bluuebunny/crossref_metadata_2025_split huggingface dataset:
A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Brande Jonathan , Crossfield Ian J. M. , Kreidberg Laura , Oklopčić Antonija , Polanski Alex S. , Barman Travis , Benneke Björn , Christiansen Jessie L. , Dragomir Diana , Foreman-Mackey Daniel , Fortney Jonathan J. , Greene Thomas P. , Howard Andrew W. , Knutson Heather A. , Lothringer Joshua D. , Mikal-Evans Thomas , Morley Caroline V. 
Published: October 2022

Abstract
We report observations of the recently discovered warm Neptune TOI-674 b (5.25 R
⊕, 23.6 M
⊕) with the Hubble Space Telescope’s Wide Field Camera 3 instrument. TOI-674 b is in the Neptune desert, an observed paucity of Neptune-size exoplanets at short orbital periods. Planets in the desert are thought to have complex evolutionary histories due to photoevaporative mass loss or orbital migration, making identifying the constituents of their atmospheres critical to understanding their origins. We obtained near-infrared transmission spectroscopy of the planet’s atmosphere with the G141 grism. After extracting, detrending, and fitting the spectral light curves to measure the planet’s transmission spectrum, we used the petitRADTRANS atmospheric spectral synthesis code to perform retrievals on the planet’s atmosphere to identify which absorbers are present. These results show moderate evidence for increased absorption at 1.4 μm due to water vapor at 2.9σ (Bayes factor = 15.8), as well as weak evidence for the presence of clouds at 2.2σ (Bayes factor = 4.0). TOI-674 b is a strong candidate for further study to refine the water abundance, which is poorly constrained by our data. We also incorporated new TESS short-cadence optical photometry, as well as Spitzer/IRAC data, and refit the transit parameters for the planet. We find the planet to have the following transit parameters: R

p
/R
* = 0.1135 ± 0.0006, T
0 = 2458544.523792 ± 0.000452 BJD, and P = 1.977198 ± 0.00007 day. These measurements refine the planet radius estimate and improve the orbital ephemerides for future transit spectroscopy observations of this highly intriguing warm Neptune.
Joint Constraints on Exoplanetary Orbits from Gaia DR3 and Doppler Data
Authors: Winn Joshua N. 
Published: October 2022

Abstract
The third Gaia data release includes a catalog of exoplanets and exoplanet candidates identified via the star’s astrometric motion. This paper reports on tests for consistency between the Gaia two-body orbital solutions and precise Doppler velocities for stars currently amenable to such a comparison. For BD-17 0063, HD 81040, and HD 132406, the Gaia orbital solution and the Doppler data were found to be consistent and were fitted jointly to obtain the best possible constraints on the planets’ orbits and masses. Inconsistencies were found for four stars: HD 111232, probably due to additional planets that were not included in the astrometric model; HD 175167 and HR 810, possibly due to inaccurate treatment of non-Gaussian uncertainties in the Gaia orbital solutions; and HIP 66074, for unknown reasons. Consistency tests were also performed for HD 114762, which was reported in 1989 to have a brown dwarf or exoplanet but has since been shown to be a binary star. The joint Gaia–Doppler analysis shows the secondary mass to be 0.215 ± 0.013 M
⊙ and the orbital inclination to be 3.°63 ± 0.°06.
DELIGHT: Deep Learning Identification of Galaxy Hosts of Transients using Multiresolution Images
Authors: Förster Francisco , Muñoz Arancibia Alejandra M. , Reyes-Jainaga Ignacio , Gagliano Alexander , Britt Dylan , Cuellar-Carrillo Sara , Figueroa-Tapia Felipe , Polzin Ava , Yousef Yara , Arredondo Javier , Rodríguez-Mancini Diego , Correa-Orellana Javier , Bayo Amelia , Bauer Franz E. , Catelan Márcio , Cabrera-Vives Guillermo , Dastidar Raya , Estévez Pablo A. , Pignata Giuliano , Hernández-García Lorena , Huijse Pablo , Reyes Esteban , Sánchez-Sáez Paula , Ramírez Mauricio , Grandón Daniela , Pineda-García Jonathan , Chabour-Barra Francisca , Silva-Farfán Javier 
Published: October 2022

