bluuebunny/crossref_metadata_2025_split huggingface dataset:
#67 Treatment of Campylobacter upsaliensis and Helicobacter canis in twin brothers with XLA
Authors: Dubois Melanie M 
Published: June 2022

Abstract

Background
X-linked agammaglobulinemia (XLA) is a primary immunodeficiency associated with mutations in the B cell tyrosine kinase gene leading to failure in B cell maturation, resulting in antibody deficiency and increased susceptibility to infections. Patients with XLA are at risk of severe disease with infections with Campylobacter and closely related Helicobacter species and warrant treatment with close follow up given risk of recurrence.

Method
We present follow up of two 5-year-old fraternal twins with XLA who were diagnosed with C. upsaliensis and H. canis respectively via microbial cell-free DNA (mcfDNA) and underwent successful treatment with multi-drug antimicrobial therapy with 12 months of follow-up.

Results
Patient #1 was diagnosed with XLA at 11 months of age. At 3 years of age, he presented with fever and diarrhea, with stool cultures that grew C. jejuni. Despite treatment with azithromycin, his symptoms persisted and repeat stool cultures grew C. upsaliensis. Testing via mcfDNA confirmed C. upsaliensis. Patient #2 was diagnosed with XLA at 12 months of age. He developed fever, erythema nodosum (EN) like lesions and arthritis at 3.5 years old. Given his twin’s diagnosis of Campylobacter sp. enteritis, he was given a presumptive diagnosis of Campylobacter reactive arthritis and EN. Despite treatment with Naprosyn and 14 days of azithromycin, his symptoms persisted and stool PCR was positive for Campylobacter sp. mcfDNA testing confirmed C. upsaliensis and H.canis. Given failure of initial antimicrobial therapy, both boys were treated with a 4-week course of IV ertapenem, and oral ciprofloxacin and amoxicillin, and both developed neutropenia and concern for drug toxicity. Therapy was transitioned to triple drug therapy with oral doxycycline, ciprofloxacin and amoxicillin. Doxycycline was discontinued after 3 weeks due to patients’ young age. Ciprofloxacin and amoxicillin were continued for 12 months. Both boys had complete resolution of symptoms after 12 months of therapy and remain without recurrence 10 weeks after discontinuation of antimicrobial therapy.

Conclusion
Physicians should be aware of the treatment challenges of chronic Campylobacter and Helicobacter infection in boys with XLA and other immunocompromised hosts. Successful treatment may require prolonged multi-drug antimicrobial therapy, with monitoring for drug toxicities.
#72 STIGMA AND DEPRESSION AMONGST ADOLESCENTS LIVING WITH HIV/AIDS
Authors: Bhat Kamalakshi G 
Published: June 2022

Abstract

Background
The Highly Active Anti-Retroviral Therapy (HAART) has revolutionized the face of treatment of People Living With HIV/AIDS (PLWHA). Perinatally infected infants are living longer, reaching adolescent age group with deaths reduced by 54% but in long term there exists many drawbacks not only in terms of adherence, complications, drug resistance but also in terms of mental health. Adolescence is a critical period to promote mental health as major mental health disorders seem to start during this period. Adolescents with HIV/AIDS are more prone to a variety of mental health problems. The stress of being infected and living with the disease is higher. These adolescents face unique psychosocial challenges and most importantly, the stigma of being sufferers of this disease. Because of stigma, very few individuals seek psychiatric care and very few further follow up even when therapy has proven benefits.

Method
OBJECTIVES: To assess the following in adolescents living with HIV/AIDS: 1. The proportion of stigma. 2. The proportion of depression. 3. Correlation between depression and stigma. 4. Correlation between CD4 count, stage of disease and duration of illness with stigma and depression. STUDY DESIGN: Cross sectional study PARTICIPANTS: 83 adolescents on ART treatment for minimum 1 year duration and are free from any psychiatric condition. INTERVENTION: Questionnaires were administered for assessment of stigma using HIV Felt Stigma Scale (is a 4-point likert scale, consisting of 17 questions and scores are namely Strongly disagree-0, Disagree-1, Agree-2, Strongly agree-3. and Depression by Centre for Epidemiological Studies-Depression Scale (is 20 item scale). Calculating the overall CES-D – style symptom score, target score for referring to psychiatrist is more than or equal to 16.

Results
The proportion of participants who scored positive in the stigma scale was 92.8% and that of depression was noted to be 20.5%. Statistically significant correlation was observed between stigma and depression (0.020), between depression and CD4 count (0.024).

