bluuebunny/crossref_metadata_2025_split huggingface dataset:
CAPABILITIES OF EARTH-BASED RADAR FACILITIES FOR NEAR-EARTH ASTEROID OBSERVATIONS
Authors: Naidu Shantanu. P. , Benner Lance. A. M. , Margot Jean-Luc , Busch Michael. W. , Taylor Patrick. A. 
Published: October 2016

ABSTRACT
We evaluated the planetary radar capabilities at Arecibo, the Goldstone 70 m DSS-14 and 34 m DSS-13 antennas, the 70 m DSS-43 antenna at Canberra, the Green Bank Telescope (GBT), and the Parkes Radio Telescope in terms of their relative sensitivities and the number of known near-Earth asteroids (NEAs) detectable per year in monostatic and bistatic configurations. In the 2015 calendar year, monostatic observations with Arecibo and DSS-14 were capable of detecting 253 and 131 NEAs respectively, with signal-to-noise ratios (SNRs) greater than 30/track. Combined, the two observatories were capable of detecting 276 NEAs. Of these, Arecibo detected 77 and Goldstone detected 32, or 30% and 24% of the numbers that were possible. The two observatories detected an additional 18 and 7 NEAs respectively, with SNRs of less than 30/track. This indicates that a substantial number of potential targets are not being observed. The bistatic configuration with DSS-14 transmitting and the GBT receiving was capable of detecting about 195 NEAs, or ∼50% more than with monostatic observations at DSS-14. Most of the detectable asteroids were targets of opportunity that were discovered less than 15 days before the end of their observing windows. About 50% of the detectable asteroids have absolute magnitudes

, which corresponds to diameters

m.
THE H i PROBABILITY DISTRIBUTION FUNCTION AND THE ATOMIC-TO-MOLECULAR TRANSITION IN MOLECULAR CLOUDS
Authors: Imara Nia , Burkhart Blakesley 
Published: October 2016

ABSTRACT
We characterize the column-density probability distribution functions (PDFs) of the atomic hydrogen gas, H i, associated with seven Galactic molecular clouds (MCs). We use 21 cm observations from the Leiden/Argentine/Bonn Galactic H i Survey to derive column-density maps and PDFs. We find that the peaks of the H i PDFs occur at column densities in the range ∼1–2 × 1021

(equivalently, ∼0.5–1 mag). The PDFs are uniformly narrow, with a mean dispersion of

(∼0.1 mag). We also investigate the H i-to-H2 transition toward the cloud complexes and estimate H i surface densities ranging from 7 to 16

at the transition. We propose that the H i PDF is a fitting tool for identifying the H i-to-H2 transition column in Galactic MCs.
OPTICAL IDENTIFICATION OF CEPHEIDS IN 19 HOST GALAXIES OF TYPE Ia SUPERNOVAE AND NGC 4258 WITH THE HUBBLE SPACE TELESCOPE*
Authors: Hoffmann Samantha L. , Macri Lucas M. , Riess Adam G. , Yuan Wenlong , Casertano Stefano , Foley Ryan J. , Filippenko Alexei V. , Tucker Brad E. , Chornock Ryan , Silverman Jeffrey M. , Welch Douglas L. , Goobar Ariel , Amanullah Rahman 
Published: October 2016

ABSTRACT
We present results of an optical search conducted as part of the SH0ES project (Supernovae and H0 for the Equation of State of dark energy) for Cepheid variable stars using the Hubble Space Telescope (HST) in 19 hosts of Type Ia supernovae (SNe Ia) and the maser-host galaxy NGC 4258. The targets include nine newly imaged SN Ia hosts using a novel strategy based on a long-pass filter that minimizes the number of HST orbits required to detect and accurately determine Cepheid properties. We carried out a homogeneous reduction and analysis of all observations, including new universal variability searches in all SN Ia hosts, which yielded a total of 2200 variables with well-defined selection criteria, the largest such sample identified outside the Local Group. These objects are used in a companion paper to determine the local value of H0 with a total uncertainty of 2.4%.
TRANSPORT AND MIXING OF r-PROCESS ELEMENTS IN NEUTRON STAR BINARY MERGER BLAST WAVES
Authors: Montes Gabriela , Ramirez-Ruiz Enrico , Naiman Jill , Shen Sijing , Lee William H. 
Published: October 2016

