bluuebunny/crossref_metadata_2025_split huggingface dataset:
THE EVOLUTION OF THE FAINT END OF THE UV LUMINOSITY FUNCTION DURING THE PEAK EPOCH OF STAR FORMATION
*
Authors: Alavi Anahita , Siana Brian , Richard Johan , Rafelski Marc , Jauzac Mathilde , Limousin Marceau , Freeman William R. , Scarlata Claudia , Robertson Brant , Stark Daniel P. , Teplitz Harry I. , Desai Vandana 
Published: November 2016

ABSTRACT
We present a robust measurement of the rest-frame UV luminosity function (LF) and its evolution during the peak epoch of cosmic star formation at

. We use our deep near-ultraviolet imaging from WFC3/UVIS on the Hubble Space Telescope and existing Advanced Camera for Surveys (ACS)/WFC and WFC3/IR imaging of three lensing galaxy clusters, Abell 2744 and MACS J0717 from the Hubble Frontier Field survey and Abell 1689. Combining deep UV imaging and high magnification from strong gravitational lensing, we use photometric redshifts to identify 780 ultra-faint galaxies with

AB mag at

. From these samples, we identified five new, faint, multiply imaged systems in A1689. We run a Monte Carlo simulation to estimate the completeness correction and effective volume for each cluster using the latest published lensing models. We compute the rest-frame UV LF and find the best-fit faint-end slopes of

,

, and

at

,

, and

, respectively. Our results demonstrate that the UV LF becomes steeper from

to

with no sign of a turnover down to

AB mag. We further derive the UV LFs using the Lyman break “dropout” selection and confirm the robustness of our conclusions against different selection methodologies. Because the sample sizes are so large and extend to such faint luminosities, the statistical uncertainties are quite small, and systematic uncertainties (due to the assumed size distribution, for example) likely dominate. If we restrict our analysis to galaxies and volumes above

completeness in order to minimize these systematics, we still find that the faint-end slope is steep and getting steeper with redshift, though with slightly shallower (less negative) values (

, −1.69 ± 0.07, and −1.79 ± 0.08 for

, 1.9, and 2.6, respectively). Finally, we conclude that the faint star-forming galaxies with UV magnitudes of

covered in this study produce the majority (55%–60%) of the unobscured UV luminosity density at

.
PROPINQUITY OF CURRENT AND VORTEX STRUCTURES: EFFECTS ON COLLISIONLESS PLASMA HEATING
Authors: Parashar Tulasi N , Matthaeus William H 
Published: November 2016

ABSTRACT
Intermittency of heating in weakly collisional plasma turbulence is an active subject of research, with significant potential impact on understanding of the solar wind, solar corona, and astrophysical plasmas. Recent studies suggest a role of vorticity in plasma heating. In magnetohydrodynamics small-scale vorticity is generated near current sheets and this effect persists in kinetic plasma, as demonstrated here with hybrid and fully kinetic particle-in-cell simulations. Furthermore, vorticity enhances local kinetic effects, with a generalized resonance condition selecting sign-dependent enhancements or reductions of proton heating and thermal anisotropy. In such plasmas heating is correlated with vorticity and current density, but more strongly with vorticity. These results help explain several prior results that find kinetic effects and energization near to, but not centered on, current sheets. Evidently intermittency in kinetic plasma involves multiple physical quantities, and the associated coherent structures and nonthermal effects are closely related.
PHOTOMETRIC MONITORING OF THE COLDEST KNOWN BROWN DWARF WITH THE SPITZER SPACE TELESCOPE*
Authors: Esplin T. L. , Luhman K. L. , Cushing M. C. , Hardegree-Ullman K. K. , Trucks J. L. , Burgasser A. J. , Schneider A. C. 
Published: November 2016

