bluuebunny/crossref_metadata_2025_split huggingface dataset:
CONTRASTING GALAXY FORMATION FROM QUANTUM WAVE DARK MATTER, ψDM, WITH ΛCDM, USING PLANCK AND HUBBLE DATA
Authors: Schive Hsi-Yu , Chiueh Tzihong , Broadhurst Tom , Huang Kuan-Wei 
Published: February 2016

ABSTRACT
The newly established luminosity functions (LFs) of high-z galaxies at 4 ≲ z ≲ 10 can provide a stringent check on dark matter models that aim to explain the core properties of dwarf galaxies. The cores of dwarf spheroidal galaxies are understood to be too large to be accounted for by free streaming of warm dark matter without overly suppressing the formation of such galaxies. Here we demonstrate with cosmological simulations that wave dark matter,

, appropriate for light bosons such as axions, does not suffer from this problem, given a boson mass of

(2σ). In this case, the halo mass function is suppressed below

at a level that is consistent with the high-z LFs, while simultaneously generating the kiloparsec-scale cores in dwarf galaxies arising from the solitonic ground state in

. We demonstrate that the reionization history in this scenario is consistent with the Thomson optical depth recently reported by Planck, assuming a reasonable ionizing photon production rate. We predict that the LF should turn over slowly around an intrinsic ultraviolet luminosity of

at

. We also show that for galaxies magnified

in the Hubble Frontier Fields,

predicts an order of magnitude fewer detections than cold dark matter at

down to

, allowing us to distinguish between these very different interpretations for the observed coldness of dark matter.
THE NANOGRAV NINE-YEAR DATA SET: ASTROMETRIC MEASUREMENTS OF 37 MILLISECOND PULSARS
Authors: Matthews Allison M. , Nice David J. , Fonseca Emmanuel , Arzoumanian Zaven , Crowter Kathryn , Demorest Paul B. , Dolch Timothy , Ellis Justin A. , Ferdman Robert D. , Gonzalez Marjorie E. , Jones Glenn , Jones Megan L. , Lam Michael T. , Levin Lina , McLaughlin Maura A. , Pennucci Timothy T. , Ransom Scott M. , Stairs Ingrid H. , Stovall Kevin , Swiggum Joseph K. , Zhu Weiwei 
Published: February 2016

ABSTRACT
Using the nine-year radio-pulsar timing data set from the North American Nanohertz Observatory for Gravitational Waves (NANOGrav), collected at Arecibo Observatory and the Green Bank Telescope, we have measured the positions, proper motions, and parallaxes for 37 millisecond pulsars. We report twelve significant parallax measurements and distance measurements, and eighteen lower limits on distance. We compare these measurements to distances predicted by the NE2001 interstellar electron density model and find them to be in general agreement. We use measured orbital-decay rates and spin-down rates to confirm two of the parallax distances and to place distance upper limits on other sources; these distance limits agree with the parallax distances with one exception, PSR J1024–0719, which we discuss at length. Using the proper motions of the 37 NANOGrav pulsars in combination with other published measurements, we calculate the velocity dispersion of the millisecond pulsar population in Galactocentric coordinates. We find the radial, azimuthal, and perpendicular dispersions to be 46, 40, and 24

, respectively, in a model that allows for high-velocity outliers; or 81, 58, and 62

for the full population. These velocity dispersions are far smaller than those of the canonical pulsar population, and are similar to older Galactic disk populations. This suggests that millisecond pulsar velocities are largely attributable to their being an old population rather than being artifacts of their birth and evolution as neutron star binary systems. The components of these velocity dispersions follow similar proportions to other Galactic populations, suggesting that our results are not biased by selection effects.
X-RAY BURST OSCILLATIONS: FROM FLAME SPREADING TO THE COOLING WAKE
Authors: Mahmoodifar Simin , Strohmayer Tod 
Published: February 2016

