bluuebunny/crossref_metadata_2025_split huggingface dataset:
Kegiatan Pendampingan Para Pengerajin Anyaman Bambu Untuk Mengembangkan Inovasi Produk Bagi UMKM di Kabupaten Purworejo
Authors: Riyanto Eko , Murtadha Muhammad Zain , Fadhilah Nariyatul , Mulyani Agustin 
Published: August 2024

Bambu merupakan salah satu sumber daya alam yang dimiliki oleh Indonesia, yang menjadi salah satu sumber pencaharian dikalangan masyarakat desa. Bambu dapat dijadikan kerajinan tangan berupa anyaman yang berkualitas. Desa Loning merupakan desa yang hampir semua warganya merupakan pengrajin anyaman bambu, namun produk yang dihasilkan kurang bervariasi dan kreatif sehingga nilai jual yang didapat rendah. Tujuan dari pengabdian ini adalah untuk meningkatkan kreatifitas dan inovasi desain produk anyaman bambu yang bernilai jual tinggi. Metode pelaksanaan dilakukan dengan sosialisasi, pelatihan dan pendampingan yang terdiri dari tiga tahap diantaranya tahap persiapan, tahap pelaksanaan dan tahap evaluasi. Hasil dari pelatihan ini adalah kreativitas dan inovasi anyaman bambu melalui sosialisasi, pelatihan dan pendampingan sehingga produk anyman bambu menjadi beragam dan bernilai jual tinggi untuk meningkatkan UMKM di desa Loning, Kemiri, Purworejo.
Accurate and Model-independent Radius Determination of Single FGK and M Dwarfs Using Gaia DR3 Data
Authors: Kiman Rocio , Brandt Timothy D. , Faherty Jacqueline K. , Popinchalk Mark 
Published: August 2024

Abstract
Measuring fundamental stellar parameters is key to fully comprehending the evolution of stars. However, current theoretical models overpredict effective temperatures, and underpredict radii, compared to observations of K and M dwarfs (radius inflation problem). In this work, we have developed a model-independent method to infer precise radii of single FGK and M dwarfs using Gaia DR3 parallaxes and photometry, and used it to study the radius inflation problem. We calibrated nine surface brightness–color relations for the three Gaia magnitudes and colors using a sample of stars with angular diameter measurements. We achieved an accuracy of 4% in our angular diameter estimations, which Gaia’s parallaxes allow us to convert to physical radii. We validated our method by comparing our radius measurements with literature samples and the Gaia DR3 catalog, which confirmed the accuracy of our method and revealed systematic offsets in the Gaia measurements. Moreover, we used a sample with measured Hα equivalent width (Hα EW), a magnetic activity indicator, to study the radius inflation problem. We demonstrated that active stars have larger radii than inactive stars, showing that radius inflation is correlated with magnetic activity. We found a correlation between the radius inflation of active stars and Hα EW for the mass bin 0.5 < M[M
⊙] ≤ 0.6, but we found no correlation for lower masses. This could be due to lack of precision in our radius estimation or a physical reason. Radius measurements with smaller uncertainties are necessary to distinguish between the two scenarios.
Performance of the SOAR Speckle Instrument
Authors: Tokovinin Andrei 
Published: August 2024

Abstract
The High Resolution Camera (HRCam) speckle imager at the 4.1 m Southern Astrophysical Research telescope is a highly productive instrument that has accumulated about 40K observations to date. Its performance (detected flux, level of the speckle signal, signal-to-noise ratio, and limiting magnitude) is studied here using both the actual data and realistic simulations, including the detector noise. In the calculation of the speckle power spectrum, signal clipping is essential to reduce the noise impact and maximize the sensitivity. Increasing exposure time of individual frames beyond 30 ms does not improve the limiting magnitude, which ranges from 11.5 to 14 mag under a seeing from 1.″6 to 0.″6 in the wide-band I filter. A gain of at least one magnitude is expected if the current electron multiplication CCD is replaced by a high-end CMOS detector with a subelectron readout noise. This study will help in planning, executing, and automating future speckle observations with HRCam and other speckle imagers.
Probe the Regolith Characteristics of Asteroids from 9 yr Infrared Observations of WISE/NEOWISE: A Case Study of The Main-belt Object (656) Beagle
Authors: Yu 余 Liang-Liang 亮亮 
Published: August 2024

Abstract
This work presents the data processing, fitting procedure, modeling, and analyzing of 9 yr infrared light curves provided by the WISE/NEOWISE telescope, by which the regolith characteristics of Main-belt Object (656) Beagle is studied. Beagle locates in the Themis family, and was proposed to be the parent of the first main-belt comet (MBC) 133P. We determine Beagle’s effective diameter

