results document the extent of environmental contamination believed to be present on McCormick Ranch. Explosive test areas having the greatest potential for containing soil contaminants were identified using several geophysical survey methods: EM 31 terrain conductivity meter, magnetometer/gradiometer, and ground penetrating radar. From the geophysical surveys, five areas selected to conduct further environmental analysis. A total of 310 soil samples were collected from the five areas and 13 specific high explosive test sites. The samples were screened for semi-volatile organic compounds, PETN, TNT, TNT-degradation products, nitrates and radioactivity. Laboratory analyses were performed and no explosives or degradation products were identified. Semi-volatile organic compounds were in 2 samples, manganese was detected in 3 samples, nitrates were discovered below soil action levels, and radiation levels were below background. Consequently, it is unlikely that significant contamination exists.

  15. Relationship between radiological knee osteoarthritis and biochemical markers of cartilage and bone degradation (urine CTX-II and NTX-I): the Matsudai Knee Osteoarthritis Survey.

    PubMed

    Tanishi, Nobuchika; Yamagiwa, Hiroshi; Hayami, Tadashi; Mera, Hisashi; Koga, Yoshio; Omori, Go; Endo, Naoto

    2009-01-01

    Biochemical markers of cartilage and bone degradation are becoming increasingly important in the evaluation of knee osteoarthritis (OA). To clarify the correlation between radiological knee OA and urine CTX-II (C-terminal crosslinking telopeptide of collagen type II) or urine NTX-I (N-terminal crosslinking telopeptide of type I collagen), we conducted a cross-sectional study in the cohorts of the epidemiological knee survey at the Matsudai district in Niigata Prefecture, Japan. Urine specimens were collected from 296 subjects, and CTX-II and NTX-I were measured using ELISA. Standing knee AP X-rays were obtained and graded according to the Kellgren-Lawrence classification. The subjects were then divided by gender, age (40- to 59-year-old group and 60- to 79-year-old group), and the X-ray grade (Grade 0, 1, Grade 2, and Grade 3, 4). In non-OA (Grade 0, 1) subjects, the 60- to 79-year-old group had significantly higher CTX-II values than the younger group only in females. The subjects of both genders aged over 60 years of age with OA Grade 3, 4 had significantly higher CTX-II values than the Grade 0, 1 group or the Grade 2 group. For NTX-I, there were no significant differences between each OA grade although the Grade 3, 4 group females from 60 to 79 years of age had higher values than the Grade 2 group. In addition, in the 60- to 79-year-old subjects of both genders, a positive correlation was observed between the urine CTX-II and urine NTX-I. For the subjects ranging from 60 to 79 years of age in both genders, the urine CTX-II values indicate the progression of OA. In addition, the weak but positive correlation between urine CTX-II and urine NTX-I in the subjects ranging from 60 to 79 years of age in both genders suggests that bone resorption and cartilage degradation appear to develop in parallel.

  16. The LAMOST survey of background quasars in the vicinity of the Andromeda and Triangulum galaxies. II. Results from the commissioning observations and the pilot surveys

    SciTech Connect

    Huo, Zhi-Ying; Bai, Zhong-Rui; Chen, Jian-Jun; Chen, Xiao-Yan; Du, Bing; Jia, Lei; Lei, Ya-Juan; Liu, Xiao-Wei; Yuan, Hai-Bo; Xiang, Mao-Sheng; Huang, Yang; Zhang, Hui-Hua; Yan, Lin; Chu, Jia-Ru; Chu, Yao-Quan; Hu, Hong-Zhuan; Cui, Xiang-Qun; Hou, Yong-Hui; Hu, Zhong-Wen; Jiang, Fang-Hua; and others

    2013-06-01

    We present new quasars discovered in the vicinity of the Andromeda and Triangulum galaxies with the Large Sky Area Multi-Object Fiber Spectroscopic Telescope, also named the Guoshoujing Telescope, during the 2010 and 2011 observational seasons. Quasar candidates are selected based on the available Sloan Digital Sky Survey, Kitt Peak National Observatory 4 m telescope, Xuyi Schmidt Telescope Photometric Survey optical, and Wide-field Infrared Survey Explorer near-infrared photometric data. We present 509 new quasars discovered in a stripe of ∼135 deg{sup 2} from M31 to M33 along the Giant Stellar Stream in the 2011 pilot survey data sets, and also 17 new quasars discovered in an area of ∼100 deg{sup 2} that covers the central region and the southeastern halo of M31 in the 2010 commissioning data sets. These 526 new quasars have i magnitudes ranging from 15.5 to 20.0, redshifts from 0.1 to 3.2. They represent a significant increase of the number of identified quasars in the vicinity of M31 and M33. There are now 26, 62, and 139 known quasars in this region of the sky with i magnitudes brighter than 17.0, 17.5, and 18.0, respectively, of which 5, 20, and 75 are newly discovered. These bright quasars provide an invaluable collection with which to probe the kinematics and chemistry of the interstellar/intergalactic medium in the Local Group of galaxies. A total of 93 quasars are now known with locations within 2.°5 of M31, of which 73 are newly discovered. Tens of quasars are now known to be located behind the Giant Stellar Stream, and hundreds are behind the extended halo and its associated substructures of M31. The much enlarged sample of known quasars in the vicinity of M31 and M33 can potentially be utilized to construct a perfect astrometric reference frame to measure the minute proper motions (PMs) of M31 and M33, along with the PMs of substructures associated with the Local Group of galaxies. Those PMs are some of the most fundamental properties of the Local

  17. Adding the s-Process Element Cerium to the APOGEE Survey: Identification and Characterization of Ce ii Lines in the H-band Spectral Window

    NASA Astrophysics Data System (ADS)

    Cunha, Katia; Smith, Verne V.; Hasselquist, Sten; Souto, Diogo; Shetrone, Matthew D.; Allende Prieto, Carlos; Bizyaev, Dmitry; Frinchaboy, Peter; García-Hernández, D. Anibal; Holtzman, Jon; Johnson, Jennifer A.; Jőnsson, Henrik; Majewski, Steven R.; Mészáros, Szabolcs; Nidever, David; Pinsonneault, Mark; Schiavon, Ricardo P.; Sobeck, Jennifer; Skrutskie, Michael F.; Zamora, Olga; Zasowski, Gail; Fernández-Trincado, J. G.

    2017-08-01

    Nine Ce ii lines have been identified and characterized within the spectral window observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey (between λ1.51 and 1.69 μm). At solar metallicities, cerium is an element that is produced predominantly as a result of the slow capture of neutrons (the s-process) during asymptotic giant branch stellar evolution. The Ce ii lines were identified using a combination of a high-resolution (R=λ /δ λ ={{100,000}}) Fourier Transform Spectrometer (FTS) spectrum of α Boo and an APOGEE spectrum (R = 22,400) of a metal-poor, but s-process enriched, red giant (2M16011638-1201525). Laboratory oscillator strengths are not available for these lines. Astrophysical gf-values were derived using α Boo as a standard star, with the absolute cerium abundance in α Boo set by using optical Ce ii lines that have precise published laboratory gf-values. The near-infrared Ce ii lines identified here are also analyzed, as consistency checks, in a small number of bright red giants using archival FTS spectra, as well as a small sample of APOGEE red giants, including two members of the open cluster NGC 6819, two field stars, and seven metal-poor N- and Al-rich stars. The conclusion is that this set of Ce ii lines can be detected and analyzed in a large fraction of the APOGEE red giant sample and will be useful for probing chemical evolution of the s-process products in various populations of the Milky Way.

  18. The Spitzer c2d Survey of Large, Nearby, Interstellar Clouds. X. The Chamaeleon II Pre-Main-Sequence Population as Observed with IRAC and MIPS

    NASA Astrophysics Data System (ADS)

    Alcalá, Juan M.; Spezzi, Loredana; Chapman, Nicholas; Evans, Neal J., II; Huard, Tracy L.; Jørgensen, Jes K.; Merín, Bruno; Stapelfeldt, Karl R.; Covino, Elvira; Frasca, Antonio; Gandolfi, Davide; Oliveira, Isa

    2008-03-01

    We discuss the results from the combined IRAC and MIPS c2d Spitzer Legacy survey observations and complementary optical and NIR data of the Chamaeleon II (Cha II) dark cloud. We perform a census of the young population in an area of ~1.75 deg2 and study the spatial distribution and properties of the cloud members and candidate pre-main-sequence (PMS) objects and their circumstellar matter. Our census is complete down to the substellar regime (M ≈ 0.03 M⊙). From the analysis of the volume density of the PMS objects and candidates we find two groups of objects with volume densities higher than 25 M⊙ pc -3 and 5-10 members each. A multiplicity fraction of about 13% +/- 3% is observed for objects with separations 0.8'' < θ < 6.0'' (142-1065 AU). No evidence for variability between the two epochs of the c2d IRAC data set, Δ t ~ 6 hr, is detected. We estimate a star formation efficiency of 1%-4%, consistent with the estimates for Taurus and Lupus, but lower than for Cha I. This might mean that different star formation activities in the Chamaeleon clouds reflect a different history of star formation. We also find that Cha II is turning some 6-7 M⊙ into stars every Myr, which is low in comparison with the star formation rate in other c2d clouds. The disk fraction of 70%-80% that we estimate in Cha II is much higher than in other star-forming regions and indicates that the population in this cloud is dominated by objects with active accretion. Finally, the Cha II outflows are discussed; a new Herbig-Haro outflow, HH 939, driven by the classical T Tauri star Sz 50, has been discovered.

  19. The Sloan Digital Sky Survey Reverberation Mapping Project: First Broad-line Hβ and Mg ii Lags at z ≳ 0.3 from Six-month Spectroscopy

    NASA Astrophysics Data System (ADS)

    Shen, Yue; Horne, Keith; Grier, C. J.; Peterson, Bradley M.; Denney, Kelly D.; Trump, Jonathan R.; Sun, Mouyuan; Brandt, W. N.; Kochanek, Christopher S.; Dawson, Kyle S.; Green, Paul J.; Greene, Jenny E.; Hall, Patrick B.; Ho, Luis C.; Jiang, Linhua; Kinemuchi, Karen; McGreer, Ian D.; Petitjean, Patrick; Richards, Gordon T.; Schneider, Donald P.; Strauss, Michael A.; Tao, Charling; Wood-Vasey, W. M.; Zu, Ying; Pan, Kaike; Bizyaev, Dmitry; Ge, Jian; Oravetz, Daniel; Simmons, Audrey

    2016-02-01

    Reverberation mapping (RM) measurements of broad-line region (BLR) lags in z\\gt 0.3 quasars are important for directly measuring black hole masses in these distant objects, but so far there have been limited attempts and success given the practical difficulties of RM in this regime. Here we report preliminary results of 15 BLR lag measurements from the Sloan Digital Sky Survey Reverberation Mapping (SDSS-RM) project, a dedicated RM program with multi-object spectroscopy designed for RM over a wide redshift range. The lags are based on the 2014 spectroscopic light curves alone (32 epochs over six months) and focus on the Hβ and Mg ii broad lines in the 100 lowest-redshift (z\\lt 0.8) quasars included in SDSS-RM; they represent a small subset of the lags that SDSS-RM (including 849 quasars to z˜ 4.5) is expected to deliver. The reported preliminary lag measurements are for intermediate-luminosity quasars at 0.3≲ z\\lt 0.8, including nine Hβ lags and six Mg ii lags, for the first time extending RM results to this redshift-luminosity regime and providing direct quasar black hole mass estimates over approximately half of cosmic time. The Mg ii lags also increase the number of known Mg ii lags by several fold and start to explore the utility of Mg ii for RM at high redshift. The location of these new lags at higher redshifts on the observed BLR size-luminosity relationship is statistically consistent with previous Hβ results at z\\lt 0.3. However, an independent constraint on the relationship slope at z\\gt 0.3 is not yet possible owing to the limitations in our current sample. Our results demonstrate the general feasibility and potential of multi-object RM for z\\gt 0.3 quasars.

  20. On the Nature of the FBS Blue Stellar Objects and the Completeness of the Bright Quasar Survey. Ii

    NASA Astrophysics Data System (ADS)

    Mickaelian, A.; Goncalves, A.; Veron-Cetty, M.; Veron, P.

    In Paper I (Mickaelian et al. 1999), we compared the surface density of QSOs in the Bright Quasar Survey (BQS) and in the First Byurakan Survey (FBS) and concluded that the completeness of the BQS is of the order of 70% rather than 30-50% as suggested by several authors. A number of new observations recently became available, allowing a re-evaluation of this completeness. We now obtain a surface density of QSOs brighter than B = 16.16 in a subarea of the FBS covering ~2250 deg^2, equal to 0.012 deg^-2 (26 QSOs), implying a completeness of 53+/-10%.

  1. On the Nature of the FBS Blue Stellar Objects and the Completeness of the Bright Quasar Survey. II

    NASA Astrophysics Data System (ADS)

    Mickaelian, A. M.; Gonçalves, A. C.; Véron-Cetty, M. P.; Véron, P.

    2001-01-01

    In Paper I we compared the surface density of QSOs in the Bright Quasar Survey (BQS) and in the First Byurakan Survey (FBS) and concluded that the completeness of the BQS is of the order of 70% rather than 30-50% as suggested by several authors. A number of new observations recently became available, allowing a reevaluation of this completeness. We now obtain a surface density of QSOs brighter than B = 16.16 in a subarea of the FBS covering 2250 deg2, equal to 0.012 deg-2 (26 QSOs), implying a completeness of 53 ± 10%.

  2. The StEllar Counterparts of COmpact high velocity clouds (SECCO) survey. II. Sensitivity of the survey and the atlas of synthetic dwarf galaxies

    NASA Astrophysics Data System (ADS)

    Beccari, G.; Bellazzini, M.; Battaglia, G.; Ibata, R.; Martin, N.; Testa, V.; Cignoni, M.; Correnti, M.

    2016-06-01

    The searching for StEllar Counterparts of COmpact high velocity clouds (SECCO) survey is devoted to the search for stellar counterparts within ultra compact high velocity clouds that are candidate low-mass, low-luminosity galaxies. We present the results of a set of simulations aimed at the quantitative estimate of the sensitivity of the survey as a function of the total luminosity, size, and distance of the stellar systems we are looking for. For all of our synthetic galaxies we assumed an exponential surface brightness profile and an old and metal-poor population. The synthetic galaxies are simulated both on the images and on the photometric catalogues, taking all the observational effects into account. In the fields where the available observational material is of top quality (≃36% of the SECCO fields), we detect synthetic galaxies as ≥5σ over-densities of resolved stars down to μV,h ≃ 30.0 mag/arcsec2, for D ≤ 1.5 Mpc, and down to μV,h ≃ 29.5 mag/arcsec2, for D ≤ 2.5 Mpc. In the field with the worst observational material of the whole survey, we detect synthetic galaxies with μV,h ≤ 28.8 mag/arcsec2 out to D ≤ 1.0 Mpc, and those with μV,h ≤ 27.5 mag/arcsec2 out to D ≤ 2.5 Mpc. Dwarf galaxies with MV = -10.0, with sizes in the range spanned by known dwarfs, are detected by visual inspection of the images up to D = 5 Mpc independent of the image quality. In the best quality images, dwarfs are partially resolved into stars up to D = 3.0 Mpc and completely unresolved at D = 5 Mpc. As an independent test of the sensitivity of our images to low surface brightness galaxies, we report on the detection of several dwarf spheroidal galaxies probably located in the Virgo cluster with MV ≲ -8.0 and μV,h ≲ 26.8 mag/arcsec2. The nature of the previously discovered SECCO 1 stellar system, also likely located in the Virgo cluster, is rediscussed in comparison with these dwarfs. While specific for the SECCO survey, our study may also provide general

  3. The GALEX Time Domain Survey. II. Wavelength-Dependent Variability of Active Galactic Nuclei in the Pan-STARRS1 Medium Deep Survey

    NASA Astrophysics Data System (ADS)

    Hung, T.; Gezari, S.; Jones, D. O.; Kirshner, R. P.; Chornock, R.; Berger, E.; Rest, A.; Huber, M.; Narayan, G.; Scolnic, D.; Waters, C.; Wainscoat, R.; Martin, D. C.; Forster, K.; Neill, J. D.

    2016-12-01

    We analyze the wavelength-dependent variability of a sample of spectroscopically confirmed active galactic nuclei selected from near-UV (NUV) variable sources in the GALEX Time Domain Survey that have a large amplitude of optical variability (difference-flux S/N > 3) in the Pan-STARRS1 Medium Deep Survey (PS1 MDS). By matching GALEX and PS1 epochs in five bands (NUV, g P1, r P1, i P1, z P1) in time, and taking their flux difference, we create co-temporal difference-flux spectral energy distributions ({{Δ }}f{SEDs}) using two chosen epochs for each of the 23 objects in our sample, on timescales of about a year. We confirm the “bluer-when-brighter” trend reported in previous studies, and measure a median spectral index of the {{Δ }}f{SEDs} of {α }λ = 2.1 that is consistent with an accretion disk spectrum. We further fit the {{Δ }}f{SEDs} of each source with a standard accretion disk model in which the accretion rate changes from one epoch to the other. In our sample, 17 out of 23 (∼74%) sources are described well by this variable accretion-rate disk model, with a median average characteristic disk temperature \\bar{T}* of 1.2× {10}5 K that is consistent with the temperatures expected, given the distribution of accretion rates and black hole masses inferred for the sample. Our analysis also shows that the variable accretion rate model is a better fit to the {{Δ }}f{SEDs} than a simple power law.

