bluuebunny/crossref_metadata_2025_split huggingface dataset:
ON THE NEED TO ACCOUNT FOR UNCERTAINTY IN THE QUANTITATIVE ASSESSMENT OF FIRE RISK
Authors: Колесников Евгений Юрьевич 
Published: December 2022

Количественная оценка пожарного риска традиционно выполняется в точечной постановке. Между тем в экспериментальной части естественных и технических наук давно принято учитывать наличие неопределенности и количественно ее оценивать. Пришло время учитывать наличие неопределенности и выполнять ее количественную оценку и при математическом моделировании, в частности, при выполнении количественной оценки пожарного риска. В статье приводится проект положения об анализе и количественной оценке неопределенности расчетных показателей пожарного риска.
Quantitative assessment of fire risk is traditionally performed in a point setting. Meanwhile, it has long been common to take into account the presence of uncertainty and quantify it in the experimental part of the natural and technical sciences. It is time to take into account the presence of uncertainty and to quantify it by mathematical modeling, in particular, when performing a quantitative assessment of fire risk. The article provides a draft of provision on the analysis and quantitative assessment of the uncertainty of calculated indicators of fire risk. In conclusion, the article states that the introduction of the interval approach to perform a quantitative risk assessment is a necessary and quite revolutionary step.
Photometric Confirmation and Characterization of the Ennomos Collisional Family in the Jupiter Trojans
Authors: Wong Ian , Brown Michael E. 
Published: December 2022

Abstract
Collisional families offer a unique window into the interior composition of asteroid populations. Previous dynamical studies of the Jupiter Trojans have uncovered a handful of potential collisional families, two of which have been subsequently confirmed through spectral characterization. In this paper, we present new multiband photometric observations of the proposed Ennomos family and derive precise g − i colors of 75 candidate family members. While the majority of the targets have visible colors that are indistinguishable from background objects, we identify 13 objects with closely grouped dynamical properties that have significantly bluer colors. We determine that the true Ennomos collisional family is tightly confined to

a

′

p

>
5.29

au

and

0.45
<
sin

i

p

<
0.47

, and the majority of its confirmed members have near-solar spectral slopes, including some of the bluest objects hitherto discovered in the Trojan population. The property of distinctly neutral colors that is shared by both the Ennomos family and the previously characterized Eurybates family indicates that the spectral properties of freshly exposed surfaces in the Jupiter region are markedly different than the surfaces of uncollided Trojans. This implies that the processes of ice sublimation and space weathering at 5.2 au yield a distinct regolith chemistry from the primordial environment within which the Trojans were initially accreted. It also suggests that the Trojans were emplaced in their present-day location from elsewhere sometime after the initial population formed, which is a key prediction of recent dynamical instability models of solar system evolution.
Importance of Sample Selection in Exoplanet-atmosphere Population Studies
Authors: Batalha Natasha E. , Wolfgang Angie , Teske Johanna , Alam Munazza K. , Alderson Lili , Batalha Natalie M. , López-Morales Mercedes , Wakeford Hannah R. 
Published: December 2022

Abstract
Understanding planet formation requires robust population studies, which are designed to reveal trends in planet properties. In this work we aim to determine if and how different methods for selecting populations of exoplanets for atmospheric characterization with JWST could influence population-level inferences. We generate three hypothetical surveys of super-Earths/sub-Neptunes, with each survey designed to span a similar radius-insolation flux space. The survey samples are constructed based on three different selection criteria (evenly spaced by eye, binned, and a quantitative selection function). Using an injection-recovery technique, we test how robustly individual-planet atmospheric parameters and population-level parameters can be retrieved. We find that all three survey designs result in equally suitable targets for individual atmospheric characterization, but not equally suitable targets for constraining population parameters. Only samples constructed with a quantitative method or that are sufficiently evenly spaced-by-eye result in robust population parameter constraints. Furthermore, we find that the sample with the best targets for individual atmospheric study does not necessarily result in the best-constrained population parameters. The method of sample selection must be considered. We also find that there may be large variability in population-level results with a sample that is small enough to fit in a single JWST cycle (∼12 planets), suggesting that the most successful population-level analyses will be multicycle. Lastly, we infer that our exploration of sample selection is limited by the small number of transiting planets with measured masses around bright stars. Our results can guide future development of programs that aim to determine underlying trends in exoplanet-atmospheric properties, and, by extension, formation and evolution processes.
The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Xu Shuangjing , Imai Hiroshi , Yun Youngjoo , Zhang Bo , Rioja María J. , Dodson Richard , Cho Se-Hyung , Kim Jaeheon , Cui Lang , Sobolev Andrey M. , Chibueze James O. , Kim Dong-Jin , Amada Kei , Nakashima Jun-ichi , Orosz Gabor , Oyadomari Miyako , Oh Sejin , Yonekura Yoshinori , Sun Yan , Mai Xiaofeng , Zhang Jingdong , Wen Shiming , Jung Taehyun 
Published: December 2022

