bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Capital Flow Volatility Spillover in Some Selected African Economies
Authors: Kwarah Abdullahi Murtala , Kaseeram Irrshad , Rafindadi Aliyu Sanusi 
Published: April 2021

Purpose: The study conducted an empirical examination of the link between capital flows and exchange rate by examining the relative influence of FDI and FPI on the exchange rates.
Method: The study proceeded with the EGARCH model and the data sample covering the period from 1990-2016. The data were subjected to cross-country screening. The screening criteria are such that all the data that constitute capital in all sampled countries must have equal sample sizes. The measurement of capital flow in each of the sampled countries was restricted to two categories capital, namely, foreign portfolio investment (FPI) and foreign direct investment (FDI).
Results: The research establishes that the behavior of capital flow volatility spillover of the sample countries' currencies exchange rate differs, with only South Africa's and Morocco's currencies revealing some slight similarity and existence of asymmetric volatility spillover from capital flows to exchange rate. Additionally, the study discloses that capital flows spillover has a considerable effect on exchange rate volatility than harmful spillover. The study also observed that positive shocks associated with capital flow volatility affect exchange rate value in Botswana more than capital outflow. Further positive capital flow spillover impending from capital inflow has a considerable effect on exchange rate volatility than the harmful spillover impending from the capital outflow. Further, the positive capital flow spill over impending from capital inflow significantly affects exchange rate volatility more than the negative spillovers that emanate from the capital outflow.
Implications: This suggests that the monetary policy should consider options that can accelerate capital flow into the Moroccan economy. However, in South Africa for any given quantum of capital flow into the economy, the South African Reserve Bank must use instruments to affect stability; otherwise, the currency exchange rate could remain unstable. Thus, capital withdrawals out of the Egyptian economy will create domestic currency instability.

Keywords: Spill-over, Foreign Direct Investments (FDI), Portfolio Investments (PI), asymmetric, capital flow volatility, Exchange rate volatility.
The Effects of Mitochondrial Mt4977 Deletion on Platelet Function in Ischemic Heart Disease Patients
Authors: ÖZAYDIN Ahmet , KERİMOVA Ayla , ONARAN İlhan 
Published: April 2021

Objective: It is known that point mutations, duplications and deletions occur in mitochondrial DNAs (mtDNA) of different tissues of individuals. Among the deletions observed, mt4977 mutation, which is located at nucleotide positions 8470-8482 and 13447-13459 and causes the loss of 4977 base pairs, is the most common. mtDNA 4977 deletion leads to the loss of 8 genes encoding subunits of respiratory chain complexes. Consequently, the deletion could be expected to inhibit the oxidative function and reduce ATP production level. It is known that mitochondrial ATP production has an important role on platelet functions. However, there is no information about this in the literature. Since platelet activation in ischemic heart disease (IHD) has been shown to play an important role in the pathophysiology of the disease, we wanted to examine the relationship between platelet function and mtDNA 4977 deletion in ischemic heart disease.
Material and Method: Platelet functions were studied by giving ADP stimulus with the help of lumiaggregometer device to evaluate in terms of secretion and aggregation. ATP measurement was performed with the bioluminescence assay kit. mtDNA 4977 deletion was determined by the modified simultaneous quantitative polymerase chain reaction method.
Results: The frequency of mtDNA 4977 deletion and mtDNA copy number were higher in platelets of the patients compared with the healthy control group (p0.05).
Conclusion: It was observed that increased deletion in patients with IHD did not have a significant effect on
platelet dysfunction compared with healthy control subjects.
Multidrug Resistance of Uropathogens at Governmental Hospitals in the Gaza Strip/Palestine
Authors: Alkhodari Sameh A. , Elmanama Abdelraouf A. 
Published: April 2021

