bluuebunny/crossref_metadata_2025_split huggingface dataset:
RESOLUSI KONFLIK DI ASIA TENGGARA PERSPEKTIF ISLAM (STUDI KASUS RESOLUSI KONFLIK CHAM ISLAM DALAM MENGHADAPI SINKRETISME ISLAM DI VIETNAM)
Authors: Eka Putri Febi , Fadhilah Eva 
Published: May 2023

Vietnam is one of the countries in Southeast Asia in the form of a Socialist country. The majority of the population in Vietnam embraces Buddhism while Islam is a minority religion there. The Muslim population in Vietnam is divided into two sects or schools, namely Cham Islam and Cham Bani. Cham Islam is a follower of the Sunni sect of Islam while Cham Bani is a sect of Islam that is still influenced by Indian culture or traditions. This study examines the resolution of the Cham Islam conflict in the face of Islamic syncretism in Vietnam from an Islamic perspective. With qualitative research methods, the authors found that the conflict resolution used in reducing conflicts that occurred because of differences in flow between Cham Islam and Cham Bani was a persuasive approach using the method of deliberation as taught by Islam. Another method when the method of deliberation is not achieved is the method of war. War in conflict resolution is not meant to solely kill lives but to survive and defend religion when threatened.

Keywords: Resolution, Conflict, Vietnam, Islam
A Catalog of Distance Determinations for the LAMOST DR8 K Giants in the Galactic Halo
Authors: Zhang Lan , Xue Xiang-Xiang , Yang Chengqun , Wang Feilu , Rix Hans-Walter , Zhao Gang , Liu Chao 
Published: May 2023

Abstract
We present a catalog of distances for 19,544 K giants drawn from Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) DR8. Most of them are located in the halo of the Milky Way up to ∼120 kpc. There are 15% K giants without Sloan Digital Sky Survey (SDSS) photometry, for which we supplements with Pan-STARRS1 (PS1) photometry calibrated to SDSS photometric system. The possible contamination of the red clumps/horizontal branch are removed according to metallicities and colors before the distance determination. Combining the LAMOST spectroscopic metallicities with the SDSS/PS1 photometry, we estimate the absolute magnitudes in the SDSS r band, the distance moduli, and the corresponding uncertainties through an Bayesian approach devised by Xue et al. for the Sloan Extension for Galactic understanding and exploration halo K giants. The typical distance precision is about 11%. The stars in the catalog lie in a region of 4–126 kpc from the Galactic center, of which with 6320 stars beyond 20 kpc and 273 stars beyond 50 kpc, forming the largest spectroscopic sample of distant tracers in the Milky Way halo so far.
The Dark Energy Survey Supernova Program: Corrections on Photometry Due to Wavelength-dependent Atmospheric Effects
Authors: Lee J. , Acevedo M. , Sako M. , Vincenzi M. , Brout D. , Sanchez B. , Chen R. , Davis T. M. , Jarvis M. , Scolnic D. , Qu H. , Galbany L. , Kessler R. , Lasker J. , Sullivan M. , Wiseman P. , Aguena M. , Allam S. , Alves O. , Andrade-Oliveira F. , Bertin E. , Bocquet S. , Brooks D. , Burke D. L. , Carnero Rosell A. , Carrasco Kind M. , Carretero J. , Costanzi M. , da Costa L. N. , Pereira M. E. S. , De Vicente J. , Desai S. , Diehl H. T. , Doel P. , Everett S. , Ferrero I. , Friedel D. , Frieman J. , García-Bellido J. , Gerdes D. W. , Gruen D. , Gruendl R. A. , Gutierrez G. , Hinton S. R. , Hollowood D. L. , Honscheid K. , James D. J. , Kent S. , Kuehn K. , Kuropatkin N. , Mena-Fernández J. , Miquel R. , Ogando R. L. C. , Palmese A. , Pieres A. , Malagón A. A. Plazas , Raveri M. , Reil K. , Rodriguez-Monroy M. , Sanchez E. , Scarpine V. , Sevilla-Noarbe I. , Smith M. , Suchyta E. , Tarle G. , To C. , Weaverdyck N. ,   DES Collaboration
Published: May 2023

