bluuebunny/crossref_metadata_2025_split huggingface dataset:
ELVES II: Globular Clusters and Nuclear Star Clusters of Dwarf Galaxies: the Importance of Environment
Authors: Carlsten Scott G. , Greene Jenny E. , Beaton Rachael L. , Greco Johnny P. 
Published: March 2022

Abstract
We present the properties of the globular clusters (GCs) and nuclear star clusters (NSCs) of low-mass (105.5 < M
⋆ < 108.5
M
⊙) early-type satellites of Milky Way–like and small group hosts in the Local Volume (LV) using deep, ground-based data from the ongoing Exploration of Local VolumE Satellites Survey. This sample of 177 dwarfs significantly increases the statistics for studying the star clusters of dwarfs in low-density environments, offering an important comparison to samples from nearby galaxy clusters. The LV dwarfs exhibit significantly lower nucleation fractions at fixed galaxy mass than dwarfs in nearby clusters. The masses of NSCs of LV dwarfs show a similar scaling of

M

⋆
,
NSC

∝

M

⋆
,
gal

0.4

as that found in clusters but offset to lower NSC masses. To deal with foreground/background contamination in the GC analysis, we employ both a statistical subtraction and Bayesian approach to infer the average GC system properties from all dwarfs simultaneously. We find that the GC occupation fraction and average abundance are both increasing functions of galaxy stellar mass, and the LV dwarfs show significantly lower average GC abundance at fixed galaxy mass than a comparable sample of Virgo dwarfs analyzed in the same way, demonstrating that GC prevalence also shows an important secondary dependence on the dwarf’s environment. This result strengthens the connection between GCs and NSCs in low-mass galaxies. We discuss these observations in the context of modern theories of GC and NSC formation, finding that the environmental dependencies can be well explained by these models.
High-latitude Observations of Inertial-range Turbulence by the Ulysses Spacecraft During the Solar Minimum of 1993–96
Authors: Watson Abigale S. , Smith Charles W. , Marchuk Anastasia V. , Argall Matthew R. , Joyce Colin J. , Isenberg Philip A. , Vasquez Bernard J. , Schwadron Nathan A. , Bzowski Maciej , Kubiak Marzena A. , Murphy Neil 
Published: March 2022

Abstract
We have examined Ulysses magnetic field measurements for the years 1993 through 1996 as the spacecraft moved sunward from 5 au at high southern latitudes, passing through perihelion during the first fast-latitude scan to achieve high northern latitudes, and finally returning to 5 au. These years represent near-solar-minimum activity, providing a clear measure of high-latitude solar-wind turbulence. We apply a series of tests to the data, examining both the magnetic variance anisotropy and the underlying wavevector anisotropy, finding them to be consistent with past 1 au observations. The variance anisotropy depends upon both the thermal proton temperature parameter and the amplitude of the magnetic power spectrum, while the underlying wavevector anisotropy is dominated by the component perpendicular to the mean magnetic field. We also examine the amplitude of the magnetic power spectrum as well as the associated turbulent transport of energy to small scales that results in the heating of the thermal plasma. The measured turbulence is found to be stronger than that seen at low latitudes by the Voyager spacecraft as it traverses the distance from 1 to 5 au during the years approaching solar maximum. If the high- and low-latitude sources are comparable, this would indicate that while the heating processes are active in both regions, the turbulence has had less decay time in the transport of energy to small scales. Alternatively, it may also be that the high-latitude source is stronger.
Bayesian Rotation Inversion of KIC 11145123
Authors: Hatta Yoshiki , Sekii Takashi , Benomar Othman , Takata Masao 
Published: March 2022

Abstract
A scheme of Bayesian rotation inversion, which allows us to compute the probability of a model of a stellar rotational profile, is developed. The validation of the scheme with simple rotational profiles and the corresponding sets of artificially generated rotational shifts has been successfully carried out, and we can correctly distinguish the (right) rotational model, prepared beforehand for generating the artificial rotational shifts, from the other (wrong) rotational model. The Bayesian scheme is applied to a γ Dor–δ Sct-type hybrid star, KIC 11145123, leading to a result that the convective core of the star might be rotating much faster (∼10 times faster) than the other regions of the star. The result is consistent with that previously suggested by Hatta et al. based on a three-zone modeling, further strengthening their argument from a Bayesian point of view.
GASP XXXVII: The Most Extreme Jellyfish Galaxies Compared with Other Disk Galaxies in Clusters, an H i Study
Authors: Luber N. , Müller A. , van Gorkom J. H. , Poggianti B. M. , Vulcani B. , Franchetto A. , Bacchini C. , Bettoni D. , Deb T. , Fritz J. , Gullieuszik M. , Ignesti A. , Jaffe Y. , Moretti A. , Paladino R. , Ramatsoku M. , Serra P. , Smith R. , Tomicic N. , Tonnesen S. , Verheijen M. , Wolter A. 
Published: March 2022

