bluuebunny/crossref_metadata_2025_split huggingface dataset:
Editorial
Authors: González Guillén Manuel de Jesús 
Published: May 2018

En México, han existido cuatro enfoques filosóficos de uso y aprovechamiento de los recursos forestales: el utilitarismo, el conservacionismo, el uso múltiple y el uso sustentable. Cada uno con una concepción diferente del papel que deben tener los recursos naturales y cómo ser aprovechados y administrados por sus dueños.
La perspectiva utilitarista (1521-1950), se basó en lograr el bien individual y colectivo a través de la satisfacción de las necesidades humanas básicas, sin considerar la escasez de los recursos. Lo anterior tuvo consecuencias en la disminución y deterioro de los mismos, que se tradujo en descontentos y presiones sociales. Como resultado, el gobierno promovió un cambio de enfoque, y surgió el conservacionismo (1950 - 1970), el cual prohibió el uso y aprovechamiento de muchos de los bosques; con ello, se intentó que estos se recuperaran. Dicho enfoque logró lo contrario: cambios de uso de la tierra, incendios, sobrepastoreo, cortas clandestinas y un desinterés en el cultivo forestal. Criterios económicos característicos de los recursos como: utilidad, escasez, valor y disponibilidad en tiempo y forma, no fueron alcanzados.
Biomasa de Lupinus mutabilis Sweet y su efecto en el suelo
Authors: Pomboza-Tamaquiza Pedro Pablo , Aldas Juan Carlos , Buenaño Marcia 
Published: May 2018

El objetivo del trabajo fue cuantificar la biomasa de Lupinus mutabilis Sweet mediante métodos dendométricos y el aporte en macronutrientes de la biomasa incorporada al suelo como abono verde. EL ensayo de campo, se realizó en la Granja de la Facultad de Ciencias Agropecuarias de la Universidad Técnica de Ambato, ubicada en Querochaca, a una altitud de 2990 msnm. Se cultivó Lupinus mutabilis Sweet en una parcela de 480 m2 hasta la floración y se incorporó al suelo. Antes de incorporar se seleccionaron aleatoriamente 30 plantas, de las cuales se tomaron datos de diámetros, longitudes, pesos de tallos y ramas, se calculó la biomasa utilizando formulas volumétricas, adicionalmente se realizaron análisis químicos de suelo, antes de la siembra y 45 días después de incorporado la biomasa al suelo. Como resultado, se desarrolló un modelo de regresión lineal múltiple para estimar el volumen de biomasa de esta especie, a partir de conocer la altura de la planta y el diámetro basal del tallo. Los análisis de suelos mostraron que la biomasa de L. mutabilis Sweet incrementaron la materia orgánica en 490%, el nitrógeno en 500% y el fósforo en 200%
Efecto del consumo voluntario de Leucaena leucocephala sobre la degradación ruminal de la materia orgánica en ovinos
Authors: Barros-Rodríguez Marcos , Sólorio-Sánchez Javier , Sandoval-Castro Carlos 
Published: May 2018

Se evaluó el efecto de la ingestión de Leucaena leucocephala sobre la degradación ruminal de MO del Pennisetum purpureum y L. leucocephala. El experimento se realizó en Facultad de Medicina Veterinaria y Zootecnia de la Universidad Autónoma de Yucatán, Se utilizaron 9 ovinos canulados en el rumen tres por tratamiento con un peso promedio de 34 ± 3.45 Kg en los que se evaluaron tres tratamientos; T1 sólo pasto, T2 leucaena (40%) pasto (60%) y T3 leucaena (20%) pasto (80%), para ello se utilizó la técnica de degradación in situ con bolsas de nylon en el rumen. Se mostró un efecto entre los tratamientos T2 y T3, ante el T1, con respecto a la tasa de degradación (% hora), manteniendo la misma tendencia para los dos forrajes evaluados. No obstante, los demás parámetros de degradación evaluados no marcaron diferencia (P>0.05) para ambos sustratos en todos los tratamientos. Se concluye que la incorporación de leucaena en la dieta favorece la tasa de degradación de la MO
Medieval Hunting and Wood Management in the Buzzart Dykes Landscape
Authors: Malloy Kevin , Hall Derek 
Published: May 2018

