bluuebunny/crossref_metadata_2025_split huggingface dataset:
A MUSE view of the core of the giant low-surface-brightness galaxy Malin 1
Authors: Johnston Evelyn J. , Galaz Gaspar , Blaña Matias , Amram Philippe , Boissier Samuel , Eigenthaler Paul , Epinat Benoît , Junais  , Ordenes-Briceño Yasna , Puzia Thomas , Weilbacher Peter M. 
Published: April 2024

Aims. The central region of the giant low-surface-brightness galaxy Malin 1 has long been known to have a complex morphology, with evidence of a bulge, disc, and potentially a bar hosting asymmetric star formation. In this work, we use VLT/MUSE data to resolve the central region of Malin 1 in order to determine its structure.
Methods. We used careful light profile fitting in every image slice of the datacube to create wavelength-dependent models of each morphological component, from which we were able to cleanly extract their spectra. We then used the kinematics and emission line properties from these spectra to better understand the nature of each component extracted from our model fitting.
Results. We report the detection of a pair of distinct sources at the centre of this galaxy with a separation of ∼1.05″, which corresponds to a separation on sky of ∼1.9 kpc. The radial velocity data of each object confirm that they both lie in the kinematic core of the galaxy. An analysis of the emission lines reveals that the central compact source is more consistent with being ionised through star formation and/or a LINER, while the off-centre compact source lies closer to the separation between star-forming galaxies and active galactic nuclei.
Conclusions. This evidence suggests that the centre of Malin 1 hosts either a bar with asymmetric star formation or two distinct components. In the latter scenario, we propose two hypotheses for the nature of the off-centre compact source-it could either be a star-forming clump, containing one or more star clusters, that is in the process of falling into the core of the galaxy and eventually merging with the central nuclear star cluster, or it could be a clump of gas falling into the centre of the galaxy from either outside or from the disc and triggering star formation there.
Comparing the three-dimensional morphological asymmetries in the ejecta of Kepler and Tycho in X-rays
Authors: Picquenot A. , Holland-Ashford T. , Williams B. J. 
Published: April 2024

Aims. Recent simulations have shown that asymmetries in the ejecta distribution of supernova remnants (SNRs) may be a reflection of asymmetries left over from the initial supernova explosion. Thus, SNR studies provide a vital means for testing and constraining model predictions in relation to the distribution of heavy elements, which are key to improving our understanding of the explosion mechanisms in Type Ia supernovae.
Methods. The use of a novel blind source separation method applied to the megasecond X-ray observations of the historic Kepler and Tycho supernova remnants has revealed maps of the ejecta distribution. These maps are endowed with an unprecedented level of detail and clear separations from the continuum emission. Our method also provides a three-dimensional (3D) view of the ejecta by individually disentangling red- and blueshifted spectral components associated with images of the Si, S, Ar, Ca, and Fe emission. This approach provides insights into the morphology of the ejecta distribution in those two remnants.
Results. Those mappings have allowed us to thoroughly investigate the asymmetries in the intermediate-mass elements and Fe distribution in two Type Ia supernova remnants. We also compared the results with the core-collapse Cassiopeia A remnant, which we had studied previously. The images obtained confirm, as expected for Type Ia SNRs, that the Fe distribution is mostly closer to the core than that of intermediate-mass elements. They also highlight peculiar features in the ejecta distribution, such as the Fe-rich southeastern knot in Tycho.
Abundances in eight bulge stars from the optical and near-infrared
Authors: da Silva Patrícia , Barbuy B. , Ernandes H. , Souza S. O. , Fernández-Trincado J. G. , González-Díaz D. 
Published: April 2024

