bluuebunny/crossref_metadata_2025_split huggingface dataset:
How typology shapes the constructional network: Denominal verb constructions in English, Dutch and German
Authors: Van Goethem Kristel , Koutsoukos Nikos 
Published: April 2022

This study proposes a cross-linguistic, corpus-based, and constructionist analysis of denominal verbs (DNVs) in English, Dutch and German. DNV constructions include various morphological construction types, such as conversion (e.g. English bottle > to bottle), prefixation (e.g. Dutch arm 'arm' > omarmen 'to embrace') and suffixation (e.g. German Katapult 'catapult' > katapultieren 'to catapult'). We investigate the correlation between the distribution of DNV constructions and the typological properties of the languages, focusing on boundary permeability, inflectional complexity, syntactic configurationality and word-class assignment. The study shows that, although the three languages have the same repertoire of DNV constructions at their disposal, a Germanic cline can be detected in their preferences for non-overt vs overt marking of the word-class change. As such, the study highlights the impact of typological factors on the shape of language-specific constructional networks.

Dieser Beitrag ist ursprünglich im Peter-Lang-Verlag erschienen (https://www.ingentaconnect.com/contentone/plg/jwf/2022/00000006/00000001/art00001)
Online Learning Review of English Language Teaching in SMK N 8 Purworejo
Authors: Indi Indiana Surya Pratiwi , Sukarni Semi , Ngafif Abdul 
Published: April 2022

This research aims to find out students’ perception on online learning of English subject during Covid-19 pandemic at SMK N 8 Purworejo. The researchers collected the data through a questionnaire and interviews. There were 72 students of 12th grade at SMK N 8 Purworejo participated in this research. This research used mixed method approach combined qualitative and quantitative approaches. Descriptive analysis was used to analyze data from questionnaire and thematic analysis was used to analyze data from interview. The result of this research shows that 12th grade students of SMK N 8 Purworejo have “medium” perception toward the implementation of online learning during Covid-19 pandemic. The mean score of the questionnaire was 3.21 that lays on the range between 2.60 – 3.39 which can be interpreted in the “Medium” category. Besides, there were several difficulties faced by students and teachers. This difficulties, such as the bad signal or internet connection, the lack of variation on online learning methods and media platform in online learning, and the lack of interaction that occurs during online learning between students and teachers, and students with students. These difficulties make online learning becomes less effective.
Review on the clinical pharmacist's role in reducing medication errors
Authors: Mujeeb  , P Narayana swamy , P Venkatesh 
Published: April 2022

Introduction: Dispensing errors are believed to be the most prevalent type of medical error and are a significant cause of preventable adverse events. Aim and Objective: The aim of this study are to discuss the underlying factors in dispensing errors, health care uncertainty and therapeutic outcomes, and to identify the extent of human- and system-based sources of errors by exploring hospital pharmacists’ attitudes and dispositions to die and uncertainties; and the implications for patient safety in a tertiary hospital. Methodology: A cross-sectional survey of clinical pharmacists in secondary care hospital in Guntur was conducted over a period of 6 months from July 2021 to Dec 2021. A stratified random sample of 64 patient’s data was collected. These study was conducted in our patients department. Results: Out of 64 patients 34(54%) patients were male and 30(46%)patients were female. 41% patients were comes in the age range of 41-60 years .most of the errors(32) were observed in general medicine only. these errors are gradually decreased from July to Dec. Conclusion: In conclusion, majority of hospital pharmacists indicated that the risk of dispensing errors was increasing and most of them were aware of dispensing errors. the profession needs to be proactive and standards must be set appropriately high (i.e. zero error tolerance) clinical pharmacist must communicate with physicians , nursing staff and other hospital pharmacist thereby we can minimize the errors.
Revisiting WASP-47 with ESPRESSO and TESS
Authors: Bryant Edward M. , Bayliss Daniel 
Published: April 2022