Abstract
We present DELIGHT, or Deep Learning Identification of Galaxy Hosts of Transients, a new algorithm designed to automatically and in real time identify the host galaxies of extragalactic transients. The proposed algorithm receives as input compact, multiresolution images centered at the position of a transient candidate and outputs two-dimensional offset vectors that connect the transient with the center of its predicted host. The multiresolution input consists of a set of images with the same number of pixels, but with progressively larger pixel sizes and fields of view. A sample of 16,791 galaxies visually identified by the Automatic Learning for the Rapid Classification of Events broker team was used to train a convolutional neural network regression model. We show that this method is able to correctly identify both relatively large (10″ < r < 60″) and small (r ≤ 10″) apparent size host galaxies using much less information (32 kB) than with a large, single-resolution image (920 kB). The proposed method has fewer catastrophic errors in recovering the position and is more complete and has less contamination (<0.86%) recovering the crossmatched redshift than other state-of-the-art methods. The more efficient representation provided by multiresolution input images could allow for the identification of transient host galaxies in real time, if adopted in alert streams from new generation of large -etendue telescopes such as the Vera C. Rubin Observatory.
Laboratory Study of the Cameron Bands and UV Doublet in the Middle Ultraviolet 180–300 nm by Electron Impact upon CO2 with Application to Mars
Authors: Lee Rena A. , Ajello Joseph M. , Malone Charles P. , Evans J. Scott , Veibell Victoir , Holsclaw Gregory M. , McClintock William E. , Hoskins Alan C. , Jain Sonal K. , Gérard Jean-Claude , Aryal Saurav , Schneider Nicholas M. 
Published: October 2022

Abstract
We have observed electron impact fluorescence from CO2 to excite the Cameron bands (CBs), CO (a
3Π → X
1Σ+; 180–280 nm), the first-negative group (1NG) bands, CO+ (B
2Σ+ → X
2Σ+; 180–320 nm), the fourth-positive group (4PG) bands, CO (A
1Π → X
1Σ+; 111–280 nm), and the UV doublet, CO2
+ (

B

˜

2

Σ

u

+

→

X

˜

2

Π

g

;

288.3 and 289.6 nm) in the ultraviolet (UV). This wavelength range matches the spectral region of past and present spacecraft equipped to observe UV dayglow and aurora emissions from the thermospheres (100–300 km) of Mars and Venus. Our large vacuum system apparatus is able to measure the emission cross sections of the strongest optically forbidden UV transitions found in planetary spectra. Based on our cross-sectional measurements, previous CB emission cross-sectional errors exceed a factor of 3. The UV doublet lifetime is perturbed through

B

˜

2

Σ

u

+

−

A

˜

2

Π

u

spin–orbit coupling. Forward modeling codes of the Mars dayglow have not been accurate in the mid-UV due to systematic errors in these two emission cross sections. We furnish absolute emission cross sections for several band systems over electron energies 20–100 eV for CO2. We present a CB lifetime, which together with emission cross sections, furnish a set of fundamental physical constants for electron transport codes such as AURIC (Atmospheric Ultraviolet Radiance Integrated Code). AURIC and Trans-Mars are used in the analysis of UV spectra from the Martian dayglow and aurora.
Phase Mixing and the 1/f Spectrum in the Solar Wind
Authors: Magyar Norbert , Doorsselaere Tom Van 
Published: October 2022

