bluuebunny/crossref_metadata_2025_split huggingface dataset:
Further perceptions of probability: Accurate, stepwise updating is contingent on prior information about the task and the response mode
Authors: Forsgren Mattias , Juslin Peter , van den Berg Ronald 
Published: November 2024

AbstractTo adapt to an uncertain world, humans must learn event probabilities. These probabilities may be stationary, such as that of rolling a 6 on a die, or changing over time, like the probability of rainfall over the year. Research on how people estimate and track changing probabilities has recently reopened an old epistemological issue. A small, mostly recent literature finds that people accurately track the probability and change their estimates only occasionally, resulting in staircase-shaped response patterns. This has been taken as evidence that people entertain beliefs about unknown, distal states of the world, which are tested against observations to produce discrete shifts between hypotheses. That idea stands in contrast to the claim that people learn by continuously updating associations between observed events. The purpose of this article is to investigate the generality and robustness of the accurate, staircase-shaped pattern. In two experiments, we find that the response pattern is contingent on the response mode and prior information about the generative process. Participants exist on continua of accuracy and staircase-ness and we only reproduce previous results when changing estimates is effortful and prior information is provided—the specific conditions of previous experiments. We conclude that explaining this solely through either hypotheses or associations is untenable. A complete theory of probability estimation requires the interaction of three components: (i) online tracking of observed data, (ii) beliefs about the unobserved “generative process,” and (iii) a response updating process. Participants’ overt estimates depend on how the specific task conditions jointly determine all three.
Pengaruh Pertumbuhan Penjualan, Intensitas Aset, Kualitas Audit, dan Profitabilitas Terhadap Penghindaran Pajak Perusahaan Pertambangan
Authors: Atikah Filzah Danuarti , Ariani Kurnia Rina 
Published: November 2024

Penelitian ini bertujuan untuk mengevaluasi dampak dari pertumbuhan penjualan, intensitas aset, kualitas audit, dan profitabilitas terhadap penghindaran pajak di perusahaan-perusahaan pertambangan yang terdaftar di Bursa Efek Indonesia (BEI) selama periode 2021-2023. Penghindaran pajak diartikan sebagai strategi yang digunakan perusahaan untuk mengurangi kewajiban pajak melalui perencanaan pajak yang sah, meskipun sering kali berdampak pada penurunan penerimaan negara. Metode yang digunakan dalam penelitian ini adalah kuantitatif dengan memanfaatkan data sekunder dari laporan keuangan perusahaan yang terdaftar di BEI. Untuk analisis data, digunakan regresi linier berganda guna mengidentifikasi pengaruh variabel independen yaitu pertumbuhan penjualan, intensitas aset, kualitas audit dan profitabilitas, dan terhadap variabel dependen, yaitu penghindaran pajak. Pengukuran penghindaran pajak dilakukan dengan menggunakan proxy effective tax rate (ETR). Diharapkan hasil penelitian ini dapat memberikan bukti empiris mengenai faktor-faktor yang memengaruhi penghindaran pajak dalam sektor pertambangan di Indonesia, serta menjadi acuan bagi manajemen perusahaan dalam merumuskan strategi pengelolaan pajak.
Correcting Turbulence-induced Errors in Fiber Positioning for the Dark Energy Spectroscopic Instrument
Authors: Schlafly E. F. , Guy J. , Honscheid K. , Kent S. , Koposov S. E. , Aguilar J. , Ahlen S. , Bailey S. , Brooks D. , Claybaugh T. , Dawson K. , Doel P. , Fanning K. , Finkbeiner D. P. , Font-Ribera A. , Forero-Romero J. E. , Gontcho A Gontcho S. , Gutierrez G. , Kirkby D. , Kisner T. , Kremin A. , Landriau M. , Lasker J. , Le Guillou L. , Levi M. E. , de la Macorra A. , Martini P. , Meisner A. , Miquel R. , Moustakas J. , Niz G. , Prada F. , Rossi G. , Sanchez E. , Schubnell M. , Sharples R. , Sprayberry D. , Tarlé G. , Weaver B. A. , Zou H. ,   DESI
Published: November 2024

