bluuebunny/crossref_metadata_2025_split huggingface dataset:
การพัฒนาโมดูลตรวจวัดคุณภาพน้ำในเวลาจริงแบบเครือข่าย
Authors: สื่อสุวรรณ วิศวะ , จิตตวิสุทธิกุล พงษ์ดนัย , วสุริย์ บุญธง 
Published: July 2023

ในปัจจุบันการบริหารการจัดการคุณภาพน้ำ เป็นส่วนสำคัญสำหรับการเพาะเลี้ยงสัตว์น้ำให้ได้คุณภาพและเหมาะสมคุ้มค่าต่อการลงทุน ดังนั้นโครงการการพัฒนาโมดูลตรวจวัดคุณภาพน้ำในเวลาจริงแบบเครือข่ายสำหรับกลุ่มบ่อเลี้ยงในฟาร์มเลี้ยงสัตว์น้ำ จึงมีวัตถุประสงค์ด้วยกันสองประการ ได้แก่ การออกแบบระบบเพื่อวัดคุณภาพน้ำแบบเรียลไทม์บนระบบเครือข่าย และเพื่อวัดประสิทธิภาพความคุ้มค่าทางเศรษฐศาสตร์รวมไปถึงการถ่ายทอดเทคโนโลยีในเชิงพาณิชย์ ซึ่งผลการดำเนินงานพบว่า โมดูลที่พัฒนาขึ้นสามารถตรวจวัดค่าออกซิเจนละลายในน้ำ ค่าความเป็นกรด-ด่าง ค่าความเค็ม และอุณหภูมิ ได้โดยพบว่า ในช่วงเวลาวิกฤติ (22.00-07.00 น.) ค่าเฉลี่ยของออกซิเจนละลายในน้ำ มีค่าเฉลี่ยต่ำกว่า 5.8 มิลลิกรัมต่อลิตร โดยมีค่าเบี่ยงเบนมาตรฐานตลอดการวัดเท่ากับ 0.168 ค่าเฉลี่ยของค่าความเป็นกรด-ด่างมีค่าเท่ากับ 5.97 โดยมีค่าเบี่ยงเบนมาตรฐานตลอดการวัดเท่ากับ 0.114 ค่าเฉลี่ยของค่าความเค็มมีค่าคงที่เท่ากับ 0.477 ส่วนในพันส่วน และค่าเฉลี่ยของอุณหภูมิค่าเท่ากับ 28.63 องศาเซลเซียสโดยมีค่าเบี่ยงเบนมาตรฐานตลอดการวัดเท่ากับ 0.203 ซึ่งระบบที่พัฒนาขึ้นสามารถจัดเก็บหรือรวบรวมข้อมูลตามเวลาจริง และความคุ้มค่าทางเศรษฐศาสตร์ที่ได้ปรากฏว่ามีค่า PBP = 0.925, NPV=43,200 บาท/ปี, จุดคุ้มทุนจะต้องผลิต 1,702 กิโลกรัมต่อปี
Overfitting Affects the Reliability of Radial Velocity Mass Estimates of the V1298 Tau Planets
Authors: Blunt Sarah , Carvalho Adolfo , David Trevor J. , Beichman Charles , Zink Jon K. , Gaidos Eric , Behmard Aida , Bouma Luke G. , Cody Devin , Dai Fei , Foreman-Mackey Daniel , Grunblatt Sam , Howard Andrew W. , Kosiarek Molly , Knutson Heather A. , Rubenzahl Ryan A. , Beard Corey , Chontos Ashley , Giacalone Steven , Hirano Teruyuki , Johnson Marshall C. , Lubin Jack , Akana Murphy Joseph M. , Petigura Erik A , Van Zandt Judah , Weiss Lauren 
Published: July 2023

