bluuebunny/crossref_metadata_2025_split huggingface dataset:
BAT AGN Spectroscopic Survey. I. Spectral Measurements, Derived Quantities, and AGN Demographics
Authors: Koss Michael , Trakhtenbrot Benny , Ricci Claudio , Lamperti Isabella , Oh Kyuseok , Berney Simon , Schawinski Kevin , Baloković Mislav , Baronchelli Linda , Crenshaw D. Michael , Fischer Travis , Gehrels Neil , Harrison Fiona , Hashimoto Yasuhiro , Hogg Drew , Ichikawa Kohei , Masetti Nicola , Mushotzky Richard , Sartori Lia , Stern Daniel , Treister Ezequiel , Ueda Yoshihiro , Veilleux Sylvain , Winter Lisa 
Published: November 2017

Abstract
We present the first catalog and data release of the Swift-BAT AGN Spectroscopic Survey. We analyze optical spectra of the majority of the detected AGNs (77%, 642/836)based on their 14–195 keV emission in the 70-month Swift-BAT all-sky catalog. This includes redshift determination, absorption and emission-line measurements, and black hole mass and accretion rate estimates for the majority of obscured and unobscured AGNs (74%, 473/642), with 340 measured for the first time. With ∼90% of sources at

, the survey represents a significant advance in the census of hard X-ray-selected AGNs in the local universe. In this first catalog paper, we describe the spectroscopic observations and data sets, and our initial spectral analysis. The FWHMs of the emission lines show broad agreement with the X-ray obscuration (∼94%), such that Sy 1–1.8 have

cm−2, and Seyfert 2 have

cm−2. Seyfert 1.9, however, show a range of column densities. Compared to narrow-line AGNs in the SDSS, the X-ray-selected AGNs have a larger fraction of dusty host galaxies (

), suggesting that these types of AGN are missed in optical surveys. Using the [O iii] λ5007/Hβ and [N ii] λ6583/Hα emission-line diagnostic, about half of the sources are classified as Seyferts; ∼15% reside in dusty galaxies that lack an Hβ detection, but for which the upper limits on line emission imply either a Seyfert or LINER,

are in galaxies with weak or no emission lines despite high-quality spectra, and a few percent each are LINERS, composite galaxies, H ii regions, or in known beamed AGNs.
A New 3D Multi-fluid Dust Model: A Study of the Effects of Activity and Nucleus Rotation on Dust Grain Behavior at Comet 67P/Churyumov–Gerasimenko
Authors: Shou Y. , Combi M. , Toth G. , Tenishev V. , Fougere N. , Jia X. , Rubin M. , Huang Z. , Hansen K. , Gombosi T. 
Published: November 2017

Abstract
Improving our capability to interpret observations of cometary dust is necessary to deepen our understanding of the role of dust in the formation of comets and in altering the cometary environments. Models including dust grains are in demand to interpret observations and test hypotheses. Several existing models have taken into account the gas–dust interaction, varying sizes of dust grains and the cometary gravitational force. In this work, we develop a multi-fluid dust model based on the BATS-R-US code. This model not only incorporates key features of previous dust models, but also has the capability of simulating time-dependent phenomena. Since the model is run in the rotating comet reference frame, the centrifugal and Coriolis forces are included. The boundary conditions on the nucleus surface can be set according to the distribution of activity and the solar illumination. The Sun revolves around the comet in this frame. A newly developed numerical mesh is also used to resolve the real-shaped nucleus in the center and to facilitate prescription of the outer boundary conditions that accommodate the rotating frame. The inner part of the mesh is a box composed of Cartesian cells and the outer surface is a smooth sphere, with stretched cells filled in between the box and the sphere. Our model achieved comparable results to the Direct Simulation Monte Carlo method and the Rosetta/OSIRIS observations. It is also applied to study the effects of the rotating nucleus and the cometary activity and offers interpretations of some dust observations of comet 67P/Churyumov–Gerasimenko.
A Detailed Study of the Interstellar Protons toward the TeV γ-Ray SNR RX J0852.0–4622 (G266.2–1.2, Vela Jr.): The Third Case of the γ-Ray and ISM Spatial Correspondence
Authors: Fukui Y. , Sano H. , Sato J. , Okamoto R. , Fukuda T. , Yoshiike S. , Hayashi K. , Torii K. , Hayakawa T. , Rowell G. , Filipović M. D. , Maxted N. , McClure-Griffiths N. M. , Kawamura A. , Yamamoto H. , Okuda T. , Mizuno N. , Tachihara K. , Onishi T. , Mizuno A. , Ogawa H. 
Published: November 2017

