bluuebunny/crossref_metadata_2025_split huggingface dataset:
Alternating force induces less pronounced fatigue-related responses than constant repeated force muscle actions
Authors: Smith Cory M. , Housh Terry J. , Hill Ethan C. , Johnson Glen O. , Schmidt Richard J. 
Published: September 2017

BACKGROUND: Little is known regarding the influence of force application during fatigue when the total amount of work is equal. That is, do changes in force applications result in different fatigue mechanisms despite the overall work being the same. OBJECTIVE: The aim of the current study was to examine the effects of alternating forces versus repeated constant force muscle actions on the time course of changes in neuromuscular responses. METHODS: Sixteen adults performed 50-intermittent isometric leg extensions at alternating 40 then 80% maximal voluntary isometric contraction (40/80% MVIC) or repeated constant forces at 60% MVIC. Each protocol resulted in equal, averaged force across all 50 repetitions. Electromyographic amplitude (EMG RMS), mechanomyographic (MMG) RMS, EMG mean power frequency (MPF), and MMG MPF were recorded from the vastus lateralis. RESULTS: Alternating force protocol resulted in less fatigue-induced changes in neuromuscular responses compared to repeated constant force protocol. The repeated constant force protocol resulted in earlier increases in EMG RMS and MMG RMS as well as earlier decreases in EMG MPF and MMG MPF compared to the alternating force protocol. CONCLUSIONS: Fatigue in occupational, sporting activities, or various fatiguing tasks may be dependent on the order that force is applied.
Persistence with Antihypertensive Drugs in Patients with Hypertension and Dementia in Germany
Authors: Jacob Louis , Adam-Schnepf Leonie , Kostev Karel 
Published: September 2017

Background: Hypertension, a chronic disease resulting from aging and its related physiopathological dysregulations, is often associated with dementia. Objective: The goal was to analyze the persistence with antihypertensive drugs in patients affected by both hypertension and dementia in Germany. Methods: This study included hypertension patients who were initially treated with antihypertensive drugs in 1,262 general practices in Germany between January 2013 and December 2015 (index date). Patients with hypertension and comorbid dementia were matched (1 : 1) to patients without dementia by age, gender, type of residence (nursing home versus home-care setting), physician, and initial antihypertensive therapy, using a propensity score method. The primary outcome was the rate of patients without treatment discontinuation with antihypertensive drugs in cases and controls in the 12 months following the index date. Cox regressions were used to determine the impact of dementia on persistence with antihypertensive treatment. Results: This study included 2,191 patients with hypertension and comorbid dementia and 2,191 patients with hypertension but without dementia. The mean age was 79.3 years (SD = 10.3 years) in both groups. Twelve months after initiation of antihypertensive therapy, 73.5% of cases and 69.5% of controls were persistent ( p < 0.001). Dementia was associated with a significant decrease in the risk of non-persistence with antihypertensive drugs in the entire population (HR = 0.86, 95% CI: 0.79–0.93). This finding was corroborated in five different subgroups (age ≤60 years, age 61–70 years, men, women, and patients living in home-care settings). Conclusions: Dementia was found to be a protective factor for persistence with antihypertensive drugs in Germany.
Genetically-Predicted Adult Height and Alzheimer’s Disease
Authors: Larsson Susanna C. , Traylor Matthew , Burgess Stephen , Markus Hugh S. 
Published: September 2017

