bluuebunny/crossref_metadata_2025_split huggingface dataset:
Evidence for Low Kick Velocities among High-mass X-Ray Binaries in the Small Magellanic Cloud from the Spatial Correlation Function
Authors: Bodaghee Arash , Antoniou Vallia , Zezas Andreas , Tomsick John A. , Jordan Zachary , Jackson Brenton , Agnew Ryan , Frechette Eric , Hornschemeier Ann E. , Rodriguez Jérôme 
Published: September 2021

Abstract
We present the two-point cross-correlation function between high-mass X-ray binaries (HMXBs) in the Small Magellanic Cloud (SMC) and their likely birthplaces (OB associations: OBAs). This function compares the spatial correlation between the observed HMXB and OBA populations against mock catalogs in which the members are distributed randomly across the sky. A significant correlation (∼15σ) is found for the HMXB and OBA populations when compared with a randomized catalog in which the OBAs are distributed uniformly over the SMC. A less significant correlation (4σ) is found for a randomized catalog of OBAs built with a bootstrap method. However, no significant correlation is detected when the randomized catalogs assume the form of a Gaussian ellipsoid or a distribution that reflects the star formation history from 40 Myr ago. Based on their observed distributions and assuming a range of migration timescales, we infer that the average value of the kick velocity inherited by an HMXB during the formation of its compact object is 2–34 km s−1. This is considerably less than the value obtained for their counterparts in the Milky Way hinting that the galactic environment affecting stellar evolution plays a role in setting the average kick velocity of HMXBs.
Flattening of Dark Matter Cusps during Mergers: Model of M31
Authors: Boldrini Pierre , Mohayaee Roya , Silk Joe 
Published: September 2021

Abstract
We run high-resolution fully GPU N-body simulations to demonstrate that the dark matter (DM) distribution in M31 is well fitted by a core-like profile. Rich observational data especially on the giant stellar stream provides stringent constraints on the initial conditions of our simulations. We demonstrate that the accretion of a satellite on a highly eccentric orbit heats up the central parts of M31, causes an outward migration of DM particles, flattens the central cusp over more than a decade in scale, and generates a new model-independent DM profile that is well fitted by a core. Our results imply that core-like central profiles could be a common feature of massive galaxies that have been initially cuspy but have accreted satellites on nearly radial orbits.
Nature of Electrostatic Fluctuations in the Terrestrial Magnetosheath
Authors: Perri Silvia , Perrone Denise , Roberts Owen , Settino Adriana , Yordanova Emilya , Sorriso-Valvo Luca , Veltri Pierluigi , Valentini Francesco 
Published: September 2021

Abstract
The high cadence plasma, electric, and magnetic field measurements by the Magnetospheric MultiScale spacecraft allow us to explore the near-Earth space plasma with an unprecedented time and spatial resolution, resolving electron-scale structures that naturally emerge from plasma complex dynamics. The formation of small-scale turbulent features is often associated to structured, non-Maxwellian particle velocity distribution functions that are not at thermodynamic equilibrium. Using measurements in the terrestrial magnetosheath, this study focuses on regions presenting bumps in the power spectral density of the parallel electric field at subproton scales. Correspondingly, it is found that the ion velocity distribution functions exhibit beam-like features at nearly the local ion thermal speed. Ion-cyclotron waves in the ion-scale range are frequently observed at the same locations. These observations, supported by numerical simulations, are consistent with the generation of ion-bulk waves that propagate at the ion thermal speed. This represents a new branch of efficient energy transfer at small scales, which may be relevant to weakly collisional astrophysical plasmas.
The Magellan-TESS Survey. I. Survey Description and Midsurvey Results*