Abstract
WASP-47 hosts a remarkable planetary system containing a hot Jupiter (WASP-47 b; P = 4.159 days) with an inner super-Earth (WASP-47 e; P = 0.7896 days), a close-orbiting outer Neptune (WASP-47 d; P = 9.031 days), and a long-period giant planet (WASP-47 c; P = 588.4 days). We use the new Transiting Exoplanet Survey Satellite (TESS) photometry to refine the orbital ephemerides of the transiting planets in the system, particularly the hot Jupiter WASP-47 b, for which we find an update equating to a 17.4 minute shift in the transit time. We report new radial-velocity measurements from the Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations (ESPRESSO) spectrograph for WASP-47, which we use to refine the masses of WASP-47 d and WASP-47 e, with a high-cadence observing strategy aimed to focus on the super-Earth WASP-47 e. We detect a periodic modulation in the K2 photometry that corresponds to a 32.5 ± 3.9 day stellar rotation, and find further stellar activity signals in our ESPRESSO data consistent with this rotation period. For WASP-47 e we measure a mass of 6.77 ± 0.57 M
⊕ and a bulk density of 6.29 ± 0.60 g cm−3, giving WASP-47 e the second most precisely measured density to date of any super-Earth. The mass and radius of WASP-47 e, combined with the exotic configuration of the planetary system, suggest the WASP-47 system formed through a mechanism different to systems with multiple small planets or more typical isolated hot Jupiters.
Is A2261 a Fossil Galaxy Cluster in a Transitional Dynamical State?
Authors: Kim Hyowon , Ko Jongwan , Smith Rory , Kim Jae-Woo , Hwang Ho Seong , Song Hyunmi , Shin Jihye , Yoo Jaewon 
Published: April 2022

Abstract
Fossil cluster A2261 is well studied, but previous studies give contradictory results on its dynamical states, such as its X-ray central entropy and magnitude gap. To improve our understanding of its dynamical state, we conduct multiobject spectroscopic observations with Hectospec on the MMT, covering an area out to 5 virial radii from the cluster center, and get improved completeness and membership. Using these new data, we calculate multiple dynamical indicators, including Gaussianity, distance offset, and velocity offset. These indicators suggest that A2261 is moderately relaxed. However, a Dressler–Shectman test reveals a group candidate to the south at a projected distance that is near the virial radius and overlaps with an X-ray tail-like feature. One of the galaxies associated with that group would be sufficiently bright to reduce the fossil magnitude gap. This raises the possibility that A2261 could have recently transited in fossil status, if the group had previously crossed the cluster and is only now found outside. In the cluster outskirts, we see an extended feature of galaxies located on the opposite side of the cluster from the group candidate. On even larger scales, we find that this feature connects, both on the sky and in velocity space, with a long (4.4 Mpc) filamentary structure in the Sloan Digital Sky Survey data. This could support the idea that a group was fed into the cluster through the filament, temporarily breaking the fossil status and resulting in a minor merger that weakly disturbed the intracluster medium of the cluster.
Extreme Variation in Star Formation Efficiency across a Compact, Starburst Disk Galaxy
Authors: Fisher D. B. , Bolatto A. D. , Glazebrook K. , Obreschkow D. , Abraham R. G. , Kacprzak G. G. , Nielsen N. M. 
Published: April 2022

Abstract
We report on the internal distribution of star formation efficiency in IRAS 08339+6517 (hereafter IRAS08), using ∼200 pc resolution CO(2 − 1) observations from NOEMA. The molecular gas depletion time changes by 2 orders-of-magnitude from disk-like values in the outer parts to less than 108 yr inside the half-light radius. This translates to a star formation efficiency per freefall time that also changes by 2 orders-of-magnitude, reaching 50%–100%, different than local spiral galaxies and the typical assumption of constant, low star formation efficiencies. Our target is a compact, massive disk galaxy that has a star formation rate 10× above the z = 0 main sequence; Toomre Q ≈ 0.5−0.7 and high gas velocity dispersion (σ
mol ≈ 25 km s−1). We find that IRAS08 is similar to other rotating, starburst galaxies from the literature in the resolved

Σ

SFR

∝

Σ

mol

N

relation. By combining resolved literature studies we find that the distance from the main sequence is a strong indicator of the Kennicutt-Schmidt power-law slope, with slopes of N ≈ 1.6 for starbursts from 100 to 104
M
⊙ pc−2. Our target is consistent with a scenario in which violent disk instabilities drive rapid inflows of gas. It has low values of Toomre-Q, and also at all radii, the inflow timescale of the gas is less than the depletion time, which is consistent with the flat metallicity gradients in IRAS08. We consider these results in light of popular star formation theories; in general observations of IRAS08 find the most tension with theories in which star formation efficiency is a constant. Our results argue for the need of high-spatial-resolution CO observations for a larger number of similar targets.
The Origin of the Unfocused XMM-Newton Background, Its Variability, and Lessons Learned for ATHENA
Authors: Gastaldello Fabio , Marelli Martino , Molendi Silvano , Bartalucci Iacopo , Kühl Patrick , Grant Catherine E. , Ghizzardi Simona , Rossetti Mariachiara , De Luca Andrea , Tiengo Andrea 
Published: April 2022

