536 research outputs found
Mathematics
No full text"Inservice education"--Final (unnumbered) p. of each document.; Includes bibliographical references.T. Teaching mathematics : elementary & middle grades / prepared by Steven P. Meiring (19 p.) -- K. Kindergarten mathematics / principal authors, James B. Wesson, Steven P. Meiring (18 p.) -- 1. First grade mathematics (18 p.) ; 2. Second grade mathematics (15 p.) ; 3. Third grade mathematics (18 p.) / principal author, C. Winston Smith, Jr. -- 4. Fourth grade mathematics (21 p.) ; 5. Fifth grade mathematics (19 p.) / principal author, James B. Wesson -- 6. Sixth grade mathematics (19 p.) ; 7. Seventh grade mathematics (23 p.) / principal author, William R. Speer -- 8. Eighth grade mathematics (19 p.) ; 8E. Eighth grade enrichment mathematics / principal author, James E. Schultz.A series of eleven monographs describing mathematics learning in the elementary and middle grades. These documents identify appropriate outcomes for each grade level and discuss teaching methods for helping students achieve those outcomes
The abundance discrepancy - recombination line versus forbidden line abundances for a northern sample of galactic planetary nebulae
No full textWe present deep optical spectra of 23 galactic planetary nebulae, which are analysed in conjunction with archival infrared and ultraviolet spectra. We derive nebular electron temperatures based on standard collisionally excited line (CEL) diagnostics as well as the hydrogen Balmer jump and find that, as expected, the Balmer jump almost always yields a lower temperature than the [O III] nebular-to-auroral line ratio. We also make use of the weak temperature dependence of helium and O II recombination line ratios to further investigate the temperature structure of the sample nebulae. We find that, in almost every case, the derived temperatures follow the relation Te(CEL) >= Te(BJ) >= Te(He I) >= Te(O II), which is the relation predicted by two-component nebular models in which one component is cold and hydrogen-deficient. Te(O II) may be as low as a few hundred Kelvin, in line with the low temperatures found for the hydrogen-deficient knots of Abell 30 by Wesson, Liu and Barlow. Elemental abundances are derived for the sample nebulae from both CELs and optical recombination lines (ORLs). ORL abundances are higher than CEL abundances in every case, by factors ranging from 1.5 to 12. Five objects with O(2+) abundance discrepancy factors greater than 5 are found. DdDm1 and Vy 2-2 are both found to have a very large abundance discrepancy factor of 11.8. We consider the possible explanations for the observed discrepancies. From the observed differences between Te(O III) and Te(BJ), we find that temperature fluctuations cannot resolve the abundance discrepancies in 22 of the 23 sample nebulae, implying some additional mechanism for enhancing ORL emission. In the one ambiguous case, the good agreement between abundances derived from temperature-insensitive infrared lines and temperature-sensitive optical lines also points away from temperature fluctuations being present. The observed recombination line temperatures, the large abundance discrepancies and the generally good agreement between infrared and optical CEL abundances all suggest instead the existence of a cold hydrogen-deficient component within the 'normal' nebular gas. The origin of this component is as yet unknown.Astronomy & AstrophysicsSCI(E)51ARTICLE2424-45436
The VST Photometric Hα Survey of the Southern Galactic Plane and Bulge (VPHAS+)
No full textContains fulltext :
127903pub.pdf (Publisher’s version ) (Open Access)
Contains fulltext :
127903.pdf (Author’s version preprint ) (Open Access
Electron temperatures and densities of planetary nebulae determined from the nebular hydrogen recombination spectrum and temperature and density variations
