bluuebunny/crossref_metadata_2025_split huggingface dataset:
5 cm OH Masers in Northern Star Formation Regions
Authors: Qiao Hai-Hua , Ouyang Xu-Jia , Shen Zhi-Qiang , Breen Shari L. , Yang Kai , Chen Xi , Li Juan 
Published: December 2024

Abstract
We present a 6.0 GHz excited-state OH maser survey toward 155 northern star formation regions utilizing the Shanghai Tianma Radio Telescope. In total, we detect 44 6.0 GHz OH masers, 8 of which are new detections (one at 6016 MHz, two at 6030 MHz, and five at 6035 MHz). Of these 44 detected 6.0 GHz OH masers, 13 sites exhibit 6030 MHz OH masers, all 44 sites show the 6035 MHz transition, one site (G009.620+0.194) has the only 6016 MHz OH maser, and one site (W3(OH)) shows the only 6049 MHz OH maser. The 6016 MHz OH maser is the first OH maser of this transition detected in star formation regions. Investigations of the association between 6030/6035 MHz OH masers with 1665 MHz ground-state OH, 6.7 GHz methanol, and 22 GHz water masers show that 1665 MHz OH masers are good indicators of 6.0 GHz OH masers (29% detection rate), which is consistent with previous results. The majority (more than 77%) of 6030 and 6035 MHz OH masers are associated with 6.7 GHz methanol and/or 22 GHz water masers. Comparison between our spectra with previous spectra, we find that only two sources remain fairly stable since their discoveries. We identify 80 Zeeman pairs in 32 6.0 GHz OH maser sites with typical magnetic field strengths of less than 10 mG. The magnetic field directions derived from these 32 maser sites with Zeeman pairs are consistent with previous work, which indicates that the 6.0 GHz OH masers may be potential tracers of the large-scale Galactic magnetic field.
Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program
Authors: Luo Wentao , Silverman John D. , More Surhud , Goulding Andy , Miyatake Hironao , Nishimichi Takahiro , Hikage Chiaki , Kawinwanichakij Lalitwadee , Li Junyao , Li Qinxun , Li Xiangchong , Medezinski Elinor , Oguri Masamune , Oogi Taira , Sifon Cristobal 
Published: December 2024

Abstract
We assess the dark matter halo masses of luminous active galactic nuclei (AGNs) over the redshift range 0.2–1.2 using galaxy–galaxy lensing based on imaging data from the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). We measure the weak lensing signal of a sample of 48,907 AGNs constructed using HSC and Wide-field Infrared Survey Explorer photometry. As expected, we find that the lensing mass profile of total AGN sample is consistent with that of massive galaxies (

log
(

M
*

/

h

−
2

M
⊙

)
∼

10.61). Surprisingly, the lensing signal remains unchanged when the AGN sample is split into four host galaxy stellar mass bins. Specifically, we find that the excess surface density of AGNs residing in galaxies with high stellar masses significantly differs from that of the control sample. We further fit a halo occupation distribution model to the data to infer the posterior distribution of parameters including the average halo mass. We find that the characteristic halo mass of the full AGN population lies near the knee (

log
(

M
h

/

h

−
1

M
⊙

)
=
12.0

) of the stellar-to-halo mass relation (SHMR). Illustrative of the results given above, the halo masses of AGNs residing in host galaxies with high stellar masses (i.e., above the knee of the SHMR) fall below the calibrated SHMR while the halo masses of the low stellar mass sample are more consistent with the established SHMR. These results indicate that massive halos with a higher clustering bias tend to suppress AGN activity, probably due to the lack of available gas.
Filament Accretion and Fragmentation in the Perseus Molecular Cloud
Authors: Chen Michael Chun-Yuan , Di Francesco James , Friesen Rachel K. , Pineda Jaime E. , Caselli Paola , Ginsburg Adam , Kirk Helen , Punanova Anna ,   The GAS Collaboration
Published: December 2024