ABSTRACT
The r-process nuclei are robustly synthesized in the material ejected during neutron star binary mergers (NSBMs). If NSBMs are indeed solely responsible for the solar system r-process abundances, a galaxy like our own would be required to host a few NSBMs per million years, with each event ejecting, on average, about 5 × 10−2
M
⊙ of r-process material. Because the ejecta velocities in the tidal tail are significantly larger than those in ordinary supernovae, NSBMs deposit a comparable amount of energy into the ISM. In contrast to extensive efforts studying spherical models for supernova remnant evolution, calculations quantifying the impact of NSBM ejecta in the ISM have been lacking. To better understand their evolution, we perform a suite of three-dimensional hydrodynamic simulations of isolated NSBM ejecta expanding in environments with conditions adopted from Milky-Way-like galaxy simulations. Although the remnant morphology is highly complex at early times, the subsequent radiative evolution is remarkably similar to that of a standard supernova. This implies that sub-resolution supernova feedback models can be used in galaxy-scale simulations that are unable to resolve the key evolutionary phases of NSBMs. Among other quantities, we examine the radius, mass, and kinetic energy content of the remnant at shell formation. We find that the shell formation epoch is attained when the swept-up mass is about 103(n
H/1 cm−3)−2/7
M
⊙; at this point, the mass fraction of r-process material is enhanced up to two orders of magnitude in relation to a solar metallicity ISM.
HOST-GALAXY PROPERTIES OF 32 LOW-REDSHIFT SUPERLUMINOUS SUPERNOVAE FROM THE PALOMAR TRANSIENT FACTORY
Authors: Perley D. A. , Quimby R. M. , Yan L. , Vreeswijk P. M. , Cia A. De , Lunnan R. , Gal-Yam A. , Yaron O. , Filippenko A. V. , Graham M. L. , Laher R. , Nugent P. E. 
Published: October 2016

ABSTRACT
We present ultraviolet through near-infrared photometry and spectroscopy of the host galaxies of all superluminous supernovae (SLSNe) discovered by the Palomar Transient Factory prior to 2013 and derive measurements of their luminosities, star formation rates, stellar masses, and gas-phase metallicities. We find that Type I (hydrogen-poor) SLSNe (SLSNe I) are found almost exclusively in low-mass (

) and metal-poor (12 + log10[O/H]

) galaxies. We compare the mass and metallicity distributions of our sample to nearby galaxy catalogs in detail and conclude that the rate of SLSNe I as a fraction of all SNe is heavily suppressed in galaxies with metallicities

. Extremely low metallicities are not required and indeed provide no further increase in the relative SLSN rate. Several SLSN I hosts are undergoing vigorous starbursts, but this may simply be a side effect of metallicity dependence: dwarf galaxies tend to have bursty star formation histories. Type II (hydrogen-rich) SLSNe (SLSNe II) are found over the entire range of galaxy masses and metallicities, and their integrated properties do not suggest a strong preference for (or against) low-mass/low-metallicity galaxies. Two hosts exhibit unusual properties: PTF 10uhf is an SLSN I in a massive, luminous infrared galaxy at redshift z = 0.29, while PTF 10tpz is an SLSN II located in the nucleus of an early-type host at z = 0.04.
KINEMATIC DOWNSIZING AT z ∼ 2
Authors: Simons Raymond C. , Kassin Susan A. , Trump Jonathan R. , Weiner Benjamin J. , Heckman Timothy M. , Barro Guillermo , Koo David C. , Guo Yicheng , Pacifici Camilla , Koekemoer Anton , Stephens Andrew W. 
Published: October 2016

