bluuebunny/crossref_metadata_2025_split huggingface dataset:
Penerapan Metode Pembelajaran Two Stay Two Stray Berbasis Peta Konsep Untuk Meningkatkan Hasil Belajar IPA
Authors: Astuti Atik Puji , Hidayati Yulia Maftuhah , Untari Rini 
Published: November 2022

Tujuan penelitian ini untuk mendeskripsikan peningkatan hasil belajar dalam pembelajaran IPA menggunakan metode Two Stay Two Stray berbasis peta konsep pada siswa kelas IV SD Negeri 2 Mriyan. Metode yang digunakan dalam penelitian adalah PTK (Penelitian Tindakan Kelas). Penelitian dilaksanakan dalam dua siklus. Setiap siklus terbagi menjadi empat tahap yaitu tahap perencanaan, tahap pelaksanaan, tahap observasi, dan tahap refleksi. Teknik pengumpulan data dilaksanakan yaitu dengan menggunakan observasi, dokumentasi dan wawancara. Subjek penelitian ini sebanyak 13 orang di kelas IV SDN 2 Mriyan, Kecamatan Tamansari, Kabupaten Boyolali. Teknik analisis data yang dilaksanakan dengan analisis interaktif yaitu reduksi data, penyajian data, dan penarikan kesimpulan. Hasil penelitian ini pada ketuntasan hasil belajar IPA siswa yang tuntas pada data prasiklus sebesar 23,07% dengan rata-rata hasil belajar 60, pada siklus I ketuntasan sebesar 61,38% dengan rata-rata hasil belajar sebesar 73,61, dan pada siklus II ketuntasan sebesar 92,30% dengan rata-rata sebesar 92,07. Maka dapat simpulkan bahwa pembelajaran dengan metode Tow Stay Two Stray berbasis peta konsep dapat meningkatkan hasil belajar IPA.
Peningkatan Keterampilan Menulis Cerpen Melalui Media Flash Card Pada Siswa Kelas IV Sekolah Dasar
Authors: Nurjannah Alfiati Intan , Hidayati Yulia Maftuhah , Samsiyah Siti 
Published: November 2022

Penelituan ini bertujuan untuk mendeskripsikan penggunaan media Flash card untuk meningkatkan keterampilan dalam menulis cerpen pada siswa kelas IV SD Negeri Nglorog 1. Metode yyang digunakan dalam penelitian adalah PTK (Penelitian Tindak Kelas). Penelitian dilaksanakan melalui dua siklus. Setiap siklus terbagi menjadi empat tahap, yaitu tahap perencanaan, tahap pelaksanaan, tahap observasi, dan tahap refleksi. Teknik pengumpulan data dilaksanakan dengan menggunakan observasi, dokumentasi, wawancara, dan angket. Subjek dalam penelitian ini adalah siswa kelas IV yang berjumlah 16. Teknik analisis data dilakukan melalui data kualitatif dan data kuantitatif. Keberhasilan dalam penelitian ini dilihat melalui dua aspek, aspek pertama pada peningkatan yang dilihat melalui proses pembelajaran. Aspek kedua berdasarkan nilai yang diperoleh dari menulis cerpen. Berdasarkan hasil menulis cerpen dari tahap prasiklus hingga siklus dua sebagai berikut: rata-rata yang diperoleh pada prasiklus 55. Rata-rata pada siklus sebesar 68,3. Skor rata-rata yang diperoleh pada sikus 2 sebesar 80. Tiap Aspek penilaian cerpen mengalami peningkatan, meliputi: kelengkapan aspek formal, kelengkapan unsur instrinsik, keterpaduan unsur cerpen, dan kesesuaian penggunaan bahasa cerpen. Berdasarkan data diatas dapat disimpulkan bahwa dengan penggunaan media flash card meningkatkan minat dan hasil menulis cerpen pada siswa kelas IV SD Negeri Nglorog 1.
Metacognition tracks sensitivity following involuntary shifts of visual attention
Authors: Recht Samuel , Mamassian Pascal , de Gardelle Vincent 
Published: November 2022