Abstract
We report very long baseline interferometry (VLBI) monitoring observations of the 22 GHz water (H2O) masers around the Mira variable BX Cam, which were carried out as a part of the EAVN Synthesis of Stellar Maser Animations project. Data of 37 epochs in total were obtained from 2018 May to 2021 June with a time interval of 3–4 weeks, spanning approximately three stellar pulsation periods (P = ∼440 days). In particular, the dual-beam system equipped on the VERA stations was used to measure the kinematics and parallaxes of the H2O maser features. The measured parallax, π = 1.79 ± 0.08 mas, is consistent with Gaia EDR3 and previously measured VLBI parallaxes within a 1σ error level. The position of the central star was estimated, based on both the Gaia EDR3 data and the center position of the ring-like 43 GHz silicon-monoxide (SiO) maser distribution imaged with the Korean VLBI Network. The three-dimensional H2O maser kinematics indicates that the circumstellar envelope is expanding at a velocity of 13 ± 4 km s−1, while there are asymmetries in both the spatial and velocity distributions of the maser features. Furthermore, the H2O maser animation achieved by our dense monitoring program manifests the propagation of shock waves in the circumstellar envelope of BX Cam.
The Host Galaxies of Hybrid Morphology Radio Sources
Authors: Stroe Andra , Catlett Victoria , Harwood Jeremy J. , Vernstrom Tessa , Mingo Beatriz 
Published: December 2022

Abstract
Based on their differing radio morphologies, powerful radio galaxies can be separated into the Fanaroff–Riley I (FR I) and II (FR II) classes. Hybrid morphology radio sources (HyMoRS) contain morphologies consistent with each type of jet on either side: a powerful, highly relativistic FR I–like jet terminating in a hotspot on one side and an FR I–like plume on the other. HyMoRS present a unique opportunity to study the conditions that give rise to the dichotomy. Using host galaxy properties, we conduct the first multiwavelength investigation into whether orientation can explain HyMoRS morphology. Through optical spectroscopy and mid-infrared photometry, we analyze the emission characteristics, and evaluate the broad characteristics of five HyMoRS host galaxies at intermediate redshifts (0.4 < z < 1.5). The HyMoRS host galaxies in our sample have properties consistent with typical host galaxies of FR II sources, suggesting that the observed hybrid morphologies may be caused by a dense, cluster-like environment bending FR II jets combined with a favorable orientation that can make one side appear similar to an FR I jet. Our results thus support the hypothesis that HyMoRS are mainly caused by environment and orientation.
Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Singh Ayushi , Martin Peter G. 
Published: December 2022

Abstract
We introduce the HOTT dust optical depth and temperature maps parameterizing thermal dust emission. Such maps have revolutionized studies of the distribution of matter in molecular clouds and processes relevant to star formation, including virial stability. HOTT maps for a suite of fields, including the Herschel Gould Belt Survey, are available online. The standardization of our robust pipeline for modified blackbody fitting of the spectral energy distribution (SED) of high-quality archival submillimeter data from the Herschel Space Observatory is based on a thorough analysis and quantification of the uncertainties of the data. This enables proper weighting in the SED fits. The uncertainties assessed fall into four main categories: instrument noise; the cosmic infrared background anisotropy, a contaminating sky signal; gradient-related noise arising because of dust signal morphology; and calibration uncertainty, scaling with the signal strength. Zero-level adjustments are important too. An analysis of residuals from the SED fits across many fields supports the overall appropriateness of the assumed modified blackbody model and points to where it breaks down. Finding χ
2 distributions close to the theoretical expectation boosts confidence in the pipeline and the optimized quality of the parameter maps and their estimated uncertainties. We compared our HOTT parameter maps to those from earlier studies to understand and quantify the potential for systematic differences.
Turbulent Magnetic Field Amplification by the Interaction of a Shock Wave and Inhomogeneous Medium
Authors: Hu Yue , Xu Siyao , M. Stone James , Lazarian Alex 
Published: December 2022