Abstract
The origin and evolution of the 1/f power law observed in the energy spectrum of solar coronal and solar wind fluctuations at scales of around an hour is not entirely understood. Several existing theories aim at explaining it, involving both linear and nonlinear mechanisms. An often overlooked property of the solar corona and solar wind is their highly inhomogeneous nature. In this paper we investigate the linear evolution of pure Alfvén and surface Alfvén waves propagating through a plasma that is inhomogeneous across the magnetic field. The inhomogeneity is given by density, which we model to be 2D colored noise, with power spectral slopes ranging from −2 to −1. Alfvén waves propagate independently on individual magnetic field lines, and eventually get completely out of phase through the process of phase mixing, leading to unrealistic spectra. When the coupling between the inhomogeneous background and the propagating waves is fully accounted for, transverse waves such as surface Alfvén waves (also referred to as kink or Alfvénic) appear, showing collective wave behavior of neighboring magnetic field lines with different Alfvén speeds. We show that the linear cascade of surface Alfvén wave energy, induced by phase mixing and resonant absorption, leads to a perpendicular wave energy spectrum, which tends to the perpendicular power spectrum of the background density. Based on our model, we propose that a perpendicular density power spectrum of 1/f in the solar corona can induce, through linear processes, the 1/f spectrum of the fluctuations that is observed at the largest scales.
Sequential Star Formation in the Young SMC Region NGC 602: Insights from ALMA
Authors: O’Neill Theo J. , Indebetouw Rémy , Sandstrom Karin , Bolatto Alberto D. , Jameson Katherine E. , Carlson Lynn R. , Finn Molly K. , Meixner Margaret , Sabbi Elena , Sewiło Marta 
Published: October 2022

Abstract
NGC 602 is a young, low-metallicity star cluster in the “Wing” of the Small Magellanic Cloud. We reveal the recent evolutionary past of the cluster through analysis of high-resolution (∼0.4 pc) Atacama Large Millimeter/submillimeter Array observations of molecular gas in the associated H ii region N90. We identify 110 molecular clumps (R < 0.8 pc) traced by CO emission, and study the relationship between the clumps and associated young stellar objects (YSOs) and pre-main-sequence (PMS) stars. The clumps have high virial parameters (typical α
vir = 4–11) and may retain signatures of a collision in the last ≲8 Myr between H i components of the adjacent supergiant shell SMC-SGS 1. We obtain a CO-bright-to-H2 gas conversion factor of X
CO,B
= (3.4 ± 0.2) × 1020 cm−2 (K km s−1)−1, and correct observed clump properties for CO-dark H2 gas to derive a total molecular gas mass in N90 of 16,600 ± 2400 M
⊙. We derive a recent (≲1 Myr) star formation rate of 130 ± 30 M
⊙ Myr−1 with an efficiency of 8% ± 3% assessed through comparing total YSO mass to total molecular gas mass. Very few significant radial trends exist between clump properties or PMS star ages and distance from NGC 602. We do not find evidence for a triggered star formation scenario among the youngest (≲2 Myr) stellar generations, and instead conclude that a sequential star formation process in which NGC 602 did not directly cause recent star formation in the region is likely.
MaNGA 8313-1901: Gas Accretion Observed in a Blue Compact Dwarf Galaxy?
Authors: Ju 居 Mengting 梦婷 , Yin 尹 Jun 君 , Liu 刘 Rongrong 蓉蓉 , Hao 郝 Lei 蕾 , Shao 邵 Zhengyi 正义 , Feng 冯 Shuai 帅 , Riffel Rogério , Liu 刘 Chenxu 辰旭 , Stark David V. , Shen 沈 Shiyin 世银 , Telles Eduardo , Fernández-Trincado José G. , Wang 王 Junfeng 俊峰 , Xu 徐 Haiguang 海光 , Bizyaev Dmitry , Rong 容 Yu 昱 
Published: October 2022