Abstract
Highly multiplexed, robotic, fiber-fed spectroscopic surveys are observing tens of millions of stars and galaxies. For many systems, accurate positioning relies on imaging the fibers in the focal plane and feeding that information back to the robotic positioners to correct their positions. Inhomogeneities and turbulence in the air between the focal plane and the imaging camera can affect the measured positions of fibers, limiting the accuracy with which fibers can be placed on targets. For the Dark Energy Spectroscopic Instrument, we dramatically reduced the effect of turbulence on measurements of positioner locations in the focal plane by taking advantage of stationary positioners and the correlation function of the turbulence. We were able to reduce positioning errors from 7.3 to 3.5 μm, speeding the survey by 1.6% under typical conditions.
New Moons of Uranus and Neptune from Ultradeep Pencil-beam Surveys
Authors: Sheppard Scott S. , Tholen David J. , Brozovic Marina , Jacobson Robert , Trujillo Chadwick A. , Lykawka Patryk Sofia , Alexandersen Mike 
Published: November 2024

Abstract
We have conducted extremely ultradeep pencil-beam observations for new satellites around both Uranus and Neptune. Tens of images on several different nights in 2021, 2022, and 2023 were obtained, shifted, and added together to reach as faint as 26.9 and 27.2 mag in the r band around Uranus and Neptune, respectively. One new moon of Uranus, S/2023 U1, and two new moons of Neptune, S/2021 N1 and S/2002 N5, were found. S/2023 U1 was 26.6 mag, is about 7 km in diameter, and has a distant, eccentric, and inclined retrograde orbit similar to Caliban and Stephano, implying these satellites are fragments from a once larger parent satellite. S/2021 N1 was 26.9 mag, about 14 km in size, and has a retrograde orbit similar to Neso and Psamathe, indicating they are a dynamical family. We find S/2021 N1 is in Kozai–Lidov orbital resonance. S/2002 N5 was 25.9 mag, is about 23 km in size, and it makes a family of distant prograde satellites with Sao and Laomedeia. This survey mostly completes the outer satellites of Uranus to about 8 km and Neptune to about 14 km in diameter. The size distributions of satellite dynamical families around the giant planets shows a strong steepening in the power-law size distribution smaller than 5 km in diameter. The satellites of a family become much more common at diameters smaller than 5 km and their size distribution is consistent with a collisional breakup of a once larger parent satellite.
Generating X-Ray Transit Profiles with Batman
Authors: King George W. , Corrales Lía R. , Wheatley Peter J. , Cilley Raven C. , Hollands Mark 
Published: November 2024

Abstract
We present an adaptation of the exoplanet transit model code batman, in order to permit the generation of X-ray transits. Our underlying extended coronal model assumes an isothermal plasma that is radially symmetric. While this ignores the effect of bright, active regions, observations of transits in X-rays will require averaging across multiple epochs of data for the foreseeable future, significantly reducing the importance of more complex modeling. Our publicly available code successfully generates the predicted W-shaped transit profile in X-rays due to the optically thin nature of the emission, which concentrates the expected observational emission around the limb of the photospheric stellar disk. We provide some examples based on the best known X-ray transit target, HD 189733 b, and examine the effect of varying the planet size, coronal temperature, and impact parameter on the resulting transit profile. We also derived scaling relationships for how the overall transit detectability is affected by changing these parameters. Over most of the parameter space, we find that the detectability scales linearly with the cross-sectional area of the planet in X-rays. The relationship with increasing coronal temperature is less fixed, but averages out to a power law with slope −1/4 except when the impact parameter is high. Indeed, varying impact parameter has little effect on detectability at all until it approaches unity.
Acoustic Wake in a Singular Isothermal Profile: Dynamical Friction and Gravitational-wave Emission
Authors: Eytan Gali , Desjacques Vincent , Buehler Robin 
Published: November 2024

Abstract
We consider the motion of a circularly moving perturber in a self-gravitating, collisional system with a spherically symmetric density profile. We concentrate on the singular isothermal sphere, which, despite its pathological features, admits a simple polarization function in linear response theory. This allows us to solve for the acoustic wake trailing the perturber and the resulting dynamical friction, in the limit where the self-gravity of the response can be ignored. In a steady state and for subsonic velocities v

p
< c

s
, the dynamical friction torque

F

φ

∝

v

p

3

is suppressed for perturbers orbiting in an isothermal sphere relative to the infinite, homogeneous medium expectation F