AbstractSalient, exogenous cues have been shown to induce a temporary boost of perceptual sensitivity in their immediate vicinity. In two experiments involving uninformative exogenous cues presented at various times before a target stimulus, we investigated whether human observers (N = 100) were able to monitor the involuntary increase in performance induced by such transients. We found that an increase of perceptual sensitivity (in a choice task) and encoding precision (in a free-estimation task) occurred approximately 100 ms after cue onset, and was accompanied by an increase in confidence about the perceptual response. These simultaneous changes in sensitivity and confidence resulted in stable metacognition across conditions. These results suggest that metacognition efficiently tracks the effects of a reflexive attentional mechanism known to evade voluntary control, and illustrate a striking ability of high-level cognition to capture fleeting, low-level sensory modulations.
Eurasian guidelines for the prevention and treatment of cardiovascular diseases in patients with obesity (2022)
Authors: Chazova I. E. , Zhernakova Yu. V. , Blinova N. V. , Markova T. N. , Mazurina N. V. , Zhirov I. V. , Uskach T. M. , Safiullina A. A. , Mironova O. Iu. , Elfimova E. M. , Litvin A. Yu. , Zheleznova E. A. , Yuricheva Yu. A. , Azizov V. A. , Grigorenko E. A. , Rahimov Z. Ya. , Kasymova S. D. , Mustafaev I. I. , Narzullaeva A. R. , Polupanov A. G. , Sarybaev A. Sh. , Srozhidinova N. Z. 
Published: November 2022

Disclaimer. The EAC Guidelines represent the views of the EAC, and were produced after careful consideration of the scientific and medical knowledge, and the evidence available at the time of their publication. The EAC is not responsible in the event of any contradiction, discrepancy, and/or ambiguity between the EAC Guidelines and any other official recommendations or guidelines issued by the relevant public health authorities, in particular in relation to good use of healthcare or therapeutic strategies. Health professionals are encouraged to take the EAC Guidelines fully into account when exercising their clinical judgment, as well as in the determination and the implementation of preventive, diagnostic, or therapeutic medical strategies; however, the EAC Guide-lines do not override, in any way whatsoever, the individual responsibility of health professionals to make appropriate and accurate decisions in consideration of each patient’s health condition and in consultation with that patient and, where appropriate and/or necessary, the patient’s caregiver. Nor do the EAC Guidelines exempt health professionals from taking into full and careful consideration the relevant official updated recommendations or guidelines issued by the competent public health authorities, in order to manage each patient’s case in light of the scientifically accepted data pursuant to their respective ethical and professional obligations. It is also the health professional’s responsibility to verify the applicable rules and regulations relating to drugs and medical devices at the time of prescription.
Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Gupta Arvind F. , Luhn Jacob , Wright Jason T. , Mahadevan Suvrath , Ford Eric B. , Stefánsson Guđmundur , Bender Chad F. , Blake Cullen H. , Halverson Samuel , Hearty Fred , Kanodia Shubham , Logsdon Sarah E. , McElwain Michael W. , Ninan Joe P. , Robertson Paul , Roy Arpita , Schwab Christian , Terrien Ryan C. 
Published: November 2022

Abstract
We report the results of observations of p-mode oscillations in the G0 subgiant star HD 35833 in both radial velocities and photometry with NEID and TESS, respectively. We achieve separate, robust detections of the oscillation signal with both instruments (radial velocity amplitude A
RV = 1.11 ± 0.09 m s−1, photometric amplitude A
phot = 6.42 ± 0.60 ppm, frequency of maximum power

ν

max

=
595.71
±
17.28

μHz, and mode spacing Δν = 36.65 ± 0.96 μHz) as well as a nondetection in a TESS sector concurrent with the NEID observations. These data shed light on our ability to mitigate the correlated noise impact of oscillations with radial velocities alone and on the robustness of commonly used asteroseismic scaling relations. The NEID data are used to validate models for the attenuation of oscillation signals for exposure times

t
<

ν

max

−
1

, and we compare our results to predictions from theoretical scaling relations and find that the observed amplitudes are weaker than expected by >4σ, hinting at gaps in the underlying physical models.
A Search for Predicted Astrometric Microlensing Events by Nearby Brown Dwarfs*
Authors: Luberto Judah , Martin Emily C. , McGill Peter , Leauthaud Alexie , Skemer Andrew J. , Lu Jessica R. 
Published: November 2022

