bluuebunny/crossref_metadata_2025_split huggingface dataset:
SCOPE OF APPLICATION OF THE MULTIFUNCTIONAL TELEMETRY COMPLEX «SSOFT: SIGNAL»
Authors: Богданов Роман Александрович , Антоненков Дмитрий Александрович 
Published: July 2022

В данной статье описывается автоматическая выдача аварийно-предупредительной сигнализации о состоянии газопровода и возможных утечках газа владельцу эксплуатирующей организации.
This article describes the automatic issuance of an emergency warning alarm about the condition of the gas pipeline and possible gas leaks to the owner of the operating organization.
PHILOSOPHY OF SCIENCE: OSCILLATORY MOTION AS A FUNDAMENTAL PRINCIPLE OF THE MATERIAL WORLD
Authors: Карпин Владимир Александрович 
Published: July 2022

Движение является неотъемлемым свойством, атрибутом материального мира. При эволюционном развитии оно приобрело множество различных видов. Построение любой современной теоретической науки должно начинаться с выявления фундаментальных принципов различного уровня. Наиболее общим фундаментальным принципом движения всего материального мира является колебательный принцип.
Movement is an inherent property, an attribute of the material world. During its evolutionary development, it has acquired many different types. The construction of any modern theoretical science should begin with the identification of fundamental principles at various levels. The most general fundamental principle of the movement of the entire material world is the oscillatory principle.
Eye movements reveal the contributions of early and late processes of enhancement and suppression to the guidance of visual search
Authors: Hamblin-Frohman Zachary , Chang Seah , Egeth Howard , Becker Stefanie I. 
Published: July 2022

AbstractIn visual search attention can be directed towards items matching top-down goals, but this must compete with factors such as salience that can capture attention. However, under some circumstances it appears that attention can avoid known distractor features. Chang and Egeth (Psychological Science, 30 (12), 1724–1732, 2019) found that such inhibitory effects reflect a combination of distractor-feature suppression and target-feature enhancement. In the present study (N = 48), we extend these findings by revealing that suppression and enhancement effects guide overt attention. On search trials (75% of trials) participants searched for a diamond shape among several other shapes. On half of the search trials all objects were the same colour (e.g., green) and on the other half of the search trials one of the non-target shapes appeared in a different colour (e.g., red). On interleaved probe trials (25% of trials), subjects were presented with four ovals. One of the ovals was in either the colour of the target or the colour of the distractor from the search trials. The other three ovals were on neutral colours. Critically, we found that attention was overtly captured by target colours and avoided distractor colours when they were viewed in a background of neutral colours. In addition, we provided a time course of attentional control. Within visual search tasks we observed inhibition aiding early attentional effects, indexed by the time it took gaze to first reach the target, as well as later decision-making processes indexed by the time for a decision to be made once the target as found.
Positive hysteresis in emotion recognition: Face processing visual regions are involved in perceptual persistence, which mediates interactions between anterior insula and medial prefrontal cortex
Authors: Verdade Andreia , Sousa Teresa , Castelhano João , Castelo-Branco Miguel 
Published: July 2022

AbstractFacial emotion perception can be studied from the point of view of dynamic systems whose output may depend not only on current input but also on prior history — a phenomenon known as hysteresis. In cognitive neuroscience, hysteresis has been described as positive (perceptual persistence) or negative (fatigue of current percept) depending on whether perceptual switching occurs later or earlier than actual physical stimulus changes. However, its neural correlates remain elusive. We used dynamic transitions between emotional expressions and combined behavioral assessment with functional magnetic resonance imaging (fMRI) to investigate the underlying circuitry of perceptual hysteresis in facial emotion recognition. Our findings revealed the involvement of face-selective visual areas — fusiform face area (FFA) and superior temporal sulcus (STS) — in perceptual persistence as well as the right anterior insula. Moreover, functional connectivity analyses revealed an interplay between the right anterior insula and medial prefrontal cortex, which showed to be dependent on the presence of positive hysteresis. Our results support the hypothesis that high-order regions are involved in perceptual stabilization and decision during perceptual persistence (positive hysteresis) and add evidence to the role of the anterior insula as a hub of sensory information in perceptual decision-making.
Limits on the Auroral Generation of H3
+ in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph
Authors: Gibbs Aidan , Fitzgerald Michael P. 
Published: July 2022