Abstract
Magnetic fields of the order of 100 μG observed in young supernova remnants cannot be amplified by shock compression alone. To investigate the amplification caused by a turbulent dynamo, we perform three-dimensional MHD simulations of the interaction between a shock wave and an inhomogeneous density distribution with a shallow spectrum in the preshock medium. The postshock turbulence is mainly driven by the strongest preshock density contrast and follows the Kolmogorov scaling. The resulting turbulence amplifies the postshock magnetic field. The time evolution of the magnetic fields agrees with the prediction of the nonlinear turbulent dynamo theory of Xu & Lazarian. When the initially weak magnetic field is perpendicular to the shock normal, the maximum amplification of the field’s strength reaches a factor of ≈200, which is twice as large as that for a parallel shock. We find that the perpendicular shock exhibits a smaller turbulent Alfvén Mach number in the vicinity of the shock front than the parallel shock. However, the strongest magnetic field has a low volume filling factor and is limited by the turbulent energy due to the reconnection diffusion taking place in a turbulent and magnetized fluid. The magnetic field strength averaged along the z-axis is reduced by a factor ≳10. We decompose the turbulent velocity and magnetic field into solenoidal and compressive modes. The solenoidal mode is dominant and evolves to follow the Kolmogorov scaling, even though the preshock density distribution has a shallow spectrum. When the preshock density distribution has a Kolmogorov spectrum, the turbulent velocity’s compressive component increases.
Inpainting Hydrodynamical Maps with Deep Learning
Authors: Mohammad Faizan G. , Villaescusa-Navarro Francisco , Genel Shy , Anglés-Alcázar Daniel , Vogelsberger Mark 
Published: December 2022

Abstract
From 1000 hydrodynamic simulations of the CAMELS project, each with a different value of the cosmological and astrophysical parameters, we generate 15,000 gas temperature maps. We use a state-of-the-art deep convolutional neural network to recover missing data from those maps. We mimic the missing data by applying regular and irregular binary masks that cover either 15% or 30% of the area. We quantify the reliability of our results using two summary statistics: (1) the distance between the probability density functions, estimated using the Kolmogorov–Smirnov (K-S) test, and (2) the 2D power spectrum. We find an excellent agreement between the model prediction and the unmasked maps when using the power spectrum: better than 1% for k < 20 h Mpc−1 for any irregular mask. For regular masks, we observe a systematic offset of ∼5% when covering 15% of the maps, while the results become unreliable when 30% of the data is missing. The observed K-S test p-values favor the null hypothesis that the reconstructed and the ground-truth maps are drawn from the same underlying distribution when irregular masks are used. For regular-shaped masks, on the other hand, we find a strong evidence that the two distributions do not match each other. Finally, we use the model, trained on gas temperature maps, to inpaint maps from fields not used during model training. We find that, visually, our model is able to reconstruct the missing pixels from the maps of those fields with great accuracy, although its performance using summary statistics depends strongly on the considered field.
Vertical Equilibrium Model for Accretion Flow: An Exact General Relativistic Self-consistent Analysis
Authors: Chatterjee Sangita , Mondal Soumen , Basu Prasad 
Published: December 2022

Abstract
We provide a complete general relativistic and fluid dynamical treatment to derive an expression for the relativistic accretion rate in curved spacetime. We exploit the Killing symmetry of stationary axisymmetric spacetime to obtain the conserved current, using which we find an integral relation between mass flux and height of the accretion disk. In comparison with the existing different models of thin- and slim-disk approaches our analysis is self-consistent and mathematically rigorous. We reviewed the previous work and surveyed the recent status in this field. Our formula is different from the existing expression in the literature. The difference arises solely due to the rotation parameter of the compact star. The effect becomes important for slim/thick disks and for rapidly spinning compact stars. Thus one needs to alter the formula