Abstract
Wavelength-dependent atmospheric effects impact photometric supernova flux measurements for ground-based observations. We present corrections on supernova flux measurements from the Dark Energy Survey Supernova Program’s 5YR sample (DES-SN5YR) for differential chromatic refraction (DCR) and wavelength-dependent seeing, and we show their impact on the cosmological parameters w and Ω
m
. We use g − i colors of Type Ia supernovae to quantify astrometric offsets caused by DCR and simulate point-spread functions (PSFs) using the GalSIM package to predict the shapes of the PSFs with DCR and wavelength-dependent seeing. We calculate the magnitude corrections and apply them to the magnitudes computed by the DES-SN5YR photometric pipeline. We find that for the DES-SN5YR analysis, not accounting for the astrometric offsets and changes in the PSF shape cause an average bias of +0.2 mmag and −0.3 mmag, respectively, with standard deviations of 0.7 mmag and 2.7 mmag across all DES observing bands (griz) throughout all redshifts. When the DCR and seeing effects are not accounted for, we find that w and Ω
m
are lower by less than 0.004 ± 0.02 and 0.001 ± 0.01, respectively, with 0.02 and 0.01 being the 1σ statistical uncertainties. Although we find that these biases do not limit the constraints of the DES-SN5YR sample, future surveys with much higher statistics, lower systematics, and especially those that observe in the u band will require these corrections as wavelength-dependent atmospheric effects are larger at shorter wavelengths. We also discuss limitations of our method and how they can be better accounted for in future surveys.
Comparing Be Star Inclination Angles Determined from Hα Fitting and Gravitational Darkening
Authors: Sigut T. A. A. , Ghafourian Nastaran R. 
Published: May 2023

Abstract
Using a sample of 92 Galactic Be stars, we compare inclination angles (the angle between a star’s rotation axis and the line of sight) determined from Hα emission-line profile fitting to those determined by the spectroscopic signature of gravitational darkening. We find good agreement: 70% of the sample (64 out of 92 stars) is consistent with zero difference between the two methods using 1σ errors, and there is a strong linear correlation coefficient between the two methods of r = +0.63 ± 0.05. There is some evidence that the Hα profile fitting method overestimates the inclination angle for i ≲ 25°, perhaps due to the neglect of incoherent electron scattering on the Hα line widths, while the gravitational darkening method underestimates the inclination angle for i ≳ 70°, perhaps due to the neglect of disk radiative transfer effects on the optical spectrum. Overall, it is demonstrated that a single Hα spectrum of modest resolution and SNR can be used to extract a useful estimate for the inclination angle of an individual Be star. This allows equatorial rotation velocities for individual Be stars to be derived from

v
sin
i

measurements and will allow Be stars to be used to search for correlated spin axes in young, open clusters if unbiased (with respect to inclination) samples of Be stars are used.
Hubble Space Telescope Proper Motion Measurements of Supernova Remnant N132D: Center of Expansion and Age
Authors: Banovetz John , Milisavljevic Dan , Sravan Niharika , Weil Kathryn E. , Subrayan Bhagya , Fesen Robert A. , Patnaude Daniel J. , Plucinsky Paul P. , Law Charles J. , Blair William P. , Morse Jon A. 
Published: May 2023

