bluuebunny/crossref_metadata_2025_split huggingface dataset:
ANALISIS PERAN AKREDITASI SEKOLAH DALAM UPAYA MENINGKATKAN MUTU PENDIDIKAN DI SDN KARANGTUMARITIS
Authors: Lestari Yunita Dewi , Jumiyanah Siti , Putri Salma Anindya , Jamaludin Ujang , Setiawan Sigit 
Published: June 2023

ABSTRACT
This study aims to describe: sources of information related to SDN Karangtumaritis Accreditation. Researchers examine related 1) the impact of good accreditation activities for schools, 2) what needs to be prepared when going to conduct an assessment of schools or accreditation assessments, 3) what are the eligibility criteria for accreditation given to schools, and 4) factors influencing the school accreditation process. The informant in this study was the Principal of SDN Karangtumaritis. This research uses a type of descriptive qualitative research which aims to describe the characteristics of the phenomenon with a narrative description. Methods of data collection in this study using observation, interviews and documentation. After obtaining the data, the researcher used the Milles and Huberman model to carry out data analysis activities, through three stages, namely: data reduction, data presentation, and drawing conclusions.

Keywords: School Accreditation; School Eligibility; Education Quality

ABSTRAK
Penelitian ini bertujuan untuk mendeskripsikan: sumber informasi yang berkaitan dengan Akreditasi Sekolah SDN Karangtumaritis. Peneliti mengkaji terkait 1) dampak dari kegiatan akreditasi baik bagi sekolah, 2) apa saja yang perlu dipersiapkan ketika hendak melakukan penilaian kepada sekolah atau penilaian akreditasi, 3) apa yang menjadi kriteria kelayakan pada akreditasi yang diberikan kepada sekolah, serta 4) faktor yang memengaruhi proses akreditasi sekolah. Informan dalam penelitian ini adalah Kepala Sekolah SDN Karangtumaritis. Penelitian ini menggunakan jenis penelitian kualitatif deskriptif yang bertujuan untuk menggambarkan karakteristik fenomena dengan penjabaran yang bersifat naratif. Metode pengumpulan data dalam penelitian ini menggunakan observasi, wawancara dan dokumentasi. Setelah didapatkan data, peneliti menggunakan model Milles and Huberman untuk melakukan kegiatan analisis data, melalui tiga tahapan yaitu: reduksi data, penyajian data, dan penarikan kesimpulan.
PENGEMBANGAN BAHAN AJAR MAJALAH BERBASIS ANDROID PADA MATERI ADIKSIMBA BAHASA INDONESIA KELAS 4 SDN PURUT KOTA SERANG
Authors: Anna Qurrotul Ain  , Sulastri Dewi , Aprilia Lusi , Jamaludin Ujang , Setiawan Sigit 
Published: June 2023

ABSTRACTThe purpose of this study was to increase students' literacy interest andstudents' reading comprehension through the development of android magazineteaching materials on the ADIKSIMBA material for grade 4 Indonesian. Theresearch method used was R&D with the borg and gall model. Analysis of researchdata using the Likert and Guttman scales. The research subjects were taken from4th grade students at SDN Purut City of Serang. The results of the validationpercentage recapitulation research by getting a value of 84.5% means that thisteaching material is categorized as a very good teaching material and is veryfeasible to be tested on students and the initial test obtained an average score of57.5 and in the final test obtained an average score 83 concluded that the use ofteaching materials for this magazine can improve students' understanding ofinterrogative sentences using the ADIKSIMBA element.
ABSTRAKTujuan pada penelitian ini adalah meningkatkan minat berliterasi siswa danpemahaman membaca siswa melalui pengembangan bahan ajar majalah androidpada materi ADIKSIMBA mata pelajaran Bahasa Indonesia kelas 4. Metodepenelitian yang digunakan adalah R&D dengan jenis model borg and gall. Analisisdata penelitian menggunakan skala likert dan guttman. Subjek penelitian diambildari siswa kelas 4 SDN Purut Kota Serang. Hasil penelitian rekapitulasi persentasivalidasi dengan mendapatkan nilai 84,5% artinya bahan ajar ini dikategorikansebagai bahan ajar yang sangat baik dan sangat layak untuk diujicobakan kepadasiswa dan tes awal didapatkan rata-rata nilai 57,5 dan pada tes akhir didapatkanrata-rata nilai 83 disimpulkan bahwa penggunaan bahan ajar majalah ini dapatmeningkatkan pemahaman siswa tentang kalimat tanya menggunakan unsurADIKSIMBA.
The Strength of the Sheared Magnetic Field in the Galactic’s Circumnuclear Disk
Authors: Guerra Jordan A. , Lopez-Rodriguez Enrique , Chuss David T. , Butterfield Natalie O. , Schmelz Joan T. 
Published: June 2023