D

eff

=

57.3

−
2.2

+
4.5

km, geometric albedo

p

v

=

0.05

−
0.007

+
0.004

, mean roughness θ
RMS = 44 ± 4°, mean grain size

b
=

100

−
90

+
350

μ
m

, mean specific heat capacity c
p = 173 ∼ 516 J Kg−1 K−1, mean thermal conductivity κ = 0.7 ∼ 1.3 × 10−3 W m−1 K−1, and mean thermal inertia Γ = 14 ∼ 32 J m−2 s−0.5 K−1. The albedo of Beagle is a little anomalous that the albedos of Beagle’s neighboring asteroids are more close to (24) Themis, rather than Beagle itself. The W1-band near-infrared (NIR) light curves do not reveal significant heterogeneous NIR features on the surface of Beagle, being inconsistent with the expectation of a family parent that has members with diverse NIR spectral types. These results add new clues of Beagle probably being an interloper or a sister, rather than the parent of its neighboring asteroids including the famous MBC 133P, hence may lead to new scenarios about the origin of 133P. Besides, we found that asteroidal shape models from inversion of optical light curves are imperfect for modeling infrared lightcurves, thus could mislead evaluations of both the heterogeneity of regolith reflectivity at NIR and thermophysical characteristics at thermal infrared.
The Zwicky Transient Facility Bright Transient Survey. III. BTSbot: Automated Identification and Follow-up of Bright Transients with Deep Learning
Authors: Rehemtulla Nabeel , Miller Adam A. , Jegou Du Laz Theophile , Coughlin Michael W. , Fremling Christoffer , Perley Daniel A. , Qin Yu-Jing , Sollerman Jesper , Mahabal Ashish A. , Laher Russ R. , Riddle Reed , Rusholme Ben , Kulkarni Shrinivas R. 
Published: August 2024

Abstract
The Bright Transient Survey (BTS) aims to obtain a classification spectrum for all bright (m
peak ≤ 18.5 mag) extragalactic transients found in the Zwicky Transient Facility (ZTF) public survey. BTS critically relies on visual inspection (“scanning”) to select targets for spectroscopic follow-up, which, while effective, has required a significant time investment over the past ∼5 yr of ZTF operations. We present BTSbot, a multimodal convolutional neural network, which provides a bright transient score to individual ZTF detections using their image data and 25 extracted features. BTSbot is able to eliminate the need for daily human scanning by automatically identifying and requesting spectroscopic follow-up observations of new bright transient candidates. BTSbot recovers all bright transients in our test split and performs on par with scanners in terms of identification speed (on average, ∼1 hr quicker than scanners). We also find that BTSbot is not significantly impacted by any data shift by comparing performance across a concealed test split and a sample of very recent BTS candidates. BTSbot has been integrated into Fritz and Kowalski, ZTF’s first-party marshal and alert broker, and now sends automatic spectroscopic follow-up requests for the new transients it identifies. Between 2023 December and 2024 May, BTSbot selected 609 sources in real time, 96% of which were real extragalactic transients. With BTSbot and other automation tools, the BTS workflow has produced the first fully automatic end-to-end discovery and classification of a transient, representing a significant reduction in the human time needed to scan.
Planck Dust Polarization Power Spectra Are Consistent with Strongly Supersonic Turbulence
Authors: Stalpes Kye A. , Collins David C. , Huffenberger Kevin M. 
Published: August 2024

Abstract
The polarization of the cosmic microwave background is rich in information but obscured by foreground emission from the Milky Way’s interstellar medium (ISM). To uncover relationships between the underlying turbulent ISM and the foreground power spectra, we simulated a suite of driven, magnetized, turbulent models of the ISM, varying the fluid properties via the sonic Mach number,

M

S

, and magnetic (Alfvén) Mach number,

M

A

. We measure the power spectra of density (ρ), velocity (v), magnetic field (H), total projected intensity (T), parity-even polarization (E), and parity-odd polarization (B). We find that the slopes of all six quantities increase with

M

S

. Most increase with

M

A

, while the magnetic field spectrum steepens with

M

A

. By comparing spectral slopes of E and B to those measured by Planck, we infer typical values of

M

S

and

M

A

for the ISM. As the fluid velocity increases,

M

S

>
4

, the ratio of BB power to EE power increases to approach a constant value near the Planck-observed value of ∼0.5, regardless of the magnetic field strength. We also examine correlation coefficients between projected quantities, and find that r
TE ≈ 0.3, in agreement with Planck, for appropriate combinations of