Abstract
We present proper motion measurements of the oxygen-rich ejecta of the LMC supernova remnant N132D using two epochs of Hubble Space Telescope Advanced Camera for Surveys data spanning 16 years. The proper motions of 120 individual knots of oxygen-rich gas were measured and used to calculate a center of expansion (CoE) of α = 5h25m01.ˢ71 and δ = −69°38′41.″64 (J2000) with a 1σ uncertainty of 2.″90. This new CoE measurement is 9.″2 and 10.″8 from two previous CoE estimates based on the geometry of the optically emitting ejecta. We also derive an explosion age of 2770 ± 500 yr, which is consistent with recent age estimates of ≈2500 yr made from 3D ejecta reconstructions. We verified our estimates of the CoE and age using a new automated procedure that detected and tracked the proper motions of 137 knots, with 73 knots that overlap with the visually identified knots. We find that the proper motions of the ejecta are still ballistic, despite the remnant’s age, and are consistent with the notion that the ejecta are expanding into an interstellar medium cavity. Evidence for explosion asymmetry from the parent supernova is also observed. Using the visually measured proper motion measurements and corresponding CoE and age, we compare N132D to other supernova remnants with proper motion ejecta studies.
A Pilot Study of Nulling in 22 Pulsars Using Mixture Modeling
Authors: Anumarlapudi Akash , Swiggum Joseph K. , Kaplan David L. , Fichtenbauer Travis D. J. 
Published: May 2023

Abstract
The phenomenon of pulsar nulling, observed as the temporary inactivity of a pulsar, remains poorly understood both observationally and theoretically. Most observational studies that quantify nulling employ a variant of Ritchings algorithm, which can suffer significant biases for pulsars where the emission is weak. Using a more robust mixture model method, we study pulsar nulling in a sample of 22 recently discovered pulsars, for which we publish the nulling fractions for the first time. These data clearly demonstrate biases of the former approach and show how an otherwise nonnulling pulsar can be classified as having significant nulls. We show that the population-wide studies that find a positive correlation of nulling with pulsar period/characteristic age can similarly be biased because of the bias in estimating the nulling fraction. We use our probabilistic approach to find the evidence for periodicity in the nulls in a subset of three pulsars in our sample. In addition, we also provide improved timing parameters for 17 of the 22 pulsars that had no prior follow-up.
A Search for OH 18 cm Emission from Intermediate-velocity Gas at High Galactic Latitudes
Authors: Smith Allison J. , Roshi D. Anish 
Published: May 2023

Abstract
We present search results of 22 high-latitude (∣b∣ > 25°) sightlines for OH 18 cm emission using the 305 m radio telescope at the Arecibo Observatory. These sightlines appear in neutral hydrogen emission at intermediate velocities −90 ≤ V
LSR ≤ −20 km s−1 and are predicted to have a sufficient molecular composition so as to be detectable in molecular emission. Such objects, known as intermediate-velocity molecular clouds (IVMCs), have historically been detected through 12CO emission. Recent studies indicate that IVMCs may be widespread in the galaxy and have important implications for models of the interstellar medium and star formation. However, we report nondetections of OH emission toward the 22 sightlines and provide stringent upper limits on the OH column density. Using available H i and A

v
data in combination with existing state-of-the-art PDR models, we estimate H2 column densities and find that they are more than an order of magnitude lower than the predicted values. We also find that the hydrogen volume density of these clouds is ≲25 cm−3. In addition, we discuss the known IVMCs with previous 12CO detections in the context of the PDR models. Our analysis of these clouds indicates that the structure of molecular material in IVMCs is morphologically clumpy. These results motivate the need for future sensitive, on-the-fly searches (rather than targeted searches) for CO emission from IVMCs with resolutions on the order of ∼1′. High angular resolution (∼1′) H i and A

v
data will also be helpful to better constrain the structure and composition of IVMCs.
Photometric and Spectroscopic Observations of GRB 190106A: Emission from Reverse and Forward Shocks with Late-time Energy Injection
Authors: Zhu Zi-Pei , Xu Dong , Fynbo Johan P. U. , Fu Shao-Yu , Zhang Jun-Bo , Liu Xing , Jiang Shuai-Qing , Xiao Shuo , Xie Wei , Zou Yuan-Chuan , Gao He , Hartmann Dieter , de Ugarte Postigo Antonio , Kann David Alexander , Valle Massimo Della , Jakobsson Pall , Zafar Tayyaba , D’Elia Valerio , Xin Li-Ping , Wei Jian-Yan , Gao Xing , Liu Jin-Zhong , Lu Tian-Hua , Lei Wei-Hua 
Published: May 2023