No full textA method is presented to derive electron temperatures and densities of planetary nebulae (PNe) simultaneously, using the observed hydrogen recombination spectrum, which includes continuum and line emission. By matching theoretical spectra to observed spectra around the Balmer jump at about 3646 Å, we determine electron temperatures and densities for 48 Galactic PNe. The electron temperatures based on this method - hereafter T e(Bal) - are found to be systematically lower than those derived from [O III] λ4959/λ4363 and [O III] (88 μm + 52 μm)/λ4959 ratios - hereafter T e([O III] na) and T e([O III] fn). The electron densities based on this method are found to be systematically higher than those derived from [O II] λ3729/λ3726, [S II] λ6731/λ6716, [Cl III] λ5537/λ5517, [Ar IV] λ4740/λ4711 and [O III] 88 μm/52 μm ratios. These results suggest that temperature and density fluctuations are generally present within nebulae. The comparison of T e([O III] na) and T e(Bal) suggests that the fractional mean-square temperature variation (t 2) has a representative value of 0.031. A majority of temperatures derived from the T e([O III] fn) ratio are found to be higher than those of T e([O III] na), which is attributed to the existence of dense clumps in nebulae - those [O III] infrared fine-structure lines are suppressed by collisional de-excitation in the clumps. By comparing T e([O III] fn), T e([O III] na) and T e(Bal) and assuming a simple two-density- component model, we find that the filling factor of dense clumps has a representative value of 7 × 10 -5. The discrepancies between T e([O III] na) and T e(Bal) are found to be anticorrelated with electron densities derived from various density indicators; high-density nebulae have the smallest temperature discrepancies. This suggests that temperature discrepancy is related to nebular evolution. In addition, He/H abundances of PNe are found to be positively correlated with the difference between T e([O III] na) and T e(Bal), suggesting that He/H abundances might have been overestimated generally because of the possible existence of H-deficient knots. Electron temperatures and densities deduced from spectra around the Paschen jump regions at 8250 Å are also obtained for four PNe: NGC 7027, NGC 6153, M 1-42 and NGC 7009. Electron densities derived from spectra around the Paschen jump regions are in good agreement with the corresponding values derived from spectra around the Balmer jump, whereas temperatures deduced from the spectra around the Paschen jump are found to be lower than the corresponding values derived from spectra around the Balmer jump for all the four cases. The reason remains unclear.link_to_OA_fulltex
VST Photometric H-alpha Survey of the Southern Galactic Plane and Bulge (VPHAS+)
No full textThe VST Photometric H-alpha survey of the Southern Galactic Plane and Bulge (VPHAS+) is collecting single-epoch Sloan u, g, r, i and H-alpha narrowband photometry, at arcsecond resolution, down to point-source (Vega) magnitudes of ~ 21. The survey footprint encloses the entire southern Galactic Plane within the Galactic latitude range -5° < b < +5°, expanding to b = ±10° in the Galactic Bulge. This brief description of VPHAS+ includes sample data and examples of early science validation
The hydrogen-deficient knot of the 'born-again' planetary nebula Abell 58 (V605 Aql)
No full textWe have analysed deep optical spectra of the 'born-again' planetary nebula Abell 58 and its hydrogen-deficient knot, surrounding V605 Aql, which underwent a nova-like eruption in 1919. Our analysis shows that the extinction towards the central knot is much higher than previously thought, with c(H beta) = 2.0. The outer nebula is less reddened, with c(H beta) = 1.04. We find that the outer nebula has a Ne/O ratio higher than the average PN value. The electron temperature we derive for the central knot varies widely depending on the diagnostic used. The [O(III)] nebular-to-auroral transition