M

S

and

M

A

. Finally, we consider parity-violating correlations r
TB and r
EB.
Observational Characteristics of Circumplanetary-mass-object Disks in the Era of James Webb Space Telescope
Authors: Sun 孙 Xilei 锡磊 , Huang 黄 Pinghui 平辉 , Dong 董 Ruobing 若冰 , Liu 刘 Shang-Fei 尚飞 
Published: August 2024

Abstract
Recent observations have confirmed circumplanetary disks (CPDs) embedded in parental protoplanetary disks (PPDs). On the other hand, planetary-mass companions and planetary-mass objects (PMOs) are likely to harbor their own accretion disks. Unlike PPDs, CPDs and other disks around planet analogs are generally too compact to be spatially resolved by current instrumentation. In this study, we generate over 4000 spectral energy distributions of circum-PMO disks (CPMODs) with various host temperature and disk properties, which can be categorized into four prototypes, i.e., full, pretransitional, transitional, and evolved CPMODs. We propose a classification scheme based on their near-to-mid-infrared colors. Using those CPMOD models, we synthesize JWST (NIRCam and MIRI) photometry for F444W, F1000W, and F2550W wide filters. We show that F444W−F1000W and F444−F2550W colors can be applied to distinguish different types of CPMODs, especially for those around hot hosts. Our results indicate that the ongoing and future JWST observations are promising to unveil structures and properties of CPMODs.
Flaring Stars in a Nontargeted Millimeter-wave Survey with SPT-3G
Authors: Tandoi C. , Guns S. , Foster A. , Ade P. A. R. , Anderson A. J. , Ansarinejad B. , Archipley M. , Balkenhol L. , Benabed K. , Bender A. N. , Benson B. A. , Bianchini F. , Bleem L. E. , Bouchet F. R. , Bryant L. , Camphuis E. , Carlstrom J. E. , Cecil T. W. , Chang C. L. , Chaubal P. , Chichura P. M. , Chou T.-L. , Coerver A. , Crawford T. M. , Cukierman A. , Daley C. , de Haan T. , Dibert K. R. , Dobbs M. A. , Doussot A. , Dutcher D. , Everett W. , Feng C. , Ferguson K. R. , Fichman K. , Galli S. , Gambrel A. E. , Gardner R. W. , Ge F. , Goeckner-Wald N. , Gualtieri R. , Guidi F. , Halverson N. W. , Hivon E. , Holder G. P. , Holzapfel W. L. , Hood J. C. , Huang N. , Kéruzoré F. , Knox L. , Korman M. , Kornoelje K. , Kuo C.-L. , Lee A. T. , Levy K. , Lowitz A. E. , Lu C. , Maniyar A. , Menanteau F. , Millea M. , Montgomery J. , Moon Y. , Nakato Y. , Natoli T. , Noble G. I. , Novosad V. , Omori Y. , Padin S. , Pan Z. , Paschos P. , Phadke K. A. , Prabhu K. , Qu Z. , Quan W. , Rahimi M. , Rahlin A. , Reichardt C. L. , Reuter C. , Rouble M. , Ruhl J. E. , Schiappucci E. , Smecher G. , Sobrin J. A. , Stark A. A. , Stephen J. , Suzuki A. , Thompson K. L. , Thorne B. , Trendafilova C. , Tucker C. , Umilta C. , Vieira J. D. , Wan Y. , Wang G. , Whitehorn N. , Wu W. L. K. , Yefremenko V. , Young M. R. , Zebrowski J. A. 
Published: August 2024

Abstract
We present a flare star catalog from 4 yr of nontargeted millimeter-wave survey data from the South Pole Telescope (SPT). The data were taken with the SPT-3G camera and cover a 1500 deg2 region of the sky from 20h40m0s to 3h20m0s in right ascension and from −42° to −70° in declination. This region was observed on a nearly daily cadence from 2019 to 2022 and chosen to avoid the plane of the galaxy. A short-duration transient search of this survey yields 111 flaring events from 66 stars, increasing the number of both flaring events and detected flare stars by an order of magnitude from the previous SPT-3G data release. We provide cross-matching to Gaia DR3, as well as matches to X-ray point sources found in the second ROSAT all-sky survey. We have detected flaring stars across the main sequence, from early-type A stars to M dwarfs, as well as a large population of evolved stars. These stars are mostly nearby, spanning 10–1000 pc in distance. Most of the flare spectral indices are constant or gently rising as a function of frequency at 95/150/220 GHz. The timescale of these events can range from minutes to hours, and the peak ν
L