Abstract
Early optical observations of gamma-ray bursts can significantly contribute to the study of the central engine and physical processes therein. However, of the thousands observed so far, only a few have data at optical wavelengths in the first minutes after the onset of the prompt emission. Here we report on GRB 190106A, whose afterglow was observed in optical bands just 36 s after the Swift/BAT trigger, i.e., during the prompt emission phase. The early optical afterglow exhibits a bimodal structure followed by a normal decay, with a faster decay after ∼T
0 + 1 day. We present optical photometric and spectroscopic observations of GRB 190106A. We derive the redshift via metal absorption lines from Xinglong 2.16 m/BFOSC spectroscopic observations. From the BFOSC spectrum, we measure z = 1.861 ± 0.002. The double-peak optical light curve is a significant feature predicted by the reverse-forward external-shock model. The shallow decay followed by a normal decay in both the X-ray and optical light curves is well explained with the standard forward-shock model with late-time energy injection. Therefore, GRB 190106A offers a case study for GRB emission from both reverse and forward shocks.
CLASSY. VI. The Density, Structure, and Size of Absorption-line Outflows in Starburst Galaxies
Authors: Xu Xinfeng , Heckman Timothy , Henry Alaina , Berg Danielle A. , Chisholm John , James Bethan L. , Martin Crystal L. , Stark Daniel P. , Hayes Matthew , Arellano-Córdova Karla Z. , Carr Cody , Huberty Mason , Mingozzi Matilde , Scarlata Claudia , Sugahara Yuma 
Published: May 2023

Abstract
Galaxy formation and evolution are regulated by the feedback from galactic winds. Absorption lines provide the most widely available probe of winds. However, since most data only provide information integrated along the line of sight, they do not directly constrain the radial structure of the outflows. In this paper, we present a method to directly measure the gas electron density in outflows (n

e
), which in turn yields estimates of outflow cloud properties (e.g., density, volume filling factor, and sizes/masses). We also estimate the distance (r

n
) from the starburst at which the observed densities are found. We focus on 22 local star-forming galaxies primarily from the COS Legacy Archive Spectroscopic SurveY (CLASSY). In half of them, we detect absorption lines from fine-structure excited transitions of Si ii (i.e., Si ii*). We determine n

e
from relative column densities of Si ii and Si ii*, given Si ii* originates from collisional excitation by free electrons. We find that the derived n

e
correlates well with the galaxy’s star formation rate per unit area. From photoionization models or assuming the outflow is in pressure equilibrium with the wind fluid, we get r

n
∼ 1–2r
* or ∼5r
*, respectively, where r
* is the starburst radius. Based on comparisons to theoretical models of multiphase outflows, nearly all of the outflows have cloud sizes large enough for the clouds to survive their interaction with the hot wind fluid. Most of these measurements are the first ever for galactic winds detected in absorption lines and, thus, will provide important constraints for future models of galactic winds.
Carnegie Supernova Project. II. Near-infrared Spectral Diversity and Template of Type Ia Supernovae
Authors: Lu 陆 Jing 晶 , Hsiao 蕭 Eric Y. 亦麒 , Phillips Mark M. , Burns Christopher R. , Ashall Chris , Morrell Nidia , Ng Lawrence , Kumar Sahana , Shahbandeh Melissa , Hoeflich Peter , Baron E. , Uddin Syed , Stritzinger Maximilian D. , Suntzeff Nicholas B. , Baltay Charles , Davis Scott , Diamond Tiara R. , Folatelli Gaston , Förster Francisco , Gagné Jonathan , Galbany Lluís , Gall Christa , González-Gaitán Santiago , Holmbo Simon , Kirshner Robert P. , Krisciunas Kevin , Marion G. H. , Perlmutter Saul , Pessi Priscila J. , Piro Anthony L. , Rabinowitz David , Ryder Stuart D. , Sand David J. 
Published: May 2023