Background: Observational studies have linked increased adult height with better cognitive performance and reduced risk of Alzheimer’s disease (AD). It is unclear whether the associations are due to shared biological processes that influence height and AD or due to confounding by early life exposures or environmental factors. Objective: To use a genetic approach to investigate the association between adult height and AD. Methods: We selected 682 single nucleotide polymorphisms (SNPs) associated with height at genome-wide significance ( p < 5×10–8) in the Genetic Investigation of ANthropometric Traits (GIANT) consortium. Summary statistics for each of these SNPs on AD were obtained from the International Genomics of Alzheimer’s Project (IGAP) of 17,008 individuals with AD and 37,154 controls. The estimate of the association between genetically predicted height and AD was calculated using the inverse-variance weighted method. Results: The odds ratio of AD was 0.91 (95% confidence interval, 0.86–0.95; p = 9.8×10–5) per one standard deviation increase (about 6.5 cm) in genetically predicted height based on 682 SNPs, which were clustered in 419 loci. In an analysis restricted to one SNP from each height-associated locus ( n = 419 SNPs), the corresponding OR was 0.92 (95% confidence interval, 0.86–0.97; p = 4.8×10–3). Conclusions: This finding suggests that biological processes that influence adult height may have a role in the etiology of AD.
FIGS—Faint Infrared Grism Survey: Description and Data Reduction
Authors: Pirzkal Norbert , Malhotra Sangeeta , Ryan Russell E. , Rothberg Barry , Grogin Norman , Finkelstein Steven L. , Koekemoer Anton M. , Rhoads James , Larson Rebecca L. , Christensen Lise , Cimatti Andrea , Ferreras Ignacio , Gardner Jonathan P. , Gronwall Caryl , Hathi Nimish P. , Hibon Pascale , Joshi Bhavin , Kuntschner Harald , Meurer Gerhardt R. , O’Connell Robert W. , Oestlin Goeran , Pasquali Anna , Pharo John , Straughn Amber N. , Walsh Jeremy R. , Watson Darach , Windhorst Rogier A. , Zakamska Nadia L , Zirm Andrew 
Published: September 2017

Abstract
The Faint Infrared Grism Survey (FIGS) is a deep Hubble Space Telescope (HST) WFC3/IR (Wide Field Camera 3 Infrared) slitless spectroscopic survey of four deep fields. Two fields are located in the Great Observatories Origins Deep Survey-North (GOODS-N) area and two fields are located in the Great Observatories Origins Deep Survey-South (GOODS-S) area. One of the southern fields selected is the Hubble Ultra Deep Field. Each of these four fields were observed using the WFC3/G102 grism (0.8 μm–1.15 μm continuous coverage) with a total exposure time of 40 orbits (≈100 kilo-seconds) per field. This reaches a

continuum depth of

AB magnitudes and probes emission lines to

. This paper details the four FIGS fields and the overall observational strategy of the project. A detailed description of the Simulation Based Extraction (SBE) method used to extract and combine over 10,000 spectra of over 2000 distinct sources brighter than

mag is provided. High fidelity simulations of the observations is shown to significantly improve the background subtraction process, the spectral contamination estimates, and the final flux calibration. This allows for the combination of multiple spectra to produce a final high quality, deep, 1D spectra for each object in the survey.
Simultaneous X-Ray, Gamma-Ray, and Radio Observations of the Repeating Fast Radio Burst FRB 121102
Authors: Scholz P. , Bogdanov S. , Hessels J. W. T. , Lynch R. S. , Spitler L. G. , Bassa C. G. , Bower G. C. , Burke-Spolaor S. , Butler B. J. , Chatterjee S. , Cordes J. M. , Gourdji K. , Kaspi V. M. , Law C. J. , Marcote B. , McLaughlin M. A. , Michilli D. , Paragi Z. , Ransom S. M. , Seymour A. , Tendulkar S. P. , Wharton R. S. 
Published: September 2017

Abstract
We undertook coordinated campaigns with the Green Bank, Effelsberg, and Arecibo radio telescopes during Chandra X-ray Observatory and XMM-Newton observations of the repeating fast radio burst FRB 121102 to search for simultaneous radio and X-ray bursts. We find 12 radio bursts from FRB 121102 during 70 ks total of X-ray observations. We detect no X-ray photons at the times of radio bursts from FRB 121102 and further detect no X-ray bursts above the measured background at any time. We place a 5σ upper limit of 3 × 10−11 erg cm−2 on the 0.5–10 keV fluence for X-ray bursts at the time of radio bursts for durations

ms, which corresponds to a burst energy of 4 × 1045 erg at the measured distance of FRB 121102. We also place limits on the 0.5–10 keV fluence of 5 × 10−10 and 1 × 10−9 erg cm−2 for bursts emitted at any time during the XMM-Newton and Chandra observations, respectively, assuming a typical X-ray burst duration of 5 ms. We analyze data from the Fermi Gamma-ray Space Telescope Gamma-ray Burst Monitor and place a 5σ upper limit on the 10–100 keV fluence of 4 × 10−9 erg cm−2 (5 × 1047 erg at the distance of FRB 121102) for gamma-ray bursts at the time of radio bursts. We also present a deep search for a persistent X-ray source using all of the X-ray observations taken to date and place a 5σ upper limit on the 0.5–10 keV flux of 4 × 10−15 erg s−1 cm−2 (3 × 1041 erg s−1 at the distance of FRB 121102). We discuss these non-detections in the context of the host environment of FRB 121102 and of possible sources of fast radio bursts in general.
The Sloan Digital Sky Survey Reverberation Mapping Project: Composite Lags at z ≤ 1
Authors: Li Jennifer , Shen Yue , Horne Keith , Brandt W. N. , Greene Jenny E. , Grier C. J. , Ho Luis C. , Kochanek Chris , Schneider Donald P. , Trump Jonathan R. , Dawson Kyle S. , Pan Kaike , Bizyaev Dmitry , Oravetz Daniel , Simmons Audrey , Malanushenko Elena 
Published: September 2017