Abstract
We analyzed the unexposed to the sky (outFOV) region of the MOS2 detector on board XMM-Newton covering 15 yr of data amounting to 255 Ms. We show convincing evidence that the origin of the unfocused background in XMM-Newton is due to energetic protons, electrons, and hard X-ray photons. Galactic cosmic rays are the main contributors as shown by the tight correlation (2.6% of total scatter) with the 1 GeV proton data of the SOHO EPHIN detector. Tight correlations are found with a proxy of the Chandra background rate, revealing the common source of background for detectors in similar orbits, and with the data of the EPIC Radiation Monitor, only when excluding Solar energetic particle events. The entrance to the outer electron belts is associated with a sudden increase in the outFOV MOS2 rate and a spectral change. These facts support the fact that MeV electrons can generate an unfocused background signal. The correlation between MOS2 outFOV data and the SOHO EPHIN data reveals a term constant in time and isotropic, similar to the one found in the study of the pn data. The most plausible origin of this component is hard unfocused X-ray photons of the cosmic X-ray background Compton scattering in the detector as supported by the strength of the signal in the two detectors with different thicknesses. Based on this physical understanding, a particle radiation monitor on board the Advanced Telescope for High Energy Astrophysics has been proposed and it is currently under study. It will be able to track different species with the necessary accuracy and precision to guarantee the challenging requirement of 2% reproducibility of the background.
Population Properties of Gravitational-wave Neutron Star–Black Hole Mergers
Authors: Zhu Jin-Ping , Wu Shichao , Qin Ying , Zhang Bing , Gao He , Cao Zhoujian 
Published: April 2022

Abstract
Over the course of the third observing run of the LIGO–Virgo–KAGRA Collaboration, several gravitational-wave (GW) neutron star–black hole (NSBH) candidates have been announced. By assuming that these candidates are real signals with astrophysical origins, we analyze the population properties of the mass and spin distributions for GW NSBH mergers. We find that the primary BH mass distribution of NSBH systems, whose shape is consistent with that inferred from the GW binary BH (BBH) primaries, can be well described as a power law with an index of

α
=

4.8

−
2.8

+
4.5

plus a high-mass Gaussian component peaking at

∼

33

−
9

+
14

M

⊙

. The NS mass spectrum could be shaped as a nearly flat distribution between ∼1.0 and 2.1 M
⊙. The constrained NS maximum mass agrees with that inferred from NSs in our Galaxy. If GW190814 and GW200210 are NSBH mergers, the posterior results of the NS maximum mass would be always larger than ∼2.5 M
⊙ and significantly deviate from that inferred in Galactic NSs. The effective inspiral spin and effective precession spin of GW NSBH mergers are measured to potentially have near-zero distributions. The negligible spins for GW NSBH mergers imply that most events in the universe should be plunging events, which support the standard isolated formation channel of NSBH binaries. More NSBH mergers to be discovered in the fourth observing run would help to more precisely model the population properties of cosmological NSBH mergers.
Exploring the Hubble Tension and Spatial Curvature from the Ages of Old Astrophysical Objects
Authors: Wei Jun-Jie , Melia Fulvio 
Published: April 2022