  4. Human Trafficking in the United States. Part II. Survey of U.S. Government Web Resources for Publications and Data

    ERIC Educational Resources Information Center

    Panigabutra-Roberts, Anchalee

    2012-01-01

    This second part of a two-part series is a survey of U.S. government web resources on human trafficking in the United States, particularly of the online publications and data included on agencies' websites. Overall, the goal is to provide an introduction, an overview, and a guide on this topic for library staff to use in their research and…

  5. Industry Wage Surveys: Banking and Life Insurance, December 1976. Part I--Banking. Part II--Life Insurance. Bulletin 1988.

    ERIC Educational Resources Information Center

    Barsky, Carl

    This report presents the results of a survey conducted by the Bureau of Labor Statistics to determine wages and related benefits in (1) the banking industry and (2) for employees in home offices and regional head offices of life insurance carriers. Part 1 discusses banking industry characteristics and presents data for tellers and selected…

  6. Survey of Public Participation in the Arts: Volume II. Changes in American's Participation, 1982-1985. Final Report.

    ERIC Educational Resources Information Center

    Robinson, John P.; And Others

    The primary purpose of this report was to compare data obtained from the 1982 and 1985 "Survey of Public Participation in the Arts." Comparisons of core questions and responses indicate that: (1) 1985 results are very close to those obtained in 1982; (2) there was a statistically significant decline in musical theater performance…

  7. DETECTING VARIABILITY IN MASSIVE ASTRONOMICAL TIME-SERIES DATA. II. VARIABLE CANDIDATES IN THE NORTHERN SKY VARIABILITY SURVEY

    SciTech Connect

    Shin, Min-Su; Yi, Hahn; Kim, Dae-Won; Chang, Seo-Won; Byun, Yong-Ik E-mail: yihahn@galaxy.yonsei.ac.kr E-mail: seowony@galaxy.yonsei.ac.kr

    2012-03-15

    We present variability analysis of data from the Northern Sky Variability Survey (NSVS). Using the clustering method, which defines variable candidates as outliers from large clusters, we cluster 16,189,040 light curves having data points at more than 15 epochs as variable and non-variable candidates in 638 NSVS fields. Variable candidates are selected depending on how strongly they are separated from the largest cluster and how rarely they are grouped together in eight-dimensional space spanned by variability indices. All NSVS light curves are also cross-correlated with IRAS, AKARI, Two Micron All Sky Survey, Sloan Digital Sky Survey (SDSS), and GALEX objects, as well as known objects in the SIMBAD database. The variability analysis and cross-correlation results are provided in a public online database, which can be used to select interesting objects for further investigation. Adopting conservative selection criteria for variable candidates, we find about 1.8 million light curves as possible variable candidates in the NSVS data, corresponding to about 10% of our entire NSVS sample. Multi-wavelength colors help us find specific types of variability among the variable candidates. Moreover, we also use morphological classification from other surveys such as SDSS to suppress spurious cases caused by blending objects or extended sources due to the low angular resolution of the NSVS.

  8. Biennial Survey of Education in the United States, 1928-1930. Bulletin, 1931, No. 20. Volume II. [Chapter IV - Index

    ERIC Educational Resources Information Center

    Office of Education, United States Department of the Interior, 1932

    1932-01-01

    This document contains the four concluding chapters and index of the Biennial Survey of Education, covering the years 1928-1930. Chapter 4, Statistics of universities, colleges, and professional schools, 1929-30, is made up of three parts: (1) Personnel, receipts, and property (Emery M. Foster and Frederick J. Kelley); (2) Expenditures (Henry G.…

  9. Industry Wage Surveys: Banking and Life Insurance, December 1976. Part I--Banking. Part II--Life Insurance. Bulletin 1988.

    ERIC Educational Resources Information Center

    Barsky, Carl

    This report presents the results of a survey conducted by the Bureau of Labor Statistics to determine wages and related benefits in (1) the banking industry and (2) for employees in home offices and regional head offices of life insurance carriers. Part 1 discusses banking industry characteristics and presents data for tellers and selected…

  10. Telecommunications Research in the United States and Selected Foreign Countries: A Preliminary Survey. Volume II, Individual Contributions.

    ERIC Educational Resources Information Center

    National Academy of Engineering, Washington, DC. Committee on Telecommunications.

    At the request of the National Science Foundation, the Panel on Telecommunications Research of the Committee on Telecommunications of the National Academy of Engineering has made a preliminary survey of the status and trends of telecommunications research in the United States and selected foreign countries. The status and trends were identified by…

  11. Survey of Land-Grant Colleges and Universities. Bulletin, 1930, No. 9. Volume II. [Part VII - Index

    ERIC Educational Resources Information Center

    Office of Education, United States Department of the Interior, 1930

    1930-01-01

    The attached document covers the concluding sections of the second volume of the Survey of Land-Grant Colleges and Universities: Part VII through the index. Part VII, Extension services, is divided into the following sections: (1) Introduction; (2) Position and objectives of Smith-Lever cooperative extension; (3) Administrative organization of…

  12. National Survey of American Attitudes on Substance Abuse II: Teens and Their Parents Conducted by Luntz Research Companies.

    ERIC Educational Resources Information Center

    Columbia Univ., New York, NY. National Center on Addiction and Substance Abuse.

    Illegal drug use by adolescents is on the rise. This alarming trend was quantified in this national survey of the attitudes of teens and their parents (1,200 teens and 1,166 parents, including 819 sets of teens and parents from the same households) towards cigarettes, alcohol, inhalants, marijuana, LSD, cocaine, heroin, and other illegal drugs.…

  13. Telecommunications Research in the United States and Selected Foreign Countries: A Preliminary Survey. Volume II, Individual Contributions.

    ERIC Educational Resources Information Center

    National Academy of Engineering, Washington, DC. Committee on Telecommunications.

    At the request of the National Science Foundation, the Panel on Telecommunications Research of the Committee on Telecommunications of the National Academy of Engineering has made a preliminary survey of the status and trends of telecommunications research in the United States and selected foreign countries. The status and trends were identified by…

  14. A Survey of Self-Advocacy Groups for People with Learning Disabilities in an English Region: Part II.

    ERIC Educational Resources Information Center

    McNally, Steve

    2003-01-01

    The second article on a survey of self-advocacy groups for people with learning disabilities in England reports key findings that included the consistency of the issues identified as important and the willingness to engage in research. Key themes were self-advocacy, rights, day service center issues, staffing, personal relationships, complaints,…

  15. Biennial Survey of Education in the United States, 1928-1930. Bulletin, 1931, No. 20. Volume II. [Chapter I - III

    ERIC Educational Resources Information Center

    Office of Education, United States Department of the Interior, 1932

    1932-01-01

    This document contains the first three chapters of the Biennial Survey of Education in the United States, covering the years 1928-1930. These chapters include: (1) Statistical summary of education, 1929-30 (Emery M. Foster); (2) Statistics of State school systems, 1929-30 (David T. Blose with the cooperation of Walter S. Deffenbaugh); and (3)…

  16. Human Trafficking in the United States. Part II. Survey of U.S. Government Web Resources for Publications and Data

    ERIC Educational Resources Information Center

    Panigabutra-Roberts, Anchalee

    2012-01-01

    This second part of a two-part series is a survey of U.S. government web resources on human trafficking in the United States, particularly of the online publications and data included on agencies' websites. Overall, the goal is to provide an introduction, an overview, and a guide on this topic for library staff to use in their research and…

  17. A Survey of Self-Advocacy Groups for People with Learning Disabilities in an English Region: Part II.

    ERIC Educational Resources Information Center

    McNally, Steve

    2003-01-01

    The second article on a survey of self-advocacy groups for people with learning disabilities in England reports key findings that included the consistency of the issues identified as important and the willingness to engage in research. Key themes were self-advocacy, rights, day service center issues, staffing, personal relationships, complaints,…

  18. Survey of Land-Grant Colleges and Universities. Bulletin, 1930, No. 9. Volume II. [Part I - Part VI

    ERIC Educational Resources Information Center

    Office of Education, United States Department of the Interior, 1930

    1930-01-01

    The attached document covers the initial sections of the second volume of the Survey of Land-Grant Colleges and Universities, from Part I to Part VI. Part I, Arts and sciences, contains the following chapters: (1) Introduction; (2) Arts and science organization; (3) Specialization; (4) Enrollments and salaries; (5) Articulation with secondary…

  19. Domestic violence and immigration status among Latina mothers in the child welfare system: findings from the National Survey of Child and Adolescent Well-being II (NSCAW II).

    PubMed

    Ogbonnaya, Ijeoma Nwabuzor; Finno-Velasquez, Megan; Kohl, Patricia L

    2015-01-01

    Many children involved with the child welfare system witness parental domestic violence. The association between children's domestic violence exposure and child welfare involvement may be influenced by certain socio-cultural factors; however, minimal research has examined this relationship. The current study compares domestic violence experiences and case outcomes among Latinas who are legal immigrants (n=39), unauthorized immigrants (n=77), naturalized citizens (n=30), and US-born citizen mothers (n=383) reported for child maltreatment. This analysis used data from the second round of the National Survey of Child and Adolescent Well-being. Mothers were asked about whether they experienced domestic violence during the past year. In addition, data were collected to assess if (a) domestic violence was the primary abuse type reported and, if so, (b) the maltreatment allegation was substantiated. Results show that naturalized citizens, legal residents, and unauthorized immigrants did not differ from US-born citizens in self-reports of domestic violence; approximately 33% of mothers reported experiences of domestic violence within the past year. Yet, unauthorized immigrants were 3.76 times more likely than US-born citizens to have cases with allegations of domestic violence as the primary abuse type. Despite higher rates of alleged domestic violence, unauthorized citizens were not more likely than US-born citizens to have these cases substantiated for domestic violence (F(2.26, 153.99)=0.709, p=.510). Findings highlight that domestic violence is not accurately accounted for in families with unauthorized immigrant mothers. We recommend child welfare workers are trained to properly assess and fulfill the needs of immigrant families, particularly as it relates to domestic violence. Copyright © 2014 Elsevier Ltd. All rights reserved.

  20. Emergence of dengue virus 4 genotype II in Guangzhou, China, 2010: survey and molecular epidemiology of one community outbreak.

    PubMed

    Jing, Qin-Long; Yang, Zhi-Cong; Luo, Lei; Xiao, Xin-Cai; Di, Biao; He, Peng; Fu, Chuan-Xi; Wang, Ming; Lu, Jia-Hai

    2012-04-12

    The re-emergence of dengue virus 4 (DENV-4) has become a public health concern in South America, Southeast Asia and South Asia. However, it has not been known to have caused a local outbreak in China for the past 20 years. The purpose of this study was to elucidate the epidemiology of one local community outbreak caused by DENV-4 in Guangzhou city, China, in 2010; and to determine the molecular characteristics of the genotype II virus involved. During September and October of 2010, one imported case, a Guangzhou resident who travelled back from Thailand, resulted in 18 secondary autochthonous cases in Guangzhou City, with an incidence rate of 5.53 per 10,000 residents. In indigenous cases, 14 serum samples tested positive for IgM against DENV and 7 for IgG from a total of 15 submitted serum samples, accompanied by 5 DENV-4 isolates. With identical envelope gene nucleotide sequences, the two isolates (D10168-GZ from the imported index case and Guangzhou 10660 from the first isolate in the autochthonous cases) were grouped into DENV-4 genotype II after comparison to 32 previous DENV-4 isolates from GenBank that originated from different areas. Based on epidemiological and phylogenetic analyses, the outbreak, which was absent for 20 years after the DENV-4 genotype I outbreak in 1990, was confirmed as DENV-4 genotype II and initially traced to the imported index case, a Guangzhou resident who travelled back from Thailand.

  1. Survey of Lake Ontario bottom sediment off Rochester, New York, to define the extent of jettisoned World War II material and its potential for sediment contamination

    USGS Publications Warehouse

    Kennedy, Gregory; Kappel, William M.

    2000-01-01

    Military-type mat??riel was recovered from the bottom of Lake Ontario near Rochester, N.Y., during bottom-trawl, fish-stock surveys at depths of 75 to 180 feet each year from 1978 through 1996. The recovered mat??riel included many shell-detonator nose cones (2 inches in diameter by about 3.5 inches long); several electronic components; one corroded box of detonators; a corrugated container of mercury-filled capsules; and corroded batteries. Most of the recovered mat??riel has been identified as defective components of shell detonators (proximity-fuze assemblies) that were jettisoned in the lake to protect them from discovery during World War II. Side-scan SONAR, metal-detector, and ROV (remotely-operated-vehicle) surveys found no evidence of any large piles of mat??riel containing potentially hazardous, toxic, or polluting materials within the 17-square-mile study site. Many scattered magnetic anomalies were detected in this area, but chemical analysis of bottom sediment and of zebra- and quagga-mussel (Dreissena spp.) tissue indicate that the concentrations of mercury and other heavy metals are within the previously documented ranges for Lake Ontario sediment. The failure of ROV videos and of SCUBA-diver surveys and probes of the lake bottom to locate any debris indicates that most, if not all, of the debris is scattered and buried under a layer of fine-grained sediment and, possibly, mussels.

  2. Part I. Synthesis and characterization of C2 substituted imidazolium room temperature ionic liquids. Part II. Survey and analysis of organic chemistry textbooks

    NASA Astrophysics Data System (ADS)

    Ennis, Elliot G.

    Part I. Among room temperature ionic liquids (RTILs), those derived from the imidazolium cation are the most common. RTILs have generally been viewed solely as solvents, but they are able to participate in certain types of reactions, particularly due to the relatively high acidity at the imidazolium C2. Deprotonation affords N-heterocyclic carbenes (NHCs), which can cause unwanted side reactions. Consequently, the major limitation of imidazolium RTILs is that they cannot be used as solvents in highly basic reactions such as the Baylis-Hillman and Grignard reactions. This work reveals a convenient route for the preparation of C2-substituted imidazolium ionic liquids. This method involves the alkylation of N-heterocyclic carbenes, which are readily generated from the C2-unsubstituted imidazolium ionic liquids. It works well for nonfunctionalized alkyl chlorides and less well for alkyl bromides and iodides, likely due to competing elimination reactions. The resulting C2-substituted salts can be transformed into ionic liquids via standard anion metathesis reactions. Part II. Recent advances in media and the increasingly encyclopedic nature of traditional textbooks have made their role in college classes uncertain. In an effort to discover what is really being taught in organic chemistry courses across the US, a survey of organic chemistry professors in all 50 states was conducted to determine what material is covered in their organic chemistry courses for science majors. Survey Monkey, an online survey program, was used to construct a short 10-item survey which was sent to organic chemistry professors at various types of institutions across the nation. We sent out 2417 surveys and received 489 responses. The results of this survey revealed what topics the professors believe is core material and what they feel is extraneous. Additionally, this research identifies the things these professors would like to see changed in the organic chemistry texts. From the open

  3. Systematic Survey for [O ii], [O iii], and Hα Blobs at z = 0.1-1.5: The Implication for Evolution of Galactic-scale Outflow

    NASA Astrophysics Data System (ADS)

    Yuma, Suraphong; Ouchi, Masami; Drake, Alyssa B.; Fujimoto, Seiji; Kojima, Takashi; Sugahara, Yuma

    2017-06-01

    We conduct a systematic search for galaxies at z=0.1{--}1.5 with [O ii]λ 3727, [O iii]λ 5007, or Hα λ 6563 emission lines extended over at least 30 kpc by using deep narrowband and broadband imaging in the Subaru-XMM Deep Survey field. These extended emission-line galaxies are dubbed [O ii], [O iii], or Hα blobs. Based on a new selection method that securely selects extended emission-line galaxies, we find 77 blobs at z=0.40{--}1.46 with the isophotal area of emission lines down to 1.2× {10}-18 erg s-1 cm-2 kpc-2. Four of them are spectroscopically confirmed to be [O iii] blobs at z = 0.83. We identify AGN activities in eight blobs with X-ray and radio data, and find that the fraction of AGN contribution increases with increasing isophotal area of the extended emission. With the Kolmogorov-Smirnov (KS) and Anderson-Darling tests, we confirm that the stellar-mass distributions of Hα and [O ii] blobs are not drawn from those of the emitters at the > 90% confidence level in that Hα and [O ii] blobs are located at the massive end of the distributions, but cannot reject a null hypothesis of being the same distributions in terms of the specific star formation rates. It is suggested that galactic-scale outflows tend to be more prominent in more massive star-forming galaxies. Exploiting our sample homogeneously selected over the large area, we derive the number densities of blobs at each epoch. The number densities of blobs decrease drastically with redshifts at a rate that is larger than that of the decrease of cosmic star formation densities.

