bluuebunny/crossref_metadata_2025_split huggingface dataset:
The effects of velocity on peak torque and neuromuscular responses during eccentric muscle actions
Authors: Hill Ethan C. , Housh Terry J. , Camic Clayton L. , Jenkins Nathaniel D.M. , Smith Cory M. , Cochrane Kristen C. , Cramer Joel T. , Schmidt Richard J. , Monaghan Molly M. , Johnson Glen O. 
Published: March 2016

BACKGROUND: Previous investigations have examined the torque and neuromuscular responses to maximal concentric and isometric muscle actions. The literature, however, has paid less attention to the effects of performing maximal eccentric muscle actions. Furthermore, the available information in this regard is contradictory. OBJECTIVE: The purpose of the present investigation was to examine eccentric, isokinetic peak moment (PMe), electromyographic (EMG) amplitude (AMP), EMG mean power frequency (MPF), mechanomyographic (MMG) AMP, and MMG MPF patterns of responses to repeated, maximal, eccentric muscle actions at 60, 120, and 180°/s. METHODS: Twelve resistance-trained men visited the laboratory on three occasions (separated by ≥ 72 h) and performed 30 repeated, maximal, eccentric muscle actions of the dominant leg extensors on an isokinetic dynamometer at randomly ordered velocities of 60, 120, and 180°/s. RESULTS: There were no changes (p > 0.05) across the 30 repeated, eccentric muscle actions for PMe, MMG AMP, and EMG MPF for any of the velocities. There were, however, increases in EMG AMP and decreases in MMG MPF for each velocity. CONCLUSIONS: The decrease in MMG MPF, which reflects the global firing rate of the activated motor units, in conjunction with the lack of change in MMG AMP, which reflects motor unit recruitment, suggested that the increase in EMG AMP was due to motor unit synchronization.
Comparison of knee extension concentric fatigue between repetition ranges
Authors: McLeland Kathryn A. , Ruas Cassio V. , Arevalo Jose A. , Bagley James R. , Ciccone Anthony B. , Brown Lee E. , Coburn Jared W. , Galpin Andrew J. , Malyszek Kylie K. 
Published: March 2016

BACKGROUND: Anaerobic fatigue is a limiting factor in performance and athletes are often tested to determine their fatigue resistance. Administering the classic Thorstensson test of fatigability is a popular method to determine fatigue percentage as it requires 50 maximal knee extension repetitions. However, there has been little research to determine whether performing more or fewer repetitions yields similar results. OBJECTIVE: The purpose of this study was to compare concentric fatigue percentage (FP) between the classic Thorstensson test (CT; average of first 3 repetitions to average of last 3 repetitions) and three different repetition ranges: peak torque repetition to repetition 30 (P30), peak torque repetition to repetition 50 (P50), and peak torque repetition to repetition 60 (P60). METHODS: Fifteen resistance trained men (age = 24.8 ± 1.3 yrs; height = 178.9 ± 5.1 cm; mass = 82.2 ± 8.0 kg) volunteered to perform 60 maximal concentric knee extension repetitions at 180°/s on an isokinetic dynamometer, measuring peak torque of each repetition. RESULTS: P30 (r= 0.81) and P50 (r= 0.77) were highly correlated with CT but P60 (r= 0.58) was only moderately correlated with CT. P30 FP (44.7 ± 8.8) was significantly less than CT (62.3 ± 6.0), P50 (66.0 ± 6.8) and P60 (69.7 ± 7.1). CONCLUSION: FP can be determined through fewer repetitions of a knee extension fatigue test on an isokinetic dynamometer. While both P30 and P50 were highly correlated with CT, performing fewer repetitions requires less time to complete as well as less residual fatigue. When measuring knee extension FP, the number of repetitions performed in the test may be reduced to 30 while still maintaining a high correlation to a longer method of 50.
LARGE MAGELLANIC CLOUD NEAR-INFRARED SYNOPTIC SURVEY. II. THE WESENHEIT RELATIONS AND THEIR APPLICATION TO THE DISTANCE SCALE
Authors: Bhardwaj Anupam , Kanbur Shashi M. , Macri Lucas M. , Singh Harinder P. , Ngeow Chow-Choong , Wagner-Kaiser R. , Sarajedini Ata 
Published: March 2016

