bluuebunny/crossref_metadata_2025_split huggingface dataset:
Hubungan Kredibilitas Host Live Streaming Dengan Keputusan Pembelian
Authors: Rifana Aufa Hapsari  , Iwan Koswara  , Ikhsan Fuady  
Published: February 2025

Penggunaan e-commerce dan fitur live streaming menjadi salah satu strategi meningkatkan keputusan pembelian produk, maka diperlukan host live streaming yang kredibel untuk mempersuasi konsumen. Penelitian ini bertujuan untuk mengetahui dan mengukur hubungan kredibilitas host live streaming Shopee @lozy_official dengan keputusan pembelian produk Lozy Hijab oleh followers. Berlandaskan pada teori kredibilitas sumber oleh Hovland, Janis, dan Kelley yang menyatakan bahwa komunikan lebih mungkin dipersuasi oleh komunikator yang memiliki kredibilitas tinggi. Pendekatan kuantitatif dengan metode survei diterapkan dalam penelitian ini untuk mengumpulkan data dari 384 followers Shopee @lozy_official selaku sampel penelitian. Jumlah sampel tersebut didapatkan dari hasil perhitungan rumus sampel Isaac & Michael, kemudian teknik pengambilan sampelnya adalah simple random sampling. Survei penelitian ini dilakukan dengan membagikan kuesioner secara daring, yang mana kuesioner tersebut telah teruji validitas dan reliabilitasnya. Analisis data penelitian dilakukan menggunakan uji korelasi Rank Spearman. Hasil temuannya menunjukkan bahwa terdapat hubungan yang positif dan searah antara kredibilitas host live streaming Shopee @lozy_official dengan keputusan pembelian produk Lozy Hijab oleh followers. Dengan demikian, disimpulkan bahwa kredibilitas host live streaming Shopee @lozy_official sudah efektif dalam menumbuhkan keputusan pembelian oleh pengikutnya. Pihak Lozy Hijab disarankan untuk meningkatkan kepercayaan audiens live dengan cara mengembangkan teknik penyampaian informasi yang menarik oleh host live, serta memastikan informasi tersampaikan dengan jelas dan akurat.
An HST Transmission Spectrum of the Closest M Dwarf Transiting Rocky Planet LTT 1445Ab
Authors: Bennett Katherine A. , Sing David K. , Stevenson Kevin B. , Wakeford Hannah R. , Rustamkulov Zafar , Allen Natalie H. , Lothringer Joshua D. , MacDonald Ryan J. , Mayne Nathan J. , Fu Guangwei 
Published: February 2025

Abstract
Which rocky exoplanets have atmospheres? This presumably simple question is the first that must be answered to understand the prevalence of nearby habitable planets. A mere 6.9 pc from Earth, LTT 1445A is the closest transiting M dwarf system, and its largest known planet, at 1.31 R⊕ and 424 K, is one of the most promising targets in which to search for an atmosphere. We use Hubble Space Telescope/Wide Field Camera 3 transmission spectroscopy with the G280 and G141 grisms to study the spectrum of LTT 1445Ab between 0.2 and 1.65 μm. In doing so, we uncover an ultraviolet (UV) flare on the neighboring star LTT 1445C that is completely invisible at optical wavelengths; we report one of the first simultaneous near-UV/optical spectra of an M dwarf flare. The planet spectrum is consistent with a flat line (with median transit depth uncertainties of 128 and 52 ppm for the G280 and G141 observations, respectively), though the infrared (IR) portion displays potential features that could be explained by known opacity sources such as HCN. Some atmospheric retrievals weakly favor (∼2σ) an atmosphere, but it remains challenging to discern between stellar contamination, an atmosphere, and a featureless spectrum at this time. We do, however, confidently rule out ≤100× solar metallicity atmospheres. Although stellar contamination retrievals cannot fit the IR features well, the overall spectrum is consistent with stellar contamination from hot or cold spots. Based on the UV/optical data, we place limits on the extent of stellar variability expected in the near-IR (30–40 ppm), which will be critical for future James Webb Space Telescope observations.
Forest Fire Clustering: A Novel Tool for Identifying Star Members of Clusters
Authors: Wei Xingyin , Chen Jing , Zhang Su , He Feilong , Zhao Yunbo , He Xuran , Fang Yongjie , Chen Xinhao , Yang Hao 
Published: February 2025