Abstract
Recent high-resolution 53 μm polarimetric observations from SOFIA/HAWC+ have revealed the inferred plane-of-the-sky magnetic field (B-field) orientation in the Galactic center’s circumnuclear disk (CND). The B-field is mostly aligned with the steamers of ionized material falling onto Sgr A* at large, differential velocities (shear). In such conditions, estimating the B-field strength with the “classical” Davis–Chandrasekhar–Fermi (DCF) method does not provide accurate results. We derive a “modified” DCF method by solving the ideal-MHD equations from first principles considering the effects of a large-scale, shear flow on the propagation of a fast magnetosonic wave. In the context of the DCF approximation, both the value of the shear and its Laplacian affect the inferred B-field strength. Using synthetic polarization data from MHD simulations for a medium dominated by shear flows, we find that the “classical” DCF determines B-field strengths only within >50% of the true value where the “modified” DCF results are improved significantly (∼3%–22%). Applying our “modified” DCF method to the CND revealed B-field strengths of 1–16 mG in the northern arm, 1–13 mG in the eastern arm, and 3–27 mG in the western arc at spatial scales ≲1 pc, with median values of 5.1 ± 0.8, 4.0 ± 1.2, and 8.5 ± 2.3 mG, respectively. The balance between turbulent gas energy (kinetic plus hydrostatic) and turbulent magnetic energy densities suggest that, along the magnetic-field-flow direction, magnetic effects become less dominant as the shear flow increases and weakens the B-field via magnetic convection. Our results indicate that the transition from magnetically to gravitationally dominated accretion of material onto Sgr A* starts at distances ∼1 pc.
Supernova 2020wnt: An Atypical Superluminous Supernova with a Hidden Central Engine
Authors: Tinyanont Samaporn , Woosley Stan E. , Taggart Kirsty , Foley Ryan J. , Yan Lin , Lunnan Ragnhild , Davis Kyle W. , Kilpatrick Charles D. , Siebert Matthew R. , Schulze Steve , Ashall Chris , Chen Ting-Wan , De Kishalay , Dimitriadis Georgios , Dong Dillon Z. , Fremling Christoffer , Gagliano Alexander , Jha Saurabh W. , Jones David O. , Kasliwal Mansi M. , Miao Hao-Yu , Pan Yen-Chen , Perley Daniel A. , Ravi Vikram , Rojas-Bravo César , Sfaradi Itai , Sollerman Jesper , Alarcon Vanessa , Angulo Rodrigo , E. Clever Karoli , Crawford Payton , Couch Cirilla , Dandu Srujan , Dhara Atirath , Johnson Jessica , Lai Zhisen , Smith Carli 
Published: June 2023

