bluuebunny/crossref_metadata_2025_split huggingface dataset:
Insights into the Evolution of Five Isolated Galaxies
Authors: Mazzei P. , Rampazzo R. , Marino A. , Trinchieri G. , Uslenghi M. , Wolter A. 
Published: March 2022

Abstract
Galaxy evolution is believed to be conditioned by the environment. Isolated galaxies or galaxies in poor groups are an excellent laboratory to study evolutionary mechanisms where effects of the environment are minimal. We present new Swift-UVOT data in six filters, three in the ultraviolet (UV), of five isolated galaxies aiming at shedding light into their evolution. For all of our targets, we present new UV integrated fluxes, and for some of them also new UBV magnitudes. Our observations allow us to improve their multiwavelength spectral energy distributions, extending them over about three orders of magnitude in wavelength. We exploit our smooth particle hydrodynamical simulations with chemo-photometric implementation anchored, a posteriori, to the global multiwavelength properties of our targets, to give insight into their evolution. Then we compare their evolutionary properties with those previously derived for several galaxies in groups. The evolution of our targets is driven by a merger that occurred several gigayears ago, in the redshift range 0.5 ≤ z ≤ 4.5, not unlike what we have already found for galaxies in groups. The merger shapes the potential well where the gas is accreting, driving the star formation rate and the galaxy evolution. Isolated galaxies should not have suffered from interactions for at least 3 Gyr. However, the initial merger is still leaving its signature on the properties of our targets. Several rejuvenation episodes, triggered by in situ accretion, are highlighted. Moreover, jellyfish morphologies appear as these galaxies achieve their maximum star formation rate, before their quenching phase.
Detailed Chemical Abundances for a Benchmark Sample of M Dwarfs from the APOGEE Survey
Authors: Souto Diogo , Cunha Katia , Smith Verne V. , Prieto C. Allende , Covey Kevin , García-Hernández D. A. , Holtzman Jon A. , Jönsson Henrik , Mahadevan Suvrath , Majewski Steven R. , Masseron Thomas , Pinsonneault Marc , Schneider Donald P. , Shetrone Matthew , Stassun Keivan G. , Terrien Ryan , Zamora Olga , Stringfellow Guy S. , Lane Richard R. , Nitschelm Christian , Rojas-Ayala Bárbara 
Published: March 2022

Abstract
Individual chemical abundances for 14 elements (C, O, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, Fe, and Ni) are derived for a sample of M dwarfs using high-resolution, near-infrared H-band spectra from the Sloan Digital Sky Survey-IV/Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. The quantitative analysis included synthetic spectra computed with 1D LTE plane-parallel MARCS models using the APOGEE Data Release 17 line list to determine chemical abundances. The sample consists of 11 M dwarfs in binary systems with warmer FGK dwarf primaries and 10 measured interferometric angular diameters. To minimize atomic diffusion effects, [X/Fe] ratios are used to compare M dwarfs in binary systems and literature results for their warmer primary stars, indicating good agreement (<0.08 dex) for all studied elements. The mean abundance difference in primaries minus this work’s M dwarfs is −0.05 ± 0.03 dex. It indicates that M dwarfs in binary systems are a reliable way to calibrate empirical relationships. A comparison with abundance, effective temperature, and surface gravity results from the APOGEE Stellar Parameter and Chemical Abundances Pipeline (ASPCAP) Data Release 16 finds a systematic offset of [M/H], T
eff, log g = +0.21 dex, −50 K, and 0.30 dex, respectively, although ASPCAP [X/Fe] ratios are generally consistent with this study. The metallicities of the M dwarfs cover the range of [Fe/H] = −0.9 to +0.4 and are used to investigate Galactic chemical evolution via trends of [X/Fe] as a function of [Fe/H]. The behavior of the various elemental abundances [X/Fe] versus [Fe/H] agrees well with the corresponding trends derived from warmer FGK dwarfs, demonstrating that the APOGEE spectra can be used to examine Galactic chemical evolution using large samples of selected M dwarfs.
Chemical Properties of the Local Disk and Halo. II. Abundances of 3745 M Dwarfs and Subdwarfs from Improved Model Fitting of Low-resolution Spectra
Authors: Hejazi Neda , Lépine Sébastien , Nordlander Thomas 
Published: March 2022