Abstract
Whilst research into medieval park landscapes has been limited in Scotland, recent efforts to enhance our understanding of the design, construction and functions of these structures through archaeological methods have been fruitful. This paper discusses the results of excavations at the site of Buzzart Dykes in Perthshire. As the site lacks historical documentation, little was known about how and when it was constructed and managed. Here we evaluate the modern interpretation of the enclosure as a medieval park used for hunting, and present evidence for additional economic utilisations that revolved around wood management. Excavations of the park bounds and associated longhouse structure clarify the landscape history of Buzzart Dykes, and demonstrate an effective methodology for studying park landscapes in Scotland.
Engagement et appartenances : les vies des magistrats Étienne de Lestang (1510-1581) et Antoine de Lestang (1541-1617)
Authors: Cassan Michel 
Published: May 2018

Fondé sur un important corpus de sources, l’article propose une reconstitution des itinéraires de deux magistrats brivistes, fervents catholiques très engagés dans la lutte contre le protestantisme, Étienne de Lestang (vers 1510-1581) et son fils
Antoine de Lestang (1541-1617). La méthode retenue ¢ l’histoire sociale nominative qui emprunte une partie de sa démarche à la microstoria ¢ permet d’interroger la diversité des engagements définis comme des manifestations du «je » liées à la part de liberté dont dispose chaque individu dans une société de type holiste. Les deux cas questionnent les effets d’engagements religieux comparables sur des appartenances plurielles, professionnelles, sociales, communautaires, politiques. Ils démontrent la singularité de chaque existence qui doit composer avec des contingences surplombantes, susceptibles de ruiner des appartenances ou difficilement compatibles avec un engagement.
On the Detectability of Planet X with LSST
Authors: Trilling David E. , Bellm Eric C. , Malhotra Renu 
Published: May 2018

Abstract
Two planetary mass objects in the far outer solar system—collectively referred to here as Planet X— have recently been hypothesized to explain the orbital distribution of distant Kuiper Belt Objects. Neither planet is thought to be exceptionally faint, but the sky locations of these putative planets are poorly constrained. Therefore, a wide area survey is needed to detect these possible planets. The Large Synoptic Survey Telescope (LSST) will carry out an unbiased, large area (around 18000 deg2), deep (limiting magnitude of individual frames of 24.5) survey (the “wide-fast-deep (WFD)” survey) of the southern sky beginning in 2022, and it will therefore be an important tool in searching for these hypothesized planets. Here, we explore the effectiveness of LSST as a search platform for these possible planets. Assuming the current baseline cadence (which includes the WFD survey plus additional coverage), we estimate that LSST will confidently detect or rule out the existence of Planet X in 61% of the entire sky. At orbital distances up to ∼75 au, Planet X could simply be found in the normal nightly moving object processing; at larger distances, it will require custom data processing. We also discuss the implications of a nondetection of Planet X in LSST data.
The Clustering of High-redshift (2.9 ≤ z ≤ 5.1) Quasars in SDSS Stripe 82
Authors: Timlin John D. , Ross Nicholas P. , Richards Gordon T. , Myers Adam D. , Pellegrino Andrew , Bauer Franz E. , Lacy Mark , Schneider Donald P. , Wollack Edward J. , Zakamska Nadia L. 
Published: May 2018

Abstract
We present a measurement of the two-point autocorrelation function of photometrically selected high-z quasars over ∼100 deg2 on the Sloan Digital Sky Survey Stripe 82 field. Selection is performed using three machine-learning algorithms in a six-dimensional optical/mid-infrared color space. Optical data from the Sloan Digital Sky Survey are combined with overlapping deep mid-infrared data from the Spitzer IRAC Equatorial Survey and the Spitzer-HETDEX Exploratory Large-Area survey. Our selection algorithms are trained on the colors of known high-z quasars. The selected quasar sample consists of 1378 objects and contains both spectroscopically confirmed quasars and photometrically selected quasar candidates. These objects span a redshift range of 2.9 ≤ z ≤ 5.1 and are generally fainter than i = 20.2, a regime that has lacked sufficient number density to perform autocorrelation function measurements of photometrically classified quasars. We compute the angular correlation function of these data, marginally detecting quasar clustering. We fit a single power law with an index of δ = 1.39 ± 0.618 and amplitude of θ
0 = 0.′71 ± 0.′546 . A dark matter model is fit to the angular correlation function to estimate the linear bias. At the average redshift of our survey (