ABSTRACT
Type I X-ray bursts are thermonuclear flashes observed from the surfaces of accreting neutron stars (NSs) in low mass X-ray binaries. Oscillations have been observed during the rise and/or decay of some of these X-ray bursts. Those seen during the rise can be well explained by a spreading hot spot model, but large amplitude oscillations in the decay phase remain mysterious because of the absence of a clear-cut source of asymmetry. To date there have not been any quantitative studies that consistently track the oscillation amplitude both during the rise and decay (cooling tail) of bursts. Here we compute the light curves and amplitudes of oscillations in X-ray burst models that realistically account for both flame spreading and subsequent cooling. We present results for several such “cooling wake” models, a “canonical” cooling model where each patch on the NS surface heats and cools identically, or with a latitude-dependent cooling timescale set by the local effective gravity, and an “asymmetric” model where parts of the star cool at significantly different rates. We show that while the canonical cooling models can generate oscillations in the tails of bursts, they cannot easily produce the highest observed modulation amplitudes. Alternatively, a simple phenomenological model with asymmetric cooling can achieve higher amplitudes consistent with the observations.
MULTI-MESSENGER TESTS FOR FAST-SPINNING NEWBORN PULSARS EMBEDDED IN STRIPPED-ENVELOPE SUPERNOVAE
Authors: Kashiyama Kazumi , Murase Kohta , Bartos Imre , Kiuchi Kenta , Margutti Raffaella 
Published: February 2016

ABSTRACT
Fast-spinning strongly magnetized newborn neutron stars (NSs), including nascent magnetars, are popularly implemented as the engine of luminous stellar explosions. Here, we consider the scenario that they power various stripped-envelope (SE) supernovae (SNe), not only superluminous SNe Ic but also broad-line (BL) SNe Ibc and possibly some ordinary SNe Ibc. This scenario is also motivated by the hypothesis that Galactic magnetars largely originate from fast-spinning NSs as remnants of SE SNe. By consistently modeling the energy injection from magnetized wind and

decay, we show that proto-NSs with

rotation and a poloidal magnetic field of

can be harbored in ordinary SNe Ibc. On the other hand, millisecond proto-NSs can solely power BL SNe Ibc if they are born with

and superluminous SNe Ic with

. Then, we study how multi-messenger emission can be used to discriminate such pulsar-driven SN models from other competitive scenarios. First, high-energy X-ray and gamma-ray emission from embryonic pulsar wind nebulae can probe the underlying newborn pulsar. Follow-up observations of SE SNe using NuSTAR

after the explosion are strongly encouraged for nearby objects. We also discuss possible effects of gravitational waves (GWs) on the spin-down of proto-NSs. If millisecond proto-NSs with

emit GWs through, e.g., non-axisymmetric rotation deformed by the inner toroidal fields of

, the GW signal can be detectable from ordinary SNe Ibc in the Virgo cluster by Advanced LIGO, Advanced Virgo, and KAGRA.
RESOLVED CO GAS INTERIOR TO THE DUST RINGS OF THE HD 141569 DISK
Authors: Flaherty Kevin M. , Hughes A. Meredith , Andrews Sean M. , Qi Chunhua , Wilner David J. , Boley Aaron C. , White Jacob A. , Harney Will , Zachary Julia 
Published: February 2016

ABSTRACT
The disk around HD 141569 is one of a handful of systems whose weak infrared emission is consistent with a debris disk, but still has a significant reservoir of gas. Here we report spatially resolved millimeter observations of the CO(3-2) and CO(1-0) emission as seen with the Submillimeter Array and CARMA. We find that the excitation temperature for CO is lower than expected from cospatial blackbody grains, similar to previous observations of analogous systems, and derive a gas mass that lies between that of gas-rich primordial disks and gas-poor debris disks. The data also indicate a large inner hole in the CO gas distribution and an outer radius that lies interior to the outer scattered light rings. This spatial distribution, with the dust rings just outside the gaseous disk, is consistent with the expected interactions between gas and dust in an optically thin disk. This indicates that gas can have a significant effect on the location of the dust within debris disks.
ON POTASSIUM AND OTHER ABUNDANCE ANOMALIES OF RED GIANTS IN NGC 2419
Authors: Iliadis C. , Karakas A. I. , Prantzos N. , Lattanzio J. C. , Doherty C. L. 
Published: February 2016