†
Authors: Teske Johanna , Wang Sharon Xuesong , Wolfgang Angie , Gan Tianjun , Plotnykov Mykhaylo , Armstrong David J. , Butler R. Paul , Cale Bryson , Crane Jeffrey D. , Howard Ward , Jensen Eric L. N. , Law Nicholas , Shectman Stephen A. , Plavchan Peter , Valencia Diana , Vanderburg Andrew , Ricker George R. , Vanderspek Roland , Latham David W. , Seager Sara , Winn Joshua N. , Jenkins Jon M. , Adibekyan Vardan , Barrado David , Barros Susana C. C. , Benkhaldoun Zouhair , Brown David J. A. , Bryant Edward M. , Burt Jennifer , Caldwell Douglas A. , Charbonneau David , Cloutier Ryan , Collins Karen A. , Collins Kevin I. , Colon Knicole D. , Conti Dennis M. , Demangeon Olivier D. S. , Eastman Jason D. , Elmufti Mohammed , Feng Fabo , Flowers Erin , Guerrero Natalia M. , Hojjatpanah Saeed , Irwin Jonathan M. , Isopi Giovanni , Lillo-Box Jorge , Mallia Franco , Massey Bob , Mori Mayuko , Mullally Susan E. , Narita Norio , Nishiumi Taku , Osborn Ares , Paegert Martin , de Leon Jerome Pitogo , Quinn Samuel N. , Reefe Michael , Schwarz Richard P. , Shporer Avi , Soubkiou Abderahmane , Sousa Sérgio G. , Stockdale Chris , Strøm Paul A. , Tan Thiam-Guan , Tang Jiaxin , Tenenbaum Peter , Wheatley Peter J. , Wittrock Justin , Yahalomi Daniel A. , Zohrabi Farzaneh 
Published: September 2021

Abstract
Kepler revealed that roughly one-third of Sunlike stars host planets orbiting within 100 days and between the size of Earth and Neptune. How do these planets form, what are they made of, and do they represent a continuous population or multiple populations? To help address these questions, we began the Magellan-TESS Survey (MTS), which uses Magellan II/PFS to obtain radial velocity (RV) masses of 30 TESS-detected exoplanets and develops an analysis framework that connects observed planet distributions to underlying populations. In the past, small-planet RV measurements have been challenging to obtain due to host star faintness and low RV semiamplitudes and challenging to interpret due to the potential biases in target selection and observation planning decisions. The MTS attempts to minimize these biases by focusing on bright TESS targets and employing a quantitative selection function and observing strategy. In this paper, we (1) describe our motivation and survey strategy, (2) present our first catalog of planet density constraints for 27 TESS Objects of Interest (TOIs; 22 in our population analysis sample, 12 that are members of the same systems), and (3) employ a hierarchical Bayesian model to produce preliminary constraints on the mass–radius (M-R) relation. We find that the biases causing previous M-R relations to predict fairly high masses at 1 R
⊕ have been reduced. This work can inform more detailed studies of individual systems and offer a framework that can be applied to future RV surveys with the goal of population inferences.
Examinations of CO Completeness Based on Three Independent CO Surveys
Authors: Sun Yan , Yang Ji , Yan Qing-Zeng , Lin Zehao , Zhang Shaobo , Su Yang , Xu Ye , Chen Xuepeng , Wang Hongchi , Zhou Xin 
Published: September 2021

Abstract
We report the global properties recovered by an ongoing CO survey of the Milky Way Imaging Scroll Painting (MWISP) toward the Galactic outskirts. Our results are also compared to those extracted by a uniform decomposition method from the CfA 1.2 m CO survey and the FCRAO 14 m outer Galaxy survey (OGS). We find that more extended and unseen structures are present in the MWISP data. The total flux across the disk recovered by the MWISP survey is 1.6 times larger than those recovered by the CfA survey and OGS in the case of the same resolution. The discrepancies are scaling with distance. For example, in the outermost Outer Scutum–Centaurus arm, the flux ratios for MWISP to CfA and MWISP to OGS increase up to 43.8 and 7.4, respectively. Nonetheless, the census of molecular gas in our Galaxy is still far from complete by the MWISP, with flux completeness of <58%. The total mass ratios of the tabulated molecular clouds between different surveys are similar to the CO flux ratio. The application of these ratios to the total H2 mass of our Galaxy yields a correction factor of at least 1.4, meaning that the H2 mass of our Galaxy should be at least 40% more massive than previously determined. Including the completeness correction, an even more significant fraction of the matter should be contributed by baryonic matter. The mass spectrum in the outer Galactic plane is better described by a nontruncating power law with γ = −1.83 ± 0.05 and an upper mass of M
0 = (1.3 ± 0.5) × 106
M
☉.
Classifying Seyfert Galaxies with Deep Learning
Authors: Chen Yen Chen 
Published: September 2021