Abstract
Gravitational microlensing has the potential to provide direct gravitational masses of single, free-floating brown dwarfs, independent of evolutionary and atmospheric models. The proper motions and parallaxes of nearby brown dwarfs can be used to predict close future alignments with distant background stars that cause a microlensing event. Targeted astrometric follow up of the predicted microlensing events permits the brown dwarf’s mass to be measured. Predicted microlensing events are typically found via searching for a peak threshold signal using an estimate of the lens mass. We develop a novel method that finds predicted events that instead will lead to a target lens-mass precision. The main advantage of our method is that it does not require a lens-mass estimate. We use this method to search for predicted astrometric microlensing events occurring between 2014 and 2032 using a catalog of 1225 low-mass star and brown-dwarf lenses in the Solar Neighborhood of spectral type M6 or later and a background source catalog from DECaLS Data Release 9. The background source catalog extends to g = 23.95, providing a more dense catalog compared to Gaia. Our search did not reveal any upcoming microlensing events. We estimate the rate of astrometric microlensing event for brown dwarfs in the Legacy Survey and find it to be low ∼10−5 yr−1. We recommend carrying out targeted searches for brown dwarfs in front of the Galactic Bulge and Plane to find astrometric microlensing events that will allow the masses of single, free-floating brown dwarfs to be measured.
The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Tamburo Patrick , Muirhead Philip S. , McCarthy Allison M. , Hart Murdock , Vos Johanna M. , Agol Eric , Theissen Christopher , Gracia David , Bardalez Gagliuffi Daniella C. , Faherty Jacqueline 
Published: November 2022

Abstract
We describe a new transit-detection algorithm designed to detect single-transit events in discontinuous Perkins INfrared Exosatellite Survey (PINES) observations of L and T dwarfs. We use this algorithm to search for transits in 131 PINES light curves and identify two transit candidates: 2MASS J18212815+1414010 (2MASS J1821+1414) and 2MASS J08350622+1953050 (2MASS J0835+1953). We disfavor 2MASS J1821+1414 as a genuine transit candidate due to the known variability properties of the source. We cannot rule out the planetary nature of 2MASS J0835+1953's candidate event and perform follow-up observations in an attempt to recover a second transit. A repeat event has yet to be observed, but these observations suggest that target variability is an unlikely cause of the candidate transit. We perform a Markov Chain Monte Carlo simulation of the light curve and estimate a planet radius ranging from

4.2

−
1.6

+
3.5

R

⊕

to

5.8

−
2.1

+
4.8

R

⊕

, depending on the host’s age. Finally, we perform an injection and recovery simulation on our light-curve sample. We inject planets into our data using measured M-dwarf planet occurrence rates and attempt to recover them using our transit-search algorithm. Our detection rates suggest that, assuming M-dwarf planet occurrence rates, we should have roughly a 1% chance of detecting a candidate that could cause the transit depth we observe for 2MASS J0835+1953. If 2MASS J0835+1953 b is confirmed, it would suggest an enhancement in the occurrence of short-period planets around L and T dwarfs in comparison to M dwarfs, which would challenge predictions from planet formation models.
Bridging the Gap—The Disappearance of the Intermediate Period Gap for Fully Convective Stars, Uncovered by New ZTF Rotation Periods
Authors: Lu Yuxi(Lucy) , Curtis Jason L. , Angus Ruth , David Trevor J. , Hattori Soichiro 
Published: November 2022

Abstract
The intermediate period gap, discovered by Kepler, is an observed dearth of stellar rotation periods in the temperature–period diagram at ∼20 days for G dwarfs and up to ∼30 days for early-M dwarfs. However, because Kepler mainly targeted solar-like stars, there is a lack of measured periods for M dwarfs, especially those at the fully convective limit. Therefore it is unclear if the intermediate period gap exists for mid- to late-M dwarfs. Here, we present a period catalog containing 40,553 rotation periods (9535 periods >10 days), measured using the Zwicky Transient Facility (ZTF). To measure these periods, we developed a simple pipeline that improves directly on the ZTF archival light curves and reduces the photometric scatter by 26%, on average. This new catalog spans a range of stellar temperatures that connect samples from Kepler with MEarth, a ground-based time-domain survey of bright M dwarfs, and reveals that the intermediate period gap closes at the theoretically predicted location of the fully convective boundary (G
BP − G
RP ∼ 2.45 mag). This result supports the hypothesis that the gap is caused by core–envelope interactions. Using gyro-kinematic ages, we also find a potential rapid spin-down of stars across this period gap.
The Properties of Fast Yellow Pulsating Supergiants: FYPS Point the Way to Missing Red Supergiants
Authors: Dorn-Wallenstein Trevor Z. , Levesque Emily M. , Davenport James R. A. , Neugent Kathryn F. , Morris Brett M. , Bostroem K. Azalee 
Published: November 2022