φ
∝ v

p
. For highly supersonic motions, both expectations agree and are consistent with a local approximation to the gravitational torque. At fixed resolution (a given Coulomb logarithm), the response of the system is maximal for Mach numbers near the constant circular velocity of the singular isothermal profile. This resonance maximizes the gravitational-wave (GW) emission produced by the trailing acoustic wake. For an inspiral around a massive black hole of mass 106
M
⊙ located at the center of a (truncated) isothermal sphere, this GW signal could be comparable to the vacuum GW emission of a black hole binary at subnanohertz frequencies when the small black hole enters the Bondi sphere of the massive one. The exact magnitude of this effect depends on departures from hydrostatic equilibrium and on the viscosity present in any realistic astrophysical fluid, which are not included in our simplified description.
Probing the Circumstellar Environment of the Highly Luminous Type IIn Supernova ASASSN-14il
Authors: Dukiya Naveen , Gangopadhyay Anjasha , Misra Kuntal , Hosseinzadeh Griffin , Bostroem K. Azalee , Ailawadhi Bhavya , Howell D. Andrew , Valenti Stefano , Arcavi Iair , McCully Curtis , Gupta Archana 
Published: November 2024

Abstract
We present long-term photometric and spectroscopic studies of circumstellar material (CSM)–ejecta interacting supernova (SN) ASASSN-14il in the galaxy PGC 3093694. The SN reaches a peak r-band magnitude of ∼−20.3 ± 0.2 mag, rivaling SN 2006tf and SN 2010jl. The multiband and the pseudo-bolometric lightcurves show a plateau lasting ∼50 days. Semi-analytical CSM interaction models can match the high luminosity and decline rates of the lightcurves but fail to faithfully represent the plateau region and the bumps in the lightcurves. The spectral evolution resembles a typical Type IIn SN dominated by CSM interaction, showing blue continuum and narrow Balmer lines. The lines are dominated by electron scattering at early epochs. The signatures of the underlying ejecta are visible as the broad component in the Hα profile from as early as day 50, hinting at asymmetry in the CSM. A narrow component is persistent throughout the evolution. The SN shows remarkable photometric and spectroscopic similarity with SN 2015da. However, the different polarization in ASASSN-14il compared to SN 2015da suggests an alternative viewing angle. The late-time blueshift in the Hα profile supports dust formation in the post-shock CSM or ejecta. The mass-loss rate of 2–7 M
⊙ yr−1 suggests a luminous blue variable progenitor in an eruptive phase for ASASSN-14il.
Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Luo Yang , Shlosman Isaac 
Published: November 2024

Abstract
We have used high-resolution zoom-in simulations of direct collapse to supermassive black hole (SMBH) seeds within dark mater halos in the presence of magnetic fields generated during the collapse, down to 10−5 pc or 2 au. We confirm an efficient amplification of magnetic field during collapse, the formation of a geometrically thick self-gravitating accretion disk inside 0.1 pc, and damping of fragmentation in the disk by the field. This disk differs profoundly from SMBH accretion disks. We find the following: (1) The accretion disk is subject to the magnetorotational instability, which further amplifies the field to near equipartition. No artificial seeding of the disk field has been used. (2) The equipartition toroidal field changes its polarity in the midplane. (3) The nonlinear Parker instability develops, accompanied by the vertical buckling of the field lines, which injects material above the disk, leading to an increase in the disk scale height. (4) With the Coriolis force producing a coherent helicity above the disk, the vertical poloidal field has been generated and amplified. (5) We estimate that the associated outflow will be most probably squashed by accretion. The resulting configuration consists of a magnetized disk with β ≳ 0.1 and its magnetosphere with β ≪ 1, where β = P
th/P

B
is the ratio of thermal to magnetic energy density. (6) The disk is highly variable, due to feeding by variable accretion flow, and strong vortical motions are present. (7) Finally, the negative gradient of the total vertical stress drives an equatorial outflow sandwiched by an inward accretion flow.
Benchmarking Dielectronic Recombination Rate Coefficients for Carbon-like Ca14+
Authors: Zhang C. Y. , Yan B. S. , Wang K. , Si R. , Yao K. , Ma W. L. , Huang Z. K. , Wen W. Q. , Ma X. W. , Zhu L. F. , Chen C. Y. , Badnell N. R. 
Published: November 2024