Abstract
We use the age measurements of 114 old astrophysical objects (OAO) in the redshift range 0 ≲ z ≲ 8 to explore the Hubble tension. The age of the universe at any z is inversely proportional to the Hubble constant, H
0, so requiring the universe to be older than the OAO it contains at any z will lead to an upper limit on H
0. Assuming flat ΛCDM and setting a Gaussian prior on the matter density parameter Ωm = 0.315 ± 0.007 informed by Planck, we obtain a 95% confidence level upper limit of H
0 < 70.6 km s−1 Mpc−1, representing a 2σ tension with the measurement using the local distance ladder. We find, however, that the inferred upper limit on H
0 depends quite sensitively on the prior for Ωm, and the Hubble tension between early-time and local measurements of H
0 may be due in part to the inference of both Ωm and H
0 in Planck, while the local measurement uses only H
0. The age-redshift data may also be used for cosmological model comparisons. We find that the R
h = ct universe accounts well for the data, with a reasonable upper limit on H
0, while Einstein–de Sitter fails to pass the cosmic-age test. Finally, we present a model-independent estimate of the spatial curvature using the ages of 61 galaxies and the luminosity distances of 1048 Pantheon Type Ia supernovae. This analysis suggests that the geometry of the universe is marginally consistent with spatial flatness at a confidence level of 1.6σ, characterized as

Ω

k

=

0.43

−
0.27

+
0.27

.
Prospects for kSZ2–Galaxy Cross-correlations during Reionization
Authors: La Plante Paul , Sipple Jackson , Lidz Adam 
Published: April 2022

Abstract
We explore a new approach for extracting reionization-era contributions to the kinetic Sunyaev–Zel’dovich (kSZ) effect. Our method utilizes the cross-power spectrum between filtered and squared maps of the cosmic microwave background (CMB) and photometric galaxy surveys during the Epoch of Reionization (EoR). This kSZ2–galaxy cross-power spectrum statistic has been successfully detected at lower redshifts (z ≲ 1.5). Here we extend this method to z ≳ 6 as a potential means to extract signatures of patchy reionization. We model the expected signal across multiple photometric redshift bins using seminumeric simulations of the reionization process. In principle, the cross-correlation statistic robustly extracts reionization-era contributions to the kSZ signal, while its redshift evolution yields valuable information regarding the timing of reionization. Specifically, the model cross-correlation signal near ℓ ∼ 1000 peaks during the early stages of the EoR, when about 20% of the volume of the universe is ionized. Detectable ℓ modes mainly reflect squeezed-triangle configurations of the related bispectrum, quantifying correlations between the galaxy overdensity field on large scales and the smaller-scale kSZ power. We forecast the prospects for detecting this signal using future wide-field samples of Lyman-break galaxies from the Roman Space Telescope and next-generation CMB surveys including the Simons Observatory, CMB-S4, and CMB-HD. We find that a roughly 13σ detection is possible for CMB-HD and Roman after summing over all ℓ modes. We discuss the possibilities for improving this approach and related statistics, with the aim of moving beyond simple detections to measure the scale and redshift dependence of the cross-correlation signals.
Mechanism of the Failed Eruption of an Intermediate Solar Filament
Authors: Peng Zou , Chaowei Jiang , Juntao Wang , Xinkai Bian 
Published: April 2022

Abstract
Solar filament eruptions can generate coronal mass ejections (CMEs), which are huge threats to space weather. Thus, we need to understand their underlying mechanisms. Although many authors have studied the mechanisms for several decades, we still do not fully understand in what conditions a filament can erupt to become a CME or not. Previous studies have discussed extensively why a highly twisted and already erupted filament will be interrupted and considered that a strong overlying constraint field seems to be the key factor. However, few of them study filaments in the weak field, namely, quiescent filaments, as it is too hard to reconstruct the magnetic configuration there. Here we show a case study, in which we can fully reconstruct the configuration of an intermediate filament with the MHD-relaxation extrapolation model and discuss its initial eruption and eventual failure. By analyzing the magnetic configuration, we suggest that the reconnection between the erupting magnetic flux rope (MFR) and the overlying field are the key factors that constrained the eruption of the filament. There is observational evidence that MFRs will reconnect with peripheral field lines. Usually, the reconnection between an MFR and peripheral fields will weaken the overlying constraint and promote further eruption, but in some cases in which the magnetic configuration of an MFR is far different from peripheral fields, the reconnection will play a negative role in MFR eruption.
Hubble Space Telescope Imaging of Luminous Extragalactic Infrared Transients and Variables from the Spitzer Infrared Intensive Transients Survey*
Authors: Bond Howard E. , Jencson Jacob E. , Whitelock Patricia A. , Adams Scott M. , Bally John , Cody Ann Marie , Gehrz Robert D. , Kasliwal Mansi M. , Masci Frank J. 
Published: April 2022