Abstract
Observations suggest that filaments in molecular clouds can grow by mass accretion while forming cores via fragmentation. Here, we present one of the first large-sample studies of filament accretion using velocity gradient measurements of star-forming filaments on the ∼0.05 pc scale with NH3 observations of the Perseus Molecular Cloud, primarily obtained as a part of the Green Bank Ammonia Survey. In this study, we find significant correlations between the velocity gradient, velocity dispersion, mass per unit length, and number of cores per unit length of the Perseus filaments. Our results suggest a scenario in which filaments not only grow through mass accretion, but also form new cores continuously in the process, well into the thermally supercritical regime. Such behavior is contrary to that expected from isolated filament models but consistent with how filaments form within a more realistic cloud environment, suggesting that the cloud environment plays a crucial role in shaping core formation and evolution in filaments. Furthermore, even though velocity gradients within filaments are not oriented randomly, we find no correlation between velocity gradient orientation and the filament properties we analyzed. This result suggests that gravity is unlikely to be the dominant mechanism imposing order on the ∼0.05 pc scale for dense star-forming gas.
A Study of Slow-mode Shocks in the Near-Earth Magnetotail with MMS Observations and Hybrid Simulations
Authors: Walia Nehpreet K. , Seki Kanako , Amano Takanobu , Kitamura Naritoshi , Saito Yoshifumi , Ahmadi Tara , Gershman Daniel J. , Pollock Craig J. , Giles Barbara L. , Fuselier Stephen A. , Russell Christopher T. , Burch James L. 
Published: December 2024

Abstract
The structure of the magnetic reconnection boundary, particularly the presence of slow-mode shocks in the near-Earth magnetotail was studied by using magnetospheric multiscale (MMS) observations and 2.5D hybrid simulations. A total of 51 crossings of MMS from 2017 to 2021 were analyzed. We found that the detection percentage of slow-mode shocks in the near-Earth magnetotail is 41%–55%. Previous studies have only reported one slow-mode shock event in the near-Earth magnetotail and a slow-mode shock detection percentage of 10% or lower in the mid-to-distant magnetotail. It was observed that if the high-energy beam region data is removed from the slow-mode shock downstream observations then the detection of slow-mode shocks reduces, implying that the kinetic effects play an important role in the detection of slow-mode shocks. For the crossings where the interface was not identified as a slow-mode shock, it was found that the turbulence in those crossings can change the mass flux values and disrupt the detection of slow-mode shock. However, the macroscopic slow-mode shock-like structure stably exists around the magnetic reconnection interface, as most of the conditions for slow-mode shocks were satisfied. This result suggests that slow-mode shocks are a general feature of magnetic reconnection geometry. We find that the lack of detection of slow-mode shocks in previous observations and simulations can be explained by taking into account the kinetic structure of slow-mode shocks and the presence of turbulence.
First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen
Authors: Radziszewski Krzysztof , Heinzel Petr , Kašparová Jana , Litwicka Michalina , Berlicki Arkadiusz , Rudawy Paweł , Falewicz Robert 
Published: December 2024

Abstract
The primary objective of this study is to develop a time-dependent model of the flaring atmosphere based on observational data. Here, we present, for the first time, a comparison between numerical simulations of the flaring emission, specifically focusing on the hydrogen Hα line, utilizing the FLARIX code and spectral observations of a compact C1.6 GOES-class flare observed on 2012 September 10, by the MSDP imaging spectrograph installed at the Białków Observatory. The Multichannel Subtractive Double Pass imaging spectrograph spectral data, collected with a temporal resolution as fine as 50 ms, enabled a comprehensive analysis of Hα line profiles and light curves measured within an area of the flare’s emission. An initial atmospheric model close to VAL-C, with a modified temperature in the upper chromosphere, was employed in simulations. To enhance temporal resolution, modulations of the nonthermal electron (NTE) beam’s parameters were introduced based on variations in observed hard X-ray (HXR) flux (using RHESSI data). The synthesized Hα line profiles were compared with the observed spectra. During the impulsive phase of the flare, the evolution of the observed and synthetic Hα line intensity agrees, but discrepancies were found in intensities at specific wavelengths of the Hα line profile. Fluctuations in the energy flux of NTEs exhibited a strong correlation with the Hα emission during the HXR pulse. After considering various effects (such as the filling factor FF = 0.20) that could influence observed emissions, relatively good agreement between theoretical and observed lines was achieved.
Dynamic 3D Simulation of Surface Charging on Rotating Asteroids
Authors: Quan Ronghui , Song Zhiying , Liu Zhigui 
Published: December 2024