M

̇

=
2
π
rH
ρ

u

r

for Newtonian or spherically symmetric spacetime while studying the accretion flows around a Kerr black hole. Our formula can also be used to connect the variability of the vertical structure of the accretion disk through the luminosity variation of X-ray binaries, and can thereby explain the origin of the hysteresis loop of the spectral states.
A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Stassun Keivan G. , Torres Guillermo , Kounkel Marina , Feliz Dax L. , Bouma Luke G. , Howell Steve B. , Gnilka Crystal L. , Furlan E. 
Published: December 2022

Abstract
We report the discovery of 2M1222−57 as a low-mass, pre-main-sequence (PMS) eclipsing binary (EB) in the Lower Centaurus Crux (LCC) association for which, using Gaia parallaxes and proper motions with a neural net age estimator, we determine an age of 16.2 ± 2.2 Myr. The broadband spectral energy distribution (SED) shows clear excess at ≳10 μm indicative of a circumbinary disk, and new speckle imaging observations reveal a faint, tertiary companion separated by ∼100 au. Hα emission is modulated on the orbital period, consistent with theoretical models of orbitally pulsed accretion streams reaching from the inner disk edge to the central stars. From a joint analysis of spectroscopically determined radial velocities and TESS light curves, together with additional tight constraints provided by the SED and the Gaia parallax, we measure masses for the eclipsing stars of 0.74 M
⊙ and 0.67 M
⊙; radii of 0.98 R
⊙ and 0.94 R
⊙; and effective temperatures of 3750 K and 3645 K. The masses and radii of both stars are measured to an accuracy of ∼1%. The measured radii are inflated, and the temperatures suppressed, relative to predictions of standard PMS evolutionary models at the age of LCC; also, the Li abundances are ∼2 dex less depleted than predicted by those models. However, models that account for the global and internal effects of surface magnetic fields are able to simultaneously reproduce the measured radii, temperatures, and Li abundances at an age of 17.0 ± 0.5 Myr. Altogether, the 2M1222−57 system presents very strong evidence that magnetic activity in young stars alters both their global properties and the physics of their interiors.
Unveiling Hidden Stellar Aggregates in the Milky Way: 1656 New Star Clusters Found in Gaia EDR3
Authors: He 何 Zhihong 治宏 , Liu 刘 Xiaochen 效臣 , Luo 罗 Yangping 杨平 , Wang 王 Kun 坤 , Jiang 蒋 Qingquan 青权 
Published: December 2022

Abstract
We report 1656 new star clusters found in the Galactic disk (∣b∣ < 20°) beyond 1.2 kpc, using Gaia EDR3 data. Based on an unsupervised machine-learning algorithm, DBSCAN, and following our previous studies, we utilized a unique method to do the data preparation and obtain the clustering coefficients, which proved to be an effective way to search blindly for star clusters. We tabulate the physical parameters and member stars of the new clusters, and present some interesting examples, including a globular cluster candidate. The cluster parameters and member stars are available in machine-readable format in the online journal. We examine the new discoveries and discuss their statistical properties. The proper-motion dispersions and radii of the star clusters are the same as those previously reported. The new clusters beyond 1.2 kpc are older than those in the solar neighborhood, and the new objects found in the third Galactic quadrant present the lowest line-of-sight extinctions. Combined with our previous results, the total population of new clusters and candidates detected through our method is 2541, corresponding to 55% of all newly published clusters in the Gaia era. The number of cataloged Gaia star clusters was also increased to nearly 6000. In the near future, it will be necessary to make a unified confirmation and member star determination for all reported clusters.
A Southern Photometric Quasar Catalog from the Dark Energy Survey Data Release 2
Authors: Yang Qian , Shen Yue 
Published: December 2022