ν
luminosities range from 1027 to 1031 erg s−1 in the SPT-3G frequency bands.
Closing the Net on Transient Sources of Ultrahigh-energy Cosmic Rays
Authors: Marafico Sullivan , Biteau Jonathan , Condorelli Antonio , Deligny Olivier , Bregeon Johan 
Published: August 2024

Abstract
The arrival directions of ultrahigh-energy cosmic rays (UHECRs) observed above 4 × 1019 eV provide evidence of localized excesses that are key to identifying their sources. We leverage the 3D matter distribution from optical and infrared surveys as a density model of UHECR sources, which are considered to be transient. Agreement of the sky model with UHECR data imposes constraints on both the emission rate per unit matter and the time spread induced by encountered turbulent magnetic fields. Based on radio measurements of cosmic magnetism, we identify the Local Sheet as the magnetized structure responsible for the kiloyear duration of UHECR bursts for an observer on Earth and find that the turbulence amplitude must be within 0.5–20 nG for a coherence length of 10 kpc. At the same time, the burst-rate density must be above 50 Gpc−3 yr−1 for Local Sheet galaxies to reproduce the UHECR excesses and below 5000 Gpc−3 yr−1 (30,000 Gpc−3 yr−1) for the Milky Way (Local Group galaxies) not to outshine other galaxies. For the transient emissions of protons and nuclei to match the energy spectra of UHECRs, the kinetic energy of the outflows responsible for UHECR acceleration must be below 4 × 1054 erg and above 5 × 1050 erg (2 × 1049 erg) if we consider the Milky Way (or not). The only stellar-sized transients that satisfy both Hillas’ and our criteria are long-duration gamma-ray bursts.
Radiation RMHD Accretion Flows around Spinning AGNs: A Comparative Study of MAD and SANE State
Authors: Aktar Ramiz , Pan Kuo-Chuan , Okuda Toru 
Published: August 2024

Abstract
In our study, we examine a 2D radiation, relativistic, magnetohydrodynamics accretion flow around a spinning supermassive black hole. We begin by setting an initial equilibrium torus around the black hole, with an embedded initial magnetic field inside the torus. The strength of the initial magnetic field is determined by the plasma beta parameter, which is the ratio of the gas pressure to the magnetic pressure. In this paper, we perform a comparative study of the magnetically arrested disc (MAD) and standard and normal evolution (SANE) states. We observe that the MAD state is possible for comparatively high initial magnetic field strength flow. Additionally, we also adopt a self-consistent two-temperature model to evaluate the luminosity and energy spectrum for our model. We observe that the total luminosity is mostly dominated by bremsstrahlung luminosity compared to the synchrotron luminosity due to the presence of a highly dense torus. We also identify similar quasi-periodic oscillations for both MAD and SANE states based on power-density spectrum analysis. Furthermore, our comparative study of the energy spectrum does not reveal any characteristic differences between MAD and SANE states. Last, we note that the MAD state is possible for both prograde and retrograde accretion flow.
Tracing Magnetic Fields with the Gradient Technique: Spatial Filtering Effect and Use of Interferometers
Authors: Hu Yue , Lazarian A. 
Published: August 2024

Abstract
Probing magnetic fields in astrophysical environments is both important and challenging. The Gradient Technique (GT) is a new tool for tracing magnetic fields, rooted in the properties of magnetohydrodynamic (MHD) turbulence and turbulent magnetic reconnection. In this work, we examine the performance of GT when applied to synthetic synchrotron emission and spectroscopic data obtained from sub-Alfvénic and trans-Alfvénic MHD simulations. We demonstrate the improved accuracy of GT in tracing magnetic fields in the absence of low spatial frequencies. Additionally, we apply a low-spatial-frequency filter to a diffuse neutral hydrogen region selected from the GALFA-H i survey. Our results show an increased alignment between the magnetic fields inferred from GT and the Planck 353 GHz polarization measurements.
A Cyclic Spectroscopy Scintillation Study of PSR B1937+21. I. Demonstration of Improved Scintillometry
Authors: Turner Jacob E. , Dolch Timothy , Cordes James M. , Ocker Stella K. , Stinebring Daniel R. , Chatterjee Shami , McLaughlin Maura A. , Catlett Victoria E. , Jessup Cody , Jones Nathaniel , Scheithauer Christopher 
Published: August 2024