Abstract
We present a model-fit pipeline to determine the stellar parameters of M-type dwarfs, which is an improvement on our previous work described in Hejazi et al. We apply this pipeline to analyze the low-resolution (R ∼ 2000) spectra of 3745 M dwarfs/subdwarfs, collected at the MDM Observatory, Lick Observatory, Kitt Peak National Observatory, and Cerro Tololo Inter-American Observatory. We examine the variation of the inferred parameter values in the H-R diagram constructed from their Gaia Early Data Release 3 (EDR3) parallaxes and optical magnitudes. We also study the distribution of our stars in the abundance diagram of [α/Fe] versus [M/H] and inspect the variation of their metallicity class, effective temperature, and surface gravity, as well as their Galactic velocity components U, V, and W, in this diagram. In addition, the analyses of the stars’ projected motions in the two-dimensional UV, VW, and UW planes, the variation of their chemical parameters in these planes, and their distribution in the abundance−velocity diagrams are important parts of this study. The precision of our model-fit pipeline is confirmed by the clear stratification of effective temperature and chemical parameters in the H-R diagram; the similarity of the stars’ distribution in the [α/Fe] versus [M/H] diagram and in the metallicity−velocity planes to those from other studies; the revealing of substructure in the abundance−velocity diagrams; and chemical homogeneity between the components of a set of binary systems.
Extending the SAGA Survey (xSAGA). I. Satellite Radial Profiles as a Function of Host-galaxy Properties
Authors: Wu John F. , Peek J. E. G. , Tollerud Erik J. , Mao Yao-Yuan , Nadler Ethan O. , Geha Marla , Wechsler Risa H. , Kallivayalil Nitya , Weiner Benjamin J. 
Published: March 2022

Abstract
We present “Extending the Satellites Around Galactic Analogs Survey” (xSAGA), a method for identifying low-z galaxies on the basis of optical imaging and results on the spatial distributions of xSAGA satellites around host galaxies. Using spectroscopic redshift catalogs from the SAGA Survey as a training data set, we have optimized a convolutional neural network (CNN) to identify z < 0.03 galaxies from more-distant objects using image cutouts from the DESI Legacy Imaging Surveys. From the sample of >100,000 CNN-selected low-z galaxies, we identify >20,000 probable satellites located between 36–300 projected kpc from NASA-Sloan Atlas central galaxies in the stellar-mass range

9.5
<
log
(

M

⋆

/

M

⊙

)
<
11

. We characterize the incompleteness and contamination for CNN-selected samples and apply corrections in order to estimate the true number of satellites as a function of projected radial distance from their hosts. Satellite richness depends strongly on host stellar mass, such that more-massive host galaxies have more satellites, and on host morphology, such that elliptical hosts have more satellites than disky hosts with comparable stellar masses. We also find a strong inverse correlation between satellite richness and the magnitude gap between a host and its brightest satellite. The normalized satellite radial distribution between 36–300 kpc does not depend on host stellar mass, morphology, or magnitude gap. The satellite abundances and radial distributions we measure are in reasonable agreement with predictions from hydrodynamic simulations. Our results deliver unprecedented statistical power for studying satellite galaxy populations and highlight the promise of using machine-learning for extending galaxy samples of wide-area surveys.
Lithium and Beryllium in NGC 752—an Open Cluster Twice the Age of the Hyades
Authors: Boesgaard Ann Merchant , Lum Michael G. , Chontos Ashley , Deliyannis Constantine P. 
Published: March 2022

Abstract
The surface abundances of the light elements lithium (Li) and beryllium (Be) reveal information about the physical processes taking place in stellar interiors. The investigation of the amount of these two elements in stars in open clusters shows the effect of age on those mechanisms. We have obtained spectra of both Li and Be in main-sequence stars in NGC 752 at high spectral resolution and high signal-to-noise ratios with HIRES on the Keck I telescope. In order to make meaningful comparisons with other clusters, we have determined the stellar parameters on a common scale. We have found abundances of Li and Be by spectral synthesis techniques. NGC 752 is twice the age of the well-studied Hyades. We find that (1) the Li dip centered near 6500 K is wider in NGC 752, having expanded toward cooler temperatures; (2) the Be dip is deeper in the older NGC 752; (3) the Li “peak” near 6200 K is lower by about 0.3 dex; (4) although there is little Be depletion in the cooler stars, it is possible that Be may be lower in NGC 752 than in the Hyades; and (5) the Li content in both clusters declines with decreasing temperature, but there is less Li in NGC 752 at a given temperature by ∼0.4 dex. These differences are consistent with the transport of the light-element nuclei below the surface convection zone as predicted by theory. That connection to rotational spin-down is indicated by the pattern of rotation with temperature in the two clusters.
Gamma-Ray Spectral Properties of the Galactic Globular Clusters: Constraint on the Number of Millisecond Pulsars
Authors: Wu Wei , Wang Zhongxiang , Xing Yi , Zhang Pengfei 
Published: March 2022