ABSTRACT
Globular clusters are of paramount importance for testing theories of stellar evolution and early galaxy formation. Strong evidence for multiple populations of stars in globular clusters derives from observed abundance anomalies. A puzzling example is the recently detected Mg–K anticorrelation in NGC 2419. We perform Monte Carlo nuclear reaction network calculations to constrain the temperature–density conditions that gave rise to the elemental abundances observed in this elusive cluster. We find a correlation between stellar temperature and density values that provide a satisfactory match between simulated and observed abundances in NGC 2419 for all relevant elements (Mg, Si, K, Ca, Sc, Ti, and V). Except at the highest densities (ρ ≳ 108 g cm−3), the acceptable conditions range from ≈100 MK at ≈108 g cm−3 to ≈200 MK at ≈10−4 g cm−3. This result accounts for uncertainties in nuclear reaction rates and variations in the assumed initial composition. We review hydrogen-burning sites and find that low-mass stars, asymptotic giant branch (AGB) stars, massive stars, or supermassive stars cannot account for the observed abundance anomalies in NGC 2419. Super-AGB stars could be viable candidates for the polluter stars if stellar model parameters can be fine-tuned to produce higher temperatures. Novae, involving either CO or ONe white dwarfs, could be interesting polluter candidates, but a current lack of low-metallicity nova models precludes firmer conclusions. We also discuss whether additional constraints for the first-generation polluters can be obtained by future measurements of oxygen, or by evolving models of second-generation low-mass stars with a non-canonical initial composition.
GLOBULAR CLUSTER POPULATIONS: RESULTS INCLUDING S4G LATE-TYPE GALAXIES
Authors: Zaritsky Dennis , McCabe Kelsey , Aravena Manuel , Athanassoula E. , Bosma Albert , Comerón Sébastien , Courtois Helene M. , Elmegreen Bruce G. , Elmegreen Debra M. , Erroz-Ferrer Santiago , Gadotti Dimitri A. , Hinz Joannah L. , Ho Luis C. , Holwerda Benne , Kim Taehyun , Knapen Johan H. , Laine Jarkko , Laurikainen Eija , Muñoz-Mateos Juan Carlos , Salo Heikki , Sheth Kartik 
Published: February 2016

ABSTRACT
Using 3.6 and 4.5 μm images of 73 late-type, edge-on galaxies from the S4G survey, we compare the richness of the globular cluster populations of these galaxies to those of early-type galaxies that we measured previously. In general, the galaxies presented here fill in the distribution for galaxies with lower stellar mass, M
*, specifically

, overlap the results for early-type galaxies of similar masses, and, by doing so, strengthen the case for a dependence of the number of globular clusters per 109
M
⊙ of galaxy stellar mass, T
N, on M
*. For

we find the relationship can be satisfactorily described as

when M
* is expressed in solar masses. The functional form of the relationship is only weakly constrained, and extrapolation outside this range is not advised. Our late-type galaxies, in contrast to our early types, do not show the tendency for low-mass galaxies to split into two T
N families. Using these results and a galaxy stellar mass function from the literature, we calculate that, in a volume-limited, local universe sample, clusters are most likely to be found around fairly massive galaxies (M
* ∼ 1010.8
M
⊙) and present a fitting function for the volume number density of clusters as a function of parent-galaxy stellar mass. We find no correlation between T
N and large-scale environment, but we do find a tendency for galaxies of fixed M
* to have larger T
N if they have converted a larger proportion of their baryons into stars.
Global distribution of vertical wavenumber spectra in the lower stratosphere observed using high-vertical-resolution temperature profiles from COSMIC GPS radio occultation
Authors:   Noersomadi, Tsuda T. 
Published: February 2016

Abstract. We retrieved temperature (T) profiles with a high vertical resolution using the full spectrum inversion (FSI) method from the Constellation Observing System for Meteorology, Ionosphere and Climate (COSMIC) GPS radio occultation (GPS-RO) data from January 2007 to December 2009. We studied the characteristics of temperature perturbations in the stratosphere at 20–27 km altitude. This height range does not include a sharp jump in the background Brunt–Väisälä frequency squared (N2) near the tropopause, and it was reasonably stable regardless of season and latitude. We analyzed the vertical wavenumber spectra of gravity waves (GWs) with vertical wavelengths ranging from 0.5 to 3.5 km, and we integrated the (total) potential energy EpT. Another integration of the spectra from 0.5 to 1.75 km was defined as EpS for short vertical wavelength GWs, which was not studied with the conventional geometrical optics (GO) retrievals. We also estimated the logarithmic spectral slope (p) for the saturated portion of spectra with a linear regression fitting from 0.5 to 1.75 km.Latitude and time variations in the spectral parameters were investigated in two longitudinal regions: (a) 90–150° E, where the topography was more complicated, and (b) 170–230° E, which is dominated by oceans. We compared EpT, EpS, and p, with the mean zonal winds (U) and outgoing longwave radiation (OLR). We also show a ratio of EpS to EpT and discuss the generation source of EpS. EpT and p clearly showed an annual cycle, with their maximum values in winter at 30–50° N in region (a), and 50–70° N in region (b), which was related to the topography. At 30–50° N in region (b), EpT and p exhibited some irregular variations in addition to an annual cycle. In the Southern Hemisphere, we also found an annual oscillation in EpT and p, but it showed a time lag of about 2 months relative to U. Characteristics of EpTand p in the tropical region seem to be related to convective activity. The ratio of EpT to the theoretical model value, assuming saturated GWs, became larger in the equatorial region and over mountainous regions.
Primary production in the Chukchi Sea with potential effects of freshwater content
Authors: Yun M. S. , Whitledge T. E. , Stockwell D. , Son S. H. , Lee J. H. , Park J. W. , Lee D. B. , Park J. , Lee S. H. 
Published: February 2016