Abstract
The molecular ion H3
+ is a potentially powerful tracer of the ionospheres and thermal structures of Jovian planets but has never been detected in a planetary mass object outside of the solar system. Models predict that H3
+ emission driven by EUV flux and solar wind on hot Jupiters, or by powerful aurorae on brown dwarfs, will be between 102 and 105 × more intense than that of Jupiter. If optimal conditions for the production of emission do exist, the emission may be detectable by current ground-based instruments or in the near future. We present the first search for H3
+ line emission in brown dwarfs with Keck Near Infrared Echelle Spectrograph L′ high-resolution spectroscopy. Additionally, we survey stars hosting giant planets at semimajor axes near 0.1–0.2 au, which models suggest may be the best planetary targets. No candidate H3
+ emission is found. The limits we place on the emission of H3
+ from brown dwarfs indicate that auroral generation of H3
+ in these environments likely does not linearly scale from the processes found on Jupiter, plausibly due to deeper atmospheric penetration by precipitating auroral electrons. Detection of H3
+ emission in brown dwarfs may be possible with the James Webb Space Telescope, or future 33 m class telescopes.
Radio Spectra of Luminous, Heavily Obscured WISE-NVSS Selected Quasars
Authors: Patil Pallavi , Whittle Mark , Nyland Kristina , Lonsdale Carol , Lacy Mark , Kimball Amy E , Lonsdale Colin , Peters Wendy , Clarke Tracy E. , Efstathiou Andreas , Giacintucci Simona , Kim Minjin , Lanz Lauranne , Mukherjee Dipanjan , Polisensky Emil 
Published: July 2022

Abstract
We present radio spectra spanning 0.1–10 GHz for the sample of heavily obscured luminous quasars with extremely red mid-infrared-optical colors and compact radio emission. The spectra are constructed from targeted 10 GHz observations and archival radio survey data that together yield 6–11 flux-density measurements for each object. Our primary result is that most (62%) of the sample have peaked or curved radio spectra and many (37%) could be classified as Gigahertz-Peaked Spectrum (GPS) sources. This indicates compact emission regions likely arising from recently triggered radio jets. Assuming synchrotron self-absorption (SSA) generates the peaks, we infer compact source sizes (3–100 pc) with strong magnetic fields (6–100 mG) and young ages (30–104 yr). Conversely, free-free absorption (FFA) could also create peaks due to the high column densities associated with the deeply embedded nature of the sample. However, we find no correlations between the existence or frequency of the peaks and any parameters of the MIR emission. The high-frequency spectral indices are steep (α ≈ −1) and correlate, weakly, with the ratio of MIR photon energy density to magnetic energy density, suggesting that the spectral steepening could arise from inverse Compton scattering off the intense MIR photon field. This study provides a foundation for combining multifrequency and mixed-resolution radio survey data for understanding the impact of young radio jets on the ISM and star-formation rates of their host galaxies. faGithub
An Old, Metal-rich Accreted Stellar Component in the Milky Way Stellar Disk
Authors: Feuillet Diane K. , Feltzing Sofia , Sahlholdt Christian , Bensby Thomas 
Published: July 2022

Abstract
We study the possibility that the Milky Ways’ cool stellar disk includes mergers with ancient stars. Galaxies are understood to form in a hierarchical manner, where smaller (proto-)galaxies merge into larger ones. Stars in galaxies, like the Milky Way, contain in their motions and elemental abundance tracers of past events and can be used to disentangle merger remnants from stars that formed in the main galaxy. The merger history of the Milky Way is generally understood to be particularly easy to study in the stellar halo. The advent of the ESA astrometric satellite Gaia has enabled the detection of completely new structures in the halo such as the Gaia-Enceladus-Sausage. However, simulations also show that mergers may be important for the build-up of the cool stellar disks. Combining elemental abundances for ∼100 giant branch stars from APOGEE DR17 and astrometric data from Gaia we use elemental abundance ratios to find a hitherto unknown, old stellar component in the cool stellar disk in the Milky Way. We further identify a small sample of RR Lyrae variables with disk kinematics that also show the same chemical signature as the accreted red giant stars in the disk. These stars allow us to date the stars in the accreted component. We find that they are exclusively old.
Spectral Variability of the Born-again Ejecta in A 58
Authors: Montoro-Molina Borja , A. Guerrero Martín , A. Toalá Jesús , Rodríguez-González Janis B. 
Published: July 2022