Abstract
We study the γ-ray spectra of 30 globular clusters (GCs) thus far detected with the Fermi Gamma-ray Space Telescope. Presuming that γ-ray emission of a GC comes from millisecond pulsars (MSPs) contained within the GC, a model that generates spectra for the GCs is built based on the γ-ray properties of the detected MSP sample. We fit the GCs’ spectra with the model, and for 27 of them, their emission can be explained as arising from MSPs. The spectra of the other three, NGC 7078, 2MS-GC01, and Terzan 1, cannot be fit with our model, indicating that MSPs’ emission should not be the dominant one in the first two and the third one has a unique hard spectrum. We also investigate six nearby GCs that have relatively high encounter rates compared to the comparison cases. The candidate spectrum of NGC 6656 can be fit with that of one MSP, supporting its possible association with the γ-ray source at its position. The five others do not have detectable γ-ray emission. Their spectral upper limits set limits of ≤1 MSPs in them, consistent with the numbers of radio MSPs found in them. The estimated numbers of MSPs in the γ-ray GCs generally match well those reported for radio pulsars. Our studies of the γ-ray GCs and the comparison nearby GCs indicate that the encounter rate should not be the only factor determining the number of γ-ray MSPs a GC contains.
DI Herculis Revisited: Starspots, Gravity Darkening, and 3D Obliquities
Authors: Liang Yan , Winn Joshua N. , Albrecht Simon H. 
Published: March 2022

Abstract
DI Herculis is an eclipsing binary famous for a longstanding disagreement between theory and observation of the apsidal precession rate, which was resolved when both stars were found to be severely misaligned with the orbit. We used data from the Transiting Exoplanet Survey Satellite (TESS) to refine our knowledge of the stellar obliquities and sharpen the comparison between the observed and theoretical precession rates. The TESS data show variations with a 1.07 day period, which we interpret as rotational modulation from starspots on the primary star. This interpretation is supported by the detection of photometric anomalies during primary eclipses consistent with starspot crossings. The secondary eclipse light curve shows a repeatable asymmetry that we interpret as an effect of gravity darkening. By combining the TESS data with previously obtained data, we determined the three-dimensional spin directions of both stars. Using this information, the updated value of the theoretical apsidal precession rate (including the effects of tides, rotation, and general relativity) is

1.35

−
0.50

+
0.58

arcsec cycle−1. The updated value of the observed rate (after including new TESS eclipse times) is

1.41

−
0.28

+
0.39

arcsec cycle−1. Given the agreement between the observed and theoretical values, we fitted all the relevant data simultaneously, assuming the theory is correct. This allowed us to place tighter constraints on the stellar obliquities, which are

75

−
3

+
3

and

80

−
3

+
3

degrees for the primary and secondary stars, respectively.
A Red-noise Eigenbasis for the Reconstruction of Blobby Images
Authors: Hallur Pravita , Medeiros Lia , Lauer Tod R. 
Published: March 2022

Abstract
We demonstrate the use of an eigenbasis that is derived from principal component analysis (PCA) applied on an ensemble of random-noise images that have a “red” power spectrum; i.e., a spectrum that decreases smoothly from large to small spatial scales. The pattern of the resulting eigenbasis allows for the reconstruction of images with a broad range of image morphologies. In particular, we show that this general eigenbasis can be used to efficiently reconstruct images that resemble possible astronomical sources for interferometric observations, even though the images in the original ensemble used to generate the PCA basis are significantly different from the astronomical images. We further show that the efficiency and fidelity of the image reconstructions depends only weakly on the particular parameters of the red-noise power spectrum used to generate the ensemble of images.
DeepZipper: A Novel Deep-learning Architecture for Lensed Supernovae Identification
Authors: Morgan R. , Nord B. , Bechtol K. , González S. J. , Buckley-Geer E. , Möller A. , Park J. W. , Kim A. G. , Birrer S. , Aguena M. , Annis J. , Bocquet S. , Brooks D. , Carnero Rosell A. , Carrasco Kind M. , Carretero J. , Cawthon R. , da Costa L. N. , Davis T. M. , De Vicente J. , Doel P. , Ferrero I. , Friedel D. , Frieman J. , García-Bellido J. , Gatti M. , Gaztanaga E. , Giannini G. , Gruen D. , Gruendl R. A. , Gutierrez G. , Hollowood D. L. , Honscheid K. , James D. J. , Kuehn K. , Kuropatkin N. , Maia M. A. G. , Miquel R. , Palmese A. , Paz-Chinchón F. , Pereira M. E. S. , Pieres A. , Plazas Malagón A. A. , Reil K. , Roodman A. , Sanchez E. , Smith M. , Suchyta E. , Swanson M. E. C. , Tarle G. , To C. 
Published: March 2022