Abstract
In the era of a data-driven landscape, the development of an efficient and interpretable method has become a pivotal tool for robustly identifying memberships of clusters. We present a novel cluster finder approach called forest fire clustering (FFC). FFC combines iterative label propagation with parallel Monte Carlo simulation to achieve internal validation of clustering results. We use a Gaia DR3 catalog comprising 322 random objects with distinct heliocentric distances from approximately 0 to 5 kpc, along with one ultrafaint dwarf galaxy Bootes I (∼63 kpc), as our validation sample. We compare the performance of FFC with that of DBSCAN and HDBSCAN on this data set by configuring them into the same processing pipeline for identifying star members. Our results indicate that FFC outperforms the two others in terms of the quality of clusters, particularly for clusters located at distances greater than 2 kpc. Additionally, FFC demonstrates robust performance and efficiency. Based on the high-quality clusters derived from FFC, we provide a detailed analysis of cluster properties. We determine various cluster parameters, including age, mass, [Fe/H], distance modulus, reddening, and binary fraction. Furthermore, dynamic properties are reliably estimated through the fitting of radial density profiles and theoretical models. This study suggests that FFC is a suitable tool for identifying reliable memberships of stellar systems, highlighting the discovery of more distant clusters and enabling the identification of high-quality clusters to accurately uncover cluster properties.
A Search for Radio Millisecond Pulsar Companions around Extremely Low-mass White Dwarfs with Ellipsoidal Variability
Authors: Huang W. J. , Tam Pak-Hin Thomas , Ren L. L. , Lin J. M. 
Published: February 2025

Abstract
Extremely low-mass (ELM) white dwarfs (WDs) are helium-core WDs with masses less than 0.3 M
⊙. Short-period ELM WD binaries that exhibit ellipsoidal variations may harbor heavier companions, either massive WDs or millisecond pulsars (MSPs). In this study, we selected ∼12,000 ELM WDs or their candidates, and searched for ellipsoidal-like lightcurves with orbital periods shorter than 1 day, by using the public data from Zwicky Transient Facility. Finally, 23 such systems were found, with 17 being newly discovered. We selected nine high-priority targets likely to evolve from the Roche lobe overflow channel and estimated their companion masses from the extracted ellipsoidal variation amplitude. Among them, four targets have companion masses exceeding 1 M
⊙. We performed a search for radio pulsations from six of these targets by using Five-hundred-meter Aperture Spherical radio Telescope. However, no convincing radio pulse signals were found, resulting in upper limits for the radio flux at around 8 μJy. Given the nondetection of radio pulsations from a total of 11 similar systems, the fraction of ellipsoidal ELM WDs around MSPs is estimated to be below 15

−
3

+
6

%. We anticipate that multiwavelength studies of more ellipsoidal-like ELM WDs will further constrain the fraction.
ALMA Observations of Massive Clouds in the Central Molecular Zone: External-pressure-confined Dense Cores and Salpeter-like Core Mass Functions
Authors: Zhang 张 Zhenying 朕荧 , Lu 吕 Xing 行 , Liu 刘 Tie 铁 , Qin 秦 Sheng-Li 胜利 , Ginsburg Adam , Cheng 程 Yu 宇 , Liu Hauyu Baobab , Walker Daniel L. , Tang 汤 Xindi 新弟 , Li 李 Shanghuo 尚活 , Zhang Qizhou , Pillai Thushara , Kauffmann Jens , Battersby Cara , Feng 冯 Siyi 思轶 , Zhang 张 Suinan 遂楠 , Gu 顾 Qi-Lao 琦烙 , Xu 许 Fengwei 峰玮 , Jiao 焦 Wenyu 文裕 , Liu 刘 Xunchuan 训川 , Chen 陈 Li 立 , Luo 罗 Qiu-yi 秋怡 , Mai 麦 Xiaofeng 晓枫 , Li 李 Zi-yang 紫杨 , Yang 杨 Dongting 东庭 , Shen 沈 Xianjin 先进 , Liu 刘 Meizhu 梅竹 , Shen Zhiqiang 
Published: February 2025

