bluuebunny/crossref_metadata_2025_split huggingface dataset:
He kura huna - Māori expressions of educational success
Authors: Martin Jennifer 
Published: March 2017

Western values have long dominated discourse on what constitutes success and achievement in education. New Zealand’s own education system has been described as one which “... gives first priority to academic and western values of success” (Lee, 2008, p. 81). Emphasis is placed upon the individual, academic excellence, literacy and numeracy, economic outcomes, and competence in what western society deems valid knowledge, and as such, current assessment measures are reflective of this. While such measures are accepted as ‘best practice’ for mainstream institutions, it is argued that where indigenous education is concerned, “...success also lies in more holistic ways of knowing and participating within a rich cultural context” (Bell, 2004, p.30).
Situated in a Māori world view, this paper considers success through a Māori lens. It is argued that Māori notions of success are not only premised upon academic results, rather cultural factors are considered equally as important to knowledge and understanding of te ao Māori (Māori world view), tikanga Māori (Māori customary practices), whakapapa (genealogy), hītori (histories and tradition) and te reo Māori (the Māori language).
This paper seeks to highlight Māori expressions of educational success for Kura Kaupapa Māori (KKM) through the implementation of a holistic approach to education, underpinned by the guiding philosophy, Te Aho Matua.
This paper will draw on my doctoral research. Graduates experiences are an integral part of this paper and research, as they give voice and validity to KKM educational success.
Maori Are Scum, Stupid, Lazy: Maori According to Google
Authors: Elers Steve 
Published: March 2017

The world has become more interconnected which has changed the way we communicate (Steinfeldt et al., 2010). As technology has continually developed allowing instant online publication, an increasing abundance of opinionated discourse has appeared on the worldwide web (Chelaru, Altingovde, Siersdorfer & Nejdl, 2012). From blogs that disseminate political ideologies, to hair and makeup tutorials, the internet has become a medium that facilitates unfiltered instantaneous communication to a potentially global audience. While most users of internet services utilise the technology to engage in civilised dialogue, it does not require much effort to locate capricious behaviour in the anonymised online environment.
I sing of Te Aitu o Te Rangi and the power of song to rejuvenate the principles, values and philosophy of Mana Wahine
Authors: Smith Sophronia 
Published: March 2017

I will sing of my tipuna wahine, Te Aitu o Te Rangi, daughter of Rangitane o Wairarapa chief, Te Whatahoronui. She was a beautiful young fourteen year old when the Ngāti Toa Chief Te Rauparaha successfully conquered the area and took her as a slave wife. Two years later Te Aitu and John Jury escaped Kapiti Island, where she was held captive and journeyed on a two man whaling boat back to Wairarapa. She was courageous amidst impending death on the turbulent waters of Wairarapa. She was also the mother of one of the most prolific writers, researchers and academic from Wairarapa, Hoani Te Whatahoro Jury, whose work ensured the preservation of knowledge regarding kauwae runga kauwae raro. In performing original contemporary composition, I celebrate the accomplishments of Te Aitu o Te Rangi, a Tuawahine, and I recall and embody the power of my matrilineal genealogy. Mana wahine stands strong in the spaces where feminist discourse continues to dominate, and composition provides a platform on which to reclaim and rewrite difference. My paper will look at the medium of contemporary music to provoke recognition and critique of the western archetype of the heroine, whilst at the same time advocating for social change.
Role of Sepsis Screening in early diagnosis of Neonatal Sepsis
Authors: Lakhey A , Shakya H 
Published: March 2017