ABSTRACT
We present new near-infrared (NIR) Cepheid period–Wesenheit (P–W) relations in the LMC using time-series observations from the Large Magellanic Cloud NIR Synoptic Survey. We also derive optical+NIR P–W relations using V and I magnitudes from the Optical Gravitational Lensing Experiment. We employ our new JHK

s
data to determine an independent distance to the LMC of

(statistical) mag, using an absolute calibration of the Galactic relations based on several distance determination methods and accounting for the intrinsic scatter of each technique. We also derive new NIR period–luminosity and Wesenheit relations for Cepheids in M31 using observations from the Panchromatic Hubble Andromeda Treasury survey. We use the absolute calibrations of the Galactic and LMC

relations to determine the distance modulus of M31,

mag. We apply a simultaneous fit to Cepheids in several Local Group galaxies covering a range of metallicities (

dex) to determine a global slope of −3.244 ± 0.016 mag dex−1 for the

relation and obtain robust distance estimates. Our distances are in good agreement with recent TRGB based distance estimates and we do not find any evidence for a metallicity dependence in the NIR P–W relations.
HATS-17b: A TRANSITING COMPACT WARM JUPITER IN A 16.3 DAY CIRCULAR ORBIT*
Authors: Brahm R. , Jordán A. , Bakos G. Á. , Penev K. , Espinoza N. , Rabus M. , Hartman J. D. , Bayliss D. , Ciceri S. , Zhou G. , Mancini L. , Tan T. G. , de Val-Borro M. , Bhatti W. , Csubry Z. , Bento J. , Henning T. , Schmidt B. , Rojas F. , Suc V. , Lázár J. , Papp I. , Sári P. 
Published: March 2016

ABSTRACT
We report the discovery of HATS-17b, the first transiting warm Jupiter of the HATSouth network. HATS-17b transits its bright (V = 12.4) G-type (

=

,

=

) metal-rich ([Fe/H] = +0.3 dex) host star in a circular orbit with a period of P =

days. HATS-17b has a very compact radius of

given its Jupiter-like mass of

. Up to 50% of the mass of HATS-17b may be composed of heavy elements in order to explain its high density with current models of planetary structure. HATS-17b is the longest period transiting planet discovered to date by a ground-based photometric survey, and is one of the brightest transiting warm Jupiter systems known. The brightness of HATS-17 will allow detailed follow-up observations to characterize the orbital geometry of the system and the atmosphere of the planet.
STAR FORMATION BLACK HOLE GROWTH AND DUSTY TORI IN THE MOST LUMINOUS AGNS AT Z = 2–3.5
Authors: Netzer Hagai , Lani Caterina , Nordon Raanan , Trakhtenbrot Benny , Lira Paulina , Shemmer Ohad 
Published: March 2016

ABSTRACT
We report Herschel/SPIRE observations of 100 very luminous, optically selected active galactic nuclei (AGNs) at

with

(erg s−1) ≥ 46.5 , where

is λL

λ
at 1350 Å. The distribution in

is similar to the general distribution of Sloan Digital Sky Survey AGNs in this redshift and luminosity interval. We measured star-formation (SF) luminosity,

, and SF rate (SFR) in 34 detected sources by fitting combined SF and torus templates, where the torus emission is based on Wide Field Infrared Survey Explorer observations. We also obtained statistically significant stacks for the undetected sources in two luminosity groups. The sample properties are compared with those of very luminous AGNs at

. The main findings are: (1) The mean and the median SFRs of the detected sources are

and

M
⊙ yr−1, respectively. The mean SFR of the undetected sources is 148 M
⊙ yr−1. The ratio of SFR to the black hole accretion rate is ≈80 for the detected sources and less than 10 for the undetected sources. Unlike a sample of sources at z ≃ 4.8 that we studied recently, there is no difference in

and only a very small difference in

between the detected and undetected sources. (2) The redshift distribution of

and

for the most luminous, redshift 2–7 AGNs are different. Similar to previous studies, the highest

are found at z ≈ 3. However, the

of such sources peaks at z ≈ 5. Assuming the objects in our sample are hosted by the most massive galaxies at those redshifts, we find that approximately 2/3 of the hosts are already below the main sequence of SF galaxies at z = 2−3.5. (3) The spectral energy distributions (SEDs) of dusty tori at high redshift are similar to the shapes found in low redshift, low luminosity AGNs. Herschel upper limits put strong constraints on the long wavelength shape of the SED, ruling out several earlier suggested torus templates as applicable for this sample. (4) We find no evidence for a luminosity dependence of the torus covering factor in sources with

