bluuebunny/crossref_metadata_2025_split huggingface dataset:
AGN STORM 2. I. First results: A Change in the Weather of Mrk 817
Authors: Kara Erin , Mehdipour Missagh , Kriss Gerard A. , Cackett Edward M. , Arav Nahum , Barth Aaron J. , Byun Doyee , Brotherton Michael S. , De Rosa Gisella , Gelbord Jonathan , Hernández Santisteban Juan V. , Hu Chen , Kaastra Jelle , Landt Hermine , Li Yan-Rong , Miller Jake A. , Montano John , Partington Ethan , Aceituno Jesús , Bai Jin-Ming , Bao Dongwei , Bentz Misty C. , Brink Thomas G. , Chelouche Doron , Chen Yong-Jie , Colmenero Encarni Romero , Bontà Elena Dalla , Dehghanian Maryam , Du Pu , Edelson Rick , Ferland Gary J. , Ferrarese Laura , Fian Carina , Filippenko Alexei V. , Fischer Travis , Goad Michael R. , González Buitrago Diego H. , Gorjian Varoujan , Grier Catherine J. , Guo Wei-Jian , Hall Patrick B. , Ho Luis C. , Homayouni Y. , Horne Keith , Ilić Dragana , Jiang Bo-Wei , Joner Michael D. , Kaspi Shai , Kochanek Christopher S. , Korista Kirk T. , Kynoch Daniel , Li Sha-Sha , Liu Jun-Rong , M. cHardy Ian M. , McLane Jacob N. , Mitchell Jake A. J. , Netzer Hagai , Olson Kianna A. , Pogge Richard W. , Popović Luka C̆. , Proga Daniel , Storchi-Bergmann Thaisa , Strasburger Erika , Treu Tommaso , Vestergaard Marianne , Wang Jian-Min , Ward Martin J. , Waters Tim , Williams Peter R. , Yang Sen , Yao Zhu-Heng , Zastrocky Theodora E. , Zhai Shuo , Zu Ying 
Published: November 2021

Abstract
We present the first results from the ongoing, intensive, multiwavelength monitoring program of the luminous Seyfert 1 galaxy Mrk 817. While this active galactic nucleus was, in part, selected for its historically unobscured nature, we discovered that the X-ray spectrum is highly absorbed, and there are new blueshifted, broad, and narrow UV absorption lines, which suggest that a dust-free, ionized obscurer located at the inner broad-line region partially covers the central source. Despite the obscuration, we measure UV and optical continuum reverberation lags consistent with a centrally illuminated Shakura–Sunyaev thin accretion disk, and measure reverberation lags associated with the optical broad-line region, as expected. However, in the first 55 days of the campaign, when the obscuration was becoming most extreme, we observe a de-coupling of the UV continuum and the UV broad emission-line variability. The correlation recovered in the next 42 days of the campaign, as Mrk 817 entered a less obscured state. The short C iv and Lyα lags suggest that the accretion disk extends beyond the UV broad-line region.
Detection of Substructures in Young Transition Disk WL 17
Authors: Gulick Hannah C. , Sadavoy Sarah , Matrà Luca , Sheehan Patrick , van der Marel Nienke 
Published: November 2021

Abstract
WL 17 is a young transition disk in the Ophiuchus L1688 molecular cloud complex. Even though WL 17 is among the brightest disks in L1688 and massive enough to expect dust self-scattering, it was undetected in polarization down to Atacama Large Millimeter/submillimeter Array’s (ALMA’s) instrument sensitivity limit. Such low polarization fractions could indicate unresolved polarization within the beam or optically thin dust emission. We test the latter case by combining the high-sensitivity 233 GHz Stokes I data from the polarization observations with previous ALMA data at 345 and 100 GHz. We use simple geometric shapes to fit the observed disk visibilities in each band. Using our simple models and assumed dust temperature profiles, we estimate the optical depth in all three bands. The optical depth at 233 GHz peaks at τ
233 ∼ 0.3, which suggests the dust emission may not be optically thick enough for dust self-scattering to be efficient. We also find the higher-sensitivity 233 GHz data show substructure in the disk for the first time. The substructure appears as brighter lobes along the major axis, on either side of the star. We attempt to fit the lobes with a simple geometric model, but they are unresolved in the 233 GHz data. We propose that the disk may be flared at 1 mm such that there is a higher column of dust along the major axis than the minor axis when viewed at an inclination. These observations highlight the strength of high-sensitivity continuum data from dust polarization observations to study disk structures.
Effects of Anisotropy on Strongly Magnetized Neutron and Strange Quark Stars in General Relativity
Authors: Deb Debabrata , Mukhopadhyay Banibrata , Weber Fridolin 
Published: November 2021