Abstract
We present a new analysis of the interstellar protons toward the TeV γ-ray SNR RX J0852.0−4622 (G266.2−1.2, Vela Jr.). We used the NANTEN2 12CO(J = 1–0) and Australia Telescope Compact Array and Parkes H i data sets in order to derive the molecular and atomic gas associated with the TeV γ-ray shell of the SNR. We find that atomic gas over a velocity range from V
LSR = −4 to 50 km s−1 or 60 km s−1 is associated with the entire SNR, while molecular gas is associated with a limited portion of the SNR. The large velocity dispersion of the H i is ascribed to the expanding motion of a few H i shells overlapping toward the SNR but is not due to the Galactic rotation. The total masses of the associated H i and molecular gases are estimated to be

M
⊙ and ∼103
M
⊙, respectively. A comparison with the High Energy Stereoscopic System TeV γ-rays indicates that the interstellar protons have an average density around 100 cm−3 and shows a good spatial correspondence with the TeV γ-rays. The total cosmic-ray proton energy is estimated to be ∼1048 erg for the hadronic γ-ray production, which may still be an underestimate by a factor of a few due to a small filling factor of the SNR volume by the interstellar protons. This result presents a third case, after RX J1713.7−3946 and HESS J1731−347, of the good spatial correspondence between the TeV γ-rays and the interstellar protons, lending further support for a hadronic component in the γ-rays from young TeV γ-ray SNRs.
Gas-phase Absorptions of
near 8300 Å below 10 K: Astronomical Implications
Authors: Campbell E. K. , Maier J. P. 
Published: November 2017

Abstract
The gas-phase electronic spectrum of

(

) with an origin band at

has been measured below

by photofragmentation of helium complexes (

) in a radiofrequency trap.

is a medium-sized polycyclic aromatic hydrocarbon (PAH) cation, and using an ion trapping technique it has been possible to record a high-quality gas-phase spectrum to directly compare with astronomical observations. No diffuse interstellar bands (DIBs) have been reported at the wavelengths of the strongest absorption bands in the

spectrum. Measurement of absolute absorption cross sections in the ion trap allows upper limits to the column density of this ion to be

, indicating that even PAH cations of this size, which are believed to be stable in the interstellar medium, should be excluded as candidates for at least the strong DIBs.
Calibrating Star Formation in WISE Using Total Infrared Luminosity
Authors: Cluver M. E. , Jarrett T. H. , Dale D. A. , Smith J.-D. T. , August Tamlyn , Brown M. J. I. 
Published: November 2017

Abstract
We present accurate resolved WISE photometry of galaxies in the combined SINGS and KINGFISH sample. The luminosities in the W3 12 μm and W4 23 μm bands are calibrated to star formation rates (SFRs) derived using the total infrared luminosity, avoiding UV/optical uncertainties due to dust extinction corrections. The W3 relation has a 1σ scatter of 0.15 dex that is over nearly 5 orders of magnitude in SFR and 12 μm luminosity, and a range in host stellar mass from dwarfs (107

) to

(1011.5

) galaxies. In the absence of deep silicate absorption features and powerful active galactic nuclei, we expect this to be a reliable SFR indicator chiefly due to the broad nature of the W3 band. By contrast, the W4 SFR relation shows more scatter (1

dex). Both relations show reasonable agreement with radio-continuum-derived SFRs and excellent accordance with so-called “hybrid” Hα + 24 μm and FUV+24 μm indicators. Moreover, the WISE SFR relations appear to be insensitive to the metallicity range in the sample. We also compare our results with IRAS-selected luminous infrared galaxies, showing that the WISE relations maintain concordance, but systematically deviate for the most extreme galaxies. Given the all-sky coverage of WISE and the performance of the W3 band as an SFR indicator, the

