bluuebunny/crossref_metadata_2025_split huggingface dataset:
Дендрофлора та ландшафтна організація арборетуму ім. В. В. Пашкевича Національного дендрологічного парку "Софіївка"
Authors: Копилова Т. В. , Рум'янков Ю. О. , Порохнява О. Л. , Музика Г. І. , Заячук В. Я. , Вегера Л. В. 
Published: April 2024

Розглянуто історію створення, збереження та реставрації історичної ділянки арборетум ім. В. В. Пашкевича Національного дендрологічного парку "Софіївка" Національної академії наук України. З'ясовано сучасний стан дендрологічної структури арборетуму та визначено, що з початкового складу посадок 1889-1991 рр. залишилось 44 види та форми. Відзначено, що на ділянках арборетуму росте багато екзотичних деревних і кущових рослин дендрологічного парку "Софіївка", які становлять теоретичний і практичний інтерес для науковців, садівників-аматорів, студентів, школярів, туристів. Встановлено, що дендрофлору арборетуму, на 2023 р., формують 458 екземпляри деревних і чагарникових рослин, які належать до 90 видів і форм з 24 родин, з них 24 аборигенних видів рослин та 66 видів інтродукованих. За кількісними показниками найбільше представників родини Rosaceae Juss. (24,3 %), Hydrangeaceae Dumort. (14,4 %), Malvaceae Juss. (9,5 %), Sapindaceae Dumrt. (9,1 %), Oleaceae Hof., & Link. (7,5 %), Caprifoliaceae Juss. (6,9 %), а найменше – Rutacea Juss. (0,2 %), Viburnaceae Raf. (0,2 %), Staphyleaceae (DC.) Lindl. (0,2 %), Cornaceae Bercht. & J. Presl. (0,2 %). За чисельністю видів (30,3 %) та екземплярів (27,9 %) переважають рослини з Північної Америки. Установлено, що найбільша частка таксонів належить до вікової групи 121-135 років – 25 %; 1-20 рр. – 22,3 %; 101-120 рр. – 19,23 %; 21-40 рр. – 12,69 %; 81-100 рр. – 10,77 %; 41-60 рр. – 4,62 %; 61-80 рр. – 4,2 %; і найменша 208 років – 1,15 %. Наразі ландшафтна структура арборетуму містить: 22 промарковані ділянки; діючий водорозподільний колодязь; басейн з колекцією водяних рослин родини Acoraceae Martinov., Pteridaceae E. DMKirchn, Cyperaceae Juss., Pontederiaceae Kunth., Hydrocharitaceae Juss., Nymphaeaceae Salisb., Araceae Juss., Salviniaceae Martinov, Alismataceae Vent., Lythraceae J. St-Hil.; кам'яна гірка, на якій висаджено рослини родини Crassuiaceae J. St-Hil., Ranunculaceae Juss., Cactaceae Juss., Apocynaceae Juss., є невеликий грот, де задекоровано розведення труб водопостачання; прогулянкова зона представленаширокими тінистими алеями, вузькими стежками та лавами для відпочинку.
Literature Review: Inquiry Social Complexity-STEAM Model Based on Math Trail-Virtual Reality Activity Nuanced with Javanese Culture in Improving Critical Thinking Ability
Authors: Suryonegoro Bayu Murti , Wuryastuti Monica Luishanda , Dewi Nuriana Rachmani 
Published: April 2024

Purpose of the study: Analyse various literature studies on the Inquiry Social Complexity-STEAM model based on Math Trail-Virtual Reality activities with Javanese cultural nuances in improving students' critical thinking skills. Methodology: This research method uses a literature review. Researchers look for data from books, journals, or relevant research articles and include them in the findings and discussion section to reach a conclusion. This research uses descriptive qualitative data analysis techniques to study literature by describing the results of sources obtained either through books, journals, or related research articles. Main Findings: The syntax of inquiry social complexity STEAM learning model based on math trail virtual reality activities with Javanese cultural nuances can be concluded that each syntax encourages students to find, investigate, construct, and integrate the knowledge gained to form better critical thinking skills by accommodating all aspects of students' abilities with different levels to participate in every aspect and step of learning. Novelty/Originality of this study: The addition of the STEAM approach, especially in the Inquiry Social Complexity Learning model, and math trail-based activities using virtual reality technology that has never been done before or integrated into a maths classroom.
Small and Large Dust Cavities in Disks around Mid-M Stars in Taurus
Authors: Shi 施 Yangfan 杨帆 , Long 龙 Feng 凤 , Herczeg 沈 Gregory J. 雷歌 , Harsono Daniel , Liu Yao , Pinilla Paola , Ragusa Enrico , Johnstone Doug , Bai Xue-Ning , Pascucci Ilaria , Manara Carlo F. , Mulders Gijs D. , Cieza Lucas A. 
Published: April 2024

