bluuebunny/crossref_metadata_2025_split huggingface dataset:
Spectrum of Lipid Abnormality among Thyroid Disorder Patients in Ucms-Th, South Western Region
Authors: Gautam N , Jayan A , Dubey Raju Kumar , Jha AC , Sharma B , Bohara S , Shrestha S 
Published: February 2018

INTRODUCTION: Hypothyroidism is the most common cause of secondary dyslipidemia. Thus, thyroid function test should be carried out before starting any hypolipidemic drugs. Even among thyroid disorder, hypothyroidism is more associated with cardiovascular and associated problems and if not detected earlier, it leads to severe clinical consequences. Our study assesses the frequency and spectrum of dyslipidemia in various types of thyroidal illness in the population residing in south western part of Nepal.MATERIALS AND METHODS: This is a cross sectional study carried out in suspected thyroid disorder patients (n=276) and categorized as Euthyroidism (n=55), Subclinical Hypothyroidism (n=89), Primary Hypothyroidism (n=122) and Primary Hyperthyroidism (n=10) patients and to see the association with lipid profiles in the Department of Biochemistry, Universal College of Medical Sciences Teaching Hospital, Bhairahawa Nepal. Serum fT / fT4 and TSH estimations were carried out by competitive 3 ELISA method and Sand-wich double antibody ELISA method respectively using commercially supplied reagents (Human, Germany). The criteria for dyslipidemia was obtained by National Cholesterol Education Expert Panel/ Adult Treatment Protocol III (NCEP/ATPIII).RESULTS: Out of 276 cases the dyslipidemia was observed in 183 cases (66.30%).The dyslipidemia was mostly associated with primary hypothyroidism (55.07%) followed by Subclinical Hypothyroidism (38.04%) than Euthyroid (5.79 %) and Primary Hyperthyroidism (3.62 %) respectively. Out of all cases, the spectrum of dyslipidemia was mostly observed for decreased HDL (18.5 %) followed by increased TG (10.1 %). Moreover, it is significantly differ in relation in HDL (p=0.009), TG/HDL (p=0.02) and Non-HDL/HDL (p=0.033) where as non significant as compared to other lipid profile in different groups.CONCLUSION: Our study revealed the close association of thyroidal illness with dyslipidemia with increased TG, low HDL, increased TG/HDL and Non-HDL/HDL. The increased TG/HDL and/or Non-HDL/HDL could be better indicator than single lipid abnormality which needs to be ascertained prospectively in large population. Journal of Universal College of Medical Sciences (2016) Vol.04 No.02 Issue 14, page: 20-24
Sample Preparation and Analytical Considerations for the US Aflatoxin Sampling Program for Shelled Peanuts
Authors: Davis J. P. , Jackson M. D. , Leek J.M. , Samadpour M. 
Published: February 2018

ABSTRACT
The USDA aflatoxin sampling program for shelled peanuts is an important component of broader industry efforts to minimize aflatoxin occurrence in the edible market. In this program, official samples are milled with either a traditional hammer/automatic sub-sampling mill, commonly called the Dickens Mill (DM) or with a vertical cutter mill (VCM). Particle size reduction and sample homogenization are the primary objectives of sample preparation (milling) to generate subsamples which best represent the parent sample composition for downstream analysis. DM particle size reduction is limited by the 3.2 mm round hole screens internal to the mill which prevent pasting of the sample. VCM grinding converts the sample to a paste while simultaneously homogenizing the sample. Experiments demonstrate that when testing aflatoxin contaminated peanuts for equivalent sized subsamples prepared from the two mill types, made into water slurries per USDA specifications and subsequently extracted and tested for total aflatoxin per USDA specifications, VCM subsamples are more normally distributed around the sample aflatoxin mean, whereas DM subsamples are more positively skewed (median lower than mean) around the sample aflatoxin mean. Accordingly, milling official samples with a DM compared to VCM promotes more lot misclassifications. It is also demonstrated that for a given subsample after extraction and immunoaffinity column (IAC) purification, the total aflatoxin measured by either high performance liquid chromatography (HPLC) or fluorometry (both USDA approved) are practically equivalent from an accuracy perspective. There are costs (time and resources) associated with decreasing natural variation due to sampling, sample preparation and analytical testing in an aflatoxin sampling/testing program. Sample preparation is a greater source of variation compared to that of the analytical testing. Resources would be better spent replacing DM with VCM mills than converting the final analytical step from IAC-fluorometry to IAC-HPLC in an effort to best classify peanut lots for the edible market.
Two Transient X-Ray Quasi-periodic Oscillations Separated by an Intermediate State in 1H 0707-495
Authors: Zhang Peng-fei , Zhang Peng , Liao Neng-hui , Yan Jing-zhi , Fan Yi-zhong , Liu Qing-zhong 
Published: February 2018