ABSTRACT
Because WISE J085510.83−071442.5 (hereafter WISE 0855-0714) is the coldest known brown dwarf (∼250 K) and one of the Sun’s closest neighbors (2.2 pc), it offers a unique opportunity to study a planet-like atmosphere in an unexplored regime of temperature. To detect and characterize inhomogeneities in its atmosphere (e.g., patchy clouds, hot spots), we have performed time-series photometric monitoring of WISE 0855-0714 at 3.6 and 4.5 μm with the Spitzer Space Telescope during two 23 hr periods that were separated by several months. For both bands, we have detected variability with peak-to-peak amplitudes of 4%–5% and 3%–4% in the first and second epochs, respectively. The light curves are semiperiodic in the first epoch for both bands, but they are more irregular in the second epoch. Models of patchy clouds have predicted a large increase in mid-infrared (mid-IR) variability amplitudes (for a given cloud covering fraction) with the appearance of water ice clouds at T
eff < 375 K, so if such clouds are responsible for the variability of WISE 0855-0714, then its small amplitudes of variability indicate a very small deviation in cloud coverage between hemispheres. Alternatively, the similarity in mid-IR variability amplitudes between WISE 0855-0714 and somewhat warmer T and Y dwarfs may suggest that they share a common origin for their variability (i.e., not water clouds). In addition to our variability data, we have examined other constraints on the presence of water ice clouds in the atmosphere of WISE 0855-0714, including the recent mid-IR spectrum from Skemer et al. (2016). We find that robust evidence of such clouds is not yet available.
CONSTRAINING THE SOLAR CORONAL MAGNETIC FIELD STRENGTH USING SPLIT-BAND TYPE II RADIO BURST OBSERVATIONS
Authors: Kishore P. , Ramesh R. , Hariharan K. , Kathiravan C. , Gopalswamy N. 
Published: November 2016

ABSTRACT
We report on low-frequency radio (85–35 MHz) spectral observations of four different type II radio bursts, which exhibited fundamental-harmonic emission and split-band structure. Each of the bursts was found to be closely associated with a whitelight coronal mass ejection (CME) close to the Sun. We estimated the coronal magnetic field strength from the split-band characteristics of the bursts, by assuming a model for the coronal electron density distribution. The choice of the model was constrained, based on the following criteria: (1) when the radio burst is observed simultaneously in the upper and lower bands of the fundamental component, the location of the plasma level corresponding to the frequency of the burst in the lower band should be consistent with the deprojected location of the leading edge (LE) of the associated CME; (2) the drift speed of the type II bursts derived from such a model should agree closely with the deprojected speed of the LE of the corresponding CMEs. With the above conditions, we find that: (1) the estimated field strengths are unique to each type II burst, and (2) the radial variation of the field strength in the different events indicate a pattern. It is steepest for the case where the heliocentric distance range over which the associated burst is observed is closest to the Sun, and vice versa.
EXPLORING THE TRANSIENT RADIO SKY WITH VLITE: EARLY RESULTS
Authors: Polisensky E. , Lane W. M. , Hyman S. D. , Kassim N. E. , Giacintucci S. , Clarke T. E. , Cotton W. D. , Cleland E. , Frail D. A. 
Published: November 2016