SFR relation could be of great use to studies of nearby galaxies and forthcoming large-area surveys at optical and radio wavelengths.
Rapid Formation of Black Holes in Galaxies: A Self-limiting Growth Mechanism
Authors: Li Zhi , Sellwood J. A. , Shen Juntai 
Published: November 2017

Abstract
We present high-quality fluid dynamical simulations of isothermal gas flows in a rotating barred potential. We show that a large quantity of gas is driven right into the nucleus of a galaxy when the model lacks a central mass concentration, but the inflow stalls at a nuclear ring in comparison simulations that include a central massive object. The radius of the nuclear gas ring increases linearly with the mass of the central object. We argue that bars drive gas right into the nucleus in the early stages of disk galaxy formation, where a nuclear star cluster and perhaps a massive black hole could be created. The process is self-limiting, however, because inflow stalls at a nuclear ring once the mass of gas and stars in the nucleus exceeds ∼1% of the disk mass, which shuts off rapid growth of the black hole. We briefly discuss the relevance of these results to the seeding of massive black holes in galaxies, the merger model for quasar evolution, and the existence of massive black holes in disk galaxies that lack a significant classical bulge.
Characterizing the Motion of Solar Magnetic Bright Points at High Resolution
Authors: Van Kooten Samuel J. , Cranmer Steven R. 
Published: November 2017

Abstract
Magnetic bright points in the solar photosphere, visible in both continuum and G-band images, indicate footpoints of kilogauss magnetic flux tubes extending to the corona. The power spectrum of bright-point motion is thus also the power spectrum of Alfvén wave excitation, transporting energy up flux tubes into the corona. This spectrum is a key input in coronal and heliospheric models. We produce a power spectrum of bright-point motion using radiative magnetohydrodynamic simulations, exploiting spatial resolution higher than can be obtained in present-day observations, while using automated tracking to produce large data quantities. We find slightly higher amounts of power at all frequencies compared to observation-based spectra, while confirming the spectrum shape of recent observations. This also provides a prediction for observations of bright points with DKIST, which will achieve similar resolution and high sensitivity. We also find a granule size distribution in support of an observed two-population distribution, and we present results from tracking passive tracers, which show a similar power spectrum to that of bright points. Finally, we introduce a simplified, laminar model of granulation, with which we explore the roles of turbulence and of the properties of the granulation pattern in determining bright-point motion.
Feeding versus Falling: The Growth and Collapse of Molecular Clouds in a Turbulent Interstellar Medium
Authors: Ibáñez-Mejía Juan C. , Mac Low Mordecai-Mark , Klessen Ralf S. , Baczynski Christian 
Published: November 2017

Abstract
In order to understand the origin of observed molecular cloud (MC) properties, it is critical to understand how clouds interact with their environments during their formation, growth, and collapse. It has been suggested that accretion-driven turbulence can maintain clouds in a highly turbulent state, preventing runaway collapse and explaining the observed non-thermal velocity dispersions. We present 3D, adaptive-mesh-refinement, magnetohydrodynamical simulations of a kiloparsec-scale, stratified, supernova-driven, self-gravitating, interstellar medium (ISM), including diffuse heating and radiative cooling. These simulations model the formation and evolution of a MC population in the turbulent ISM. We use zoom-in techniques to focus on the dynamics of the mass accretion and its history for individual MCs. We find that mass accretion onto MCs proceeds as a combination of turbulent flow and near free-fall accretion of a gravitationally bound envelope. Nearby supernova explosions have a dual role, compressing the envelope and increasing mass accretion rates, but also disrupting parts of the envelope and eroding mass from the cloud’s surface. It appears that the inflow rate of kinetic energy onto clouds from supernova explosions is insufficient to explain the net rate of change of the cloud kinetic energy. In the absence of self-consistent star formation, the conversion of gravitational potential into kinetic energy during contraction seems to be the main driver of non-thermal motions within clouds. We conclude that although clouds interact strongly with their environments, bound clouds are always in a state of gravitational contraction, close to runaway, and their properties are a natural result of this collapse.
Quiescent Prominence Dynamics Observed with the Hinode Solar Optical Telescope. II. Prominence Bubble Boundary Layer Characteristics and the Onset of a Coupled Kelvin–Helmholtz Rayleigh–Taylor Instability
Authors: Berger Thomas , Hillier Andrew , Liu Wei 
Published: November 2017