ratio gives a temperature of 20 800 K, while the ratio of the [N(II)] nebular and auroral lines gives T(e) = 15 200 K. The helium line ratios lambda 5876/lambda 4471 and lambda 6678/lambda 4471 imply temperatures of 350 and 550 K, respectively. Weakly temperature-sensitive O(II) recombination line ratios imply similarly low electron temperatures. Abundances derived from recombination lines are vastly higher than those found from collisionally excited lines, with the abundance discrepancy factor (ADF) for O(2+) reaching 89 - the second highest known value after that found for the hydrogen-deficient knots in Abell 30. The observed temperature diagnostics and abundances support the idea that, like Abell 30, the knot of Abell 58 contains some very cold ionized material. Although the central star is carbon-rich (C/O > 1), the knot is found to be oxygen-rich, a situation not predicted by the single-star 'born-again' theory of its formation. We compare the known properties of Abell 58 to those of Abell 30, Sakurai's Object and several novae and nova remnants. We argue that the abundances in the ejecta observed in A 30 and A 58 have more in common with neon novae than with Sakurai's Object, which is believed to have undergone a final helium flash. In particular, the C/O ratio of less than unity and the presence of substantial quantities of neon in the ejecta of both Abell 30 and Abell 58 are not predicted by very late thermal pulse models.Astronomy & AstrophysicsSCI(E)0ARTICLE41639-164838
The second data release of the INT Photometric H Survey of the Northern Galactic Plane (IPHAS DR2)
No full textThe INT/WFC Photometric Hα Survey of the Northern Galactic Plane (IPHAS) is a 1800 deg2 imaging survey covering Galactic latitudes |b| < 5° and longitudes ℓ = 30°–215° in the r, i, and Hα filters using the Wide Field Camera (WFC) on the 2.5-m Isaac Newton Telescope (INT) in La Palma. We present the first quality-controlled and globally calibrated source catalogue derived from the survey, providing single-epoch photometry for 219 million unique sources across 92 per cent of the footprint. The observations were carried out between 2003 and 2012 at a median seeing of 1.1 arcsec (sampled at 0.33 arcsec pixel−1) and to a mean 5σ depth of 21.2 (r), 20.0 (i), and 20.3 (Hα) in the Vega magnitude system. We explain the data reduction and quality control procedures, describe and test the global re-calibration, and detail the construction of the new catalogue. We show that the new calibration is accurate to 0.03 mag (root mean square) and recommend a series of quality criteria to select accurate data from the catalogue. Finally, we demonstrate the ability of the catalogue's unique (r − Hα, r − i) diagram to (i) characterize stellar populations and extinction regimes towards different Galactic sightlines and (ii) select and quantify Hα emission-line objects. IPHAS is the first survey to offer comprehensive CCD photometry of point sources across the Galactic plane at visible wavelengths, providing the much-needed counterpart to recent infrared surveys
A Regional Health System Journey from Volume to Value: Roadmap to the Recognition as a 15 Top Health System in the USA for Quality Excellence
No full textNidal H Harb,1,2 Patricia A Said,1 Shirley L Gusta,1 Amanda M Wesson,1 Jordan D Brautigam,1 Jon H Lemke,1 Stephen T DeLessio,1 Douglas P Cropper,1 Nicolas W Shammas1,3 1Quality and Safety Department, Genesis Health System, Davenport, IA, USA; 2Cardiovascular Division, University of Iowa Hospitals and Clinics, Iowa City, IA, USA; 3Cardiology Research Unit, Midwest Cardiovascular Research Foundation, Davenport, IA, USACorrespondence: Nicolas W Shammas, Midwest Cardiovascular Research Foundation, 630 E 4th Street, Davenport, IA, 52801, USA, Tel +1 563-320-0263, Email [email protected]: The 15 Top Health System program, an IBM Watson study, objectively measures health systems’ performance