Abstract
Mass, radius, and age measurements of young (≲100 Myr) planets have the power to shape our understanding of planet formation. However, young stars tend to be extremely variable in both photometry and radial velocity (RV) measurements, which makes constraining these properties challenging. The V1298 Tau system of four ∼0.5 R
J planets transiting a pre-main-sequence star presents an important, if stress-inducing, opportunity to observe and measure directly the properties of infant planets. Suárez Mascareño et al. published radial-velocity-derived masses for two of the V1298 Tau planets using a state-of-the-art Gaussian process regression framework. The planetary densities computed from these masses were surprisingly high, implying extremely rapid contraction after formation in tension with most existing planet-formation theories. In an effort to constrain further the masses of the V1298 Tau planets, we obtained 36 RVs using Keck/HIRES, and analyzed them in concert with published RVs and photometry. Through performing a suite of cross-validation tests, we found evidence that the preferred model of Suárez Mascareño et al. suffers from overfitting, defined as the inability to predict unseen data, rendering the masses unreliable. We detail several potential causes of this overfitting, many of which may be important for other RV analyses of other active stars, and recommend that additional time and resources be allocated to understanding and mitigating activity in active young stars such as V1298 Tau.
Accurate and Efficient Photoeccentric Transit Modeling
Authors: MacDougall Mason G. , Gilbert Gregory J. , Petigura Erik A. 
Published: July 2023

Abstract
A planet’s orbital eccentricity is fundamental to understanding the present dynamical state of a system and is a relic of its formation history. There is high scientific value in measuring the eccentricities of Kepler and Transiting Exoplanet Survey Satellite (TESS) planets given the sheer size of these samples and the diversity of their planetary systems. However, Kepler and TESS light curves typically only permit robust determinations of the planet-to-star radius ratio r, orbital period P, and transit midpoint t
0. Three other orbital properties, including the impact parameter b, eccentricity e, and argument of periastron ω, are more challenging to measure because they are all encoded in the light curve through subtle effects on a single observable—the transit duration T
14. In Gilbert et al., we showed that a five-parameter transit description {P, t
0, r, b, T
14} naturally yields unbiased measurements of r and b. Here, we build upon our previous work and introduce an accurate and efficient prescription to measure e and ω. We validate this approach through a suite of injection-and-recovery experiments. Our method agrees with previous approaches that use a seven-parameter transit description {P, t
0, r, b, ρ
⋆, e, ω}, which explicitly fits the eccentricity vector and mean stellar density. The five-parameter method is simpler than the seven-parameter method and is “future-proof” in that posterior samples can be quickly reweighted (via importance sampling) to accommodate updated priors and updated stellar properties. This method thus circumvents the need for an expensive reanalysis of the raw photometry, offering a streamlined path toward large-scale population analyses of the eccentricity from transit surveys.
Analytic Post-Newtonian Astrometric and Spectroscopic Models of Orbits around Black Holes
Authors: Hyman Sóley Ó. , Psaltis Dimitrios , Özel Feryal 
Published: July 2023

Abstract
Observations of the S stars, the cluster of young stars in the inner 0.1 pc of the Galactic center, have been crucial in providing conclusive evidence for a supermassive black hole at the center of our galaxy. Since some of the stars have orbits less than that of a typical human lifetime, it is possible to observe multiple orbits and test the weak-field regime of general relativity. Current calculations of orbits require relatively slow and expensive computations in order to perform numerical integrations for the position and momentum of each star at each observing time. In this paper, we present a computationally efficient, first-order post-Newtonian model for the astrometric and spectroscopic data gathered for the S stars. We find that future, 30 m class telescopes—and potentially even current large telescopes with very high spectroscopic resolution—may be able to detect the Shapiro effect for an S star in the next decade or so.
RadioAstron Space VLBI Imaging of the Jet in M87. I. Detection of High Brightness Temperature at 22 GHz
Authors: Kim Jae-Young , Savolainen Tuomas , Voitsik Petr , Kravchenko Evgeniya V. , Lisakov Mikhail M. , Kovalev Yuri Y. , Müller Hendrik , Lobanov Andrei P. , Sokolovsky Kirill V. , Bruni Gabriele , Edwards Philip G. , Reynolds Cormac , Bach Uwe , Gurvits Leonid I. , Krichbaum Thomas P. , Hada Kazuhiro , Giroletti Marcello , Orienti Monica , Anderson James M. , Lee Sang-Sung , Sohn Bong Won , Zensus J. Anton 
Published: July 2023