Abstract
In the narrow-line Seyfert 1 galaxy 1H 0707-495, recently a transient quasi-periodic oscillation (QPO) signal with a frequency of

Hz has been detected at a high statistical significance. Here, we reanalyze the same set of XMM-Newton data observed on 2008 February 4 with the weighted-wavelet Z-transform method. In addition to confirming the previous findings, we also find another QPO signal with a frequency of

Hz in a separated X-ray emission phase at the significance level of

. The signal is also found fitting an autoregressive model though at a lower significance. The frequency ratio between these two signals is

. The analysis of other XMM-Newton measurements of 1H 0707-495 also reveals the presence of the

Hz (

Hz) QPO signal on 2007 May 14 (2010 September 17) at the significance level of

(

). The QPO frequency found in this work follows the

relation reported in previous works spanning from stellar mass to supermassive black holes. This is the first observation of two separated transient X-ray QPO signals in active galactic nuclei, which sheds a new light on the physics of accreting supermassive black holes.
GPI Spectroscopy of the Mass, Age, and Metallicity Benchmark Brown Dwarf HD 4747 B
Authors: Crepp Justin R. , Principe David A. , Wolff Schuyler , Godfrey Paige A. Giorla , Rice Emily L. , Cieza Lucas , Pueyo Laurent , Bechter Eric B. , Gonzales Erica J. 
Published: February 2018

Abstract
The physical properties of brown dwarf companions found to orbit nearby, solar-type stars can be benchmarked against independent measures of their mass, age, chemical composition, and other parameters, offering insights into the evolution of substellar objects. The TRENDS high-contrast imaging survey has recently discovered a (mass/age/metallicity) benchmark brown dwarf orbiting the nearby (d = 18.69 ± 0.19 pc), G8V/K0V star HD 4747. We have acquired follow-up spectroscopic measurements of HD 4747 B using the Gemini Planet Imager to study its spectral type, effective temperature, surface gravity, and cloud properties. Observations obtained in the H-band and K
1-band recover the companion and reveal that it is near the L/T transition (T1 ± 2). Fitting atmospheric models to the companion spectrum, we find strong evidence for the presence of clouds. However, spectral models cannot satisfactorily fit the complete data set: while the shape of the spectrum can be well-matched in individual filters, a joint fit across the full passband results in discrepancies that are a consequence of the inherent color of the brown dwarf. We also find a 2σ tension in the companion mass, age, and surface gravity when comparing to evolutionary models. These results highlight the importance of using benchmark objects to study “secondary effects” such as metallicity, non-equilibrium chemistry, cloud parameters, electron conduction, non-adiabatic cooling, and other subtleties affecting emergent spectra. As a new L/T transition benchmark, HD 4747 B warrants further investigation into the modeling of cloud physics using higher resolution spectroscopy across a broader range of wavelengths, polarimetric observations, and continued Doppler radial velocity and astrometric monitoring.
Hubble Space Telescope Wide Field Camera 3 Observations of Escaping Lyman Continuum Radiation from Galaxies and Weak AGN at Redshifts z ∼ 2.3–4.1
Authors: Smith Brent M. , Windhorst Rogier A. , Jansen Rolf A. , Cohen Seth H. , Jiang Linhua , Dijkstra Mark , Koekemoer Anton M. , Bielby Richard , Inoue Akio K. , MacKenty John W. , O’Connell Robert W. , Silk Joseph I. 
Published: February 2018

Abstract
We present observations of escaping Lyman Continuum (LyC) radiation from 34 massive star-forming galaxies (SFGs) and 12 weak AGN with reliably measured spectroscopic redshifts at

. We analyzed Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) mosaics of the Early Release Science (ERS) field in three UVIS filters to sample the rest-frame LyC over this redshift range. With our best current assessment of the WFC3 systematics, we provide

upper limits for the average LyC emission of galaxies at

= 2.35, 2.75, and 3.60 to ∼28.5, 28.1, and 30.7 mag in image stacks of 11–15 galaxies in the WFC3/UVIS F225W, F275W, and F336W, respectively. The LyC flux of weak AGN at

= 2.62 and 3.32 are detected at 28.3 and 27.4 mag with S/Ns of ∼2.7 and 2.5 in F275W and F336W for stacks of 7 and 3 AGN, respectively, while AGN at