Abstract
We present composite broad-line region (BLR) reverberation mapping lag measurements for Hα, Hβ, He ii
λ4686, and Mg ii for a sample of 144, z ≲ 1 quasars from the Sloan Digital Sky Survey Reverberation Mapping (SDSS-RM) project. Using only the 32-epoch spectroscopic light curves in the first six-month season of SDSS-RM observations, we compile correlation function measurements for individual objects and then coadd them to allow the measurement of the average lags for our sample at mean redshifts of 0.4 (for Hα) and ∼0.65 (for the other lines). At similar quasar luminosities and redshifts, the sample-averaged lag decreases in the order of Mg ii, Hα, Hβ, and He ii. This decrease in lags is accompanied by an increase in the mean line width of the four lines, and is roughly consistent with the virialized motion for BLR gas in photoionization equilibrium. These are among the first RM measurements of stratified BLR structure at z > 0.3. Dividing our sample by luminosity, Hα shows clear evidence of increasing lags with luminosity, consistent with the expectation from the measured BLR size–luminosity relation based on Hβ. The other three lines do not show a clear luminosity trend in their average lags due to the limited dynamic range of luminosity probed and the poor average correlation signals in the divided samples, a situation that will be improved with the incorporation of additional photometric and spectroscopic data from SDSS-RM. We discuss the utility and caveats of composite lag measurements for large statistical quasar samples with reverberation mapping data.
Probing the Physics of Narrow-line Regions in Active Galaxies. IV. Full Data Release of the Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7)
Authors: Thomas Adam D. , Dopita Michael A. , Shastri Prajval , Davies Rebecca , Hampton Elise , Kewley Lisa , Banfield Julie , Groves Brent , James Bethan L. , Jin Chichuan , Juneau Stéphanie , Kharb Preeti , Sairam Lalitha , Scharwächter Julia , Shalima P. , Sundar M. N. , Sutherland Ralph , Zaw Ingyin 
Published: September 2017

Abstract
We present the second and final data release of the Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7). Data are presented for 63 new galaxies not included in the first data release, and we provide 2D emission-line fitting products for the full S7 sample of 131 galaxies. The S7 uses the WiFeS instrument on the ANU 2.3 m telescope to obtain spectra with a spectral resolution of R = 7000 in the red (540–700 nm) and R = 3000 in the blue (350–570 nm), over an integral field of 25 × 38 arcsec2 with 1 × 1 arcsec2 spatial pixels. The S7 contains both the largest sample of active galaxies and the highest spectral resolution of any comparable integral field survey to date. The emission-line fitting products include line fluxes, velocities, and velocity dispersions across the WiFeS field of view, and an artificial neural network has been used to determine the optimal number of Gaussian kinematic components for emission-lines in each spaxel. Broad Balmer lines are subtracted from the spectra of nuclear spatial pixels in Seyfert 1 galaxies before fitting the narrow lines. We bin nuclear spectra and measure reddening-corrected nuclear fluxes of strong narrow lines for each galaxy. The nuclear spectra are classified on optical diagnostic diagrams, where the strength of the coronal line [Fe vii] λ6087 is shown to be correlated with [O iii]/Hβ. Maps revealing gas excitation and kinematics are included for the entire sample, and we provide notes on the newly observed objects.
Massive Quenched Galaxies at z ∼ 0.7 Retain Large Molecular Gas Reservoirs
Authors: Suess Katherine A. , Bezanson Rachel , Spilker Justin S. , Kriek Mariska , Greene Jenny E. , Feldmann Robert , Hunt Qiana , Narayanan Desika 
Published: September 2017