Conclusion
The study demonstrates that a rise in stigmatising attitudes is linked to a rise in depressive symptoms, implying the necessity for multilevel treatments in stigma reduction initiatives to prevent the mental health issues in this vulnerable population.
Epidemiology of Congenital Rubella Syndrome Related to the 2012–2013 Rubella Epidemic in Japan
Authors: Kanai Mizue , Kamiya Hajime , Okuno Hideo , Sunagawa Tomimasa , Tanaka-Taya Keiko , Matsui Tamano , Oishi Kazunori , Kitajima Hiroyuki , Takeda Makoto , Mori Yoshio 
Published: June 2022

Abstract
This study assessed the epidemiological characteristics of 45 congenital rubella syndrome cases in Japan following the 2012–2013 rubella epidemic. Rubella still poses significant health burdens and the uptake of rubella-containing vaccines among women of childbearing age should be improved.
Identification of new hot subdwarf binary systems by means of Virtual Observatory tools
Authors: Solano E , Ulla A , Pérez-Fernández E , Rodrigo C , Oreiro R , Aller A , Manteiga M , Santoveña-Gómez R , Álvarez M A , Dafonte C 
Published: June 2022

ABSTRACT
The estimation of the binary fraction of hot subdwarfs is key to shed light on the different evolution scenarios proposed to explain the loss of the hydrogen envelope during the red giant branch phase. In this paper, we analyse the spectral energy distribution of the hot subdwarfs included in a recent and comprehensive catalogue with the aim of identifying companions. Our methodology shows a performance superior to the photometric criteria used in that study, identifying 202 objects wrongly classified as binaries according to their spectral energy distributions, and finding 269 new binaries. Out of an initial sample of 3186 objects, we classified 2469 as single and 615 as binary hot subdwarfs. The rest of the objects (102) were not classified because of their inadequate spectral energy distribution fitting due, in turn, to poor quality photometry. Effective temperatures, luminosities, and radii were computed for 192 singles and 42 binaries. They, in particular the binary sample, constitute an excellent data set to further perform a more careful spectroscopic analysis that could provide detailed values for the chemical composition, masses, ages, rotation properties, or reflection effects for the shortest period systems. The results obtained in this paper will be used as a reference for a forthcoming work where we aim to generalize binary and single hot subdwarf classification using Artificial Intelligence-based techniques.
Wavelike nature of the vertical shear instability in global protoplanetary discs
Authors: Svanberg Eleonora , Cui Can , Latter Henrik N 
Published: June 2022

ABSTRACT
The vertical shear instability (VSI) is a robust phenomenon in irradiated protoplanetary discs (PPDs). The majority of previous numerical simulations have focused on the turbulent properties of its saturated state. However, the saturation of the VSI manifests as large-scale coherent radially travelling inertial waves. In this paper, we study inertial-wave-disc interactions and their impact on VSI saturation. Inertial-wave linear theory is developed and applied to a representative global 2D simulation using the athena++ code. It is found that the VSI saturates by separating the disc into several radial wave zones roughly demarcated by Lindblad resonances (turning points); this structure also manifests in a modest radial variation in the vertical turbulence strength. Future numerical work should employ large radial domains to accommodate this radial structure of the VSI, while concurrently adopting sufficiently fine resolutions to resolve the parametric instability that attacks the saturated VSI inertial waves.
First optical identification of the SRG/eROSITA-detected supernova remnant G 116.6 − 26.1. I. Preliminary results
Authors: Palaiologou E V , Leonidaki I , Kopsacheili M 
Published: June 2022

