bluuebunny/crossref_metadata_2025_split huggingface dataset:
Circulating interleukins (IL6)-An early predictor of insulin resistance
Authors: Porwal Naveen Bhartia , Ghildiyal Archna , Singh Shraddha , Bhattarcharya Sandeep , Iqbal Bushra , Tiwari Sunita , Singh Kalpana 
Published: October 2016

Background: Obesity is an increasing health concern that is highly correlated with the risk of developing insulin resistance and type-2 diabetes The insulin resistance represents an important association between obesity and the morbidities that lead concomitantly to increase in visceral adiposity. The more resistant to insulin the individual is, the higher the risk for the development of type-2 diabetes and cardiovascular disease. The purpose of this study was to assess the correlation between insulin resistance and the production of cytokines (IL6) and to establish the relations between interleukins IL-6 and various anthropometric measurementsMaterial and Methods: A cross-sectional study was carried on 100 healthy individuals (55 males and 45 females) aged between 18-25 years were enrolled after obtaining their written consent in Department of Physiology, KGMU. All the subjects were evaluated anthropometric: Body mass index (BMI), Waist circumference (WC), Hip circumference (HC), Waist hip ratio and Waist height ratio as per standard protocol. Metabolic measures ( Fasting glucose and insulin) were done using commercial kit. Insulin resistance was measured using homeostasis model.Results: There was a significant positive correlation between interleukin 6 and fasting serum insulin (r=0.56, p=0.001) & HOMA IR (r=0.57, p=0.001). Correlation between anthropometric measure and Interleukins (IL-6) was also observed to be positive and mild.Conclusion: A significant positive correlation was seen between IL-6 and fasting serum insulin and HOMA-IR indicating IL 6 as a good predictive marker for insulin resistance.Asian Journal of Medical Sciences Vol.7(6) 2016 20-25
The outcome of vitrectomy with internal limiting membrane peeling for chronic macular hole at Biratnagar eye hospital: A tertiary eye care center in Nepal
Authors: Agarwal Lalit , Agrawal Nisha , Karki Pratap , Anand Abhishek 
Published: October 2016

Background: A macular hole is a full-thickness defect of retinal tissue involving the anatomic fovea, thereby affecting central visual acuity. Pars plana vitrectomy and gas tamponade is a recognised modality of treatment for macular hole.Larger holes are more likely to remain open after repair and late reopening after an initially closed macular hole is seen in macular holes larger than 400 μm.Aims and Objective: To evaluate the anatomical and functional outcome of pars plana vitrectomy with internal limiting membrane peeling for chronic stage 3 macular hole.Materials and Methods: Records of 15 patients with stage 3 chronic macular holes operated from 1st January 2013 to 30th June 2013 and completed 1 year of follow up were retrospectively evaluated and included in the study. Preoperative best distance corrected visual acuity (BCVA), preoperative macular hole size, final BCVA and macular hole status at 1 year follow up were recorded. Macular hole closure and visual improvement was calculated. Correlation of macular hole closure and visual improvement with various macular hole parameter was estimated.Results: Eleven (73.3%) macular holes closed at 1 year follow-up. Mean BCVA improved from 1.2 ± 0.27 to 0.89 ± 0.36 logarithm of minimum angle of resolution at 1 year (p<0.001). Visual improvement was seen in only eight (53.3%) eyes. Both macular hole closure and visual improvement showed no correlation with minimum linear diameter, base diameter and hole height.Conclusion: Chronic stage 3 macular hole can be closed successfully in majority of patients with fairly good visual improvement. Macular hole parameters of stage 3 holes may not have any correlation with the anatomical and visual outcome.Asian Journal of Medical Sciences Vol.7(6) 2016 43-46
Diagnosis of diabetes mellitus on the basis of HbA1c: Is this true in hypothyroidism also?
Authors: Singhai Abhishek , Kabra Prakhar 
Published: October 2016