ABSTRACT
We report on a search for radio transients at 340 MHz with the Jansky Very Large Array Low-band Ionosphere and Transient Experiment (VLITE). Between 2015 July 29 and September 27, operating in commensal mode, VLITE imaged approximately 2800 pointings covering 12,000 deg2 on the sky, sampling timescales ranging from tens of seconds to several hours on a daily basis. In addition, between 2015 February 25 and May 9, VLITE observed 55 epochs of roughly 2–4 hr each toward the COSMOS field. Using existing radio source catalogs, we have searched all of the daily VLITE images for transients, while for the COSMOS field we compared individual images and the summed image to search for new sources in repeated observations of the same field. The wide range of timescales makes VLITE sensitive to both coherent and incoherent transient source classes. No new transients are found, allowing us to set stringent upper limits on transients at milli-jansky levels and at low frequencies where comparatively few such surveys have been carried out to date. An all-sky isotropic surface density of bursting radio transients with similar rates, durations, and intensities as the unusual transient GCRT J1745−3009, discovered in wide-field monitoring toward the Galactic center, is ruled out with high confidence. The resulting non-detections allows us to argue that this is a coherent source, whose properties most resemble the growing class of nulling pulsars. We end with a discussion of the future prospects for the detection of transients by VLITE and other experiments.
DISCOVERY OF A POSSIBLE COOL WHITE DWARF COMPANION FROM THE AllWISE MOTION SURVEY
Authors: Fajardo-Acosta Sergio B. , Kirkpatrick J. Davy , Schneider Adam C. , Cushing Michael C. , Stern Daniel , Gelino Christopher R. , Bardalez-Gagliuffi Daniella C. , Kellogg Kendra , Wright Edward L. 
Published: November 2016

ABSTRACT
We present optical and near-infrared spectroscopy of WISEA J061543.91−124726.8, which we rediscovered as a high motion object in the AllWISE survey. The spectra of this object are unusual; while the red optical (λ > 7000 Å) and near-infrared spectra exhibit characteristic TiO, VO, and H2O bands of a late-M dwarf, the blue portion of its optical spectrum shows a significant excess of emission relative to late-M-type templates. The excess emission is relatively featureless, with the exception of a prominent and very broad Na i D doublet. We find that no single, ordinary star can reproduce these spectral characteristics. The most likely explanation is an unresolved binary system of an M7 dwarf and a cool white dwarf. The flux of a cool white dwarf drops in the optical red and near-infrared, due to collision-induced absorption, thus allowing the flux of a late-M dwarf to show through. This scenario, however, does not explain the Na D feature, which is unlike that of any known white dwarf, but which could perhaps be explained via unusual abundance or pressure conditions.
HARD X-RAY ASYMMETRY LIMITS IN SOLAR FLARE CONJUGATE FOOTPOINTS
Authors: Daou Antoun G. , Alexander David 
Published: November 2016

ABSTRACT
The transport of energetic electrons in a solar flare is modeled using a time-dependent one-dimensional Fokker–Planck code that incorporates asymmetric magnetic convergence. We derive the temporal and spectral evolution of the resulting hard X-ray (HXR) emission in the conjugate chromospheric footpoints, assuming thick target photon production, and characterize the time evolution of the numerically simulated footpoint asymmetry and its relationship to the photospheric magnetic configuration. The thick target HXR asymmetry in the conjugate footpoints is found to increase with magnetic field ratio as expected. However, we find that the footpoint HXR asymmetry saturates for conjugate footpoint magnetic field ratios ≥4. This result is borne out in a direct comparison with observations of 44 double-footpoint flares. The presence of such a limit has not been reported before, and may serve as both a theoretical and observational benchmark for testing a range of particle transport and flare morphology constraints, particularly as a means to differentiate between isotropic and anisotropic particle injection.
LONG-TERM TRENDS IN THE SOLAR WIND PROTON MEASUREMENTS
Authors: Elliott Heather A. , McComas David J. , DeForest Craig E. 
Published: November 2016

ABSTRACT
We examine the long-term time evolution (1965–2015) of the relationships between solar wind proton temperature (T
p) and speed (V
p) and between the proton density (n
p) and speed using OMNI solar wind observations taken near Earth. We find a long-term decrease in the proton temperature–speed (T
p–V
p) slope that lasted from 1972 to 2010, but has been trending upward since 2010. Since the solar wind proton density–speed (n
p–V
p) relationship is not linear like the T
p–V
p relationship, we perform power-law fits for n
p–V
p. The exponent (steepness in the n
p–V
p relationship) is correlated with the solar cycle. This exponent has a stronger correlation with current sheet tilt angle than with sunspot number because the sunspot number maxima vary considerably from cycle to cycle and the tilt angle maxima do not. To understand this finding, we examined the average n
p for different speed ranges, and found that for the slow wind n
p is highly correlated with the sunspot number, with a lag of approximately four years. The fast wind n
p variation was less, but in phase with the cycle. This phase difference may contribute to the n
p–V
p exponent correlation with the solar cycle. These long-term trends are important since empirical formulas based on fits to T
p and V
p data are commonly used to identify interplanetary coronal mass ejections, but these formulas do not include any time dependence. Changes in the solar wind density over a solar cycle will create corresponding changes in the near-Earth space environment and the overall extent of the heliosphere.
THE ORBIT, ROTATION, AND GRANULATION OF THE G7 GIANT β Her
Authors: Gray David F. 
Published: November 2016