Abstract
The physical mechanisms that quench star formation, turning blue star-forming galaxies into red quiescent galaxies, remain unclear. In this Letter, we investigate the role of gas supply in suppressing star formation by studying the molecular gas content of post-starburst galaxies. Leveraging the wide area of the Sloan Digital Sky Survey, we identify a sample of massive intermediate-redshift galaxies that have just ended their primary epoch of star formation. We present Atacama Large Millimeter/submillimeter Array CO(2-1) observations of two of these post-starburst galaxies at z ∼ 0.7 with

. Their molecular gas reservoirs of

and

are an order of magnitude larger than comparable-mass galaxies in the local universe. Our observations suggest that quenching does not require the total removal or depletion of molecular gas, as many quenching models suggest. However, further observations are required both to determine if these apparently quiescent objects host highly obscured star formation and to investigate the intrinsic variation in the molecular gas properties of post-starburst galaxies.
Integral Formula for Spectral Flow for -Summable Operators
Authors: Georgescu Magdalena Cecilia 
Published: September 2017

AbstractFix a von Neumann algebra ${\mathcal{N}}$ equipped with a suitable trace $\unicode[STIX]{x1D70F}$. For a path of self-adjoint Breuer–Fredholm operators, the spectral flow measures the net amount of spectrum that moves from negative to non-negative. We consider specifically the case of paths of bounded perturbations of a fixed unbounded self-adjoint Breuer–Fredholm operator affiliated with ${\mathcal{N}}$. If the unbounded operator is $p$-summable (that is, its resolvents are contained in the ideal $L^{p}$), then it is possible to obtain an integral formula that calculates spectral flow. This integral formula was first proved by Carey and Phillips, building on earlier approaches of Phillips. Their proof was based on first obtaining a formula for the larger class of $\unicode[STIX]{x1D703}$-summable operators, and then using Laplace transforms to obtain a $p$-summable formula. In this paper, we present a direct proof of the $p$-summable formula that is both shorter and simpler than theirs.
Chemical characterization and source apportionment of submicron aerosols measured in Senegal during the 2015 SHADOW campaign
Authors: Rivellini Laura-Hélèna , Chiapello Isabelle , Tison Emmanuel , Fourmentin Marc , Féron Anaïs , Diallo Aboubacry , N'Diaye Thierno , Goloub Philippe , Canonaco Francesco , Prévôt André Stephan Henry , Riffault Véronique 
Published: September 2017

Abstract. The present study offers the first chemical characterization of the submicron (PM1) fraction in western Africa at a high time resolution, thanks to collocated measurements of nonrefractory (NR) species with an Aerosol Chemical Speciation Monitor (ACSM), black carbon and iron concentrations derived from absorption coefficient measurements with a 7-wavelength Aethalometer, and total PM1 determined by a TEOM-FDMS (tapered element oscillating microbalance–filtered dynamic measurement system) for mass closure. The field campaign was carried out over 3 months (March to June 2015) as part of the SHADOW (SaHAran Dust Over West Africa) project at a coastal site located in the outskirts of the city of Mbour, Senegal. With an averaged mass concentration of 5.4 µg m−3, levels of NR PM1 in Mbour were 3 to 10 times lower than those generally measured in urban and suburban polluted environments. Nonetheless the first half of the observation period was marked by intense but short pollution events (NR PM1 concentrations higher than 15 µg m−3), sea breeze phenomena and Saharan desert dust outbreaks (PM10 up to 900 µg m−3). During the second half of the campaign, the sampling site was mainly under the influence of marine air masses. The air masses on days under continental and sea breeze influences were dominated by organics (36–40 %), whereas sulfate particles were predominant (40 %) for days under oceanic influence. Overall, measurements showed that about three-quarters of the total PM1 were explained by NR PM1, BC (black carbon) and Fe (a proxy for dust) concentrations, leaving approximately one-quarter for other refractory species. A mean value of 4.6 % for the Fe ∕ PM1 ratio was obtained. Source apportionment of the organic fraction, using positive matrix factorization (PMF), highlighted the impact of local combustion sources, such as traffic and residential activities, which contribute on average to 52 % of the total organic fraction. A new organic aerosol (OA) source, representing on average 3 % of the total OA fraction, showed similar variation to nonrefractory particulate chloride. Its rose plot and daily pattern pointed to local combustion processes, i.e., two open waste-burning areas located about 6 and 11 km away from the receptor site and to a lesser extent a traditional fish-smoking location. The remaining fraction was identified as oxygenated organic aerosols (OOA), a factor that prevailed regardless of the day type (45 %) and was representative of regional (approximately three-quarters) but also local (approximately one-quarter) sources due to enhanced photochemical processes.
Calibration and evaluation of CCD spectroradiometers for ground-based and airborne measurements of spectral actinic flux densities
Authors: Bohn Birger , Lohse Insa 
Published: September 2017