Context. The abundances of the α-elements are key for understanding the early chemical enrichment of the Galactic bulge. The elements of interest present lines in different wavelength regions, and some of them show lines only in part of the spectra. In the present work, the CNO trio, the a-elements Mg, Si, Ca, and Ti, and odd-Z Na and Al are examined as measured from optical and H-band lines.
Aims. The aim of this work is to carry out a detailed comparison of stellar parameters and abundances derived in the optical and near-infrared (H-band). We also inspect the best available lines for a list of bulge stars previously analyzed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) team in the H-band and by our group in the optical. This work is mainly of interest to spectroscopists.
Methods. In the present work, we compared the stellar parameters and abundance results derived from APOGEE H-band spectra with optical analyses based on Ultraviolet and Visual Echelle Spectrograph at the Very Large Telescope (VLT/UVES) data for eight bulge stars.
Results. We point out the most suitable wavelength region for each of the studied elements, and highlight difficulties in the derivation of stellar parameters both in the optical and H-band. The near-infrared will allow observations of a large number of stars in the near future given new instruments soon to be available. The identification of spectral lines in this spectral region and the investigation of their reliability are ongoing efforts worldwide. New instruments will also allow simultaneous observation of H-band and optical.
The formation of the magnetic symbiotic star FN Sgr
Authors: Belloni Diogo , Mikołajewska Joanna , Schreiber Matthias R. 
Published: April 2024

Context. There are several symbiotic stars (e.g., BF Cyg, Z And, and FN Sgr) in which periodic signals of tens of minutes have been detected. These periods have been interpreted as the spin period of magnetic white dwarfs that accrete through a magnetic stream originating from a truncated accretion disc.
Aims. To shed light on the origin of magnetic symbiotic stars, we investigated the system FN Sgr in detail. We searched for a reasonable formation pathway to explain its stellar and binary parameters including the magnetic field of the accreting white dwarf.
Methods. We used the MESA code to carry out pre-CE and post-CE binary evolution and determined the outcome of CE evolution assuming the energy formalism. For the origin and evolution of the white dwarf magnetic field, we adopted the crystallization scenario.
Results. We found that FN Sgr can be explained as follows. First, a non-magnetic white dwarf is formed through CE evolution. Later, during post-CE evolution, the white dwarf starts to crystallize and a weak magnetic field is generated. After a few hundred million years, the magnetic field penetrates the white dwarf surface and becomes detectable. Meanwhile, its companion evolves and becomes an evolved red giant. Subsequently, the white dwarf accretes part of the angular momentum from the red giant stellar winds. As a result, the white dwarf spin period decreases and its magnetic field reaches super-equipartition, getting amplified due to a rotation- and crystallization-driven dynamo. The binary then evolves into a symbiotic star, with a magnetic white dwarf accreting from an evolved red giant through atmospheric Roche-lobe overflow.
Conclusions. We conclude that the rotation- and crystallization-driven dynamo scenario, or any age-dependent scenario, can explain the origin of magnetic symbiotic stars reasonably well. This adds another piece to the pile of evidence supporting this scenario. If our formation channel is correct, our findings suggest that white dwarfs in most symbiotic stars formed through CE evolution might be magnetic, provided that the red giant has spent ≳3 Gyr as a main-sequence star.
Hypertonietherapie bei Nierenerkrankungen
Authors: Boger Leonard , Saritas Turgay 
Published: April 2024