Background: Hypothyroidism may leads to hypoproliferative anemia. It is possible that this reduced erythropoiesis may result false elevation of HbA1c in some cases and further leading to an erroneous diagnosis of pre diabetes or diabetes.Aims and Objective: This study was planned to assess changes in HbA1c after initiation of thyroxine replacement in patients with subclinical and overt hypothyroidism.Settings and Design: This prospective study was conducted at Department of General Medicine of a tertiary care centre over one year.Methods and Material: 100 subjects were recruited for the study. Fasting blood glucose, serum creatinine, hemoglobin, HbA1c, reticulocyte count, serum free T4 and TSH estimation done in all subjects. Hypothyroid patients were started on thyroxine. After three months of documentation of euthyroidism, same investigations were repeated.Statistical analysis used: Statistical software, SPSS version 17.0 was used for analysis.Results: After correction of hypothyroidism, TSH decreased from 92.3(±30.9) to 3.4±2.9 µIU/L and 12.2(±4.5) to 4.4±2.9 µIU/ml in overt hypothyroidism and subclinical hypothyroidism respectively. There was a statistically significant fall in the HbA1c (SD) from 5.9% (0.8) to 5.6% (0.6) and 6.0% (0.3) to 5.7% (0.3) following the correction of hypothyroidism in overt hypothyroidism and subclinical hypothyroidism respectively. However, there were no statistically significant changes in the fasting as well as postprandial blood glucose.Conclusions: Our study demonstrated that HbA1c values are falsely increased in patients with hypothyroidism. This falsely raised HbA1c became normal after thyroxine supplement.Asian Journal of Medical Sciences Vol.7(6) 2016 36-39
Morphometric analysis of mental foramen in human dry mandibles of nepalese population
Authors: Kadel Muna , Sedhain Bishwo P , Dangol Prakash MS 
Published: October 2016

Background: Mental foramina are located bilaterally in the antero-lateral aspect of the body of mandible. It transmits mental nerve, and vessels. The location, shape, size, direction and number of mental foramen in human mandibles are subject of variation. Aims and Objective: To establish the location, shape, size, direction and incidence of mental foramen (MF) in dry human mandibles of Nepalese population.Materials and Methods: One hundred dry human mandibles of unknown age and sex were selected randomly. Shape, size, position of MF with respect to tooth and other anatomical landmark were determined. Student paired t-test was used for specific statistical analysis.Results: In most cases (61%), the MF was oval in shape & situated below the apex of second premolar (58% on right side and 69% on left side). Various parameters investigated were, the horizontal distance between (1) base of mandible and MF was 12.24 mm on right and 12.26mm on the left, (2) alveolar margin and MF was 13.95 mm on right &13.75 mm on left (3) symphysis menti of mandible and MF was 26.71 mm on right and 26.49 mm on left, (4) posterior border of mandible and MF was 65.34 mm on right and 65.68mm on left.Conclusion: By the knowledge of position, shape, size, direction and distance of the mental foramen from various landmarks and the presence of the accessory foramen may be of much use to dental surgeons.Asian Journal of Medical Sciences Vol.7(5) 2016 82-86
FILTERING METEOROID FLIGHTS USING MULTIPLE UNSCENTED KALMAN FILTERS
Authors: Sansom E. K. , Bland P. A. , Rutten M. G. , Paxman J. , Towner M. C. 
Published: October 2016