Abstract
We present observations of a peculiar hydrogen- and helium-poor stripped-envelope (SE) supernova (SN) 2020wnt, primarily in the optical and near-infrared (near-IR). Its peak absolute bolometric magnitude of −20.9 mag (L
bol, peak = (6.8 ± 0.3) × 1043 erg s−1) and a rise time of 69 days are reminiscent of hydrogen-poor superluminous SNe (SLSNe I), luminous transients potentially powered by spinning-down magnetars. Before the main peak, there is a brief peak lasting <10 days post explosion, likely caused by interaction with circumstellar medium (CSM) ejected ∼years before the SN explosion. The optical spectra near peak lack a hot continuum and O ii absorptions, which are signs of heating from a central engine; they quantitatively resemble those of radioactivity-powered hydrogen/helium-poor Type Ic SESNe. At ∼1 yr after peak, nebular spectra reveal a blue pseudo-continuum and narrow O i recombination lines associated with magnetar heating. Radio observations rule out strong CSM interactions as the dominant energy source at +266 days post peak. Near-IR observations at +200–300 days reveal carbon monoxide and dust formation, which causes a dramatic optical light-curve dip. Pair-instability explosion models predict slow light curve and spectral features incompatible with observations. SN 2020wnt is best explained as a magnetar-powered core-collapse explosion of a 28 M
⊙ pre-SN star. The explosion kinetic energy is significantly larger than the magnetar energy at peak, effectively concealing the magnetar-heated inner ejecta until well after peak. SN 2020wnt falls into a continuum between normal SNe Ic and SLSNe I, and demonstrates that optical spectra at peak alone cannot rule out the presence of a central engine.
A 7 Day Multiwavelength Flare Campaign on AU Mic. I. High-time-resolution Light Curves and the Thermal Empirical Neupert Effect
Authors: Tristan Isaiah I. , Notsu Yuta , Kowalski Adam F. , Brown Alexander , Wisniewski John P. , Osten Rachel A. , Vrijmoet Eliot H. , White Graeme L. , Carter Brad D. , Grady Carol A. , Henry Todd J. , Hinojosa Rodrigo H. , Lomax Jamie R. , Neff James E. , Paredes Leonardo A. , Soutter Jack 
Published: June 2023

Abstract
We present light curves and flares from a 7 day, multiwavelength observational campaign of AU Mic, a young and active dM1e star with exoplanets and a debris disk. We report on 73 unique flares between the X-ray to optical data. We use high-time-resolution near-UV (NUV) photometry and soft X-ray (SXR) data from the X-ray Multi-Mirror Mission to study the empirical Neupert effect, which correlates the gradual and impulsive phase flaring emissions. We find that 65% (30 of 46) flares do not follow the Neupert effect, which is 3 times more excursions than seen in solar flares, and propose a four-part Neupert effect classification (Neupert, quasi-Neupert, non-Neupert types I and II) to explain the multiwavelength responses. While the SXR emission generally lags behind the NUV as expected from the chromospheric evaporation flare models, the Neupert effect is more prevalent in larger, more impulsive flares. Preliminary flaring rate analysis with X-ray and U-band data suggests that previously estimated energy ratios hold for a collection of flares observed over the same time period, but not necessarily for an individual, multiwavelength flare. These results imply that one model cannot explain all stellar flares and care should be taken when extrapolating between wavelength regimes. Future work will expand wavelength coverage using radio data to constrain the nonthermal empirical and theoretical Neupert effects to better refine models and bridge the gap between stellar and solar flare physics.
HD 222925: A New Opportunity to Explore the Astrophysical and Nuclear Conditions of r-process Sites
Authors: Holmbeck Erika M. , Surman Rebecca , Roederer Ian U. , McLaughlin G. C. , Frebel Anna 
Published: June 2023

Abstract
With the most trans-iron elements detected of any star outside the solar system, HD 222925 represents the most complete chemical inventory among metal-poor stars enhanced with elements made by the rapid neutron capture (“r”) process. As such, HD 222925 may be a new “template” for the observational r-process, where before the (much higher-metallicity) solar r-process residuals were used. In this work, we test under which conditions a single site accounts for the entire elemental r-process abundance pattern of HD 222925. We found that several of our tests—with the single exception of the black hole–neutron star merger case—challenge the single-site assumption by producing an ejecta distribution that is highly constrained, in disagreement with simulation predictions. However, we found that ejecta distributions that are more in line with simulations can be obtained under the condition that the nuclear data near the second r-process peak are changed. Therefore, for HD 222925 to be a canonical r-process template likely as a product of a single astrophysical source, the nuclear data need to be reevaluated. The new elemental abundance pattern of HD 222925—including the abundances obtained from space-based, ultraviolet (UV) data—call for a deeper understanding of both astrophysical r-process sites and nuclear data. Similar UV observations of additional r-process–enhanced stars will be required to determine whether the elemental abundance pattern of HD 222925 is indeed a canonical template (or an outlier) for the r-process at low metallicity.
A Spectroscopic Model of the Type Ia Supernova–Host-galaxy Mass Correlation from SALT3
Authors: Jones D. O. , Kenworthy W. D. , Dai M. , Foley R. J. , Kessler R. , Pierel J. D. R. , Siebert M. R. 
Published: June 2023