Abstract
We use cyclic spectroscopy to perform high-frequency resolution analyses of multihour baseband Arecibo observations of the millisecond pulsar PSR B1937+21. This technique allows for the examination of scintillation features in far greater detail than is otherwise possible under most pulsar timing array observing setups. We measure scintillation bandwidths and timescales in each of eight subbands across a 200 MHz observing band in each observation. Through these measurements we obtain intra-epoch estimates of the frequency scalings for scintillation bandwidth and timescale. Thanks to our high-frequency resolution and the narrow scintles of this pulsar, we resolve scintillation arcs in the secondary spectra due to the increased Nyquist limit, which would not have been resolved at the same observing frequency with a traditional filterbank spectrum using NANOGrav’s current time and frequency resolutions, and the frequency-dependent evolution of scintillation arc features within individual observations. We observe the dimming of prominent arc features at higher frequencies, possibly due to a combination of decreasing flux density and the frequency dependence of the plasma refractive index of the interstellar medium. We also find agreement with arc curvature frequency dependence predicted by Stinebring et al. in some epochs. Thanks to the frequency-resolution improvement provided by cyclic spectroscopy, these results show strong promise for future such analyses with millisecond pulsars, particularly for pulsar timing arrays, where such techniques can allow for detailed studies of the interstellar medium in highly scattered pulsars without sacrificing the timing resolution that is crucial to their gravitational-wave detection efforts.
A High-resolution Imaging Survey of Massive Young Stellar Objects in the Magellanic Clouds
Authors: Kalari Venu M. , Salinas Ricardo , Zinnecker Hans , Rubio Monica , Herczeg Gregory , Andersen Morten 
Published: August 2024

Abstract
Constraints on the binary fraction of massive young stellar objects (mYSOs) are important for binary and massive star formation theory. Here, we present speckle imaging of 34 mYSOs located in the Large Magellanic Cloud (1/2 Z
⊙) and Small Magellanic Cloud (∼1/5 Z
⊙), probing projected separations in the 2000 to 20,000 au (at angular scales of 0.″02–0.″2) range, for stars above 8 M
⊙. We find two wide binaries in the Large Magellanic Cloud (from a sample of 23 targets), but none in a sample of 11 in the Small Magellanic Cloud, leading us to adopt a wide binary fraction of 9% ± 5% and <5%, respectively. We rule out a wide binary fraction greater than 35% in the Large Magellanic Cloud and 38% in the Small Magellanic Cloud at the 99% confidence level. This is in contrast to the wide binary fraction of mYSOs in the Milky Way (presumed to be 1 Z
⊙), which within the physical parameter space probed by this study is ∼15%–60% from the literature. We argue that while selection effects could be responsible for the lower binary fraction observed, it is more likely that there are underlying physical mechanisms responsible for the observed properties. This indicates that metallicity and environmental effects may influence the formation of wide binaries among massive stars. Future larger, more statistically significant samples of high-mass systems in low-metallicity environments for comparison to the Milky Way, are essential to confirm or repudiate our claim.
Time Profile Study of Type III Solar Radio Bursts Using Parker Solar Probe
Authors: Thapa Tulsi , Yan Yihua 
Published: August 2024

Abstract
Solar type III radio bursts are crucial indicators of energetic electron activity in the solar corona and interplanetary space. Our assessment of 43 interplanetary type III bursts, recorded by the FIELDS instrument on board the Parker Solar Probe during Encounters 05 to 11, has led to significant and complex findings. We have analyzed time profile features across a frequency range of 19–0.5 MHz, revealing dependencies on frequency and providing insights into duration, burst speeds, bandwidths, and drift rates. This novel analysis has unveiled a spectral index of −0.63 ± 0.04 for rise, −0.69 ± 0.03 for decay time, and −0.68 ± 0.03 for the total duration. We have determined the average electron beam velocities for front, middle, and back as 0.15c, 0.13c, and 0.08c, respectively. Our findings show that faster electron beams generate emissions with shorter duration. The average ratio of the front-to-back velocity is 1.87, and the ratio of front-to-middle velocity is 1.23. We have also discovered a strong relationship between burst duration with rise, peak, and decay times, particularly pronounced with decay time (correlation coefficient = 0.95). This indicates that the entire temporal profile, including rise, peak, and decay phases, collectively contributes to event duration and is not solely influenced by external factors like plasma conditions or electron beam dynamics but also by internal burst processes. These complex findings shed light on the physical mechanisms governing burst dynamics, revealing intricate interactions between electron beam characteristics and observed temporal and spectral traits of type III solar radio bursts.