  4. Robo-AO Kepler Planetary Candidate Survey. II. Adaptive Optics Imaging of 969 Kepler Exoplanet Candidate Host Stars

    NASA Astrophysics Data System (ADS)

    Baranec, Christoph; Ziegler, Carl; Law, Nicholas M.; Morton, Tim; Riddle, Reed; Atkinson, Dani; Schonhut, Jessica; Crepp, Justin

    2016-07-01

    We initiated the Robo-AO Kepler Planetary Candidate Survey in 2012 to observe each Kepler exoplanet candidate host star with high angular resolution, visible light, laser adaptive optics (AOs) imaging. Our goal is to find nearby stars lying in Kepler's photometric apertures that are responsible for the relatively high probability of false-positive exoplanet detections and that cause underestimates of the size of transit radii. Our comprehensive survey will also shed light on the effects of stellar multiplicity on exoplanet properties and will identify rare exoplanetary architectures. In this second part of our ongoing survey, we observed an additional 969 Kepler planet candidate hosts and we report blended stellar companions up to {{Δ }}m≈ 6 that contribute to Kepler's measured light curves. We found 203 companions within ˜4″ of 181 of the Kepler stars, of which 141 are new discoveries. We measure the nearby star probability for this sample of Kepler planet candidate host stars to be 10.6% ± 1.1% at angular separations up to 2.″5, significantly higher than the 7.4% ± 1.0% probability discovered in our initial sample of 715 stars; we find the probability increases to 17.6% ± 1.5% out to a separation of 4.″0. The median position of Kepler Objects of Interest (KOIs) observed in this survey are 1.°1 closer to the galactic plane, which may account for some of the nearby star probability enhancement. We additionally detail 50 Keck AO images of Robo-AO observed KOIs in order to confirm 37 companions detected at a <5σ significance level and to obtain additional infrared photometry on higher significance detected companions.

  5. The 6-GHz multibeam maser survey - II. Statistical analysis and Galactic distribution of 6668-MHz methanol masers

    NASA Astrophysics Data System (ADS)

    Green, J. A.; Breen, S. L.; Fuller, G. A.; McClure-Griffiths, N. M.; Ellingsen, S. P.; Voronkov, M. A.; Avison, A.; Brooks, K.; Burton, M. G.; Chrysostomou, A.; Cox, J.; Diamond, P. J.; Gray, M. D.; Hoare, M. G.; Masheder, M. R. W.; Pestalozzi, M.; Phillips, C.; Quinn, L. J.; Richards, A. M. S.; Thompson, M. A.; Walsh, A. J.; Ward-Thompson, D.; Wong-McSweeney, D.; Yates, J. A.

    2017-08-01

    The Methanol Multibeam survey has produced the largest and most complete census of methanol and excited-state hydroxyl masers in the Galaxy to date. Observing the entire Galactic plane visible from the Southern hemisphere for 6668-MHz methanol and 6030/6035-MHz hydroxyl masers, to an rms sensitivity of 0.015 Jy km s-1, the survey has detected a total of 972 methanol maser sources, implying a total Galactic population of ˜1290 sources with flux densities above the survey 3σ peak flux density limit of 0.51 Jy. We present here the statistical properties of the methanol detections of the survey, including distributions in flux density, variability and range of source velocities. The data suggest that the weaker masers exhibit greater variability. We also present an analysis of the Galactic distribution of 6668-MHz methanol masers. For the Galactic distribution, we present kinematic distance resolutions to an additional 202 sources to those published previously, and collate these with previous allocations, as well as exploring a recent Bayesian distance approach based on maser parallaxes to separately determine distances. We examine Galactic structure and determine the luminosity function of the Galactic population of methanol masers. We find that more luminous masers have an evenly distributed wide range of velocity widths compared with less luminous masers being dominated by narrow velocity ranges, with the implication that this may be tied to the evolution of the host protostar(s). We also see an indication that brighter sources are seen towards the arm origins.

  6. Massive open star clusters using the VVV survey. II. Discovery of six clusters with Wolf-Rayet stars

    NASA Astrophysics Data System (ADS)

    Chené, A.-N.; Borissova, J.; Bonatto, C.; Majaess, D. J.; Baume, G.; Clarke, J. R. A.; Kurtev, R.; Schnurr, O.; Bouret, J.-C.; Catelan, M.; Emerson, J. P.; Feinstein, C.; Geisler, D.; de Grijs, R.; Hervé, A.; Ivanov, V. D.; Kumar, M. S. N.; Lucas, P.; Mahy, L.; Martins, F.; Mauro, F.; Minniti, D.; Moni Bidin, C.

    2013-01-01

    Context. The ESO Public Survey "VISTA Variables in the Vía Láctea" (VVV) provides deep multi-epoch infrared observations for an unprecedented 562 sq. degrees of the Galactic bulge, and adjacent regions of the disk. Nearly 150 new open clusters and cluster candidates have been discovered in this survey. Aims: This is the second in a series of papers about young, massive open clusters observed using the VVV survey. We present the first study of six recently discovered clusters. These clusters contain at least one newly discovered Wolf-Rayet (WR) star. Methods: Following the methodology presented in the first paper of the series, wide-field, deep JHKs VVV observations, combined with new infrared spectroscopy, are employed to constrain fundamental parameters for a subset of clusters. Results: We find that the six studied stellar groups are real young (2-7 Myr) and massive (between 0.8 and 2.2 × 103 M⊙) clusters. They are highly obscured (AV ~ 5-24 mag) and compact (1-2 pc). In addition to WR stars, two of the six clusters also contain at least one red supergiant star, and one of these two clusters also contains a blue supergiant. We claim the discovery of 8 new WR stars, and 3 stars showing WR-like emission lines which could be classified WR or OIf. Preliminary analysis provides initial masses of ~30-50 M⊙ for the WR stars. Finally, we discuss the spiral structure of the Galaxy using the six new clusters as tracers, together with the previously studied VVV clusters. Based on observations with ISAAC, VLT, ESO (programme 087.D-0341A), New Technology Telescope at ESO's La Silla Observatory (programme 087.D-0490A) and with the Clay telescope at the Las Campanas Observatory (programme CN2011A-086). Also based on data from the VVV survey (programme 172.B-2002).

  7. The OmegaWhite Survey for short period variable stars - II. An overview of results from the first four years

    NASA Astrophysics Data System (ADS)

    Toma, R.; Ramsay, G.; Macfarlane, S.; Groot, P. J.; Woudt, P. A.; Dhillon, V.; Jeffery, C. S.; Marsh, T.; Nelemans, G.; Steeghs, D.

    2016-11-01

    OmegaWhite is a wide-field, high cadence, synoptic survey targeting fields in the southern Galactic plane, with the aim of discovering short period variable stars. Our strategy is to take a series of 39 s exposures in the g band of a 1 deg2 of sky lasting 2 h using the OmegaCAM wide field imager on the VLT Survey Telescope (VST). We give an overview of the initial 4 yr of data which covers 134 deg2 and includes 12.3 million light curves. As the fields overlap with the VLT Survey Telescope Hα Photometric Survey of the Galactic plane and Bulge (VPHAS+), we currently have ugriHα photometry for ˜1/3 of our fields. We find that a significant fraction of the light curves have been affected by the diffraction spikes of bright stars sweeping across stars within a few dozen of pixels over the two hour observing time interval due to the alt-az nature of the VST. We select candidate variable stars using a variety of variability statistics, followed by a manual verification stage. We present samples of several classes of short period variables, including: an ultra compact binary, a DQ white dwarf, a compact object with evidence of a 100 min rotation period, three CVs, one eclipsing binary with an 85 min period, a symbiotic binary which shows evidence of a 31 min photometric period, and a large sample of candidate δ Sct type stars including one with a 9.3 min period. Our overall goal is to cover 400 deg2, and this study indicates we will find many more interesting short period variable stars as a result.

  8. The Chandra Planetary Nebula Survey (ChanPlaNS). II. X-Ray Emission from Compact Planetary Nebulae

    NASA Astrophysics Data System (ADS)

    Freeman, M.; Montez, R., Jr.; Kastner, J. H.; Balick, B.; Frew, D. J.; Jones, D.; Miszalski, B.; Sahai, R.; Blackman, E.; Chu, Y.-H.; De Marco, O.; Frank, A.; Guerrero, M. A.; Lopez, J. A.; Zijlstra, A.; Bujarrabal, V.; Corradi, R. L. M.; Nordhaus, J.; Parker, Q. A.; Sandin, C.; Schönberner, D.; Soker, N.; Sokoloski, J. L.; Steffen, M.; Toalá, J. A.; Ueta, T.; Villaver, E.

    2014-10-01

    We present results from the most recent set of observations obtained as part of the Chandra X-ray observatory Planetary Nebula Survey (ChanPlaNS), the first comprehensive X-ray survey of planetary nebulae (PNe) in the solar neighborhood (i.e., within ~1.5 kpc of the Sun). The survey is designed to place constraints on the frequency of appearance and range of X-ray spectral characteristics of X-ray-emitting PN central stars and the evolutionary timescales of wind-shock-heated bubbles within PNe. ChanPlaNS began with a combined Cycle 12 and archive Chandra survey of 35 PNe. ChanPlaNS continued via a Chandra Cycle 14 Large Program which targeted all (24) remaining known compact (R neb <~ 0.4 pc), young PNe that lie within ~1.5 kpc. Results from these Cycle 14 observations include first-time X-ray detections of hot bubbles within NGC 1501, 3918, 6153, and 6369, and point sources in HbDs 1, NGC 6337, and Sp 1. The addition of the Cycle 14 results brings the overall ChanPlaNS diffuse X-ray detection rate to ~27% and the point source detection rate to ~36%. It has become clearer that diffuse X-ray emission is associated with young (lsim 5 × 103 yr), and likewise compact (R neb <~ 0.15 pc), PNe with closed structures and high central electron densities (ne >~ 1000 cm-3), and is rarely associated with PNe that show H2 emission and/or pronounced butterfly structures. Hb 5 is one such exception of a PN with a butterfly structure that hosts diffuse X-ray emission. Additionally, two of the five new diffuse X-ray detections (NGC 1501 and NGC 6369) host [WR]-type central stars, supporting the hypothesis that PNe with central stars of [WR]-type are likely to display diffuse X-ray emission.

  9. Massachusetts--Stony Brook Galactic Plane CO Survey. II. (l,V) Maps of the First Galactic Quadrant

    NASA Astrophysics Data System (ADS)

    Clemens, D. P.; Sanders, D. B.; Scoville, N. Z.; Solomon, P. M.

    1986-06-01

    The Massachusetts-Stony Brook Galactic Plane CO Survey data set, consisting of 40,551 12CO J =1-0 spectra covering longitudes 8° -90° and latitudes -1.°05 to + 1°, is presented in longitude-velocity (l, V) format. Spectra from the 42 latitudes sampled were averaged to yield seven (l, V) gray scale maps with 18' latitude resolution. One contour (l, V) map along the Galactic equator is included to show the spatially clumpy nature of the CO emission. The integrated CO intensity is presented as a function of longitude for the 18' averaged data, and as a function of longitude and latitude in contour and gray scale maps at the full survey spatial resolution. The presentations of the data set contained here are most useful for comparison with other Galactic surveys of the first quadrant, for tracing out large-scale features, and for identifying emission-line velocities associated with continuum (e.g., radio and IRAS) sources.

  10. Synthesizing exoplanet demographics from radial velocity and microlensing surveys. II. The frequency of planets orbiting M dwarfs

    SciTech Connect

    Clanton, Christian; Gaudi, B. Scott

    2014-08-20

    In contrast to radial velocity (RV) surveys, results from microlensing surveys indicate that giant planets with masses greater than the critical mass for core accretion (∼0.1 M {sub Jup}) are relatively common around low-mass stars. Using the methodology developed in the first paper, we predict the sensitivity of M-dwarf RV surveys to analogs of the population of planets inferred by microlensing. We find that RV surveys should detect a handful of super-Jovian (>M {sub Jup}) planets at the longest periods being probed. These planets are indeed found by RV surveys, implying that the demographic constraints inferred from these two methods are consistent. Finally, we combine the results from both methods to estimate planet frequencies spanning wide regions of parameter space. We find that the frequency of Jupiters and super-Jupiters (1 ≲ m{sub p} sin i/M {sub Jup} ≲ 13) with periods 1 ≤ P/days ≤ 10{sup 4} is f{sub J}=0.029{sub −0.015}{sup +0.013}, a median factor of 4.3 (1.5-14 at 95% confidence) smaller than the inferred frequency of such planets around FGK stars of 0.11 ± 0.02. However, we find the frequency of all giant planets with 30 ≲ m{sub p} sin i/M {sub ⊕} ≲ 10{sup 4} and 1 ≤ P/days ≤ 10{sup 4} to be f{sub G}=0.15{sub −0.07}{sup +0.06}, only a median factor of 2.2 (0.73-5.9 at 95% confidence) smaller than the inferred frequency of such planets orbiting FGK stars of 0.31 ± 0.07. For a more conservative definition of giant planets (50 ≲ m{sub p} sin i/M {sub ⊕} ≲ 10{sup 4}), we find f{sub G{sup ′}}=0.11±0.05, a median factor of 2.2 (0.73-6.7 at 95% confidence) smaller than that inferred for FGK stars of 0.25 ± 0.05. Finally, we find the frequency of all planets with 1 ≤ m{sub p} sin i/M {sub ⊕} ≤ 10{sup 4} and 1 ≤ P/days ≤ 10{sup 4} to be f{sub p} = 1.9 ± 0.5.

  11. EMISSION-LINE GALAXIES FROM THE HUBBLE SPACE TELESCOPE PROBING EVOLUTION AND REIONIZATION SPECTROSCOPICALLY (PEARS) GRISM SURVEY. II. THE COMPLETE SAMPLE

    SciTech Connect

    Pirzkal, Nor; Rothberg, Barry; Ly, Chun; Grogin, Norman A.; Dahlen, Tomas; Noeske, Kai G.; Bellini, Andrea; Malhotra, Sangeeta; Rhoads, James E.; Cohen, Seth H.; Mechtley, Matthew; Windhorst, Rogier A.; Meurer, Gerhardt R.; Walsh, Jeremy R.; Hathi, Nimish P.; Holwerda, Benne W.; Straughn, Amber N.

    2013-07-20

    We present a full analysis of the Probing Evolution And Reionization Spectroscopically (PEARS) slitess grism spectroscopic data obtained with the Advanced Camera for Surveys on board Hubble Space Telescope. PEARS covers fields within both the Great Observatories Origins Deep Survey (GOODS) North and South fields, making it ideal as a random survey of galaxies, as well as the availability of a wide variety of ancillary observations complemented by the spectroscopic results. Using the PEARS data, we are able to identify star-forming galaxies (SFGs) within the redshift volume 0 < z < 1.5. Star-forming regions in the PEARS survey are pinpointed independently of the host galaxy. This method allows us to detect the presence of multiple emission-line regions (ELRs) within a single galaxy. We identified a total of 1162 H{alpha}, [O III], and/or [O II] emission lines in the PEARS sample of 906 galaxies to a limiting flux of {approx}10{sup -18} erg s{sup -1} cm{sup -2}. The ELRs have also been compared to the properties of the host galaxy, including morphology, luminosity, and mass. From this analysis, we find three key results: (1) the computed line luminosities show evidence of a flattening in the luminosity function with increasing redshift; (2) the star-forming systems show evidence of complex morphologies with star formation occurring predominantly within one effective (half-light) radius. However, the morphologies show no correlation with host stellar mass. (3) Also, the number density of SFGs with M{sub *} {>=} 10{sup 9} M{sub Sun} decreases by an order of magnitude at z {<=} 0.5 relative to the number at 0.5 < z < 0.9, supporting the argument of galaxy downsizing.

  12. FIRST-based survey of Compact Steep Spectrum sources. II. MERLIN and VLA observations of medium-sized symmetric objects

    NASA Astrophysics Data System (ADS)

    Kunert-Bajraszewska, M.; Marecki, A.; Thomasson, P.; Spencer, R. E.

    2005-09-01

    A new sample of candidate Compact Steep Spectrum (CSS) sources that are much weaker than the CSS source prototypes has been selected from the VLA FIRST catalogue. MERLIN "snapshot" observations of the sources at 5 GHz indicate that six of them have an FR II-like morphology, but are not edge-brightened as is normal for Medium-sized Symmetric Objects (MSOs) and FR IIs. Further observations of these six sources with the VLA at 4.9 GHz and MERLIN at 1.7 GHz, as well as subsequent full-track observations with MERLIN at 5 GHz of what appeared to be the two sources of greatest interest are presented. The results are discussed with reference to the established evolutionary model of CSS sources being young but in which not all of them evolve to become old objects with extended radio structures. A lack of stable fuelling in some of them may result in an early transition to a so-called coasting phase so that they fade away instead of growing to become large-scale objects. It is possible that one of the six sources (1542+323) could be labelled as a prematurely "dying" MSO or a "fader".