Abstract
We present the results of a Very Large Array H i imaging survey aimed at understanding why some galaxies develop long extraplanar Hα tails, becoming extreme jellyfish galaxies. The observations are centered on five extreme jellyfish galaxies optically selected from the WINGS and OMEGAWINGS surveys and confirmed to have long Hα tails through MUSE observations. Each galaxy is located in a different cluster. In the observations, there are in total 88 other spiral galaxies within the field of view (40′ × 40′) and observed bandwidth (6500 km s−1). We detect 13 of these 88 spirals, plus one uncataloged spiral, with H i masses ranging from 1 to 7 × 109
M
⊙. Many of these detections have extended H i disks, two show direct evidence for ram pressure stripping, and others are possibly affected by tidal forces and/or ram pressure stripping. We stack the 75 nondetected spiral galaxies and find an average H i mass of 1.9 × 108
M
⊙, which, given their average stellar mass, implies that they are very H i deficient. Comparing the extreme jellyﬁsh galaxies to the other disk galaxies, we ﬁnd that they are at smaller projected distance from the cluster center, and have a higher stellar mass and higher relative velocity than all other H i detections and most nondetections. We conclude that the high stellar mass allows extreme jellyfish galaxies to fall deeply into the cluster before being stripped, and the surrounding ICM pressure gives rise to their spectacular star-forming tails.
Atmospheric Dynamics of Temperate Sub-Neptunes. I. Dry Dynamics
Authors: Innes Hamish , Pierrehumbert Raymond T. 
Published: March 2022

Abstract
Sub-Neptunes (planets with radii between 2 and 4 R
⊕) are abundant around M-dwarf stars, yet the atmospheric dynamics of these planets is relatively unexplored. In this paper, we aim to provide a basic underpinning of the dry dynamics of general low-mean-molecular-weight, temperate sub-Neptune atmospheres. We use the ExoFMS general circulation model (GCM) with an idealized gray-gas radiation scheme to simulate planetary atmospheres with different levels of instellation and rotation rates, using the atmosphere of K2-18b as our control. We find that the atmospheres of tidally locked (TL), temperate sub-Neptunes have weak horizontal temperature gradients owing to their slow rotation rates and hydrogen-dominated composition. The zonal wind structure is dominated by high-latitude cyclostrophic jets driven by the conservation of angular momentum. At low pressures we observe superrotating equatorial jets, which we propose are driven by a Rossby–Kelvin instability similar to the type seen in simulations of idealized atmospheres with axisymmetric forcing. By viewing the flow in TL coordinates, we find the predominant overturning circulation to be between the day side and night side, and we derive scaling relations linking the TL stream function and vertical velocities to instellation. Comparing our results to the only other GCM study of K2-18b, we find significant qualitative differences in dynamics, highlighting the need for further collaboration and investigation into the effects of different dynamical cores and physical parameterizations. This paper provides a baseline for studying the dry dynamics of temperate sub-Neptunes, which will be built on in part II with the introduction of moist effects.
LAGER Lyα Luminosity Function at z ∼ 7: Implications for Reionization
Authors: Wold Isak G. B. , Malhotra Sangeeta , Rhoads James , Wang Junxian , Hu Weida , Perez Lucia A. , Zheng Zhen-Ya , Khostovan Ali Ahmad , Walker Alistair R. , Barrientos L. Felipe , González-López Jorge , Harish Santosh , Infante Leopoldo , Jiang Chunyan , Pharo John , Moya-Sierralta Cristóbal , Bauer Franz E. , Galaz Gaspar , Valdes Francisco , Yang Huan 
Published: March 2022