= 2.37 are constrained to ≳27.9 mag at

in a stack of 2 AGN. The stacked AGN LyC light profiles are flatter than their corresponding non-ionizing UV continuum profiles out to radii of

, which may indicate a radial dependence of porosity in the ISM. With synthetic stellar SEDs fit to UV continuum measurements longward of

and IGM transmission models, we constrain the absolute LyC escape fractions to

% at

= 2.35 and ≲55% at

= 2.75 and 3.60, respectively. All available data for galaxies, including published work, suggests a more sudden increase of

with redshift at

. Dust accumulating in (massive) galaxies over cosmic time correlates with increased H i column density, which may lead to reducing

more suddenly at

. This may suggest that SFGs collectively contributed to maintaining cosmic reionization at redshifts

, while AGN likely dominated reionization at

.
Magnetic Flux Cancelation as the Trigger of Solar Coronal Jets in Coronal Holes
Authors: Panesar Navdeep K. , Sterling Alphonse C. , Moore Ronald L. 
Published: February 2018

Abstract
We investigate in detail the magnetic cause of minifilament eruptions that drive coronal-hole jets. We study 13 random on-disk coronal-hole jet eruptions, using high-resolution X-ray images from the Hinode/X-ray telescope(XRT), EUV images from the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA), and magnetograms from the SDO/Helioseismic and Magnetic Imager (HMI). For all 13 events, we track the evolution of the jet-base region and find that a minifilament of cool (transition-region-temperature) plasma is present prior to each jet eruption. HMI magnetograms show that the minifilaments reside along a magnetic neutral line between majority-polarity and minority-polarity magnetic flux patches. These patches converge and cancel with each other, with an average cancelation rate of ∼0.6 × 1018 Mx hr−1 for all 13 jets. Persistent flux cancelation at the neutral line eventually destabilizes the minifilament field, which erupts outward and produces the jet spire. Thus, we find that all 13 coronal-hole-jet-driving minifilament eruptions are triggered by flux cancelation at the neutral line. These results are in agreement with our recent findings for quiet-region jets, where flux cancelation at the underlying neutral line triggers the minifilament eruption that drives each jet. Thus, from that study of quiet-Sun jets and this study of coronal-hole jets, we conclude that flux cancelation is the main candidate for triggering quiet-region and coronal-hole jets.
The Properties of Reconnection Current Sheets in GRMHD Simulations of Radiatively Inefficient Accretion Flows
Authors: Ball David , Özel Feryal , Psaltis Dimitrios , Chan Chi-Kwan , Sironi Lorenzo 
Published: February 2018

Abstract
Non-ideal magnetohydrodynamic (MHD) effects may play a significant role in determining the dynamics, thermal properties, and observational signatures of radiatively inefficient accretion flows onto black holes. In particular, particle acceleration during magnetic reconnection events may influence black hole spectra and flaring properties. We use representative general relativistic magnetohydrodynamic (GRMHD) simulations of black hole accretion flows to identify and explore the structures and properties of current sheets as potential sites of magnetic reconnection. In the case of standard and normal evolution (SANE) disks, we find that in the reconnection sites, the plasma beta ranges from 0.1 to 1000, the magnetization ranges from 10−4 to 1, and the guide fields are weak compared with the reconnecting fields. In magnetically arrested (MAD) disks, we find typical values for plasma beta from 10−2 to 103, magnetizations from 10−3 to 10, and typically stronger guide fields, with strengths comparable to or greater than the reconnecting fields. These are critical parameters that govern the electron energy distribution resulting from magnetic reconnection and can be used in the context of plasma simulations to provide microphysics inputs to global simulations. We also find that ample magnetic energy is available in the reconnection regions to power the fluence of bright X-ray flares observed from the black hole in the center of the Milky Way.
From Cool to Hot F-stars: The Influence of Two Ionization Regions in the Acoustic Oscillations
Authors: Brito Ana , Lopes Ilídio 
Published: February 2018