ABSTRACT
We present results from a survey of the internal kinematics of 49 star-forming galaxies at

in the CANDELS fields with the Keck/MOSFIRE spectrograph, Survey in the near-Infrared of Galaxies with Multiple position Angles (SIGMA). Kinematics (rotation velocity V
rot and gas velocity dispersion

) are measured from nebular emission lines which trace the hot ionized gas surrounding star-forming regions. We find that by

, massive star-forming galaxies (

) have assembled primitive disks: their kinematics are dominated by rotation, they are consistent with a marginally stable disk model, and they form a Tully–Fisher relation. These massive galaxies have values of

that are factors of 2–5 lower than local well-ordered galaxies at similar masses. Such results are consistent with findings by other studies. We find that low-mass galaxies (

) at this epoch are still in the early stages of disk assembly: their kinematics are often dominated by gas velocity dispersion and they fall from the Tully–Fisher relation to significantly low values of V
rot. This “kinematic downsizing” implies that the process(es) responsible for disrupting disks at

have a stronger effect and/or are more active in low-mass systems. In conclusion, we find that the period of rapid stellar mass growth at

is coincident with the nascent assembly of low-mass disks and the assembly and settling of high-mass disks.
Hα VARIABILITY IN PTFO 8-8695 AND THE POSSIBLE DIRECT DETECTION OF EMISSION FROM A 2 MILLION YEAR OLD EVAPORATING HOT JUPITER
Authors: Johns-Krull Christopher M. , Prato Lisa , McLane Jacob N. , Ciardi David R. , Eyken Julian C. van , Chen Wei , Stauffer John R. , Beichman Charles A. , Frazier Sarah A. , Boden Andrew F. , Morales-Calderón Maria , Rebull Luisa M. 
Published: October 2016

ABSTRACT
We use high time cadence, high spectral resolution optical observations to detect excess Hα emission from the 2–3 Myr old weak-lined T Tauri star PTFO 8-8695. This excess emission appears to move in velocity as expected if it were produced by the suspected planetary companion to this young star. The excess emission is not always present, but when it is, the predicted velocity motion is often observed. We have considered the possibility that the observed excess emission is produced by stellar activity (flares), accretion from a disk, or a planetary companion; we find the planetary companion to be the most likely explanation. If this is the case, the strength of the Hα line indicates that the emission comes from an extended volume around the planet, likely fed by mass loss from the planet which is expected to be overflowing its Roche lobe.
AN IMPROVED DISTANCE AND MASS ESTIMATE FOR SGR A* FROM A MULTISTAR ORBIT ANALYSIS
Authors: Boehle A. , Ghez A. M. , Schödel R. , Meyer L. , Yelda S. , Albers S. , Martinez G. D. , Becklin E. E. , Do T. , Lu J. R. , Matthews K. , Morris M. R. , Sitarski B. , Witzel G. 
Published: October 2016

ABSTRACT
We present new, more precise measurements of the mass and distance of our Galaxy’s central supermassive black hole, Sgr A*. These results stem from a new analysis that more than doubles the time baseline for astrometry of faint stars orbiting Sgr A*, combining 2 decades of speckle imaging and adaptive optics data. Specifically, we improve our analysis of the speckle images by using information about a star’s orbit from the deep adaptive optics data (2005–2013) to inform the search for the star in the speckle years (1995–2005). When this new analysis technique is combined with the first complete re-reduction of Keck Galactic Center speckle images using speckle holography, we are able to track the short-period star S0-38 (K-band magnitude = 17, orbital period = 19 yr) through the speckle years. We use the kinematic measurements from speckle holography and adaptive optics to estimate the orbits of S0-38 and S0-2 and thereby improve our constraints of the mass (M
bh) and distance (R

o
) of Sgr A*: M
bh = (4.02 ± 0.16 ± 0.04) × 106
M
⊙ and 7.86 ± 0.14 ± 0.04 kpc. The uncertainties in M
bh and R