Abstract
We present a catalog of 1.4 million photometrically selected quasar candidates in the southern hemisphere over the ∼5000 deg2 Dark Energy Survey (DES) wide survey area. We combine optical photometry from the DES second data release (DR2) with available near-infrared (NIR) and the all-sky unWISE mid-infrared photometry in the selection. We build models of quasars, galaxies, and stars with multivariate skew-t distributions in the multidimensional space of relative fluxes as functions of redshift (or color for stars) and magnitude. Our selection algorithm assigns probabilities for quasars, galaxies, and stars and simultaneously calculates photometric redshifts (photo-z) for quasar and galaxy candidates. Benchmarking on spectroscopically confirmed objects, we successfully classify (with photometry) 94.7% of quasars, 99.3% of galaxies, and 96.3% of stars when all IR bands (NIR YJHK and WISE W1W2) are available. The classification and photo-z regression success rates decrease when fewer bands are available. Our quasar (galaxy) photo-z quality, defined as the fraction of objects with the difference between the photo-z z

p
and the spectroscopic redshift z

s
, ∣Δz∣ ≡ ∣z

s
− z

p
∣/(1 + z

s
) ≤ 0.1, is 92.2% (98.1%) when all IR bands are available, decreasing to 72.2% (90.0%) using optical DES data only. Our photometric quasar catalog achieves an estimated completeness of 89% and purity of 79% at r < 21.5 (0.68 million quasar candidates), with reduced completeness and purity at 21.5 < r ≲ 24. Among the 1.4 million quasar candidates, 87,857 have existing spectra, and 84,978 (96.7%) of them are spectroscopically confirmed quasars. Finally, we provide quasar, galaxy, and star probabilities for all (0.69 billion) photometric sources in the DES DR2 coadded photometric catalog.
Drechslerella daliensis and D. xiaguanensis (Orbiliales, Orbiliaceae), two new nematode-trapping fungi from Yunnan, China
Authors: Zhang Fa , Boonmee Saranyaphat , Monkai Jutamart , Yang Xiao-Yan , Xiao Wen 
Published: December 2022

Nematode-trapping fungi are a highly specialised group in fungi and are essential regulators of natural nematode populations. At present, more than 130 species have been discovered in Zygomycota (Zoopagaceae), Basidiomycota (Nematoctonus), and Ascomycota (Orbiliaceae). Amongst them, nematode-trapping fungi in Orbiliaceae have become the research focus of carnivorous fungi due to their abundant species. During the investigation of carnivorous fungi in Yunnan, China, four fungal strains isolated from burned forest soil were identified as two new nematode-trapping species in Drechslerella (Orbiliaceae), based on multigene phylogenetic analysis and morphological characters.
Drechslerella daliensis sp. nov. is characterised by its ellipsoid, 1–2-septate macroconidia, clavate or bottle-shaped, 0–1-septate microconidia and unbranched, simple conidiophores. D. xiaguanensis sp. nov. is characterised by fusiform or spindle-shaped, 2–4-septate conidia and unbranched, simple conidiophores. Both of them produce constricting rings to capture nematodes. The phylogenetic analysis, based on combined ITS, TEF1-α and RPB2 sequences, determined their placement in Drechslerella. D. daliensis forms a basal lineage closely nested with D. hainanensis (YMF1.03993). D. xiaguanensis forms a sister lineage with D. bembicodes (1.01429), D. aphrobrocha (YMF1.00119) and D. coelobrocha (FWY03-25-1).
Critique pour qui ? Politisation par l’enquête et objectivation de sa réception
Authors: Simonet Maud 
Published: December 2022

En comparant sur plusieurs scènes la réception de mes recherches sur le travail bénévole – désenchantement pour les un.es, truisme pour les autres – et en prenant au sérieux le processus de politisation par l’enquête qui a été le mien, cet article propose une analyse située à la fois socialement et politiquement du désenchantement que produirait la sociologie catégorisée comme critique. Il met en lumière deux défenses de l’autonomie de l’engagement, au cœur de la critique de la critique : celui de l’autonomie de « l’engagement citoyen » des acteur.trices et de leur rapport au travail, et celui de l’autonomie du travail du chercheur.se et de ses « engagements », généralement présenté sous le topos de la « neutralité » de la recherche. Ce retour réflexif sur les effets de l’enquête sur les autres, mais aussi sur moi-même, vient questionner in fine la portée sociale et politique de cette « conception des mondes antagonistes » inscrite dans une « doctrine de la séparation des sphères » du travail et de l’engagement qui concerne ici tant l’objet que la pratique de recherche.