bluuebunny/crossref_metadata_2025_split huggingface dataset:
MOTIVATION OF CHILDREN'S HEALTH SCREENING VOLUNTEERS AT PUSKESMAS CIPTOMULYO AND MULYOREJO, MALANG CITY
Authors: Ispriantari Aloysia , Priasmoro Dian Pitaloka 
Published: April 2022

In 2019, Children's Health Screening was held because there is volunteers from universities in Malang City. This volunteers motivation needs to be concerned because it is requires a lot of energy and time. The study was to determine the motivation of volunteers for School Children's Health Screening at Puskesmas Ciptomulyo and Mulyorejo. Respondents are volunteers for health screening at Puskesmas Ciptomulyo and Mulyorejo with total respondents are 34 respondents. Data was collected using “The Volunteer Functions Inventory” instrument. Data presented in descriptive and then used the unpaired t-test for analysis. The result is most of them (97.1%) of respondents had high motivation and the rest of them (2.9%) had moderate motivation. The factor of motivation that affect volunteers as following: understanding, career development, self-enrichment, personal value, self-protection and social factors. In addition, there is no difference in the motivation of volunteers based on the years of college education. Based on the results of this study, we suggest that academic institution prepare students to improve their clinical skills and motivate students to take part in volunteer activities in the community. Keywords: Motivation, Volunteers, School Children’s Health Screening
Conditions and possibilities of using Baltic amber heritage in the development of territorial cooperation
Authors: Studzieniecki Tomasz 
Published: April 2022

Baltic amber, also referred to as the “gold of the Baltic Sea”, is one of the most valuable fossil resins in the world. Due to its valuable properties, it has been the subject of international cooperation and exchange since ancient times. Then numerous trade routes were laid, which gradually turned into tourist attractions. Nowadays, amber contributes to the development of cities and regions where it is mined and processed. This gives them a competitive advantage, creates a positive image and stimulates territorial cooperation. The essence of this cooperation lies in the use of the socio-economic capital of interested parties connected by common interests. Representatives of the world of science, business and non-governmental organizations participate in this cooperation.
An example of the effective use of amber and its heritage in activities that stimulate territorial development is Pomeranian Voivodeship with its capital in Gdańsk. The article analyses the activities in this area carried out since 1996 by two non-governmental organizations: the Agencja Rozwoju Regionalnego Foundation (Agency for Regional Development) and the association Academia Europa Nostra. The study was conducted using of secondary sources, including the resources of both organizations and the knowledge of the author, the initiator and coordinator of numerous initiatives related to the heritage of amber.
A Pluto–Charon Sonata IV. Improved Constraints on the Dynamical Behavior and Masses of the Small Satellites
Authors: Kenyon Scott J. , Bromley Benjamin C. 
Published: April 2022

Abstract
We discuss a new set of ∼500 numerical n-body calculations designed to constrain the masses and bulk densities of Styx, Nix, Kerberos, and Hydra. Comparisons of different techniques for deriving the semimajor axis and eccentricity of the four satellites favor methods relying on the theory of Lee & Peale, where satellite orbits are derived in the context of the restricted three-body problem (Pluto, Charon, and one massless satellite). In each simulation, we adopt the nominal satellite masses derived in Kenyon & Bromley, multiply the mass of at least one satellite by a numerical factor f ≥ 1, and establish whether the system ejects at least one satellite on a timescale ≤4.5 Gyr. When the total system mass is large (f ≫ 1), ejections of Kerberos are more common. Systems with lower satellite masses (f ≈ 1) usually eject Styx. In these calculations, Styx often “signals” an ejection by moving to higher orbital inclination long before ejection; Kerberos rarely signals in a useful way. The n-body results suggest that Styx and Kerberos are more likely to have bulk densities comparable with water ice, ρ
SK ≲ 2 g cm−3, than with rock. A strong upper limit on the total system mass, M
SNKH ≲ 9.5 × 1019 g, also places robust constraints on the average bulk density of the four satellites, ρ
SNKH ≲ 1.4 g cm−3. These limits support models where the satellites grow out of icy material ejected during a major impact on Pluto or Charon.
Relativistic Description of Dense Matter Equation of State and Compatibility with Neutron Star Observables: A Bayesian Approach
Authors: Malik Tuhin , Ferreira Márcio , Agrawal B. K. , Providência Constança 
Published: April 2022