Abstract
We investigate the properties of anisotropic, spherically symmetric compact stars, especially neutron stars (NSs) and strange quark stars (SQSs), made of strongly magnetized matter. The NSs are described by the SLy equation of state (EOS) and the SQSs by an EOS based on the MIT Bag model. The stellar models are based on an a priori assumed density dependence of the magnetic field and thus anisotropy. Our study shows that not only the presence of a strong magnetic field and anisotropy, but also the orientation of the magnetic field itself, have an important influence on the physical properties of stars. Two possible magnetic field orientations are considered: a radial orientation where the local magnetic fields point in the radial direction, and a transverse orientation, where the local magnetic fields are perpendicular to the radial direction. Interestingly, we find that for a transverse orientation of the magnetic field, the stars become more massive with increasing anisotropy and magnetic-field strength and increase in size since the repulsive, effective anisotropic force increases in this case. In the case of a radially oriented magnetic field, however, the masses and radii of the stars decrease with increasing magnetic-field strength because of the decreasing effective anisotropic force. Importantly, we also show that in order to achieve hydrostatic equilibrium configurations of magnetized matter, it is essential to account for both the local anisotropy effects as well as the anisotropy effects caused by a strong magnetic field. Otherwise, hydrostatic equilibrium is not achieved for magnetized stellar models.
Successive H-atom Addition to Solid OCS on Compact Amorphous Solid Water
Authors: Nguyen Thanh , Oba Yasuhiro , Sameera W. M. C. , Kouchi Akira , Watanabe Naoki 
Published: November 2021

Abstract
Carbonyl sulfide (OCS) is an abundant sulfur (S)-bearing species in the interstellar medium. It is present not only in the gas phase, but also on interstellar grains as a solid; therefore, OCS very likely undergoes physicochemical processes on icy surfaces at very low temperatures. The present study experimentally and computationally investigates the reaction of solid OCS with hydrogen (H) atoms on amorphous solid water at low temperatures. The results show that the addition of H to OCS proceeds via quantum tunneling, and further addition of H leads to the formation of carbon monoxide (CO), hydrogen sulfide (H2S), formaldehyde (H2CO), methanol (CH3OH), and thioformic acid (HC(O)SH). These experimental results are explained by our quantum chemical calculations, which demonstrate that the initial addition of H to the S atom of OCS is the most predominant, leading to the formation of OCS-H radicals. Once the formed OCS-H radical is stabilized on ice, further addition of H to the S atom yields CO and H2S, while that to the C atom yields HC(O)SH. We have also confirmed, in a separate experiment, the HC(O)SH formation by the HCO reactions with the SH radicals. The present results would have an important implication for the recent detection of HC(O)SH toward G+0.693–0.027.
Most “Young” α-rich Stars Have High Masses but are Actually Old
Authors: Zhang Meng , Xiang Maosheng , Zhang Hua-Wei , Ting Yuan-Sen , Rix Hans-Walter , Wu Ya-Qian , Huang Yang , Sun Wei-Xiang , Tian Zhi-Jia , Wang Chun , Liu Xiao-Wei 
Published: November 2021

Abstract
Recent observations have revealed a population of α-element abundances, enhanced giant stars with unexpected high masses (≳1 M
⊙) from asteroseismic analysis and spectroscopy. Assuming single-star evolution, their masses imply young ages (τ < 6 Gyr) incompatible with the canonical Galactic chemical evolution scenario. Here we study the chemistry and kinematics of a large sample of such α-rich, high-mass red giant branch (RGB) stars drawn from the LAMOST spectroscopic surveys. Using LAMOST and Gaia, we found these stars share the same kinematics as the canonical high-α old stellar population in the Galactic thick disk. The stellar abundances show that these high-α massive stars have α- and iron-peak element abundances similar to those of the high-α old thick-disk stars. However, a portion of them exhibit higher [(N+C)/Fe] and [Ba/Fe] ratios, which implies they have gained C- and Ba-rich materials from extra sources, presumably asymptotic giant branch (AGB) companions. The results support the previous suggestion that these RGB stars are products of binary evolution. Their high masses thus mimic “young” single stars, yet in fact they belong to an intrinsic old stellar population. To fully explain the stellar abundance patterns of our sample stars, a variety of binary evolution channels, such as main-sequence (MS) + RGB, MS + AGB, RGB + RGB, and RGB + AGB, are required, pointing to diverse formation mechanisms of these seemly rejuvenated cannibals. With this larger sample, our results confirm earlier findings that most, if not all, α-rich stars in the Galactic disk seem to be old.
Rotation Curves in z ∼ 1–2 Star-forming Disks: Comparison of Dark Matter Fractions and Disk Properties for Different Fitting Methods
Authors: Price S. H. , Shimizu T. T. , Genzel R. , Übler H. , Förster Schreiber N. M. , Tacconi L. J. , Davies R. I. , Coogan R. T. , Lutz D. , Wuyts S. , Wisnioski E. , Nestor A. , Sternberg A. , Burkert A. , Bender R. , Contursi A. , Davies R. L. , Herrera-Camus R. , Lee M.-J. , Naab T. , Neri R. , Renzini A. , Saglia R. , Schruba A. , Schuster K. 
Published: November 2021