Abstract
The high-precision data available from the Kepler satellite allows us to study the complex outer convective envelopes of solar-type stars. We use a seismic diagnostic, specialized for investigating the outer layers of solar-type stars, to infer the impact of the ionization processes on the oscillation spectrum, for a sample of Kepler stars. These stars, of spectral type F, cover all of the observational seismic domain of the acoustic oscillation spectrum in solar-type stars. They also cover the range between a cool F-dwarf (∼6000 K) and a hotter F-star (∼6400 K). Our study reveals the existence of two relevant ionization regions. One of these regions, which is located closer to the surface of the star, is commonly associated with the second ionization of helium, although other chemical species also contribute to ionization. The second region, located deeper in the envelope, is linked with the ionization of heavy elements. Specifically, in this study, we analyze the elements carbon, nitrogen, oxygen, neon, and iron. Both regions can be related to the K electronic shell. We show that, while for cooler stars like the Sun, the influence of this second region on the oscillation frequencies is small; in hotter stars, its influence becomes comparable to the influence of the region of the second ionization of helium. This can guide us in the study of the outer layers of F-stars, specifically with the understanding of phenomena related to rotation and magnetic activity in these stars.
An Empirical Correlation of Tmax–MWD of Dwarf Novae and the Average White Dwarf Mass in Cataclysmic Variables in the Galactic Bulge
Authors: Yu Zhuo-li , Xu Xiao-jie , Li Xiang-Dong , Bao Tong , Li Ying-xi , Xing Yu-chen , Shen Yu-fu 
Published: February 2018

Abstract
The mean white dwarf (WD) mass in the Galactic bulge cataclysmic variables (CVs) was measured by applying the shock temperature-WD mass correlation of magnetic cataclysmic variables (mCVs) to the Galactic bulge X-ray emission (GBXE) spectra. However, the resulting mean WD mass is lower than that of the local CVs. This discrepancy could be explained by the dominating sources in the GBXE, which are non-mCVs instead of mCVs. In this work, we conduct a thorough investigation of the X-ray spectra of local DNe from the Suzaku archives and derive semi-empirical correlations between the shock temperature T
max, the flux ratio of Fe xxvi–Lyα to Fe xxv–Heα lines, and WD mass for quiescent, nonmagnetic CVs. By applying these correlations to the GBXE, we derive the average WD mass of CVs in the Galactic bulge to be 0.81 ± 0.07M
⊙. This value is consistent with previous optical measurements of WD mass in local CVs.
PHIBSS: Unified Scaling Relations of Gas Depletion Time and Molecular Gas Fractions*
Authors: Tacconi L. J. , Genzel R. , Saintonge A. , Combes F. , García-Burillo S. , Neri R. , Bolatto A. , Contini T. , Schreiber N. M. Förster , Lilly S. , Lutz D. , Wuyts S. , Accurso G. , Boissier J. , Boone F. , Bouché N. , Bournaud F. , Burkert A. , Carollo M. , Cooper M. , Cox P. , Feruglio C. , Freundlich J. , Herrera-Camus R. , Juneau S. , Lippa M. , Naab T. , Renzini A. , Salome P. , Sternberg A. , Tadaki K. , Übler H. , Walter F. , Weiner B. , Weiss A. 
Published: February 2018

Abstract
This paper provides an update of our previous scaling relations between galaxy-integrated molecular gas masses, stellar masses, and star formation rates (SFRs), in the framework of the star formation main sequence (MS), with the main goal of testing for possible systematic effects. For this purpose our new study combines three independent methods of determining molecular gas masses from CO line fluxes, far-infrared dust spectral energy distributions, and ∼1 mm dust photometry, in a large sample of 1444 star-forming galaxies between z = 0 and 4. The sample covers the stellar mass range log(M
*/M
⊙) = 9.0–11.8, and SFRs relative to that on the MS, δMS = SFR/SFR(MS), from 10−1.3 to 102.2. Our most important finding is that all data sets, despite the different techniques and analysis methods used, follow the same scaling trends, once method-to-method zero-point offsets are minimized and uncertainties are properly taken into account. The molecular gas depletion time t
depl, defined as the ratio of molecular gas mass to SFR, scales as (1 + z)−0.6 × (δMS)−0.44 and is only weakly dependent on stellar mass. The ratio of molecular to stellar mass μ
gas depends on (

1
+
z

)

2.5

×

(
δ
MS
)

0.52

×

(

M

*

)

−
0.36

, which tracks the evolution of the specific SFR. The redshift dependence of μ
gas requires a curvature term, as may the mass dependences of t
depl and μ
gas. We find no or only weak correlations of t
depl and μ
gas with optical size R or surface density once one removes the above scalings, but we caution that optical sizes may not be appropriate for the high gas and dust columns at high z.
The Coronal Monsoon: Thermal Nonequilibrium Revealed by Periodic Coronal Rain
Authors: Auchère Frédéric , Froment Clara , Soubrié Elie , Antolin Patrick , Oliver Ramon , Pelouze Gabriel 
Published: February 2018