Abstract
The surface-charging phenomenon of asteroids, mainly resulting from solar wind plasma and solar radiation, has been extensively studied. However, the influence of the asteroid’s rotation on surface charging is not yet fully understood. In this study, a neural network is established to replace numerical integration, improving the efficiency of dynamic 3D simulations. We simulate rotating asteroids and their surrounding plasma environments under various conditions, including the quiet solar wind and solar storms. Different minerals on the asteroid surface are also considered. Additionally, the effects of orbital motion and obliquity are studied for asteroids with rotation periods comparable to their orbital periods. The results show that under the typical solar wind, the maximum and minimum potentials of asteroids gradually decrease with increasing rotation periods, especially when the solar wind is obliquely incident. For asteroids with rotation periods longer than one week, this decreasing trend becomes extremely slow. During a solar storm, the solar wind plasma changes sharply, and the susceptibility of an asteroid’s surface potential to rotation is greatly pronounced. Surface minerals also play a role; plagioclase is the most sensitive mineral among those explored, while ilmenite appears indifferent to changes in rotation periods. Understanding the surface charging of asteroids under various rotation periods and angles is crucial for further research on solar wind plasma and asteroids’ surface dust motion, providing a reference for the safe landing and exploration of asteroids.
Reverse Shock Emission from Misaligned Structured Jets in Gamma-Ray Bursts
Authors: Pang Sen-Lin , Dai Zi-Gao 
Published: December 2024

Abstract
The afterglow of gamma-ray bursts (GRBs) has been extensively discussed in the context of shocks generated during an interaction of relativistic outflows with their ambient medium. This process leads to the formation of both a forward and a reverse shock. While the emission from the forward shock, observed off-axis, has been well-studied as a potential electromagnetic counterpart to a gravitational-wave-detected merger, the contribution of the reverse shock is commonly overlooked. In this paper, we investigate the contribution of the reverse shock to the GRB afterglows observed off-axis. In our analysis, we consider jets with different angular profiles, including two-component jets, power-law structured jets, Gaussian jets, and “mixed jets” featuring a Poynting-flux-dominated core surrounded by a baryonic wing. We apply our model to GRB 170817A/GW170817 and employ the Markov Chain Monte Carlo method to obtain model parameters. Our findings suggest that the reverse shock emission can significantly contribute to the early afterglow. In addition, our calculations indicate that the light curves observable in future off-axis GRBs may exhibit either double peaks or a single peak with a prominent feature, depending on the jet structure, viewing angle, and microphysics shock parameters.
Challenges for Fast Radio Bursts as Multimessenger Sources from Binary Neutron Star Mergers
Authors: Bhardwaj Mohit , Palmese Antonella , Magaña Hernandez Ignacio , D’Emilio Virginia , Morisaki Soichiro 
Published: December 2024

Abstract
Fast radio bursts (FRBs) are millisecond-duration transients from extragalactic sources, with their origins remaining a topic of active debate. Among the proposed progenitors, binary neutron star (BNS) mergers are compelling candidates for some nonrepeating FRBs. However, associating FRBs with BNS mergers cannot be based solely on low chance coincidence probability. This study delineates necessary criteria for associating FRBs with BNS mergers, focusing on the postmerger ejecta environment. To underscore the significance of these criteria, we scrutinise the proposed association between GW190425 and FRB 20190425A, considering the requirement for the FRB signal to traverse the dense merger ejecta without significant attenuation to remain detectable at 400 MHz. Our investigation reveals that if the FRB is linked to the gravitational-wave (GW) event, the GW data support a highly off-axis configuration, with a probability of the BNS merger viewing angle p(θ

v
> 30°) being ≈99.99%. This strongly excludes an on-axis system, which is required for this FRB to be detectable. We also find faraway FRB emission models inadequate to explain the FRB 20190425A–GW190425 connection. Thus, we conclude that GW190425 is not related to FRB 20190425A. We discuss the implications for future multimessenger observations, suggesting that BNS merger remnants are unlikely to account for more than 1% of FRB sources. This finding implies that short gamma-ray bursts, which are expected to occur in only a fraction of all BNS mergers, cannot account for the overall characteristics of the FRB host population.
Exploring Magnetic Fields in a Merging Galaxy: Comparing Polarization and Velocity Gradient in the Centaurus Galaxy
Authors: Nguyen Quynh Lan , Hu Yue , Lazarian Alex 
Published: December 2024