  13. BAT AGN spectroscopic survey-II. X-ray emission and high-ionization optical emission lines

    NASA Astrophysics Data System (ADS)

    Berney, Simon; Koss, Michael; Trakhtenbrot, Benny; Ricci, Claudio; Lamperti, Isabella; Schawinski, Kevin; Baloković, Mislav; Crenshaw, D. Michael; Fischer, Travis; Gehrels, Neil; Harrison, Fiona; Hashimoto, Yasuhiro; Ichikawa, Kohei; Mushotzky, Richard; Oh, Kyuseok; Stern, Daniel; Treister, Ezequiel; Ueda, Yoshihiro; Veilleux, Sylvain; Winter, Lisa

    2015-12-01

    We investigate the relationship between X-ray and optical line emission in 340 nearby (z ≃ 0.04) AGN selected above 10 keV using Swift BAT. We find a weak correlation between the extinction corrected [O III] and hard X-ray luminosity (L_[O III]^{int} ∝ L_{14-195}) with a large scatter (RPear = 0.64, σ = 0.62 dex) and a similarly large scatter with the intrinsic 2-10 keV to [O III] luminosities (RPear = 0.63, σ = 0.63 dex). Correlations of the hard X-ray fluxes with the fluxes of high-ionization narrow lines ([O III], He II, [Ne III] and [Ne V]) are not significantly better than with the low-ionization lines (H α, [S II]). Factors like obscuration or physical slit size are not found to be a significant part of the large scatter. In contrast, the optical emission lines show much better correlations with each other (σ = 0.3 dex) than with the X-ray flux. The inherent large scatter questions the common usage of narrow emission lines as AGN bolometric luminosity indicators and suggests that other issues such as geometrical differences in the scattering of the ionized gas or long-term AGN variability are important.

  14. Polarimetric survey of main-belt asteroids. II. Results for 58 B- and C-type objects

    NASA Astrophysics Data System (ADS)

    Gil-Hutton, R.; Cañada-Assandri, M.

    2012-03-01

    Aims: We present results of a polarimetric survey of main-belt asteroids at Complejo Astronómico el Leoncito (CASLEO), San Juan, Argentina. The aims of this survey are to increase the database of asteroid polarimetry, to estimate diversity in polarimetric properties of asteroids that belong to different taxonomic classes, and to search for objects that exhibit anomalous polarimetric properties. Methods: The data were obtained with the Torino and CASPROF polarimeters at the 2.15m telescope. The Torino polarimeter is an instrument that allows simultaneous measurement of polarization in five different bands, and the CASPROF polarimeter is a two-hole aperture polarimeter with rapid modulation. Results: The survey began in 2003, and up to 2009 data on a sample of more than 170 asteroids were obtained. In this paper the results for 58 B- and C-type objects are presented, most of them polarimetrically observed for the first time. Using these data we find phase-polarization curves and polarimetric parameters for these taxonomic classes. Based on observations carried out at the Complejo Astronómico El Leoncito, operated under agreement between the Consejo Nacional de Investigaciones Científicas y Técnicas de la República Argentina and the National Universities of La Plata, Córdoba, and San Juan.Tables 1 and 2 are available in electronic form at CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/539/A115

  15. OT2_eegami_5: Herschel Lensing Survey II: Completing the Herschel Legacy with the HST/MCT CLASH Sample

    NASA Astrophysics Data System (ADS)

    Egami, E.

    2011-09-01

    For deep imaging longward of 100 um, confusion noise sets the fundamental sensitivity limits achievable with Herschel, and these limits cannot be improved by integrating longer. To penetrate through this confusion limit and detect faint high-redshift galaxies, gravitational lensing by massive galaxy clusters offers a very powerful and yet cheap solution. For this reason, our team has been conducting a PACS/SPIRE imaging survey of 44 massive lensing clusters as one of the Herschel Key Programs, "The Herschel Lensing Survey" (PI: Egami, 292.3 hrs). Deep PACS/SPIRE imaging data of massive clusters are quite rich with a variety of information, which allows us to study not only the properties of gravitationally lensed high-redshift galaxies but also those of cluster member galaxies and the intracluster medium through the analysis of the Sunyaev-Zel'dovich effect. In January 2010, a massive HST program targeting powerful lensing clusters was accepted as one of the three multi-cycle treasury (MCT) programs. This program, ``the Cluster Lensing And Supernova survey with Hubble'' (CLASH), has an allocation of 524 orbits, and will obtain deep ACS and WFC3 images of 25 massive galaxy clusters using 16 broad-band filters from near-UV (2250 A) to near-IR (1.6 um). These extensive multi-filter imaging observations will produce high-precision photometric redshifts (sigma/(1+z)<0.02). On average, the program spends 20 orbits per cluster. Considering this enormous investment of HST time, the CLASH program will define the ultimate sample of massive galaxy clusters on which future studies will focus. Here, we propose to obtain deep PACS and SPIRE images for 10 CLASH clusters that still lack such data (the other 15 clusters already have a good Herschel coverage). To fully exploit the combination of the Herschel and HST data, the HLS and CLASH teams are submitting this proposal jointly with the participation of key scientists from both teams.

  16. OT2_eegami_6: SPIRE Snapshot Survey II: Using SPT/CODEX Massive Clusters as Powerful Gravitational Lenses

    NASA Astrophysics Data System (ADS)

    Egami, E.

    2011-09-01

    On the extragalactic side, one of the most remarkable results coming out of Herschel is the discovery of extremely bright (>100 mJy in the SPIRE bands) gravitationally lensed galaxies. The great sensitivity and mapping speed of SPIRE have enabled us to find these rare extraordinary objects. What is truly exciting about these bright lensed galaxies is that they enable a variety of detailed multi-wavelength follow-up observations, shedding new light on the physical properties of these high-redshift sources. In this regard, our OT1 program, "SPIRE Snapshot Survey of Massive Galaxy Clusters" turned out to be a great success. After imaging ~50 galaxies out of 279 in the program, we have already found two spectacularly bright lensed galaxies, one of which is at a redshift of 4.69. This type of cluster-lensed sources are not only bright but also spatially stretched over a large scale, so ALMA (or NOEMA in the north) is likely to be able to study them at the level of individual GMCs. Such studies will open up a new frontier in the study of high-redshift galaxies. Here, we propose to extend this highly efficient and effective survey of gravitationally lensed galaxies to another 353 clusters carefully chosen from the SPT and CODEX cluster samples. These samples contain newly discovered high-redshift (z>0.3) massive (>3-4e14 Msun) clusters, which can be used as powerful gravitational lenses to magnify sources at high redshift. With the OT1 and OT2 surveys together, we expect to find ~20 highly magnified SPIRE sources with exceptional brightnesses (assuming a discovery rate of ~1/30). Such a unique sample of extraordinary objects will enable a variety of follow-up sciences, and will therefore remain as a great legacy of the Herschel mission for years to come.

  17. Young Plastic Surgeons Forum member survey: Part II. Advocacy in plastic surgery: opinions toward the ASPS and PlastyPAC.

    PubMed

    Ver Halen, Jon P; Chen, Andrew; Jeffers, Lynn; Basu, C Bob

    2014-08-01

    Given the continued evolution of the American health system, the authors explored young plastic surgeons' attitudes on challenges affecting the specialty and the future role of organized plastic surgery and its advocacy mission. A 21-question online survey was distributed to all members of the Young Plastic Surgeons Forum. Questions were related to demographics, attitudes toward policy issues, participation in the American Society of Plastic Surgeons, and its advocacy efforts. The survey was e-mailed to 2155 Forum members, of which 397 responded (19% response rate). Young plastic surgeons appear to be interested in American Society of Plastic Surgeons and PlastyPAC, as evidenced by a higher than normal response rate to this survey and rate of contribution. However, a lack of awareness about the details of the organizations and mechanisms for involvement remains. Scope-of-practice issues and encroachment on the specialty by noncore providers remain the top concern of young plastic surgeons. Other top concerns were financial barriers to participation in advocacy efforts and concerns with return on investment on PlastyPAC contributions. A majority received minimal or no public policy education on issues affecting plastic surgery during training. A minority currently participate in American Society of Plastic Surgeons advocacy efforts. These data represent the first such collection of opinions from Young Plastic Surgeons members regarding goals and directions of the American Society of Plastic Surgeons and PlastyPAC. These organizations are in a uniquely strong position to enlist participation from and provide for the future success of the profession's younger members.

  18. The Chandra Deep Survey of the Hubble Deep Field-North Area. II. Results from the Caltech Faint Field Galaxy Redshift Survey Area

    NASA Astrophysics Data System (ADS)

    Hornschemeier, A. E.; Brandt, W. N.; Garmire, G. P.; Schneider, D. P.; Barger, A. J.; Broos, P. S.; Cowie, L. L.; Townsley, L. K.; Bautz, M. W.; Burrows, D. N.; Chartas, G.; Feigelson, E. D.; Griffiths, R. E.; Lumb, D.; Nousek, J. A.; Ramsey, L. W.; Sargent, W. L. W.

    2001-06-01

    A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9 ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6‧×8.7‧ area covered by the Caltech Faint Field Galaxy Redshift Survey (the ``Caltech area''). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2 keV (soft) and 2-8 keV (hard) bands are ~1.3×10-16 and ~6.5×10-16 ergs cm-2 s-1, respectively. More than ~80% of the extragalactic X-ray background in the hard band is resolved. The 82 Chandra sources detected in the Caltech area are correlated with more than 25 multiwavelength source catalogs, and the results of these correlations as well as spectroscopic follow-up results obtained with the Keck and Hobby-Eberly Telescopes are presented. All but nine of the Chandra sources are detected optically with R<~26.5. Redshifts are available for 39% of the Chandra sources, including 96% of the sources with R<23 the redshift range is 0.1-3.5, with most sources having z<1.5. Eight of the X-ray sources are located in the HDF-N itself, including two not previously reported. A population of X-ray faint, optically bright, nearby galaxies emerges at soft-band fluxes of <~3×10-16 ergs cm-2 s-1. Our multiwavelength correlations have set the tightest constraints to date on the X-ray emission properties of μJy radio sources, mid-infrared sources detected by the Infrared Space Observatory (ISO), and very red (R-Ks>5.0) objects. A total of 16 of the 67 1.4 GHz μJy sources in the Caltech area are detected in the

  19. Report for borehole explosion data acquired in the 1999 Los Angeles Region Seismic Experiment (LARSE II), Southern California: Part I, description of the survey

    USGS Publications Warehouse

    Fuis, Gary S.; Murphy, Janice M.; Okaya, David A.; Clayton, Robert W.; Davis, Paul M.; Thygesen, Kristina; Baher, Shirley A.; Ryberg, Trond; Benthien, Mark L.; Simila, Gerry; Perron, J. Taylor; Yong, Alan K.; Reusser, Luke; Lutter, William J.; Kaip, Galen; Fort, Michael D.; Asudeh, Isa; Sell, Russell; Van Schaack, John R.; Criley, Edward E.; Kaderabek, Ronald; Kohler, Will M.; Magnuski, Nickolas H.

    2001-01-01

    explosions and vibrating-truck sources onshore. The two chief LARSE transects pass near recent moderate earthquakes, including the 1971 M 6.7 San Fernando, 1987 M 5.9 Whittier Narrows, 1991 M 5.8 Sierra Madre, and 1994 M 6.7 Northridge earthquakes. The first transect extended from San Clemente Island northeastward to the Mojave Desert (Line 1, Fig. 1), passing near the epicenter of the Whittier Narrows and Sierra Madre earthquakes. The second transect extended from west of San Clemente Island northward to the western Mojave Desert (Line 2, Figs. 1, 2), passing through the epicenter of the Northridge earthquake and near the epicenter of the San Fernando earthquake. Data along Line 1 were acquired during the years 1993-1994, and data along Line 2, during the years 1994–2000. In this open-file report and that of Murphy and others (in preparation), we present the details of the October 1999 explosion survey along Line 2, which extended from Santa Monica Bay northward to the western Mojave Desert (Figs. 1, 2). This survey is referred to as LARSE II. In this survey, 93 borehole explosions were detonated along the main north-south line and along 5 auxiliary lines in the San Fernando Valley and Santa Monica areas. These explosions were recorded by ~1400 seismographs. A variety of seismic instrumentation was used in these imaging surveys and was obtained from collaborators from around the world, including the Geological Survey of Canada (Ottawa, Canada), IRIS/PASSCAL (Socorro, NM), Lamont-Doherty Earth Observatory (Palisades, NY), Stanford University (Stanford, CA), SCEC (Los Angeles, CA), USGS (Menlo Park, CA, and Woods Hole, MA), University of Texas at El Paso (El Paso, TX), GeoForschungsZentrum (Potsdam, Germany), University of Karlsruhe (Karlsruhe, Germany), and University of Copenhagen (Copenhagen, Denmark). The reader is referred to Table 1 for instrumentation used in LARSE II.

  20. A survey of the 158 micron forbidden C II fine-structure line in the central 50 parsecs of the Galaxy

    NASA Technical Reports Server (NTRS)

    Poglitsch, A.; Geis, N.; Haggerty, M.; Jackson, J.; Stacey, G. J.

    1991-01-01

    NASA's Kuiper Airborne Observatory has been used to conduct an extensive, velocity-resolved survey at 1-arcsec resolution of the 158-micron forbidden C II fine-structure line emission in the central 50 pc of the Galaxy. The emission is found to be strongest toward the rotating circumnuclear disk surrounding Sgr A West; a continuous bridge of the emission connects the Sgr A complex to the thermal radio filaments in the radio arc 10 arcmin north of the center. This suggests a direct physical connection. The brightest emission occurs preferentially near the edges of the massive Galactic center molecular clouds. It is concluded that these clouds are predominantly ionized by external UV photons.

  1. A survey of the 158 micron forbidden C II fine-structure line in the central 50 parsecs of the Galaxy

    NASA Technical Reports Server (NTRS)

    Poglitsch, A.; Geis, N.; Haggerty, M.; Jackson, J.; Stacey, G. J.

    1991-01-01

    NASA's Kuiper Airborne Observatory has been used to conduct an extensive, velocity-resolved survey at 1-arcsec resolution of the 158-micron forbidden C II fine-structure line emission in the central 50 pc of the Galaxy. The emission is found to be strongest toward the rotating circumnuclear disk surrounding Sgr A West; a continuous bridge of the emission connects the Sgr A complex to the thermal radio filaments in the radio arc 10 arcmin north of the center. This suggests a direct physical connection. The brightest emission occurs preferentially near the edges of the massive Galactic center molecular clouds. It is concluded that these clouds are predominantly ionized by external UV photons.

  2. Survey of the seroprovalence of HTLV I/II in hemodialysis patients and blood donors in Urmia.

    PubMed

    Khameneh, Zakieh Rostamzadeh; Baradaran, Mohammad; Sepehrvand, Nariman

    2008-09-01

    Human T lymphocytotropic virus HTLV is a virus from retroviridae family, and more than 20 million people are infected with this virus worldwide. It can cause leukemia/lymphoma in adults, tropical spastic paralysis, HTLV associated myelopathy, spastic paraparesis, tropical myelopathy (HAM/TSP), and some other nervous system diseases. It is transmitted by means of blood products via blood transfusion. In Iran, except the Great Khorasan region, none of blood products undergo screening for HTLV. Immunodeficiency in HD patients, results in increased risk of infection. The aim of this study was to determine the prevalence of anti-HTLV-I/II antibody among hemo-dialysis patients and healthy blood donors in Urmia, Iran. A cross-sectional study was conducted from April 2005 to January 2006 among healthy blood donors and in 2006 among hemodialysis patients. The serum of 2046 blood donors and 95 Hemodialysis patients was checked with enzyme-linked immunosorbent assay (ELISA) for anti HTLV-I/II, and positive cases were confirmed by western blot. Three seropositive cases among 95 hemodialysis patients were detected, and only one of them was confirmed by western blot. Of the healthy blood donors 1910 (93.4%) were males and 136 (6.6%) were females. Serum of 1997 (97.6%) subjects was negative, and 49 (2.6%) cases were positive for HTLV by ELISA. Among the positive cases western blot confirmed only 7 (14.3%) persons as HTLV positive, 37 (75.5%) as negative, and 5 (10.2%) as indeterminate. Among the 7 positive cases 6 (85.6%) were infected with HTLV-I, and only one (14.3%) with HTLV-I /II infection. Total Serologic prevalence of HTLV in healthy blood donors was 0.34%. We conclude that such high serologic prevalence in the population of blood donors in Urmia city, suggests the high probability of transmission through blood transfusion, and therefore screening of blood donors for human T-lymphocyte virus is essential in this region. HD patients should be screened for HTLV and positive

  3. An empirical mass-loss law for Population II giants from the Spitzer-IRAC survey of Galactic globular clusters

    NASA Astrophysics Data System (ADS)

    Origlia, L.; Ferraro, F. R.; Fabbri, S.; Fusi Pecci, F.; Dalessandro, E.; Rich, R. M.; Valenti, E.