Urinary tract infection is a public health problem worldwide. E. coli and klebsiella are among the main etiologic for UTI in Gaza Strip. The growing variations in resistance among uropathogens to antimicrobials is multifactorial and varies globally. It greatly reduces/limits or complicate treatment option.
Aims: To determine the pattern of antimicrobial resistance and multidrug resistance among uropathogens at governmental hospitals.
Methods: We analyzed the data of 11,890 urine samples processed in governmental hospitals in the Gaza Strip, Palestine during 2019. The percentage of resistance was calculated for uropathogens, and then multidrug resistance was calculated according to “CDC” definition.
Results: Of 11,890 urine samples, 2910 (24.5%) showed significant growth. Escherichia coli was isolated most frequently (1743; 59.9%), followed by Klebsiella spp. (725; 24.9%), Pseudomonas spp. (123; 4.2%), Streptococcus spp. (98; 3.4%), Staphylococcus aureus (41; 1.4%). Microorganisms resistance was high against Ampicillin (92.4%) and Amoxicillin (91.1%), Co-Trimoxazole (68.2%), Cefalexin (64.9%), Doxycycline (61.9%), Nalidixic acid (53.6%), Cefuroxime (53.0%), Ceftriaxone (48.9%), Ceftazidime (43.1%), Ciprofloxacin (36.9%), Gentamicin (25.8%), Amikacin (3.2%). The resistance of microorganisms in males is higher than females. Multidrug resistance was detected in 37% of E. coli and 53% in Klebsiella spp.
Conclusion: Resistance is high and variable among uropathogens isolated from patients in Gaza strip. Both age and gender are risk factors in both infection and resistance pattern. The multidrug resistance percentage is growing remarkably in Gaza Strip.
Keywords: Uropathogens, Resistance, Urinary tract infection, Multidrug resistance, Gaza strip, Palestine
The Location of Young Pulsar PSR J0837–2454: Galactic Halo or Local Supernova Remnant?
Authors: Pol Nihan , Burke-Spolaor Sarah , Hurley-Walker Natasha , Blumer Harsha , Johnston Simon , Keith Michael , Keane Evan F. , Burgay Marta , Possenti Andrea , Petroff Emily , Bhat N. D. Ramesh 
Published: April 2021

Abstract
We present the discovery and timing of the young (age ∼28.6 kyr) pulsar PSR J0837–2454. Based on its high latitude (b = 98) and dispersion measure (DM = 143 pc cm−3), the pulsar appears to be at a z-height of >1 kpc above the Galactic plane, but near the edge of our Galaxy. This is many times the observed scale height of the canonical pulsar population, which suggests this pulsar may have been born far out of the plane. If accurate, the young age and high z-height imply that this is the first pulsar known to be born from a runaway O/B star. In follow-up imaging with the Australia Telescope Compact Array (ATCA), we detect the pulsar with a flux density S
1400 = 0.18 ± 0.05 mJy. We do not detect an obvious supernova remnant around the pulsar in our ATCA data, but we detect a colocated, low-surface-brightness region of ∼15 extent in archival Galactic and Extragalactic All-sky MWA Survey data. We also detect colocated Hα emission from the Southern Hα Sky Survey Atlas. Distance estimates based on these two detections come out to ∼0.9 kpc and ∼0.2 kpc, respectively, both of which are much smaller than the distance predicted by the NE2001 model (6.3 kpc) and YMW model (>25 kpc) and place the pulsar much closer to the plane of the Galaxy. If the pulsar/remnant association holds, this result also highlights the inherent difficulty in the classification of transients as “Galactic” (pulsar) or “extragalactic” (fast radio burst) toward the Galactic anticenter based solely on the modeled Galactic electron contribution to a detection.
Enhanced X-Ray Emission from the Most Radio-powerful Quasar in the Universe’s First Billion Years
Authors: Connor Thomas , Bañados Eduardo , Stern Daniel , Carilli Chris , Fabian Andrew , Momjian Emmanuel , Rojas-Ruiz Sofía , Decarli Roberto , Farina Emanuele Paolo , Mazzucchelli Chiara , Earnshaw Hannah P. 
Published: April 2021

Abstract
We present deep (265 ks) Chandra X-ray observations of PSO J352.4034−15.3373, a quasar at z = 5.831 that, with a radio-to-optical flux ratio of R > 1000, is one of the radio-loudest quasars in the early universe and is the only quasar with observed extended radio jets of kiloparsec scale at z ≳ 6. Modeling the X-ray spectrum of the quasar with a power law, we find a best fit of