Abstract
We present results from the first 22 GHz space very long baseline interferometric (VLBI) imaging observations of M87 by RadioAstron. As a part of the Nearby AGN Key Science Program, the source was observed in 2014 February at 22 GHz with 21 ground stations, reaching projected (u, v) spacings up to ∼11 Gλ. The imaging experiment was complemented by snapshot RadioAstron data of M87 obtained during 2013–2016 from the AGN Survey Key Science Program. Their longest baselines extend up to ∼25 Gλ. For all of these measurements, fringes are detected only up to ∼2.8 Earth diameter or ∼3 Gλ baseline lengths, resulting in a new image with angular resolution of ∼150 μas or ∼20 Schwarzschild radii spatial resolution. The new image not only shows edge-brightened jet and counterjet structures down to submilliarcsecond scales but also clearly resolves the VLBI core region. While the overall size of the core is comparable to those reported in the literature, the ground-space fringe detection and slightly superresolved RadioAstron image suggest the presence of substructures in the nucleus, whose minimum brightness temperature exceeds

T

B
,
min

∼

10

12

K. It is challenging to explain the origin of this record-high

T

B
,
min

value for M87 by pure Doppler boosting effect with a simple conical jet geometry and known jet speed. Therefore, this can be evidence for more extreme Doppler boosting due to a blazar-like small jet viewing angle or highly efficient particle acceleration processes occurring already at the base of the outflow.
Buckyball-metal Complexes as Potential Carriers of Astronomical Unidentified Infrared Emission Bands
Authors: Hou Gao-Lei , Lushchikova Olga V. , Bakker Joost M. , Lievens Peter , Decin Leen , Janssens Ewald 
Published: July 2023

Abstract
Efforts over 40 yr still leave the source of astronomical infrared emission bands largely unidentified. Here, we report the first laboratory infrared (6–25 μm) spectra of gas-phase fullerene-metal complexes, [C60-Metal]+ (Metal = Fe, V) and show with density functional theory calculations that complexes of C60 with cosmically abundant metals, including Li, Na, K, Mg, Ca, Al, V, and Fe, all have similar spectral patterns. Comparison with observational infrared spectra from several fullerene-rich planetary nebulae demonstrates a strong positive linear cross-correlation. The infrared features of [C60-Metal]+ coincide with four bands attributed earlier to neutral C60 bands and in addition also with several bands unexplained to date. Abundance and collision theory estimates indicate that [C60-Metal]+ could plausibly form and survive in astrophysical environments. Hence, [C60-Metal]+ are proposed as promising carriers, in supplement to C60, of observational bands, potentially representing the largest molecular species in space other than C60, C60
+, and C70.
X-Ray Activity Variations and Coronal Abundances of the Star–Planet Interaction Candidate HD 179949
Authors: Acharya Anshuman , Kashyap Vinay L. , Saar Steven H. , Singh Kulinder Pal , Cuntz Manfred 
Published: July 2023