    2014-04-01

    Aims: The main aim of the present work is to derive an empirical mass-loss (ML) law for Population II stars in first and second ascent red giant branches. Methods: We used the Spitzer InfraRed Array Camera (IRAC) photometry obtained in the 3.6-8 μm range of a carefully chosen sample of 15 Galactic globular clusters spanning the entire metallicity range and sampling the vast zoology of horizontal branch (HB) morphologies. We complemented the IRAC photometry with near-infrared data to build suitable color-magnitude and color-color diagrams and identify mass-losing giant stars. Results: We find that while the majority of stars show colors typical of cool giants, some stars show an excess of mid-infrared light that is larger than expected from their photospheric emission and that is plausibly due to dust formation in mass flowing from them. For these stars, we estimate dust and total (gas + dust) ML rates and timescales. We finally calibrate an empirical ML law for Population II red and asymptotic giant branch stars with varying metallicity. We find that at a given red giant branch luminosity only a fraction of the stars are losing mass. From this, we conclude that ML is episodic and is active only a fraction of the time, which we define as the duty cycle. The fraction of mass-losing stars increases by increasing the stellar luminosity and metallicity. The ML rate, as estimated from reasonable assumptions for the gas-to-dust ratio and expansion velocity, depends on metallicity and slowly increases with decreasing metallicity. In contrast, the duty cycle increases with increasing metallicity, with the net result that total ML increases moderately with increasing metallicity, about 0.1 M⊙ every dex in [Fe/H]. For Population II asymptotic giant branch stars, we estimate a total ML of ≤0.1 M⊙, nearly constant with varying metallicity. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory

  4. Cefepime and amikacin as empirical therapy in patients with febrile neutropaenia: a single-centre phase II prospective survey.

    PubMed

    Mebis, J; Vandeplassche, S; Goossens, H; Berneman, Z N

    2009-01-01

    The aim of the survey was to prospectively evaluate the effectiveness of the combination therapy cefepime and amikacin in the initial treatment of haematology patients with febrile neutropaenia. Two hundred twenty (220) episodes of febrile neutropaenia were analysed in 54 males and 82 females (median age 58 years), most patients had a severe neutropaenia with in 72% of all periods a neutrophil count of less than 100. Microbiological infection was confirmed in 72 cases (32.8%). Sixty-one (61) bacteria were isolated from blood cultures of which 22 were identified as Gram-negative bacteria and 38 as Gram-positive bacteria. Sixty-three (63) episodes (28.6%) were clinically documented, 85 episodes (38.6%) were fever of unknown origin. Clinical cure was achieved in 123 febrile episodes (56%) after initiation of the current antibiotic protocol; another 22 patients (10%) became afebrile after modifying the initial antibiotic regimen 48 hours or longer after treatment initiation. In 61 cases (27.7%) there was persistent fever or re-occurrence of fever, these cases were considered as treatment failure. Eight patients (3.6%) died during the study. This survey has demonstrated that the combination therapy with cefepime and amikacin can be considered as an effective treatment for febrile neutropaenia in high-risk haematological patients in our centre with a high incidence of resistance to Gram-negative bacteria.

  5. Large Magellanic Cloud Near-infrared Synoptic Survey. II. The Wesenheit Relations and Their Application to the Distance Scale

    NASA Astrophysics Data System (ADS)

    Bhardwaj, Anupam; Kanbur, Shashi M.; Macri, Lucas M.; Singh, Harinder P.; Ngeow, Chow-Choong; Wagner-Kaiser, R.; Sarajedini, Ata

    2016-04-01

    We present new near-infrared (NIR) Cepheid period-Wesenheit (P-W) relations in the LMC using time-series observations from the Large Magellanic Cloud NIR Synoptic Survey. We also derive optical+NIR P-W relations using V and I magnitudes from the Optical Gravitational Lensing Experiment. We employ our new JHKs data to determine an independent distance to the LMC of {μ }{{LMC}}\\=\\18.47+/- 0.07(statistical) mag, using an absolute calibration of the Galactic relations based on several distance determination methods and accounting for the intrinsic scatter of each technique. We also derive new NIR period-luminosity and Wesenheit relations for Cepheids in M31 using observations from the Panchromatic Hubble Andromeda Treasury survey. We use the absolute calibrations of the Galactic and LMC {W}J,H relations to determine the distance modulus of M31, {μ }{{M31}}\\=\\24.46+/- 0.20 mag. We apply a simultaneous fit to Cepheids in several Local Group galaxies covering a range of metallicities (7.7\\lt 12+{log}[{{O}}/{{H}}]\\lt 8.6 dex) to determine a global slope of -3.244 ± 0.016 mag dex-1 for the {W}J,{Ks} relation and obtain robust distance estimates. Our distances are in good agreement with recent TRGB based distance estimates and we do not find any evidence for a metallicity dependence in the NIR P-W relations.

  6. Phase II Characterization Survey of the USNS Bridge (T-AOE 10), Military Sealift Fleet Support Command, Naval Station, Norfolk, Virginia

    SciTech Connect

    ALTIC, NICK A

    2012-08-30

    In March 2011, the USNS Bridge was deployed off northeastern Honshu, Japan with the carrier USS Ronald Reagan to assist with relief efforts after the 2011 Tōhoku earthquake and tsunami. During that time, the Bridge was exposed to air-borne radioactive materials leaking from the damaged Fukushima I Nuclear Power Plant. The proximity of the Bridge to the air-borne impacted area resulted in the contamination of the ship’s air-handling systems and the associated components, as well as potential contamination of other ship surfaces due to either direct intake/deposition or inadvertent spread from crew/operational activities. Preliminary surveys in the weeks after the event confirmed low-level contamination within the heating, ventilation, and air conditioning (HVAC) ductwork and systems, and engine and other auxiliary air intake systems. Some partial decontamination was performed at that time. In response to the airborne contamination event, Military Sealift Fleet Support Command (MSFSC) contracted Oak Ridge Associated Universities (ORAU), under provisions of the Oak Ridge Institute for Science and Education (ORISE) contract, to assess the radiological condition of the Bridge. Phase I identified contamination within the CPS filters, ventilation systems, miscellaneous equipment, and other suspect locations that could not accessed at that time (ORAU 2011b). Because the Bridge was underway during the characterization, all the potentially impacted systems/spaces could not be investigated. As a result, MSFSC contracted with ORAU to perform Phase II of the characterization, specifically to survey systems/spaces previously inaccessible. During Phase II of the characterization, the ship was in port to perform routine maintenance operations, allowing access to the previously inaccessible systems/spaces.

  7. An optical spectroscopic survey of the 3CR sample of radio galaxies with z < 0.3. V. Implications for the unified model for FR IIs

    NASA Astrophysics Data System (ADS)

    Baldi, Ranieri D.; Capetti, Alessandro; Buttiglione, Sara; Chiaberge, Marco; Celotti, Annalisa

    2013-12-01

    We explore the implications of our optical spectroscopic survey of 3CR radio sources with z < 0.3 for the unified model (UM) for radio-loud AGN, focusing on objects with a "edge-brightened" (FR II) radio morphology. The sample contains 33 high ionization galaxies (HIGs) and 18 broad line objects (BLOs). According to the UM, HIGs, the narrow line sources, are the nuclearly obscured counterparts of BLOs. The fraction of HIGs indicates a covering factor of the circumnuclear matter of 65% that corresponds, adopting a torus geometry, to an opening angle of 50° ± 5. No dependence on redshift and luminosity on the torus opening angle emerges. We also consider the implications for a "clumpy" torus. The distributions of total radio luminosity of HIGs and BLOs are not statistically distinguishable, as expected from the UM. Conversely, BLOs have a radio core dominance, R, more than ten times larger with respect to HIGs, as expected in case of Doppler boosting when the jets in BLOs are preferentially oriented closer to the line of sight than in HIGs. Modeling the R distributions leads to an estimate of the jet bulk Lorentz factor of Γ ~ 3-5. The test of the UM based on the radio source size is not conclusive due to the limited number of objects and because the size distribution is dominated by the intrinsic scatter rather than by projection effects. The [O II] line luminosities in HIGs and BLOs are similar but the [O III] and [O I] lines are higher in BLOs by a factor of ~2. We ascribe this effect to the presence of a line emitting region located within the walls of the obscuring torus, visible in BLOs but obscured in HIGs, with a density higher than the [O II] critical density. We find evidence that BLOs have broader [O I] and [O III] lines than HIGs of similar [O II] width, as expected in the presence of high density gas in the proximity of the central black hole. In conclusion, the radio and narrow line region (NLR) properties of HIGs and BLOs are consistent with the UM

  8. Constraints on the Geometry of the Obscuring Torus from the NuSTAR Survey of the Local Seyfert II Population

    NASA Astrophysics Data System (ADS)

    Balokovic, Mislav; Harrison, Fiona; Brightman, Murray

    2017-08-01

    The obscuring torus is one of the main components of the basic unified model of active galactic nuclei (AGN), needed to create anisotropy in obscuration as a function of the viewing angle. We present the first study of the geometrical properties of the AGN torus in a large and representative sample of type II Seyfert nuclei. The sample consists of 124 AGN selected in the hard X-ray band from the Swift/BAT 70-month catalog and observed simultaneously with NuSTAR and Swift/XRT. These data enable us to explore the constraints that observed spectra place on the properties of the obscuring torus in individual AGN and in the local population of Seyfert II nuclei. We make use of empirically motivated spectral models for X-ray reprocessing in approximately toroidal geometry for constraining the distribution of the average column density of the torus, and the distribution of the torus covering factor within this sample. We find that the torus-averaged column density is independent of the line-of-sight column density, with typical column density that is borderline Compton-thick, i.e., around the unity optical depth for Compton scattering. The distribution of torus covering factors is broad but shows a preference for high covering, peaking around the covering factor of 90%, with the median at 70%, in agreement with recent sample studies in the infrared band. We also examine the dependence of the covering factor on intrinsic luminosity, finding that the median covering factor peaks around the intrinsic X-ray luminosity of 10^42.5 erg/s and decreases toward both lower and higher luminosities.

  9. PROBING THE PHYSICS OF NARROW LINE REGIONS IN ACTIVE GALAXIES. II. THE SIDING SPRING SOUTHERN SEYFERT SPECTROSCOPIC SNAPSHOT SURVEY (S7)

    SciTech Connect

    Dopita, Michael A.; Davies, Rebecca; Kewley, Lisa; Hampton, Elise; Sutherland, Ralph; Shastri, Prajval; Kharb, Preeti; Jose, Jessy; Bhatt, Harish; Ramya, S.; Scharwächter, Julia; Jin, Chichuan; Banfield, Julie; Zaw, Ingyin; Juneau, Stéphanie; Srivastava, Shweta

    2015-03-15

    Here we describe the Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7) and present results on 64 galaxies drawn from the first data release. The S7 uses the Wide Field Spectrograph mounted on the ANU 2.3 m telescope located at the Siding Spring Observatory to deliver an integral field of 38 × 25 arcsec at a spectral resolution of R = 7000 in the red (530–710 nm), and R = 3000 in the blue (340–560 nm). From these data cubes we have extracted the narrow-line region spectra from a 4 arcsec aperture centered on the nucleus. We also determine the Hβ and [O iii] λ5007 fluxes in the narrow lines, the nuclear reddening, the reddening-corrected relative intensities of the observed emission lines, and the Hβ and [O iii] λ5007 luminosities determined from spectra for which the stellar continuum has been removed. We present a set of images of the galaxies in [O iii] λ5007, [N ii] λ6584, and Hα, which serve to delineate the spatial extent of the extended narrow-line region and also to reveal the structure and morphology of the surrounding H ii regions. Finally, we provide a preliminary discussion of those Seyfert 1 and Seyfert 2 galaxies that display coronal emission lines in order to explore the origin of these lines.

  10. The ROSAT-ESO flux limited X-ray galaxy cluster survey (REFLEX II). I. Newly identified X-ray luminous clusters at z ≥ 0.2

    NASA Astrophysics Data System (ADS)

    Chon, G.; Böhringer, H.

    2012-02-01

    We report 19 intermediate redshift clusters newly detected in the ROSAT All-Sky survey that are spectroscopically confirmed. They form a part of 911 objects in the REFLEX II cluster catalogue with a limiting flux of 1.8 × 10-12 erg/s/cm2 in the 0.1-2.4 keV ROSAT band at redshift z ≥ 0.2. In addition we report three clusters from the REFLEX III supplementary catalogue, which contains objects below the REFLEX II flux limit but satisfies the redshift constraint above. These clusters are spectroscopically followed-up by our ESO NTT-EFOSC2 campaigns for the redshift measurement. We describe our observing and data reduction methods. We show how X-ray properties such as spectral hardness ratio and source extent can be used as important diagnostics in selecting galaxy cluster candidates. Physical properties of the clusters are subsequently calculated from the X-ray observations. This sample contains the high mass and intermediate-redshift galaxy clusters for astrophysical and cosmological applications. Based on the data obtained at the European Southern Observatory, La Silla, Chile.

  11. Probing the Physics of Narrow Line Regions in Active Galaxies. II. The Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7)

    NASA Astrophysics Data System (ADS)

    Dopita, Michael A.; Shastri, Prajval; Davies, Rebecca; Kewley, Lisa; Hampton, Elise; Scharwächter, Julia; Sutherland, Ralph; Kharb, Preeti; Jose, Jessy; Bhatt, Harish; Ramya, S.; Jin, Chichuan; Banfield, Julie; Zaw, Ingyin; Juneau, Stéphanie; James, Bethan; Srivastava, Shweta

    2015-03-01

    Here we describe the Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7) and present results on 64 galaxies drawn from the first data release. The S7 uses the Wide Field Spectrograph mounted on the ANU 2.3 m telescope located at the Siding Spring Observatory to deliver an integral field of 38 × 25 arcsec at a spectral resolution of R = 7000 in the red (530-710 nm), and R = 3000 in the blue (340-560 nm). From these data cubes we have extracted the narrow-line region spectra from a 4 arcsec aperture centered on the nucleus. We also determine the Hβ and [O iii] λ5007 fluxes in the narrow lines, the nuclear reddening, the reddening-corrected relative intensities of the observed emission lines, and the Hβ and [O iii] λ5007 luminosities determined from spectra for which the stellar continuum has been removed. We present a set of images of the galaxies in [O iii] λ5007, [N ii] λ6584, and Hα, which serve to delineate the spatial extent of the extended narrow-line region and also to reveal the structure and morphology of the surrounding H ii regions. Finally, we provide a preliminary discussion of those Seyfert 1 and Seyfert 2 galaxies that display coronal emission lines in order to explore the origin of these lines.