Γ
=

1.99

−
0.28

+
0.29

, leading to an X-ray luminosity of

L

2
–
10

=

1.26

−
0.33

+
0.45

×

10

45

erg

s

−
1

and an X-ray to UV brightness ratio of α
OX = −1.45 ± −0.11. We identify a diffuse structure 50 kpc (∼8″) to the NW of the quasar along the jet axis that corresponds to a 3σ enhancement in the angular density of emission and can be ruled out as a background fluctuation with a probability of P = 0.9985. While with few detected photons the spectral fit of the structure is uncertain, we find that it has a luminosity of L
2–10 ∼ 1044 erg s−1. These observations therefore potentially represent the most distant quasar jet yet seen in X-rays. We find no evidence for excess X-ray emission where the previously reported radio jets are seen (which have an overall linear extent of 0.″28), and a bright X-ray point source located along the jet axis to the SE is revealed by optical and NIR imaging to not be associated with the quasar.
Two-fluid Modeling of Acoustic Wave Propagation in Gravitationally Stratified Isothermal Media
Authors: Zhang Fan , Poedts Stefaan , Lani Andrea , Kuźma Błażej , Murawski Kris 
Published: April 2021

Abstract
To study acoustic wave propagation and the corresponding energy deposition in partially ionized plasmas, we use a two-fluid computational model that treats neutrals and charged particles (electrons and ions) as two separate fluids. This two-fluid model takes into account the ion–neutral collisions, ionization, and recombination, allowing us to investigate both the collisional and reactive interactions between uncoupled ions and neutrals in the plasmas. In the present numerical simulations, the initial density is specified to reach hydrostatic equilibrium, and as a comparison, chemical equilibrium is also taken into account to provide a density profile that differs from typical hydrostatic equilibrium profiles. External velocity drivers are then imposed to generate monochromatic acoustic waves. As is well known, the upward propagating acoustic waves steepen in gravitationally stratified plasmas due to the exponentially decreasing density, and they heat the plasmas in the nonlinear regimes where kinetic energy is dissipated by shock waves and collisional interactions. In particular, the lower ionization fraction resulting from the present initial chemical equilibrium significantly enhances the heating efficiency. Moreover, the ionization process absorbs a significant amount of energy, and the decoupling between ions and neutrals is also enhanced while considering ionization and recombination. Therefore, simulations without considering ionization and recombination may overestimate the overall heating effects but also underestimate the energy dissipation. The results also suggest that a more accurate ionization and recombination model could be essential for improving the modeling of partially ionized plasmas.
The Far Ultraviolet M-dwarf Evolution Survey. I. The Rotational Evolution of High-energy Emissions*
Authors: Pineda J. Sebastian , Youngblood Allison , France Kevin 
Published: April 2021

Abstract
M-dwarf stars are prime targets for exoplanet searches because of their close proximity and favorable properties for both planet detection and characterization. However, the potential habitability and atmospheric characterization of these exoplanetary systems depends critically on the history of high-energy stellar radiation from X-rays to NUV, which drive atmospheric mass loss and photochemistry in the planetary atmospheres. With the Far Ultraviolet M-dwarf Evolution Survey, we have assessed the evolution of the FUV radiation, specifically eight prominent emission lines, including Lyα, of M-dwarf stars with stellar rotation period and age. We demonstrate tight power-law correlations between the spectroscopic FUV features, and measure the intrinsic scatter of the quiescent FUV emissions. The luminosity evolution with rotation of these spectroscopic features is well-described by a broken power law, saturated for fast rotators, and decays with increasing Rossby number, with a typical power-law slope of −2, although likely shallower for Lyα. Our regression fits enable FUV emission-line luminosity estimates relative to bolometric from known rotation periods to within ∼0.3 dex, across eight distinct UV emission lines, with possible trends in the fit parameters as a function of source layer in the stellar atmosphere. Our detailed analysis of the UV luminosity evolution with age further shows that habitable-zone planets orbiting lower-mass stars experience much greater high-energy radiative exposure relative the same planets orbiting more massive hosts. Around early- to mid-M dwarfs, these exoplanets, at field ages, accumulate up to 10–20× more EUV energy, relative to modern Earth. Moreover, the bulk of this UV exposure likely takes place within the first Gyr of the stellar lifetime.
FUMES. II. Lyα Reconstructions of Young, Active M Dwarfs
Authors: Youngblood Allison , Pineda J. Sebastian , France Kevin 
Published: April 2021