Abstract
Fast yellow pulsating supergiants (FYPS) are a recently discovered class of evolved massive pulsators. As candidate supergiant objects, and one of the few classes of pulsating evolved massive stars, these objects have incredible potential to change our understanding of the structure and evolution of massive stars. Here we examine the lightcurves of a sample of 126 cool supergiants in the Magellanic Clouds observed by the Transiting Exoplanet Survey Satellite in order to identify pulsating stars. After making quality cuts and filtering out contaminant objects, we examine the distribution of pulsating stars in the Hertzprung–Russel (HR) diagram, and find that FYPS occupy a region above

log
L

/

L

⊙

≳
5.0

. This luminosity boundary corresponds to stars with initial masses of ∼18–20 M
⊙, consistent with the most massive red supergiant progenitors of supernovae (SNe) II-P, as well as the observed properties of SNe IIb progenitors. This threshold is in agreement with the picture that FYPS are post-RSG stars. Finally, we characterize the behavior of FYPS pulsations as a function of their location in the HR diagram. We find low-frequency pulsations at higher effective temperatures, and higher-frequency pulsations at lower temperatures, with a transition between the two behaviors at intermediate temperatures. The observed properties of FYPS make them fascinating objects for future theoretical study.
A GMOS/IFU Study of Jellyfish Galaxies in Massive Clusters
Authors: Lee Jeong Hwan , Lee Myung Gyoon , Mun Jae Yeon , Cho Brian S. , Kang Jisu 
Published: November 2022

Abstract
Jellyfish galaxies are an intriguing snapshot of galaxies undergoing ram pressure stripping (RPS) in dense environments, showing spectacular star-forming knots in their disks and tails. We study the ionized gas properties of five jellyfish galaxies in massive clusters with Gemini GMOS/Integral Field Unit observations: MACSJ0916-JFG1 (z = 0.330), MACSJ1752-JFG2 (z = 0.353), A2744-F0083 (z = 0.303), MACSJ1258-JFG1 (z = 0.342), and MACSJ1720-JFG1 (z = 0.383). “Baldwin, Phillips, and Terlevich” diagrams show that star formation, active galactic nuclei (AGNs), or mixed effects are ionizing gas in these galaxies. Radial velocity distributions of ionized gas seem to follow disk rotation of galaxies, with the appearance of a few high-velocity components in the tails as a sign of RPS. Mean gas velocity dispersion is lower than 50 km s−1 in most star-forming regions except near AGNs or shock-heated regions, indicating that the ionized gas is dynamically cold. Integrated star formation rates (SFRs) of these galaxies range from 7 M
⊙ yr−1 to 35 M
⊙ yr−1, and the tail SFRs are from 0.6 M
⊙ yr−1 to 16 M
⊙ yr−1, which are much higher than those of other jellyfish galaxies in the local universe. These high SFR values imply that RPS triggers intense star formation activity in these extreme jellyfish galaxies. The phase-space diagrams demonstrate that the jellyfish galaxies with higher stellar masses and higher host cluster velocity dispersion are likely to have more enhanced star formation activity. The jellyfish galaxies in this study have similar gas kinematics and dynamical states to those in the local universe, but they show a much higher SFR.
Charting Galactic Accelerations with Stellar Streams and Machine Learning
Authors: Nibauer Jacob , Belokurov Vasily , Cranmer Miles , Goodman Jeremy , Ho Shirley 
Published: November 2022

Abstract
We present a data-driven method for reconstructing the galactic acceleration field from phase-space (position and velocity) measurements of stellar streams. Our approach is based on a flexible and differentiable fit to the stream in phase-space, enabling a direct estimate of the acceleration vector along the stream. Reconstruction of the local acceleration field can be applied independently to each of several streams, allowing us to sample the acceleration field due to the underlying galactic potential across a range of scales. Our approach is methodologically different from previous works, as a model for the gravitational potential does not need to be adopted beforehand. Instead, our flexible neural-network-based model treats the stream as a collection of orbits with a locally similar mixture of energies, rather than assuming that the stream delineates a single stellar orbit. Accordingly, our approach allows for distinct regions of the stream to have different mean energies, as is the case for real stellar streams. Once the acceleration vector is sampled along the stream, standard analytic models for the galactic potential can then be rapidly constrained. We find our method recovers the correct parameters for a ground-truth triaxial logarithmic halo potential when applied to simulated stellar streams. Alternatively, we demonstrate that a flexible potential can be constrained with a neural network, and standard multipole expansions can also be constrained. Our approach is applicable to simple and complicated gravitational potentials alike and enables potential reconstruction from a fully data-driven standpoint using measurements of slowly phase-mixing tidal debris.
Change of Rankine–Hugoniot Relations during Postshock Relaxation of Anisotropic Distributions
Authors: Gedalin Michael , Golan Michal , Pogorelov Nikolai V. , Roytershteyn Vadim 
Published: November 2022