Abstract
We present a new measurement of the Lyα luminosity function (LF) at redshift z = 6.9, finding moderate evolution from z = 5.7 that is consistent with a fully or largely ionized z ∼ 7 intergalactic medium. Our result is based on four fields of the LAGER (Lyman Alpha Galaxies in the Epoch of Reionization) project. Our survey volume of 6.1 × 106 Mpc3 is double that of the next largest z ∼ 7 survey. We combine two new LAGER fields (WIDE12 and GAMA15A) with two previously reported LAGER fields (COSMOS and CDFS). In the new fields, we identify N = 95 new z = 6.9 Lyα emitter (LAEs) candidates, characterize our survey’s completeness and reliability, and compute Lyα LFs. The best-fit Schechter LF parameters for all four LAGER fields are in good general agreement. Two fields (COSMOS and WIDE12) show evidence for a bright-end excess above the Schechter function fit. We find that the Lyα luminosity density declines at the same rate as the UV continuum LF from z = 5.7 to 6.9. This is consistent with an intergalactic medium that was fully ionized as early as redshift z ∼ 7 or with a volume-averaged neutral hydrogen fraction of x
H I < 0.33 at 1σ.
Modeling Fast Radio Burst Dispersion and Scattering Properties in the First CHIME/FRB Catalog
Authors: Chawla P. , Kaspi V. M. , Ransom S. M. , Bhardwaj M. , Boyle P. J. , Breitman D. , Cassanelli T. , Cubranic D. , Dong F. Q. , Fonseca E. , Gaensler B. M. , Giri U. , Josephy A. , Kaczmarek J. F. , Leung C. , Masui K. W. , Mena-Parra J. , Merryfield M. , Michilli D. , Münchmeyer M. , Ng C. , Patel C. , Pearlman A. B. , Petroff E. , Pleunis Z. , Rahman M. , Sanghavi P. , Shin K. , Smith K. M. , Stairs I. , Tendulkar S. P. 
Published: March 2022

Abstract
We present a Monte Carlo–based population synthesis study of fast radio burst (FRB) dispersion and scattering focusing on the first catalog of sources detected with the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst (CHIME/FRB) project. We simulate intrinsic properties and propagation effects for a variety of FRB population models and compare the simulated distributions of dispersion measures and scattering timescales with the corresponding distributions from the CHIME/FRB catalog. Our simulations confirm the results of previous population studies, which suggested that the interstellar medium of the host galaxy alone (simulated based on the NE2001 model) cannot explain the observed scattering timescales of FRBs. We therefore consider additional sources of scattering, namely, the circumgalactic medium (CGM) of intervening galaxies and the circumburst medium whose properties are modeled based on typical Galactic plane environments. We find that a population of FRBs with scattering contributed by these media is marginally consistent with the CHIME/FRB catalog. In this scenario, our simulations favor a population of FRBs offset from their galaxy centers over a population that is distributed along the spiral arms. However, if the models proposing the CGM as a source of intense scattering are incorrect, then we conclude that FRBs may inhabit environments with more extreme properties than those inferred for pulsars in the Milky Way.
Exploring Gravitationally Lensed z ≳ 6 X-Ray Active Galactic Nuclei Behind the RELICS Clusters
Authors: Bogdán Ákos , Kovács Orsolya E. , Jones Christine , Forman William R. , Kraft Ralph P. , Strait Victoria , Coe Dan , Bradač Maruša 
Published: March 2022

Abstract
Although observations of high-redshift quasars demonstrate that many supermassive black holes (BHs) reached large masses within one billion years after the Big Bang, the origin of the first BHs is still a mystery. A promising way to constrain the origin of the first BHs is to explore the average properties of z ≳ 6 BHs. However, typical BHs remain hidden from X-ray surveys, which is due to their relatively faint nature and the limited sensitivity of X-ray telescopes. Gravitational lensing provides an attractive way to study this unique galaxy population as it magnifies the faint light from these high-redshift galaxies. Here, we study the X-ray emission originating from 155 gravitationally lensed z ≳ 6 galaxies that were detected in the Reionization Lensing Cluster Survey. We utilize Chandra X-ray observations to search for active galactic nuclei (AGNs) in the individual galaxies and in the stacked galaxy samples. We did not identify an individual X-ray source that was undoubtedly associated with a high-redshift galaxy. We stack the signal from all galaxies and do not find a statistically significant detection. We split our sample based on stellar mass, star formation rate, and lensing magnification and stack these subsamples. We obtain a 2.2σ detection for massive galaxies with an X-ray luminosity of (3.7 ± 1.6) × 1042 erg s−1, which corresponds to a (3.0 ± 1.3) × 105
M
⊙ BH accreting at its Eddington rate. Other stacks remain undetected and we place upper limits on the AGN emission. These limits imply that the bulk of BHs at z ≳ 6 either accrete at a few percent of their Eddington rate and/or are 1–2 orders of magnitude less massive than expected based on the stellar mass of their host galaxy.
CHORUS. IV. Mapping the Spatially Inhomogeneous Cosmic Reionization with Subaru HSC
Authors: Yoshioka Takehiro , Kashikawa Nobunari , Inoue Akio K. , Yamanaka Satoshi , Shimasaku Kazuhiro , Harikane Yuichi , Shibuya Takatoshi , Momose Rieko , Ito Kei , Liang Yongming , Ishimoto Rikako , Takeda Yoshihiro , Ouchi Masami , Lee Chien-Hsiu 
Published: March 2022