), the bias is b = 6.78 ± 1.79. Using this bias, we calculate a characteristic dark matter halo mass of 1.70–9.83

. Our bias estimate suggests that quasar feedback intermittently shuts down the accretion of gas onto the central supermassive black hole at early times. If confirmed, these results hint at a level of luminosity dependence in the clustering of quasars at high-z.
Generation of a Large-scale Magnetic Field in a Convective Full-sphere Cross-helicity Dynamo
Authors: Pipin V. V. , Yokoi N. 
Published: May 2018

Abstract
We study the effects of the cross-helicity in the full-sphere large-scale mean-field dynamo models of a 0.3 M
⊙ star rotating with a period of 10 days. In exploring several dynamo scenarios that stem from magnetic field generation by the cross-helicity effect, we found that the cross-helicity provides the natural generation mechanisms for the large-scale scale axisymmetric and nonaxisymmetric magnetic field. Therefore, the rotating stars with convective envelopes can produce a large-scale magnetic field generated solely due to the turbulent cross-helicity effect (we call it γ
2-dynamo). Using mean-field models we compare the properties of the large-scale magnetic field organization that stems from dynamo mechanisms based on the kinetic helicity (associated with the α
2 dynamos) and cross-helicity. For the fully convective stars, both generation mechanisms can maintain large-scale dynamos even for the solid body rotation law inside the star. The nonaxisymmetric magnetic configurations become preferable when the cross-helicity and the α-effect operate independently of each other. This corresponds to situations with purely γ
2 or α
2 dynamos. The combination of these scenarios, i.e., the γ
2
α
2 dynamo, can generate preferably axisymmetric, dipole-like magnetic fields at strengths of several kGs. Thus, we found a new dynamo scenario that is able to generate an axisymmetric magnetic field even in the case of a solid body rotation of the star. We discuss the possible applications of our findings to stellar observations.
The Peculiar Radial Distribution of Multiple Populations in the Massive Globular Cluster M80
Authors: Dalessandro E. , Cadelano M. , Vesperini E. , Salaris M. , Ferraro F. R. , Lanzoni B. , Raso S. , Hong J. , Webb J. J. , Zocchi A. 
Published: May 2018

Abstract
We present a detailed analysis of the radial distribution of light-element multiple populations (LE-MPs) in the massive and dense globular cluster M80, based on a combination of UV and optical Hubble Space Telescope data. Surprisingly, we find that first-generation (FG) stars (FG) are significantly more centrally concentrated than extreme second-generation (SG) stars out to ∼2.5r

h
from the cluster center. To understand the origin of such peculiar behavior, we used a set of N-body simulations following the long-term dynamical evolution of LE-MPs. We find that, given the advanced dynamical state of the cluster, the observed difference does not depend on the primordial relative distributions of FG and SG stars. On the contrary, a difference of ∼0.05–0.10 M
⊙ between the average masses of the two subpopulations is needed to account for the observed radial distributions. We argue that such a mass difference might be the result of the higher He abundance of SG stars (of the order of ΔY ∼ 0.05–0.06) with respect to FG stars. Interestingly, we find that a similar He variation is necessary to reproduce the horizontal branch morphology of M80. These results demonstrate that differences in mass among LE-MPs, due to different He content, should be properly taken into account for a correct interpretation of their radial distribution, at least in dynamically evolved systems.
A Particle Module for the PLUTO Code. I. An Implementation of the MHD–PIC Equations
Authors: Mignone A. , Bodo G. , Vaidya B. , Mattia G. 
Published: May 2018