ABSTRACT
The supernova remnant (SNR) candidate G 116.6 − 26.1 is one of the few high Galactic latitude (|b| &gt; 15°) remnants detected so far in several wavebands. It was discovered recently in the SRG/eROSITA all-sky X-ray survey and also displays a low-frequency weak radio signature. In this study, we report the first optical detection of G 116.6 − 26.1 through deep, wide-field, and higher resolution narrowband imaging in H$\alpha$, $[\rm S\,{\small{\rm II}}]$ and $[\rm O\,{\small{\rm III}}]$ light. The object exhibits two major and distinct filamentary emission structures in a partial shell-like formation. The optical filaments are found in an excellent positional match with available X-ray, radio, and UV maps, can be traced over a relatively long angular distance (38 and 70 arcmin) and appear unaffected by any strong interactions with the ambient interstellar medium. We also present a flux-calibrated, optical emission spectrum from a single location, with Balmer and several forbidden lines detected, indicative of emission from shock excitation in a typical evolved SNR. Confirmation of the most likely SNR nature of G 116.6 − 26.1 is provided from the observed value of the line ratio [S ii] / H$\alpha$ = $0.56\, \pm \, 0.06$, which exceeds the widely accepted threshold 0.4, and is further strengthened by the positive outcome of several diagnostic tests for shock emission. Our results indicate an approximate shock velocity range 70–100 km s−1 at the spectroscopically examined filament, which, when combined with the low emissivity in H$\alpha$ and other emission lines, suggest that G 116.6 − 26.1 is a SNR at a mature evolutionary stage.
Modelling galaxy clustering in redshift space with a Lagrangian bias formalism and N-body simulations
Authors: Pellejero Ibañez Marcos , Stücker Jens , Angulo Raul E , Zennaro Matteo , Contreras Sergio , Aricò Giovanni 
Published: June 2022

ABSTRACT
Improving the theoretical description of galaxy clustering on small scales is an important challenge in cosmology, as it can considerably increase the scientific return of forthcoming galaxy surveys – e.g. tightening the bounds on neutrino masses and deviations from general relativity. In this paper, we propose and test a new model for the clustering of galaxies that is able to accurately describe redshift-space distortions even down to small scales. This model corresponds to a second-order perturbative Lagrangian bias expansion which is advected to Eulerian space employing a displacement field extracted from N-body simulations. Eulerian coordinates are then transformed into redshift space by directly employing simulated velocity fields augmented with nuisance parameters capturing various possible satellite fractions and intra-halo small-scale velocities. We quantify the accuracy of our approach against samples of physically motivated mock galaxies selected according to either stellar mass (SM) or star formation rate (SFR) at multiple abundances and at z = 0 and 1. We find our model describes the monopole, quadrupole, and hexadecapole of the galaxy-power spectra down to scales of k ≈ 0.6 [h Mpc−1] within the accuracy of our simulations. This approach could pave the way to significantly increase the amount of cosmological information to be extracted from future galaxy surveys.
A numerical study of the 1/2, 2/1, and 1/1 retrograde mean motion resonances in planetary systems
Authors: Caritá Gabriel Antonio , Cefali Signor Alan , Morais Maria Helena Moreira 
Published: June 2022

ABSTRACT
We present a numerical study on the stability of the 1/2, 2/1, and 1/1 retrograde mean motion resonances in the three-body problem composed of a solar mass star, a Jupiter mass planet, and an additional body with zero mass (elliptic restricted three-body problem) or masses corresponding to either Neptune, Saturn, or Jupiter (planetary three-body problem). For each system, we obtain stability maps using the n-body numerical integrator REBOUND and computing the chaos indicator mean exponential growth factor of nearby orbits (MEGNO). We show that families of periodic orbits exist in all configurations and they correspond to the libration of either a single resonant argument or all resonant arguments (fixed points). We compare the results obtained in the elliptic restricted three-body problem with previous results in the literature, and we show the differences and similarities between the phase space topology for these retrograde resonances in the circular restricted, elliptic restricted, and planetary three-body problems.
Estimating accurate reddening values of LAMOST M dwarfs
Authors: Shen H , Chen B-Q , Guo H-L , Yuan H-B , Sun W-X , Li J 
Published: June 2022

ABSTRACT
M dwarfs are the dominating type of stars in the solar neighbourhood. They serve as excellent tracers for the study of the distribution and properties of the nearby interstellar dust. In this work, we aim to obtain high accuracy reddening values of M dwarf stars from the Large Sky Area Multi-Object Fibre Spectroscopic Telescope (LAMOST) Data Release 8 (DR8). Combining the LAMOST spectra with the high-quality optical photometry from the Gaia Early Data Release 3 (EDR3), we have estimated the reddening values E(GBP − GRP) of 641 426 M dwarfs with the machine learning algorithm random forest regression. The typical reddening uncertainty is only 0.03 mag in E(GBP − GRP). We have obtained the reddening coefficient $R_{(G_{\rm BP}-G_{\rm RP})}$, which is a function of the stellar intrinsic colour (GBP − GRP)0 and reddening value E(B − V). The values of E(B − V) are also provided for the individual stars in our catalogue. Our resultant high accuracy reddening values of M dwarfs, combined with the Gaia parallaxes, will be very powerful to map the fine structures of the dust in the solar neighbourhood.
Multiwavelength study of blazar 4C  + 01.02 during its long-term flaring activity in 2014–2017
Authors: Malik Zahoor , Shah Zahir , Sahayanathan Sunder , Iqbal Naseer , Manzoor Aaqib 
Published: June 2022