Abstract
The unknown cause of the correlation between Type Ia supernova (SN Ia) Hubble residuals and their host-galaxy masses (the “mass step”) may bias cosmological parameter measurements. To better understand the mass step, we develop a SALT3 light-curve model for SN cosmology that uses the host-galaxy masses of 296 low-redshift SNe Ia to derive a spectral energy distribution–host-galaxy mass relationship. The resulting model has larger Ca ii H and K, Ca ii near-infrared triplet, and Si ii equivalent widths for SNe in low-mass host galaxies at 2.2–2.7σ significance; this indicates higher explosion energies per unit mass in low-mass-hosted SNe. The model has phase-dependent changes in SN Ia colors as a function of host mass, indicating intrinsic differences in mean broadband light curves. Although the model provides a better fit to the SN data overall, it does not substantially reduce data–model residuals for a typical light curve in our sample nor does it significantly reduce Hubble residual dispersion. This is because we find that previous SALT models parameterized most host-galaxy dependencies with their first principal component, although they failed to model some significant spectral variations. Our new model is luminosity and cosmology independent, and applying it to data reduces the mass step by 0.021 ± 0.002 mag (uncertainty accounts for correlated data sets); these results indicate that ∼35% of the mass step can be attributed to luminosity-independent effects. This SALT model version could be trained using alternative host-galaxy properties and at different redshifts, and therefore will be a tool for understanding redshift-dependent correlations between SNe Ia and their host properties as well as their impact on cosmological parameter measurements.
X-Ray and Ultraviolet Emission of the Young Planet-hosting Star V1298 Tau from Coordinated Observations with XMM-Newton and Hubble Space Telescope
Authors: Maggio A. , Pillitteri I. , Argiroffi C. , Benatti S. , Sanz-Forcada J. , D’Orazi V. , Biazzo K. , Borsa F. , Cabona L. , Claudi R. , Desidera S. , Locci D. , Nardiello D. , Mancini L. , Micela G. , Rainer M. , Spinelli R. , Bignamini A. , Damasso M. 
Published: June 2023