Abstract
The general behavior of the nuclear equation of state (EOS), relevant for the description of neutron stars (NSs), is studied within a Bayesian approach applied to a set of models based on a density-dependent relativistic mean-field description of nuclear matter. The EOS is subjected to a minimal number of constraints based on nuclear saturation properties and the low-density pure neutron matter EOS obtained from a precise next-to-next-to-next-to-leading order (N3LO) calculation in chiral effective field theory (χEFT). The posterior distributions of the model parameters obtained under these minimal constraints are employed to construct the distributions of various nuclear matter properties and NS properties such as radii, tidal deformabilities, central energy densities, speeds of sound, etc. We found that a 90% confidence interval for the allowed NS mass–radius relationship and tidal deformabilities is compatible with GW170817 and recent Neutron star Interior Composition ExploreR observations, without invoking the exotic degrees of freedom. A central speed of sound of the order of

2

/

3

c is obtained. The maximum NS mass allowed by the model is 2.5 M
⊙.
Massive Young Stellar Objects in the Galactic Center. II. Seeing Through the Ice-rich Envelopes
Authors: Jang Dajeong , An Deokkeun , Sellgren Kris , Ramírez Solange V. , Boogert A. C. Adwin , Schultheis Mathias 
Published: April 2022

Abstract
To study the demographics of interstellar ices in the Central Molecular Zone (CMZ) of the Milky Way, we obtain near-infrared spectra of 109 red point sources using NASA IRTF/SpeX at Maunakea. We select the sample from near- and mid-infrared photometry, including 12 objects in the previous paper of this series, to ensure that these sources trace a large amount of absorption through clouds in each line of sight. We find that most of the sample (100 objects) show CO band-head absorption at 2.3 μm, tagging them as red (super-) giants. Despite the photospheric signature, however, a fraction of the sample with L-band spectra (9/82 = 0.11) exhibit large H2O ice column densities (N > 2 × 1018 cm−2), and six of them also reveal CH3OH ice absorption. As one of such objects is identified as a young stellar object (YSO) in our previous work, these ice-rich sight lines are likely associated with background stars in projection to an extended envelope of a YSO or a dense cloud core. The low frequency of such objects in the early stage of stellar evolution implies a low star-formation rate (≲0.02 M
⊙ yr−1), reinforcing the previous claim on the suppressed star-formation activity in the CMZ. Our data also indicate that the strong “shoulder” CO2 ice absorption at 15.4 μm observed in YSO candidates in the previous paper arises from CH3OH-rich ice grains having a large CO2 concentration [N(CO2)/N(CH3OH) ≈ 1/3].
SpeX Near-infrared Spectroscopic Extinction Curves in the Milky Way
Authors: Decleir Marjorie , Gordon Karl D. , Andrews Jennifer E. , Clayton Geoffrey C. , Cushing Michael C. , Misselt Karl A. , Pendleton Yvonne , Rayner John , Vacca William D. , Whittet D. C. B. 
Published: April 2022

Abstract
Interstellar dust extinction curves provide valuable information about dust properties, including the composition and size of the dust grains, and are essential to correct observations for the effects of interstellar dust. In this work, we measure a representative sample of near-infrared (NIR; 0.8–5.5 μm) spectroscopic extinction curves for the first time, enabling us to investigate the extinction at wavelengths where it is usually only measured in broad photometric bands. We use IRTF/SpeX spectra of a sample of reddened and comparison stars to measure 15 extinction curves with the pair method. Our sample spans A(V) values from 0.78 to 5.65 and R(V) values from 2.43 to 5.33. We confirm that the NIR extinction curves are well fit by a power law, with indices and amplitudes differing from sight line to sight line. Our average diffuse NIR extinction curve can be represented by a single power law with index α = 1.7, but because of the sight line-to-sight line variations, the shape of any average curve will depend on the parental sample. We find that most of the variation in our sample can be linked to the ratio of total-to-selective extinction R(V), a rough measurement of the average dust grain size. Two sight lines in our sample clearly show the ice extinction feature at 3 μm, which can be fitted by a modified Drude profile. We find tentative ice detections with slightly over 3σ significance in two other sight lines. In our average diffuse extinction curve, we measure a 3σ upper limit of A(ice)/A(V) = 0.0021 for this ice feature.
Wave-optical Effects in the Microlensing of Continuous Gravitational Waves by Star Clusters
Authors: Suvorov Arthur G. 
Published: April 2022