Abstract
We describe an implementation of a particle physics module available for the PLUTO code appropriate for the dynamical evolution of a plasma consisting of a thermal fluid and a nonthermal component represented by relativistic charged particles or cosmic rays (CRs). While the fluid is approached using standard numerical schemes for magnetohydrodynamics, CR particles are treated kinetically using conventional Particle-In-Cell (PIC) techniques. The module can be used either to describe test-particle motion in the fluid electromagnetic field or to solve the fully coupled magnetohydrodynamics (MHD)–PIC system of equations with particle backreaction on the fluid as originally introduced by Bai et al. Particle backreaction on the fluid is included in the form of momentum–energy feedback and by introducing the CR-induced Hall term in Ohm’s law. The hybrid MHD–PIC module can be employed to study CR kinetic effects on scales larger than the (ion) skin depth provided that the Larmor gyration scale is properly resolved. When applicable, this formulation avoids resolving microscopic scales, offering substantial computational savings with respect to PIC simulations. We present a fully conservative formulation that is second-order accurate in time and space, and extends to either the Runge–Kutta (RK) or the corner transport upwind time-stepping schemes (for the fluid), while a standard Boris integrator is employed for the particles. For highly energetic relativistic CRs and in order to overcome the time-step restriction, a novel subcycling strategy that retains second-order accuracy in time is presented. Numerical benchmarks and applications including Bell instability, diffusive shock acceleration, and test-particle acceleration in reconnecting layers are discussed.
The Dust and [C ii] Morphologies of Redshift ∼4.5 Sub-millimeter Galaxies at ∼200 pc Resolution: The Absence of Large Clumps in the Interstellar Medium at High-redshift
Authors: Gullberg B. , Swinbank A. M. , Smail I. , Biggs A. D. , Bertoldi F. , Breuck C. De , Chapman S. C. , Chen C.-C. , Cooke E. A. , Coppin K. E. K. , Cox P. , Dannerbauer H. , Dunlop J. S. , Edge A. C. , Farrah D. , Geach J. E. , Greve T. R. , Hodge J. , Ibar E. , Ivison R. J. , Karim A. , Schinnerer E. , Scott D. , Simpson J. M. , Stach S. M. , Thomson A. P. , van der Werf P. , Walter F. , Wardlow J. L. , Weiss A. 
Published: May 2018

Abstract
We present deep, high-resolution (0.″03, 200 pc) ALMA Band 7 observations covering the dust continuum and [C ii] λ157.7 μm emission in four z ∼ 4.4–4.8 sub-millimeter galaxies (SMGs) selected from the ALESS and AS2UDS surveys. The data show that the rest-frame 160 μm (observed 345 GHz) dust emission is consistent with smooth morphologies on kpc scales for three of the sources. One source, UDS 47.0, displays apparent substructure, but this is also consistent with a smooth morphology—as indicated by simulations showing that smooth exponential disks can appear clumpy when observed at the high angular resolution (0.″03) and depth of these observations (

μJy beam−1). The four SMGs are bright [C ii] emitters. We extract [C ii] spectra from the high-resolution data, and recover ∼20%–100% of the [C ii] flux and ∼40%–80% of the dust continuum emission, compared to the previous lower-resolution observations. When tapered to 0.″2 resolution, our maps recover ∼80%–100% of the continuum emission, indicating that ∼60% of the emission is resolved out on ∼200 pc scales. We find that the [C ii] emission in high-redshift galaxies is more spatially extended than the rest-frame 160 μm dust continuum by a factor of 1.6 ± 0.4. By considering the

/

ratio as a function of the star formation rate surface density (

), we revisit the [C ii] deficit and suggest that the decline in the

/

ratio as a function of

is consistent with local processes. We also explore the physical drivers that may be responsible for these trends and can give rise to the properties found in the densest regions of SMGs.
Dust Attenuation Curves in the Local Universe: Demographics and New Laws for Star-forming Galaxies and High-redshift Analogs
Authors: Salim Samir , Boquien Médéric , Lee Janice C. 
Published: May 2018

Abstract
We study the dust attenuation curves of 230,000 individual galaxies in the local universe, ranging from quiescent to intensely star-forming systems, using GALEX, SDSS, and WISE photometry calibrated on the Herschel ATLAS. We use a new method of constraining SED fits with infrared luminosity (SED+LIR fitting), and parameterized attenuation curves determined with the CIGALE SED-fitting code. Attenuation curve slopes and UV bump strengths are reasonably well constrained independently from one another. We find that