Abstract
The H i Lyα (1215.67 Å) emission line dominates the far-UV spectra of M dwarf stars, but strong absorption from neutral hydrogen in the interstellar medium makes observing Lyα challenging even for the closest stars. As part of the Far-Ultraviolet M-dwarf Evolution Survey, the Hubble Space Telescope has observed 10 early-to-mid M dwarfs with ages ranging from ∼24 Myr to several Gyr in order to evaluate how the incident UV radiation evolves through the lifetime of exoplanetary systems. We reconstruct the intrinsic Lyα profiles from STIS G140L and E140M spectra, and achieve reconstructed fluxes with 1σ uncertainties ranging from 5% to a factor of two for the low-resolution spectra (G140L) and 3%–20% for the high-resolution spectra (E140M). We observe broad, 500–1000 km s−1 wings of the Lyα line profile, and analyze how the line width depends on stellar properties. We find that stellar effective temperature and surface gravity are the dominant factors influencing the line width with little impact from the star’s magnetic activity level, and that the surface flux density of the Lyα wings may be used to estimate the chromospheric electron density. The Lyα reconstructions on the G140L spectra are the first attempted on λ/Δλ ∼ 1000 data. We find that the reconstruction precision is not correlated with the signal-to-noise ratio of the observation—rather, it depends on the intrinsic broadness of the stellar Lyα line. Young, low-gravity stars have the broadest lines and therefore provide more information at low spectral resolution to the fit to break degeneracies among model parameters.
One–Two Quench: A Double Minor Merger Scenario
Authors: Sanchez N. Nicole , Tremmel Michael , Werk Jessica K. , Pontzen Andrew , Christensen Charlotte , Quinn Thomas , Loebman Sarah , Cruz Akaxia 
Published: April 2021

Abstract
Using the N-body+Smoothed particle hydrodynamics code, ChaNGa, we identify two merger-driven processes—disk disruption and supermassive black hole (SMBH) feedback—which work together to quench L
* galaxies for over 7 Gyr. Specifically, we examine the cessation of star formation in a simulated Milky Way (MW) analog, driven by an interaction with two minor satellites. Both interactions occur within ∼100 Myr of each other, and the satellites both have masses 5–20 times smaller than that of their MW-like host galaxy. Using the genetic modification process of Roth et al., we generate a set of four zoom-in, MW-mass galaxies all of which exhibit unique star formation histories due to small changes to their assembly histories. In two of these four cases, the galaxy is quenched by z = 1. Because these are controlled modifications, we are able to isolate the effects of two closely spaced minor merger events, the relative timing of which determines whether the MW-mass main galaxy quenches. This one–two punch works to: (1) fuel the SMBH at its peak accretion rate and (2) disrupt the cold, gaseous disk of the host galaxy. The end result is that feedback from the SMBH thoroughly and abruptly ends the star formation of the galaxy by z ≈ 1. We search for and find a similar quenching event in Romulus25, a hydrodynamical (25 Mpc)3 volume simulation, demonstrating that the mechanism is common enough to occur even in a small sample of MW-mass quenched galaxies at z = 0.
Biased Tracer Reconstruction with Halo Mass Information
Authors: Liu Yu , Yu Yu , Li Baojiu 
Published: April 2021