ABSTRACT
Estimator algorithms are immensely versatile and powerful tools that can be applied to any problem where a dynamic system can be modeled by a set of equations and where observations are available. A well designed estimator enables system states to be optimally predicted and errors to be rigorously quantified. Unscented Kalman filters (UKFs) and interactive multiple models can be found in methods from satellite tracking to self-driving cars. The luminous trajectory of the Bunburra Rockhole fireball was observed by the Desert Fireball Network in mid-2007. The recorded data set is used in this paper to examine the application of these two techniques as a viable approach to characterizing fireball dynamics. The nonlinear, single-body system of equations, used to model meteoroid entry through the atmosphere, is challenged by gross fragmentation events that may occur. The incorporation of the UKF within an interactive multiple model smoother provides a likely solution for when fragmentation events may occur as well as providing a statistical analysis of the state uncertainties. In addition to these benefits, another advantage of this approach is its automatability for use within an image processing pipeline to facilitate large fireball data analyses and meteorite recoveries.
HIGH-MASS STAR FORMATION TOWARD SOUTHERN INFRARED BUBBLE S10
Authors: Das Swagat Ranjan , Tej Anandmayee , Vig Sarita , Ghosh Swarna K. , Ishwara Chandra C. H. 
Published: October 2016

ABSTRACT
An investigation in radio and infrared wavelengths of two high-mass star-forming regions toward the southern Galactic bubble S10 is presented here. The two regions under study are associated with the broken bubble S10 and Extended Green Object, G345.99-0.02, respectively. Radio continuum emission mapped at 610 and 1280 MHz using the Giant Metrewave Radio Telescope, India, is detected toward both of the regions. These regions are estimated to be ionized by early-B- to late-O-type stars. Spitzer GLIMPSE mid-infrared data is used to identify young stellar objects (YSOs) associated with these regions. A Class-I/II-type source, with an estimated mass of 6.2 M
⊙, lies ∼7″ from the radio peak. Pixel-wise, modified blackbody fits to the thermal dust emission using Herschel far-infrared data is performed to construct dust temperature and column density maps. Eight clumps are detected in the two regions using the 250 μm image. The masses and linear diameter of these range between ∼300–1600 M
⊙ and 0.2–1.1 pc, respectively, which qualifies them as high-mass star-forming clumps. Modeling of the spectral energy distribution of these clumps indicates the presence of high luminosity, high accretion rate, massive YSOs possibly in the accelerating accretion phase. Furthermore, based on the radio and MIR morphology, the occurrence of a possible bow wave toward the likely ionizing star is explored.
X-RAY FLARING ACTIVITY OF MRK 421 IN THE FIRST HALF OF 2013
Authors: Kapanadze B. , Dorner D. , Vercellone S. , Romano P. , Aller H. , Aller M. , Hughes P. , Reynolds M. , Kapanadze S. , Tabagari L. 
Published: October 2016

ABSTRACT
We present the results of the Swift and NuSTAR observations of the nearby BL Lac object Mrk 421 during 2013 January–June. The source exhibited a strong long-term variability in the 0.3–10 keV and 3–79 keV bands with the maximum-to-minimum daily-binned flux ratios of 22 and 95, respectively, in about 3 months, mainly due to unprecedented strong X-ray outbursts by more than an order of magnitude in both bands within 2 weeks in 2013 April when the 0.3–10 keV count rate exceeded the level of 200 cts s−1 for the first time, and Mrk 421 became one of the brightest sources in the X-ray sky. The source was also very active on intra-day timescales, and it showed flux doubling and halving timescales of 1.16–7.20 hr and 1.04–3.54 hr, respectively. On some occasions, the flux varied by 4%–23% within 300–840 s. During this period, the source also exhibited some of the most extreme X-ray spectral variability ever reported for BL Lacs—the location of the synchrotron spectral energy distribution peak shifted from a few eV to ∼10 keV, and the photon index at 1 keV and curvature parameter varied on timescales from a few weeks down to intervals shorter than 1 ks. MAGIC and First G-APD Cherenkov Telescope observations also revealed a very strong very high energy (VHE) flare during April 11–17. The UV and HE γ-ray flares were much weaker compared to their X-ray counterparts, and they generally showed significantly stronger correlation with each other than with the X-ray fluxes.
RADIAL DISTRIBUTION OF ISM GAS-PHASE METALLICITY IN CLASH CLUSTERS AT z ∼ 0.35: A NEW OUTLOOK ON ENVIRONMENTAL IMPACT ON GALAXY EVOLUTION
Authors: Gupta Anshu , Yuan Tiantian , Tran Kim-Vy H. , Martizzi Davide , Taylor Philip , Kewley Lisa J. 
Published: October 2016