Abstract
Large-scale astronomical surveys have the potential to capture data on large numbers of strongly gravitationally lensed supernovae (LSNe). To facilitate timely analysis and spectroscopic follow-up before the supernova fades, an LSN needs to be identified soon after it begins. To quickly identify LSNe in optical survey data sets, we designed ZipperNet, a multibranch deep neural network that combines convolutional layers (traditionally used for images) with long short-term memory layers (traditionally used for time series). We tested ZipperNet on the task of classifying objects from four categories—no lens, galaxy-galaxy lens, lensed Type-Ia supernova, lensed core-collapse supernova—within high-fidelity simulations of three cosmic survey data sets: the Dark Energy Survey, Rubin Observatory’s Legacy Survey of Space and Time (LSST), and a Dark Energy Spectroscopic Instrument (DESI) imaging survey. Among our results, we find that for the LSST-like data set, ZipperNet classifies LSNe with a receiver operating characteristic area under the curve of 0.97, predicts the spectroscopic type of the lensed supernovae with 79% accuracy, and demonstrates similarly high performance for LSNe 1–2 epochs after first detection. We anticipate that a model like ZipperNet, which simultaneously incorporates spatial and temporal information, can play a significant role in the rapid identification of lensed transient systems in cosmic survey experiments.
The FloRes Database: A floral resources trait database for pollinator habitat-assessment generated by a multistep workflow
Authors: Baden-Böhm Franziska , App Mario , Thiele Jan 
Published: March 2022

The decline of pollinating insects in agricultural landscapes proceeds due to intensive land use and the associated loss of habitat and food sources. Those insects depend on the spatial and temporal distribution of nectar and pollen as food resource. Hence, for nature conservation the spatio-temporal assessment of food quantity of habitats is necessary. Therefore, sufficient data of floral plant traits are required.
We present a raw database with the plant traits 1. flowering period, 2. floral-unit density, 3. nectar (nectar volume or sugar content of floral unit), 4. sugar concentration in nectar, 5. pollen mass or volume per floral unit, 6. protein content of pollen and 7. corolla depth. All traits are sampled from literature and online databases. The raw database consists of 843 unspecified (sp.) and specified plant species belong to 488 genera and 102 families with missing information. For utilizing the raw data, we developed a stepwise workflow unifying traits to comparable entities with identical units and aggregating them to an application database, called the FloRes Database (Floral Resources Database). FloRes contains the complete information of traits for 38 taxa and, when corolla depth is excluded, for 70 taxa. The stepwise workflow is implemented in five consecutive scripts written in R, that allow other users easily add information to the raw data and to compute their own application data set. FloRes can be used to evaluate food-resource supply of habitats for pollinators, e.g., to compare seed mixtures of agri-environmental measure, such as flower strips, taking into account flower phenology on a daily basis. Further, calculated for-resource supply can be used as input for simulation models of pollinator populations, such as the agent-based models BumbleBEEHAVE and SyrFitSources.
L’art à l’ère de la globalisation
Authors: Belting Hans 
Published: March 2022

Ce texte est extrait d’un ouvrage coédité par l’historien allemand Hans Belting, consacré à la nouvelle géographie de l’art contemporain dans un contexte globalisé. L’auteur dresse un panorama de l’évolution de l’art et de l’histoire de l’art depuis 1989, année marquée par de grands événements historiques et par les premières expositions globales et inclusives. Belting analyse le passage de l’art « mondial » (dans lequel l’Autre est exclu de l’art occidental et du modernisme) à l’art « global » (postcolonial, polyphonique et multiculturel). En mettant en cause les notions de centre et de périphérie, il met en lumière comment cette évolution, tout comme l’impact des changements géopolitiques, ont eu des conséquences sur l’écriture de l’histoire de l’art.
L’art à l’ère de la globalisation
Authors: Soh Bejeng Ndikung Bonaventure 
Published: March 2022