o
as determined by the combined orbital fit of S0-2 and S0-38 are improved by a factor of 2 and 2.5, respectively, compared to an orbital fit of S0-2 alone and a factor of ∼2.5 compared to previous results from stellar orbits. This analysis also limits the extended dark mass within 0.01 pc to less than 0.13 × 106
M
⊙ at 99.7% confidence, a factor of 3 lower compared to prior work.
ON THE ECCENTRICITY EXCITATION IN POST-MAIN-SEQUENCE BINARIES
Authors: Rafikov Roman R. 
Published: October 2016

ABSTRACT
Several classes of stellar binaries with post-main-sequence (post-MS) components—millisecond pulsars with the white dwarf companions (MSP+WD) and periods of

days, binaries hosting post-asymptotic giant branch stars, or barium stars with

several years—feature high eccentricities (up to 0.4) despite the expectation of their efficient tidal circularization during their post-MS evolution. It was suggested that the eccentricities of these binaries can be naturally excited by their tidal coupling to the circumbinary disk, formed by the material ejected from the binary. Here we critically reassess this idea using simple arguments rooted in the global angular momentum conservation of the disk+binary system. Compared to previous studies, we (1) fully account for the viscous spreading of the circumbinary disk, (2) consider the possibility of reaccretion from the disk onto the binary (in agreement with simulations and empirical evidence), and (3) allow for the reduced viscosity after the disk expands, cools, and forms dust. These ingredients conspire to significantly lower the efficiency of eccentricity excitation by the disk tides. We find that explaining eccentricities of the post-MS binaries is difficult and requires massive (

), long-lived (

years) circumbinary disks that do not reaccrete. While disk tides may account for the eccentricities of the MSP+WD binaries, we show reaccretion to also be detrimental for these systems. Reduced efficiency of the disk-driven excitation motivates the study of alternative mechanisms for producing the peculiar eccentricities of the post-MS binaries.
ANALYSIS OF CO-SPATIAL UV-OPTICAL HST/STIS SPECTRA OF PLANETARY NEBULA NGC 3242*
Authors: Miller Timothy R. , Henry Richard B. C. , Balick Bruce , Kwitter Karen B. , Dufour Reginald J. , Shaw Richard A. , Corradi Romano L. M. 
Published: October 2016

ABSTRACT
This project sought to consider two important aspects of the planetary nebula NGC 3242 using new long-slit HST/STIS spectra. First, we investigated whether this object is chemically homogeneous by spatially dividing the slit into different regions and calculating the abundances of each region. The major result is that the elements of He, C, O, and Ne are chemically homogeneous within uncertainties across the regions probed, implying that the stellar outflow was well-mixed. Second, we constrained the stellar properties using photoionization models computed by CLOUDY and tested the effects of three different density profiles on these parameters. The three profiles tested were a constant density profile, a Gaussian density profile, and a Gaussian with a power-law density profile. The temperature and luminosity were not affected significantly by the choice of density structure. The values for the stellar temperature and luminosity from our best-fit model are

kK and log(L/L
⊙) =

, respectively. Comparing to evolutionary models on an HR diagram, this corresponds to an initial and final mass of

and

, respectively.
Heterogeneity of Cortical Breaks in Hand Joints of Patients with Rheumatoid Arthritis and Healthy Controls Imaged by High-resolution Peripheral Quantitative Computed Tomography
Authors: Scharmga Andrea , Peters Michiel , van Tubergen Astrid , van den Bergh Joop , Barnabe Cheryl , Finzel Stephanie , van Rietbergen Bert , Geusens Piet 
Published: October 2016