ABSTRACT
The G7 IIIa single-lined spectroscopic binary, β Her, is studied with high-resolution, high-signal-to-noise spectra taken over 10 seasons from 23MR2000 to 10MY2009. Absolute radial velocities, corrected for convective blueshifts, are determined and new orbital parameters are derived. Line-depth ratios are used to measure temperature variation ∼2 K. A Fourier analysis is done for the line broadening, yielding a projected rotation velocity of 3.27 ± 0.20 km s−1 and a radial–tangential macroturbulence dispersion of 6.43 ± 0.08 km s−1. The “C” shaped bisector of Fe i
λ6253 has its blue-most point at a relative flux level of 0.52, consistent with what is expected from β Her’s absolute magnitude. The third-signature plot indicates granulation velocities 20% larger than the Sun’s. Mapping the λ6253 line bisector onto the third-signature curve results in a flux deficit of 12.6 ± 1.0% that can be interpreted as arising from a temperature difference between granules and inter-granular lanes of 132 K. The flux deficit peaks near 5.5 km s−1 from the line center, suggesting the velocity difference between granules and lanes is ∼20% larger than that found for recently analyzed K giants.
THE SAMI GALAXY SURVEY: GALAXY INTERACTIONS AND KINEMATIC ANOMALIES IN ABELL 119
Authors: Oh Sree , Yi Sukyoung K. , Cortese Luca , Sande Jesse van de , Mahajan Smriti , Jeong Hyunjin , Sheen Yun-Kyeong , Allen James T. , Bekki Kenji , Bland-Hawthorn Joss , Bloom Jessica V. , Brough Sarah , Bryant Julia J. , Colless Matthew , Croom Scott M. , Fogarty L. M. R. , Goodwin Michael , Green Andy , Konstantopoulos Iraklis S. , Lawrence Jon , López-Sánchez Á. R. , Lorente Nuria P. F. , Medling Anne M. , Owers Matt S. , Richards Samuel , Scott Nicholas , Sharp Rob , Sweet Sarah M. 
Published: November 2016

ABSTRACT
Galaxy mergers are important events that can determine the fate of a galaxy by changing its morphology, star formation activity and mass growth. Merger systems have commonly been identified from their disturbed morphologies, and we now can employ integral field spectroscopy to detect and analyze the impact of mergers on stellar kinematics as well. We visually classified galaxy morphology using deep images (

) taken by the Blanco 4 m telescope at the Cerro Tololo Inter-American Observatory. In this paper we investigate 63 bright (

) spectroscopically selected galaxies in Abell 119, of which 53 are early type and 20 show a disturbed morphology by visual inspection. A misalignment between the major axes in the photometric image and the kinematic map is conspicuous in morphologically disturbed galaxies. Our sample is dominated by early-type galaxies, yet it shows a surprisingly tight Tully–Fisher relation except for the morphologically disturbed galaxies which show large deviations. Three out of the eight slow rotators in our sample are morphologically disturbed. The morphologically disturbed galaxies are generally more asymmetric, visually as well as kinematically. Our findings suggest that galaxy interactions, including mergers and perhaps fly-bys, play an important role in determining the orientation and magnitude of a galaxy’s angular momentum.
THE CHANDRA COSMOS LEGACY SURVEY: CLUSTERING OF X-RAY-SELECTED AGNs AT 2.9 ≤ z ≤ 5.5 USING PHOTOMETRIC REDSHIFT PROBABILITY DISTRIBUTION FUNCTIONS
Authors: Allevato V. , Civano F. , Finoguenov A. , Marchesi S. , Shankar F. , Zamorani G. , Hasinger G. , Salvato M. , Miyaji T. , Gilli R. , Cappelluti N. , Brusa M. , Suh H. , Lanzuisi G. , Trakhtenbrot B. , Griffiths R. , Vignali C. , Schawinski K. , Karim A. 
Published: November 2016