Abstract
High angular resolution imaging by Atacama Large Millimeter/submillimeter Array (ALMA) has revealed the near universality and diversity of substructures in protoplanetary disks. However, disks around M-type pre-main-sequence stars are still poorly sampled, despite the prevalence of M dwarfs in the Galaxy. Here we present high-resolution (∼50 mas, 8 au) ALMA Band 6 observations of six disks around mid-M stars in Taurus. We detect dust continuum emission in all six disks, 12CO in five disks, and 13CO line in two disks. The size ratios between gas and dust disks range from 1.6 to 5.1. The ratio of about 5 for 2M0436 and 2M0450 indicates efficient dust radial drift. Four disks show rings and cavities, and two disks are smooth. The cavity sizes occupy a wide range: 60 au for 2M0412, and ∼10 au for 2M0434, 2M0436, and 2M0508. Detailed visibility modeling indicates that small cavities of 1.7 and 5.7 au may hide in the two smooth disks 2M0450 and CIDA 12. We perform radiative transfer fitting of the infrared spectral energy distributions to constrain the cavity sizes, finding that micron-sized dust grains may have smaller cavities than millimeter grains. Planet–disk interactions are the preferred explanation to produce the large 60 au cavity, while other physics could be responsible for the three ∼10 au cavities under current observations and theories. Currently, disks around mid- to late M stars in Taurus show a higher detection frequency of cavities than earlier-type stars, although a more complete sample is needed to evaluate any dependence of substructure on stellar mass.
Impact of Electron Precipitation on Brown Dwarf Atmospheres and the Missing Auroral
H3+
Emission
Authors: Pineda J. Sebastian , Hallinan Gregg , Desert Jean-Michel , Harding Leon K. 
Published: April 2024

Abstract
Recent observations have demonstrated that very low-mass stars and brown dwarfs are capable of sustaining strong magnetic fields despite their cool and neutral atmospheres. These kilogauss field strengths are inferred based on strong, highly circularly polarized gigahertz radio emission, a consequence of the electron cyclotron maser instability. Crucially, these observations imply the existence of energetic nonthermal electron populations, associated with strong current systems, as are found in the auroral regions of the magnetized planets of the solar system. Intense auroral electron precipitation will lead to electron collisions with the H2 gas that should generate the ion

H

3

+

. With this motivation, we targeted a sample of ultracool dwarfs, known to exhibit signatures associated with aurorae, in search of the K-band emission features of

H

3

+

using the Keck telescopes on Maunakea. From our sample of nine objects, we found no clear indication of

H

3

+

emission features in our low-to-medium-resolution spectra (R ∼ 3600). We also modeled the impact of an auroral electron beam on a brown dwarf atmosphere, determining the depth at which energetic beams deposit their energy and drive particle impact ionization. We find that the

H

3

+

nondetections can be explained by electron beams of typical energies ≳2–10 keV, which penetrate deeply enough that any

H

3

+

produced is chemically destroyed before radiating energy through its infrared transitions. Strong electron beams could further explain the lack of UV auroral detections and suggest that most or nearly all of the precipitating auroral energy must ultimately emerge as thermal emissions deep in brown dwarf atmospheres.
Test for Echo: X-Ray Reflection Variability in the Seyfert-2 Active Galactic Nucleus NGC 4388
Authors: Gediman Ben , Miller Jon M. , Zoghbi Abderahmen , Draghis Paul , Arzoumanian Zaven , Brandt W. N. , Gendreau Keith 
Published: April 2024

Abstract
We report on a study of the narrow Fe Kα line and reflection spectrum in the well-known Seyfert-2 active galactic nucleus (AGN), NGC 4388. X-ray spectra summed from two extensive NICER monitoring campaigns, separated by years, show strong evidence of variation in the direct continuum and reflected emission, but only small variations in the obscuring gas. Fits to the spectra from individual NICER observations find a strong, positive correlation between the power-law photon index, Γ, and direct flux that is commonly observed in unobscured AGN. A search for a reverberation lag between the direct and reflected spectra—dominated by the narrow Fe Kα emission line—measures a timescale of

t
=

16.37

−
0.38

+
0.46

days, or a characteristic radius of

r
=

1.374

−
0.032

+
0.039

×

10

−
2

pc

=

3.4

−
0.1

+
0.1

×

10

4

GM

/

c

2

. Only one cycle of this tentative lag is observed, but it is driven by a particularly sharp drop in the direct continuum that leads to the subsequent disappearance of the otherwise prominent Fe Kα line. Physically motivated fits to high-resolution Chandra spectra of NGC 4388 measure a line production radius of

