bluuebunny/crossref_metadata_2025_split huggingface dataset:
Кey signs of ecosystem assets valuation
Authors: Kolmakova Valentyna M. 
Published: February 2023

The purpose of the article is to develop scientific approaches and identify key features of the assessment of ecosystem assets of territorial communities.
The article examines modern scientific approaches to the assessment of ecosystem assets of territorial communities in the context of deepening processes of decentralization of management. The essence of the definition of ecosystem assets from the standpoint of ecosystem accounting is revealed, in particular, it is focused on one of their main characteristics: the ability of natural reserves (stocks) to provide a constant flow (flow) of ecosystem services. The necessity of taking into account the market value of ecosystem assets in the process of monitoring their use and involvement in economic circulation at the local level has been determined. In this sense, the role of ecosystem services in providing links between ecosystem assets and benefits is considered. The main characteristics of ecosystem assets are investigated, their common and distinctive features from natural resource and production assets of spatial territorial entities are revealed. A systematization of generalized approaches to the methodology for assessing ecosystem assets according to the recommendations of the TEEB (The Economics of Ecosystems and Biodiversity), which is advisable to apply for territorial communities as key strategic guidelines for sustainable spatial development, is proposed. It is recommended to include the indicator “ecosystem assets” (EA) as a mandatory component of annual national accounts.
Further research has prospects in the following areas:

formation of an integrated strategic approach to the implementation of ecosystem asset valuation at the local level;
development and implementation of effective methodological approaches to the assessment of ecosystem assets for the formation of investment attractiveness of the territory through the use of local natural resources as ecosystem assets for sustainable spatial development.
La deserción escolar en el bachillerato del colegio Gabriela Mistral
Authors: Caizapanta Puruncaja Geovanny , Guamán Garcés Calixto , Ocampo Contreras Paola 
Published: February 2023

El presente artículo tiene como objetivo explicar los factores psicosociales que influyen en la deserción escolar en los estudiantes del 1er año de bachillerato general unificado del Colegio Nacional Nocturno Gabriela Mistral, institución educativa ubicada en Ecuador, también busca plantear una nueva visión sobre como este grave problema afecta al desarrollo del país. Los factores económicos, familiares, académicos y psicológicos que se mencionan en el texto son los que se han determinado como las principales causas de la deserción parcial o total de los estudiantes en el nivel indicado; para obtener los resultados se ha realizado una investigación profunda y se ha aplicado un instrumento confiable para la determinación de los mismos.
Se ha escogido una muestra de estudiantes que pertenecen a un colegio nocturno dado que en la educación matutina y vespertina los casos de deserción escolar no son tan comunes. Los estudiantes de bachillerato encuestados han vivido de cerca la situación de deserción, problemas familiares, embarazo no deseado, etc.
Este artículo permitirá marcar un antes y un después acerca del problema de la deserción escolar en el país, pues la investigación se ubica en el año lectivo 2019-2020, mientras que en estos momentos la sociedad y el mundo verá una nueva realidad en el año escolar 2020-2021 debido a la pandemia.
South Africa Education Data and Visualisations
Authors: Combrink Herkulaas 
Published: February 2023

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<p>The tabular and visual dataset focuses on South African basic education and provides insights into the distribution of schools and basic population statistics across the country. This tabular and visual data are stratified across different quintiles for each provincial and district boundary. The quintile system is used by the South African government to classify schools based on their level of socio-economic disadvantage, with quintile 1 being the most disadvantaged and quintile 5 being the least disadvantaged. The data was joined by extracting information from the debarment of basic education with StatsSA population census data. Thereafter, all tabular data and geo located data were transformed to maps using GIS software and the Python integrated development environment. The dataset includes information on the number of schools and students in each quintile, as well as the population density in each area. The data is displayed through a combination of charts, maps and tables, allowing for easy analysis and interpretation of the information.</p>
ELM of ELM-WD: An Extremely-low-mass Hot Star Discovered in LAMOST Survey
Authors: Yuan (袁海龙) Hailong , Li (李振威) Zhenwei , Bai (白仲瑞) Zhongrui , Dong (董义乔) Yiqiao , Wang (汪梦欣) Mengxin , Yu (余思成) Sicheng , Chen (陈雪飞) Xuefei , Zhao (赵永恒) Yongheng , Chu (褚耀泉) Yaoquan , Zhang (张昊彤) Haotong 
Published: February 2023