Objective.Conventional radiographs (CR) of the hands are the gold standard for imaging bone erosions. The presence of bone erosions, reflected by the presence of cortical breaks, is a poor prognostic factor in patients with rheumatoid arthritis (RA). The availability of high-resolution peripheral quantitative computed tomography (HR-pQCT) enables detailed investigation of cortical breaks in rheumatic diseases. The aim of this image review is to show HR-pQCT images of the spectrum of cortical breaks with and without underlying trabecular bone changes in metacarpophalangeal (MCP) joints of healthy controls (HC) and patients with RA, with corresponding images on CR and magnetic resonance imaging (MRI).Methods.Second and third MCP joints of 41 patients (of which 10 were early RA with ≤ 2 years and 24 longstanding RA with ≥ 10 years of disease duration) and 38 HC were imaged by CR, MRI, and HR-pQCT (XtremeCT1, Scanco Medical AG). Representative images of the spectrum of cortical breaks were selected.Results.Cortical breaks were found in early and longstanding RA, but also in HC. They were heterogeneous in size, location, and number per joint, with a variety of surrounding cortical and underlying trabecular bone characteristics.Conclusion.Using HR-pQCT images of MCP joints, heterogeneous cortical breaks with and without surrounding trabecular bone changes were found, not only in RA but also in HC. The underlying mechanisms and significance of this spectrum of cortical breaks as found with high 3-D resolution needs further investigation.
Definition for Rheumatoid Arthritis Erosions Imaged with High Resolution Peripheral Quantitative Computed Tomography and Interreader Reliability for Detection and Measurement
Authors: Barnabe Cheryl , Toepfer Dominique , Marotte Hubert , Hauge Ellen-Margrethe , Scharmga Andrea , Kocijan Roland , Kraus Sebastian , Boutroy Stephanie , Schett Georg , Keller Kresten Krarup , de Jong Joost , Stok Kathryn S. , Finzel Stephanie ,   the SPECTRA Collaboration
Published: October 2016

Objective.High-resolution peripheral quantitative computed tomography (HR-pQCT) sensitively detects erosions in rheumatoid arthritis (RA); however, nonpathological cortical bone disruptions are potentially misclassified as erosive. Our objectives were to set and test a definition for pathologic cortical bone disruptions in RA and to standardize reference landmarks for measuring erosion size.Methods.HR-pQCT images of metacarpophalangeal joints of RA and control subjects were used in an iterative process to achieve consensus on the definition and reference landmarks. Independent readers (n = 11) applied the definition to score 58 joints and measure pathologic erosions in 2 perpendicular multiplanar reformations for their maximum width and depth. Interreader reliability for erosion detection and variability in measurements between readers [root mean square coefficient of variation (RMSCV), intraclass correlation (ICC)] were calculated.Results.Pathologic erosions were defined as cortical breaks extending over a minimum of 2 consecutive slices in perpendicular planes, with underlying trabecular bone loss and a nonlinear shape. Interreader agreement for classifying pathologic erosions was 90.2%, whereas variability for width and depth erosion assessment was observed (RMSCV perpendicular width 12.3%, axial width 20.6%, perpendicular depth 24.0%, axial depth 22.2%; ICC perpendicular width 0.206, axial width 0.665, axial depth 0.871, perpendicular depth 0.783). Mean erosion width was 1.84 mm (range 0.16–8.90) and mean depth was 1.86 mm (range 0.30–8.00).Conclusion.We propose a new definition for erosions visualized with HR-pQCT imaging. Interreader reliability for erosion detection is good, but further refinement of selection of landmarks for erosion size measurement, or automated volumetric methods, will be pursued.
La « pacification » et ses rumeurs : les incidences des Unités de Police Pacificatrices sur les problèmes publics dans les favelas de Rio de Janeiro
Authors: Menezes Palloma Valle 
Published: October 2016