Abstract
Atmospheric mass loss plays a major role in the evolution of exoplanets. This process is driven by the stellar high-energy irradiation, especially in the first hundreds of millions of years after dissipation of the proto-planetary disk. A major source of uncertainty in modeling atmospheric photoevaporation and photochemistry is due to the lack of direct measurements of the stellar flux at extreme-UV (EUV) wavelengths. Several empirical relationships have been proposed in the past to link EUV fluxes to emission levels in X-rays, but the stellar samples employed for this aim are heterogeneous, and the available scaling laws provide significantly different predictions, especially for very active stars. We present new far-UV and X-ray observations of V1298 Tau with Hubble Space Telescope/Cosmic Origins Spectrograph and XMM-Newton, aimed to determine more accurately the high-energy emission of this solar-mass pre-main-sequence star, which hosts four exoplanets. Spectroscopic data were employed to derive the plasma emission measure distribution versus temperature, from the chromosphere to the corona, and the possible variability of this irradiation on short and year-long timescales, due to magnetic activity. As a side result, we have also measured the chemical abundances of several elements in the outer atmosphere of V1298 Tau. We employ our results as a new benchmark point for the calibration of the X-ray to EUV scaling laws, and hence to predict the time evolution of the irradiation in the EUV band, and its effect on the evaporation of exo-atmospheres.
A SPectroscopic Survey of Biased Halos in the Reionization Era (ASPIRE): A First Look at the Rest-frame Optical Spectra of z > 6.5 Quasars Using JWST
Authors: Yang Jinyi , Wang Feige , Fan Xiaohui , Hennawi Joseph F. , Barth Aaron J. , Bañados Eduardo , Sun Fengwu , Liu Weizhe , Cai Zheng , Jiang Linhua , Li Zihao , Onoue Masafusa , Schindler Jan-Torge , Shen Yue , Wu Yunjing , Bhowmick Aklant K. , Bieri Rebekka , Blecha Laura , Bosman Sarah , Champagne Jaclyn B. , Colina Luis , Connor Thomas , Costa Tiago , Davies Frederick B. , Decarli Roberto , De Rosa Gisella , Drake Alyssa B. , Egami Eiichi , Eilers Anna-Christina , Evans Analis E. , Farina Emanuele Paolo , Habouzit Melanie , Haiman Zoltan , Jin Xiangyu , Jun Hyunsung D. , Kakiichi Koki , Khusanova Yana , Kulkarni Girish , Loiacono Federica , Lupi Alessandro , Mazzucchelli Chiara , Pan Zhiwei , Rojas-Ruiz Sofía , Strauss Michael A. , Tee Wei Leong , Trakhtenbrot Benny , Trebitsch Maxime , Venemans Bram , Vestergaard Marianne , Volonteri Marta , Walter Fabian , Xie Zhang-Liang , Yue Minghao , Zhang Haowen , Zhang Huanian , Zou Siwei 
Published: June 2023

Abstract
Studies of rest-frame optical emission in quasars at z > 6 have historically been limited by the wavelengths accessible by ground-based telescopes. The James Webb Space Telescope (JWST) now offers the opportunity to probe this emission deep into the reionization epoch. We report the observations of eight quasars at z > 6.5 using the JWST/NIRCam Wide Field Slitless Spectroscopy as a part of the “A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE)” program. Our JWST spectra cover the quasars’ emission between rest frame ∼4100 and 5100 Å. The profiles of these quasars’ broad Hβ emission lines span a full width at half maximum from 3000 to 6000 km s−1. The Hβ-based virial black hole (BH) masses, ranging from 0.6 to 2.1 billion solar masses, are generally consistent with their Mg ii-based BH masses. The new measurements based on the more reliable Hβ tracer thus confirm the existence of a billion solar-mass BHs in the reionization epoch. In the observed [O iii] λ
λ 4960,5008 doublets of these luminous quasars, broad components are more common than narrow core components (≤ 1200 km s−1), and only one quasar shows stronger narrow components than broad. Two quasars exhibit significantly broad and blueshifted [O iii] emission, thought to trace galactic-scale outflows, with median velocities of −610 and −1430 km s−1 relative to the [C ii] 158 μm line. All eight quasars show strong optical Fe ii emission and follow the eigenvector 1 relations defined by low-redshift quasars. The entire ASPIRE program will eventually cover 25 quasars and provide a statistical sample for the studies of the BHs and quasar spectral properties.
The Dynamic Evolution of Multipoint Interplanetary Coronal Mass Ejections Observed with BepiColombo, Tianwen-1, and MAVEN
Authors: Chi Yutian , Shen Chenglong , Liu Junyan , Zhong Zhihui , Owens Mathew , Scott Christopher , Barnard Luke , Yu Bingkun , Heyner Daniel , Auster Hans-Ulrich , Richter Ingo , Wang Yuming , Zhang Tielong , Guo Jingnan , Sánchez-Cano Beatriz , Pan Zonghao , Zou Zhuxuan , Xu Mengjiao , Cheng Long , Su Zhenpeng , Mao Dongwei , Zhang Zhiyong , Wang Can , Wu Zhiyong , Wang Guoqiang , Xiao Sudong , Liu Kai , Hao Xinjun , Li Yiren , Chen Manming , Lockwood Mike 
Published: June 2023