Abstract
Gas accretion is an important process in the evolution of galaxies, but it has limited direct observational evidences. In this paper, we report the detection of a possible ongoing gas accretion event in a blue compact dwarf (BCD) galaxy, MaNGA 8313-1901, observed by the Mapping Nearby Galaxies and Apache Point Observatory (MaNGA) program. This galaxy has a distinct off-centered blue clump to the northeast (the NE clump) that shows low metallicity and enhanced star formation. The kinematics of the gas in the NE clump also seems to be detached from the host BCD galaxy. Together with the metallicity drop of the NE clump, it suggests that the NE clump likely has an external origin, such as gas accretion or galaxy interaction, rather than an internal origin, such as an H II complex in the disk. After removing the underlying host component, we find that the spectrum of the “pure” clump can match very well with a modeled spectrum containing a stellar population of the young stars (≤7 Myr) only. This may imply that the galaxy is experiencing an accretion of cold gas, instead of a merger event involving galaxies with significant preexisting old stars. We also find signs of another clump (the SW clump) at the southwest corner of the host galaxy, and the two clumps may share the same origin of gas accretion.
Tracking a Beam of Electrons from the Low Solar Corona into Interplanetary Space with the Low Frequency Array, Parker Solar Probe, and 1 au Spacecraft
Authors: Badman Samuel T. , Carley Eoin , Cañizares Luis Alberto , Dresing Nina , Jian Lan K. , Lario David , Gallagher Peter T. , Martínez Oliveros Juan C. , Pulupa Marc , Bale Stuart D. 
Published: October 2022

Abstract
Type III radio bursts are the result of plasma emission from mildly relativistic electron beams propagating from the low solar corona into the heliosphere where they can eventually be detected in situ if they align with the location of a heliospheric spacecraft. Here we observe a type III radio burst from 0.1 to 16 MHz using the Parker Solar Probe (PSP) FIELDS Radio Frequency Spectrometer (RFS) and from 20 to 80 MHz using the Low Frequency Array (LOFAR). This event was not associated with any detectable flare activity but was part of an ongoing type III and noise storm that occurred during PSP encounter 2. A deprojection of the LOFAR radio sources into 3D space shows that the type III radio burst sources were located on open magnetic field from 1.6 to 3 R
⊙ and originated from a near-equatorial active region around longitude E48°. Combining PSP/RFS observations with WIND/WAVES and Solar Terrestrial Relations Observatory (STEREO) WAVES, we reconstruct the type III radio source trajectory in the heliosphere interior to PSP’s position, assuming ecliptic confinement. An energetic electron enhancement is subsequently detected in situ at the STEREO A spacecraft at compatible times, although the onset and duration suggests the individual burst contributes a subset of the enhancement. This work shows relatively small-scale flux emergence in the corona can cause the injection of electron beams from the low corona into the heliosphere, without needing a strong solar flare. The complementary nature of combined ground and space-based radio observations, especially in the era of PSP, is also clearly highlighted by this study.
Effective Drag in Rotating, Poorly Conducting Plasma Turbulence
Authors: Benavides Santiago J. , Burns Keaton J. , Gallet Basile , Flierl Glenn R. 
Published: October 2022

Abstract
Despite the increasing sophistication of numerical models of hot Jupiter atmospheres, the large timescale separation required in simulating the wide range in electrical conductivity between the dayside and nightside has made it difficult to run fully consistent magnetohydrodynamic (MHD) models. This has led to many studies that resort to drag parameterizations of MHD. In this study, we revisit the question of the Lorentz force as an effective drag by running a series of direct numerical simulations of a weakly rotating, poorly conducting flow in the presence of a misaligned, strong background magnetic field. We find that the drag parameterization fails once the timescale associated with the Lorentz force becomes shorter than the dynamical timescale in the system, beyond which the effective drag coefficient remains roughly constant, despite orders-of-magnitude variation in the Lorentz (magnetic) timescale. We offer an improvement to the drag parameterization by considering the relevant asymptotic limit of low conductivity and strong background magnetic field, known as the quasi-static MHD approximation of the Lorentz force. This approximation removes the fast timescale associated with magnetic diffusion, but retains a more complex version of the Lorentz force, which could be utilized in future numerical models of hot Jupiter atmospheric circulation.
Gênero e inclusão na leitura para todos e todas: histórias da/para comunidade com abordagens da tecnologia e do desenho universal para aprendizagem
Authors: Castelini Alessandra Lopes de Oliveira , Sousa Célia Maria Adão Oliveira Aguiar , Quaresma da Silva Denise Regina 
Published: October 2022