Abstract
We present Atacama Large Millimeter/submillimeter Array Band 6 (1.3 mm) observations of dense cores in three massive molecular clouds within the central molecular zone (CMZ) of the Milky Way, including the Dust Ridge cloud e, Sgr C, and the 20 km s−1 cloud, at a spatial resolution of 2000 au. Among the 834 cores identified from the 1.3 mm continuum, we constrain temperatures and linewidths of 253 cores using local thermodynamic equilibrium methods to fit the H2CO and/or CH3CN spectra. We determine their masses using the 1.3 mm dust continuum and derived temperatures, and then evaluate their virial parameters using the H2CO and/or CH3CN linewidths and construct the core mass functions (CMFs). We find that the contribution of external pressure is crucial for the virial equilibrium of the dense cores in the three clouds, which contrasts with the environment in the Galactic disk where dense cores are already bound, even without the contribution of external pressure. With our new temperature estimates we also find that the CMFs show a Salpeter-like slope in the high-mass (≳3–6 M
⊙) end, a change from previous works. Combined with the possible top-heavy initial mass functions (IMFs) in the CMZ, our result suggests that gas accretion and further fragmentation may play important roles in transforming the CMF to the IMF.
Revisiting Near-infrared Features of Kilonovae: The Importance of Gadolinium
Authors: Rahmouni Salma , Tanaka Masaomi , Domoto Nanae , Kato Daiji , Hotokezaka Kenta , Aoki Wako , Hirano Teruyuki , Kotani Takayuki , Kuzuhara Masayuki , Tamura Motohide 
Published: February 2025

Abstract
The observation of the kilonova AT2017gfo and investigations of its light curves and spectra confirmed that neutron star mergers are sites of r-process nucleosynthesis. However, the identification of elements responsible for the spectral features is still challenging, particularly at the near-infrared wavelengths. In this study, we systematically searched for all possible near-infrared transitions of heavy elements using experimentally calibrated energy levels. Our analysis reveals that most candidate elements with strong absorption lines are lanthanides (Z = 57–71) and actinides (Z = 89–103). This is due to their complex structures leading to many low-lying energy levels, which results in strong transitions in the near-infrared range. N. Domoto et al. (2022) have shown that La iii and Ce iii can explain the absorption features at λ ∼ 12000–15000 Å. While our results confirm that these two elements show strong infrared features, we additionally identify Gd iii as the next most promising species. Due to its unique atomic structure involving the half-filled 4f and the outer 5d orbitals, Gd iii has one of the lowest-lying energy levels, between which relatively strong transitions occur. We also find absorption lines caused by Gd iii in the near-infrared spectrum of a chemically peculiar star HR 465, which supports their emergence in kilonova spectra. By performing radiative transfer simulations, we confirm that Gd iii lines affect the feature at ∼12000 Å previously attributed to La iii. Future space-based time-series observations of kilonova spectra will allow the identification of Gd iii lines.
AEOS: Star-by-star Cosmological Simulations of Early Chemical Enrichment and Galaxy Formation
Authors: Brauer Kaley , Emerick Andrew , Mead Jennifer , Ji Alexander P. , Wise John H. , Bryan Greg L. , Mac Low Mordecai-Mark , Côté Benoit , Andersson Eric P. , Frebel Anna 
Published: February 2025