Abstract
The extremely-low-mass white dwarfs (ELM WDs) and pre-ELM WDs are helium-core white dwarfs with mass <∼ 0.3M
⊙. Evolution simulations show that a lower mass limit for ELM WDs exists at ≈0.14M
⊙ and no ELM WD is proposed by observation to be less massive than that. Here we report the discovery of a binary system, LAMOST J224040.77-020732.8 (J2240 in short), which consists of a very low-mass hot star and a compact companion. Multiepoch spectroscopy shows an orbital period P
orb = 0.219658 ± 0.000002 days and a radial-velocity semiamplitude K1 = 318.5 ± 3.3 km s−1, which gives the mass function of 0.74M
⊙, indicating the companion is a compact star. The F-type low-resolution spectra illustrate no emission features, and the temperature (∼7400 K) is consistent with that from spectral energy distribution fitting and multicolor light-curve solution. The optical light curves, in ZTF g, r, and i bands and the Catalina V band, show ellipsoidal variability with amplitudes of ∼30%, suggesting that the visible component is heavily tidally distorted. Combining the distance from Gaia survey, the ZTF light curves are modeled with Wilson–Devinney code and the result shows that the mass of the visible component is

M
1
=

0.085

−
0.024

+
0.036

M

⊙

, and the mass of the invisible component is

M
2
=

0.98

−
0.09

+
0.16

M

⊙

. The radius of the visible component is

R
1
=

0.29

−
0.03

+
0.04

R

⊙

. The inclination angle is approximately between 60° and 90°. The observations indicate the system is most likely a pre-ELM WD + WD/NS binary, and the mass of pre-ELM is possibly lower than the 0.14M
⊙ theoretical limit.
A Reinforcement Learning–Based Follow-up Framework
Authors: Astudillo Javiera , Protopapas Pavlos , Pichara Karim , Becker Ignacio 
Published: February 2023

Abstract
Classification and characterization of variable and transient phenomena are critical for astrophysics and cosmology. Given the volume of nightly data produced by ongoing and future surveys such as LSST, it is critical to develop automatic tools that assist in observation decision-making, maximizing scientific output without resource wastage. We propose a reinforcement learning–based recommendation system for real-time astronomical observation of sources. We assess whether it is worth making further observations and recommend the best instrument from a preexisting candidate set of instruments. Current possible choices include single-band, multiband, and spectroscopic observations, although it is generalizable to any other kind of instrumentation. We rely on a reward metric to make recommendations, which incorporates the gain in a classification sense and the cost incurred for the queried observations. This metric is flexible and easily adaptable to different application scenarios. We run 24 simulations in an offline setting with preexisting observations from Gaia DR2 and SDSS DR14. We propose four comparison strategies, including the baseline strategy, which recommends based on the most similar past cases to the current case. Our strategy surpasses all other strategies in regard to reward. We reach an accuracy of 0.932, comparable to using the accuracy reached using all possible resources (0.948) but with half the number of photometric observations and 1000 times fewer spectroscopic resources. The baseline strategy lacks the complexity to achieve competitive results with our proposed strategy. Our framework is meant to aid continuous online observation decision-making and can be extended to incorporate multiple environmental and observation conditions.
Patchy Forsterite Clouds in the Atmospheres of Two Highly Variable Exoplanet Analogs
Authors: Vos Johanna M. , Burningham Ben , Faherty Jacqueline K. , Alejandro Sherelyn , Gonzales Eileen , Calamari Emily , Gagliuffi Daniella Bardalez , Visscher Channon , Tan Xianyu , Morley Caroline V. , Marley Mark , Gemma Marina E. , Whiteford Niall , Gaarn Josefine , Park Grace 
Published: February 2023