  12. CONTINUUM HALOS IN NEARBY GALAXIES: AN EVLA SURVEY (CHANG-ES). II. FIRST RESULTS ON NGC 4631

    SciTech Connect

    Irwin, Judith; Henriksen, Richard N.; Beck, Rainer; Krause, Marita; Mora, Silvia Carolina; Schmidt, Philip; Benjamin, R. A.; Dettmar, Ralf-Juergen; Miskolczi, Arpad; English, Jayanne; Heald, George; Oosterloo, Tom; Johnson, Megan; Li, Jiang-Tao; Murphy, E. J.; Porter, Troy A.; Rand, Richard J.; Saikia, D. J.; Strong, A. W.; Walterbos, Rene E-mail: henriksn@astro.queensu.ca E-mail: rbeck@mpifr-bonn.mpg.de E-mail: cmora@mpifr-bonn.mpg.de; and others

    2012-08-15

    We present the first results from the Continuum Halos in Nearby Galaxies-an EVLA Survey (CHANG-ES), a new survey of 35 edge-on galaxies to search for both in-disk and extraplanar radio continuum emission. CHANG-ES is exploiting the new wide-band, multi-channel capabilities of the Karl G. Jansky Very Large Array (i.e., the Expanded Very Large Array or EVLA) with observations in two bands centered at 1.5 and 6 GHz in a variety of array configurations with full polarization. The motivation and science case for the survey are presented in a companion paper (Paper I). These first results are based on C-array test observations in both observing bands of the well-known radio halo galaxy, NGC 4631. In this paper, we outline the observations and the data reduction steps that are required for wide-band calibration and mapping of EVLA data, including polarization. With modest on-source observing times (30 minutes at 1.5 GHz and 75 minutes at 6 GHz for the test data), we have achieved best rms noise levels of 22 and 3.5 {mu}Jy beam{sup -1} at 1.5 GHz and 6 GHz, respectively. New disk-halo features have been detected, among them two at 1.5 GHz that appear as loops in projection. We present the first 1.5 GHz spectral index map of NGC 4631 to be formed from a single wide-band observation in a single array configuration. This map represents tangent slopes to the intensities within the band centered at 1.5 GHz, rather than fits across widely separated frequencies as has been done in the past and is also the highest spatial resolution spectral index map yet presented for this galaxy. The average spectral index in the disk is {alpha}-bar{sub 1.5GHz} = -0.84 {+-} 0.05 indicating that the emission is largely non-thermal, but a small global thermal contribution is sufficient to explain a positive curvature term in the spectral index over the band. Two specific star-forming regions have spectral indices that are consistent with thermal emission. Polarization results (uncorrected for

  13. Continuum Halos in Nearby Galaxies: An EVLA Survey (CHANG-ES). II. First Results on NGC 4631

    NASA Astrophysics Data System (ADS)

    Irwin, Judith; Beck, Rainer; Benjamin, R. A.; Dettmar, Ralf-Jürgen; English, Jayanne; Heald, George; Henriksen, Richard N.; Johnson, Megan; Krause, Marita; Li, Jiang-Tao; Miskolczi, Arpad; Mora, Silvia Carolina; Murphy, E. J.; Oosterloo, Tom; Porter, Troy A.; Rand, Richard J.; Saikia, D. J.; Schmidt, Philip; Strong, A. W.; Walterbos, Rene; Wang, Q. Daniel; Wiegert, Theresa

    2012-08-01

    We present the first results from the Continuum Halos in Nearby Galaxies—an EVLA Survey (CHANG-ES), a new survey of 35 edge-on galaxies to search for both in-disk and extraplanar radio continuum emission. CHANG-ES is exploiting the new wide-band, multi-channel capabilities of the Karl G. Jansky Very Large Array (i.e., the Expanded Very Large Array or EVLA) with observations in two bands centered at 1.5 and 6 GHz in a variety of array configurations with full polarization. The motivation and science case for the survey are presented in a companion paper (Paper I). These first results are based on C-array test observations in both observing bands of the well-known radio halo galaxy, NGC 4631. In this paper, we outline the observations and the data reduction steps that are required for wide-band calibration and mapping of EVLA data, including polarization. With modest on-source observing times (30 minutes at 1.5 GHz and 75 minutes at 6 GHz for the test data), we have achieved best rms noise levels of 22 and 3.5 μJy beam-1 at 1.5 GHz and 6 GHz, respectively. New disk-halo features have been detected, among them two at 1.5 GHz that appear as loops in projection. We present the first 1.5 GHz spectral index map of NGC 4631 to be formed from a single wide-band observation in a single array configuration. This map represents tangent slopes to the intensities within the band centered at 1.5 GHz, rather than fits across widely separated frequencies as has been done in the past and is also the highest spatial resolution spectral index map yet presented for this galaxy. The average spectral index in the disk is \\bar{\\alpha }_{1.5 \\,GHz} =-0.84+/- 0.05 indicating that the emission is largely non-thermal, but a small global thermal contribution is sufficient to explain a positive curvature term in the spectral index over the band. Two specific star-forming regions have spectral indices that are consistent with thermal emission. Polarization results (uncorrected for internal

  14. Properties of the H II Region Populations of M51 and NGC 4449 from Hα Images with the Advanced Camera for Surveys on the Hubble Space Telescope

    NASA Astrophysics Data System (ADS)

    Gutiérrez, Leonel; Beckman, John E.; Buenrostro, Valeria

    2011-04-01

    We have used images from the Advanced Camera for Surveys on the Hubble Space Telescope in Hα, and in the neighboring continuum, to produce flux-calibrated images of the large spiral galaxy M51 and the dwarf irregular NGC 4449. From these images, we have derived the absolute luminosities in Hα, the areas, and the positions with respect to the galactic centers as reference points of over 2600 H II regions in M51 and over 270 H II regions in NGC 4449. Using this database, we have derived luminosity-volume (L-V) relations for the regions in the two galaxies, showing that within the error limits these obey the equation L ~ V 2/3, which differs from the linear relation expected for regions of constant uniform electron density. We briefly discuss possible models which would give rise to this behavior—notably models with strong density inhomogeneities within the regions. Plotting the luminosity functions for the two galaxies, we find a break in the slope for M51 at log(L) = 38.5 dex (units in erg s-1) for M51 in good agreement with the previous ground-based study by Rand, and above this luminosity NGC 4449 also shows a sharp decline in its luminosity function, although the number of regions is too small to plot the function well at higher luminosities. The cumulative diameter distribution for the H II regions of M51 shows dual behavior, with a break at a radius close to 100 pc, the radius of regions with the break luminosity. Here too we indicate possible physical implications.

  15. The ACS Nearby Galaxy Survey Treasury. II. Young Stars and their Relation to Hα and UV Emission Timescales in the M81 Outer Disk

    NASA Astrophysics Data System (ADS)

    Gogarten, Stephanie M.; Dalcanton, Julianne J.; Williams, Benjamin F.; Seth, Anil C.; Dolphin, Andrew; Weisz, Daniel; Skillman, Evan; Holtzman, Jon; Cole, Andrew; Girardi, Leo; de Jong, Roelof S.; Karachentsev, Igor D.; Olsen, Knut; Rosema, Keith

    2009-01-01

    We have obtained resolved stellar photometry from Hubble Space Telescope Advanced Camera for Surveys observations of a field in the outer disk of M81 as part of ANGST. Motivated by the recent discovery of extended UV disks around many nearby spiral galaxies, we use the observed stellar population to derive the recent star formation histories of five ~ 0.5 kpc-sized regions within this field. These regions were selected on the basis of their UV luminosity from GALEX and include two H II regions, two regions that are UV-bright but Hα-faint, and one "control" region faint in both UV and Hα. We estimate our effective star formation rate detection limit at ~2 × 10-4 M sun yr-1, which is lower than that of GALEX for regions of this size. As expected, the H II regions contain massive main-sequence stars (in the mass range 18-27 M sun, based on our best extinction estimates), while similar massive main-sequence stars are lacking in the UV-bright/Hα-faint regions. The observations are consistent with stellar ages lsim 10 Myr in the H II regions, and gsim 16 Myr in the UV-bright/Hα-faint regions. All regions but the control have formed ~ 104 M sun of stars over the past ~ 65 Myr. Thus, our results, for at least one small area in the outer disk of M81, are consistent with an age difference being sufficient to explain the observed discrepancy between star forming regions detected in Hα and those detected exclusively in UV. However, our data cannot conclusively rule out other explanations, such as a strongly truncated initial mass function.

  16. Spectral analysis of the Stromlo-APM Survey - II. Galaxy luminosity function and clustering by spectral type

    NASA Astrophysics Data System (ADS)

    Loveday, J.; Tresse, L.; Maddox, S.

    1999-11-01

    We study the luminosity function and clustering properties of subsamples of local galaxies selected from the Stromlo-APM Survey by the rest-frame equivalent widths of their Hα and [Oii] emission lines. The bJ luminosity function of star-forming galaxies has a significantly steeper faint-end slope than that for quiescent galaxies: the majority of sub-L* galaxies are currently undergoing significant star formation. Emission-line galaxies are less strongly clustered, both amongst themselves and with the general galaxy population, than are quiescent galaxies. Thus as well as being less luminous, star-forming galaxies also inhabit lower density regions of the Universe than quiescent galaxies.

  17. The Gould’s Belt Distances Survey (GOBELINS) II. Distances and Structure toward the Orion Molecular Clouds

    NASA Astrophysics Data System (ADS)

    Kounkel, Marina; Hartmann, Lee; Loinard, Laurent; Ortiz-León, Gisela N.; Mioduszewski, Amy J.; Rodríguez, Luis F.; Dzib, Sergio A.; Torres, Rosa M.; Pech, Gerardo; Galli, Phillip A. B.; Rivera, Juana L.; Boden, Andrew F.; Evans, Neal J., II; Briceño, Cesar; Tobin, John J.

    2017-01-01

    We present the results of the Gould’s Belt Distances Survey of young star-forming regions toward the Orion Molecular Cloud Complex. We detected 36 young stellar objects (YSOs) with the Very Large Baseline Array, 27 of which have been observed in at least three epochs over the course of two years. At least half of these YSOs belong to multiple systems. We obtained parallax and proper motions toward these stars to study the structure and kinematics of the Complex. We measured a distance of 388 ± 5 pc toward the Orion Nebula Cluster, 428 ± 10 pc toward the southern portion L1641, 388 ± 10 pc toward NGC 2068, and roughly ∼420 pc toward NGC 2024. Finally, we observed a strong degree of plasma radio scattering toward λ Ori.

  18. [A survey on condition of outpatients at prosthodontics II, University Hospital, Faculty of Dentistry, Tokyo Medical and Dental University].

    PubMed

    Sugawara, N; Shiozawa, I; Masuda, T; Takei, H; Tsuruta, J; Ogura, N; Hasegawa, S

    1998-06-01

    The number of dental patients who have medical illnesses is increasing at the hospital of the Faculty of Dentistry, Tokyo Medical and Dental University. Although prosthodontic treatments are considered less invasive in all dental treatments, invasive procedures such as tooth extraction may be required occasionally. Therefore, it is necessary to treat patients in consideration of their condition. Under this situation, a clinical survey was conducted by health questionnaires answered by the patients who visited our clinic between October 1992 and March 1997. The number of patients whose illness was heart disease, hypertension, diabetes, nephritic disease, hepatitis, tuberculosis, hemodyscrasia, asthma, epilepsy, and so on during dental treatment was higher than the national average according to the Ministry of Health and Welfare. Dental psychosomatic diseases such as TMD and dental phobia were increased every year. These data reflect the contemporary disease structure in Japan characterized by the spreading of life-style related diseases and increase of neuropsychological and infectious diseases.

  19. OBSERVATIONS OF BINARY STARS WITH THE DIFFERENTIAL SPECKLE SURVEY INSTRUMENT. II. HIPPARCOS STARS OBSERVED IN 2010 JANUARY AND JUNE

    SciTech Connect

    Horch, Elliott P.; Gomez, Shamilia C.; Anderson, Lisa M.; Sherry, William H.; Howell, Steve B.; Ciardi, David R.; Van Altena, William F. E-mail: shamilia.gomez@gmail.com E-mail: wsherry@noao.edu E-mail: ciardi@ipac.caltech.edu

    2011-02-15

    The results of 497 speckle observations of Hipparcos stars and selected other targets are presented. Of these, 367 were resolved into components and 130 were unresolved. The data were obtained using the Differential Speckle Survey Instrument at the WIYN 3.5 m Telescope. (The WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, Yale University, and the National Optical Astronomy Observatories.) Since the first paper in this series, the instrument has been upgraded so that it now uses two electron-multiplying CCD cameras. The measurement precision obtained when comparing to ephemeris positions of binaries with very well known orbits is approximately 1-2 mas in separation and better than 0.{sup 0}6 in position angle. Differential photometry is found to be in very good agreement with Hipparcos measures in cases where the comparison is most relevant. We derive preliminary orbits for two systems.

  20. [Hungarian Diet and Nutritional Status Survey - OTÁP2014. II. Energy and macronutrient intake of the Hungarian population].

    PubMed

    Sarkadi Nagy, Eszter; Bakacs, Márta; Illés, Éva; Nagy, Barbara; Varga, Anita; Kis, Orsolya; Schreiberné Molnár, Erzsébet; Martos, Éva

    2017-04-01

    The aim of the study was to assess and monitor the dietary habits and nutrient intake of Hungarian adults. Three-day dietary records were used for dietary assessment, the sample was representative for the Hungarian population aged ≥18ys by gender and age. The mean proportion of energy from fat was higher (men: 38 energy%, women: 37 energy%), that from carbohydrates was lower (men: 45 energy%, women: 47 energy%) than recommended, the protein intake is adequate. Unfavorable change compared to the previous survey in 2009 was the increase of fat and saturated fatty acid energy percent in women, the decrease in fruit and vegetable consumption, which explains the decreased fiber intake. An increasing trend in added sugar energy percent in each age groups of both genders was observed compared to 2009. Interventions focusing on the promotion of fruit and vegetable consumption and decreasing of saturated fat and added sugar intake are needed. Orv. Hetil., 2017, 158(15), 587-597.

  1. NuSTAR Hard X-Ray Survey of the Galactic Center Region. II. X-Ray Point Sources

    NASA Astrophysics Data System (ADS)

    Hong, JaeSub; Mori, Kaya; Hailey, Charles J.; Nynka, Melania; Zhang, Shuo; Gotthelf, Eric; Fornasini, Francesca M.; Krivonos, Roman; Bauer, Franz; Perez, Kerstin; Tomsick, John A.; Bodaghee, Arash; Chiu, Jeng-Lun; Clavel, Maïca; Stern, Daniel; Grindlay, Jonathan E.; Alexander, David M.; Aramaki, Tsuguo; Baganoff, Frederick K.; Barret, Didier; Barrière, Nicolas; Boggs, Steven E.; Canipe, Alicia M.; Christensen, Finn E.; Craig, William W.; Desai, Meera A.; Forster, Karl; Giommi, Paolo; Grefenstette, Brian W.; Harrison, Fiona A.; Hong, Dooran; Hornstrup, Allan; Kitaguchi, Takao; Koglin, Jason E.; Madsen, Kristen K.; Mao, Peter H.; Miyasaka, Hiromasa; Perri, Matteo; Pivovaroff, Michael J.; Puccetti, Simonetta; Rana, Vikram; Westergaard, Niels J.; Zhang, William W.; Zoglauer, Andreas

    2016-07-01

    We present the first survey results of hard X-ray point sources in the Galactic Center (GC) region by NuSTAR. We have discovered 70 hard (3-79 keV) X-ray point sources in a 0.6 deg{}2 region around Sgr A* with a total exposure of 1.7 Ms, and 7 sources in the Sgr B2 field with 300 ks. We identify clear Chandra counterparts for 58 NuSTAR sources and assign candidate counterparts for the remaining 19. The NuSTAR survey reaches X-ray luminosities of ˜4× and ˜8 × 10{}32 erg s{}-1 at the GC (8 kpc) in the 3-10 and 10-40 keV bands, respectively. The source list includes three persistent luminous X-ray binaries (XBs) and the likely run-away pulsar called the Cannonball. New source-detection significance maps reveal a cluster of hard (>10 keV) X-ray sources near the Sgr A diffuse complex with no clear soft X-ray counterparts. The severe extinction observed in the Chandra spectra indicates that all the NuSTAR sources are in the central bulge or are of extragalactic origin. Spectral analysis of relatively bright NuSTAR sources suggests that magnetic cataclysmic variables constitute a large fraction (>40%-60%). Both spectral analysis and logN-logS distributions of the NuSTAR sources indicate that the X-ray spectra of the NuSTAR sources should have kT > 20 keV on average for a single temperature thermal plasma model or an average photon index of Γ = 1.5-2 for a power-law model. These findings suggest that the GC X-ray source population may contain a larger fraction of XBs with high plasma temperatures than the field population.

  2. Molecular-cloud-scale Chemical Composition. II. Mapping Spectral Line Survey toward W3(OH) in the 3 mm Band

    NASA Astrophysics Data System (ADS)

    Nishimura, Yuri; Watanabe, Yoshimasa; Harada, Nanase; Shimonishi, Takashi; Sakai, Nami; Aikawa, Yuri; Kawamura, Akiko; Yamamoto, Satoshi

    2017-10-01

    To study a molecular-cloud-scale chemical composition, we conducted a mapping spectral line survey toward the Galactic molecular cloud W3(OH), which is one of the most active star-forming regions in the Perseus arm. We conducted our survey through the use of the Nobeyama Radio Observatory 45 m telescope, and observed the area of 16‧ × 16‧, which corresponds to 9.0 pc × 9.0 pc. The observed frequency ranges are 87–91, 96–103, and 108–112 GHz. We prepared the spectrum averaged over the observed area, in which eight molecular species (CCH, HCN, HCO+, HNC, CS, SO, C18O, and 13CO) are identified. On the other hand, the spectrum of the W3(OH) hot core observed at a 0.17 pc resolution shows the lines of various molecules such as OCS, H2CS CH3CCH, and CH3CN in addition to the above species. In the spatially averaged spectrum, emission of the species concentrated just around the star-forming core, such as CH3OH and HC3N, is fainter than in the hot core spectrum, whereas emission of the species widely extended over the cloud such as CCH is relatively brighter. We classified the observed area into five subregions according to the integrated intensity of 13CO, and evaluated the contribution to the averaged spectrum from each subregion. The CCH, HCN, HCO+, and CS lines can be seen even in the spectrum of the subregion with the lowest 13CO integrated intensity range (<10 K km s‑1). Thus, the contributions of the spatially extended emission is confirmed to be dominant in the spatially averaged spectrum.