ABSTRACT
We conducted a detailed long-term spectral and temporal study of flat spectrum radio quasar 4C  + 01.02, by using the multiwavelength observations from Fermi-LAT, Swift-XRT, and Swift-UVOT. The 2-d bin γ-ray light curve in the 2014–2017 active state displays 14 peak structures with a maximum integral flux $(\rm \mathit{ E} \gt 100 \ MeV)$ of $\rm (2.5 \pm 0.2) \times 10^{-6}\ ph\ cm^{-2}\ s^{-1}$ at MJD 57579.1, which is approximately 61 times higher than the base flux of $\rm (4.1 \pm 0.3) \times 10^{-8}\ ph\ cm^{-2}\ s^{-1}$, calculated by averaging the flux points when the source was in quiescent state. The shortest γ-ray variability of 0.66 ± 0.08 d is observed for the source. The correlation study between γ-ray spectral index and flux suggests that the source deviates from the usual trend of harder when brighter feature shown by blazars. To understand the likely physical scenario responsible for the flux variation, we performed a detailed broad-band spectral analysis of the source by selecting different flux states from the multiwavelength light curve. A single zone leptonic model was able to reproduce the broad-band spectral energy distribution (SED) of each state. The parameters of the model in each flux state are determined using a χ2 fit. We observed that the synchrotron, synchrotron-self-Compton (SSC), and External-Compton (EC) processes produce the broad-band SED under varied flux states. The adjoining contribution of the seed photons from the broad-line region (BLR) and the IR torus for the EC process are required to provide adequate fits to the GeV spectrum in all the chosen states.
Massive central galaxies of galaxy groups in the Romulus simulations: an overview of galaxy properties at z = 0
Authors: Jung S Lyla , Rennehan Douglas , Saeedzadeh Vida , Babul Arif , Tremmel Michael , Quinn Thomas R , Loubser S Ilani , O’Sullivan E , Yi Sukyoung K 
Published: June 2022

ABSTRACT
Contrary to many stereotypes about massive galaxies, observed brightest group galaxies (BGGs) are diverse in their star formation rates, kinematic properties, and morphologies. Studying how they evolve into and express such diverse characteristics is an important piece of the galaxy formation puzzle. We use a high-resolution cosmological suite of simulations Romulus and compare simulated central galaxies in group-scale haloes at z = 0 to observed BGGs. The comparison encompasses the stellar mass–halo mass relation, various kinematic properties and scaling relations, morphologies, and the star formation rates. Generally, we find that Romulus reproduces the full spectrum of diversity in the properties of the BGGs very well, albeit with a tendency toward lower than the observed fraction of quenched BGGs. We find both early-type S0 and elliptical galaxies as well as late-type disc galaxies; we find Romulus galaxies that are fast-rotators as well as slow-rotators; and we observe galaxies transforming from late-type to early-type following strong dynamical interactions with satellites. We also carry out case studies of selected Romulus galaxies to explore the link between their properties, and the recent evolution of the stellar system as well as the surrounding intragroup/circumgalactic medium. In general, mergers/strong interactions quench star-forming activity and disrupt the stellar disc structure. Sometimes, however, such interactions can also trigger star formation and galaxy rejuvenation. Black hole feedback can also lead to a decline of the star formation rate but by itself, it does not typically lead to complete quenching of the star formation activity in the BGGs.
Radiative shock oscillation model for the long-term flares of Sgr A*
Authors: Okuda Toru , Singh Chandra B , Aktar Ramiz 
Published: June 2022