Abstract
The traditional classification for a subclass of the Seyfert galaxies is visual inspection or using a quantity defined as a flux ratio between the Balmer line and forbidden line. One algorithm of deep learning is the convolution neural network (CNN), which has shown successful classification results. We build a one-dimensional CNN model to distinguish Seyfert 1.9 spectra from Seyfert 2 galaxies. We find that our model can recognize Seyfert 1.9 and Seyfert 2 spectra with an accuracy of over 80% and pick out an additional Seyfert 1.9 sample that was missed by visual inspection. We use the new Seyfert 1.9 sample to improve the performance of our model and obtain a 91% precision of Seyfert 1.9. These results indicate that our model can pick out Seyfert 1.9 spectra among Seyfert 2 spectra. We decompose the Hα emission line of our Seyfert 1.9 galaxies by fitting two Gaussian components and derive the line width and flux. We find that the velocity distribution of the broad Hα component of the new Seyfert 1.9 sample has an extending tail toward the higher end, and the luminosity of the new Seyfert 1.9 sample is slightly weaker than the original Seyfert 1.9 sample. This result indicates that our model can pick out the sources that have a relatively weak broad Hα component. In addition, we check the distributions of the host galaxy morphology of our Seyfert 1.9 samples and find that the distribution of the host galaxy morphology is dominated by a large bulge galaxy. In the end, we present an online catalog of 1297 Seyfert 1.9 galaxies with measurements of the Hα emission line.
Structures and Properties of Known and Postulated Interstellar Cations
Authors: Tinacci Lorenzo , Pantaleone Stefano , Maranzana Andrea , Balucani Nadia , Ceccarelli Cecilia , Ugliengo Piero 
Published: September 2021

Abstract
Positive ions play a fundamental role in interstellar chemistry, especially in cold environments where chemistry is believed to be mainly ion driven. However, in contrast with neutral species, most of the cations present in the astrochemical reaction networks are not fully characterized in the astrochemical literature. To fill this gap, we have carried out new accurate quantum chemical calculations to identify the structures and energies of 262 cations with up to 14 atoms that are postulated to have a role in interstellar chemistry. Optimized structures and rotational constants were obtained at the M06-2X/cc-pVTZ level, while electric dipoles and total electronic energies were computed with CCSD(T)/aug-cc-pVTZ//M06-2X/cc-pVTZ single-point energy calculations. The present work complements the study by Woon & Herbst, who characterized the structure and energies of 200 neutral species also involved in interstellar chemistry. Taken together, the two data sets can be used to estimate whether a reaction, postulated in present astrochemical reaction networks, is feasible from a thermochemistry point of view and, consequently, to improve the reliability of the present networks used to simulate the interstellar chemistry. We provide an actual example of the potential use of the cations plus neutral data sets. It shows that two reactions, involving Si-bearing ions and present in the widely used reaction networks KIDA and UMIST, cannot occur in the cold interstellar medium because they are endothermic.
Sunspot Catalog (1921–1935) and Area Series (1886–1940) from the Stonyhurst College Observatory
Authors: Carrasco V. M. S. , Muñoz-Jaramillo A. , Nogales J. M. , Gallego M. C. , Vaquero J. M. 
Published: September 2021

Abstract
A sunspot observation program was started at the end of the 19th century at the Stonyhurst College Observatory (hereafter SCO) by Father Perry, director of the observatory at that time. A digitization of the daily sunspot area series recorded in this observatory from 1886 to 1940 (with a gap between 1889 and 1897) is provided in this work. This depicts one of the oldest sunspot area series available. A comparison of this series with contemporary area series made in other observatories shows that SCO generally recorded larger areas than those in some of the observatories of that time such as, for example, the Royal Greenwich Observatory (RGO). Furthermore, SCO published a sunspot group catalog for the period 1921–1935. We provide a machine-readable version of this catalog. We compared the SCO group number series with other sunspot data obtained from other observatories. In this case, for example, the RGO systematically recorded more groups than the SCO. We compared SCO and RGO area distribution functions obtaining the calibration constant between both data sets. We also obtained the butterfly diagram from the group latitudes recorded by SCO and compared the percentages of group types computed from the SCO catalog with those from Valencia Observatory (following the Cortie morphological classification of sunspot groups), identifying their similarities and differences.
Detection of Ionized Calcium in the Atmosphere of the Ultra-hot Jupiter WASP-76b
Authors: Deibert Emily K. , de Mooij Ernst J. W. , Jayawardhana Ray , Turner Jake D. , Ridden-Harper Andrew , Fossati Luca , Hood Callie E. , Fortney Jonathan J. , Flagg Laura , MacDonald Ryan , Allart Romain , Sing David K. 
Published: September 2021