Abstract. The in situ primary production rates and various environmental variables were investigated in the Chukchi Sea during the RUSALCA expedition, which was conducted in 2012, to identify the current status of primary production. A 13C–15N dual-tracer technique was used to measure the daily primary production rates, which ranged from 0.02 to 1.61 g C m−2 d−1 (mean ±SD  =  0.42 ± 0.52 g C m−2 d−1). The primary production rates showed large regional differences, with the southern region (0.66 ± 0.62 g C m−2 d−1) producing approximately 5 times as much as the northern region (0.14 ± 0.10 g C m−2 d−1), which was primarily due to the differences in phytoplankton biomasses induced by regional nutrient conditions. The primary production rates in the Chukchi Sea were averaged using data acquired during the three different RUSALCA expeditions (2004, 2009, and 2012) as 0.33 g C m−2 d−1 (SD  =  0.40 g C m−2 d−1), which was significantly lower than previously reported rates. In addition to strong seasonal and interannual variations in primary production, recent decreases in the concentrations of major inorganic nutrients and chlorophyll a could be among the reasons for the recent low primary production in the Chukchi Sea because the primary production is mainly affected by nutrient concentration and phytoplankton biomass. The nutrient inventory and primary production appear to be largely influenced by the freshwater content (FWC) variability in the region due to the significant relationships between FWC, nitrate inventory (r  =  0.54, p < 0.05), and primary production rates (r  =  0.56, p < 0.05). Moreover, we found highly significant relationships between the nutrient inventory and the primary production rates (r  =  0.75, p < 0.001). In conclusion, the primary production in the Chukchi Sea is primarily controlled by nutrient availability, which is strongly related to the FWC variability. Our results imply that the predicted increase in freshwater accumulation might cause a decrease in primary production by lowering the nutrient inventory in the euphotic zone of the Chukchi Sea.
MÉTODOS DE ENSEÑANZA DE FÍSICA, MODALIDAD A DISTANCIA EN EL INSTITUTO SABATINO “ESPERANZA”, MUNICIPIO DE SIUNA
Authors: Tinoco Méndez Marta Nidia , Hernández Herrera Reina Isabel 
Published: February 2016

Este estudio realizado durante el 2011 caracteriza los métodos de enseñanza en Física con estudiantes del cuarto año, modalidad a distancia en el Instituto sabatino “Esperanza”, barrio “Sol de Libertad”, municipio de Siuna, Región Autónomas Atlántico Norte (RAAN). Fue cualitativo y describe los métodos de enseñanza aplicados en Física. Se realizaron entrevistas, revisión documental y observación directa. Según los resultados, el docente es graduado en Ciencias de la Educación con mención en Biología, una profesión afín con la Física. El método que el docente aplica es predominantemente expositivo que es apropiado, pero se abusa de él así como de los mismos materiales didácticos como textos, pizarra, tizas, en ocasiones papelógrafos.SummaryThis study conducted in 2011 characterizes the teaching methods in Physics with fourth year students, through distance learning at the “Esperanza” Sabbath Institute, located in the “Sol de Libertad” neighborhood, municipality of Siuna, North Atlantic Autonomous Region (RAAN). The investigation was qualitative and it describes the teaching methods applied in Physics. Interviews, document review, and direct observation were carried out. According to the results, the teacher has a degree in Science Education with a major in Biology, a profession related to Physics. The method that is applied by the teacher is predominantly expositive, which is appropriate, but he abuses of it as well as of the teaching materials such as texts, blackboard, chalk, and sometimes flipcharts.
COMPORTAMIENTO DISCIPLINARIO EN LA ESCUELA “NIÑO JESÚS”, SIUNA, REGIÓN AUTÓNOMA ATLÁNTICO NORTE, 2011
Authors: Montenegro Flores Rosa Francisca , Hernández Herrera Reina Isabel , Ruiz Calderón Angélica Leonor 
Published: February 2016