AbstractWe present an atmospheric retrieval analysis of a pair of highly variable, ∼200 Myr old, early T type planetary-mass exoplanet analogs SIMP J01365662+0933473 and 2MASS J21392676+0220226 using the Brewster retrieval framework. Our analysis, which makes use of archival 1–15μm spectra, finds almost identical atmospheres for both objects. For both targets, we find that the data is best described by a patchy, high-altitude forsterite (Mg2SiO4) cloud above a deeper, optically thick iron (Fe) cloud. Our model constrains the cloud properties well, including the cloud locations and cloud particle sizes. We find that the patchy forsterite slab cloud inferred from our retrieval may be responsible for the spectral behavior of the observed variability. Our retrieved cloud structure is consistent with the atmospheric structure previously inferred from spectroscopic variability measurements, but clarifies this picture significantly. We find consistent C/O ratios for both objects, which supports their formation within the same molecular cloud in the Carina-Near moving group. Finally, we note some differences in the constrained abundances of H2O and CO, which may be caused by data quality and/or astrophysical processes such as auroral activity and their differing rotation rates. The results presented in this work provide a promising preview of the detail with which we will characterize extrasolar atmospheres with JWST, which will yield higher-quality spectra across a wider wavelength range.
Tidal Disruption of Stellar Clusters and the Spatial Distribution of Their Remnants Near the Galactic Center
Authors: Wang 王 Long 龙 , Lin 林 D. N. C. 潮 
Published: February 2023

Abstract
The accretion of massive star clusters via dynamical friction has previously been established to be a likely scenario for the buildup of nuclear stellar clusters (NSCs). A remaining issue is whether strong external tidal perturbation may lead to the severe disruption of loosely bound clusters well before they sink deeply into the center of their host galaxies. We carry out a series of N-body simulations and verify our early idealized analytic models. We show that if the density profile of the host galaxies can be described by a power-law distribution with an index of α < 1, the cluster would be compressed in the radial direction by the external galactic tidal field. In contrast, the galactic tidal perturbation is disruptive in regions with a steep, α > 1, density falloff or in the very center where gravity is dominated by the point-mass potential of supermassive black holes (SMBHs). This sufficient criterion supplements the conventional necessary Roche-lobe-filling condition in determining the preservation versus disintegration of satellite stellar systems. We simulate the disruption of stellar clusters that venture onto nearly circular, modestly, or highly eccentric orbits into the center of galaxies with a range of background density profiles and SMBHs. We obtain the spatial distribution of the stellar cluster remnants. We apply these results to the NSC within a few parsecs from SMBH Sgr A* at the Galactic Center. Recent observations indicate the coexistence of two populations of stars with distinctively separate ages and metallicities. We verify that the subsolar-metallicity population can be the debris of disrupted stellar clusters.
The Art of Measuring Physical Parameters in Galaxies: A Critical Assessment of Spectral Energy Distribution Fitting Techniques
Authors: Pacifici Camilla , Iyer Kartheik G. , Mobasher Bahram , da Cunha Elisabete , Acquaviva Viviana , Burgarella Denis , Calistro Rivera Gabriela , Carnall Adam C. , Chang Yu-Yen , Chartab Nima , Cooke Kevin C. , Fairhurst Ciaran , Kartaltepe Jeyhan , Leja Joel , Małek Katarzyna , Salmon Brett , Torelli Marianna , Vidal-García Alba , Boquien Médéric , Brammer Gabriel G. , Brown Michael J. I. , Capak Peter L. , Chevallard Jacopo , Circosta Chiara , Croton Darren , Davidzon Iary , Dickinson Mark , Duncan Kenneth J. , Faber Sandra M. , Ferguson Harry C. , Fontana Adriano , Guo Yicheng , Haeussler Boris , Hemmati Shoubaneh , Jafariyazani Marziye , Kassin Susan A. , Larson Rebecca L. , Lee Bomee , Mantha Kameswara Bharadwaj , Marchi Francesca , Nayyeri Hooshang , Newman Jeffrey A. , Pandya Viraj , Pforr Janine , Reddy Naveen , Sanders Ryan , Shah Ekta , Shahidi Abtin , Stevans Matthew L. , Triani Dian Puspita , Tyler Krystal D. , Vanderhoof Brittany N. , de la Vega Alexander , Wang Weichen , Weston Madalyn E. 
Published: February 2023