Abstract
We present two multipoint interplanetary coronal mass ejections (ICMEs) detected by the Tianwen-1 and Mars Atmosphere and Volatile Evolution spacecraft at Mars and the BepiColombo (0.56 au ∼0.67 au) upstream of Mars from 2021 December 5 to 31. This is the first time that BepiColombo is used as an upstream solar wind monitor ahead of Mars and that Tianwen-1 is used to investigate the magnetic field characteristics of ICMEs at Mars. The Heliospheric Upwind Extrapolation time model was used to connect the multiple in situ observations and the coronagraph observations from STEREO/SECCHI and SOHO/LASCO. The first fast coronal mass ejection event (∼761.2 km s−1), which erupted on December 4, impacted Mars centrally and grazed BepiColombo by its western flank. The ambient slow solar wind decelerated the west flank of the ICME, implying that the ICME event was significantly distorted by the solar wind structure. The second slow ICME event (∼390.7 km s−1) underwent an acceleration from its eruption to a distance within 0.69 au and then traveled with the constant velocity of the ambient solar wind. These findings highlight the importance of background solar wind in determining the interplanetary evolution and global morphology of ICMEs up to Mars distance. Observations from multiple locations are invaluable for space weather studies at Mars and merit more exploration in the future.
Search for an Isotropic Gravitational-wave Background with the Parkes Pulsar Timing Array
Authors: Reardon Daniel J. , Zic Andrew , Shannon Ryan M. , Hobbs George B. , Bailes Matthew , Di Marco Valentina , Kapur Agastya , Rogers Axl F. , Thrane Eric , Askew Jacob , Bhat N. D. Ramesh , Cameron Andrew , Curyło Małgorzata , Coles William A. , Dai Shi , Goncharov Boris , Kerr Matthew , Kulkarni Atharva , Levin Yuri , Lower Marcus E. , Manchester Richard N. , Mandow Rami , Miles Matthew T. , Nathan Rowina S. , Osłowski Stefan , Russell Christopher J. , Spiewak Renée , Zhang Songbo , Zhu Xing-Jiang 
Published: June 2023

Abstract
Pulsar timing arrays aim to detect nanohertz-frequency gravitational waves (GWs). A background of GWs modulates pulsar arrival times and manifests as a stochastic process, common to all pulsars, with a signature spatial correlation. Here we describe a search for an isotropic stochastic gravitational-wave background (GWB) using observations of 30 millisecond pulsars from the third data release of the Parkes Pulsar Timing Array (PPTA), which spans 18 yr. Using current Bayesian inference techniques we recover and characterize a common-spectrum noise process. Represented as a strain spectrum

h

c

=
A

(
f

/

1

yr

−
1

)

α

, we measure

A
=

3.1

−
0.9

+
1.3

×

10

−
15

and α = −0.45 ± 0.20, respectively (median and 68% credible interval). For a spectral index of α = −2/3, corresponding to an isotropic background of GWs radiated by inspiraling supermassive black hole binaries, we recover an amplitude of

A
=

2.04

−
0.22

+
0.25

×

10

−
15

. However, we demonstrate that the apparent signal strength is time-dependent, as the first half of our data set can be used to place an upper limit on A that is in tension with the inferred common-spectrum amplitude using the complete data set. We search for spatial correlations in the observations by hierarchically analyzing individual pulsar pairs, which also allows for significance validation through randomizing pulsar positions on the sky. For a process with α = −2/3, we measure spatial correlations consistent with a GWB, with an estimated false-alarm probability of p ≲ 0.02 (approx. 2σ). The long timing baselines of the PPTA and the access to southern pulsars will continue to play an important role in the International Pulsar Timing Array.
An Observational Upper Limit on the Rate of Gamma-Ray Bursts with Neutron Star–Black Hole Merger Progenitors
Authors: Biscoveanu Sylvia , Burns Eric , Landry Philippe , Vitale Salvatore 
Published: June 2023

Abstract
Compact-object binary mergers consisting of one neutron star and one black hole (NSBHs) have long been considered promising progenitors for gamma-ray bursts, whose central engine remains poorly understood. Using gravitational-wave constraints on the population-level NSBH mass and spin distributions we find that at most 20 Gpc−3 yr−1 of gamma-ray bursts in the local universe can have NSBH progenitors.