Abstract
We report on the discovery of periodic coronal rain in an off-limb sequence of Solar Dynamics Observatory/Atmospheric Imaging Assembly images. The showers are co-spatial and in phase with periodic (6.6 hr) intensity pulsations of coronal loops of the sort described by Auchère et al. and Froment et al. These new observations make possible a unified description of both phenomena. Coronal rain and periodic intensity pulsations of loops are two manifestations of the same physical process: evaporation/condensation cycles resulting from a state of thermal nonequilibrium. The fluctuations around coronal temperatures produce the intensity pulsations of loops, and rain falls along their legs if thermal runaway cools the periodic condensations down and below transition-region temperatures. This scenario is in line with the predictions of numerical models of quasi-steadily and footpoint heated loops. The presence of coronal rain—albeit non-periodic—in several other structures within the studied field of view implies that this type of heating is at play on a large scale.
Numerical Simulations of Multiphase Winds and Fountains from Star-forming Galactic Disks. I. Solar Neighborhood TIGRESS Model
Authors: Kim Chang-Goo , Ostriker Eve C. 
Published: February 2018

Abstract
Gas blown away from galactic disks by supernova (SN) feedback plays a key role in galaxy evolution. We investigate outflows utilizing the solar neighborhood model of our high-resolution, local galactic disk simulation suite, TIGRESS. In our numerical implementation, star formation and SN feedback are self-consistently treated and well resolved in the multiphase, turbulent, magnetized interstellar medium. Bursts of star formation produce spatially and temporally correlated SNe that drive strong outflows, consisting of hot (

) winds and warm (

) fountains. The hot gas at distance

from the midplane has mass and energy fluxes nearly constant with d. The hot flow escapes our local Cartesian box barely affected by gravity, and is expected to accelerate up to terminal velocity of

. The mean mass and energy loading factors of the hot wind are 0.1 and 0.02, respectively. For warm gas, the mean outward mass flux through

is comparable to the mean star formation rate, but only a small fraction of this gas is at velocity

. Thus, the warm outflows eventually fall back as inflows. The warm fountain flows are created by expanding hot superbubbles at

at larger d neither ram pressure acceleration nor cooling transfers significant momentum or energy flux from the hot wind to the warm outflow. The velocity distribution at launching near

is a better representation of warm outflows than a single mass loading factor, potentially enabling development of subgrid models for warm galactic winds in arbitrary large-scale galactic potentials.
Distributed Star Formation throughout the Galactic Center Cloud Sgr B2
Authors: Ginsburg Adam , Bally John , Barnes Ashley , Bastian Nate , Battersby Cara , Beuther Henrik , Brogan Crystal , Contreras Yanett , Corby Joanna , Darling Jeremy , De Pree Chris , Galván-Madrid Roberto , Garay Guido , Henshaw Jonathan , Hunter Todd , Kruijssen J. M. Diederik , Longmore Steven , Lu Xing , Meng Fanyi , Mills Elisabeth A. C. , Ott Juergen , Pineda Jaime E. , Sánchez-Monge Álvaro , Schilke Peter , Schmiedeke Anika , Walker Daniel , Wilner David 
Published: February 2018

Abstract
We report ALMA observations with resolution ≈0.″5 at 3 mm of the extended Sgr B2 cloud in the Central Molecular Zone (CMZ). We detect 271 compact sources, most of which are smaller than 5000 au. By ruling out alternative possibilities, we conclude that these sources consist of a mix of hypercompact H ii regions and young stellar objects (YSOs). Most of the newly detected sources are YSOs with gas envelopes that, based on their luminosities, must contain objects with stellar masses

M

*

≳
8

M

⊙

. Their spatial distribution spread over a ∼12 × 3 pc region demonstrates that Sgr B2 is experiencing an extended star formation event, not just an isolated “starburst” within the protocluster regions. Using this new sample, we examine star formation thresholds and surface density relations in Sgr B2. While all of the YSOs reside in regions of high column density (

N
(

H

2

)
≳
2
×

10

23

cm

−
2

), not all regions of high column density contain YSOs. The observed column density threshold for star formation is substantially higher than that in solar vicinity clouds, implying either that high-mass star formation requires a higher column density or that any star formation threshold in the CMZ must be higher than in nearby clouds. The relation between the surface density of gas and stars is incompatible with extrapolations from local clouds, and instead stellar densities in Sgr B2 follow a linear

Σ

*

–

Σ

gas

relation, shallower than that observed in local clouds. Together, these points suggest that a higher volume density threshold is required to explain star formation in CMZ clouds.