Abstract
We present a follow-up analysis examining the dynamics and structures of 41 massive, large star-forming galaxies at z ∼ 0.67 − 2.45 using both ionized and molecular gas kinematics. We fit the galaxy dynamics with models consisting of a bulge, a thick, turbulent disk, and an NFW dark matter halo, using code that fully forward-models the kinematics, including all observational and instrumental effects. We explore the parameter space using Markov Chain Monte Carlo (MCMC) sampling, including priors based on stellar and gas masses and disk sizes. We fit the full sample using extracted 1D kinematic profiles. For a subset of 14 well-resolved galaxies, we also fit the 2D kinematics. The MCMC approach robustly confirms the results from least-squares fitting presented in Paper I: the sample galaxies tend to be baryon-rich on galactic scales (within one effective radius). The 1D and 2D MCMC results are also in good agreement for the subset, demonstrating that much of the galaxy dynamical information is captured along the major axis. The 2D kinematics are more affected by the presence of noncircular motions, which we illustrate by constructing a toy model with constant inflow for one galaxy that exhibits residual signatures consistent with radial motions. This analysis, together with results from Paper I and other studies, strengthens the finding that massive, star-forming galaxies at z ∼ 1 − 2 are baryon-dominated on galactic scales, with lower dark matter fractions toward higher baryonic surface densities. Finally, we present details of the kinematic fitting code used in this analysis.
Asteroseismological Analysis of the DAV HS 0507+0434B: The Influence of Chemical Profile on the Pulsation Periods
Authors: Guifang Lin , Jie Su , Yan Li , Jianning Fu 
Published: November 2021

Abstract
Asteroseismology is a powerful tool to infer the details of the inner chemical structure of white dwarfs. Using the nine observed frequencies of HS 0507+0434B, we explore the influence of the inner chemical profile on the pulsation periods. Based on the evolutionary C/O profile, we modify slightly the C/O core profile and make an asteroseismic analysis for HS 0507+0434B. We find that the trapped mode with the period of 445.3 s is mainly affected by the hydrogen and helium mass fraction. The inner C/O core profile has an influence on all modes extending into the inner core. When we use the iteration method with the optimal C/O core profile, the fit between the theoretical periods and observed ones is significantly improved. For the best-fitting model with the optimal parametric C/O core, there is a smaller C/O ratio and a smaller overshooting zone in the stellar interior. The fundamental parameters of the model with the optimal C/O core are M
*/M
⊙ ∼ 0.710 ± 0.005, T
eff ∼ 12570 ± 106K,

log

M

H

/

M

*

∼
−
8.01
±
0.08

, and

log

M

He

/

M

*

∼
−
2.51
±
0.08

.
Constraining Cosmic Microwave Background Temperature Evolution With Sunyaev–Zel’Dovich Galaxy Clusters from the Atacama Cosmology Telescope
Authors: Li 李 Yunyang 云炀 , Hincks Adam D. , Amodeo Stefania , Battistelli Elia S. , Bond J. Richard , Calabrese Erminia , Choi Steve K. , Devlin Mark J. , Dunkley Jo , Ferraro Simone , Gluscevic Vera , Guan Yilun , Halpern Mark , Hilton Matt , Hlozek Renee , Marriage Tobias A. , McMahon Jeff , Moodley Kavilan , Naess Sigurd , Nati Federico , Niemack Michael D. , Orlowski-Scherer John , Page Lyman , Partridge Bruce , Salatino Maria , Schaan Emmanuel , Schillaci Alessandro , Sehgal Neelima , Sifón Cristóbal , Staggs Suzanne T. , van Engelen Alexander , Wollack Edward J. , Xu Zhilei 
Published: November 2021

