bluuebunny/crossref_metadata_2025_split huggingface dataset:
Exploring Music Therapists’ Experiences With and Perceptions About Copyrighted Music: A Thematic Analysis
Authors: Reid Amanda , Nicolla Sydney K 
Published: August 2022

Abstract
Patient-preferred music is often copyrighted music; prior research, however, has paid scant attention to music therapists’ understanding and use of copyrighted music. To fill a gap in the literature, this exploratory study sought to understand music therapists’ experiences and perceptions about permissible therapeutic uses of copyrighted music. Semi-structured interviews were conducted with 18 board-certified music therapists working in the United States. Collectively, these participants had over 300 years of professional experience. The interview transcripts were analyzed using an inductive approach to thematic analysis. Five main themes were identified: (1) copyright concerns created a complex psychological burden; (2) therapeutic needs warranted use of copyrighted music; (3) perceptions varied on permissible therapeutic practices using copyrighted music; (4) varied sources informed an understanding of copyright law; and (5) copyright clarity was needed to reduce the psychological burden. These themes suggest that psychological stress was produced by copyright uncertainty coupled with attempts by participants to satisfy diverse interests and protect multiple stakeholders, including patients, employers, their profession, and the law. Our findings suggest that a lack of clarity about permissible uses of copyrighted music can complicate music therapists’ decision-making about appropriate therapeutic interventions. Clarity on permissible therapeutic uses of music could yield benefits for music therapists, patients, and the community.
Epicyclic frequencies of spheroidal stars with non-uniform density
Authors: Bollimpalli D A 
Published: August 2022

ABSTRACT
We consider the gravitational potential of a rotating star with non-uniform density to derive the orbital and epicyclic frequencies of the particles orbiting the star. We assume that the star is composed of concentric spheroids of constant density, with a global power-law distribution of density inside the star. At the lowest order approximation, we recover the known result for the Maclaurin spheroid that the maximum in the radial epicyclic frequency occurs at $r=\sqrt{2}ae$, for eccentricities ${\ge} 1/\sqrt{2}$. We find that the nature of these characteristic frequencies differs based on the geometry of the rotating star. For an oblate spheroid, the orbits resemble retrograde Kerr orbits and the location of the radial epicyclic maximum approaches the stellar surface as the density variation inside the star becomes steeper. On the contrary, orbits around a prolate spheroid resemble prograde Kerr orbits, but the marginally stable orbit does not exist for prolate-shaped stars. The orbital frequency is larger (smaller) than the Keplerian value for an oblate (prolate) star with the equality attained as e → 0 or r → ∞. The radial profiles of the angular velocity and the angular momentum allow for a stable accreting disc around any nature of oblate/prolate spheroid.
New highly precise weak gravitational lensing flexions measurement method based on ERA method
Authors: Okura Yuki , Futamase Toshifumi 
Published: August 2022

ABSTRACT
Weak gravitational lensing flexions are a kind of weak lensing distortion that are defined as the spin 1 and spin 3 combinations of the third order derivatives of gravitational lensing potential. Since the shear has spin 2 combination of the second-order derivative, the flexion signal gives partly independent information from shear signal and is more sensitive to the local mass distribution than shear signal. Thus its measurement is expected to play important roles in observational cosmology. However, since the weakness of the flexion signal, as well as the complicatedness of its intrinsic noise, made its accurate observation very difficult. We propose a new method of measuring the flexion signal using ERA method which is a method to measure weak lensing shear without any approximation. We find two particular combinations of the flexions which provide the quantities with only lensing information and free of intrinsic noise when taken average. It is confirmed by simple numerical simulation that the statistical average of these combinations do not in fact depend on the strength of the intrinsic distortion. Then, we introduce a method which measures flexions with PSF correction. This method is developed by applying the ERA method for flexion distortions and we call this method the FIRE method. It uses the expansion technique with an assumption of weak flexion, and we show by using typical examples of 1st and 2nd flexion images that the estimated errors become less than 1 per cent in most cases with the lowest order of the expansion. Finally, we apply the method for real data to measure flexion components in real galaxy images.
BFS 10: a nascent bipolar H ii region in a filamentary molecular cloud
Authors: Larose Nicholas , Kerton C R 
Published: August 2022