Abstract
In this study, we apply the velocity gradient technique to the merging Centaurus galaxy. We compare gradient maps derived from the PHANGS-Atacama Large Millimeter/submillimeter Array survey using CO emission lines with magnetic field tracings from dust polarization data obtained via the HAWC+ instrument. Our analysis reveals a strong correspondence between the directions indicated by these two tracers across most of the galactic image. Specifically, we identify jet regions as areas of antialignment, consistent with previous reports that gradients tend to rotate 90° in outflow regions. Statistically, we find that the alignment of magnetic fields, as revealed by polarization, is most accurate in regions with the highest signal-to-noise ratios. Our findings underscore the utility of velocity gradients as a valuable complementary tool for probing magnetic fields and dynamical processes in merging galaxies. This proves the general utility of velocity gradients for mapping magnetic fields in astrophysical objects with complex dynamics.
Developing a Pilot Curriculum to Enhance Undergraduate Student Well-Being
Authors: Owen Melissa I. , Pfeiffer Katherine , Jordan Dorothy , Dittmann Andrea 
Published: December 2024

Background
The purpose of this article is to describe the development and implementation of a program to improve well-being in undergraduate students and promote positive transitions into the workplace. College students experience anxiety, depression, and impaired coping, which were exacerbated during the COVID-19 (coronavirus disease 2019) pandemic. As students transition into their career, it is imperative they develop positive coping strategies and resiliency to manage workplace stress.

Method
The Personal Leadership Collective (PLC) is designed as a four-semester series for third- and fourth-year nursing and business students. Four themes guided the activities: awareness, connection, agility, and growth. Students participated in asynchronous online learning modules and in-person activities. Fourth-year students who completed the series served as peer mentors to third-year students.

Results
The program is undergoing formal evaluation. Anecdotal feedback from participants is positive.

Conclusion

The PLC is a program that could enhance professional development in undergraduate students.

[
J Nurs Educ
. 2024;63(X):XXX–XXX.]
Les activités cliniques comme l’une des portes dans la « tour d’ivoire universitaire »
Authors: Frouville Olivier de 
Published: December 2024

Alors que l’universitaire (étudiant ou enseignant) voit le droit avant tout comme un système de normes, la clinique juridique lui permet de l’envisager dans son contexte social. Elle lui sert aussi à comprendre le droit par la connaissance des communautés épistémiques qui font un certain droit et le parlent dans une langue qui leur est propre. Le « bon » juriste parvient alors à intégrer la théorie et la pratique dans un geste unique.
Les visions du monde de Sylvie Germain et de Victor Hugo
Authors: Goulet Alain 
Published: December 2024

Alors qu’on ne peut parler d’influence de Victor Hugo sur Sylvie Germain, en revanche on peut constater une grande affinité de leurs univers spirituels. L’un et l’autre sont des songeurs, des voyants et des visionnaires qui savent nous transmettre et nous faire partager par leurs œuvres bien des visions de l’immensité et nous ouvrir à l’au-delà du visible. La contemplation leur est familière et tous deux, penchés « au bord de l’infini », ont accès à la « Bouche d’ombre » qui dévoile au poète l’ensemble de la création et l’unité cosmique et mystique de l’échelle des êtres qui mène de Dieu à Satan, avec, en son milieu, « l’homme qui plane et rampe ». Et tous deux mettent en évidence l’importance de la nuit, une nuit qu’il faut traverser pour accéder à la véritable clarté.
Racial Anthropology in Colonial Korea: “Japanese-Korean Common Ancestry” vs Nativism and Eugenics (1916–1940)
Authors: Nanta Arnaud 
Published: December 2024