Abstract. The properties and performance of charge-coupled device (CCD) array spectroradiometers for the measurement of atmospheric spectral actinic flux densities (280–650 nm) and photolysis frequencies were investigated. These instruments are widely used in atmospheric research and are suitable for aircraft applications because of high time resolutions and high sensitivities in the UV range. The laboratory characterization included instrument-specific properties like the wavelength accuracy, dark signal, dark noise and signal-to-noise ratio (SNR). Spectral sensitivities were derived from measurements with spectral irradiance standards. The calibration procedure is described in detail, and a straightforward method to minimize the influence of stray light on spectral sensitivities is introduced. From instrument dark noise, minimum detection limits  ≈  1  ×  1010 cm−2 s−1 nm−1 were derived for spectral actinic flux densities at wavelengths around 300 nm (1 s integration time). As a prerequisite for the determination of stray light under field conditions, atmospheric cutoff wavelengths were defined using radiative transfer calculations as a function of the solar zenith angle (SZA) and total ozone column (TOC). The recommended analysis of field data relies on these cutoff wavelengths and is also described in detail taking data from a research flight on HALO (High Altitude and Long Range Research Aircraft) as an example. An evaluation of field data was performed by ground-based comparisons with a double-monochromator-based, highly sensitive reference spectroradiometer. Spectral actinic flux densities were compared as well as photolysis frequencies j(NO2) and j(O1D), representing UV-A and UV-B ranges, respectively. The spectra expectedly revealed increased daytime levels of stray-light-induced signals and noise below atmospheric cutoff wavelengths. The influence of instrument noise and stray-light-induced noise was found to be insignificant for j(NO2) and rather limited for j(O1D), resulting in estimated detection limits of 5  ×  10−7 and 1  ×  10−7 s−1, respectively, derived from nighttime measurements on the ground (0.3 s integration time, 10 s averages). For j(O1D) the detection limit could be further reduced by setting spectral actinic flux densities to zero below atmospheric cutoff wavelengths. The accuracies of photolysis frequencies were determined from linear regressions with data from the double-monochromator reference instrument. The agreement was typically within ±5 %. Because optical-receiver aspects are not specific for the CCD spectroradiometers, they were widely excluded in this work and will be treated in a separate paper, in particular with regard to airborne applications.
Time-stamp correction of magnetic observatory data acquired during unavailability of time-synchronization services
Authors: Coïsson Pierdavide , Telali Kader , Heumez Benoit , Lesur Vincent , Lalanne Xavier , Xin Chang Jiang 
Published: September 2017

Abstract. During magnetic observatory data acquisition, the data time stamp is kept synchronized with a precise source of time. This is usually done using a GPS-controlled pulse per second (PPS) signal. For some observatories located in remote areas or where internet restrictions are enforced, only the magnetometer data are transmitted, limiting the capabilities of monitoring the acquisition operations. The magnetic observatory in Lanzhou (LZH), China, experienced an unnoticed interruption of the GPS PPS starting 7 March 2013. The data logger clock drifted slowly in time: in 6 months a lag of 27 s was accumulated. After a reboot on 2 April 2014 the drift became faster, −2 s per day, before the GPS PPS could be restored on 8 July 2014. To estimate the time lags that LZH time series had accumulated, we compared it with data from other observatories located in East Asia. A synchronization algorithm was developed. Natural sources providing synchronous events could be used as markers to obtain the time lag between the observatories. The analysis of slices of 1 h of 1 s data at arbitrary UTC allowed estimating time lags with an uncertainty of ∼ 11 s, revealing the correct trends of LZH time drift. A precise estimation of the time lag was obtained by comparing data from co-located instruments controlled by an independent PPS. In this case, it was possible to take advantage of spikes and local noise that constituted precise time markers. It was therefore possible to determine a correction to apply to LZH time stamps to correct the data files and produce reliable 1 min averaged definitive magnetic data.