Abstract
Recent observations of the ultra-hot Jupiter WASP-76b have revealed a diversity of atmospheric species. Here we present new high-resolution transit spectroscopy of WASP-76b with GRACES at the Gemini North Observatory, serving as a baseline for the Large and Long Program “Exploring the Diversity of Exoplanet Atmospheres at High Spectral Resolution” (Exoplanets with Gemini Spectroscopy, or ExoGemS for short). With a broad spectral range of 400–1050 nm, these observations allow us to search for a suite of atomic species. We recover absorption features due to neutral sodium (Na i), and report a new detection of the ionized calcium (Ca ii) triplet at ∼850 nm in the atmosphere of WASP-76b, complementing a previous detection of the Ca ii H and K lines. The triplet has line depths of 0.295% ± 0.034% at ∼849.2 nm, 0.574% ± 0.041% at ∼854.2 nm, and 0.454% ± 0.024% at ∼866.2 nm, corresponding to effective radii close to (but within) the planet’s Roche radius. These measured line depths are significantly larger than those predicted by model LTE and NLTE spectra obtained on the basis of a pressure–temperature profile computed assuming radiative equilibrium. The discrepancy suggests that the layers probed by our observations are either significantly hotter than predicted by radiative equilibrium and/or in a hydrodynamic state. Our results shed light on the exotic atmosphere of this ultra-hot world, and will inform future analyses from the ExoGemS survey.
The Widefield Arecibo Virgo Extragalactic Survey: Early Results on Known Dark Sources
Authors: Minchin Robert , Taylor Rhys , Deshev Boris 
Published: September 2021

Abstract
The Widefield Arecibo Virgo Extragalactic Survey (WAVES) was an ongoing H i survey of the Virgo Cluster with the Arecibo Observatory’s 305 m William E. Gordon Telescope at the time of its structural failure. The full 20 square degrees of the southern field and 10 of the planned 35 square degrees of the northern field had been observed to full depth, adding to 25 square degrees observed to the same depth in the cluster by the Arecibo Galaxy Environment Survey. We here review what WAVES reveals about four optically dark H i structures that were previously discovered in the survey area, including two that are not seen despite being well above our detection limit.
The Road to an Archival Data Format—Data Structures
Authors: Raugh Anne , Hughes J. Steven 
Published: September 2021

Abstract
The current data formatting and labeling standards for the Planetary Data System (PDS) are known as the PDS4 Standards. They supersede the PDS3 Standards, but they represent a complete redesign of the requirements and implementation, rather than even a major incremental revision, from the previous standard. At the heart of the PDS4 Standards lies a fundamental, philosophical change from the PDS3 paradigm: the PDS4 Standards clearly and specifically constrain the way that the bytes comprising observational data may be stored in their data files—that is, the data structures—to a much greater degree than the PDS3 Standards ever did, even in their most mature realization. In PDS4, the PDS has defined data structures optimized for the long-term preservation of observational data. We explore the history of the PDS and its standards through the examination of a single, simple data structure (the 2D image), to understand the evolutionary pressures on the data and on the PDS that led to the development of the archival data structure requirements for observational data at the core of the PDS4 standards.
Megafauna of the German exploration licence area for seafloor massive sulphides along the Central and South East Indian Ridge (Indian Ocean)
Authors: Gerdes Klaas , Kihara Terue , Martínez Arbizu Pedro , Kuhn Thomas , Schwarz-Schampera Ulrich , Mah Christopher , Norenburg Jon , Linley Thomas , Shalaeva Kate , Macpherson Enrique , Gordon Dennis , Stöhr Sabine , Messing Charles , Bober Simon , Guggolz Theresa , Christodoulou Magdalini , Gebruk Andrey , Kremenetskaia Antonina , Kroh Andreas , Sanamyan Karen , Bolstad Kathrin , Hoffman Leon , Gooday Andrew , Molodtsova Tina 
Published: September 2021

The growing interest in mineral resources of the deep sea, such as seafloor massive sulphide deposits, has led to an increasing number of exploration licences issued by the International Seabed Authority. In the Indian Ocean, four licence areas exist, resulting in an increasing number of new hydrothermal vent fields and the discovery of new species. Most studies focus on active venting areas including their ecology, but the non-vent megafauna of the Central Indian Ridge and South East Indian Ridge remains poorly known.
In the framework of the Indian Ocean Exploration project in the German license area for seafloor massive sulphides, baseline imagery and sampling surveys were conducted yearly during research expeditions from 2013 to 2018, using video sledges and Remotely Operated Vehicles.
This is the first report of an imagery collection of megafauna from the southern Central Indian- and South East Indian Ridge, reporting the taxonomic richness and their distribution. A total of 218 taxa were recorded and identified, based on imagery, with additional morphological and molecular confirmed identifications of 20 taxa from 89 sampled specimens. The compiled fauna catalogue is a synthesis of megafauna occurrences aiming at a consistent morphological identification of taxa and showing their regional distribution. The imagery data were collected during multiple research cruises in different exploration clusters of the German licence area, located 500 km north of the Rodriguez Triple Junction along the Central Indian Ridge and 500 km southeast of it along the Southeast Indian Ridge.
Four new species of Metapocyrtus Heller, 1912 (Coleoptera, Curculionidae, Entiminae, Pachyrhynchini) from Mindanao Island, Philippines
Authors: Cabras Analyn , Medina Milton Norman 
Published: September 2021