ABSTRACT
We present the measurement of the projected and redshift-space two-point correlation function (2pcf) of the new catalog of Chandra COSMOS-Legacy active galactic nucleus (AGN) at 2.9 ≤ z ≤ 5.5 (

〈

L

bol

〉

∼

1046 erg s−1) using the generalized clustering estimator based on phot-z probability distribution functions in addition to any available spec-z. We model the projected 2pcf, estimated using π
max = 200 h−1 Mpc with the two-halo term and we derive a bias at z ∼ 3.4 equal to b =

6.6

−
0.55

+
0.60

, which corresponds to a typical mass of the hosting halos of log M
h =

12.83

−
0.11

+
0.12

h−1
M
⊙. A similar bias is derived using the redshift-space 2pcf, modeled including the typical phot-z error σ

z
= 0.052 of our sample at z ≥ 2.9. Once we integrate the projected 2pcf up to π
max = 200 h−1 Mpc, the bias of XMM and Chandra COSMOS at z = 2.8 used in Allevato et al. is consistent with our results at higher redshifts. The results suggest only a slight increase of the bias factor of COSMOS AGNs at z ≳ 3 with the typical hosting halo mass of moderate-luminosity AGNs almost constant with redshift and equal to log M
h =

12.92

−
0.18

+
0.13

at z = 2.8 and log M
h =

12.83

−
0.11

+
0.12

at z ∼ 3.4, respectively. The observed redshift evolution of the bias of COSMOS AGNs implies that moderate-luminosity AGNs still inhabit group-sized halos at z ≳ 3, but slightly less massive than observed in different independent studies using X-ray AGNs at z ≤ 2.
Histoire de Laura : une protestation du soi
Authors: Conesa Élisabeth 
Published: November 2016

Le soi est présent chez l’enfant dès le début de sa vie. Celui-ci n’a pas les mots, mais sous la poussée du soi, soi corporel et soi relationnel œuvrant de concert, il peut protester et se faire entendre. En reprenant le cours d’une thérapie d’enfant, l’auteure donne à voir une protestation du soi qui est « authentifiée » par l’analyste dans sa fonction de soi relationnel.
La réception perdue : La monadologie démontrée de Michael Gottlieb Hansch
Authors: Pelletier Arnaud 
Published: November 2016

La première réception de la philosophie leibnizienne ne s’est certainement pas réduite à sa reprise dans le soi-disant « système leibnizo-wolffien », qui fut le prisme majoritaire, et déformant, de la lecture de Leibniz au xviii	e	siècle. Au contraire, Michael Gottlieb Hansch, traducteur de la Monadologie en latin, essaya de s’élever contre cette réappropriation de l’héritage leibnizien et de présenter le « vrai » Leibniz hors de tout système leibnizo-wolffien. Il se proposa alors d’expliciter les propositions parfois denses de la Monadologie à partir de Leibniz lui-même, et en particulier de leur correspondance privée. Sa correspondance l’incite aussi à proposer une lecture « platonisante » de la Monadologie . À bien des égards, cette réception perdue révèle simplement des aspects encore largement méconnus de la philosophie leibnizienne.
Idéalité de la monade et réalité de la « monadologie » : sur un lieu commun de l’interprétation
Authors: Fichant Michel 
Published: November 2016