ABSTRACT
We present the first observation of cluster-scale radial metallicity gradients from star-forming galaxies. We use DEIMOS on the Keck II telescope to observe two CLASH clusters at z ∼ 0.35: MACS J1115+0129 and RX J1532+3021. Based on our measured interstellar medium properties of star-forming galaxies out to a radius of 2.5 Mpc from the cluster center, we find that the galaxy metallicity decreases as a function of projected cluster-centric distance (−0.15 ± 0.08 dex/Mpc) in MACS 1115+01. On the mass–metallicity relation (MZR), star-forming galaxies in MACS J1115+01 are offset to higher metallicity (∼0.2 dex) than the local Sloan Digital Sky Survey galaxies at a fixed mass range. In contrast, the MZR of RX J1532+30 is consistent with the local comparison sample. RX J1532+30 exhibits a bimodal radial metallicity distribution, with one branch showing a similar negative gradient to MACS J1115+01 (−0.14 ± 0.05 dex/Mpc) and the other branch showing a positive radial gradient. The positive gradient branch in RX J1532+30 is likely caused by either interloper galaxies or an in-plane merger, indicating that cluster-scale abundance gradients probe cluster substructures and thus the dynamical state of a cluster. Most strikingly, we discover that neither the radial metallicity gradient nor the offset from the MZR is driven by the stellar mass. We compare our observations with Rhapsody-G cosmological hydrodynamical zoom-in simulations of relaxed galaxy clusters and find that the simulated galaxy cluster also exhibits a negative abundance gradient, albeit with a shallower slope (−0.04 ± 0.03 dex/Mpc). Our observations suggest that the negative radial gradient originates from ram pressure stripping and/or strangulation processes in the cluster environments.
GLOBAL ENERGETICS OF SOLAR FLARES. IV. CORONAL MASS EJECTION ENERGETICS
Authors: Aschwanden Markus J. 
Published: October 2016

ABSTRACT
This study entails the fourth part of a global flare energetics project, in which the mass m
cme, kinetic energy E
kin, and the gravitational potential energy E
grav of coronal mass ejections (CMEs) is measured in 399 M and X-class flare events observed during the first 3.5 years of the Solar Dynamics Observatory (SDO) mission, using a new method based on the EUV dimming effect. EUV dimming is modeled in terms of a radial adiabatic expansion process, which is fitted to the observed evolution of the total emission measure of the CME source region. The model derives the evolution of the mean electron density, the emission measure, the bulk plasma expansion velocity, the mass, and the energy in the CME source region. The EUV dimming method is truly complementary to the Thomson scattering method in white light, which probes the CME evolution in the heliosphere at r ≳ 2 R
⊙, while the EUV dimming method tracks the CME launch in the corona. We compare the CME parameters obtained in white light with the LASCO/C2 coronagraph with those obtained from EUV dimming with the Atmospheric Imaging Assembly onboard the SDO for all identical events in both data sets. We investigate correlations between CME parameters, the relative timing with flare parameters, frequency occurrence distributions, and the energy partition between magnetic, thermal, nonthermal, and CME energies. CME energies are found to be systematically lower than the dissipated magnetic energies, which is consistent with a magnetic origin of CMEs.
FERMI/LAT STUDY OF GAMMA-RAY EMISSION IN THE DIRECTION OF THE MONOCEROS LOOP SUPERNOVA REMNANT
Authors: Katagiri H. , Sugiyama S. , Ackermann M. , Ballet J. , Casandjian J. M. , Hanabata Y. , Hewitt J. W. , Kerr M. , Kubo H. , Lemoine-Goumard M. , Ray P. S. 
Published: October 2016