Abstract
The Sunyaev–Zel’dovich (SZ) effect introduces a specific distortion of the blackbody spectrum of the cosmic microwave background (CMB) radiation when it scatters off hot gas in clusters of galaxies. The frequency dependence of the distortion is only independent of the cluster redshift when the evolution of the CMB radiation is adiabatic. Using 370 clusters within the redshift range 0.07 ≲ z ≲ 1.4 from the largest SZ-selected cluster sample to date from the Atacama Cosmology Telescope, we provide new constraints on the deviation of CMB temperature evolution from the standard model

α
=

0.017

−
0.032

+
0.029

, where

T
(
z
)
=

T

0

1
+
z

1
−
α

. This result is consistent with no deviation from the standard adiabatic model. Combining it with previous, independent data sets we obtain a joint constraint of α = −0.001 ± 0.012. Attributing deviation from adiabaticity to the decay of dark energy, this result constrains its effective equation of state

w

eff

=
−

0.998

−
0.010

+
0.008

.
Multiple Electron Acceleration Instances during a Series of Solar Microflares Observed Simultaneously at X-Rays and Microwaves
Authors: Battaglia Marina , Sharma Rohit , Luo 骆 Yingjie 英杰 , Chen 陈 Bin 彬 , Yu 余 Sijie 思捷 , Krucker Säm 
Published: November 2021

Abstract
Even small solar flares can display a surprising level of complexity regarding their morphology and temporal evolution. Many of their properties, such as energy release and electron acceleration can be studied using highly complementary observations at X-ray and radio wavelengths. We present X-ray observations from the Reuven Ramaty High Energy Solar Spectroscopic Imager and radio observations from the Karl G. Jansky Very Large Array (VLA) of a series of GOES A3.4–B1.6 class flares observed on 2013 April 23. The flares, as seen in X-ray and extreme ultraviolet, originated from multiple locations within active region NOAA 11726. A veritable zoo of different radio emissions between 1 GHz and 2 GHz was observed cotemporally with the X-ray flares. In addition to broadband continuum emission, broadband short-lived bursts and narrowband spikes, indicative of accelerated electrons, were observed. However, these sources were located up to 150″ away from the flaring X-ray sources but only some of these emissions could be explained as signatures of electrons that were accelerated near the main flare site. For other sources, no obvious magnetic connection to the main flare site could be found. These emissions likely originate from secondary acceleration sites triggered by the flare, but may be due to reconnection and acceleration completely unrelated to the cotemporally observed flare. Thanks to the extremely high sensitivity of the VLA, not achieved with current X-ray instrumentation, it is shown that particle acceleration happens frequently and at multiple locations within a flaring active region.
Long-term dynamics of the abundance of earthworms and enchytraeids (Annelida, Clitellata: Lumbricidae, Enchytraeidae) in forests of the Central Urals, Russia
Authors: Vorobeichik Evgenii , Nesterkov Alexey , Golovanova Elena , Nesterkova Dina , Ermakov Alexander , Grebennikov Maxim 
Published: November 2021

Since the late 1980s, long-term monitoring of terrestrial ecosystems in metal-contaminated areas has been carried out in the Central Urals. As a part of these monitoring programmes, the data on soil macroinvertebrates in undisturbed areas as reference sites continues to be gathered. These data help study the local biodiversity and long-term dynamics of soil macroinvertebrate abundance in non-polluted areas.The dataset (available from the GBIF network at https://www.gbif.org/dataset/bf5bc7f6-71a3-4abd-8abc-861ee3cbf84a) includes information from a long-term monitoring programme for two taxa of Annelids, Lumbricidae and Enchytraeidae, which dwell in the topsoil of spruce-fir, birch, pine and floodplain forests in the Central Urals. The dataset includes information on the earthworm community structure (list of species, species abundance, number of egg cocoons, cocoon exuvia, juveniles and adults) and enchytraeid abundance. The dataset consists of 553 sampling events (= samples, corresponding to upper and lower layers of the soil monoliths) and 12739 occurrences (earthworms, mainly identified to species and earthworm cocoons and enchytraeids, identified to family) collected during 1990–1991, 2004, 2014–2016 and 2018–2020. In total, 3305 individuals of earthworms were collected, representing ten (out of twelve) species and all eight genera recorded for the fauna of the Central Urals. In addition, 7292 earthworm egg cocoons and cocoon exuvia and 6926 individuals of enchytraeids were accumulated. The presence-absence data on each of the ten earthworm species, egg cocoons, cocoon exuvia and enchytraeids are provided for each sampling event. All data were collected in undisturbed non-polluted areas and are used as a local reference for ecotoxicological monitoring. The dataset provides valuable information for estimating the composition and abundance of earthworm communities in different habitats over a long time and contributes to the study of soil fauna biodiversity in the Urals.
Identité et image de marque employeur des Big Four : entre différences et indifférence
Authors: Guillot-Soulez Chloé , Chastenet Édouard 
Published: November 2021