(erg s−1) = 44−47.5. This conclusion is based on the recognition that the estimated

in several earlier studies is highly uncertain and non-uniformally treated. The median covering factors over this range are 0.68 for isotropic dust emission and 0.4 for anisotropic emission.
SYNTHESIZING EXOPLANET DEMOGRAPHICS: A SINGLE POPULATION OF LONG-PERIOD PLANETARY COMPANIONS TO M DWARFS CONSISTENT WITH MICROLENSING, RADIAL VELOCITY, AND DIRECT IMAGING SURVEYS
Authors: Clanton Christian , Gaudi B. Scott 
Published: March 2016

ABSTRACT
We present the first study to synthesize results from five different exoplanet surveys using three independent detection methods: microlensing, radial velocity, and direct imaging. The constraints derived herein represent the most comprehensive picture of the demographics of large-separation (≳2 AU) planets orbiting the most common stars in our Galaxy that has been constructed to date. We assume a simple, joint power-law planet distribution function of the form

with an outer cutoff radius of the separation distribution function of a
out. Generating populations of planets from these models and mapping them into the relevant observables for each survey, we use actual or estimated detection sensitivities to determine the expected observations for each survey. Comparing with the reported results, we derive constraints on the parameters

that describe a single population of planets that is simultaneously consistent with the results of microlensing, radial velocity, and direct imaging surveys. We find median and 68% confindence intervals of

(

),

(

),

(

), and

AU (

AU) assuming “hot-start” (“cold-start”) planet evolutionary models. These values are consistent with all current knowledge of planets on orbits beyond ∼2 AU around single M dwarfs.
TYPE Ia SUPERNOVAE: CAN CORIOLIS FORCE BREAK THE SYMMETRY OF THE GRAVITATIONAL CONFINED DETONATION EXPLOSION MECHANISM?
Authors: García-Senz D. , Cabezón R. M. , Domínguez I. , Thielemann F. K. 
Published: March 2016

ABSTRACT
Currently the number of models aimed at explaining the phenomena of type Ia supernovae is high and distinguishing between them is a must. In this work we explore the influence of rotation on the evolution of the nuclear flame that drives the explosion in the so-called gravitational confined detonation models. Assuming that the flame starts in a pointlike region slightly above the center of the white dwarf (WD) and adding a moderate amount of angular velocity to the star we follow the evolution of the deflagration using a smoothed particle hydrodynamics code. We find that the results are very dependent on the angle between the rotational axis and the line connecting the initial bubble of burned material with the center of the WD at the moment of ignition. The impact of rotation is larger for angles close to 90° because the Coriolis force on a floating element of fluid is maximum and its principal effect is to break the symmetry of the deflagration. Such symmetry breaking weakens the convergence of the nuclear flame at the antipodes of the initial ignition volume, changing the environmental conditions around the convergence region with respect to non-rotating models. These changes seem to disfavor the emergence of a detonation in the compressed volume at the antipodes and may compromise the viability of the so-called gravitational confined detonation mechanism.
PLANETARY SIGNATURES IN THE SAO 206462 (HD 135344B) DISK: A SPIRAL ARM PASSING THROUGH VORTEX?
Authors: Bae Jaehan , Zhu Zhaohuan , Hartmann Lee 
Published: March 2016

ABSTRACT
The disk surrounding SAO 206462, an 8 Myr old Herbig Ae star, has recently been reported to exhibit spiral arms, an asymmetric dust continuum, and a dust-depleted inner cavity. By carrying out two-dimensional, two-fluid hydrodynamic calculations, we find that a planetary-mass companion located at the outer disk could be responsible for these observed structures. In this model, the planet excites primary and secondary arms interior to its orbit. It also carves a gap and generates a local pressure bump at the inner gap edge where a vortex forms through Rossby wave instability. The vortex traps radially drifting dust particles, forming a dust-depleted cavity in the inner disk. We propose that the vortex is responsible for the brightest southwestern peak seen in infrared scattered light and sub-millimeter dust continuum emission. In particular, it is possible that the scattered light is boosted as one of the spiral arms passes through the high density vortex region, although the vortex alone may be able to explain the peak. We suggest that a planetary companion with a mass of 10–15

is orbiting SAO 206462 at 100–120 au. Monitoring of the brightest peak over the next few years will help reveal its origin because the spiral arms and vortex will show distinguishable displacement.
OSCILLATOR STRENGTHS OF VIBRIONIC EXCITATIONS OF NITROGEN DETERMINED BY THE DIPOLE (γ, γ) METHOD
Authors: Liu Ya-Wei , Kang Xu , Xu Long-Quan , Ni Dong-Dong , Yang Ke , Hiraoka Nozomu , Tsuei Ku-Ding , Zhu Lin-Fan 
Published: March 2016