Abstract
Spatial inhomogeneity is one of the important features for understanding the reionization process; however, it has not yet been fully quantified. To map this inhomogeneous distribution, we simultaneously detect Lyα emitters (LAEs) and Lyman-break galaxies (LBGs) at z ∼ 6.6 from the Subaru/Hyper Suprime-Cam large-area (∼1.5 deg2 = 34,000 cMpc2) deep survey. We estimate the neutral fraction, x
HI, from the observed number density ratio of LAEs to LBGs, n(LAE)/n(LBG), using numerical radiative transfer simulations, in which model galaxies are selected to satisfy the observed selection function. While the average x
HI within the field of view is found to be x
HI < 0.4, which is consistent with previous studies, the variation of n(LAE)/n(LBG) within the field of view for every 140 pMpc2 area is found to be as large as a factor of 3. This may suggest a spatially inhomogeneous topology of reionization, but it also leaves open the possibility that the variation is based on the inherent large-scale structure of the galaxy distribution. Based on the simulations, it may be difficult to distinguish between the two from the current survey. We also find that LAEs in the high-LAE-density region are more numerous at high EW0, supporting the fact that the observed n(LAE)/n(LBG) is more or less driven by the neutral fraction, though the statistical significance is not high.
A Guide to Realistic Uncertainties on the Fundamental Properties of Solar-type Exoplanet Host Stars
Authors: Tayar Jamie , Claytor Zachary R. , Huber Daniel , van Saders Jennifer 
Published: March 2022

Abstract
Our understanding of the properties and demographics of exoplanets critically relies on our ability to determine the fundamental properties of their host stars. The advent of Gaia and large spectroscopic surveys has now made it possible, in principle, to infer the properties of individual stars, including most exoplanet hosts, to very high precision. However, we show that, in practice, such analyses are limited by uncertainties in both the fundamental scale and our models of stellar evolution, even for stars similar to the Sun. For example, we show that current uncertainties on measured interferometric angular diameters and bolometric fluxes set a systematic uncertainty floor of ≈2.4% in temperature, ≈2.0% in luminosity, and ≈4.2% in radius. Comparisons between widely available model grids suggest uncertainties of order ≈5% in mass and ≈20% in age for main-sequence and subgiant stars. While the radius uncertainties are roughly constant over this range of stars, the model-dependent uncertainties are a complex function of luminosity, temperature, and metallicity. We provide open-source software for approximating these uncertainties for individual targets and discuss strategies for reducing these uncertainties in the future.
Modeling Photoionized Turbulent Material in the Circumgalactic Medium. III. Effects of Corotation and Magnetic Fields
Authors: Buie Edward , Scannapieco Evan , Mark Voit G. 
Published: March 2022

Abstract
Absorption-line measurements of the circumgalactic medium (CGM) display a highly nonuniform distribution of lower ionization state species accompanied by more widespread higher ionization state material. This suggests that the CGM is a dynamic, multiphase medium, such as arises in the presence of turbulence. To better understand this evolution, we perform hydrodynamic and magnetohydrodynamic (MHD) simulations of the CGM surrounding Milky Way–like galaxies. In both cases, the CGM is initially in hydrostatic balance in a 1012
M
⊙ dark matter gravitational potential, and the simulations include rotation in the inner halo and turbulence that decreases radially. They also track ionizations, recombinations, and species-by-species radiative cooling in the presence of the redshift-zero UV background, employing the MAIHEM nonequilibrium chemistry package. We find that after 9 Gyr of evolution, the presence of a magnetic field leads to an overall hotter CGM, with cool gas in the center where magnetic pressure dominates. While the non-MHD run produces more cold clouds overall, we find similar Si iv/O vi and N v/O vi ratios between the MHD and non-MHD runs, which are both very different from their equilibrium values. The non-MHD halo develops cool, low angular momentum filaments above the central disk, in comparison to the MHD run that has more efficient angular momentum transport, especially for the cold gas, which forms a more ordered and extended disk late into its evolution.
How Do the Galaxy Stellar Spins Acquire a Peculiar Tidal Connection?
Authors: Lee Jounghun , Moon Jun-Sung , Yoon Suk-Jin 
Published: March 2022