Abstract
We analyze solar quiescent prominence bubble characteristics and instability dynamics using Hinode/Solar Optical Telescope data. We measure the bubble expansion rate, prominence downflows, and the profile of the boundary layer brightness and thickness as a function of time. The largest bubble analyzed rises into the prominence with a speed of about

1.3

km

s

−
1

until it is destabilized by a localized shear flow on the boundary. Boundary layer thickness grows gradually as prominence downflows deposit plasma onto the bubble with characteristic speeds of

20
–
35

km

s

−
1

. Lateral downflows initiate from the thickened boundary layer with characteristic speeds of

25
–
50

km

s

−
1

, “draining” the layer of plasma. Strong shear flow across one bubble boundary leads to an apparent coupled Kelvin–Helmholtz Rayleigh–Taylor (KH–RT) instability. We measure shear flow speeds above the bubble of

10

km

s

−
1

and infer interior bubble flow speeds on the order of

100

km

s

−
1

. Comparing the measured growth rate of the instability to analytic expressions, we infer a magnetic flux density across the bubble boundary of ∼10−3 T (10 Gauss) at an angle of

∼
70
°

to the prominence plane. The results are consistent with the hypothesis that prominence bubbles are caused by magnetic flux that emerges below a prominence, setting up the conditions for RT, or combined KH–RT, instability flows that transport flux, helicity, and hot plasma upward into the overlying coronal magnetic flux rope.
Pre-explosion Spiral Mass Loss of a Binary Star Merger
Authors: Pejcha Ondřej , Metzger Brian D. , Tyles Jacob G. , Tomida Kengo 
Published: November 2017

Abstract
Binary stars commonly pass through phases of direct interaction, which result in the rapid loss of mass, energy, and angular momentum. Though crucial to understanding the fates of these systems, including their potential as gravitational wave sources, this short-lived phase is poorly understood and has thus far been unambiguously observed in only a single event, V1309 Sco. Here we show that the complex and previously unexplained photometric behavior of V1309 Sco prior to its main outburst results naturally from the runaway loss of mass and angular momentum from the outer Lagrange point, which lasts for thousands of orbits prior to the final dynamical coalescence, much longer than predicted by contemporary models. This process enshrouds the binary in a “death spiral” outflow, which affects the amplitude and phase modulation of its light curve, and contributes to driving the system together. The total amount of mass lost during this gradual phase (

) rivals the mass lost during the subsequent dynamical interaction phase, which has been the main focus of “common envelope” modeling so far. Analogous features in related transients suggest that this behavior is ubiquitous.
L’anticipation du prédicat dans l’argument externe
Authors: Cadiot Pierre 
Published: November 2017

Résumé Notre objectif est de montrer certaines difficultés inhérentes à la notion de prédicat sémantique dans sa corrélation avec un argument externe. On présente successivement la question des requalifications du rôle « sujet » (ou argument externe), l’opposition prédicativité forte vs prédicativité faible, le conflit entre référence présupposée et fond thématique, puis des éléments d’approfondissement de l’opposition jugement thétique / jugement catégorique.
Phrase nominale, « parties du discours » et théorie syntaxique
Authors: de Carvalho Paulo 
Published: November 2017