The genusMetapocyrtusHeller, 1912 is the most speciose and complex amongst the tribe Pachyrhynchini with seven subgenera and more than 200 described species. The genus is endemic to the Philippines and remains largely unknown particularly in the less explored areas or mountains.Four new species ofMetapocyrtusHeller, 1912 (Coleoptera, Curculionidae, Entiminae, Pachyrhynchini), are described from Mindanao Island, Philippines. Brief bionomical notes and mimicry with their sympatric beetles and other insect counterparts are also reported.
Acoustémologie et empreinte sonore. Faire avec et faire par les sons. Être avec et être par les sons
Authors: Baltazar Marie , Legrain Laurent 
Published: September 2021

Au xviiie siècle, un pasteur anglais déclame des vers de Virgile dans une vallée de sa paroisse et s’émerveille de la puissance de l’écho. En 2018, des chasseurs se réunissent sur le massif du Massacre dans le Jura pour se répartir des points d’écoute avant de s’en aller, seuls dans la nuit qui tombe, se baigner dans les sonorités du brame des cerfs. En 2014, un jeune homme gravit la montagne qui jouxte les quartiers les plus au sud d’Ulaanbaatar et se rend attentif à la sonorité délicate du frottement de tiges engoncées dans le givre printanier. Ces vignettes ethnographiques, très disparates, se font pourtant écho et cet article met l’accent sur cette correspondance : leur capacité à porter sur le devant de la scène descriptive une somme de petites opérations que subsume le verbe « écouter ». Dans le sillage de l’épistémologie acoustique et de l’attachement, les auteurs proposent de modéliser la notion d’« empreinte sonore » non pas en pensant l’empreinte comme la simple réactivation d’une sensibilité incorporée au préalable – bien qu’il soit difficile de nier totalement l’existence d’un tel processus – mais en ethnographiant tout le travail consenti pour « faire avec » et « être par » les sons.
Témoignage. Écrire, trouver-créer, penser. Un moment de respiration trans-formatrice
Authors: Bréant Françoise 
Published: September 2021

Venant de l’intérieur du récit, ma réflexion, à la fois clinique et critique, s’ancre dans l’analyse de l’expérience d’ateliers d’écriture proposés à des étudiants stagiaires en Licence Professionnelle de formateur et en formation des cadres de santé (I.F.C.S.). Il s’agit de montrer comment peuvent s’ouvrir des chemins d’imagination radicale singulière (Castoriadis, 1997) vers le plaisir de penser et vers l’autonomie réflexive du sujet. En prenant appui sur la notion de défonctionnalisation de l’objet (écrit), la réflexion porte sur la manière dont le processus de subjectivation se réalise dans l’écriture, en particulier lors des passages entre l’imaginaire nécessaire (illusion, rêve, fiction) et la fonction symbolique du langage (frustration, arrachement, deuil).L’atelier d’écriture, lieu de découverte, d’écoute, d’échange et de coopération, propice à l’accueil de l’incertitude et du doute, pourrait alors constituer un espace clinique de création (de soi, de la pensée, d’objets) dans lequel le travail du groupe peut mettre en œuvre ce que j’appellerais un imaginaire social transitionnel. Entre saveur et savoir (Barthes, 1977), ce travail de création, où la notion d’autorisation est centrale, prend du temps, mais ne serait-il pas l’essence même du processus de transformation ? Ne serait-il pas indispensable au développement d’une posture critique chez chaque sujet, lui permettant ainsi de subvertir la logique gestionnaire de rentabilité qui tend à s’imposer dans tous les secteurs des métiers de l’humain, et plus particulièrement en sciences de l’éducation ? Écrire, trouver-créer, penser, tel un mouvement pour ouvrir des brèches dans la clôture où la pensée tend toujours à s’enfermer à nouveau.