  3. NuSTAR Hard X-Ray Survey of the Galactic Center Region. II. X-Ray Point Sources

    NASA Technical Reports Server (NTRS)

    Hong, Jaesub; Mori, Kaya; Hailey, Charles J.; Nynka, Melania; Zhang, Shou; Gotthelf, Eric; Fornasini, Francesca M.; Krivonos, Roman; Bauer, Franz; Perez, Kerstin; hide

    2016-01-01

    We present the first survey results of hard X-ray point sources in the Galactic Center (GC) region by NuSTAR. We have discovered 70 hard (3-79 keV) X-ray point sources in a 0.6 deg(sup 2) region around Sgr?A* with a total exposure of 1.7 Ms, and 7 sources in the Sgr B2 field with 300 ks. We identify clear Chandra counterparts for 58 NuSTAR sources and assign candidate counterparts for the remaining 19. The NuSTAR survey reaches X-ray luminosities of approx. 4× and approx. 8 ×10(exp 32) erg/s at the GC (8 kpc) in the 3-10 and 10-40 keV bands, respectively. The source list includes three persistent luminous X-ray binaries (XBs) and the likely run-away pulsar called the Cannonball. New source-detection significance maps reveal a cluster of hard (>10 keV) X-ray sources near the Sgr A diffuse complex with no clear soft X-ray counterparts. The severe extinction observed in the Chandra spectra indicates that all the NuSTAR sources are in the central bulge or are of extragalactic origin. Spectral analysis of relatively bright NuSTAR sources suggests that magnetic cataclysmic variables constitute a large fraction (>40%-60%). Both spectral analysis and logN-logS distributions of the NuSTAR sources indicate that the X-ray spectra of the NuSTAR sources should have kT > 20 keV on average for a single temperature thermal plasma model or an average photon index of Lambda = 1.5-2 for a power-law model. These findings suggest that the GC X-ray source population may contain a larger fraction of XBs with high plasma temperatures than the field population.

  4. Do Substance Use Norms and Perceived Drug Availability Mediate Sexual Orientation Differences in Patterns of Substance Use? Results from the California Quality of Life Survey II

    PubMed Central

    Cochran, Susan D.; Grella, Christine E.; Mays, Vickie M.

    2012-01-01

    Objective: Illicit drug and heavy alcohol use is more common among sexual minorities compared with heterosexuals. This difference has sometimes been attributed to more tolerant substance use norms within the gay community, although evidence is sparse. The current study investigated the role of perceived drug availability and tolerant injunctive norms in mediating the linkage between minority sexual orientation status and higher rates of prior-year substance use. Method: We used data from the second California Quality of Life Survey (Cal-QOL II), a followback telephone survey in 2008–2009 of individuals first interviewed in the population-based 2007 California Health Interview Survey. The sample comprised 2,671 individuals, oversampled for minority sexual orientation. Respondents were administered a structured interview assessing past-year alcohol and illicit drug use, perceptions of perceived illicit drug availability, and injunctive norms concerning illicit drug and heavier alcohol use. We used structural equation modeling methods to test a mediational model linking sexual orientation and substance use behaviors via perceptions of drug availability and social norms pertaining to substance use. Results: Compared with heterosexual individuals, sexual minorities reported higher levels of substance use, perceived drug availability, and tolerant social norms. A successfully fitting model suggests that much of the association between minority sexual orientation and substance use is mediated by these sexual orientation–related differences in drug availability perceptions and tolerant norms for substance use. Conclusions: Social environmental context, including subcultural norms and perceived drug availability, is an important factor influencing substance use among sexual minorities and should be addressed in community interventions. PMID:22630806

  5. The Exoplanet Mass-ratio Function from the MOA-II Survey: Discovery of a Break and Likely Peak at a Neptune Mass

    NASA Astrophysics Data System (ADS)

    Suzuki, D.; Bennett, D. P.; Sumi, T.; Bond, I. A.; Rogers, L. A.; Abe, F.; Asakura, Y.; Bhattacharya, A.; Donachie, M.; Freeman, M.; Fukui, A.; Hirao, Y.; Itow, Y.; Koshimoto, N.; Li, M. C. A.; Ling, C. H.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Nagakane, M.; Onishi, K.; Oyokawa, H.; Rattenbury, N.; Saito, To.; Sharan, A.; Shibai, H.; Sullivan, D. J.; Tristram, P. J.; Yonehara, A.; MOA Collaboration

    2016-12-01

    We report the results of the statistical analysis of planetary signals discovered in MOA-II microlensing survey alert system events from 2007 to 2012. We determine the survey sensitivity as a function of planet-star mass ratio, q, and projected planet-star separation, s, in Einstein radius units. We find that the mass-ratio function is not a single power law, but has a change in slope at q ˜ 10-4, corresponding to ˜20 M ⊕ for the median host-star mass of ˜0.6 {M}⊙ . We find significant planetary signals in 23 of the 1474 alert events that are well-characterized by the MOA-II survey data alone. Data from other groups are used only to characterize planetary signals that have been identified in the MOA data alone. The distribution of mass ratios and separations of the planets found in our sample are well fit by a broken power-law model of the form {{dN}}{pl}/{(d{log}qd{log}s)=A(q/{q}{br})}n{s}m {{dex}}-2 for q > q br and {{dN}}{pl}/{(d{log}qd{log}s)=A(q/{q}{br})}p{s}m {{dex}}-2 for q < q br, where q br is the mass ratio of the break. We also combine this analysis with the previous analyses of Gould et al. and Cassan et al., bringing the total sample to 30 planets. This combined analysis yields A={0.61}-0.16+0.21, n = -0.93 ± 0.13, m={0.49}-0.49+0.47, and p={0.6}-0.4+0.5 for q br ≡ 1.7 × 10-4. The unbroken power-law model is disfavored with a p-value of 0.0022, which corresponds to a Bayes factor of 27 favoring the broken power-law model. These results imply that cold Neptunes are likely to be the most common type of planets beyond the snow line.

  6. THE SPITZER SURVEY OF INTERSTELLAR CLOUDS IN THE GOULD BELT. II. THE CEPHEUS FLARE OBSERVED WITH IRAC AND MIPS

    SciTech Connect

    Kirk, Jason M.; Ward-Thompson, Derek; Di Francesco, James E-mail: derek.ward-thompson@astro.cf.ac.uk

    2009-11-01

    We present Spitzer Infrared Array Camera (IRAC; {approx}2 deg{sup 2}) and Multiband Imaging Photometer for Spitzer (MIPS; {approx}8 deg{sup 2}) observations of the Cepheus Flare, which is associated with the Gould Belt, at an approximate distance of {approx}300 pc. Around 6500 sources are detected in all four IRAC bands, of which {approx}900 have MIPS 24 {mu}m detections. We identify 133 young stellar object (YSO) candidates using color-magnitude diagram techniques, and a large number of the YSO candidates are associated with the NGC 7023 reflection nebula. Cross-identifications were made with the Guide Star Catalog II and the IRAS Faint Source Catalog, and spectral energy distributions (SEDs) were constructed. SED modeling was conducted to estimate the degree of infrared excess. It was found that a large majority of disks were optically thick accreting disks, suggesting that there has been little disk evolution in these sources. Nearest-neighbor clustering analysis identified four small protostellar groups (L1228, L1228N, L1251A, and L1251B) with 5-15 members each and the larger NGC 7023 association with 32 YSO members. The star-formation efficiency for cores with clusters of protostars and for those without clusters was found to be {approx}8% and {approx}1%, respectively. The cores L1155, L1241, and L1247 are confirmed to be starless down to our luminosity limit of L {sub bol} = 0.06 L {sub sun}.

  7. Spectroscopic survey of Kepler stars - II. FIES/NOT observations of A- and F-type stars

    NASA Astrophysics Data System (ADS)

    Niemczura, E.; Polińska, M.; Murphy, S. J.; Smalley, B.; Kołaczkowski, Z.; Jessen-Hansen, J.; Uytterhoeven, K.; Lykke, J. M.; Triviño Hage, A.; Michalska, G.

    2017-09-01

    We have analysed high-resolution spectra of 28 A and 22 F stars in the Kepler field, observed using the Fibre-Fed Échelle Spectrograph at the Nordic Optical Telescope. We provide spectral types, atmospheric parameters and chemical abundances for 50 stars. Balmer, Fe i and Fe ii lines were used to derive effective temperatures, surface gravities and microturbulent velocities. We determined chemical abundances and projected rotational velocities using a spectrum synthesis technique. Effective temperatures calculated by spectral energy distribution fitting are in good agreement with those determined from the spectral line analysis. The stars analysed include chemically peculiar stars of the Am and λ Boo types, as well as stars with approximately solar chemical abundances. The wide distribution of projected rotational velocity, vsin i, is typical for A and F stars. The microturbulence velocities obtained are typical for stars in the observed temperature and surface gravity ranges. Moreover, we affirm the results of Niemczura et al. that Am stars do not have systematically higher microturbulent velocities than normal stars of the same temperature.

  8. Evidence for elevated cortical hyperexcitability and its association with out-of-body experiences in the non-clinical population: new findings from a pattern-glare task.

    PubMed

    Braithwaite, Jason J; Broglia, Emma; Bagshaw, Andrew P; Wilkins, Arnold J

    2013-03-01

    Individuals with no history of neurological or psychiatric illness can report hallucinatory Out-of-Body Experiences (OBEs) and display elevated scores on measures of temporal-lobe dysfunction (Braithwaite et al., 2011). However, all previous investigations of such biases in non-clinical populations are based on indirect questionnaire measures. Here we present the first empirical investigation that a non-clinical OBE group is subject to pattern-glare, possibly as a result of cortical hyperexcitability (Wilkins et al., 1984). Fifty-nine students at the University of Birmingham viewed a series of square-wave gratings with spatial frequencies of approximately .7, 3 and 11 cycles-per-degree, both black/white and of contrasting colours. The illusions and discomfort reported when viewing gratings with mid-range spatial frequency have been hypothesized to reflect cortical hyperexcitability (Wilkins, 1995; Huang et al., 2003). Participants also completed the Cardiff Anomalous Perception Scale (CAPS: Bell et al., 2006) which included experiential measures of disruptions in 'Temporal-lobe Experience'. Participants who reported OBEs also reported significantly more visual illusions/distortions and significantly greater discomfort as a result of viewing the mid-frequency gratings. There were no such differences with respect to gratings with relatively lower or higher spatial frequency. The OBE group also produced significantly elevated scores on the CAPS measures of Temporal-lobe Experience, relative to controls. Collectively, the results are consistent with there being a neural 'vulnerability' in the cortices of individuals pre-disposed to some hallucinations, even in the non-clinical population. Copyright © 2011 Elsevier Ltd. All rights reserved.

  9. The VIPERS Multi-Lambda Survey. II. Diving with massive galaxies in 22 square degrees since z = 1.5

    NASA Astrophysics Data System (ADS)

    Moutard, T.; Arnouts, S.; Ilbert, O.; Coupon, J.; Davidzon, I.; Guzzo, L.; Hudelot, P.; McCracken, H. J.; Van Werbaeke, L.; Morrison, G. E.; Le Fèvre, O.; Comte, V.; Bolzonella, M.; Fritz, A.; Garilli, B.; Scodeggio, M.

    2016-05-01

    We investigate the evolution of the galaxy stellar mass function and stellar mass density from redshift z = 0.2 to z = 1.5 of a Ks < 22-selected sample with highly reliable photometric redshifts and over an unprecedentedly large area. Our study is based on near-infrared observations carried out with the WIRCam instrument at CFHT over the footprint of the VIPERS spectroscopic survey and benefits from the high-quality optical photometry from the CFHTLS and ultraviolet observations with the GALEX satellite. The accuracy of our photometric redshifts is σΔz/ (1 + z) < 0.03 and 0.05 for the bright (iAB< 22.5) and faint (iAB > 22.5) samples, respectively. The galaxy stellar mass function is measured with ~760 000 galaxies down to Ks ~ 22 and over an effective area of ~22.4 deg2, the latter of which drastically reduces the statistical uncertainties (i.e. Poissonian error and cosmic variance). We point out the importance of carefully controlling the photometric calibration, whose effect becomes quickly dominant when statistical uncertainties are reduced, which will be a major issue for future cosmological surveys with EUCLID or LSST, for instance. By exploring the rest-frame (NUV-r) vs. (r-Ks) colour-colour diagram with which we separated star-forming and quiescent galaxies, (1) we find that the density of very massive log (M∗/M⊙) > 11.5 galaxies is largely dominated by quiescent galaxies and increases by a factor 2 from z ~ 1 to z ~ 0.2, which allows for additional mass assembly through dry mergers. (2) We also confirm the scenario in which star formation activity is impeded above a stellar mass log(ℳ*SF/M⊙) = 10.64±0.01. This value is found to be very stable at 0.2

  10. The Survey for Ionization in Neutral Gas Galaxies. II. The Star Formation Rate Density of the Local Universe

    NASA Astrophysics Data System (ADS)

    Hanish, D. J.; Meurer, G. R.; Ferguson, H. C.; Zwaan, M. A.; Heckman, T. M.; Staveley-Smith, L.; Bland-Hawthorn, J.; Kilborn, V. A.; Koribalski, B. S.; Putman, M. E.; Ryan-Weber, E. V.; Oey, M. S.; Kennicutt, R. C., Jr.; Knezek, P. M.; Meyer, M. J.; Smith, R. C.; Webster, R. L.; Dopita, M. A.; Doyle, M. T.; Drinkwater, M. J.; Freeman, K. C.; Werk, J. K.

    2006-09-01

    We derive observed Hα and R-band luminosity densities of an H I-selected sample of nearby galaxies using the SINGG sample to be l'Hα=(9.4+/-1.8)×1038 h70 ergs s-1 Mpc-3 for Hα and l'R=(4.4+/-0.7)×1037 h70 ergs s-1 Å-1 Mpc-3 in the R band. This R-band luminosity density is approximately 70% of that found by the Sloan Digital Sky Survey. This leads to a local star formation rate density of log(ρ˙SFR [Msolar yr-1 Mpc-3])=-1.80+0.13-0.07(random)+/-0.03(systematic)+log(h70) after applying a mean internal extinction correction of 0.82 mag. The gas cycling time of this sample is found to be tgas=7.5+1.3-2.1 Gyr, and the volume-averaged equivalent width of the SINGG galaxies is EW(Hα)=28.8+7.2-4.7 Å (21.2+4.2-3.5 Å without internal dust correction). As with similar surveys, these results imply that ρ˙SFR(z) decreases drastically from z~1.5 to the present. A comparison of the dynamical masses of the SINGG galaxies evaluated at their optical limits with their stellar and H I masses shows significant evidence of downsizing: the most massive galaxies have a larger fraction of their mass locked up in stars compared with H I, while the opposite is true for less massive galaxies. We show that the application of the Kennicutt star formation law to a galaxy having the median orbital time at the optical limit of this sample results in a star formation rate decay with cosmic time similar to that given by the ρ˙SFR(z) evolution. This implies that the ρ˙SFR(z) evolution is primarily due to the secular evolution of galaxies, rather than interactions or mergers. This is consistent with the morphologies predominantly seen in the SINGG sample.

  11. The VISTA Carina Nebula Survey. II. Spatial distribution of the infrared-excess-selected young stellar population

    NASA Astrophysics Data System (ADS)

    Zeidler, P.; Preibisch, T.; Ratzka, T.; Roccatagliata, V.; Petr-Gotzens, M. G.

    2016-01-01

    We performed a deep wide-field (6.76 sq. deg) near-infrared survey with the VISTA telescope that covers the entire extent of the Carina nebula complex (CNC). The point-source catalog created from these data contains around four million individual objects down to masses of 0.1 M⊙. We present a statistical study of the large-scale spatial distribution and an investigation of the clustering properties of infrared-excesses objects, which are used to trace disk-bearing young stellar objects (YSOs). A selection based on a near-infrared (J-H) versus (H-Ks) color-color diagram shows an almost uniform distribution over the entire observed area. We interpret this as a result of the very high degree of background contamination that arises from the Carina Nebula's location close to the Galactic plane. Complementing the VISTA near-infrared catalog with Spitzer IRAC mid-infrared photometry improves the situation of the background contamination considerably. We find that a (J-H) versus (Ks- [4.5]) color-color diagram is well suited to tracing the population of YSO-candidates (cYSOs) by their infrared excess. We identify 8781 sources with strong infrared excess, which we consider as cYSOs. This sample is used to investigate the spatial distribution of the cYSOs with a nearest-neighbor analysis. The surface density distribution of cYSOs agrees well with the shape of the clouds as seen in our Herschel far-infrared survey. The strong decline in the surface density of excess sources outside the area of the clouds supports the hypothesis that our excess-selected sample consists predominantly of cYSOs with a low level of background contamination. This analysis allows us to identify 14 groups of cYSOs outside the central area.Our results suggest that the total population of cYSOs in the CNC comprises about 164 000 objects, with a substantial fraction (~35%) located in the northern, still not well studied parts. Our cluster analysis suggests that roughly half of the cYSOs constitute a

  12. The German Environmental Survey 1990/92 (GerES II): sources of personal exposure to volatile organic compounds.

    PubMed

    Hoffmann, K; Krause, C; Seifert, B; Ullrich, D

    2000-01-01

    In the framework of the second German Environmental Survey carried out in the Western part of Germany in 1990/91 (GerES IIa) 113 adults aged 25-69 years were selected at random from the total study population of about 2500 to investigate personal exposure to about 70 volatile organic compounds (VOCs). Each subject wore a diffusive badge-type sampler for 1 week. The VOCs determined included alkanes, aromatics, aliphatic halocarbons, terpenes, and oxygen-containing compounds. Multivariate regression analysis was carried out to determine and quantify the major sources of personal exposure to various VOCs. In this paper, results are given for benzene, and C8- and C9-aromatics. Being subject to environmental tobacco smoke was found to be the most important determinant of benzene exposure, but automobile-related activities such as driving a car or refuelling, were also associated with significantly increased levels of benzene. The major determinant of C8- and C9-aromatics concentrations was occupational exposure. Emissions from paints, lacquers, newspapers, magazines and print-works were also important contributors to C8-aromatics exposure. Renovation, painting and smoking were associated with a significant increase of the exposure to C9-aromatics.