Abstract
The study of galaxy evolution hinges on our ability to interpret multiwavelength galaxy observations in terms of their physical properties. To do this, we rely on spectral energy distribution (SED) models, which allow us to infer physical parameters from spectrophotometric data. In recent years, thanks to wide and deep multiwave band galaxy surveys, the volume of high-quality data have significantly increased. Alongside the increased data, algorithms performing SED fitting have improved, including better modeling prescriptions, newer templates, and more extensive sampling in wavelength space. We present a comprehensive analysis of different SED-fitting codes including their methods and output with the aim of measuring the uncertainties caused by the modeling assumptions. We apply 14 of the most commonly used SED-fitting codes on samples from the CANDELS photometric catalogs at z ∼ 1 and z ∼ 3. We find agreement on the stellar mass, while we observe some discrepancies in the star formation rate (SFR) and dust-attenuation results. To explore the differences and biases among the codes, we explore the impact of the various modeling assumptions as they are set in the codes (e.g., star formation histories, nebular, dust and active galactic nucleus models) on the derived stellar masses, SFRs, and A

V
values. We then assess the difference among the codes on the SFR–stellar mass relation and we measure the contribution to the uncertainties by the modeling choices (i.e., the modeling uncertainties) in stellar mass (∼0.1 dex), SFR (∼0.3 dex), and dust attenuation (∼0.3 mag). Finally, we present some resources summarizing best practices in SED fitting.
Similar Signatures of Coplanar Gas Inflow and Disk Warps in Galactic Gas Kinematic Maps
Authors: Wang Enci , Lilly Simon J. 
Published: February 2023

Abstract
Hydrodynamic simulations suggest that galactic gas disks form when coplanar gas spirals into the inner regions of the disk. We recently presented a simple modified accretion disk model of viscous galactic disks in which star formation is fed by a radial flow of gas. However, little observational evidence has been presented for such inflows, which are expected to be only a few kilometers per second in the central regions of the disk, i.e., within four disk scale lengths, but could reach of order 50–100 km s−1 in the very outer disk. The effects of systematic inflow on the 2D velocity field are examined and it is shown that these are quite similar to those produced by geometric warps of the disks, with twist distortions of both the kinematic major and minor axes. This makes it potentially difficult to distinguish between these in practice. By comparing the handedness of the observed twisting of the kinematic axes and of the spiral arms for a sample of nearby galaxies, we find (assuming that the spiral arms are generally trailing) that the effects of warps are in fact likely to dominate over the effects of radial inflows. However, the common practice of treating these twist distortions of the kinematic major and minor axes as being due only to warps can lead, for galaxies of low-to-intermediate inclinations, to substantial underestimates of any systematic inflow.
Weighing the Darkness. III. How Gaia Could, but Probably Will Not, Astrometrically Detect Free-floating Black Holes
Authors: Andrews Jeff J. 
Published: February 2023

Abstract
The gravitational pull of an unseen companion to a luminous star is well known to cause deviations to the parallax and proper motion of a star. In a previous paper in this series, we argue that the astrometric mission Gaia can identify long-period binaries by precisely measuring these arcs. An arc in a star’s path can also be caused by a flyby: a hyperbolic encounter with another massive object. We quantify the apparent acceleration over time induced by a companion star as a function of the impact parameter, velocity of interaction, and companion mass. In principle, Gaia could be used to astrometrically identify the contribution of massive compact halo objects to the local dark matter potential of the Milky Way. However, after quantifying their rate and Gaia’s sensitivity, we find that flybys are so rare that Gaia will probably never observe one. Therefore, every star in the Gaia database exhibiting astrometric acceleration is likely in a long-period binary with another object. Nevertheless, we show how intermediate-mass black holes, if they exist in the local stellar neighborhood, can induce anomalously large accelerations on stars.
Quantifying the Agyrotropy of Proton and Electron Heating in Turbulent Plasmas
Authors: Yang Yan , Pecora Francesco , Matthaeus William H. , Roy Sohom , Cuesta Manuel Enrique , Chasapis Alexandros , Parashar Tulasi , Bandyopadhyay Riddhi , Gershman D. J. , Giles B. L. , Burch J. L. 
Published: February 2023