Abstract
We explore how the galaxy stellar spins acquire a peculiar tendency of being aligned with the major principal axes of the local tidal fields, in contrast to their dark matter (DM) counterparts, which tend to be perpendicular to them, regardless of their masses. Analyzing the halo and subhalo catalogs from IllustrisTNG 300 hydrodynamic simulations at z ≤ 1, we determine the cosines of the alignment angles,

cos
α

, between the galaxy stellar and DM spins. Creating four

cos
α

-selected samples of the galaxies and then controlling them to share the same density and mass distributions, we determine the average strengths of the alignments between the galaxy stellar spins and the tidal tensor major axes over each sample. It is clearly shown that at z ≤ 0.5 the more severely the galaxy stellar spin directions deviate from the DM counterparts, the stronger the peculiar tidal alignments become. Taking the ensemble averages of such galaxy properties as central black hole-to-stellar mass ratio, specific star formation rate, formation epoch, stellar-to-total mass ratio, velocity dispersions, average metallicity, and degree of the cosmic web anisotropy over each sample, we also find that all of these properties exhibit either strong correlations or anticorrelations with

cos
α

. Our results imply that the peculiar tidal alignments of the galaxy stellar spins may be caused by anisotropic occurrence of some baryonic process responsible for discharging stellar materials from the galaxies along the tidal major directions at z < 1.
Constraining the CME Core Heating and Energy Budget with SOHO/UVCS
Authors: Wilson Maurice L. , Raymond John C. , Lepri Susan T. , Lionello Roberto , Murphy Nicholas A. , Reeves Katharine K. , Shen Chengcai 
Published: March 2022

Abstract
We describe the energy budget of a coronal mass ejection (CME) observed on 1999 May 17 with the Ultraviolet Coronagraph Spectrometer (UVCS). We constrain the physical properties of the CME’s core material as a function of height along the corona by using the spectra taken by the single-slit coronagraph spectrometer at heliocentric distances of 2.6 and 3.1 solar radii. We use plasma diagnostics from intensity ratios, such as the O vi doublet lines, to determine the velocity, density, temperature, and nonequilibrium ionization states. We find that the CME core’s velocity is approximately 250 km s−1, and its cumulative heating energy is comparable to its kinetic energy for all of the plasma heating parameterizations that we investigated. Therefore, the CME’s unknown heating mechanisms have the energy to significantly affect the CME’s eruption and evolution. To understand which parameters might influence the unknown heating mechanism, we constrain our model heating rates with the observed data and compare them to the rate of heating generated within a similar CME that was constructed by the MAS code’s 3D MHD simulation. The rate of heating from the simulated CME agrees with our observationally constrained heating rates when we assume a quadratic power law to describe a self-similar CME expansion. Furthermore, the heating rates agree when we apply a heating parameterization that accounts for the CME flux rope’s magnetic energy being converted directly into thermal energy. This UVCS analysis serves as a case study for the importance of multislit coronagraph spectrometers for CME studies.
L’animation socioculturelle : émergence et structuration des diplômes comme indicateurs de la professionnalisation
Authors: Bock Cyrille 
Published: March 2022

Les diplômes dans le monde de l’animation socioculturelle sont organisés depuis la fin de la Seconde Guerre mondiale. Ils sont un indicateur pertinent pour analyser le processus de professionnalisation du monde de l’animation. Trois périodes scandent l’émergence et la structuration de l’offre de formation. Trois marqueurs sont mobilisés afin d’éclairer cette professionnalisation : le contexte politique qui définit les fonctions sociales du monde de l’animation, les acteurs en grande partie structurés autour de la jeunesse et de l’éducation populaire et les diplômes en tant que tels.
La féminisation du sport fédéral : une affaire de petites et jeunes filles ?
Authors: Garcia Marie-Carmen , Ottogalli-Mazzacavallo Cécile 
Published: March 2022

Cet article est fondé sur une analyse des données produites par le ministère des sports à partir d’un recensement des licences dans les fédérations sportives françaises par sexe de 2012 à 2017. Il met à l’épreuve l’idée commune selon laquelle les filles se désengageraient du sport fédéral à l’adolescence. Or, proportionnellement, les jeunes filles n’abandonnent pas plus souvent le sport que les jeunes garçons : le différentiel sexué d’engagement dans le sport fédéral se construit durant l’enfance. En outre, les données étudiées montrent que d’une manière générale on assiste, depuis 2012, à une progression constante des licences féminines alors que les licences masculines stagnent ou déclinent. Ainsi, si les filles ne sont guère plus décrocheuses que les garçons à l’adolescence, on peut supposer que leurs socialisations sportives sont aussi, voire plus, consolidées que celles des garçons.