Abstract
We present the largest and most homogeneous collection of near-infrared (NIR) spectra of Type Ia supernovae (SNe Ia): 339 spectra of 98 individual SNe obtained as part of the Carnegie Supernova Project-II. These spectra, obtained with the FIRE spectrograph on the 6.5 m Magellan Baade telescope, have a spectral range of 0.8–2.5 μm. Using this sample, we explore the NIR spectral diversity of SNe Ia and construct a template of spectral time series as a function of the light-curve-shape parameter, color stretch s

BV
. Principal component analysis is applied to characterize the diversity of the spectral features and reduce data dimensionality to a smaller subspace. Gaussian process regression is then used to model the subspace dependence on phase and light-curve shape and the associated uncertainty. Our template is able to predict spectral variations that are correlated with s

BV
, such as the hallmark NIR features: Mg ii at early times and the H-band break after peak. Using this template reduces the systematic uncertainties in K-corrections by ∼90% compared to those from the Hsiao template. These uncertainties, defined as the mean K-correction differences computed with the color-matched template and observed spectra, are on the level of 4 × 10−4 mag on average. This template can serve as the baseline spectral energy distribution for light-curve fitters and can identify peculiar spectral features that might point to compelling physics. The results presented here will substantially improve future SN Ia cosmological experiments, for both nearby and distant samples.
The Dark Side of Using Dark Sirens to Constrain the Hubble–Lemaître Constant
Authors: Zhu Liang-Gui , Chen Xian 
Published: May 2023

Abstract
Dark sirens, i.e., gravitational-wave (GW) sources without electromagnetic counterparts, are new probes of the expansion of the universe. The efficacy of this method relies on correctly localizing the host galaxies. However, recent theoretical studies have shown that astrophysical environments could mislead the spatial localization by distorting the GW signals. It is unclear whether and to what degree the incorrect spatial localizations of dark sirens would impair the accuracy of the measurement of the cosmological parameters. To address this issue, we consider the future observations of dark sirens using the Cosmic Explorer and the Einstein Telescope, and we design a Bayesian framework to access the precision of measuring the Hubble–Lemaître constant H
0. Interestingly, we find that the precision is not compromised when the number of well-localized dark sirens is significantly below 300, even in the extreme scenario that all the dark sirens are localized incorrectly. As the number exceeds 300, the incorrect spatial localizations start to produce statistically noticeable effects, such as a slow convergence of the posterior distribution of H
0. We propose several tests that can be used in future observations to verify the spatial localizations of dark sirens. Simulations of these tests suggest that incorrect spatial localizations will dominate a systematic error of H
0 if as much as 10% of a sample of 300 well-localized dark sirens are affected by their environments. Our results have important implications for the long-term goal of measuring H
0 to a precision of <1% using dark sirens.
Evidence of First Stars-enriched Gas in High-redshift Absorbers*
Authors: Saccardi Andrea , Salvadori Stefania , D’Odorico Valentina , Cupani Guido , Fumagalli Michele , Berg Trystyn A. M. , Becker George D. , Ellison Sara , Lopez Sebastian 
Published: May 2023