ABSTRACT
The oscillator strengths of the valence-shell excitations of molecular nitrogen have significant applicational values in studies of the Earth's atmosphere and interstellar gases. In this work, the absolute oscillator strengths of the valence-shell excitations of molecular nitrogen in 12.3–13.4 eV were measured by the novel dipole (γ, γ) method, in which the high-resolution inelastic X-ray scattering is operated at a negligibly small momentum transfer and can simulate the photoabsorption process. Because the experimental technique used in the present work is distinctly different from those used previously, the present experimental results give an independent cross-check to previous experimental and theoretical data. The excellent coincidence of the present results with the dipole (e, e) and those that were extrapolated indicates that the present oscillator strengths can serve as benchmark data.
THE ISLANDS PROJECT. I. ANDROMEDA XVI, AN EXTREMELY LOW MASS GALAXY NOT QUENCHED BY REIONIZATION*
Authors: Monelli Matteo , Martínez-Vázquez Clara E. , Bernard Edouard J. , Gallart Carme , Skillman Evan D. , Weisz Daniel R. , Dolphin Andrew E. , Hidalgo Sebastian L. , Cole Andrew A. , Martin Nicolas F. , Aparicio Antonio , Cassisi Santi , Boylan-Kolchin Michael , Mayer Lucio , McConnachie Alan , McQuinn Kristen B. W. , Navarro Julio F. 
Published: March 2016

ABSTRACT
Based on data aquired in 13 orbits of Hubble Space Telescope time, we present a detailed evolutionary history of the M31 dSph satellite Andromeda XVI, including its lifetime star formation history (SFH), the spatial distribution of its stellar populations, and the properties of its variable stars. And XVI is characterized by prolonged star formation activity from the oldest epochs until star formation was quenched ∼6 Gyr ago, and, notably, only half of the mass in stars of And XVI was in place 10 Gyr ago. And XVI appears to be a low-mass galaxy for which the early quenching by either reionization or starburst feedback seems highly unlikely, and thus it is most likely due to an environmental effect (e.g., an interaction), possibly connected to a late infall in the densest regions of the Local Group. Studying the SFH as a function of galactocentric radius, we detect a mild gradient in the SFH: the star formation activity between 6 and 8 Gyr ago is significantly stronger in the central regions than in the external regions, although the quenching age appears to be the same, within 1 Gyr. We also report the discovery of nine RR Lyrae (RRL) stars, eight of which belong to And XVI. The RRL stars allow a new estimate of the distance, (m − M)0 = 23.72 ± 0.09 mag, which is marginally larger than previous estimates based on the tip of the red giant branch.
REVEALING THE NATURE OF EXTREME CORONAL-LINE EMITTER SDSS J095209.56+214313.3
Authors: Palaversa Lovro , Gezari Suvi , Sesar Branimir , Stuart J. Scott , Wozniak Przemyslaw , Holl Berry , Ivezić Željko 
Published: March 2016

ABSTRACT
Extreme coronal-line emitter (ECLE) SDSS J095209.56+214313.3, known by its strong, fading, high-ionization lines, has been a long-standing candidate for a tidal disruption event; however, a supernova (SN) origin has not yet been ruled out. Here we add several new pieces of information to the puzzle of the nature of the transient that powered its variable coronal lines: (1) an optical light curve from the Lincoln Near Earth Asteroid Research (LINEAR) survey that serendipitously catches the optical flare, and (2) late-time observations of the host galaxy with the Swift Ultraviolet and Optical Telescope (UVOT) and X-ray telescope (XRT) and the ground-based Mercator telescope. The well-sampled, ∼10 yr long, unfiltered LINEAR light curve constrains the onset of the flare to a precision of ±5 days and enables us to place a lower limit on the peak optical magnitude. Difference imaging allows us to estimate the location of the flare in proximity of the host galaxy core. Comparison of the GALEX data (early 2006) with the recently acquired Swift UVOT (2015 June) and Mercator observations (2015 April) demonstrates a decrease in the UV flux over a ∼10 yr period, confirming that the flare was UV-bright. The long-lived UV-bright emission, detected 1.8 rest-frame years after the start of the flare, strongly disfavors an SN origin. These new data allow us to conclude that the flare was indeed powered by the tidal disruption of a star by a supermassive black hole and that tidal disruption events are in fact capable of powering the enigmatic class of ECLEs.
THE NANOGRAV NINE-YEAR DATA SET: NOISE BUDGET FOR PULSAR ARRIVAL TIMES ON INTRADAY TIMESCALES
Authors: Lam M. T. , Cordes J. M. , Chatterjee S. , Arzoumanian Z. , Crowter K. , Demorest P. B. , Dolch T. , Ellis J. A. , Ferdman R. D. , Fonseca E. F. , Gonzalez M. E. , Jones G. , Jones M. L. , Levin L. , Madison D. R. , McLaughlin M. A. , Nice D. J. , Pennucci T. T. , Ransom S. M. , Siemens X. , Stairs I. H. , Stovall K. , Swiggum J. K. , Zhu W. W. 
Published: March 2016