Le commissaire d’exposition d’origine camerounaise et directeur de la Haus der Kulturen der Welt [Maison des cultures du monde] de Berlin, Bonaventure Soh Bejeng Ndikung, examine dans ce texte l’évolution des musées à l’aune du phénomène de la globalisation. Si celui-ci a d’abord généré une tentative de diversification des institutions muséales (à partir des perspectives du genre, de l’origine ethnique, sociale ou géographique), elle est restée symbolique et sans conséquence majeure. C’est pourquoi l’auteur propose une méthode « décanonisante » qui consiste à élargir les canons esthétiques, supposés universels, en rassemblant au sein du musée des communautés et des géographies plurielles. La première étape de cette entreprise sera de démanteler les structures hiérarchiques qui produisent ces canons.
L’art à l’ère de la globalisation
Authors: Weibel Peter 
Published: March 2022

Ce texte de l’historien de l’art autrichien d’origine hongroise Peter Weibel propose des pistes de réflexion sur les conséquences de la globalisation dans le champ de l’art contemporain. En pensant en termes d’intégration et d’assimilation, deux caractéristiques du système social à l’origine de la modernité, Weibel montre comment le mécanisme d’inclusion et d’exclusion se poursuit au cœur de la globalisation, qui apparaît dès lors comme le produit de la modernité occidentale. Il fait également le constat d’un double tournant : celui initié par la photographie, le film et la vidéo dans le phénomène de globalisation, et le « tournant performatif », avec la participation du public à l’œuvre d’art.
L’art à l’ère de la globalisation
Authors: Enwezor Okwui 
Published: March 2022

Issu du texte inaugural de la documenta 11 (2002), cet essai marque un tournant dans la conception de l’art global. Le commissaire d’exposition d’origine nigériane Okwui Enwezor souligne le rôle du postcolonialisme dans l’émergence de la globalisation – qu’il définit en termes spatio-temporels. Par la transformation de « l’autre » en quelqu’un de visible et présent partout et tout le temps, le postcolonialisme permet, en effet, un dépassement des frontières du monde colonial. Dans le premier chapitre, Enwezor montre comment la globalisation et les nouvelles écritures postcoloniales de l’histoire remettent en cause la notion d’avant-garde. Dans le second chapitre, il met en évidence la façon dont les années 2000, signent, d’un point de vue éthique et politique, l’avènement d’un nouvel ordre de société globale, dans lequel, au-delà du colonialisme, la marge émerge violemment au centre, à l’image de Ground Zero.
L’art à l’ère de la globalisation
Authors: Brown Rebecca M. 
Published: March 2022

Ce texte est une réponse à l’essai de Partha Mitter, qui défendait au milieu des années 2000 une histoire de l’art plus inclusive et proposait d’élargir la définition du modernisme communément admise. L’historienne de l’art Rebecca M. Brown conteste cette perspective et montre que l’intégration de régions périphériques dans les conceptions modernistes relègue les artistes non occidentaux à des modernités distantes ou dérivées. L’auteure plaide pour une réévaluation radicale de l’art moderne et propose un démantèlement de ses fondements spatio-temporels. Elle reprend ainsi à son compte la question de la provincialisation de l’Europe posée par Dipesh Chakrabarty dans Provincialiser l’Europe. La pensée postcoloniale et la différence historique (2000).
Les priorités de la présidence française du Comité des Ministres du Conseil de l’Europe (17 mai – 27 novembre 2019)
Authors: Mattéi Jean-Baptiste 
Published: March 2022

Du 17 mai au 27 novembre 2019, la France assure la présidence du Comité des Ministres du Conseil de l’Europe. Afin de préserver le caractère paneuropéen de l’organisation au bénéfice des 830 millions d’Européens, la France a soutenu le retour de la délégation russe à l’Assemblée parlementaire. Elle met en avant trois priorités : préserver et consolider le système européen de protection des droits de l’homme ; promouvoir l’égalité et le vivre ensemble ; répondre aux nouveaux défis en matière de droits de l’homme et d’État de droit.
« Répondre et rassurer » : quelques enseignements à propos du premier avis consultatif de la Cour européenne des droits de l’homme
Authors: Szymczak David 
Published: March 2022

Rendu le 10 avril 2019, le premier avis consultatif de la Cour européenne des droits de l’homme est riche d’enseignements. D’une part, et en première lecture, concernant la réponse apportée à la juridiction interne qui avait sollicité l’avis. D’autre part, et plus largement, s’agissant de la façon dont la Cour de Strasbourg paraît envisager la nouvelle compétence consultative prévue par le Protocole n o 16. En ce sens, il semble possible d’avancer que, par son premier avis, la Cour européenne cherche à la fois à « répondre » et à « rassurer ».