Abstract
Born-again planetary nebulae (PNs) allow investigating stellar evolution, dust production, and nebular shocks in human timescales. Here we present an analysis of multiepoch optical spectroscopic observations of the born-again PN A 58 around V605 Aql, which experienced a very late thermal pulse about a century ago. The H-deficient ejecta has experienced a considerable brightening in the time period considered, from 1996 to 2021, with notable changes also in many emission line ratios. Neither the reduction of the extinction caused by the dilution of the ejecta nor the increase of the ionizing photon flux from the central star seem capable to produce these spectral changes, which are instead attributed to shocks in the bipolar H-poor outflow, dissociating molecular material, and propagating through the outer nebula.
Search for Periodicities in High Energy AGNs with a Time Domain Approach
Authors: Rueda Héctor , Glicenstein Jean-François , Brun François 
Published: July 2022

Abstract
This paper investigates a new methodology to search for periods in light curves of high-energy gamma-ray sources such as active galactic nuclei (AGNs). High-energy light curves have significant stochastic components, making period detection somewhat challenging. In our model, periodic terms, drifts of the light curves, and random walk with a correlation between flux points due to colored noise are taken into account independently. The parameters of the model are obtained directly from a Markov Chain Monte Carlo minimization. The time periods found are compared to the output of the publicly available Agatha program. The search method is applied to high-energy periodic AGN candidates from the Fermi-LAT catalog. The significance of periodic models over pure noise models is discussed. Finally, the variability of the period and amplitude of oscillating terms is studied on the most significant candidates.
Statistical Analysis of H i Profile Asymmetry and Shape for Nearby Galaxies
Authors: Yu 余 Niankun 捻坤 , Ho Luis C. , Wang Jing , Li Hangyuan 
Published: July 2022

Abstract
We present a uniform analysis of the integrated profile of the H i emission line of 29,958 nearby (z < 0.06) galaxies extracted from the ALFALFA 21 cm survey. We apply the curve-of-growth technique to derive a database of spectral parameters and robust estimates of their associated uncertainties. Besides the central velocity and total flux, the main catalog provides new measures of line width, profile asymmetry, and profile shape. For a subsample of 13,511 galaxies with optical properties available from the Sloan Digital Sky Survey, we compute inclination angle-corrected line widths, rotation velocities empirically calibrated from spatially resolved observations, and dynamical masses based on H i sizes estimated from the H i mass. To facilitate subsequent scientific applications of the database, we also compile a number of ancillary physical properties of the galaxies, including their optical morphology, stellar mass, and various diagnostics of star formation activity. We use the homogeneous catalog of H i parameters to examine the statistical properties of profile asymmetry and shape. Across the full sample, which covers a wide range of stellar masses and environments, statistically significant H i profile asymmetry is detected in ∼20% of the galaxy population. The global H i profiles are 35.2% ± 0.3% single-peaked, 26.9% ± 0.3% flat-topped, and 37.9% ± 0.3% double-horned. At a given inclination angle, double-horned profiles are preferentially associated with galaxies of higher stellar mass or optical concentration, while galaxies of lower mass or concentration tend to have single-peaked profiles.
Water Masers as an Early Tracer of Star Formation
Authors: Ladeyschikov Dmitry A. , Gong Yan , Sobolev Andrey M. , Menten Karl M. , Urquhart James S. , Breen Shari L. , Shakhvorostova Nadezhda N. , Bayandina Olga S. , Tsivilev Alexander P. 
Published: July 2022