Cet article a pour objectif central l’analyse des rumeurs qui circulent dans les favelas de Santa Marta et Cidade de Deus depuis que la police a commencé à les occuper en novembre 2008, avant que n’y soient inaugurées les premières UPP, les Unités de police pacificatrices de Rio de Janeiro. Dans cet article, je postule que l’analyse de ces « informations improvisées » peut aider à comprendre la manière dont ont évolué les préoccupations et les problèmes publics qui ont affecté la routine des habitants des favelas « pacifiées » au cours des cinq dernières années. Cette réflexion s’appuie sur un travail de recherche ethnographique effectuée dans les favelas de Santa Marta depuis 2009 et de Cidade de Deus depuis 2012.
Ammonium carbonate loss rates from lures differentially affect trap captures ofRhagoletis indifferens(Diptera: Tephritidae) and non-target flies
Authors: Yee W. L. 
Published: October 2016

AbstractWestern cherry fruit fly,Rhagoletis indifferensCurran (Diptera: Tephritidae), is a pest of cherry (PrunusLinnaeus, Rosaceae) in western North America that can be monitored using traps baited with ammonia. However, ammonia-based attractants also attract non-target Diptera that clutter traps. Here, the hypothesis that ammonium carbonate (AC) loss rates from lures differentially affect numbers ofR.indifferensand non-target flies caught on sticky yellow rectangles in sweet cherry trees was tested in Washington State, United States of America. Ammonium carbonate loss rates were varied from seven-dram plastic vials hung ~1 cm above traps. A total of six experiments were conducted in which progressively lower AC loss rates within a range of 0.10–26.19 mg AC/hour were tested. For captures ofR. indifferens, no AC loss rate comparisons within 0.19–26.19 mg/hour differed, and captures were not reduced until losses were lowered to 0.10–0.13 mg/hour. In contrast, captures of medium to large (⩾5 mm long) non-target flies, which were mostly Sarcophagidae (Diptera), were reduced at a rate ~30 times higher, at 3.34 or 3.80 mg AC/hour. Results suggest that using lures with an AC loss rate of 0.19 mg/hour can maintain highR. indifferenscaptures while reducing non-target fly captures and thus can improve monitoring efficiency.
Association of Physical Inactivity, Weight, Smoking, and Prior Injury on Physical Performance in a Military Setting
Authors: Teyhen Deydre S. , Rhon Daniel I. , Butler Robert J. , Shaffer Scott W. , Goffar Stephen L. , McMillian Danny J. , Boyles Robert E. , Kiesel Kyle B. , Plisky Phillip J. 
Published: October 2016

Context: Although inactivity, being overweight, smoking, and a history of injury are identified as risk factors for poor health and injury, few authors have examined their association on physical performance. Young adults may be more likely to adopt healthier lifestyles if they understand the effect of health behaviors on performance.
Objective: To determine the association of being overweight, smoking, inactivity, and a history of injury with physical performance.
Design: Cross-sectional study.
Setting: Military population.
Patients or Other Participants: Active-duty service members (N = 1466; 1380 men, 86 women; age = 24.7 ± 5.0 years; body mass index = 26.7 ± 3.4 kg/m2).
Main Outcome Measure(s): Participants performed 8 measures (the triple-crossover hop for distance, the 6-m timed-hop test, the Functional Movement Screen, the Lower Quarter Y-Balance Test, the Upper Quarter Y-Balance Test, and the 3-event Army Physical Fitness Test) for evaluation of endurance, strength, muscular endurance, power, agility, balance, and motor control. Participants were categorized based on the number of health risk factors present. Using an analysis of covariance, we assessed the relationship between risk factors and physical performance with age and sex as covariates.
Results: Compared with those who had no risk factors (27.9% of men, 34.9% of women), physical performance was worse in those who had 1, 2, or 3 to 4 risk factors present by 4.3%, 6.7%, and 10.3%, respectively. Decrements in performance for those with 3 to 4 risk factors ranged from 3.3% to 14.4%.
Conclusions: An unhealthy lifestyle habit or a history of injury was negatively associated with physical performance. Physical performance decrements were associated with the number of risk factors present. Understanding how risk factors contribute to decreased physical performance may enable clinicians to improve compliance with injury-prevention programs in occupational settings in which a young and relatively healthy workforce may be more concerned about performance than health.