attenuation curves exhibit a very wide range of slopes that are on average as steep as the curve slope of the Small Magellanic Cloud (SMC). The slope is a strong function of optical opacity. Opaque galaxies have shallower curves—in agreement with recent radiative transfer models. The dependence of slopes on the opacity produces an apparent dependence on stellar mass: more massive galaxies have shallower slopes. Attenuation curves exhibit a wide range of UV bump amplitudes, from none to Milky Way (MW)-like, with an average strength one-third that of the MW bump. Notably, local analogs of high-redshift galaxies have an average curve that is somewhat steeper than the SMC curve, with a modest UV bump that can be, to first order, ignored, as its effect on the near-UV magnitude is 0.1 mag. Neither the slopes nor the strengths of the UV bump depend on gas-phase metallicity. Functional forms for attenuation laws are presented for normal star-forming galaxies, high-z analogs, and quiescent galaxies. We release the catalog of associated star formation rates and stellar masses (GALEX–SDSS–WISE Legacy Catalog 2).
The Mochi LabJet Experiment for Measurements of Canonical Helicity Injection in a Laboratory Astrophysical Jet
Authors: You Setthivoine , von der Linden Jens , Lavine Eric Sander , Carroll Evan Grant , Card Alexander , Quinley Morgan , Azuara-Rosales Manuel 
Published: May 2018

Abstract
The Mochi device is a new pulsed power plasma experiment designed to produce long, collimated, stable, magnetized plasma jets when set up in the LabJet configuration. The LabJet configuration aims to simulate an astrophysical jet in the laboratory by mimicking an accretion disk threaded by a poloidal magnetic field with concentric planar electrodes in front of a solenoidal coil. The unique setup consists of three electrodes, each with azimuthally symmetric gas slits. Two of the electrodes are biased independently with respect to the third electrode to control the radial electric field profile across the poloidal bias magnetic field. This design approximates a shear azimuthal rotation profile in an accretion disk. The azimuthally symmetric gas slits provide a continuously symmetric mass source at the footpoint of the plasma jet, so any azimuthal rotation of the plasma jet is not hindered by a discrete number of gas holes. The initial set of diagnostics consists of current Rogowski coils, voltage probes, magnetic field probe arrays, an interferometer and ion Doppler spectroscopy, supplemented by a fast ion gauge and a retarding grid energy analyzer. The measured parameters of the first plasmas are ∼1022 m−3, ∼0.4 T, and 5–25 eV, with velocities of ∼20–80 km s−1. The combination of a controllable electric field profile, a flared poloidal magnetic field, and azimuthally symmetric mass sources in the experiment successfully produces short-lived (∼10 μs, ≳5 Alfvén times) collimated magnetic jets with a ∼10:1 aspect ratio and long-lived (∼100 μs, ≳40 Alfvén times) flow-stabilized, collimated, magnetic jets with a ∼30:1 aspect ratio.
New Y and T Dwarfs from WISE Identified by Methane Imaging*

†
Authors: Tinney C. G. , Kirkpatrick J. Davy , Faherty Jacqueline K. , Mace Gregory N. , Cushing Mike , Gelino Christopher R. , Burgasser Adam J. , Sheppard Scott S. , Wright Edward L. 
Published: May 2018

Abstract
We identify new Y- and T-type brown dwarfs from the WISE All Sky data release using images obtained in filters that divide the traditional near-infrared H and J bands into two halves—specifically

and CH4l in the H and J2, and J3 in the J. This proves to be very effective at identifying cool brown dwarfs via the detection of their methane absorption, as well as providing preliminary classification using methane colors and WISE -to-near-infrared colors. New and updated calibrations between T/Y spectral types and

–CH4l J3–W2, and

–W2 colors are derived, producing classification estimates good to a few spectral sub-types. We present photometry for a large sample of T and Y dwarfs in these filters, together with spectroscopy for 23 new ultra-cool dwarfs—2 Y dwarfs and 21 T dwarfs. We identify a further 8 new cool brown dwarfs, which we have high confidence are T dwarfs based on their methane photometry. We find that, for objects observed on a 4 m class telescope at J-band magnitudes of ∼20 or brighter,

–CH4l is the more powerful color for detecting objects and then estimating spectral types. Due to the lower sky background in the J-band, the J3 and J2 bands are more useful for identifying fainter cool dwarfs at J ≳ 22. The J3–J2 color is poor at estimating spectral types. But fortunately, once J3–J2 confirms that an object is a cool dwarf, the J3–W2 color is very effective at estimating approximate spectral types.