Background: Neonatal sepsis, a clinical syndrome of bacteremia with systemic signs and symptoms of infection in the first 4 weeks of life is a major cause of morbidity and mortality in newborn inborn. Early diagnosis is critical, as sepsis can progress more rapidly in neonates than in adults. An attempt was made to establish correlation between early neonatal sepsis screening & blood culture in neonates presenting with features of sepsis. The aim of this study is to assess the usefulness of sepsis screen in early diagnosis of neonatal septicemia.Materials and Methods: The study was done in Kist medical college and hospital, Nepal from October 2015 to October 2016. Statistical correlation between early indicators of sepsis screen & blood culture (considered as gold standard) was established in clinically suspicious cases of neonatal sepsis. Results: Out of 150 cases studied, 72 were culture positive. CRP (77.8%) and immature: total neutrophils ratio (73%) showed highest sensitivity. CRP (66.7%), I/T ratio (61.5%) and micro ESR (60.2%) showed highest specificity. Positive predictive value was highest for CRP (68.2%) followed by I/T ratio (63.8%) and corrected total leukocyte count (56.2%)Conclusion: Serum CRP is the most sensitive marker of sepsis. Use of peripheral smear study and CRP can be implicated effectively as a sepsis screen for early diagnosis of neonatal sepsis. The combination of parameters yielded better results than single tests and proved to be an invaluable tool for early diagnosis of neonatal sepsis.
NGC 1980 Is Not a Foreground Population of Orion: Spectroscopic Survey of Young Stars with Low Extinction in Orion A
Authors: Fang Min , Kim Jinyoung Serena , Pascucci Ilaria , Apai Dániel , Zhang Lan , Sicilia-Aguilar Aurora , Alonso-Martínez Miguel , Eiroa Carlos , Wang Hongchi 
Published: March 2017

Abstract
We perform a spectroscopic survey of the foreground population in Orion A with MMT/Hectospec. We use these data, along with archival spectroscopic data and photometric data, to derive spectral types, extinction values, and masses for 691 stars. Using the Spitzer Space Telescope data, we characterize the disk properties of these sources. We identify 37 new transition disk (TD) objects, 1 globally depleted disk candidate, and 7 probable young debris disks. We discover an object with a mass of less than 0.018–0.030 M
⊙, which harbors a flaring disk. Using the Hα emission line, we characterize the accretion activity of the sources with disks, and confirm that the fraction of accreting TDs is lower than that of optically thick disks (46% ± 7% versus 73% ± 9%, respectively). Using kinematic data from the Sloan Digital Sky Survey and APOGEE INfrared Spectroscopy of the Young Nebulous Clusters program (IN-SYNC), we confirm that the foreground population shows similar kinematics to their local molecular clouds and other young stars in the same regions. Using the isochronal ages, we find that the foreground population has a median age of around 1–2 Myr, which is similar to that of other young stars in Orion A. Therefore, our results argue against the presence of a large and old foreground cluster in front of Orion A.
Discovery of 16 New z ∼ 5.5 Quasars: Filling in the Redshift Gap of Quasar Color Selection
Authors: Yang Jinyi , Fan Xiaohui , Wu Xue-Bing , Wang Feige , Bian Fuyan , Yang Qian , McGreer Ian D. , Yi Weimin , Jiang Linhua , Green Richard , Yue Minghao , Wang Shu , Li Zefeng , Ding Jiani , Dye Simon , Lawrence Andy 
Published: March 2017

Abstract
We present initial results from the first systematic survey of luminous z ∼ 5.5 quasars. Quasars at z ∼ 5.5, the post-reionization epoch, are crucial tools to explore the evolution of intergalactic medium, quasar evolution, and the early super-massive black hole growth. However, it has been very challenging to select quasars at redshifts 5.3 ≤ z ≤ 5.7 using conventional color selections, due to their similar optical colors to late-type stars, especially M dwarfs, resulting in a glaring redshift gap in quasar redshift distributions. We develop a new selection technique for z ∼ 5.5 quasars based on optical, near-IR, and mid-IR photometric data from Sloan Digital Sky Survey (SDSS), UKIRT InfraRed Deep Sky Surveys—Large Area Survey (ULAS), VISTA Hemisphere Survey (VHS), and Wide Field Infrared Survey Explorer. From our pilot observations in the SDSS-ULAS/VHS area, we have discovered 15 new quasars at 5.3 ≤ z ≤ 5.7 and 6 new lower redshift quasars, with SDSS z band magnitude brighter than 20.5. Including other two z ∼ 5.5 quasars already published in our previous work, we now construct a uniform quasar sample at 5.3 ≤ z ≤ 5.7, with 17 quasars in a ∼4800 square degree survey area. For further application in a larger survey area, we apply our selection pipeline to do a test selection by using the new wide field J-band photometric data from a preliminary version of the UKIRT Hemisphere Survey (UHS). We successfully discover the first UHS selected z ∼ 5.5 quasar.
Gas Removal in the Ursa Minor Galaxy: Linking Hydrodynamics and Chemical Evolution Models
Authors: Caproni Anderson , Lanfranchi Gustavo Amaral , Baio Gabriel Henrique Campos , Kowal Grzegorz , Falceta-Gonçalves Diego 
Published: March 2017