ABSTRACT
We present an analysis of the gamma-ray measurements by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope in the region of the supernova remnant (SNR) Monoceros Loop (G205.5+0.5). The brightest gamma-ray peak is spatially correlated with the Rosette Nebula, which is a molecular cloud complex adjacent to the southeast edge of the SNR. After subtraction of this emission by spatial modeling, the gamma-ray emission from the SNR emerges, which is extended and fit by a Gaussian spatial template. The gamma-ray spectra are significantly better reproduced by a curved shape than a simple power law. The luminosities between 0.2 and 300 GeV are

erg s−1 for the SNR and

erg s−1 for the Rosette Nebula, respectively. We argue that the gamma-rays likely originate from the interactions of particles accelerated in the SNR. The decay of neutral pions produced in nucleon–nucleon interactions of accelerated hadrons with interstellar gas provides a reasonable explanation for the gamma-ray emission of both the Rosette Nebula and the Monoceros SNR.
BAYESIAN ESTIMATION OF THERMONUCLEAR REACTION RATES
Authors: Iliadis C. , Anderson K. S. , Coc A. , Timmes F. X. , Starrfield S. 
Published: October 2016

ABSTRACT
The problem of estimating non-resonant astrophysical S-factors and thermonuclear reaction rates, based on measured nuclear cross sections, is of major interest for nuclear energy generation, neutrino physics, and element synthesis. Many different methods have been applied to this problem in the past, almost all of them based on traditional statistics. Bayesian methods, on the other hand, are now in widespread use in the physical sciences. In astronomy, for example, Bayesian statistics is applied to the observation of extrasolar planets, gravitational waves, and Type Ia supernovae. However, nuclear physics, in particular, has been slow to adopt Bayesian methods. We present astrophysical S-factors and reaction rates based on Bayesian statistics. We develop a framework that incorporates robust parameter estimation, systematic effects, and non-Gaussian uncertainties in a consistent manner. The method is applied to the reactions d(p,γ)3He, 3He(3He,2p)4He, and 3He(α,γ)7Be, important for deuterium burning, solar neutrinos, and Big Bang nucleosynthesis.
GLOBULAR CLUSTERS, ULTRACOMPACT DWARFS, AND DWARF GALAXIES IN ABELL 2744 AT A REDSHIFT OF 0.308
Authors: Lee Myung Gyoon , Jang In Sung 
Published: October 2016

ABSTRACT
We report a photometric study of globular clusters (GCs), ultracompact dwarfs (UCDs), and dwarf galaxies in the giant merging galaxy cluster Abell 2744 at z = 0.308. Color–magnitude diagrams of the point sources derived from deep F814W (rest frame r′) and F105W (rest frame I) images of Abell 2744 in the Hubble Space Telescope Frontier Field show a rich population of point sources, which have colors that are similar to those of typical GCs. These sources are as bright as

(26.0 < F814W(Vega) ≤ 29.5) mag, being mostly UCDs and bright GCs in Abell 2744. The luminosity function (LF) of these sources shows a break at

(F814W ≈ 28.0) mag, indicating a boundary between UCDs and bright GCs. The numbers of GCs and UCDs are estimated to be 1,711,640+589,760
−430,500 and 147 ± 26, respectively. The clustercentric radial number density profiles of the UCDs and bright GCs show similar slopes, but these profiles are much steeper than those of the dwarf galaxies and the mass density profile based on gravitational lensing analysis. We derive an LF of the red sequence galaxies for

mag. The faint end of this LF is fit well by a flat power law with

, showing no faint upturn. These results support the galaxy-origin scenario for bright UCDs: they are the nuclei of dwarf galaxies that are stripped when they pass close to the center of massive galaxies or a galaxy cluster, while some of the faint UCDs are at the bright end of the GCs.
GRAPHITE REVISITED
Authors: Draine B. T. 
Published: October 2016