Abstract
Dielectronic recombination (DR) rate coefficients for C-like Ca14+ were measured by Wen et al. at the electron cooler storage ring in Lanzhou, China. The measured DR rate coefficients from 0 to 92 eV cover most of the DR resonances associated with the 2s
22p
2 → 2s
22p
2 and 2s
22p
2 → 2s2p
3 core transitions. In addition, Wen et al. reported theoretical results calculated with the Flexible Atomic Code (FAC) and AUTOSTRUCTURE (AS). However, these theoretical results show widespread and significant differences from the measured DR spectrum in both resonance energies and strengths, as well as between each other. In the present work, we uncover the reasons behind these large differences, both theoretical and experimental. The new FAC and AS results reproduce the observed spectrum in detail, especially at resonance energies below 8 eV, and they are in very close agreement with each other. The present plasma rate coefficients agree with the experimentally determined values to within 20% and 2% in the photoionized plasma (PP) and collisional ionized plasma (CP) temperature ranges, respectively. This is in contrast to the previous theoretical results, which showed differences with the experiment of up to ∼40% over the PP temperature range. The present FAC and AS results agree with each other within 5% in the PP and CP temperature ranges. Thus, the theoretical uncertainty is greatly reduced for the DR of Ca14+ and the present benchmarking with the experiment gives confidence to data users modeling non–local thermodynamic equilibrium plasma.
Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Tu Zhijun , Wang Shu , Liu Jifeng 
Published: November 2024

Abstract
We present a comprehensive analysis of 20 T and Y dwarfs using spectroscopy from the Near-Infrared Spectrograph (NIRSpec) CLEAR/PRISM and Mid-Infrared Instrument (MIRI) low-resolution spectrometer instruments on the James Webb Space Telescope. To characterize the atmospheric parameters, we utilize two atmospheric model grids: the Sonora Elf Owl and ATMO2020++. The effective temperatures derived from the two models are relatively consistent, and metallicities are both close to solar values. However, significant discrepancies are found in other parameters, particularly in surface gravity, with the values obtained from the Sonora Elf Owl models typically being about 1 dex lower than those from the ATMO2020++ models. Further comparisons using the ATMO2020 models highlight that the adiabatic convective process introduced in the ATMO2020++ models has a significant impact on the determination of surface gravity. Using the fitted effective temperatures and absolute parallaxes from the literature, we derive radii for the brown dwarfs, which range from approximately 0.8–1.2 R
Jup. The estimated masses and ages, derived using evolutionary tracks, indicate that most brown dwarfs in our sample have masses below 30 M
Jup and are younger than 6 Gyr. Specifically, Y dwarfs have masses ranging from 2 to 20 M
Jup and ages between 0.1 and 6.7 Gyr. In addition, we discuss the determination of atmospheric parameters using only NIRSpec or MIRI spectra. Comparisons with results from the combined spectra show that the effective temperatures and surface gravities derived solely from NIRSpec spectra are largely consistent with those obtained from the combined spectra.
“Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability
Authors: Chang Eonho , Youdin Andrew N. 
Published: November 2024

Abstract
The Rossby wave instability (RWI) is the fundamental nonaxisymmetric radial shear instability in disks. The RWI can facilitate disk accretion, set the shape of planetary gaps, and produce large vortices. It arises from density and/or temperature features, such as radial gaps, bumps, or steps. A general, sufficient condition to trigger the RWI is lacking, which we address by studying the linear RWI in a suite of simplified models, including incompressible and compressible shearing sheets and global, cylindrical disks. We focus on enthalpy amplitude and width as the fundamental properties of disk features with various shapes. We find analytic results for the RWI boundary and growth rates across a wide parameter space, in some cases with exact derivations and in others as a description of numerical results. Features wider than a scale height generally become unstable about halfway to Rayleigh instability, i.e., when the squared epicyclic frequency is about half the Keplerian value, reinforcing our previous finding. RWI growth rates approximately scale as enthalpy amplitude to the 1/3 power, with a weak dependence on width, across much of the parameter space. Global disk curvature affects wide planetary gaps, making the outer gap edge more susceptible to the RWI. Our simplified models are barotropic and height integrated, but the main results should carry over to more complex and realistic scenarios.
GTC Optical/Near-infrared Upper Limits and NICER X-Ray Analysis of SGR J1935+2154 for the Outburst in 2022
Authors: Shao Yi-Xuan , Zhou Ping , Li Xiang-Dong , Zhang Bin-Bin , Castro-Tirado Alberto Javier , Wang Pei , Li Di , Zhang Zeng-Hua , Zhang Zi-Jian , Hu You-Dong , Pandey Shashi B. 
Published: November 2024