Abstract
The first stars were born from chemically pristine gas. They were likely massive, and thus they rapidly exploded as supernovae, enriching the surrounding gas with the first heavy elements. In the Local Group, the chemical signatures of the first stellar population were identified among low-mass, long-lived, very metal-poor ([Fe/H] < −2) stars, characterized by high abundances of carbon over iron ([C/Fe] > +0.7): the so-called carbon-enhanced metal-poor stars. Conversely, a similar carbon excess caused by first-star pollution was not found in dense neutral gas traced by absorption systems at different cosmic time. Here we present the detection of 14 very metal-poor, optically thick absorbers at redshift z ∼ 3–4. Among these, 3 are carbon-enhanced and reveal an overabundance with respect to Fe of all the analyzed chemical elements (O, Mg, Al, and Si). Their relative abundances show a distribution with respect to [Fe/H] that is in very good agreement with those observed in nearby very metal-poor stars. All the tests we performed support the idea that these C-rich absorbers preserve the chemical yields of the first stars. Our new findings suggest that the first-star signatures can survive in optically thick but relatively diffuse absorbers, which are not sufficiently dense to sustain star formation and hence are not dominated by the chemical products of normal stars.
Structure of the Plasma near the Heliospheric Current Sheet as Seen by WISPR/Parker Solar Probe from inside the Streamer Belt
Authors: Liewer Paulett C. , Vourlidas Angelos , Stenborg Guillermo , Howard Russell A. , Qiu Jiong , Penteado Paulo , Panasenco Olga , Braga Carlos R. 
Published: May 2023

Abstract
Parker Solar Probe (PSP) crossed the heliospheric current sheet (HCS) near the perihelion on encounters E8 and E11, enabling the Wide-field Imager for Solar Probe (WISPR) to image the streamer belt plasma in high resolution while flying through it. With perihelia of 16 R
⊙ and 13 R
⊙ for E8 and E11, respectively, WISPR images enable investigation of the structure of density encasing the HCS at much higher resolution than reported previously. As PSP flies closer to the Sun, fine-scale structures are resolved within the coronal rays of the streamer belt. Near the HCS, WISPR observes a fan of rays of various sizes and brightnesses, indicating large density variations in the HCS plasma sheet transverse to the radial direction. Near the perihelion, when PSP’s speed exceeds the solar corotation speed, some rays exhibit large changes in apparent latitude as the HCS is encountered, and rays pass over and under the spacecraft. The multiple viewpoints provided during the HCS crossing enable us to extract the coordinates of a few rays in a heliocentric frame. The rays were found to lie near the HCS from a PFSS model. We compare their locations to the location of the streamers as seen in synoptic maps from the Large Angle and Spectrometric Coronagraph, and find that the rays generally fall within the bright streamer bands seen in these maps, which confirms that they are features of the streamer belt plasma. We speculate that the density variations in the helmet streamer plasma result from continuous interchange reconnection along the coronal hole boundaries.
ABYSS. I. Targeting Strategy for the APOGEE and BOSS Young Star Survey in SDSS-V
Authors: Kounkel Marina , Zari Eleonora , Covey Kevin , Tkachenko Andrew , Zúñiga Carlos Román , Stassun Keivan , Stutz Amelia M. , Stringfellow Guy , Roman-Lopes Alexandre , Hernández Jesús , Ramírez Karla Peña , Bayo Amelia , Kim Jinyoung Serena , Cao Lyra , Wolk Scott J. , Kollmeier Juna , López-Valdivia Ricardo , Rojas-Ayala Bárbara 
Published: May 2023

Abstract
The fifth iteration of the Sloan Digital Sky Survey is set to obtain optical and near-infrared spectra of ∼5 million stars of all ages and masses throughout the Milky Way. As a part of these efforts, APOGEE and BOSS Young Star Survey (ABYSS) will observe ∼105 stars with ages <30 Myr that have been selected using a set of homogeneous selection functions that make use of different tracers of youth. The ABYSS targeting strategy we describe in this paper is aimed to provide the largest spectroscopic census of young stars to date. It consists of eight different types of selection criteria that take the position on the H-R diagram, infrared excess, variability, as well as the position in phase space in consideration. The resulting catalog of ∼200,000 sources (of which a half are expected to be observed) provides representative coverage of the young Galaxy, including both nearby diffuse associations as well as more distant massive complexes, reaching toward the inner Galaxy and the Galactic center.