Abstract
The Aeos project introduces a series of high-resolution cosmological simulations that model star-by-star chemical enrichment and galaxy formation in the early Universe, achieving 1 pc resolution. These simulations capture the complexities of galaxy evolution within the first ~300 Myr by modeling individual stars and their feedback processes. By incorporating chemical yields from individual stars, Aeos generates galaxies with diverse stellar chemical abundances, linking them to hierarchical galaxy formation and early nucleosynthetic events. These simulations underscore the importance of chemical abundance patterns in ancient stars as vital probes of early nucleosynthesis, star formation histories, and galaxy formation. We examine the metallicity floors of various elements resulting from Population III enrichment, providing best-fit values for eight different metals (e.g., [O/H] = −4.0) to guide simulations without Population III models. Additionally, we identify galaxies that begin star formation with Population II after external enrichment and investigate the frequency of carbon-enhanced metal-poor stars at varying metallicities. The Aeos simulations offer detailed insights into the relationship between star formation, feedback, and chemical enrichment. Future work will extend these simulations to later epochs to interpret the diverse stellar populations of the Milky Way and its satellites.
Little Red Dots: Rapidly Growing Black Holes Reddened by Extended Dusty Flows
Authors: Li Zhengrong , Inayoshi Kohei , Chen Kejian , Ichikawa Kohei , Ho Luis C. 
Published: February 2025

Abstract
The James Webb Space Telescope (JWST) observations have revolutionized extragalactic research, particularly with the discovery of little red dots (LRDs), which have been discovered as a population of dust-reddened broad-line active galactic nuclei (AGNs). Their unique V-shaped spectral feature, characterized by a red optical continuum and a UV excess in the rest frame, challenges us to discern the relative contributions of the galaxy and AGN. We study a spectral energy distribution (SED) model for LRDs from rest-frame UV to infrared bands. We hypothesize that the incident radiation from an AGN, characterized by a typical SED, is embedded in an extended dusty medium with an extinction law similar to those seen in dense regions such as Orion Nebula or certain AGN environments. The UV−optical spectrum is described by dust-attenuated AGN emission, featuring a red optical continuum at λ > 4000 Å and a flat UV spectral shape established through a gray extinction curve at λ < 3000 Å, due to the absence of small-size grains. There is no need for additional stellar emission or AGN scattered light. In the infrared, the SED is shaped by an extended dust and gas distribution (γ < 1; ρ ∝ r
−γ
) with characteristic gas densities of ≃10–103 cm−3, which allows relatively cool dust temperatures to dominate the radiation. As a result, these dust structures shift the emission energy peak from near-infrared to mid-infrared bands in the rest frame; for sources at z ~ 4–7, the corresponding wavelengths shift from the JWST/MIRI to Herschel range. This model, unlike the typical AGN hot torus models, can produce an infrared SED flattening that is consistent with LRD observations through JWST MIRI. Such a density structure can arise from the coexistence of inflows and outflows during the early assembly of galactic nuclei. This might be the reason why LRDs emerge preferentially in the high-redshift Universe younger than 1 billion years.
The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA
Authors: Fuller Lindsay , Lopez-Rodriguez Enrique , García-Bernete Ismael , Ramos Almeida Cristina , Alonso-Herrero Almudena , Packham Chris , Zhang Lulu , Leist Mason , Levenson Nancy A. , Imanishi Masatoshi , Hoenig Sebastian , Stalevski Marko , Ricci Claudio , Hicks Erin , Bellocchi Enrica , Combes Francoise , Davies Ric , García Burillo Santiago , González Martín Omaira , Izumi Takuma , Labiano Alvaro , Pereira Santaella Miguel , Rigopoulou Dimitra , Rosario David , Rouan Daniel , Shimizu Taro , Ward Martin 
Published: February 2025