ABSTRACT
We examine time-dependent 2D relativistic radiation magnetohydrodynamic (MHD) flows to develop the shock oscillation model for the long-term flares of Sagittarius A* (Sgr A*). Adopting modified flow parameters in addition to the previous studies, we confirm quasi-periodic flares with periods of ∼5 and 10 d that are compatible with observations by Chandra, Swift, and XMM–Newton monitoring of Sgr A*. Using a simplified two-temperature model of ions and electrons, we find that the flare due to synchrotron emission lags that of bremsstrahlung emission by 1–2 h that are qualitatively comparable to the time lags of 1–5 h reported in several simultaneous observations of radio and X-ray variability in Sgr A*. The synchrotron emission is confined in a core region of 3Rg size with the strong magnetic field, while the bremsstrahlung emission mainly originates in a distant region of 10–20Rg behind the oscillating shock, where Rg is the Schwarzschild radius. The time lag is estimated as the transit time of the acoustic wave between the above two regions. The time-averaged distribution of radiation shows a strong anisotropic nature along the rotational axis but isotropic distribution in the radial direction. A high-velocity jet with ∼0.6c along the rotational axis is intermittently found in a narrow funnel region with a collimation angle ∼15°. The shock oscillating model explains well the flaring rate and the time lag between radio and X-ray emissions for the long-term flares of Sgr A*.
Stellar migration in the Auriga simulations
Authors: Okalidis Periklis , Grand Robert J J , Yates Robert M , Springel Volker 
Published: June 2022

ABSTRACT
We study the presence and importance of stellar migration in the evolution of 17 Milky-Way like disc galaxies with stellar mass 10 &lt; log(M*/M⊙) &lt; 11 from the Auriga suite of zoom-in cosmological hydrodynamical simulations. We compare the birth radii of the stars to their radii at z = 0 for each system and present mean values of the strength of stellar migration as a function of radius and stellar age which vary between 1–4 kpc. We also investigate the effect of migration on age and metallicity radial profiles in the discs. We find several cases of age gradient flattening due to migration, but significant changes to metallicity profiles only for older stellar populations and discs that develop a strong bar. Furthermore, we study stellar migration from the perspective of the change of the galactocentric radius (ΔR) and orbital guiding centre radius (ΔRg) of stellar particles between given time intervals. We find that stars migrate approximately as a diffusion process only in the outer parts of the discs and for particular galaxies that have a weak bar. Strongly barred galaxies in our sample show larger stellar migration but its timestep evolution is slower-than-diffusion. Finally, we give parametrizations that encapsulate the dependence of the strength of the radial migration as a function of time and radius, for incorporation into (semi-)analytic models of galaxy evolution.
Specific Zn(II)-binding site in the C-terminus of Aspf2, a zincophore from Aspergillus fumigatus
Authors: Garstka Kinga , Hecel Aleksandra , Kozłowski Henryk , Rowińska-Żyrek Magdalena 
Published: June 2022

Abstract
Aspergillus fumigatus, one of the most widespread opportunistic human fungal pathogens, adapts to zinc limitation by secreting a 310 amino acid Aspf2 zincophore, able to specifically bind Zn(II) and deliver it to a transmembrane zinc transporter, ZrfC. In this work, we focus on the thermodynamics of Zn(II) complexes with unstructured regions of Aspf2; basing on a variety of spectrometric and potentiometric data, we show that the C-terminal part has the highest Zn(II)-binding affinity among the potential binding sites, and Ni(II) does not compete with Zn(II) binding to this region. The 14 amino acid Aspf2 C-terminus coordinates Zn(II) via two Cys thiolates and two His imidazoles and it could be considered as a promising A. fumigatus targeting molecule.
REVERSE: a user-friendly web server for analyzing next-generation sequencing data from in vitro selection/evolution experiments
Authors: Weiss Zoe , DasGupta Saurja 
Published: June 2022

Abstract
Next-generation sequencing (NGS) enables the identification of functional nucleic acid sequences from in vitro selection/evolution experiments and illuminates the evolutionary process at single-nucleotide resolution. However, analyzing the vast output from NGS can be daunting, especially with limited programming skills. We developed REVERSE (Rapid EValuation of Experimental RNA Selection/Evolution) (https://www.reverseserver.org/), a web server that implements an integrated computational pipeline through a graphical user interface, which performs both pre-processing and detailed sequence level analyses within minutes. Raw FASTQ files are quality-filtered, dereplicated, and trimmed before being analyzed by either of two pipelines. The first pipeline counts, sorts, and tracks enrichment of unique sequences and user-defined sequence motifs. It also identifies mutational intermediates present in the sequence data that connect two input sequences. The second pipeline sorts similar sequences into clusters and tracks enrichment of peak sequences. It also performs nucleotide conservation analysis on the cluster of choice and generates a consensus sequence. Both pipelines generate downloadable spreadsheets and high-resolution figures. Collectively, REVERSE is a one-stop solution for the rapid analysis of NGS data obtained from in vitro selection/evolution experiments that obviates the need for computational expertise.