Este artigo objetiva discutir as possibilidades de abarcar questões de gênero e inclusão por meio de um projeto internacional de Leitura para Todos/Todas que decorre em Portugal e propõe livros em multiformatos e multissensoriais baseadas na mediação da Tecnologia e abordagens do Desenho Universal para a Aprendizagem – DUA. O estudo em questão culminou na criação e difusão de uma história da/para comunidade que foi ressignificada no trabalho coletivo intergeracional, enquanto artefato cultural e que impulsiona o papel dos educadores/docentes na desmistificação de temas da inclusão e sexismo naturalizados nas histórias infantis. A questão que motivou esse estudo foi analisar quais as potencialidades do livro em multiformatos/multissensoriais “Rainha das Rosas” para discussões de temas que abarcam os estudos de gênero, diversidade e inclusão. O estudo trata de uma pesquisa exploratória, de natureza qualitativa e apoia-se metodologicamente no estudo de caso etnográfico. Após a recolha dos dados optou-se pela triangulação para validação dos resultados. As reflexões descritas nesse artigo caracterizam-se como recorte de pesquisa das autoras e de processo doutoral, articuladas a um projeto de pesquisa internacional entre Brasil e Portugal com apoio financeiro da CAPES. A análise evidenciou que a obra oportuniza reflexões sobre as diferentes tecnologias em prol da comunicação e inclusão, favorece a discussões de diversidade e gênero ao ressaltar o papel da mulher na sociedade e as formas sexistas, patriarcais e culturais evidenciadas nessa obra infantil, bem como a viabilização de novas formas de ressignificar práticas de leitura, a ampliar o conhecimento das relações existentes entre inclusão e diversidade, e que tensiona o (re) pensar de forma crítica as criações/adaptações de obras literárias além de estimular o diálogo inter, trans e multidisciplinar.
Pandémie de Covid-19 : contribution de la métrologie à l’évaluation de l’efficacité de filtration des masques de protection
Authors: Gaie-Levrel François , Bescond Alexandre , Fouqueau Axel , Macé Tatiana , Vaslin-Reimann Sophie 
Published: October 2022

En 2020, la communauté scientifique et l’Organisation mondiale de la santé confirmaient le risque de transmission aérienne du coronavirus Sars-CoV-2. En raison de la pénurie mondiale de masques, plusieurs pays ont introduit de nouveaux types de protection. Dans ce contexte, la Commission européenne a identifié le besoin urgent d’harmoniser les exigences en la matière, notamment en termes de performances de filtration et de confort associées au port du masque. Un guide de l’Afnor et un guide européen CEN ont alors été élaborés ; et, en lien avec les demandes des pouvoirs publics français formulées pendant le premier confinement, en 2020, le LNE a été mobilisé afin de répondre à la question centrale de l’efficacité des masques de protection apportant en la matière toute son expertise en métrologie des aérosols. Pour ce faire, une plateforme expérimentale a été développée en un temps record pour évaluer l’efficacité de filtration de différents types de masques de protection. Ce nouveau moyen d’essai permet, depuis le début de la crise, d’accompagner les pouvoirs publics, les industriels et les importateurs dans la qualification des masques FFP2, chirurgicaux, barrières et grand public. Dans cet article, nous présentons le banc expérimental développé par le LNE pour réaliser les mesures d’efficacité de filtration des masques barrières et grand public, ainsi que les comparaisons inter-laboratoires organisées dans ce cadre. En termes de perspectives, des axes d’amélioration du contexte normatif associé à chaque type de masques sont également présentés.
La Covid-19 et ses impacts psychologiques
Authors: Vancappel Alexis , Jansen Eline , El-Hage Wissam 
Published: October 2022