Abstract
We carry out detailed spectral and timing analyses of the Chandra X-ray data of HD 179949, a prototypical example of a star with a close-in giant planet with possible star–planet interaction (SPI) effects. We find a low coronal abundance A(Fe)/AH) ≈ 0.2 relative to the solar photospheric baseline of Anders & Grevesse, and significantly lower than the stellar photosphere as well. We further find low abundances of high first ionization potential (FIP) elements A(O)/A(Fe) ≲ 1, A(Ne)/A(Fe) ≲ 0.1, but with indications of higher abundances of A(N)/A(Fe) ≫ 1, A(Al)/A(Fe) ≲ 10. We estimate a FIP bias for this star in the range ≈ − 0.3 to −0.1, larger than the ≲ −0.5 expected for stars of this type, but similar to stars hosting close-in hot Jupiters. We detect significant intensity variability over timescales ranging from 100 s to 10 ks, and also evidence for spectral variability over timescales of 1–10 ks. We combine the Chandra flux measurements with Swift and XMM-Newton measurements to detect periodicities, and determine that the dominant signal is tied to the stellar polar rotational period, consistent with expectations that the corona is rotational-pole dominated. We also find evidence for periodicity at both the planetary orbital frequency and at its beat frequency with the stellar polar rotational period, suggesting the presence of a magnetic connection between the planet and the stellar pole. If these periodicities represent an SPI signal, it is likely driven by a quasi-continuous form of heating (e.g., magnetic field stretching) rather than sporadic, hot, impulsive flare-like reconnections.
pygwb: A Python-based Library for Gravitational-wave Background Searches
Authors: Renzini Arianna I. , Romero-Rodríguez Alba , Talbot Colm , Lalleman Max , Kandhasamy Shivaraj , Turbang Kevin , Biscoveanu Sylvia , Martinovic Katarina , Meyers Patrick , Tsukada Leo , Janssens Kamiel , Davis Derek , Matas Andrew , Charlton Philip , Liu Guo-Chin , Dvorkin Irina , Banagiri Sharan , Bose Sukanta , Callister Thomas , De Lillo Federico , D’Onofrio Luca , Garufi Fabio , Harry Gregg , Lawrence Jessica , Mandic Vuk , Macquet Adrian , Michaloliakos Ioannis , Mitra Sanjit , Pham Kiet , Poggiani Rosa , Regimbau Tania , Romano Joseph D. , van Remortel Nick , Zhong Haowen 
Published: July 2023

Abstract
The collection of gravitational waves (GWs) that are either too weak or too numerous to be individually resolved is commonly referred to as the gravitational-wave background (GWB). A confident detection and model-driven characterization of such a signal will provide invaluable information about the evolution of the universe and the population of GW sources within it. We present a new, user-friendly, Python-based package for GW data analysis to search for an isotropic GWB in ground-based interferometer data. We employ cross-correlation spectra of GW detector pairs to construct an optimal estimator of the Gaussian and isotropic GWB, and Bayesian parameter estimation to constrain GWB models. The modularity and clarity of the code allow for both a shallow learning curve and flexibility in adjusting the analysis to one’s own needs. We describe the individual modules that make up pygwb, following the traditional steps of stochastic analyses carried out within the LIGO, Virgo, and KAGRA Collaboration. We then describe the built-in pipeline that combines the different modules and validate it with both mock data and real GW data from the O3 Advanced LIGO and Virgo observing run. We successfully recover all mock data injections and reproduce published results.
The Large Deficit of HMXB Emission from Luminous Infrared Galaxies: The Case of the Circumnuclear Starburst Ring in NGC 7552
Authors: West Lacey , Garofali Kristen , Lehmer Bret D. , Prestwich Andrea , Eufrasio Rafael , Luangtip Wasutep , Roberts Timothy P. , Zezas Andreas 
Published: July 2023

Abstract
Luminous infrared galaxies (LIRGs), the most extreme star-forming galaxies in the nearby (D < 30 Mpc) universe, show a notable X-ray emission deficiency (up to a factor of ∼10) compared with predictions from scaling relations of galaxy-wide high-mass X-ray binary (HMXB) luminosity with star formation rate. In the nearby (≈20 Mpc) LIRG NGC 7552, the majority of the IR emission originates in a circumnuclear starburst ring, which has been resolved into several discrete knots of star formation. We present results from recent Chandra observations of NGC 7552, which reveal significant deficits in the 2–7 keV X-ray luminosities from two of the most powerful star-forming knots. We hypothesize that the expected luminous HMXB populations in these knots are either (1) obscured by very large column densities or (2) suppressed due to the knots having relatively high metallicity and/or very young ages (≲5 Myr). We distinguish between these possibilities using data from recent NuSTAR observations, whose sensitivity above 10 keV is capable of uncovering heavily obscured HMXB populations, since emission at these energies is more immune to absorption effects. We find no evidence of a heavily obscured HMXB population in the central region of NGC 7552, suggesting suppressed HMXB formation. We further show that metallicity-dependent scaling relations cannot fully account for the observed deficit from the most powerful star-forming knots or the central region as a whole. Thus, we suggest that recent bursts in local star formation activity likely drive the high L
IR within these regions on timescales ≲5 Myr, shorter than the timescale required for the formation of HMXBs.
Effects of Partial Ionization on Magnetic Flux Emergence in the Sun
Authors: Chouliaras Georgios , Syntelis P. , Archontis V. 
Published: July 2023