ABSTRACT
We present a study of the compact blister H ii region BFS 10 and its highly filamentary molecular cloud. We utilize 12CO observations from the Five College Radio Astronomy Observatory to determine the distance, size, mass, and velocity structure of the molecular cloud. Infrared observations obtained from the UKIRT Infrared Deep Sky Survey and the Spitzer Infrared Array Camera, as well as radio continuum observations from the Canadian Galactic Plane Survey, are used to extract information about the central H ii region. This includes properties such as the ionizing photon rate and infrared luminosity, as well as identifying a rich embedded star cluster associated with the central O9 V star. Time-scales regarding the expansion rate of the H ii region and lifetime of the ionizing star reveal a high likelihood that BFS 10 will develop into a bipolar H ii region. Although the region is expected to become bipolar, we conclude from the cloud’s velocity structure that there is no evidence to support the idea that star formation at the location of BFS 10 was triggered by two colliding clouds. A search for embedded young stellar objects (YSOs) within the molecular cloud was performed. Two distinct regions of YSOs were identified: one region associated with the rich embedded cluster and another sparse group associated with an intermediate-mass YSO.
A Giant Arc on the Sky
Authors: Lopez Alexia M , Clowes Roger G , Williger Gerard M 
Published: August 2022

ABSTRACTWe present the serendipitous discovery of a ‘Giant Arc on the Sky’ at $z$ ∼ 0.8. The Giant Arc (GA) spans ∼1 Gpc (proper size, present epoch) and appears to be almost symmetrical on the sky. It was discovered via intervening Mg ii absorbers in the spectra of background quasars, using the catalogues of Zhu & Ménard. The use of Mg ii absorbers represents a new approach to the investigation of large-scale structures (LSSs) at redshifts $0.45 \la z \la 2.25$. We present the observational properties of the GA, and we assess it statistically using methods based on (i) single-linkage hierarchical clustering (∼4.5σ); (ii) the Cuzick-Edwards test (∼3.0σ); and (iii) power-spectrum analysis (∼4.8σ). Each of these methods has distinctive attributes and powers, and we advise considering the evidence from the ensemble. We discuss our approaches to mitigating any post hoc aspects of analysing significance after discovery. The overdensity of the GA is δρ/ρ ∼ 1.3 ± 0.3. The GA is the newest and one of the largest of a steadily accumulating set of very large LSSs that may (cautiously) challenge the Cosmological Principle, upon which the ‘standard model’ of cosmology is founded. Conceivably, the GA is the precursor of a structure like the Sloan Great Wall (but the GA is about twice the size), seen when the Universe was about half its present age.
Laser Guide Star uplink beam: scattering and Raman emission measurements with the 10.4m Gran Telescopio CANARIAS
Authors: Lombardi G , Bonaccini Calia D , Centrone M , de Ugarte Postigo A , Geier S 
Published: August 2022

ABSTRACT
Laser Guide Star Adaptive Optics (LGS-AO) is becoming routine in several astronomical observatories. The use of powerful lasers generates sensible Raman emissions on the uplink laser beam path, plus secondary Rayleigh scattering from atmospheric molecules and Mie scattering from aerosols. This paper reports the results of a campaign done with the 10.4m Gran Telescopio CANARIAS (GTC); this campaign was undertaken to assess the spectral and photometric contamination coming from a 589 nm laser uplink beam scattering and Raman emission induced on the GTC spectro-imager OSIRIS by laser launched ∼1 km off-axis. The photometric contamination is due to primary and secondary scattering of the uplink photons, as well by the Raman inelastic scattering. We have propagated the laser beam creating a mesospheric LGS, then pointed and focused the GTC telescope towards the uplink laser beam, at different heights and up to the LGS, taking into account the observing geometry. In our observations, the Raman emissions for O2 and N2 vibrational lines are visible at 20 km, weakening with altitude and becoming undetectable above 30 km. The scattering of the focused uplink beam is detectable at less than ±0.2 arcmin from the centre of the beam, while for the focused LGS the scattering is narrower, being detectable at less than ±0.1 arcmin around the plume. Recommendations for Laser Traffic Control Systems are given accordingly.
AutoEnRichness: A hybrid empirical and analytical approach for estimating the richness of galaxy clusters
Authors: Chan Matthew C , Stott John P 
Published: August 2022