Abstract
The Galactic magnetar SGR J1935+2154 has undergone another outburst since 2022 October 10. We present the results of searching for an optical/near-infrared (NIR) counterpart of SGR J1935+2154 before and during this outburst. No counterpart was detected at the magnetar’s position in

r
′

and

z
′

bands, providing stringent upper limits of

r
′
≳
28.65

and

z
′
≳
26.27

. Using archival X-ray data from NICER, we investigated the properties of the bursts and the spectral evolution of persistent emission. The burst flux F showed a power-law distribution of N ∝ F
−0.76±0.10 for flux ≳2.6 × 10−9erg cm−2 s−1, while the temperature and radius followed a log-normal distribution with

kT
=

1.63

−
0.50

+
0.73

keV

and

R

bb

=

4.35

−
1.35

+
1.95

km

, respectively. The persistent flux evolution experienced a quick decay and an enhancement ∼27 days after the Burst Alert Telescope trigger. Using the NIR and X-ray emission, together with the Gran Telescopio Canarias optical/NIR upper limits, we discussed the origin of the NIR emission from the magnetar based on the fallback disk model and magnetosphere model. We found that either model cannot be ruled out with currently available data. Further mid-infrared observations are needed to find out the mechanism for producing the NIR emission from SGR J1935+2154.
A SPectroscopic Survey of Biased Halos In the Reionization Era (ASPIRE): JWST Supports Earlier Reionization around [O iii] Emitters
Authors: Jin Xiangyu , Yang Jinyi , Fan Xiaohui , Wang Feige , Kakiichi Koki , Meyer Romain A. , Becker George D. , Zou Siwei , Bañados Eduardo , Champagne Jaclyn B. , D’Odorico Valentina , Yue Minghao , Bosman Sarah E. I. , Cai Zheng , Eilers Anna-Christina , Hennawi Joseph F. , Jun Hyunsung D. , Li Mingyu , Li Zihao , Liu 刘 Weizhe 伟哲 , Pudoka Maria , Satyavolu Sindhu , Sun Fengwu , Tee Wei Leong , Wu Yunjing 
Published: November 2024

Abstract
Understanding when and how reionization happened is crucial for studying the early structure formation and the properties of the first galaxies in the Universe. At z > 5.5, the observed intergalactic medium (IGM) optical depth shows a significant scatter, indicating an inhomogeneous reionization process. However, the nature of the inhomogeneous reionization remains debated. A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE) is a JWST Cycle 1 program that has spectroscopically identified >400 [O iii] emitters in 25 quasar fields at z > 6.5. Combined with deep ground-based optical spectroscopy of ASPIRE quasars, the ASPIRE program provides the current largest sample for IGM-galaxy connection studies during cosmic reionization. We present the first results of IGM effective optical depth measurements around [O iii] emitters using 14 ASPIRE quasar fields. We find the IGM transmission is tightly related to reionization era galaxies to the extent that a significant excess of Lyα transmission exists around [O iii] emitters. We measure the stacked IGM effective optical depth of IGM patches associated with [O iii] emitters and find they reach the same IGM effective optical depth at least d
z ∼ 0.1 ahead of those IGM patches where no [O iii] emitters are detected, supporting earlier reionization around [O iii] emitters. Our results indicate an enhancement in IGM Lyα transmission around [O iii] emitters at scales beyond 25 h
−1 cMpc, consistent with the predicted topology of reionization from fluctuating UV background models.