Abstract
The SPitzer InfraRed Intensive Transients Survey (SPIRITS) searched for luminous infrared (IR) transients and variables in nearly 200 nearby galaxies from 2014 to 2019, using the warm Spitzer telescope at 3.6 and 4.5 μm. Among the SPIRITS variables are IR-bright objects that are undetected in ground-based optical surveys. We classify them as (1) transients, (2) periodic variables, and (3) irregular variables. The transients include eSPecially Red Intermediate-luminosity Transient Events (SPRITEs), having maximum luminosities fainter than supernovae, red IR colors, and a wide range of outburst durations (days to years). Here we report deep optical and near-IR imaging with the Hubble Space Telescope (HST) of 21 SPIRITS variables. They were initially considered SPRITE transients, but many eventually proved instead to be periodic or irregular variables as more data were collected. HST images show most of these cool and dusty variables are associated with star-forming regions in late-type galaxies, implying an origin in massive stars. Two SPRITEs lacked optical progenitors in deep preoutburst HST images; however, one was detected during eruption at J and H, indicating a dusty object with an effective temperature of ∼1050 K. One faint SPRITE turned out to be a dusty classical nova. About half the HST targets proved to be periodic variables, with pulsation periods of 670–2160 days; they are likely dusty asymptotic-giant-branch (AGB) stars with masses of ∼5–10 M
⊙. A few of them were warm enough to be detected in deep HST frames, but most are too cool. Out of six irregular variables, two were red supergiants with optical counterparts in HST images; four were too enshrouded for HST detection.
Variation in Cosmic-Ray Intensity Lags Sunspot Number: Implications of Late Opening of Solar Magnetic Field
Authors: Wang Yuming , Guo Jingnan , Li Gang , Roussos Elias , Zhao Junwei 
Published: April 2022

Abstract
Galactic cosmic rays (GCRs), the highly energetic particles that may raise critical health issues for astronauts in space, are modulated by solar activity, with their intensity lagging behind the variation in sunspot number (SSN) by about one year. Previously, this lag has been attributed to the combined effect of outward convecting solar wind and inward propagating GCRs. However, the lag’s amplitude and its solar-cycle dependence are still not fully understood. By investigating the solar surface magnetic field, we find that the source of heliospheric magnetic field—the open magnetic flux on the Sun—already lags behind SSN before it convects into the heliosphere along with the solar wind. The delay during odd cycles is longer than that during sequential even cycles. Thus, we propose that the GCR lag is primarily due to the very late opening of the solar magnetic field with respect to SSN, though solar wind convection and particle transport in the heliosphere also matter. We further investigate the origin of the open flux from different latitudes of the Sun and find that the total open flux is significantly contributed by that from low latitudes, where coronal mass ejections frequently occur and also show an odd–even cyclic pattern. Our findings challenge existing theories, and may serve as the physical basis of long-term forecasts of radiation dose estimates for manned deep-space exploration missions.
The 3D Dust and Opacity Distribution of Protoplanets in Multifluid Global Simulations
Authors: Krapp Leonardo , Kratter Kaitlin M. , Youdin Andrew N. 
Published: April 2022

Abstract
The abundance and distribution of solids inside the Hill sphere are central to our understanding of the giant planet dichotomy. Here, we present a 3D characterization of the dust density, mass flux, and mean opacities in the envelope of subthermal and superthermal-mass planets. We simulate the dynamics of multiple dust species in a global protoplanetary disk model accounting for dust feedback. We find that the meridional flows do not effectively stir dust grains at scales of the Bondi sphere. Thus the dust settling driven by the stellar gravitational potential sets the latitudinal dust density gradient within the planet envelope. Not only does the planet’s potential enhance this gradient, but also the spiral wakes serve as another source of asymmetry. These asymmetries substantially alter the inferred mean Rosseland and Planck opacities. In cases with moderate-to-strong dust settling, the opacity gradient can range from a few percent to more than two orders of magnitude between the midplane and the polar regions of the Bondi sphere. Finally, we show that this strong latitudinal opacity gradient can introduce a transition between optically thick and thin regimes at the scales of the planet envelope. We suggest that this transition is likely to occur when the equilibrium scale height of hundred-micron-sized particles is smaller than the Hill radius of the forming planet. This work calls into question the adoption of a constant opacity derived from well-mixed distributions and demonstrates the need for global radiation hydrodynamics models of giant planet formation that account for dust dynamics.