ABSTRACTWe introduce AutoEnRichness, a hybrid approach that combines empirical and analytical strategies to determine the richness of galaxy clusters (in the redshift range of 0.1 ≤ z ≤ 0.35) using photometry data from the Sloan Digital Sky Survey Data Release 16, where cluster richness can be used as a proxy for cluster mass. In order to reliably estimate cluster richness, it is vital that the background subtraction is as accurate as possible when distinguishing cluster and field galaxies to mitigate severe contamination. AutoEnRichness is comprised of a multistage machine learning algorithm that performs background subtraction of interloping field galaxies along the cluster line of sight and a conventional luminosity distribution fitting approach that estimates cluster richness based only on the number of galaxies within a magnitude range and search area. In this proof-of-concept study, we obtain a balanced accuracy of 83.20 per cent when distinguishing between cluster and field galaxies as well as a median absolute percentage error of 33.50 per cent between our estimated cluster richnesses and known cluster richnesses within r200. In the future, we aim for AutoEnRichness to be applied on upcoming large-scale optical surveys, such as the Legacy Survey of Space and Time and Euclid, to estimate the richness of a large sample of galaxy groups and clusters from across the halo mass function. This would advance our overall understanding of galaxy evolution within overdense environments as well as enable cosmological parameters to be further constrained.
High resolution X-ray spectroscopy of V4641 Sgr during its 2020 outburst
Authors: Shaw A W , Miller J M , Grinberg V , Buisson D J K , Heinke C O , Plotkin R M , Tomsick J A , Bahramian A , Gandhi P , Sivakoff G R 
Published: August 2022

ABSTRACT
We observed the Galactic black hole X-ray binary V4641 Sgr with the high resolution transmission gratings on Chandra during the source’s 2020 outburst. Over two epochs of Chandra gratings observations, we see numerous highly ionized metal lines, superimposed on a hot, disc-dominated X-ray continuum. The measured inner disc temperatures and luminosities imply an unfeasibly small inner disc radius, such that we suggest that the central engine of V4641 Sgr is obscured, and we are viewing scattered X-rays. We find that the emission lines in the Chandra spectra cannot be constrained by a single photoionized model, instead finding that two separate photoionized model components are required, one to reproduce the iron lines and a second for the other metals. We compare the observed X-ray spectra of V4641 Sgr to optical studies during previous outbursts of the source, suggesting that the lines originate in an accretion disc wind, potentially with a spherical geometry.
An ab initio study for the photodissociation of HCl and HF
Authors: Qin Zhi , Bai Tianrui , Liu Linhua 
Published: August 2022

ABSTRACT
Detailed studies of HCl and HF photodissociation are required for an in-depth understanding the chlorine and fluorine chemistry in Venus and exoplanets. Here, we present an ab initio study of photodissociation of HCl and HF. Except for the widely studied A 1Π←X 1Σ+ photodissociation process, the ground-state photodissociation processes for HCl and HF via higher excited states are considered. State-resolved cross-sections are computed for nine photodissociation processes of HCl from a total of 871 ground rovibrational levels. For HF, seven photodissociation processes are considered for the computation of state-resolved cross-sections from all the rovibrational levels in the ground state. Subsequently, temperature-dependent cross-sections for the considered transition processes of HCl and HF are estimated from 0 to 10 000 K with a grid of 34 temperatures. Careful comparisons with the recent ExoMol study and the Leiden Observatory database are made. The photodissociation rates in the interstellar and blackbody radiation fields are also discussed.
Chaotic diffusion of asteroids in the exterior 1:2 mean motion resonance with Mars
Authors: Christou Apostolos A , Dermott Stanley F , Li Dan 
Published: August 2022