ABSTRACT
The use of pulsars as astrophysical clocks for gravitational wave (GW) experiments demands the highest possible timing precision. Pulse times of arrival (TOAs) are limited by stochastic processes that occur in the pulsar itself, along the line of sight through the interstellar medium, and in the measurement process. On timescales of seconds to hours, the TOA variance exceeds that from template-fitting errors due to additive noise. We assess contributions to the total variance from two additional effects: amplitude and phase jitter intrinsic to single pulses and changes in the interstellar impulse response from scattering. The three effects have different dependencies on time, frequency, and pulse signal-to-noise ratio. We use data on 37 pulsars from the North American Nanohertz Observatory for GWs to assess the individual contributions to the overall intraday noise budget for each pulsar. We detect jitter in 22 pulsars and estimate the average value of rms jitter in our pulsars to be

of pulse phase. We examine how jitter evolves as a function of frequency and find evidence for evolution. Finally, we compare our measurements with previous noise parameter estimates and discuss methods to improve GW detection pipelines.
Biological richness of a large urban cemetery in Berlin. Results of a multi-taxon approach
Authors: Buchholz Sascha , Blick Theo , Hannig Karsten , Kowarik Ingo , Lemke Andreas , Otte Volker , Scharon Jens , Schönhofer Axel , Teige Tobias , von der Lippe Moritz , Seitz Birgit 
Published: March 2016

Urban green spaces can harbor a considerable species richness of plants and animals. A few studies on single species groups indicate important habitat functions of cemeteries, but this land use type is clearly understudied compared to parks. Such data are important as they (i) illustrate habitat functions of a specific, but ubiquitous urban land-use type and (ii) may serve as a basis for management approaches.
We sampled different groups of plants and animals in the Weißensee Jewish Cemetery in Berlin (WJC) which is one of the largest Jewish cemeteries in Europe. With a total of 608 species of plants and animals, this first multi-taxon survey revealed a considerable biological richness in the WJC. In all, 363 wild-growing vascular plant, 72 lichen and 26 bryophyte taxa were recorded. The sampling also yielded 34 bird and 5 bat species as well as 39 ground beetle, 5 harvestman and 64 spider species. Some species are new records for Berlin.
Two new species of Prionomastix Mayr (Hymenoptera: Encyrtidae) with a key to Indian species
Authors: Krishnachaitanya Tirunagaru , Manickavasagam Sagadai 
Published: March 2016

Species of Prionomastix Mayr were not known from India when Manickavasagam and Rameshkumar 2011 and Rameshkumar and Poorani 2015 misidentified a new species as P. siccarius. Now it is corrected by explaining the characters as to why it is new and not P. siccarius along with another new species. As we have one another new species, P. orientialis, described by Rameshkumar and Poorani 2015 our two new species are compared with P. orientalis also.
Two new species of Prionomastix Mayr (Hymenoptera: Encyrtidae), one from Bihar state and the other from Tamil Nadu state, India, are described viz., P. tamilnadensis sp. nov and P. biharensis sp. nov. and a key to all known Indian species is provided.
Aperçus sur la christologie de Thomas d’Aquin
Authors: Ols Daniel 
Published: March 2016

L’article s’emploie à comparer la doctrine de l’Incarnation dans les trois grandes œuvres spéculatives de saint Thomas : Scriptum super Sententiis, Summa contra Gentiles, Summa theologiae . Il examine d’abord le plan suivi dans les trois ouvrages pour traiter ce thème ; puis la façon dont saint Thomas remédie à deux lacunes de la christologie du Lombard (convenances de l’Incarnation, mystères de la vie du Christ) ; ensuite, les deux opinions christologiques du Lombard rejetées par les docteurs parisiens et concernant, l’une, l’âme séparée du corps et, l’autre, la question de savoir si, durant le triduum mortis , le Christ était un homme ; enfin, dix-sept des articuli in quibus . Malgré son caractère pointilliste, cette recherche permet d’explorer les aspects essentiels de la christologie de saint Thomas, de souligner les progrès de sa pensée et aussi de relever quelques positions problématiques de son enseignement.