Abstract
We present a 19.7–214 μm imaging atlas of local (4–181 Mpc; median 43 Mpc) active galactic nuclei (AGN) observed with FORCAST and HAWC+ on board the SOFIA telescope with angular resolutions ~3″–20″. This atlas comprises 22 Seyferts (17 Type 2 and five Type 1) with a total of 69 images, 41 of which have not been previously published. The AGN span a range of luminosities of

log
10

(

L
bol

[
erg

s

-
1

]
)
=
[
42
,
46
]

with a median of

log

10

(

L

bol

[

erg

s

−
1

]
)
=
44.1
±
1.0

. We provide the total fluxes of our sample using aperture photometry for point-source objects and a 2D Gaussian fitting for objects with extended host galaxy emission, which was used to estimate the unresolved nuclear component. Most galaxies in our sample are pointlike sources; however, four sources (Centaurus A, Circinus, NGC 1068, and NGC 4388) show extended emission in all wavelengths. The 30–40 μm extended emission in NGC 4388 is coincident with the narrow-line region at PA ~ 50°, while the dusty extension at longer wavelengths arises from the host galaxy at PA ~ 90°. Our new observations allow us to construct the best-sampled parsec-scales (spectral energy distributions, SEDs) available between 30 and 500 μm for a sample of nearby AGN. We estimate that the average peak wavelength of the nuclear SEDs is ~40 μm in νF

ν
, which we associate with an unresolved extended dusty region heated by the AGN.
Calibrating the Color–Magnitude Relation of M Giants by Using Open Clusters
Authors: Tang X. Y. , Hao C. J. , Li J. , Yan Z. Z. , Xu Y. , Zhong J. , Lin Z. H. , Li Y. J. , Liu D. J. , Ding L. F. , Long X. F. 
Published: February 2025

Abstract
M giants, with their distinctive properties such as high luminosity, serve as excellent indicators for mapping the structure of the Milky Way. The distance to distant M giants can be determined by using the color–magnitude relation (CMR), which is derived from color–magnitude diagrams of specific systems in previous studies. In this work, we aimed to achieve more accurate distance determination for M giants by focusing on open clusters (OCs) with a large number of member stars and thus improve the CMR. For the first time, we compiled a census of OCs harboring M giants using Gaia Data Release 3 (DR3) and Large Sky Area Multi-Object Fiber Spectroscopic Telescope Data Release 9. We identified 58 M giants associated with 43 OCs and obtained their astrometric and photometric parameters from Gaia DR3. Using the distances of these OCs, we derived the CMR for M giants as a linear correlation, expressed as

M

K

s

=
3.85
−
8.26
(
J
−

K

s

)

. This linear relation proved superior to the empirical distance relation in characterizing the CMR of M giants. The photometric distances of M giants derived from the CMR are consistent with the parallax distances from Gaia and known spectroscopic distances, with median deviations of 1.5% and 2.3%, respectively. Using the distances of M giants derived from the CMR, we computed their radial velocity (V

R
), azimuthal velocity (V

ϕ
), and vertical velocity (V

Z
), respectively. The distributions of these velocities revealed key features of the Galactic disk, including oscillation, north–south rotational asymmetry, and warp. These findings are consistent with previous studies and further validate the reliability of the derived CMR.
Woody flora of the Prof. Dr. Karl Arens Reserve, Corumbataí, São Paulo, Brazil
Authors: Santos Lilian , de Moraes Pedro Luís 
Published: February 2025