ABSTRACT
The inner asteroid belt between 2.1 and 2.5 au is of particular dynamical significance because it is the dominant source of both chondritic meteorites and near-Earth asteroids. This inner belt is bounded by an eccentricity-type secular resonance and by the 1:3 mean motion resonance with Jupiter. Unless asteroid perihelia are low enough to allow scattering by Mars, escape requires transport to one of the bounding resonances. In addition Yarkovsky forces are generally ineffective in changing either the eccentricity and/or inclination for asteroids with diameter ≳30 km. Thus, large asteroids with pericentres far from Mars may only escape from the inner belt through large changes in their eccentricities. In this paper, we study chaotic diffusion of orbits near the 1:2 mean motion resonance with Mars in a systematic way. We show that, while chaotic orbital evolution in both resonant and non-resonant orbits increase the dispersion of the inclinations and eccentricities, it does not significantly change their mean values. We show further that, while the dispersive growth is greatest for resonant orbits, at high e the resonance acts to mitigate asteroid scattering by Mars - making the asteroid lifetime in the belt longer than it would have been for a non-resonant orbit. For asteroids of all sizes in both resonant and non-resonant orbits, the changes in eccentricity needed to account for the observations cannot be achieved by gravitational forces alone. The role of resonant trapping in protecting asteroids from encounters with Mars is also analysed.
Formation of black holes in the pair-instability mass gap: Evolution of a post-collision star
Authors: Costa Guglielmo , Ballone Alessandro , Mapelli Michela , Bressan Alessandro 
Published: August 2022

ABSTRACT
The detection of GW190521 by the LIGO–Virgo collaboration has revealed the existence of black holes (BHs) in the pair-instability (PI) mass gap. Here, we investigate the formation of BHs in the PI mass gap via star–star collisions in young stellar clusters. To avoid PI, the stellar-collision product must have a relatively small core and a massive envelope. We generate our initial conditions from the outputs of a hydrodynamical simulation of the collision between a core helium burning star (∼58 M⊙) and a main-sequence star (∼42 M⊙). The hydrodynamical simulation allows us to take into account the mass lost during the collision (∼12 M⊙) and to build the chemical composition profile of the post-collision star. We then evolve the collision product with the stellar evolution codes parsec and mesa. We find that the post-collision star evolves through all the stellar burning phases until core collapse, avoiding PI. At the onset of core collapse, the post-collision product is a blue supergiant star. We estimate a total mass-loss of about 1 M⊙ during the post-collision evolution, due to stellar winds and shocks induced by neutrino emission in a failed supernova. The final BH mass is ≈87 M⊙. Therefore, we confirm that the collision scenario is a suitable formation channel to populate the PI mass gap.
Metalation calculators for E. coli strain JM109 (DE3): aerobic, anaerobic, and hydrogen peroxide exposed cells cultured in LB media
Authors: Foster Andrew W , Clough Sophie E , Aki Zeynep , Young Tessa R , Clarke Alison R , Robinson Nigel J 
Published: August 2022

Abstract
Three Web-based calculators, and three analogous spreadsheets, have been generated that predict in vivo metal occupancies of proteins based on known metal affinities. The calculations exploit estimates of the availabilities of the labile buffered pools of different metals inside a cell. Here, metal availabilities have been estimated for a strain of Escherichia coli that is commonly used in molecular biology and biochemistry research, e.g. in the production of recombinant proteins. Metal availabilities have been examined for cells grown in Luria-Bertani (LB) medium aerobically, anaerobically, and in response to H2O2 by monitoring the abundance of a selected set of metal-responsive transcripts by quantitative polymerase chain reaction (qPCR). The selected genes are regulated by DNA-binding metal sensors that have been thermodynamically characterized in related bacterial cells enabling gene expression to be read out as a function of intracellular metal availabilities expressed as free energies for forming metal complexes. The calculators compare these values with the free energies for forming complexes with the protein of interest, derived from metal affinities, to estimate how effectively the protein can compete with exchangeable binding sites in the intracellular milieu. The calculators then inter-compete the different metals, limiting total occupancy of the site to a maximum stoichiometry of 1, to output percentage occupancies with each metal. In addition to making these new and conditional calculators available, an original purpose of this article was to provide a tutorial that discusses constraints of this approach and presents ways in which such calculators might be exploited in basic and applied research, and in next-generation manufacturing.
Layer Hall effect induced by hidden Berry curvature in antiferromagnetic insulators
Authors: Chen Rui , Sun Hai-Peng , Gu Mingqiang , Hua Chun-Bo , Liu Qihang , Lu Hai-Zhou , Xie X C 
Published: August 2022