r
=

2.9

−
0.7

+
1.2

×

10

4

GM

/

c

2

, formally consistent with the tentative lag. The line profile also prefers a Compton-thick reflector, indicating an origin in the disk and/or thick clumps within a wind. We discuss the strengths and weaknesses of our analysis and methods for testing our results in future observations, and we note the potential for X-ray reverberation lags to constrain black hole masses in obscured Seyferts wherein the optical broad line region is not visible.
Comprehensive High-resolution Chemical Spectroscopy of Barnard’s Star with SPIRou
Authors: Jahandar Farbod , Doyon René , Artigau Étienne , Cook Neil J. , Cadieux Charles , Lafrenière David , Forveille Thierry , Donati Jean-François , Fouqué Pascal , Carmona Andrés , Cloutier Ryan , Cristofari Paul , Gaidos Eric , Gomes da Silva João , Malo Lison , Martioli Eder , do Nascimento J.-D. , Pelletier Stefan , Vandal Thomas , Venn Kim 
Published: April 2024

Abstract
Determination of fundamental parameters of stars impacts all fields of astrophysics, from galaxy evolution to constraining the internal structure of exoplanets. This paper presents a detailed spectroscopic analysis of Barnard’s star (otherwise known as Gl 699) that compares an exceptionally high-quality (an average signal-to-noise ratio of ∼1000 in the entire domain), high-resolution near-infrared (NIR) spectrum taken with Canada-France-Hawaii Telescope/SPIRou to PHOENIX-ACES stellar atmosphere models. The observed spectrum shows thousands of lines not identified in the models with a similarly large number of lines present in the model but not in the observed data. We also identify several other caveats, such as continuum mismatch, unresolved contamination, and spectral lines significantly shifted from their expected wavelengths; all of these can be a source of bias for the determination of abundance. Out of >104 observed lines in the NIR that could be used for chemical spectroscopy, we identify a short list of a few hundred lines that are reliable. We present a novel method for determining the effective temperature (T
eff) and overall metallicity of slowly rotating M dwarfs that uses several groups of lines as opposed to bulk spectral fitting methods. With this method, we infer T
eff = 3231 ± 21 K for Barnard's star, consistent with the value of 3238 ± 11 K inferred from the interferometric method. We also provide measurements of the abundance of 15 different elements for Barnard's star, including the abundances of four elements (K, O, Y, Th) never reported before for this star. This work emphasizes the need to improve current atmosphere models to fully exploit the NIR domain for chemical spectroscopy analysis.
The Size–Linewidth Relation and Signatures of Feedback from Quiescent to Active Star Forming Regions in the LMC
Authors: Green Alex , Wong Tony , Indebetouw Rémy , Nayak Omnarayani , Bolatto Alberto , Tarantino Elizabeth , Rubio Mónica , Madden Suzanne C. , Hirschauer Alec S. 
Published: April 2024