Depuis Léon Brunschvicg s’est établie une sorte de lieu commun de l’interprétation de la métaphysique de Leibniz, dont la cohérence serait compromise par la contradiction entre la monade, pour qui l’espace est idéal, et la « monadologie » ou système de toutes les monades coexistantes, qui présupposerait un réalisme de l’espace. Dans cet article, l’argument de Brunschvicg est reconstitué, puis critiqué par la restitution de la pensée réelle de Leibniz sur les rapports entre monade et espace : on ne doit en aucun cas se représenter la pluralité des monades comme une multiplicité spatiale – l’espace est un ordre non des substances simples, mais des phénomènes, – seule l’union constante et universelle de chaque monade à un corps organique permet de parler d’un « point de vue », qui n’est autre que la localisation de ce corps parmi les autres et non de la monade qui, en tant que telle, n’a pas de lieu.
Au-delà de la philosophie
Authors: Gädeke Nora , Leloutre Françoise 
Published: November 2016

Dans l’édition historique et critique de Leibniz, la série I ( Correspondance générale, politique et historique ) est la série la plus volumineuse, la plus avancée et aussi la moins connue. Le fait qu’à côté des noms célèbres et des grandes problématiques qui concernent les autres séries de correspondances (philosophie ainsi que mathématiques et physique), elle contienne une foule de petites nouvelles et de correspondants de « second rang » a conduit dans le cours de l’édition à une critique fondamentale. Cependant, non seulement parce que la multitude des thèmes reflète l’état du discours de l’époque, en deçà même du mainstream , et qu’entrent en scène nombre de « lettrés » dont l’activité serait autrement oubliée. Mais la conservation exceptionnellement bonne du fonds épistolaire rend aussi possible de suivre en détail le parcours des nouvelles. L’édition de Leibniz devient ainsi une ressource pour la République des Lettres et un atelier pour les recherches sur la culture épistolaire de l’époque.
Human Basophils Modulate Plasma Cell Differentiation and Maturation
Authors: Dijkstra Dorothea , Meyer-Bahlburg Almut 
Published: November 2016

Abstract
Basophils represent &lt;1% of circulating leukocytes. They play a crucial role during allergy and helminth-induced Th2 responses. However, recent data also suggest a contribution to the pathogenesis of autoimmune diseases. Basophils from patients with systemic lupus erythematosus show an activated phenotype, correlating to disease activity. Furthermore, murine basophils or their mediators enhance memory responses and plasma cell (PC) survival, suggesting that they directly modulate the function of B cells. This is highly relevant with respect to human allergy and autoimmunity because a possible modulation of B cell differentiation by basophils could point to new therapeutic targets. Therefore, the interaction between human B cells and basophils and the mechanism underlying this interaction were investigated in detail. Using two different methods to induce PC differentiation, we found that human basophils enhance B cell proliferation, class switching, differentiation into PC, maturation of PC, and production of Igs, especially IgG. Basophil supernatants enhanced the expression of the B cell markers CD23 and CD40, which are important for B cell differentiation into IgG-producing PC. This was mainly IL-4 dependent. IL-3 amplified the number of PC in vitro, and acted synergistically with basophils in enhancing Ab production. Thus, human basophils modulate B cell differentiation into Ab-producing PC. Their contribution as modulators and effectors during allergy and autoimmunity should be considered when designing new therapeutic options.
The Gradient Superconvergence of Bilinear Finite Volume Element for Elliptic Problems
Authors: Zhang Tie , Tang Lixin 
Published: November 2016

AbstractWe study the gradient superconvergence of bilinear finite volume element (FVE) solving the elliptic problems. First, a superclose weak estimate is established for the bilinear form of the FVE method. Then, we prove that the gradient approximation of the FVE solution has the superconvergence property:where denotes the average gradient on elements containing point P and S is the set of optimal stress points composed of the mesh points, the midpoints of edges and the centers of elements.