ZUSAMMENFASSUNGDie arterielle Hypertonie bei Patienten mit einer chronischen Nierenerkrankung (CKD: „chronic kidney disease“) ist häufig schlecht kontrolliert und der wichtigste modifizierbare Risikofaktor, der zur Progression der CKD beiträgt. Dieser Beitrag gibt einen Überblick über die aktuelle Diagnostik und Therapie der arteriellen Hypertonie in den verschiedenen CKD-Stadien, inklusive für Patienten mit Nierenersatztherapie und für Patienten nach einer Nierentransplantation. Die Diagnose und die Therapieüberwachung der Blutdruckwerte sollte bei allen CKD-Stadien ohne Nierenersatztherapie und bei Nierentransplantation primär mittels ambulanter Blutdruckmessung (ABDM) erfolgen. Bei allen CKD-Patienten empfiehlt die europäische Hypertonie-Leitlinie aus dem Jahr 2023 einen Zielblutdruck von < 140/90 mmHg (Praxisblutdruck) anzustreben. Insbesondere bei jüngeren Patienten mit Albuminurie und/oder Diabetes erscheint ein Blutdruckziel von < 130/80 mmHg vorteilhaft. In den CKD-Stadien 1–3 werden in erster Linie ACE-Inhibitoren (ACE: „angiotensin converting enzyme“) beziehungsweise Angiotensin-II-Rezeptor-Blocker (ACEi/ARB), Dihydropyridin-Kalzium-Antagonisten (CCB: „calcium channel blocker“) und Thiaziddiuretika eingesetzt. Als Reservemedikament ist Spironolacton zu bevorzugen. Die renale Denervation rückt als zusätzliche antihypertensive Option zunehmend in den Vordergrund. Die Gabe und das Erreichen der Maximaldosis von ACEi/ARB und MRA kann in fortgeschrittenen CKD-Stadien durch kaliumsenkende Ionenaustauscher ermöglicht werden. Bei hochgradig reduzierter Nierenfunktion (CKD-Stadien 4 und 5 ohne Nierensatztherapie) ist statt einem Thiaziddiuretikum der Einsatz eines Schleifendiuretikums ratsam. Bei Patienten mit Nierenersatztherapie sind Grundpfeiler der Therapie das Erreichen des Trockengewichts, eine effektive Dialysedosis und eine Kochsalzrestriktion. Medikamentös sind, im Gegensatz zu anderen CKD-Subgruppen, Betablocker und Kalziumantagonisten bevorzugte Medikamente. Patienten nach einer Nierentransplantation haben aufgrund vaskulärer Vorerkrankungen und unter Glukokortikoiden und Calcineurininhibitoren häufig einen schlecht kontrollierten Blutdruck. Kalziumantagonisten sind als Erstlinientherapie bei Hypertonie nach einer Nierentransplantation in Bezug auf die Blutdrucksenkung und das Transplantatüberleben wirksam.
American Society for Gastrointestinal Endoscopy–European Society of Gastrointestinal Endoscopy guideline on primary endoscopic bariatric and metabolic therapies for adults with obesity
Authors: Jirapinyo Pichamol , Hadefi Alia , Huberty Vincent , Sullivan Shelby , Thompson Christopher C. , Patai Árpád V. , Pannala Rahul , Goelder Stefan K. , Kushnir Vladimir , Barthet Marc , Apovian Caroline M. , Boskoski Ivo , Chapman Christopher G. , Davidson Paul , Donatelli Gianfranco , Kumbhari Vivek , Hayee Bu , Esker Janelle , Hucl Tomas , Pryor Aurora D. , Maselli Roberta , Schulman Allison R. , Pattou Francois , Zelber-Sagi Shira , Bain Paul A. , Durieux Valérie , Triantafyllou Konstantinos , Thosani Nirav 
Published: April 2024

AbstractThis joint ASGE-ESGE guideline provides an evidence-based summary and recommendations regarding the role of endoscopic bariatric and metabolic therapies (EBMTs) in the management of obesity. The document was developed using the Grading of Recommendations, Assessment, Development and Evaluation (GRADE) framework. It evaluates the efficacy and safety of EBMT devices and procedures that currently have CE mark or FDA-clearance/approval, or that had been approved within five years of document development. The guideline suggests the use of EBMTs plus lifestyle modification in patients with a BMI of ≥30 kg/m2, or with a BMI of 27.0–29.9 kg/m2 with at least 1 obesity-related comorbidity. Furthermore, it suggests the utilization of intragastric balloons and devices for endoscopic gastric remodeling (EGR) in conjunction with lifestyle modification for this patient population.
Temporal Analysis in Outcomes of Long-Term Mechanical Circulatory Support: Retrospective Study
Authors: Ondrusek Matej , Artemiou Panagiotis , Bezak Branislav , Gasparovic Ivo , By Theo MMH de , Durdik Stefan , Lesny Peter , Goncalvesova Eva , Hulman Michal 
Published: April 2024