Abstract
We present results from a non-cosmological, three-dimensional hydrodynamical simulation of the gas in the dwarf spheroidal galaxy Ursa Minor. Assuming an initial baryonic-to-dark-matter ratio derived from the cosmic microwave background radiation, we evolved the galactic gas distribution over 3 Gyr, taking into account the effects of the types Ia and II supernovae. For the first time, we used in our simulation the instantaneous supernovae rates derived from a chemical evolution model applied to spectroscopic observational data of Ursa Minor. We show that the amount of gas that is lost in this process is variable with time and radius, being the highest rates observed during the initial 600 Myr in our simulation. Our results indicate that types Ia and II supernovae must be essential drivers of the gas loss in Ursa Minor galaxy (and probably in other similar dwarf galaxies), but it is ultimately the combination of galactic winds powered by these supernovae and environmental effects (e.g., ram-pressure stripping) that results in the complete removal of the gas content.
Star Formation In Nearby Clouds (SFiNCs): X-Ray and Infrared Source Catalogs and Membership
Authors: Getman Konstantin V. , Broos Patrick S. , Kuhn Michael A. , Feigelson Eric D. , Richert Alexander J. W. , Ota Yosuke , Bate Matthew R. , Garmire Gordon P. 
Published: March 2017

Abstract
The Star Formation in Nearby Clouds (SFiNCs) project is aimed at providing a detailed study of the young stellar populations and of star cluster formation in the nearby 22 star-forming regions (SFRs) for comparison with our earlier MYStIX survey of richer, more distant clusters. As a foundation for the SFiNCs science studies, here, homogeneous data analyses of the Chandra X-ray and Spitzer mid-infrared archival SFiNCs data are described, and the resulting catalogs of over 15,300 X-ray and over 1,630,000 mid-infrared point sources are presented. On the basis of their X-ray/infrared properties and spatial distributions, nearly 8500 point sources have been identified as probable young stellar members of the SFiNCs regions. Compared to the existing X-ray/mid-infrared publications, the SFiNCs member list increases the census of YSO members by 6%–200% for individual SFRs and by 40% for the merged sample of all 22 SFiNCs SFRs.
Revised Stellar Properties of Kepler Targets for the Q1-17 (DR25) Transit Detection Run
Authors: Mathur Savita , Huber Daniel , Batalha Natalie M. , Ciardi David R. , Bastien Fabienne A. , Bieryla Allyson , Buchhave Lars A. , Cochran William D. , Endl Michael , Esquerdo Gilbert A. , Furlan Elise , Howard Andrew , Howell Steve B. , Isaacson Howard , Latham David W. , MacQueen Phillip J. , Silva David R. 
Published: March 2017

Abstract
The determination of exoplanet properties and occurrence rates using Kepler data critically depends on our knowledge of the fundamental properties (such as temperature, radius, and mass) of the observed stars. We present revised stellar properties for 197,096 Kepler targets observed between Quarters 1–17 (Q1-17), which were used for the final transiting planet search run by the Kepler Mission (Data Release 25, DR25). Similar to the Q1–16 catalog by Huber et al., the classifications are based on conditioning published atmospheric parameters on a grid of Dartmouth isochrones, with significant improvements in the adopted method and over 29,000 new sources for temperatures, surface gravities, or metallicities. In addition to fundamental stellar properties, the new catalog also includes distances and extinctions, and we provide posterior samples for each stellar parameter of each star. Typical uncertainties are ∼27% in radius, ∼17% in mass, and ∼51% in density, which is somewhat smaller than previous catalogs because of the larger number of improved

constraints and the inclusion of isochrone weighting when deriving stellar posterior distributions. On average, the catalog includes a significantly larger number of evolved solar-type stars, with an increase of 43.5% in the number of subgiants. We discuss the overall changes of radii and masses of Kepler targets as a function of spectral type, with a particular focus on exoplanet host stars.
The InterPlanetary Network Supplement to the Second Fermi GBM Catalog of Cosmic Gamma-Ray Bursts
Authors: Hurley K. , Aptekar R. L. , Golenetskii S. V. , Frederiks D. D. , Svinkin D. S. , Pal’shin V. D. , Briggs M. S. , Meegan C. , Connaughton V. , Goldsten J. , Boynton W. , Fellows C. , Harshman K. , Mitrofanov I. G. , Golovin D. V. , Kozyrev A. S. , Litvak M. L. , Sanin A. B. , Rau A. , Kienlin A. von , Zhang X. , Yamaoka K. , Fukazawa Y. , Ohno M. , Tashiro M. , Terada Y. , Barthelmy S. , Cline T. , Gehrels N. , Cummings J. , Krimm H. A. , Smith D. M. , Monte E. Del , Feroci M. , Marisaldi M. 
Published: March 2017