Abstract
Plenty of crucial information about our universe is encoded in the cosmic large-scale structure (LSS). However, extractions of this information are usually hindered by the nonlinearities of the LSS, which can be largely alleviated by various techniques known as reconstruction. In realistic applications, the efficiencies of these methods are always degraded by many limiting factors, a quite important one being the shot noise induced by the finite number density of biased matter tracers (i.e., luminous galaxies or dark matter halos) in observations. In this work, we explore the gains of biased tracer reconstruction achieved from halo mass information, which can suppress the shot-noise component and dramatically improves the cross-correlation between tracer field and dark matter. To this end, we first closely study the clustering biases and the stochasticity properties of halo fields with various number densities under different weighting schemes, i.e., the uniform, mass, and optimal weightings. Then, we apply the biased tracer reconstruction method to these different weighted halo fields and investigate how linear bias and observational mass scatter affect the reconstruction performance. Our results demonstrate that halo masses are critical information for significantly improving the performance of biased tracer reconstruction, indicating great application potential for substantially promoting the precision of cosmological measurements (especially for baryon acoustic oscillations) in ambitious ongoing and future galaxy surveys.
Broadening Astronomy Education through Professional Development
Authors: Fies C. , Packham C. , Fuller L. , Drozdov D. , Schlegel E. , Bayless A. , Roming P. 
Published: April 2021

Abstract
We report on the processes and findings related to the iterative design of the San Antonio Teacher Training Astronomy Academy (SATTAA). In particular, we show how the initial iteration in 2018, limited to only future (or preservice) secondary school STEM teachers, broadened to include current (or in-service) secondary school teachers in 2019, and then added primary school pre- and in-service teachers in 2020. The participants of all three years are now part of a community of practice that continues to engage in astronomy education in varied ways.
3D Radiative Transfer Simulations of the Atmospheric Environment of the Carbon-rich AGB Star RU Vir
Authors: Rau Gioia 
Published: April 2021

Abstract
We report the preliminary near- and mid-infrared 3D radiative transfer simulations of the carbon-rich AGB star RU Vir using the 3D radiative transfer code RADMC-3D. We found that the inclusion of molecular and dust species reproduces the extended atmosphere of this star well. This study is the beginning of an in-progress effort toward a more systematic 3D radiative transfer modeling of RU Vir’s extended atmosphere, and other AGB stars. These efforts aim at constraining the stars’ stellar parameters, and as preparatory work for the first multi-wavelength imaging of carbon-rich AGB stars with the newest VLTI/MATISSE interferometric instrument.
Tafazzin Modulates Allergen-Induced Mast Cell Inflammatory Mediator Secretion
Authors: Maguire Aindriu R R , Crozier Robert W E , Hunter Katie D , Claypool Steven M , Fajardo Val A , LeBlanc Paul J , MacNeil Adam J 
Published: April 2021

Abstract
Allergic inflammatory diseases are a steadily growing health concern. Mast cells, a driving force behind allergic pathologies, modulate metabolic pathways to carry out various functions following IgE-FcεRI–mediated activation. Tafazzin (TAZ) is a cardiolipin transacylase that functions to remodel, and thereby mature, cardiolipin, which is important for efficient energy production through oxidative phosphorylation. In this study, we aimed to evaluate the contribution of TAZ in IgE-mediated mast cell activation. Fetal liver-derived mast cells (FLMCs) were differentiated from mice with a doxycycline (dox)-inducible TAZ short hairpin RNA (shRNA) cassette (TAZ shRNA+/+) and littermate wild-types (WTs). TAZ knockdown in FLMCs following dox treatment was confirmed by Western blotting (99.1% by day 5), whereas flow cytometry confirmed FLMC phenotype (c-kit+ FcεRI+) and retention of receptor expression post-dox. Five-day dox-treated WT and TAZ shRNA+/+ FLMCs were activated via allergen-bound IgE cross-linking of FcεRI under stem cell factor potentiation. With dox, and in response to allergen, TAZ shRNA+/+ FLMCs displayed a 25% reduction in oxygen consumption and a significant 31% reduction in mast cell degranulation compared with dox-treated WT FLMCs. Secretion of TNF, CCL1, and CCL2 were significantly reduced, with CCL9 also impaired. Notably, gene expression was not impaired for any inflammatory mediator measured. Functionally, this suggests that TAZ is a contributor to mast cell degranulation and inflammatory mediator secretion. Given unimpacted induced gene expression for mediators measured, we propose that TAZ reduction impairs mast cell exocytosis mechanisms. We thus identify a potential new contributor to immunometabolism that enhances our understanding of mast cell signaling metabolic pathway interactions during allergic inflammation.