Abstract
We have performed 3D numerical simulations to investigate the effect of partial ionization on the process of magnetic flux emergence. In our study, we have modified the single-fluid MHD equations to include the presence of neutrals and have performed two basic experiments: one that assumes a fully ionized plasma (FI case) and one that assumes a partially ionized plasma (PI case). We find that the PI case brings less dense plasma to and above the solar surface. Furthermore, we find that partial ionization alters the emerging magnetic field structure, leading to a different shape of the polarities in the emerged bipolar regions compared to the FI case. The amount of emerging flux into the solar atmosphere is larger in the PI case, which has the same initial plasma beta as the FI case, but a larger initial magnetic field strength. The expansion of the field above the photosphere occurs relatively earlier in the PI case, and we confirm that the inclusion of partial ionization reduces cooling due to adiabatic expansion. However, it does not appear to work as a heating mechanism for the atmospheric plasma. The performance of these experiments in three dimensions shows that PI does not prevent the formation of unstable magnetic structures, which erupt into the outer solar atmosphere.
The GLASS-JWST Early Release Science Program. II. Stage I Release of NIRCam Imaging and Catalogs in the Abell 2744 Region
Authors: Paris Diego , Merlin Emiliano , Fontana Adriano , Bonchi Andrea , Brammer Gabriel , Correnti Matteo , Treu Tommaso , Boyett Kristan , Calabrò Antonello , Castellano Marco , Chen Wenlei , Yang Lilan , Glazebrook Karl , Kelly Patrick , Koekemoer Anton M. , Leethochawalit Nicha , Mascia Sara , Mason Charlotte , Morishita Takahiro , Nonino Mario , Pentericci Laura , Polenta Gianluca , Roberts-Borsani Guido , Santini Paola , Trenti Michele , Vanzella Eros , Vulcani Benedetta , Windhorst Rogier A. , Nanayakkara Themiya , Wang Xin 
Published: July 2023

Abstract
We present images and a multiwavelength photometric catalog based on all of the JWST NIRCam observations obtained to date in the region of the Abell 2744 galaxy cluster. These data come from three different programs, namely, the GLASS-JWST Early Release Science Program, UNCOVER, and the Director’s Discretionary Time program 2756. The observed area in the NIRCam wide-band filters—covering the central and extended regions of the cluster, as well as new parallel fields—is 46.5 arcmin2 in total. All images in eight bands (F090W, F115W, F150W, F200W, F277W, F356W, F410M, and F444W) have been reduced adopting the latest calibration and reference files available. Data reduction has been performed using an augmented version of the official JWST pipeline, with improvements aimed at removing or mitigating defects in the raw images and improving the background subtraction and photometric accuracy. We obtain an F444W-detected multiband catalog, including all NIRCam and available Hubble Space Telescope data, adopting forced-aperture photometry on point-spread-function-matched images. The catalog is intended to enable early scientific investigations and is optimized for the study of faint galaxies; it contains 24,389 sources, with a 5σ limiting magnitude in the F444W band ranging from 28.5 AB to 30.5 AB, as a result of the varying exposure times of the surveys that observed the field. We publicly release the reduced NIRCam images, associated multiwavelength catalog, and the code adopted for 1/f noise removal with the aim of aiding users in familiarizing themselves with JWST NIRCam data and identifying suitable targets for follow-up observations.
Investigating the IBEX Ribbon Structure a Solar Cycle Apart
Authors: Dayeh M. A. , Zirnstein E. J. , Swaczyna P. , McComas D. J. 
Published: July 2023