Abstract
Background Mechanical assist device indications have changed in recent years. Reduced incidence of complications, better survival, and the third generation of mechanical support devices contributed to this change. In this single-center study, we focused on two time periods that are characterized by the use of different types of mechanical support devices, different patient characteristics, and change in the indications.
Methods The data were processed from the European Registry for Patients with Mechanical Circulatory Support (EUROMACS). We retrospectively defined two time intervals to reflect changes in ventricular assist device technology (period 1: 2007–2015; period 2: 2016–20222). A total of 181 patients underwent left ventricular assist device implantation. Device utilization was the following: HeartMate II = 52 (76.4%) and HeartWare = 16 (23.6%) in period 1 and HeartMate II = 2 (1.8%), HeartMate 3 = 70 (61:9%), HeartWare = 29 (25.7%), SynCardia TAH = 10 (8.8%), and BerlinHeart EXCOR = 2 (1.8%) in period 2. The outcomes of the time intervals were analyzed and evaluated.
Results Survival was significantly higher during the second time period. Multivariate analysis revealed that age and bypass pump time are independent predictors of mortality. Idiopathic cardiomyopathy, bypass time, and the Interagency Registry for Mechanically Assisted Circulatory Support (INTERMACS) score are independent predictors of adverse events. Furthermore, the first period was noted to be at an increased risk of the following adverse events: pump thrombosis, gastrointestinal bleeding, and bleeding events.
Conclusion Despite the higher risk profile of the patients and persistent challenges, during the second period, there was a significant decrease in mortality and morbidity. The use of the HeartMate 3 device may have contributed to this result.
Attacking epistemic personhood on Twitter/X
Authors: Padilla Cruz Manuel 
Published: April 2024

Abstract
This paper reports on an examination of the actions that Spanish epistemic agents perform in order to question,
challenge, undermine and/or destroy the epistemic personhood of an informer on Twitter, recently been renamed ‘X’. Relying on a
corpus of reactions to information about sanitary measures released during the COVID-19 pandemic by an allegedly reliable and
trustworthy information source, namely the Spanish Ministry of Health, the analysis looks into the said actions and how these are
arranged in larger digital discourse sequences. While contributing to extant research on conflict talk in Spanish on social
networks, the paper also aims to raise vulnerable epistemic agents’ awareness of the varied forms and dynamics of threats to
epistemic personhood as a way of empowering them to identify and counteract such threats.
Neural network time-series classifiers for gravitational-wave searches in single-detector periods
Authors: Trovato A , Chassande-Mottin E , Bejger M , Flamary R , Courty N 
Published: April 2024

Abstract
The search for gravitational-wave (GW) signals is limited by non-Gaussian transient noises that mimic astrophysical signals. Temporal coincidence between two or more detectors is used to mitigate contamination by these instrumental glitches. However, when a single detector is in operation, coincidence is impossible, and other strategies have to be used. We explore the possibility of using neural network classifiers and present the results obtained with three types of architectures: convolutional neural network, temporal convolutional network, and inception time. The last two architectures are specifically designed to process time-series data. The classifiers are trained on a month of data from the LIGO Livingston detector during the first observing run (O1) to identify data segments that include the signature of a binary black hole merger. Their performances are assessed and compared. We then apply trained classifiers to the remaining three months of O1 data, focusing specifically on single-detector times. The most promising candidate from our search is 4 January 2016 12:24:17 UTC. Although we are not able to constrain the significance of this event to the level conventionally followed in GW searches, we show that the signal is compatible with the merger of two black holes with masses

m
1

=

50.7

−
8.9

+
10.4

M

⊙

and

m
2

=

24.4

−
9.3

+
20.2

M

⊙

at the luminosity distance of

d

L

=

564

−
338

+
812

Mpc

.
Simulating electromagnetic cascades with Lorentz invariance violation
Authors: Saveliev Andrey , Alves Batista Rafael 
Published: April 2024

Abstract
Lorentz invariance violation (LIV) is a phenomenon featuring in various quantum gravity models whereby Lorentz symmetry is broken at high energies, potentially impacting the behaviour of particles and their interactions. Here we investigate the phenomenology of LIV within the context of gamma-ray–induced electromagnetic cascades. We conduct detailed numerical simulations to explore the expected manifestations of LIV on gamma-ray fluxes, taking into account relevant effects such as pair production and inverse Compton scattering. Additionally, we consider processes forbidden in the standard model, namely vacuum Cherenkov emission and photon decay. Our analysis reveals that these modifications result in distinct characteristics within the measured particle fluxes at Earth, which have the potential to be observed in high-energy gamma-ray observations.
Gravitational wave peeps from EMRIs and their implication for LISA signal confusion noise
Authors: Oliver Daniel J , Johnson Aaron D , Berrier Joel , Glampedakis Kostas , Kennefick Daniel 
Published: April 2024