La Corée colonisée (1905‑1945) vit se déployer sous l’égide du Japon des savoirs visant à la compréhension de la société de la « péninsule », dans un objectif à la fois académique mais aussi de légitimation du pouvoir japonais. Au sein de ce dispositif, la question de la saisie, de la compréhension et du classement des corps – qui avait d’abord constitué une obsession nationale au Japon comme en Europe – s’imposa comme l’une des grandes préoccupations des savants coloniaux. Ainsi les trois chaires d’anatomie de l’université impériale de Keijō (Seoul), fondée en 1924, incluaient-elles deux chaires d’anthropologie physique, une configuration inédite au sein des universités d’État japonaises. Ses responsables s’efforcèrent de démontrer la validité de la théorie des « origines communes entre Japonais et Coréens » au moyen de la biologie, théorie qui avait servi depuis 1910 à légitimer l’annexion par une « proximité de race » entre conquérants et conquis. Cependant, l’entre-deux-guerres allait voir la montée d’un discours ethniciste porté par le nouveau courant eugéniste, qui s’opposait à tout rapprochement entre le « peuple japonais » saisi comme pur et les populations colonisées. La seconde moitié des années 1930 et la période de guerre virent un affrontement entre deux visions opposées du Japon, entre empire ou peuple réethnicisé.
JBZ (Abidjan) et Bogolan (Bamako) : itinéraire biographique de deux “studios live” de légende et de leurs principaux protagonistes
Authors: Olivier Emmanuelle , Pras Amandine 
Published: December 2024

À la croisée entre ethnomusicologie et science de l’ingénierie sonore, cet article propose une lecture des musiques ouest-africaines au prisme des lieux et des technologies de la production musicale. Octobre 2022 : le studio Bogolan de Bamako ferme définitivement ses portes. Quatre ans auparavant à Abidjan, c’est JBZ qui disparaissait. Ces deux grands studios hérités de l’ère analogique qui ont « fait » la musique ouest-africaine des années 1980-2010 n’ont plus leur place dans l’écosystème de la musique à l’ère post-globale, caractérisé par une profusion de petits studios basés sur des stations audionumériques. À travers un itinéraire biographique de ces deux studios de légende et de leurs principaux protagonistes (propriétaires, réalisateurs, producteurs, arrangeurs et ingénieurs du son), cet article entend brosser le portrait d’une époque et d’un milieu, celui d’une première industrie musicale indépendante des pouvoirs étatiques, initiant là le mouvement ouest-africain de la world music. Mais la trajectoire et l’activité de ces studios révèlent aussi des différences notables dans les politiques culturelles et économiques des deux pays : quand Bogolan privilégie le folklore malien et les collaborations avec des musicien·ne·s et ingénieurs du son des pays du Nord, JBZ attire les plus grandes vedettes des musiques urbaines d’Afrique de l’Ouest et d’Afrique centrale. Ce texte montre enfin les conséquences des choix différents de Bogolan et JBZ sur la culture des studios numériques dans chacun des pays : continuité de la transmission des savoirs de l’analogique au numérique à Abidjan dont la production musicale est aujourd’hui connectée au marché global, contre peu d’échanges et une rupture entre un « studio live » international et les studios numériques à Bamako, largement déconnectés de l’industrie globale.
Du studio à la « scène ». Les lieux du beatmaking à Dakar
Authors: Péneau Maël 
Published: December 2024

Les studios où est produite et enregistrée la musique hip-hop sénégalaise se distinguent les uns des autres selon des critères qui tiennent autant aux équipements utilisés qu’aux configurations spatiales et géographiques. En fonction de leur localisation, des parcours de leurs propriétaires, de leurs utilisateurs, mais aussi de leurs usages, ces studios entretiennent en effet des liens spécifiques avec leur environnement social, culturel, et urbain. À Dakar, des studios sont installés dans une chambre, elle-même située dans un appartement familial ; d’autres occupent un appartement individuel entièrement consacré à la production sonore et à l’enregistrement. Certains lieux réunissent plusieurs studios, des bureaux, et des salles de réunion. Bien que partageant la même dénomination, ces lieux recouvrent des réalités sociales et créatives différentes. En s’appuyant sur les données recueillies lors d’un terrain de recherche ethnographique réalisé entre 2019 et 2020 à Dakar auprès d’une quinzaine de beatmakers et d’ingénieurs du son sénégalais dans le cadre de ma thèse, cet article analyse la façon dont ces lieux s’inscrivent à la fois dans les circuits de création et de diffusion de la musique (à l’échelle locale comme à l’échelle globale), et aussi dans la vie sociale des quartiers où ils sont implantés, en interrogeant les pratiques musicales qui y ont lieu au prisme des relations qu’ils entretiennent avec leur environnement social et urbain.