ABSTRACT
Laboratory measurements are used to constrain the dielectric tensor for graphite, from microwave to X-ray frequencies. The dielectric tensor is strongly anisotropic even at X-ray energies. The discrete dipole approximation is employed for accurate calculations of absorption and scattering by single-crystal graphite spheres and spheroids. For randomly oriented single-crystal grains, the so-called

approximation for calculating absorption and scattering cross sections is exact in the limit

and provides better than ∼10% accuracy in the optical and UV even when

is not small, but becomes increasingly inaccurate at infrared wavelengths, with errors as large as ∼40% at

. For turbostratic graphite grains, the Bruggeman and Maxwell Garnett treatments yield similar cross sections in the optical and ultraviolet, but diverge in the infrared, with predicted cross sections differing by over an order of magnitude in the far-infrared. It is argued that the Maxwell Garnett estimate is likely to be more realistic, and is recommended. The out-of-plane lattice resonance of graphite near 11.5 μm may be observable in absorption with the MIRI spectrograph on James Webb Space Telescope. Aligned graphite grains, if present in the interstellar medium, could produce polarized X-ray absorption and polarized X-ray scattering near the carbon K edge.
MC2: DYNAMICAL ANALYSIS OF THE MERGING GALAXY CLUSTER MACS J1149.5+2223
Authors: Golovich Nathan , Dawson William A. , Wittman David , Ogrean Georgiana , Weeren Reinout van , Bonafede Annalisa 
Published: October 2016

ABSTRACT
We present an analysis of the merging cluster MACS J1149.5+2223 using archival imaging from Subaru/Suprime-Cam and multi-object spectroscopy from Keck/DEIMOS and Gemini/GMOS. We employ two- and three-dimensional substructure tests and determine that MACS J1149.5+2223 is composed of two separate mergers among three subclusters occurring ∼1 Gyr apart. The primary merger gives rise to elongated X-ray morphology and a radio relic in the southeast. The brightest cluster galaxy is a member of the northern subcluster of the primary merger. This subcluster is very massive (

). The southern subcluster is also very massive (

), yet it lacks an associated X-ray surface brightness peak, and it has been unidentified previously despite the detailed study of this Frontier Field cluster. A secondary merger is occurring in the north along the line of sight (LOS) with a third, less massive subcluster (

). We perform a Monte Carlo dynamical analysis on the main merger and estimate a collision speed at pericenter of

km s−1. We show the merger to be returning from apocenter with core passage occurring

Gyr before the observed state. We identify the LOS merging subcluster in a strong lensing analysis in the literature and show that it is likely bound to MACS J1149 despite having reached an extreme collision velocity of ∼4000 km s−1.
DEEP OPTICAL OBSERVATIONS OF UNUSUAL NEUTRON STAR CALVERA WITH THE GTC∗
Authors: Shibanov Yury , Danilenko Andrey , Zharikov Sergey , Shternin Peter , Zyuzin Dima 
Published: October 2016

ABSTRACT
Calvera is an unusual, isolated neutron star with a pure thermal X-ray spectrum typical of central compact objects in supernova remnants. On the other hand, its rotation period and spin-down rate are typical of ordinary rotation-powered pulsars. It was discovered and studied through X-rays, and has not yet been detected in other spectral domains. We present deep optical imaging of the Calvera field, obtained with the Gran Telescopio Canarias, in the

and

bands. Within the vicinity of

of Calvera, we detected two point-like objects that were invisible at previous shallow observations. However, accurate astrometry showed that neither of them can be identified with the pulsar. We put new upper limits of

and

on its optical brightness. We also reanalyzed all available archival X-ray data on Calvera. Comparison of the Calvera thermal emission parameters and upper limits on optical and non-thermal X-ray emission with respective data on rotation-powered pulsars shows that Calvera might belong to the class of ordinary middle-aged pulsars, if we assume that its distance is in the range of 1.5–5 kpc.