Abstract
Rapidly rotating neutron stars are promising sources for existing and upcoming gravitational-wave interferometers. While relatively dim, these systems are expected to emit continuously, allowing for signal to be accumulated through persistent monitoring over year-long timescales. If, at some point during the observational window, the source comes to lie behind a dense collection of stars, transient gravitational lensing may occur. Such events, though rare, would modulate the waveform, induce phase drifts, and ultimately affect parameter inferences concerning the nuclear equation of state and/or magnetic field structure of the neutron star. Importantly, the radiation wavelength will typically exceed the Schwarzschild radius of the individual perturbers in this scenario, implying that (micro)lensing occurs in the diffractive regime, where geometric optics does not apply. In this paper, we make use of numerical tools that borrow from Picard–Lefschetz theory to efficiently evaluate the relevant Fresnel–Kirchhoff integrals for n ≳ 102 microlenses. Modulated strain profiles are constructed both in general and for particular neutron star trajectories relative to some simulated macrolenses.
The Curious Case of ASASSN-20hx: A Slowly Evolving, UV- and X-Ray-Luminous, Ambiguous Nuclear Transient
Authors: Hinkle Jason T. , Holoien Thomas W.-S. , Shappee Benjamin. J. , Neustadt Jack M. M. , Auchettl Katie , Vallely Patrick J. , Shahbandeh Melissa , Kluge Matthias , Kochanek Christopher S. , Stanek K. Z. , Huber Mark E. , Post Richard S. , Bersier David , Ashall Christopher , Tucker Michael A. , Williams Jonathan P. , de Jaeger Thomas , Do Aaron , Fausnaugh Michael , Gruen Daniel , Hopp Ulrich , Myles Justin , Obermeier Christian , Payne Anna V. , Thompson Todd A. 
Published: April 2022

Abstract
We present observations of ASASSN-20hx, a nearby ambiguous nuclear transient (ANT) discovered in NGC 6297 by the All-Sky Automated Survey for Supernovae (ASAS-SN). We observed ASASSN-20hx from −30 to 275 days relative to the peak UV/optical emission using high-cadence, multiwavelength spectroscopy and photometry. From Transiting Exoplanet Survey Satellite data, we determine that the ANT began to brighten on 2020 June 22.8 with a linear rise in flux for at least the first week. ASASSN-20hx peaked in the UV/optical 30 days later on 2020 July 22.8 (MJD = 59052.8) at a bolometric luminosity of L = (3.15 ± 0.04) × 1043 erg s−1. The subsequent decline is slower than any TDE observed to date and consistent with many other ANTs. Compared to an archival X-ray detection, the X-ray luminosity of ASASSN-20hx increased by an order of magnitude to L

x
∼ 1.5 × 1042 erg s−1 and then slowly declined over time. The X-ray emission is well fit by a power law with a photon index of Γ ∼ 2.3–2.6. Both the optical and near-infrared spectra of ASASSN-20hx lack emission lines, unusual for any known class of nuclear transient. While ASASSN-20hx has some characteristics seen in both tidal disruption events and active galactic nuclei, it cannot be definitively classified with current data.
A Highly Settled Disk around Oph163131
Authors: Villenave M. , Stapelfeldt K. R. , Duchêne G. , Ménard F. , Lambrechts M. , Sierra A. , Flores C. , Dent W. R. F. , Wolff S. , Ribas Á. , Benisty M. , Cuello N. , Pinte C. 
Published: April 2022

Abstract
High dust density in the midplane of protoplanetary disks is favorable for efficient grain growth and can allow fast formation of planetesimals and planets, before disks dissipate. Vertical settling and dust trapping in pressure maxima are two mechanisms allowing dust to concentrate in geometrically thin and high-density regions. In this work, we aim to study these mechanisms in the highly inclined protoplanetary disk SSTC2D J163131.2-242627 (Oph 163131, i ∼ 84°). We present new high-angular-resolution continuum and 12CO ALMA observations of Oph 163131. The gas emission appears significantly more extended in the vertical and radial direction compared to the dust emission, consistent with vertical settling and possibly radial drift. In addition, the new continuum observations reveal two clear rings. The outer ring, located at ∼100 au, is well-resolved in the observations, allowing us to put stringent constraints on the vertical extent of millimeter dust particles. We model the disk using radiative transfer and find that the scale height of millimeter-sized grains is 0.5 au or less at 100 au from the central star. This value is about one order of magnitude smaller than the scale height of smaller micron-sized dust grains constrained by previous modeling, which implies that efficient settling of the large grains is occurring in the disk. When adopting a parametric dust settling prescription, we find that the observations are consistent with a turbulent viscosity coefficient of about α ≲ 10−5 at 100 au. Finally, we find that the thin dust scale height measured in Oph 163131 is favorable for planetary growth by pebble accretion: a 10 M
E planet may grow within less than 10 Myr, even in orbits exceeding 50 au.
Rotation Distributions around the Kraft Break with TESS and Kepler: The Influences of Age, Metallicity, and Binarity
Authors: Avallone Ellis A. , Tayar Jamie N. , van Saders Jennifer L. , Berger Travis A. , Claytor Zachary R. , Beaton Rachael L. , Teske Johanna , Godoy-Rivera Diego , Pan Kaike 
Published: April 2022