Abstract
An important aspect of energy dissipation in weakly collisional plasmas is that of energy partitioning between different species (e.g., protons and electrons) and between different energy channels. Here we analyse pressure–strain interaction to quantify the fractions of isotropic compressive, gyrotropic, and nongyrotropic heating for each species. An analysis of kinetic turbulence simulations is compared and contrasted with corresponding observational results from Magnetospheric Multiscale Mission data in the magnetosheath. In assessing how protons and electrons respond to different ingredients of the pressure–strain interaction, we find that compressive heating is stronger than incompressive heating in the magnetosheath for both electrons and protons, while incompressive heating is stronger in kinetic plasma turbulence simulations. Concerning incompressive heating, the gyrotropic contribution for electrons is dominant over the nongyrotropic contribution, while for protons nongyrotropic heating is enhanced in both simulations and observations. Variations with plasma β are also discussed, and protons tend to gain more heating with increasing β.
Exploring Magnetic Loops and Serpentine Fields in the Quiet Sun with the GRIS-IFU
Authors: Campbell Ryan J. , Gafeira Ricardo , Mathioudakis Mihalis , Noda C. Quintero , Collados Manuel 
Published: February 2023

Abstract
Synthetic observations produced from radiative magnetohydrodynamic simulations have predicted that higher polarization fractions in the quiet solar photosphere would be revealed by increasing the total integration time of observations at GREGOR resolutions. We present recently acquired disk center observations of the Fe i 15648.5 Å line obtained with the GREGOR telescope equipped with the GRIS-IFU during excellent seeing conditions, showing exceptionally high polarization fractions. Our observations reveal an internetwork region with a majority (>60%) of magnetized pixels displaying a clear transverse component of the magnetic field. This result is in stark contrast to previous disk center GRIS-IFU observations in this spectral line, which had predominantly vertical magnetic fields in the deep photosphere. At the same time, the median magnetic field strength is weaker than previous GRIS-IFU observations, indicating that the larger fraction of polarization signals cannot be explained by a more active target. We use the Stokes Inversion based on Response functions (SIR) code to analyze the data, performing over 45 million inversions, and interrogate the impact of two conflicting approaches to the treatment of noise on the retrieval of the magnetic inclination and azimuth. We present several case studies of the zoo of magnetic features present in these data, including small-scale magnetic loops that seem to be embedded in a sea of magnetism, and serpentine fields, focusing on regions where full-vector spectropolarimetry has been achieved. We also present a new open-source Python 3 analysis tool, SIR Explorer, which we use to examine the dynamics of these small-scale magnetic features.
Data-driven Cosmology from Three-dimensional Light Cones
Authors: Cheng Yun-Ting , Wandelt Benjamin D. , Chang Tzu-Ching , Doré Olivier 
Published: February 2023

Abstract
We present a data-driven technique to analyze multifrequency images from upcoming cosmological surveys mapping large sky area. Using full information from the data at the two-point level, our method can simultaneously constrain the large-scale structure (LSS), the spectra and redshift distribution of emitting sources, and the noise in the observed data without any prior assumptions beyond the homogeneity and isotropy of cosmological perturbations. In particular, the method does not rely on source detection or photometric or spectroscopic redshift estimates. Here, we present the formalism and demonstrate our technique with a mock observation from nine optical and near-infrared photometric bands. Our method can recover the input signal and noise without bias, and quantify the uncertainty on the constraints. Our technique provides a flexible framework to analyze the LSS observation traced by different types of sources, which has potential for wide application to current or future cosmological data sets such as SPHEREx, Rubin Observatory, Euclid, or the Nancy Grace Roman Space Telescope.