Résumé On défend ici, avec des arguments et des développements théoriques nouveaux, une position tenue depuis plus de 20 ans, qui consiste à affirmer, contre une tradition encore solidement ancrée, que la phrase dite « canonique », engendrée, dans les langues indo-européennes occidentales modernes, et singulièrement en français, par instanciation d’un vocable verbal, ne recouvre pas, loin s’en faut, tout le champ de la syntaxe : il y a urgence à reconnaître l’existence d’un « cas premier », ou « primaire », de phrase, qu’il faut bien appeler « nominale », plutôt qu’« averbale ». On la définira comme une « phrase-prédicat », engendrée par l’apport, à un support pré-linguistique, d’une expression nominale, identifiante ou qualifiante, et en elle-même plus ou moins complexe. De cette référence, qui lui est consubstantielle, au « présent locutif », ou « énonciatif » – à distinguer du présent « délocuté » – la phrase nominale tire son apport significatif spécifique : ce n’est pas du monde, et de ce qui (s’) y passe, qu’elle parle, mais, plutôt, de l’instant locutif lui-même, et, en fin de compte, de « moi hic et nunc », qui instaure celui-ci. La démonstration passera par une reformulation, en termes de « personne » (invariable vs variable), de l’opposition NOM vs VERBE.
The Role of Macrophages in the Response to TNF Inhibition in Experimental Arthritis
Authors: Huang Qi-Quan , Birkett Robert , Doyle Renee , Shi Bo , Roberts Elyssa L. , Mao Qinwen , Pope Richard M. 
Published: November 2017

Abstract
The reduction of synovial tissue macrophages is a reliable biomarker for clinical improvement in patients with rheumatoid arthritis (RA), and macrophages are reduced in synovial tissue shortly after initiation of TNF inhibitors. The mechanism for this initial response is unclear. These studies were performed to identify the mechanisms responsible for the initial reduction of macrophages following TNF inhibition, positing that efflux to draining lymph nodes was involved. RA synovial tissue and synovial fluid macrophages expressed CCR7, which was increased in control macrophages following incubation with TNF-α. Human TNF transgenic (hTNF-Tg) mice were treated with infliximab after development of arthritis. Ankles were harvested and examined by histology, immunohistochemistry, quantitative RT-PCR, ELISA, and flow cytometry. hTNF-Tg mice treated with infliximab demonstrated significant clinical and histologic improvement 3 d after the initiation of therapy, at which time Ly6C+ macrophages were significantly reduced in the ankles. However, no evidence was identified to support a role of macrophage efflux to draining lymph nodes following treatment with infliximab. In contrast, apoptosis of Ly6C+ macrophages in the ankles and popliteal lymph nodes, decreased migration of monocytes into the ankles, and a reduction of CCL2 were identified following the initiation of infliximab. These observations demonstrate that Ly6C+ macrophage apoptosis and decreased ingress of circulating monocytes into the joint are responsible for the initial reduction of macrophages following infliximab treatment in hTNF-Tg mice.
Teachers’ perceptions of reading instruction in selected primary schools in the Eastern Cape
Authors: Cekiso Madoda 
Published: November 2017

Background: There is a general outcry that too many South African Foundation Phase (Grades 1–3) teachers do not know how to teach reading and are currently teaching reading in an ad hoc, unsystematic way.Objectives: In response to this, this study explored the Foundation Phase teachers’ perceptions of their role in teaching reading. The focus was on the relevance of the initial training, awareness of reading strategies and how these strategies were reflected in their classroom practice.Method: The study was qualitative in nature and a case study design was followed. Semi-structured interviews were conducted with nine teachers who were purposively selected from three public schools. Content analysis was used to analyse the data.Results: Regarding the initial training programme, teachers received at tertiary institutions, the findings of the study showed that the majority of teachers were not adequately prepared to teach reading and to deal with learners who experience problems in reading. Some teachers indicated that they were not even trained to teach in the Foundation Phase. The findings also showed that the majority of respondents doubted if their classroom practice would yield positive results as far as reading instruction is concerned. The findings further indicated that the majority of respondents only paid attention to oral reading (observing punctuation marks and pronunciation), without attending to reading comprehension. There was a general consensus that the new ways of teaching reading were necessary in order to improve the reading ability of learners.Conclusion: Recommendations based on the findings are that institutions of higher learning that train Foundation Phase teachers should do so in ways that adequately equip them to produce student teachers who are knowledgeable about research and theory regarding how individuals learn to read. Workshops on appropriate instruction of reading strategies are recommended for in-service teachers.