Abstract
We present a study of the correlation between 22 GHz water maser emission and far-infrared/submillimeter (IR/sub-mm) sources. The generalized linear model (GLM) is used to predict H2O maser detection in a particular source with defined physical parameters. We checked the GLM predictions by observing a sample of selected sources with the Effelsberg 100 m telescope. In total, 359 sources were observed. H2O masers were detected in 124 sources, with 56 new detections. We found 22 sources with a significant flux variability. Using the GLM analysis, we estimate that 2392 ± 339 star formation regions (SFRs) in the Galaxy may harbor H2O masers detectable by single-dish observations at the noise level of ∼0.05 Jy. Analyzing the luminosity-to-mass ratio (L/M) of the ATLASGAL and Hi-GAL clumps associated with different maser species, we find that 22 GHz water masers have significantly lower values of L/M in comparison to 6.7 GHz class II methanol and 1665 MHz OH masers. This implies that 22 GHz water masers may appear prior to 6.7 GHz methanol and OH masers in the evolutionary sequence of SFRs. From the analysis of physical offsets between host clumps and maser interferometric positions, we found no significant difference between the H2O and class II methanol maser offsets against the host clump position. We conclude that the tight association between water masers and IR/sub-mm sources may provide insight into the pumping conditions of these masers and the evolutionary stages of their onset.
Catalog of High-velocity Dispersion Compact Clouds in the Central Molecular Zone of Our Galaxy
Authors: Oka Tomoharu , Uruno Asaka , Enokiya Rei , Nakamura Taichi , Yamasaki Yuto , Watanabe Yuto , Tokuyama Sekito , Iwata Yuhei 
Published: July 2022

Abstract
This study developed an automated identification procedure for compact clouds with broad velocity widths in the spectral-line data cubes of highly crowded regions. The procedure was applied to the CO J = 3 − 2 line data, obtained using the James Clerk Maxwell Telescope, to identify 184 high-velocity dispersion compact clouds (HVDCCs), which are a category of peculiar molecular clouds found in the central molecular zone of our Galaxy. A list of HVDCCs in the area −1.°4 ≤ l ≤ +2.°0, −0.°25 ≤ b ≤ +0.°25 was presented with their physical parameters, CO J = 3 − 2/J = 1 − 0 intensity ratios, and morphological classifications. Consequently, the list provides several intriguing sources that may have been driven by encounters with pointlike massive objects, local energetic events, or cloud-to-cloud collisions.
Are There Larger Stellar Velocity Dispersions in Low-redshift Type 1 AGNs than in Type 2 AGNs?
Authors: Zhang XueGuang 
Published: July 2022

Abstract
The main objective of this article is to check the Unified Model (UM) for the expected similar stellar velocity dispersions between Type 1 and Type 2 active galactic nuclei (AGNs) and then to provide further clues on black hole (BH) mass properties. Unlike previous comparisons of BH masses estimated from M
BH–σ relations for Type 2 AGNs and from virial BH masses for Type 1 AGNs, reliable stellar velocity dispersions σ measured from absorption features around 4000 Å are directly compared between the thus far largest samples of 6260 low-redshift (z < 0.3) Type 1 AGNs and almost all Type 2 AGNs in SDSS DR12. Although half of Type 1 AGNs do not have a measured σ due to unapparent absorption features overwhelmed by AGN activities, both properties of the mean spectra of Type 1 AGNs with and without a measured σ and a positive dependence of σ on the [O iii] luminosity can lead to a statistically larger σ for all Type 1 AGNs compared to the 6260 Type 1 AGNs with measured stellar velocity dispersions. Then, direct σ comparisons can lead to a statistically larger σ in Type 1 AGNs, with a confidence level higher than 10σ, after considering the necessary effects of different redshifts and different central AGN activities. Although Type 1 AGNs have a σ of only about (9 ± 3)% larger than Type 2 AGNs, the difference cannot be well explained at the current stage. Unless there is strong evidence to support different M
BH–σ relations or to support quite different evolutionary histories between Type 1 and Type 2 AGNs, the statistically larger σ in Type 1 AGNs provides a strong challenge to the UM of AGNs.
Systematically Measuring Ultra-diffuse Galaxies (SMUDGes). III. The Southern SMUDGes Catalog
Authors: Zaritsky Dennis , Donnerstein Richard , Karunakaran Ananthan , Barbosa C. E. , Dey Arjun , Kadowaki Jennifer , Spekkens Kristine , Zhang 张 Huanian 华年 
Published: July 2022