Abstract
Stellar rotation is a complex function of mass, metallicity, and age and can be altered by binarity. To understand the importance of these parameters in main-sequence stars, we have assembled a sample of observations that spans a range of these parameters using a combination of observations from The Transiting Exoplanet Survey Satellite (TESS) and the Kepler Space Telescope. We find that while we can measure rotation periods and identify other classes of stellar variability (e.g., pulsations) from TESS light curves, instrument systematics prevent the detection of rotation signals longer than the TESS orbital period of 13.7 days. Due to this detection limit, we also use rotation periods constrained using rotational velocities measured by the APOGEE spectroscopic survey and radii estimated using the Gaia mission for both TESS and Kepler stars. From these rotation periods, we (1) find we can track rotational evolution along discrete mass tracks as a function of stellar age, (2) find we are unable to recover trends between rotation and metallicity that were observed by previous studies, and (3) note that our sample reveals that wide binary companions do not affect rotation, while close binary companions cause stars to exhibit more rapid rotation than single stars.
First Observation of the MeV Gamma-Ray Universe with Bijective Imaging Spectroscopy Using the Electron-tracking Compton Telescope on Board SMILE-2+
Authors: Takada Atsushi , Takemura Taito , Yoshikawa Kei , Mizumura Yoshitaka , Ikeda Tomonori , Nakamura Yuta , Onozaka Ken , Abe Mitsuru , Hamaguchi Kenji , Kubo Hidetoshi , Kurosawa Shunsuke , Miuchi Kentaro , Saito Kaname , Sawano Tatsuya , Tanimori Toru 
Published: April 2022

Abstract
MeV gamma-rays provide a unique window for the direct measurement of line emissions from radioisotopes, but observations have made little significant progress since COMPTEL on board the Compton Gamma-ray Observatory (CGRO). To observe celestial objects in this band, we are developing an electron-tracking Compton camera (ETCC) that realizes both bijective imaging spectroscopy and efficient background reduction gleaned from the recoil-electron track information. The energy spectrum of the observation target can then be obtained by a simple ON–OFF method using a correctly defined point-spread function on the celestial sphere. The performance of celestial object observations was validated on the second balloon SMILE-2+ , on which an ETCC with a gaseous electron tracker was installed that had a volume of 30 × 30 × 30 cm3. Gamma-rays from the Crab Nebula were detected with a significance of 4.0σ in the energy range 0.15–2.1 MeV with a live time of 5.1 hr, as expected before launch. Additionally, the light curve clarified an enhancement of gamma-ray events generated in the Galactic center region, indicating that a significant proportion of the final remaining events are cosmic gamma-rays. Independently, the observed intensity and time variation were consistent with the prelaunch estimates except in the Galactic center region. The estimates were based on the total background of extragalactic diffuse, atmospheric, and instrumental gamma-rays after accounting for the variations in the atmospheric depth and rigidity during the level flight. The Crab results and light curve strongly support our understanding of both the detection sensitivity and the background in real observations. This work promises significant advances in MeV gamma-ray astronomy.
Detection of Extended Millimeter Emission in the Host Galaxy of 3C 273 and Its Implications for QSO Feedback via High Dynamic Range ALMA Imaging
Authors: Komugi Shinya , Toba Yoshiki , Matsuoka Yoshiki , Saito Toshiki , Yamashita Takuji 
Published: April 2022