  13. A Deep Proper Motion Catalog Within the Sloan Digital Sky Survey Footprint. II. The White Dwarf Luminosity Function

    NASA Astrophysics Data System (ADS)

    Munn, Jeffrey A.; Harris, Hugh C.; von Hippel, Ted; Kilic, Mukremin; Liebert, James W.; Williams, Kurtis A.; DeGennaro, Steven; Jeffery, Elizabeth; Dame, Kyra; Gianninas, A.; Brown, Warren R.

    2017-01-01

    A catalog of 8472 white dwarf (WD) candidates is presented, selected using reduced proper motions from the deep proper motion catalog of Munn et al. Candidates are selected in the magnitude range 16< r< 21.5 over 980 square degrees, and 16< r< 21.3 over an additional 1276 square degrees, within the Sloan Digital Sky Survey (SDSS) imaging footprint. Distances, bolometric luminosities, and atmospheric compositions are derived by fitting SDSS ugriz photometry to pure hydrogen and helium model atmospheres (assuming surface gravities {log} {\\text{}}g=8). The disk white dwarf luminosity function (WDLF) is constructed using a sample of 2839 stars with 5.5< {M}{bol}< 17, with statistically significant numbers of stars cooler than the turnover in the luminosity function. The WDLF for the halo is also constructed, using a sample of 135 halo WDs with 5< {M}{bol}< 16. We find space densities of disk and halo WDs in the solar neighborhood of 5.5+/- 0.1× {10}-3 {{pc}}-3 and 3.5+/- 0.7× {10}-5 {{pc}}-3, respectively. We resolve the bump in the disk WDLF due to the onset of fully convective envelopes in WDs, and see indications of it in the halo WDLF as well.

  14. Galaxy evolution and large-scale structure in the far-infrared. II - The IRAS faint source survey

    NASA Astrophysics Data System (ADS)

    Lonsdale, Carol J.; Hacking, Perry B.; Conrow, T. P.; Rowan-Robinson, M.

    1990-07-01

    The new IRAS Faint Source Survey data base is used to confirm the conclusion of Hacking et al. (1987) that the 60 micron source counts fainter than about 0.5 Jy lie in excess of predictions based on nonevolving model populations. The existence of an anisotropy between the northern and southern Galactic caps discovered by Rowan-Robinson et al. (1986) and Needham and Rowan-Robinson (1988) is confirmed, and it is found to extend below their sensitivity limit to about 0.3 Jy in 60 micron flux density. The count anisotropy at f(60) greater than 0.3 can be interpreted reasonably as due to the Local Supercluster; however, no one structure accounting for the fainter anisotropy can be easily identified in either optical or far-IR two-dimensional sky distributions. The far-IR galaxy sky distributions are considerably smoother than distributions from the published optical galaxy catalogs. It is likely that structure of the large size discussed here have been discriminated against in earlier studies due to insufficient volume sampling.

  15. The California-Kepler Survey. II. Precise Physical Properties of 2025 Kepler Planets and Their Host Stars

    NASA Astrophysics Data System (ADS)

    Johnson, John Asher; Petigura, Erik A.; Fulton, Benjamin J.; Marcy, Geoffrey W.; Howard, Andrew W.; Isaacson, Howard; Hebb, Leslie; Cargile, Phillip A.; Morton, Timothy D.; Weiss, Lauren M.; Winn, Joshua N.; Rogers, Leslie A.; Sinukoff, Evan; Hirsch, Lea A.

    2017-09-01

    We present stellar and planetary properties for 1305 Kepler Objects of Interest hosting 2025 planet candidates observed as part of the California-Kepler Survey. We combine spectroscopic constraints, presented in Paper I, with stellar interior modeling to estimate stellar masses, radii, and ages. Stellar radii are typically constrained to 11%, compared to 40% when only photometric constraints are used. Stellar masses are constrained to 4%, and ages are constrained to 30%. We verify the integrity of the stellar parameters through comparisons with asteroseismic studies and Gaia parallaxes. We also recompute planetary radii for 2025 planet candidates. Because knowledge of planetary radii is often limited by uncertainties in stellar size, we improve the uncertainties in planet radii from typically 42% to 12%. We also leverage improved knowledge of stellar effective temperature to recompute incident stellar fluxes for the planets, now precise to 21%, compared to a factor of two when derived from photometry. Based on observations obtained at the W. M. Keck Observatory, which is operated jointly by the University of California and the California Institute of Technology. Keck time has been granted by the University of California, and California Institute of Technology, the University of Hawaii, and NASA.

  16. High-Redshift Quasars Found in Sloan Digital Sky Survey Commissioning Data. II. The Spring Equatorial Stripe

    SciTech Connect

    Fan, Xiaohui; Strauss, Michael A.; Schneider, Donald P.; Gunn, James E.; Lupton, Robert H.; Anderson, Scott F.; Voges, Wolfgang; Margon, Bruce; Annis, James; Bahcall, Neta A.

    2000-01-01

    This is the second paper in a series aimed at finding high-redshift quasars from five-color (u{sup '} g{sup '} r{sup '} i{sup '} z{sup '}) imaging data taken along the Celestial Equator by the Sloan Digital Sky Survey (SDSS) during its commissioning phase. In this paper, we present 22 high-redshift quasars (z>3.6) discovered from {approx}250 deg2 of data in the spring Equatorial Stripe, plus photometry for two previously known high-redshift quasars in the same region of the sky. Our success rate in identifying high-redshift quasars is 68%. Five of the newly discovered quasars have redshifts higher than 4.6 (z=4.62, 4.69, 4.70, 4.92, and 5.03). All the quasars have i{sup *} <20.2 with absolute magnitude - 28.8

  17. The Galactic Center Molecular Cloud Survey. II. A lack of dense gas and cloud evolution along Galactic center orbits

    NASA Astrophysics Data System (ADS)

    Kauffmann, Jens; Pillai, Thushara; Zhang, Qizhou; Menten, Karl M.; Goldsmith, Paul F.; Lu, Xing; Guzmán, Andrés E.; Schmiedeke, Anika

    2017-07-01

    We present the first systematic study of the density structure of clouds found in a complete sample covering all major molecular clouds in the central molecular zone (CMZ; inner 200 pc) of the Milky Way. This is made possible with data from the Galactic Center Molecular Cloud Survey (GCMS), which is the first study resolving all major molecular clouds in the CMZ at interferometer angular resolution. We find that many CMZ molecular clouds have unusually shallow density gradients compared to regions elsewhere in the Milky Way. This is possibly a consequence of weak gravitational binding of the clouds. The resulting relative absence of dense gas on spatial scales 0.1 pc is probably one of the reasons why star formation (SF) in dense gas of the CMZ is suppressed by a factor 10, compared to solar neighborhood clouds. Another factor suppressing star formation is the high SF density threshold that likely results from the observed gas kinematics. Further, it is possible but not certain that the star formation activity and cloud density structure evolve systematically as clouds orbit the CMZ.

  18. Completing Subar-HiZELS: a uniquely matched Halpha & [O ii] survey at z=1.5

    NASA Astrophysics Data System (ADS)

    Sobral, David

    2014-01-01

    With HiZELS we have found thousands of distant sources with strong emission lines (mostly Halpha) redshifted into the JHK bands using existing and custom-made narrow-band filters. In the H band, we found 1000s of potential Halpha emitters at z = 1.47, but in Lockman, BOOTES and ELAIS N1 the photo-zs are of very poor quality and do not allow us to distinguish Halpha from other emitters. Fortunately, all genuine z = 1.47 emitters can be easily confirmed/rejected using the perfectly suited S-Cam's NB921 filter to detect [Oii]. This is by far the most efficient method of robustly selecting these z = 1.47 line emitters (Sobral et al. 2012), and significantly more complete than spectroscopy. The large (> 1000), clean (contamination < 3%) and complete (> 97%) samples obtained with the NB921 data (spread over a wide range of environments and properties) will finally allow us to: 1) robustly measure the clustering of z=1.47 SF galaxies as a function of SFR, luminosity, [Oii]/Halpha and mass, 2) unveil fundamental inter-dependencies between mass, environment, Halpha/[Oii] ratios and Halpha or [Oii] luminosity at z ~ 1.5, comparing those with the results at z ~ 0 and without depending on he complex selection function from spectroscopic surveys and 3) calibrate [Oii] as a star-formation indicator at z ~ 1.5.

  19. VizieR Online Data Catalog: The M33 Synoptic Stellar Survey. II. Mira variables (Yuan+, 2017)

    NASA Astrophysics Data System (ADS)

    Yuan, W.; He, S.; Macri, L. M.; Long, J.; Huang, J. Z.

    2017-08-01

    We carried out a search for Mira variables in M33 using sparsely sampled I-band light curves. We based our search on the observations of M33 obtained by Macri et al. 2001 (Cat. J/AJ/121/861) and Pellerin et al. 2011 (Cat. J/ApJS/193/26). These surveys covered most of the disk of this galaxy with a combined baseline of nearly a decade (1996 September to 1999 November for Macri et al. 2001, Cat. J/AJ/121/861; 2002 August to 2006 August for Pellerin et al. 2011, Cat. J/ApJS/193/26) mainly using the Fred L. Whipple Observatory (FLWO) 1.2m and the WIYN observatory 3.5m telescopes with a variety of cameras (see the respective publications for details). While images were obtained in multiple bandpasses (BVI), our analysis is only based on the I-band time-series photometry because Mira candidates fall below the detection limit in the bluer bands. Our final sample consists of 1847 Mira candidates (see Table2). (1 data file).

  20. The OPD photometric survey of open clusters II. robust determination of the fundamental parameters of 24 open clusters

    NASA Astrophysics Data System (ADS)

    Monteiro, H.; Dias, W. S.; Hickel, G. R.; Caetano, T. C.

    2017-02-01

    In the second paper of the series we continue the investigation of open cluster fundamental parameters using a robust global optimization method to fit model isochrones to photometric data. We present optical UBVRI CCD photometry (Johnsons-Cousins system) observations for 24 neglected open clusters, of which 14 have high quality data in the visible obtained for the first time, as a part of our ongoing survey being carried out in the 0.6 m telescope of the Pico dos Dias Observatory in Brazil. All objects were then analyzed with a global optimization tool developed by our group which estimates the membership likelihood of the observed stars and fits an isochrone from which a distance, age, reddening, total to selective extinction ratio RV (included in this work as a new free parameter) and metallicity are estimated. Based on those estimates and their associated errors we analyzed the status of each object as real clusters or not, finding that two are likely to be asterisms. We also identify important discrepancies between our results and previous ones obtained in the literature which were determined using 2MASS photometry.

  1. Aedes albopictus (Diptera: Culicidae) population size survey in the 2007 chikungunya outbreak area in Italy. II: Estimating epidemic thresholds.

    PubMed

    Carrieri, M; Angelini, P; Venturelli, C; Maccagnani, B; Bellini, R

    2012-03-01

    Our study compared different estimates of adult mosquito abundance (Pupal Demographic Survey [PDS], Human Landing Collection [HLC], Number of Bites declared by Citizens during interviews [NBC]) to the mean number of eggs laid in ovitraps. We then calculated a disease risk threshold in terms of number of eggs per ovitrap above which an arbovirus epidemic may occur. The study was conducted during the summers of 2007 and 2008 in the Emilia-Romagna region of Italy where a chikungunya epidemic occurred in 2007. Ovitrap monitoring lasted from May to September, while adult sampling by means of PDS, HLC, and NBC was repeated three times each summer. Based on calculated rate of increase of the disease (R(0)) and the number of bites per human per day measured during the outbreak, we estimated that only 10.1% of the females transmitted the chikungunya virus in the principal focus. Under our conditions, we demonstrated that a positive correlation can be found between the females' density estimated by means of PDS, HLC, and NBC and the mean number of eggs in the ovitraps. We tested our hypothesis during the 2007 secondary outbreak of CHIKV in Cervia, and found that R(0) calculated based on the number of biting females estimated from the egg density was comparable to the R(0) calculated based on the progression of the human cases. The identification of an epidemic threshold based on the mean egg density may define the high risk areas and focus control programs.

  2. Galaxy evolution and large-scale structure in the far-infrared. II. The IRAS faint source survey

    SciTech Connect

    Lonsdale, C.J.; Hacking, P.B.; Conrow, T.P.; Rowan-Robinson, M. Queen Mary College, London )

    1990-07-01

    The new IRAS Faint Source Survey data base is used to confirm the conclusion of Hacking et al. (1987) that the 60 micron source counts fainter than about 0.5 Jy lie in excess of predictions based on nonevolving model populations. The existence of an anisotropy between the northern and southern Galactic caps discovered by Rowan-Robinson et al. (1986) and Needham and Rowan-Robinson (1988) is confirmed, and it is found to extend below their sensitivity limit to about 0.3 Jy in 60 micron flux density. The count anisotropy at f(60) greater than 0.3 can be interpreted reasonably as due to the Local Supercluster; however, no one structure accounting for the fainter anisotropy can be easily identified in either optical or far-IR two-dimensional sky distributions. The far-IR galaxy sky distributions are considerably smoother than distributions from the published optical galaxy catalogs. It is likely that structure of the large size discussed here have been discriminated against in earlier studies due to insufficient volume sampling. 105 refs.

  3. Galaxy evolution and large-scale structure in the far-infrared. II - The IRAS faint source survey

    NASA Technical Reports Server (NTRS)

    Lonsdale, Carol J.; Hacking, Perry B.; Conrow, T. P.; Rowan-Robinson, M.

    1990-01-01

    The new IRAS Faint Source Survey data base is used to confirm the conclusion of Hacking et al. (1987) that the 60 micron source counts fainter than about 0.5 Jy lie in excess of predictions based on nonevolving model populations. The existence of an anisotropy between the northern and southern Galactic caps discovered by Rowan-Robinson et al. (1986) and Needham and Rowan-Robinson (1988) is confirmed, and it is found to extend below their sensitivity limit to about 0.3 Jy in 60 micron flux density. The count anisotropy at f(60) greater than 0.3 can be interpreted reasonably as due to the Local Supercluster; however, no one structure accounting for the fainter anisotropy can be easily identified in either optical or far-IR two-dimensional sky distributions. The far-IR galaxy sky distributions are considerably smoother than distributions from the published optical galaxy catalogs. It is likely that structure of the large size discussed here have been discriminated against in earlier studies due to insufficient volume sampling.

  4. The extended ROSAT-ESO Flux-Limited X-ray Galaxy Cluster Survey (REFLEX II) - III. Construction of the first flux-limited supercluster sample

    NASA Astrophysics Data System (ADS)

    Chon, Gayoung; Böhringer, Hans; Nowak, Nina

    2013-03-01

    We present the first supercluster catalogue constructed with the extended ROSAT-ESO Flux-Limited X-ray (REFLEX II) Galaxy Cluster survey data, which comprises 919 X-ray selected galaxy clusters with a flux limit of 1.8 × 10-12 erg s-1 cm-2. Based on this cluster catalogue we construct a supercluster catalogue using a friends-of-friends algorithm with a linking length depending on the (local) cluster density, which thus varies with redshift. The resulting catalogue comprises 164 superclusters at redshift z ≤ 0.4. The choice of the linking length in the friends-of-friends method modifies the properties of the superclusters. We study the properties of different catalogues such as the distributions of the redshift, extent and multiplicity by varying the choice of parameters. In addition to the supercluster catalogue for the entire REFLEX II sample, we compile a large volume-limited cluster sample from REFLEX II with the redshift and luminosity constraints of z ≤ 0.1 and LX ≥ 5 × 1043 erg s-1. With this catalogue we construct a volume-limited sample of superclusters. This sample is built with a homogeneous linking length, and hence selects effectively the same type of superclusters. By increasing the luminosity cut we can build a hierarchical tree structure of the volume-limited samples, where systems at the top of the tree are only formed via the most luminous clusters. This allows us to test if