Abstract
InterPlanetary Network (IPN) data are presented for the gamma-ray bursts in the second Fermi Gamma-Ray Burst Monitor (GBM) catalog. Of the 462 bursts in that catalog between 2010 July 12 and 2012 July 11, 428, or 93%, were observed by at least 1 other instrument in the 9-spacecraft IPN. Of the 428, the localizations of 165 could be improved by triangulation. For these bursts, triangulation gives one or more annuli whose half-widths vary between about 2.′3° and 16°, depending on the peak flux, fluence, time history, arrival direction, and the distance between the spacecraft. We compare the IPN localizations with the GBM 1σ, 2σ, and 3σ error contours and find good agreement between them. The IPN 3σ error boxes have areas between about 8 square arcminutes and 380 square degrees, and are an average of 2500 times smaller than the corresponding GBM 3σ localizations. We identify four bursts in the IPN/GBM sample whose origins were given as “uncertain,” but may in fact be cosmic. This leads to an estimate of over 99% completeness for the GBM catalog.
A Comparison of Grid-based and SPH Binary Mass-transfer and Merger Simulations
Authors: Motl Patrick M. , Frank Juhan , Staff Jan , Clayton Geoffrey C. , Fryer Christopher L. , Even Wesley , Diehl Steven , Tohline Joel E. 
Published: March 2017

Abstract
There is currently a great amount of interest in the outcomes and astrophysical implications of mergers of double degenerate binaries. In a commonly adopted approximation, the components of such binaries are represented by polytropes with an index of n = 3/2. We present detailed comparisons of stellar mass-transfer and merger simulations of polytropic binaries that have been carried out using two very different numerical algorithms—a finite-volume “grid” code and a smoothed-particle hydrodynamics (SPH) code. We find that there is agreement in both the ultimate outcomes of the evolutions and the intermediate stages if the initial conditions for each code are chosen to match as closely as possible. We find that even with closely matching initial setups, the time it takes to reach a concordant evolution differs between the two codes because the initial depth of contact cannot be matched exactly. There is a general tendency for SPH to yield higher mass transfer rates and faster evolution to the final outcome. We also present comparisons of simulations calculated from two different energy equations: in one series, we assume a polytropic equation of state and in the other series an ideal gas equation of state. In the latter series of simulations, an atmosphere forms around the accretor, which can exchange angular momentum and cause a more rapid loss of orbital angular momentum. In the simulations presented here, the effect of the ideal equation of state is to de-stabilize the binary in both SPH and grid simulations, but the effect is more pronounced in the grid code.
Variation of Ionizing Continuum: The Main Driver of Broad Absorption Line Variability
Authors: He Zhicheng , Wang Tinggui , Zhou Hongyan , Bian Weihao , Liu Guilin , Yang Chenwei , Dou Liming , Sun Luming 
Published: March 2017

Abstract
We present a statistical analysis of the variability of broad absorption lines (BALs) in quasars using the large multi-epoch spectroscopic data set of the Sloan Digital Sky Survey Data Release 12 (SDSS DR12). We divide the sample into two groups according to the pattern of the variation of C iv BAL with respect to that of a continuum: the equivalent widths (EW) of the BAL decreases (increases) when the continuum brightens (dims) as group T1; and the variation of the EW and the continuum in the opposite relation of group T2. We find that T2 has significantly (

, Students T Test) higher EW ratios (R) of Si iv to C iv BAL than T1. Our result agrees with the prediction of photoionization models that

column density increases (decreases) if there is a (or no)

ionization front, while R decreases with the incident continuum. We show that BAL variabilities in at least 80% of quasars are driven by the variation of an ionizing continuum, while other models that predict uncorrelated BAL and continuum variability contribute less than 20%. Considering large uncertainty in the continuum flux calibration, the latter fraction may be much smaller. When the sample is binned into different time intervals between the two observations, we find significant difference in the distribution of R between T1 and T2 in all time-bins down to

days, suggesting that the BAL outflow in a fraction of quasars has a recombination timescale of only a few days.
Spectroscopy of Ultra-diffuse Galaxies in the Coma Cluster
Authors: Kadowaki Jennifer , Zaritsky Dennis , Donnerstein R. L. 
Published: March 2017