Le concept de marque employeur renvoie à l’ensemble des bénéfices qui permettent de définir une entreprise en tant qu’employeur et d’identifier ce qui la rend désirable et différente des autres employeurs pour attirer et retenir les ressources humaines. Cette recherche se centre sur l’analyse de la marque employeur des Big Four (Deloitte, EY, KPMG, PwC). Ces quatre grands cabinets d’audit et de conseil ont chaque année besoin d’attirer de nouveaux collaborateurs, pour la plupart des jeunes diplômés issus des grandes écoles et des universités. Cette recherche questionne et analyse la capacité de ces quatre entreprises à définir une marque employeur différenciée dans une perspective d’attractivité des ressources humaines potentielles. À partir de l’analyse des sites Internet de recrutement des Big Four et d’une enquête par questionnaires menée auprès d’étudiants en comptabilité/finance, cette recherche propose une analyse comparée de l’identité et de l’image de marque employeur des Big Four. Il ressort que si les quatre cabinets essaient de se différencier lorsqu’ils communiquent leur identité de marque employeur sur les pages « carrières » de leurs sites Internet au niveau des bénéfices valorisés, ces éléments de différenciation ne sont que marginalement perçus par les ressources humaines potentielles qui ont une image peu différenciée des bénéfices de la marque employeur de ces quatre entreprises. Cette recherche dévoile ainsi une situation archétypale inédite où la valorisation d’une promesse d’emploi unique constitue un véritable défi pour la gestion de la marque employeur dans la mesure où celle-ci relève davantage de l’image commune des Big Four en tant que groupe d’entreprises que de celles des entreprises elles-mêmes.
Les enjeux de la religion et de la religiosité au travail
Authors: Honoré Lionel 
Published: November 2021

La spiritualité au travail est de plus en plus acceptée et encouragée. La limite que fixent les entreprises est souvent celle de la religion. Le salarié qui s’investit personnellement dans son travail et l’activité de l’entreprise peut amener sa spiritualité au travail sauf si elle est religieuse. Comment expliquer ces phénomènes ? Quels sens pouvons-nous leur donner ? Quels en sont les enjeux pour les salariés, les entreprises, la performance ? Cet article se propose d’apporter des réponses à ces questions en s’appuyant sur l’analyse une revue de la littérature consacrée à la spiritualité et la religion au travail. Il propose notamment un travail de définition des concepts centraux (religion, religiosité) et d’analyse des manières respectives dont ils permettent de problématiser la question de la diversité. Pour cela deux formes de diversité (intrinsèque et extrinsèque) sont différenciées.
Les tarificateurs des conseils départementaux aux prises avec les instruments d’action publique : le cas des EHPAD
Authors: Xing-Bongioanni Jingyue 
Published: November 2021

Fondé sur une enquête ethnographique en immersion au sein d’une collectivité territoriale, cet article étudie les indicateurs et outils standardisés pour la tarification des Ehpad conçus et mis en place par une équipe de tarificateurs travaillant dans un conseil départemental, ainsi que la rétroaction de ces outils sur ce même groupe professionnel. L’article montre que la mise en œuvre d’outils et indicateurs standardisés « faits maison » a non seulement pour effet de normaliser la production des services dans les Ehpad, mais également de transformer les rapports entre le groupe des tarificateurs et d’autres groupes professionnels de l’administration publique locale en jouant un rôle majeur dans leur quête de reconnaissance institutionnelle et professionnelle.
Comment émerge un indice boursier ? Histoire du BEL 20
Authors: Duterme Tom 
Published: November 2021

Cet article retrace l’émergence du principal indice boursier belge (BEL 20), à travers une revue des autres indices qui ont, tout au long du xx e siècle, fait autorité à la Bourse de Bruxelles. L’étude des méthodologies mobilisées et des publics représentés met au jour la variété des significations – tant cognitives que politiques – que peut cristalliser un indice boursier, mais aussi les raisons du succès du BEL 20 dans cette lutte entre « conventions financières ».