Abstract
To investigate the effects of stellar feedback on the gravitational state of giant molecular clouds (GMCs), we study 12CO and 13CO Atacama Large Millimeter/submillimeter Array maps of nine GMCs distributed throughout the Large Magellanic Cloud (LMC), the nearest star-forming galaxy to our own. We perform noise and resolution matching on the sample, working at a common resolution of 3.″5 (0.85 pc at the LMC distance of 50 kpc), and we use the Spectral Clustering for Molecular Emission Segmentation clustering algorithm to identify discrete substructure, or “clumps.” We supplement these data with three tracers of recent star formation: 8 μm surface brightness, continuum-subtracted Hα flux, and interstellar radiation field energy density inferred from dust emission. The 12CO clumps identified cover a range of 3.6 dex in luminosity-based mass and 2.4 dex in average 8 μm surface brightness, representative of the wide range of conditions of the interstellar medium in the LMC. Our observations suggest evidence for increased turbulence in these clouds. While the turbulent linewidths are correlated with clump surface density, in agreement with previous observations, we find even better correlation with the three star formation activity tracers considered, suggesting stellar energy injection plays a significant role in the dynamical state of the clumps. The excess linewidths we measure do not appear to result from opacity broadening. 12CO clumps are found to be typically less gravitationally bound than 13CO clumps, with some evidence of the kinetic-to-gravitational potential energy ratio increasing with star formation tracers. Further multiline analysis may better constrain the assumptions made in these calculations.
Exploring the Coronal Magnetic Field with Galactic Cosmic Rays: The Sun Shadow Observed by HAWC
Authors: Alfaro R. , Alvarez C. , Arteaga-Velázquez J. C. , Arunbabu K. P. , Avila Rojas D. , Babu R. , Belmont-Moreno E. , Caballero-Mora K. S. , Capistrán T. , Carramiñana A. , Casanova S. , Colín-Farias P. , Cotti U. , Cotzomi J. , Coutiño de León S. , De la Fuente E. , de León C. , Depaoli D. , Diaz Hernandez R. , Díaz-Vélez J. C. , Durocher M. , DuVernois M. A. , Engel K. , Espinoza C. , Fan K. L. , Fraija N. , García-González J. A. , Garfias F. , Gonzalez Muñoz A. , González M. M. , Goodman J. A. , Harding J. P. , Huang D. , Hueyotl-Zahuantitla F. , Iriarte A. , Kaufmann S. , Lara A. , Lee J. , León Vargas H. , Longinotti A. L. , Luis-Raya G. , Malone K. , Martinez O. , Martínez-Castro J. , Matthews J. A. , Miranda-Romagnoli P. , Moreno E. , Mostafá M. , Nayerhoda A. , Nellen L. , Niembro T. , Noriega-Papaqui R. , Omodei N. , Pérez-Pérez E. G. , Rho C. D. , Rosa-González D. , Ruiz-Velasco E. , Ryan J. , Salazar H. , Salazar-Gallegos D. , Sandoval A. , Serna-Franco J. , Smith A. J. , Son Y. , Springer R. W. , Tibolla O. , Tollefson K. , Torres I. , Turner R. , Ureña-Mena F. , Varela E. , Villaseñor L. , Wang X. , Watson I. J. , Willox E. , Yun-Cárcamo S. , Zhou H. 
Published: April 2024

Abstract
Galactic cosmic rays (GCRs) are charged particles that reach the heliosphere almost isotropically in a wide energy range. In the inner heliosphere, the GCR flux is modulated by solar activity so that only energetic GCRs reach the lower layers of the solar atmosphere. In this work, we propose that high-energy GCRs can be used to explore the solar magnetic fields at low coronal altitudes. We used GCR data collected by the High-Altitude Water Cherenkov observatory to construct maps of GCR flux coming from the Sun’s sky direction and studied the observed GCR deficit, known as Sun shadow (SS), over a 6 yr period (2016–2021) with a time cadence of 27.3 days. We confirm that the SS is correlated with sunspot number, but we focus on the relationship between the photospheric solar magnetic field measured at different heliolatitudes and the relative GCR deficit at different energies. We found a linear relationship between the relative deficit of GCRs represented by the depth of the SS and the solar magnetic field. This relationship is evident in the observed energy range of 2.5–226 TeV, but is strongest in the range of 12.4 33.4 TeV, which implies that this is the best energy range to study the evolution of magnetic fields in the low solar atmosphere.
Probing the Stellar Populations and Star Formation History of Early-type Galaxies at 0 < z < 1.1 in the Rest-frame Ultraviolet
Authors: Ali Sadman S. , De Propris Roberto , Chung Chul , Phillipps Steven , Bremer Malcolm N. , Onodera Masato , Sawicki Marcin , Desprez Guillaume , Gwyn Stephen 
Published: April 2024

Abstract
We measure the evolution of the rest-frame near-ultraviolet (NUV)−V colors for early-type galaxies in clusters at 0 < z < 1.1 using data from the Hyper Suprime-Cam Subaru Strategic Program, CFHT Large Area U-band Deep Survey, and local Sloan Digital Sky Survey clusters observed with Galaxy Evolution Explorer. Our results show that there is an excess in the ultraviolet spectrum in most quiescent galaxies (compared to the expectations from models fitting their optical/infrared colors and spectra) below z ∼ 0.6, beyond which the excess UV emission fades rapidly. This evolution of the UV color is only consistent with the presence of a highly evolved, hot horizontal branch subpopulation in these galaxies (among the majority of cool and optically bright stars), comprising on average 10% of the total stellar mass and forming at z > 3. The blue UV colors of early-type galaxies at low–intermediate redshifts are likely driven by this subpopulation being enriched in helium up to ∼44%. At z > 0.8 (when the extra UV component has not yet appeared) the data allow us to constrain the star formation histories of galaxies by fitting models to the evolution of their UV colors: we find that the epoch at which the stellar populations formed lies in the range 3 < z
form < 10 (corresponding to 0.5–2.2 Gyr after the Big Bang) with a star formation e-folding timescale of τ = 0.35–0.7 Gyr, suggesting that these galaxies formed the majority of stars at very high redshift, with a brief yet intense burst of star formation activity. The star formation history and chemical evolution of early-type galaxies resemble those of globular clusters, albeit on much larger scales.
A New Dissociative Galaxy Cluster Merger: RM J150822.0+575515.2
Authors: Stancioli Rodrigo , Wittman David , Finner Kyle , Bouhrik Faik 
Published: April 2024