El estudio se realizó en el Centro Escolar “Niño Jesús” del barrio “Dolores Marín”, sector urbano del municipio de Siuna, Región Autónoma Atlántico Norte (RAAN), a 334 km de la capital Managua. El objetivo fue determinar el comportamiento disciplinario con una población de estudio de 82 niñas y 103 niños del centro educativo, 7 docentes, 1 director, 78 padres y madres de familia. Destacándose que los factores sociales que han afectado el comportamiento disciplinario en la niñez es producto de la educación brindada desde el entorno familiar. En la etapa de la niñez se está propenso a tener problemas conductuales, cuando se es afectado por la situación económica, su condición de vida, el estado emocional, la desintegración familiar y la pedagogía inadecuada; asimismo, el papel que ha desempeñado la Consejería Escolar en este contexto en la orientación e implementación de planes pedagógicos para resolver los diferentes problemas. La investigación fue cualitativa de carácter descriptivo. Las técnicas empleadas fueron: grupo focal, entrevista y observación directa en las aulas de clase.SummaryThe study was conducted at the “Niño Jesus” School, located in the “Dolores Marin” neighborhood, urban sector of Siuna Municipality, North Atlantic Autonomous Region (RAAN), at a distance of 334 km from the capital Managua. The objective was to determine the disciplinary behavior with a study population of 82 girls and 103 boys of the school, 7 teachers, 1 director, and 78 fathers and mothers. We highlight that the social factors that have affected the disciplinary behavior in the childhood is a product of the education provided from the family environment. In the stage of childhood is likely to have behavioral problems, when someone is affected by the economic situation, their living conditions, emotional state, family disintegration and an inadequate pedagogy; also the role played by the School Counseling in this context is very important in the orientation and implementation of educational plans to solve different problems. The research was qualitative -descriptive. The techniques used were: focus group interview and direct observation in the classroom.
MA-KUAGRO: ELEMENTO DE LA CULTURA PALENQUERA Y SU INCIDENCIA EN LAS PRÁCTICAS PEDAGÓGICAS EN LA ESCUELA, SAN BASILIO PALENQUE, COLOMBIA
Authors: De Ávila Torres Dimas Del Rosario , Simarra Obeso Rutsely 
Published: February 2016

La investigación analizó los elementos de la cultura palenquera presentes en la escuela, particularmente “kuagro” que es manifestación organizativa propia, y su vínculo con las prácticas pedagógicas del personal docente y el aprovechamiento académico estudiantil. Este estudio aporta al proceso etno-educativo llevado a cabo en San Basilio de Palenque y otras comunidades culturalmente diferenciadas en Colombia. La investigación fue de tipo cualitativo, se hizo uso del método de la consulta a la memoria colectiva, creado por la comunidad palenquera en el marco del proceso de etno-educación. Las técnicas y herramientas fueron la observación, entrevista y conversatorios con docentes, estudiantes, líderes y lideresas, miembros del consejo comunitario. Entre los resultados se menciona que existe una articulación en la Institución Educativa Benkos Biohó y la comunidad, ya que el acervo cultural es el eje principal de las prácticas pedagógicas. Entre estos, se ha incluido los patios productivos, las ceremonias fúnebres, la música, entre otros, con la participación de la gente anciana y sabia de la comunidad. Sin embargo, a pesar de lo anterior, los saberes y prácticas pedagógicas son diversos desde la perspectiva de los docentes sensibilizados, no sensibilizados y los que están en proceso de sensibilización. Los docentes sensibilizados han logrado un mejor desempeño académico en los estudiantes.Summary The research analyzed the elements of the palenque culture that are present in the school, particularly "kuagro" that it’s his own organizational manifestation, and its link with the teachers pedagogical practices and student achievement. This study contributes to the ethno-educational process conducted in San Basilio de Palenque and other communities in Colombia that are culturally different. The research was qualitative; we made use of the method of consulting the collective memory, created by the palenque community in the framework of the ethno-education process. The techniques and tools that guided the investigation were: the observation, interviews and conversations with teachers, students, women and men leaders, as well as with the members of the community council. Among the results we can highlight that there is an articulation between the Benkos Bioho educational institution and the community, being that cultural heritage is the axis of the teaching practices. Among these, we have included the productive yards, funeral ceremonies, music, among others, with the participation of the wise and elderly people in the community. However, despite this, the knowledge and pedagogical practices are different from the perspective of sensitized teachers, non-sensitized and those in processes of sensitization. Sensitized teachers have achieved a better academic performance in students.