Abstract
Scattering events around the center of massive galaxies will occasionally toss a stellar-mass compact object into an orbit around the massive black hole (MBH) at the center, beginning an extreme mass ratio inspiral (EMRI). The early stages of such a highly eccentric orbit are not likely to produce detectable gravitational waves (GWs), as the source will only be in a suitable frequency band briefly when it is close to periapsis during each long-period orbit. This repeated burst of emission, firmly in the millihertz band, is the GW peep. While a single peep is not likely to be detectable, if we consider an ensemble of such subthreshold sources, spread across the Universe, together they may produce an unresolvable background noise that could obscure sources otherwise detectable by the Laser Interferometer Space Antenna. Previous studies of the extreme mass ratio signal confusion background focused either on parabolic orbits near the MBH or events closer to merger. We seek to improve this characterization by implementing numerical kludge waveforms that can calculate highly eccentric orbits with relativistic effects. Our focus is on orbits at the point of capture that are farther away from the MBH. Here we present the waveforms and spectra of peeps generated from recent calculations of EMRIs/extreme mass ratio bursts capture parameters and discuss how these can be used to estimate the signal confusion noise generated by such events. We demonstrate the effects of changing the orbital parameters on the resulting spectra as well as showing direct comparisons to parabolic orbits and why the GW ‘peep’ needs to be studied further. The results of this study will be expanded upon in a further paper that aims to provide an update on the EMRI signal confusion noise problem.
Semi-analytical calculation of the force between two magnets with rhombus-shaped cross-sections
Authors: Li Tianjian , Ding Chenyang , Yang Xiaofeng 
Published: April 2024

Abstract
Analytical calculations of interaction forces between permanent magnets are essential for the fast and accurate modeling of magnetic springs and bearings. Whereas extensive research has been conducted on interaction forces between cuboidal magnets, there is a lack of research on force calculations between other prismatic magnets in existing literature. This paper newly develops a semi-analytical method for force calculation between two magnets with rhombus-shaped cross-sections. The method is based on interaction force between two rectangular magnetically charged surfaces which are inclined toward each other. Under a Cartesian coordinate system, two components of the force between inclined rectangular magnetically charged surfaces are presented with fully analytical expressions, whereas the other component is expressed with one numerical integral. By applying these expressions repeatedly, the force between two magnets with rhombus-shaped cross-sections is derived. Moreover, a test rig is constructed to validate this semi-analytical method. Furthermore, the method can be extended to force calculations between prismatic magnets with arbitrary-shaped cross-sections, which allows a simple and fast modeling of many magnetic applications.
Nanosecond repetitively pulsed plasmas with MHz bursts for CO2 dissociation
Authors: Post Antoine , Budde Maik , Vervloedt S C L , Engeln Richard , Huiskamp Tom 
Published: April 2024

Abstract
A novel pulsed power source capable of nanosecond pulses with burst frequencies up to 1 MHz is employed to create atmospheric pressure pulsed plasma in pure CO2 gas. The short bursts contain up to four nanosecond pulses. The CO2 conversion and corresponding energy efficiency are measured ex-situ with Fourier-transform infrared absorption spectroscopy. Trends in the absorption line profile of in-situ quantum cascade laser infrared absorption spectroscopy indicate an elevated vibrational temperature of CO2 with an increasing number of pulses per burst. The key result of this paper is that the dissociation energy efficiency is higher when operating the plasma in burst mode. Furthermore, a larger number of pulses in a burst is associated with a further increase of the dissociation efficiency. The highest efficiency measured is

(
17.7
±
0.3
)

% for single pulses spaced 2 ms apart, and

(
20.0
±
0.3
)

% for bursts of three pulses, with an in-burst frequency of 1 MHz and bursts spaced 4 ms apart.