Abstract
Galaxy cluster mergers that exhibit clear dissociation between their dark matter, intracluster gas, and stellar components are great laboratories for probing dark matter properties. Mergers that are binary and in the plane of the sky have the additional advantage of being simpler to model, allowing for a better understanding of the merger dynamics. We report the discovery of a galaxy cluster merger with all these characteristics and present a multiwavelength analysis of the system, which was found via a search in the redMaPPer optical cluster catalog. We perform a galaxy redshift survey to confirm the two subclusters are at the same redshift (0.541, with 368 ± 519 km s−1 line-of-sight velocity difference between them). The X-ray morphology shows two surface brightness peaks between the brightest cluster galaxies (BCGs). We construct weak-lensing mass maps that reveal a mass peak associated with each subcluster. Fitting Navarro–Frenk–White profiles to the lensing data, we find masses of M
200c = 36 ± 11 × 1013 and 38 ± 11 × 1013
M
⊙
h
−1 for the southern and northern subclusters, respectively. From the mass maps, we infer that the two mass peaks are separated by

520

−
125

+
162

kpc along the merger axis, whereas the two BCGs are separated by 697 kpc. We also present deep GMRT 650 MHz data to search for a radio relic or halo and find none. Using the observed merger parameters, we find analog systems in cosmological n-body simulations and infer that this system is observed between 96 and 236 Myr after pericenter, with the merger axis within 28° of the plane of the sky.
Occurrence dataset of campus birds in Nanjing, Jiangsu Province, China
Authors: Jun Xiao , Chen Ding , Xu Zheping , Zhang Yong 
Published: April 2024

The protection of urban biodiversity plays a critical role in maintaining urban ecological security. As a unique taxon of urban wildlife, birds have been intensively used as an indicator of our surrounding environment. Although the diversity of urban bird species has received increasing attention, present studies are mainly focused on urban parks. As one of the important components of the urban ecosystem, the university campus also plays a critical role in maintaining bird diversity. Due to the lack of observation data, it is a challenge to evaluate the impact of the environmental conditions on campus bird diversity. Given the most concentrated higher education resources in China, Nanjing has a large number of universities, covering a wide area of the urban landscape. The landscape of these universities usually has a high percentage of green space as well as water bodies, which is conducive to attracting various bird species to inhabit. Here, we conducted a one-year bird survey from January 2019 to December 2019 in 12 universities in Nanjing and provided an occurrence dataset containing detailed species and geographical information, providing a good source to study the ecological and anthropogenic factors on urban bird diversity on a local and larger scale.
This dataset represents the first annual record of birds publicly released by 12 universities in Nanjing, Jiangsu Province. It includes classification information, population, distribution, and survey details. All data has been published on GBIF.
La mystérieuse puissance de la vie
Authors: Ulivieri Stiozzi Stefania 
Published: April 2024

Le présent article examine l’œuvre de Sándor Ferenczi en mettant en relation ses conceptions psychanalytiques et les questions éducatives qui, bien que sous-jacentes, constituent une trame omniprésente dans son œuvre. Son attention aiguë à l’imbrication des dynamiques intrapsychiques, des relations intersubjectives et des influences environnementales conduit Ferenczi à une lecture du traumatisme comme résultat d’un processus relationnel dysfonctionnel dans lequel la dimension contextuelle joue un rôle fondamental dès les premières étapes de la vie du nouveau-né. Sa sensibilité est à la base d’une recherche sur la technique psychanalytique qui introduit dans la relation de soin des modalités créatives qui, avant et au-delà de la parole, interrogent le contre-transfert de l’analyste et ses résonances vécues au contact du noyau irreprésentable du traumatisme du patient. Ses théories gardent aujourd’hui encore une résonance prégnante dans la formation des professionnels de l’éducation et du soin, les appelant à réfléchir sur leurs propres dynamiques affectives et sur les formes de ressenti qui orientent leur relation à la souffrance de ceux qui ont vécu des expériences « limites ». Comment s’en inspirer pour développer l’apprentissage par l’expérience dans un contexte universitaire ? Comment aider les éducateurs en formation à faire l’expérience d’un apprentissage insaturé, alimenté par un cadre éthico-esthétique, ouvert aux langages de l’art et de la poésie, visant à développer et à affiner leur sensibilité et leur empathie ?