Dans cet article, nous abordons l’impact psychologique de la pandémie de Covid-19. Cette pandémie a en effet entraîné un bouleversement de nos modes de vie depuis le 11 mars 2020. Pour limiter la circulation du virus, tous les gouvernements ont pris diverses mesures de confinement avec, de facto , des conséquences individuelles, sociales, culturelles, économiques, environnementales… et psychologiques. Ces changements ont entraîné une perturbation de la santé mentale au sein de la population générale, et plus particulièrement auprès de certaines catégories de la population : les enfants, les adolescents, les étudiants, les professionnels de santé et les patients souffrant de troubles psychiatriques. Nous avons ainsi observé dans ces groupes de personnes une augmentation significative des symptômes anxieux, des symptômes thymiques et des idéations suicidaires.
La surveillance épidémiologique comme outil de la gouvernance des risques : le cas de la Covid-19
Authors: Hadna Saliha 
Published: October 2022

En France, depuis deux ans, les médias ne cessent de diffuser les chiffres des contaminations et des décès liés à la Covid-19, produisant un effet paradoxal en suscitant la crainte, tout en rendant ces drames singuliers (Pujol et al ., 2020). Une surveillance épidémiologique a été mise en place par Santé publique France (SPF), dès mars 2020. Les mesures gouvernementales qui se sont appuyées sur ces chiffres ont fait l’objet de nombreuses critiques (Mucchielli et al ., 2020), voire d’une défiance (Idelson, 2021). L’urgence a placé au second plan un problème majeur : l’évolution des maladies chroniques (Jornayvaz et Wojtusciszyn, 2021), notamment du cancer. Or, certains cancers, comme celui du pancréas, ont eu un taux d’incidence en hausse entre 2010 et 2018, le cancer restant la première cause de mortalité en France. Dans cet article, nous nous intéresserons d’abord au dispositif de surveillance épidémiologique de SPF. Nous analyserons ensuite la manière dont les experts ont été mobilisés lors de cette crise sanitaire. Enfin, nous montrerons que cette gestion de crise a été construite sur une approche court-termiste, dans la mesure où la déprogrammation des opérations jugées « non urgentes » pour donner la priorité aux soins Covid-19 par rapport aux soins liés au cancer n’a pas permis d’anticiper la prochaine vague de surmortalité par cancer pourtant annoncée par plusieurs études médicales.
Vivre le décès d’un proche en temps de pandémie
Authors: Verdon Chantal , Grenier Josée , Cherblanc Jacques , Simard Chantale , Bergeron-Leclerc Christiane , Maltais Danielle , Zech Emmanuelle , Cadell Susan 
Published: October 2022

La pandémie suscite de nombreux questionnements liés au phénomène du deuil, où les circonstances entourant le décès d’un proche sont une source de connaissances extrêmement importantes et inédites permettant de mieux saisir l’importance des événements entourant un tel malheur. Une étude québécoise s’est intéressée à l’expérience de personnes ayant perdu un proche pendant la pandémie. Trois thèmes émergent de cette étude qui s’appuie sur des données qualitatives : le temps laissé ; le sens donné à cette épreuve ; et l’attitude du personnel soignant. L’étude livre des témoignages sur ce qui peut influencer les trajectoires du mourir et du deuil. De ces circonstances chaotiques et imprévisibles, les personnes endeuillées peuvent quand même y donner un sens quand elles peuvent poser des actes concrets : faire leurs adieux ; voir une dernière fois le défunt ; procéder à des rituels significatifs et recevoir une attention empreinte d’humanisme.