Abstract
The layer Hall effect describes electrons spontaneously deflected to opposite sides at different layers, which has been experimentally reported in the MnBi2Te4 thin films under perpendicular electric fields. Here, we reveal a universal origin of the layer Hall effect in terms of the so-called hidden Berry curvature, as well as material design principles. Hence, it gives rise to zero Berry curvature in momentum space but non-zero layer-locked hidden Berry curvature in real space. We show that, compared to that of a trivial insulator, the layer Hall effect is significantly enhanced in antiferromagnetic topological insulators. Our universal picture provides a paradigm for revealing the hidden physics as a result of the interplay between the global and local symmetries, and can be generalized in various scenarios.
Cavitation in a soft porous material
Authors: Leng Yu , Vlachos Pavlos P , Juanes Ruben , Gomez Hector 
Published: August 2022

Abstract
We study the collapse and expansion of a cavitation bubble in a deformable porous medium. We develop a continuum-scale model that couples compressible fluid flow in the pore network with the elastic response of a solid skeleton. Under the assumption of spherical symmetry, our model can be reduced to an ordinary differential equation that extends the Rayleigh–Plesset equation to bubbles in soft porous media. The extended Rayleigh–Plesset equation reveals that finite-size effects lead to the breakdown of the universal scaling relation between bubble radius and time that holds in the infinite-size limit. Our data indicate that the deformability of the porous medium slows down the collapse and expansion processes, a result with important consequences for wide-ranging phenomena, from drug delivery to spore dispersion.
Mass-selective and ice-free electron cryomicroscopy protein sample preparation via native electrospray ion-beam deposition
Authors: Esser Tim K , Böhning Jan , Fremdling Paul , Agasid Mark T , Costin Adam , Fort Kyle , Konijnenberg Albert , Gilbert Joshua D , Bahm Alan , Makarov Alexander , Robinson Carol V , Benesch Justin L P , Baker Lindsay , Bharat Tanmay A M , Gault Joseph , Rauschenbach Stephan 
Published: August 2022

Abstract
Despite tremendous advances in sample preparation and classification algorithms for electron cryomicroscopy (cryo-EM) and single-particle analysis (SPA), sample heterogeneity remains a major challenge and can prevent access to high-resolution structures. In addition, optimization of preparation conditions for a given sample can be time-consuming. In the current work, it is demonstrated that native electrospray ion-beam deposition (native ES-IBD) is an alternative, reliable approach for the preparation of extremely high-purity samples, based on mass selection in vacuum. Folded protein ions are generated by native electrospray ionization, separated from other proteins, contaminants, aggregates, and fragments, gently deposited on cryo-EM grids, frozen in liquid nitrogen, and subsequently imaged by cryo-EM. We demonstrate homogeneous coverage of ice-free cryo-EM grids with mass-selected protein complexes. SPA reveals that the complexes remain folded and assembled, but variations in secondary and tertiary structures are currently limiting information in 2D classes and 3D EM density maps. We identify and discuss challenges that need to be addressed to obtain a resolution comparable to that of the established cryo-EM workflow. Our results show the potential of native ES-IBD to increase the scope and throughput of cryo-EM for protein structure determination and provide an essential link between gas-phase and solution-phase protein structures.
Comment on the subtlety of defining a real-time path integral in lattice gauge theories
Authors: Matsumoto Nobuyuki 
Published: August 2022

Abstract
Recently, Hoshina, Fujii, and Kikukawa pointed out that the naive lattice gauge theory action in the Minkowski signature does not result in a unitary theory in the continuum limit, and Kanwar and Wagman proposed alternative lattice actions to the Wilson action without divergences. We show here that the subtlety can be understood from the asymptotic expansion of the modified Bessel function, which has been discussed for the path integral of compact variables in nonrelativistic quantum mechanics. The essential ingredient for defining the appropriate continuum theory is the iε prescription, and with the proper implementation of this we show that the Wilson action can be used for real-time path integrals. It is important that iε should be implemented for both timelike and spacelike plaquettes. We also suggest why iε is required for the Wilson action from the Hamiltonian formalism: it is needed to manifestly suppress the contributions from singular paths, for which the Wilson action can give different values from those of the actual continuum action.