Abstract
Collisionless shocks channel the energy of the directed plasma flow into the heating of the plasma species and magnetic field enhancement. The kinetic processes at the shock transition cause the ion distributions just behind the shock to be nongyrotropic. Gyrotropization and subsequent isotropization occur at different spatial scales. Accordingly, for a given upstream plasma and magnetic field state, there would be different downstream states corresponding to the anisotropic and isotropic regions. Thus, at least two sets of Rankine–Hugoniot relations are needed, in general, to describe the connection of the downstream measurable parameters to the upstream ones. We establish the relation between the two sets.
Perfecting Our Set of Spectrophotometric Standard DA White Dwarfs
Authors: Calamida Annalisa , Matheson Thomas , Olszewski Edward W. , Saha Abhijit , Axelrod Tim , Shanahan Clare , Holberg Jay , Points Sean , Narayan Gautham , Malanchev Konstantin , Ridden-Harper Ryan , Gentile-Fusillo Nicola , Raddi Roberto , Bohlin Ralph , Rest Armin , Hubeny Ivan , Deustua Susana , Mackenty John , Sabbi Elena , Stubbs Christopher W. 
Published: November 2022

Abstract
We verified for photometric stability a set of DA white dwarfs with Hubble Space Telescope magnitudes from the near-ultraviolet to the near-infrared and ground-based spectroscopy by using time-spaced observations from the Las Cumbres Observatory network of telescopes. The initial list of 38 stars was whittled to 32 final ones, which comprise a high-quality set of spectrophotometric standards. These stars are homogeneously distributed around the sky and are all fainter than r ∼ 16.5 mag. Their distribution is such that at least two of them would be available to be observed from any observatory on the ground at any time at airmass less than 2. Light curves and different variability indices from the Las Cumbres Observatory data were used to determine the stability of the candidate standards. When available, Pan-STARRS1, Zwicky Transient Facility, and TESS data were also used to confirm the star classification. Our analysis showed that four DA white dwarfs may exhibit evidence of photometric variability, while a fifth is cooler than our established lower temperature limit, and a sixth star might be a binary. In some instances, due to the presence of faint nearby red sources, care should be used when observing a few of the spectrophotometric standards with ground-based telescopes. Light curves and finding charts for all the stars are provided.
Constraining the Origin of Stellar Binary Black Hole Mergers by Detections of Their Lensed Host Galaxies and Gravitational Wave Signals
Authors: Chen Zhiwei , Lu Youjun , Zhao Yuetong 
Published: November 2022

Abstract
A significant number of stellar binary black hole (sBBH) mergers may be lensed and detected by the third generation of gravitational wave (GW) detectors. Their lensed host galaxies may be detectable, which would thus help to accurately localize these sources and provide a new approach to study the origin of sBBHs. In this paper, we investigate the detectability of lensed host galaxies for lensed sBBH mergers. We find that the detection fraction of galaxies hosting lensed GW events can be significantly different for a survey with a given limiting magnitude if sBBHs are produced by different mechanisms, such as the evolution of massive binary stars, dynamical interactions in dense star clusters, and production assisted by active galactic nuclei or massive black holes. Furthermore, we illustrate that the statistical spatial distributions of those lensed sBBHs in their hosts resulting from different sBBH formation channels can differ. Therefore, with the third generation of GW detectors and future large-scale galaxy surveys, it is possible to independently constrain the origin of sBBHs via the detection fraction of those lensed events with identifiable lensing host signatures and/or even to constrain the fractional contributions from different sBBH formation mechanisms.
Modeling Redshift-space Clustering with Abundance Matching
Authors: DeRose Joseph , Becker Matthew R. , Wechsler Risa H. 
Published: November 2022

Abstract
We explore the degrees of freedom required to jointly fit projected and redshift-space clustering of galaxies selected in three bins of stellar mass from the Sloan Digital Sky Survey Main Galaxy Sample (SDSS MGS) using a subhalo abundance matching (SHAM) model. We employ emulators for relevant clustering statistics in order to facilitate our analysis, leading to large speed gains with minimal loss of accuracy. We are able to simultaneously fit the projected and redshift-space clustering of the two most massive galaxy samples that we consider with just two free parameters: scatter in stellar mass at fixed SHAM proxy, and the dependence of the SHAM proxy on dark matter halo concentration. We find some evidence for models that include velocity bias, but including orphan galaxies improves our fits to the lower-mass samples significantly. We also model the clustering signals of specific star formation rate (sSFR) selected samples using conditional abundance matching (CAM). We obtain acceptable fits to projected and redshift-space clustering as a function of sSFR and stellar mass using two CAM variants, although the fits are worse than for stellar-mass-selected samples alone. By incorporating nonunity correlations between the CAM proxy and sSFR, we are able to resolve previously identified discrepancies between CAM predictions and SDSS observations of the environmental dependence of quenching for isolated central galaxies.