Abstract
We estimate the amount of negative feedback energy injected into the interstellar medium (ISM) of the host galaxy of 3C 273, a prototypical radio-loud quasar. We obtained 93, 233, and 343 GHz continuum images with the Atacama Large Millimeter/submillimeter Array (ALMA). After self-calibration and point-source subtraction, we reach an image dynamic range of ∼85,000 at 93 GHz, ∼39,000 at 233 GHz, and ∼2500 at 343 GHz. These are currently the highest image dynamic range obtained using ALMA. We detect spatially extended millimeter emission associated with the host galaxy, cospatial with the extended emission line region (EELR) observed in the optical. The millimeter spectral energy distribution and comparison with centimeter data show that the extended emission cannot be explained by dust thermal emission or synchrotron or thermal bremsstrahlung arising from massive star formation. We interpret the extended millimeter emission as thermal bremsstrahlung from gas directly ionized by the central source. The extended flux indicates that at least ∼7% of the bolometric flux of the nuclear source was used to ionize atomic hydrogen in the host galaxy. The ionized gas is estimated to be as massive as 1010–1011
M
⊙, but the molecular gas fraction with respect to the stellar mass is consistent with other ellipticals, suggesting that direct ionization ISM by the QSO may not be sufficient to suppress star formation, or we are witnessing a short timescale before negative feedback becomes observable. The discovery of a radio counterpart to EELRs provides a new pathway to studying the QSO–host ISM interaction.
Infrared Spectroscopic Survey of the Quiescent Medium of Nearby Clouds. II. Ice Formation and Grain Growth in Perseus and Serpens
Authors: Madden M. C. L. , Boogert A. C. A. , Chiar J. E. , Knez C. , Pendleton Y. J. , Tielens A. G. G. M. , Yip A. 
Published: April 2022

Abstract
The properties of dust change during the transition from diffuse to dense clouds as a result of ice formation and dust coagulation, but much is still unclear about this transformation. We present 2–20 μm spectra of 49 field stars behind the Perseus and Serpens Molecular Clouds and establish relationships between the near-infrared continuum extinction (A
K) and the depths of the 9.7 μm silicate (τ
9.7) and 3.0 μm H2O ice (τ
3.0) absorption bands. The τ
9.7/A
K ratio varies from large, diffuse interstellar medium-like values (∼0.55), to much lower ratios (∼0.26). Above extinctions of A
K ∼ 1.2 (A
V ∼ 10; Perseus, Lupus, dense cores) and ∼2.0 (A
V ∼ 17; Serpens), the τ
9.7/A
K ratio is lowest. The τ
9.7/A
K reduction from diffuse to dense clouds is consistent with a moderate degree of grain growth (sizes up to ∼0.5 μm), increasing the near-infrared color excess (and thus A
K), but not affecting the ice and silicate band profiles. This grain growth process seems to be related to the ice column densities and dense core formation thresholds, highlighting the importance of density. After correction for Serpens foreground extinction, the H2O ice formation threshold is in the range of A
K = 0.31–0.40 (A
V = 2.6–3.4) for all clouds, and thus grain growth takes place after the ices are formed. Finally, abundant CH3OH ice (∼21% relative to H2O) is reported for 2MASSJ18285266+0028242 (Serpens), a factor of >4 larger than for the other targets.
Serge Moscovici dans sa vie. Une marginalité centrale
Authors: Dibie Pascal 
Published: April 2022

Serge Moscovici dans sa vie. Une marginalité centrale Entre les années 1970 et 1980 s’est opéré dans les sciences humaines un tournant éthique indiscutable. Dans le secteur de la psychologie et de l’ethnologie, et plus particulièrement dans le sillage de Serge Moscovici et Robert Jaulin, occupant une marginalité centrale au sein de l’université, s’opérait un changement de l’approche de notre rapport au politique et à la nature. Un nouvel ordre critique s’instaurait qui allait bouleverser la façon d’appréhender le monde et ses problèmes. Dans le même temps où monte le souci de l’identité et des civilisations, le colonialisme est mis en accusation et la question naturelle devient la question centrale.
Hermès
Authors: Rouane Sihem , Azzam Jamal Eddine , Pezé Stéphan 
Published: April 2022

Cette étude de cas aborde les sujets relatifs aux stratégies corporate et plus précisément les voies de développement (croissance horizontale et verticale) et les modes de développement (croissance organique, externe et relationnelle) d’une entreprise, souvent mobilisés en Management Stratégique de façon isolée ou alternative. La conduite stratégique de la maison du luxe Hermès traite ces différents concepts et illustre un « pattern » de développement stratégique complexe qui combine à la fois la croissance horizontale (diversification), la croissance verticale (intégration amont et aval) et l’exploitation de synergies de ressources et compétences et les synergies commerciales émergentes.