Abstract
A “Ribbon” of enhanced energetic neutral atom (ENA) emissions was discovered by the Interstellar Boundary Explorer in 2009, redefining our understanding of the heliosphere boundaries and the physical processes occurring at the interstellar interface. The Ribbon signal is intertwined with that of a globally distributed flux (GDF) that spans the entire sky. To a certain extent, Ribbon separation methods enabled examining its evolution independent of the underlying GDF. Observations over a full solar cycle revealed the Ribbon’s evolving nature, with intensity variations closely tracking those of the solar wind (SW) structure after a few years delay, accounting for the SW–ENA recycling process. In this work, we examine the Ribbon structure, namely its ENA fluxes, angular extent, width, and circularity properties for two years, 2009 and 2019, representative of the declining phases of two adjacent solar cycles. We find that, (i) the Ribbon ENA fluxes have recovered in the nose direction and south of it down to ∼25° (for energies below 1.7 keV) and not at mid and high ecliptic latitudes; (ii) the Ribbon width exhibits significant variability as a function of azimuthal angle; (iii) circularity analysis suggests that the 2019 Ribbon exhibits a statistically consistent radius with that in 2009. The Ribbon’s partial recovery is aligned with the consensus of a heliosphere with its closest point being southward of the nose region. The large variability of the Ribbon width as a function of azimuth in 2019 compared to 2009 is likely indicative of small-scale processes within the Ribbon.
Magnetic Helicity Associated with the Proton Temperature Anisotropy Instabilities in the Presence of an Imbalanced Solar Wind Turbulence
Authors: Markovskii S. A. , Vasquez Bernard J. 
Published: July 2023

Abstract
Some of the most common processes in the solar wind, such as turbulence and wave generation by instabilities, are associated with spectral magnetic helicity. Therefore, the helicity is a convenient tool to investigate these processes. We use three-dimensional nonlinear kinetic simulations with particle ions and fluid electrons to analyze the magnetic helicity produced by proton temperature anisotropy instabilities coexisting with an ambient turbulence. The symmetry of the unstable system is violated by alpha-particle streaming with respect to protons along the mean magnetic field. At the same time, the turbulent fluctuations are also imbalanced by a nonzero cross-helicity. We show that in the nonlinear phase of the instability the resulting helicity structure is different from the prediction of the linear theory. In particular, it contains sign reversals and multiple domains of nonzero helicity. The turbulence generates its own magnetic helicity signature, which extends over a wide range of angles around the direction perpendicular to the mean magnetic field, and can have a sign the same as or opposite to that of the instability. These findings are consistent with the observed helicity spectra in the solar wind.
V-type Asteroids as the Origin of Mesosiderites
Authors: Libourel Guy , Beck Pierre , Nakamura Akiko M. , Vernazza Pierre , Ganino Clement , Michel Patrick 
Published: July 2023

Abstract
We present the results of a campaign of hypervelocity impact experiments on natural mesosiderite targets, using representative main asteroid belt impact speeds. The objective is to document further the surface evolution of iron-rich asteroids. In contrast with iron meteorites, we demonstrate the fragile behavior of mesosiderite at impact since experiments result in both cratering and catastrophic disruption. The behavior of metal-rich asteroids at impact is thus highly influenced by the original ratio of metal/silicate. A visible to near-infrared spectral analysis shows that the pyroxene silicate signature of impacted mesosiderites, or their ejecta, is fully preserved. Our results thus rule out a mesosiderite hypothesis for the very nature of M/X-type asteroids including (16) Psyche, despite a small fraction of its surface possibly being covered by mesosiderite-like materials. Finally, we address the question of whether mesosiderites and howardite–eucrite–diogenite (HED) meteorites are genetically linked to (4) Vesta or other differentiated asteroids in the main belt based on their spectral similarity.