overall on an annual basis using publicly reported data available from the Center for Medicare and Medicaid Services (CMS) and state data banks. Genesis Health System was recognized as an IBM Watson Health 15 Top Health System for two consecutive years in 2020 and 2021. A system-based approach with a “physician-lead, professionally-managed” framework, led to accomplishing the 15 Top Health System. The steps needed included adoption of the IBM Watson database to determine current status of certain key performance indicators, establishing a clinical effectiveness program and governance structure, and adopting Lean methodologies to analyze and determine appropriate interventions with long-term solution. The desire and willingness to accomplish this ambitious goal start with adoption by the Board and the administration of the health system while supplying appropriate financial and human resources that are dedicated to the success of the journey. In this manuscript, we describe the journey and steps implemented to accomplish the outcomes that led to the recognition as a 15 Top Health System for quality excellence.Keywords: 15 Top Health System, physician lead, clinical effectiveness, Lean methodology, Value of car
The UV-excess survey of the Northern Galactic Plane
No full textThe UV-Excess survey of the northern Galactic plane images a 10 degrees x 185 degrees wide band, centred on the Galactic equator using the 2.5-m Isaac Newton Telescope in four bands (U, g, r, He 15875) down to similar to 21-22 mag (similar to 20 in He 15875). The setup and data reduction procedures are described. Simulations of the colours of main-sequence stars, giant, supergiants, DA and DB white dwarfs and AM Canum Venaticorum stars are made, including the effects of reddening. A first look at the data of the survey (currently 30 per cent complete) is given
The 1952 Bulldog
No full textPages from Bentley High School 1952 yearbook including the following staff and students: Shirley Allen, Barbara Baucus, Dennis Beam, Lee Berridge, Jamees Blackhurst, Lenis Bond, Billie Booth, Jerry Brigance, Kay Collins, Everill Craze, John Eddy, Betty Jean Gallaway, Ernest Gifford, William Gusie, Peggy Ann Hall, Bernard Hansen, Kenneth Harrison, Shirley Heiser, Robert Howell, Patricia Keyes, Gerald Miley, Mansfield Park, Charles Roat, Joanne Robinson, Nina Sanborn, Donna Lee Shaum, Delores Sprague, Joan Sweet, Donald Travis, Grace Williams, Harry Williamson, J. Barnett, J. Berridge, J. Bostator, F. Burton, R. Callesen, B. Christle, A. Coates, P. Curry, E. Day, R. Galant, M. Gallaway, D. Glasco, J. Herod, E. Ives, E. Jackson, M. Kirbyson, P. Kruse, G. Langley, B. Lannon, Mary Miller, M. Miller, K. Moore, R. Richardson, L. Roat, T. Tessner, D. Wightman, R. Wiselogle, L. Anderson, L. Avery, C. Blackhurst, T. Blanchard, C. Coates, N. Dechman,J. Dickerson, E. Draper, R. Draper, J. Dyer, J. Edmonson, G. Fallis, Jon Grahn, F. Grooms, C. Gusie, D. Hansen, P. Harmon, L. Hill, B. Hixenbaugh, T. Hockins, J. Horne, A. Ives, B. Katona, G. Kerr, R. Kline, M. Kovacs, D. LaDuke, W. Lakey, M. LeClaire, G. Lukomen, L. McClure, B. Meeks, G. Mitchell, R. Mumford, D. Neil, R. Page, C. Penrod, O. Pickard, R. Pugmire, C. Smith, B. Swanson, W. Tarno, G. Thomas, J. Vickerman, C. Viers, J. Walton, A. Wesson, W. Aldred, L. Anderson, J. Armstrong, W. Atherton, Sh. Barnett, R. Beldin, R. Bolinger, P. Bond, C. Brown, J. Budd, A. Burdick, R. Callesen, E. Eddy, W. Fairchild, B. Finch, A. Garwold, B. Gill, R. Hamilton, P. Hoffman, M. Horne, T. Howay, J. Katona, L. Kutzur, R. Kissinger, M. LaDuke, C, Lawrence, D. Love, R. Martin, F. McClure, N. McGaughey, J. Meder, R. Mitchell, C. Modine, Ch. Monroe, J. Qualls, B. Redburn, D. Roat, M. Roat, B. Slinglend, I. Smith, H. Stagg, D. Stowers, G. Streeter, C. Swanson, J. Swatzel, W. Sweet, N. Tear, G. Vickerman, C. Wallace, S. Wells, N. Wooley
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