This study was conducted in the Prof. Dr. Karl Arens Reserve, Corumbataí, São Paulo. The area is a Cerrado fragment, with no records of fire since 1962 and is characterised by the predominance of Cerradão phytophysiognomy. Although several studies have been conducted in the Reserve, there was no testimony material for some species in the Herbarium Rioclarense (HRCB), nor a list of vouchers for any taxon in the main publications. Thus, the objective of this work was to undertake a floristic survey of the woody species in the Reserve, based on herbarium specimens and fieldwork.
The survey in HRCB recorded 510 exsiccatae belonging to 160 species and 44 families. We also conducted 24 fieldwork expeditions between 2019 and 2021 and recorded 118 species in 39 families. In total, 193 woody species were recorded for the Reserve in Corumbataí. Species such as Copaifera langsdorffii and Myrcia neoclusiifolia had already been cited for the area, but there was no testimony material in the herbarium. Machaerium nyctitans and Alchornea glandulosa are examples of new records for the Reserve. Fabaceae, Asteraceae, Myrtaceae, Melastomataceae and Rubiaceae were the families with the greatest species diversity.
La place des femmes dans l’enseignement technique agricole en France, XIX e –XX e siècle
Authors: Charmasson Thérèse , Lelorrain Anne-Marie 
Published: February 2025

Au sein de l’enseignement professionnel de l’agriculture, placé sous la tutelle du ministère de l’Agriculture, qui se met progressivement en place à compter de 1848, les femmes sont absentes jusqu’en 1886, date de la fondation de la première école professionnelle agricole spécialement destinée aux ﬁlles : l’École pratique de laiterie de Coëtlogon. Ce n’est que dans les premières années du xx e siècle, qu’on voit se développer deux types d’enseignement : l’enseignement postscolaire agricole et l’enseignement saisonnier, où les ﬁlles trouvent leur place avec l’enseignement agricole ménager, et l’enseignement postscolaire ménager. Pour la première fois, la loi du 2 août 1918 donne, à côté de celle des écoles destinées aux jeunes gens, la liste des établissements « dispensant un enseignement professionnel ou technique de l’agriculture » destiné aux jeunes ﬁlles et organisé en trois niveaux. La loi du 2 août 1960 prévoit une élévation générale des niveaux de formation, mais l’enseignement féminin reste toujours sanctionné par des diplômes spéciﬁques. Avec les lois Rocard (1984), de nouvelles missions sont assignées à l’enseignement agricole, mais ce n’est que très progressivement que les différences s’estompent entre les formations ouvertes aux jeunes gens et celles ouvertes aux jeunes ﬁlles. Le pourcentage des jeunes ﬁlles augmente dans l’enseignement supérieur, mais leur devenir professionnel n’est pas toujours au sein de l’exploitation proprement dite.
Satisfaction des patients hospitalisés lors du premier confinement :
Authors: Cazeneuve Hervé , Capgras Jean-Baptiste , Pascal Christophe , Michel Philippe 
Published: February 2025

Dans le cadre du projet COPING (Covid pandemic institutional management), cet article se propose d’étudier les éventuelles variations des perceptions des patients hospitalisés pendant l’épidémie de Covid-19. Pour ce faire, une comparaison entre les périodes confinées et non confinées a été menée à partir des résultats de l’enquête e-Satis disponibles dans les quatre centres hospitaliers universitaires (CHU) de la région Auvergne-Rhône-Alpes (Hospices civils de Lyon, CHU Grenoble-Alpes, CHU de Saint-Étienne, CHU de Clermont-Ferrand). Ce travail permet de constater qu’il existe peu de différences importantes entre les périodes, certaines statistiquement significatives en raison de la puissance de l’étude. Les patients de ces CHU ont vécu pendant l’ensemble de la période une expérience assez similaire à celle des années « non-Covid-19 ». Néanmoins, la période « Covid-19 » est marquée par une contradiction. D’un côté, on observe un renforcement global de la vision positive de l’hôpital et des soignants, ce qui se reflète dans les appréciations portées sur les éléments matériels (des repas et des chambres plus confortables) et immatériels (soins, accueil). De l’autre côté, la baisse de satisfaction concernant les visites et les variations observées tout au long de la période interrogent sur la manière dont des catégories de patients ont appréhendé ces transformations.