Abstract
We present spectra of five ultra-diffuse galaxies (UDGs) in the vicinity of the Coma cluster obtained with the Multi-object Double Spectrograph on the Large Binocular Telescope. We confirm four of these as members of the cluster, quintupling the number of spectroscopically confirmed systems. Like the previously confirmed large (projected half-light radius >4.6 kpc) UDG, DF44, the systems we targeted all have projected half-light radii

. As such, we spectroscopically confirm a population of physically large UDGs in the Coma cluster. The remaining UDG is located in the field, about 45 Mpc behind the cluster. We observe Balmer and Ca ii H and K absorption lines in all of our UDG spectra. By comparing the stacked UDG spectrum against stellar population synthesis models, we conclude that, on average, these UDGs are composed of metal-poor stars ([Fe/H] ≲ −1.5). We also discover the first UDG with [O ii] and [O iii] emission lines within a clustered environment, demonstrating that not all cluster UDGs are devoid of gas and sources of ionizing radiation.
On the Absence of Non-thermal X-Ray Emission around Runaway O Stars
Authors: Toalá 杜 J. A. 宇君 , Oskinova L. M. , Ignace R. 
Published: March 2017

Abstract
Theoretical models predict that the compressed interstellar medium around runaway O stars can produce high-energy non-thermal diffuse emission, in particular, non-thermal X-ray and γ-ray emission. So far, detection of non-thermal X-ray emission was claimed for only one runaway star, AE Aur. We present a search for non-thermal diffuse X-ray emission from bow shocks using archived XMM-Newton observations for a clean sample of six well-determined runaway O stars. We find that none of these objects present diffuse X-ray emission associated with their bow shocks, similarly to previous X-ray studies toward ζ Oph and BD+43°3654. We carefully investigated multi-wavelength observations of AE Aur and could not confirm previous findings of non-thermal X-rays. We conclude that so far there is no clear evidence of non-thermal extended emission in bow shocks around runaway O stars.
Dusty Winds in Active Galactic Nuclei: Reconciling Observations with Models
Authors: Hönig Sebastian F. , Kishimoto Makoto 
Published: March 2017

Abstract
This Letter presents a revised radiative transfer model for the infrared (IR) emission of active galactic nuclei (AGNs). While current models assume that the IR is emitted from a dusty torus in the equatorial plane of the AGNs, spatially resolved observations indicate that the majority of the IR emission from ≲100 pc in many AGNs originates from the polar region, contradicting classical torus models. The new model CAT3D-WIND builds upon the suggestion that the dusty gas around the AGNs consists of an inflowing disk and an outflowing wind. Here, it is demonstrated that (1) such disk+wind models cover overall a similar parameter range of observed spectral features in the IR as classical clumpy torus models, e.g., the silicate feature strengths and mid-IR spectral slopes, (2) they reproduce the 3–5 μm bump observed in many type 1 AGNs unlike torus models, and (3) they are able to explain polar emission features seen in IR interferometry, even for type 1 AGNs at relatively low inclination, as demonstrated for NGC3783. These characteristics make it possible to reconcile radiative transfer models with observations and provide further evidence of a two-component parsec-scale dusty medium around AGNs: the disk gives rise to the 3–5 μm near-IR component, while the wind produces the mid-IR emission. The model SEDs will be made available for download.
Preparing Engineering Students for the Global Sourcing Environment
Authors: Manzione Louis , Abuaisheh Akram , Sumukadas Narendar , Congden Steve 
Published: March 2017

<p><strong><span style="font-size: small;"><span style="font-family: Times New Roman;"><em>Abstract</em>—Globalization and rapid changes in modern product development and realization are creating gaps in engineering education systems around the world. The global economy has changed the way that engineering firms design, develop, and produce their products. Companies need to evaluate many options available worldwide, not just locally. The current trends are only likely to continue as the world economy becomes more competitive, interdependent, and characterized by global relationships among supply chain partners. This paper presents a plan for preparing engineering students for the new global sourcing environments and product realization processes. Infusions of supply chain management and project management skills into the curriculum are recommended, as well as use of university-industry partnerships, course portfolios, and study abroad programs.</span></span></strong></p>