Abstract
We present a catalog of 5598 ultra-diffuse galaxy (UDG) candidates with effective radius r

e
> 5.″3 distributed throughout the southern portion of the DESI Legacy Imaging Survey covering ∼15,000 deg2. The catalog is most complete for physically large (r

e
> 2.5 kpc) UDGs lying in the redshift range 1800 ≲ cz/km s−1 ≲ 7000, where the lower bound is defined by where incompleteness becomes significant for large objects on the sky and the upper bound by our minimum angular size selection criterion. Because physical size is integral to the definition of a UDG, we develop a method of distance estimation using existing redshift surveys. With three different galaxy samples, two of which contain UDGs with spectroscopic redshifts, we estimate that the method has a redshift accuracy of ∼75% when the method converges, although larger, more representative spectroscopic UDG samples are needed in order to fully understand the behavior of the method. We are able to estimate distances for 1079 of our UDG candidates (19%). Finally, to illustrate some uses of the catalog, we present both distance-independent and distance-dependent results. In the latter category, we establish that the red sequence of UDGs lies on the extrapolation of the red sequence relation for bright ellipticals and that the environment–color relation is at least qualitatively similar to that of high surface brightness galaxies. Both of these results challenge some of the models proposed for UDG evolution.
Magnetic Fields in Low-mass Stars Increase Photometric Masses, Thereby Reducing Inferred Radius Inflation
Authors: MacDonald J. , Mullan D. J. 
Published: July 2022

Abstract
Standard evolution models of a given age provide a relationship between stellar mass and T
eff. Based on this, Cruz et al. have derived stellar masses and radii for a sample of Kepler stars using photometry alone: their radii are found to be inflated by up to 100% relative to standard models. However, magnetic fields distort the M–T
eff relationship in a systematic way: here, we quantify this distortion, and show that radius inflations in the Cruz et al. stars are likely to be significantly smaller than 100%.
A strategy for successful integration of DNA-based methods in aquatic monitoring
Authors: Blancher Philippe , Lefrançois Estelle , Rimet Frédéric , Vasselon Valentin , Argillier Christine , Arle Jens , Beja Pedro , Boets Pieter , Boughaba Jeanne , Chauvin Christian , Deacon Michael , Duncan Willie , Ejdung Gunilla , Erba Stefania , Ferrari Benoit , Fischer Helmut , Hänfling Bernd , Haldin Michael , Hering Daniel , Hette-Tronquart Nicolas , Hiley Alice , Järvinen Marko , Jeannot Benjamin , Kahlert Maria , Kelly Martyn , Kleinteich Julia , Koyuncuoğlu Serdar , Krenek Sascha , Langhein-Winther Sidsel , Leese Florian , Mann David , Marcel Rémy , Marcheggiani Stefania , Meissner Kristian , Mergen Patricia , Monnier Olivier , Narendja Frank , Neu Diane , Onofre Pinto Veronica , Pawlowska Alina , Pawlowski Jan , Petersen Martin , Poikane Sandra , Pont Didier , Renevier Marie-Sophie , Sandoy Steinar , Svensson Jonas , Trobajo Rosa , Tünde Zagyva Andrea , Tziortzis Iakovos , van der Hoorn Berry , Vasquez Marlen Ines , Walsh Kerry , Weigand Alexander , Bouchez Agnès 
Published: July 2022

Recent advances in molecular biomonitoring open new horizons for aquatic ecosystem assessment. Rapid and cost-effective methods based on organismal DNA or environmental DNA (eDNA) now offer the opportunity to produce inventories of indicator taxa that can subsequently be used to assess biodiversity and ecological quality. However, the integration of these new DNA-based methods into current monitoring practices is not straightforward, and will require coordinated actions in the coming years at national and international levels.
To plan and stimulate such an integration, the European network DNAqua-Net (COST Action CA15219) brought together international experts from academia, as well as key environmental biomonitoring stakeholders from different European countries. Together, this transdisciplinary consortium developed a roadmap for implementing DNA-based methods with a focus on inland waters assessed by the EU Water Framework Directive (2000/60/EC). This was done through a series of online workshops held in April 2020, which included fifty participants, followed by extensive synthesis work.
The roadmap is organised around six objectives: 1) to highlight the effectiveness and benefits of DNA-based methods, 2) develop an adaptive approach for the implementation of new methods, 3) provide guidelines and standards for best practice, 4) engage stakeholders and ensure effective knowledge transfer, 5) support the environmental biomonitoring sector to achieve the required changes, 6) steer the process and harmonise efforts at the European level.
This paper provides an overview of the forum discussions and the common European views that have emerged from them, while reflecting the diversity of situations in different countries. It highlights important actions required for a successful implementation of DNA-based biomonitoring of aquatic ecosystems by 2030.