bluuebunny/crossref_metadata_2025_split huggingface dataset:
Powerful ionized gas outflows in the interacting radio galaxy 4C+29.30
Authors: Couto Guilherme S , Storchi-Bergmann Thaisa , Siemiginowska Aneta , Riffel Rogemar A , Morganti Raffaella 
Published: August 2020

ABSTRACT
We investigate the ionized gas excitation and kinematics in the inner $4.3\, \times \, 6.2$ kpc2 of the merger radio galaxy 4C+29.30. Using optical integral field spectroscopy with the Gemini North Telescope, we present flux distributions, line-ratio maps, peak velocities and velocity dispersion maps as well as channel maps with a spatial resolution of $\approx\! 955\,$ pc. We observe high blueshifts of up to $\sim\! -650\,$$\rm km\, s^{-1}$ in a region ∼1 arcsec south of the nucleus (the southern knot – SK), which also presents high velocity dispersions ($\sim\! 250\,$$\rm km\, s^{-1}$), which we attribute to an outflow. A possible redshifted counterpart is observed north from the nucleus (the northern knot – NK). We propose that these regions correspond to a bipolar outflow possibly due to the interaction of the radio jet with the ambient gas. We estimate a total ionized gas mass outflow rate of $\dot{M}_{\mathrm{ out}} = 25.4 ^{+11.5 }_{ -7.5}\,$ M⊙ yr−1with a kinetic power of $\dot{E} = 8.1 ^{+10.7 }_{ -4.0} \times 10^{42}\,$ erg s−1, which represents $5.8 ^{+7.6 }_{ -2.9} {{\ \rm per\ cent}}$ of the active galactic nucleus (AGN) bolometric luminosity. These values are higher than usually observed in nearby active galaxies with the same bolometric luminosities and could imply a significant impact of the outflows in the evolution of the host galaxy. The excitation is higher in the NK – that correlates with extended X-ray emission, indicating the presence of hotter gas – than in the SK, supporting a scenario in which an obscuring dust lane is blocking part of the AGN radiation to reach the southern region of the galaxy.
Exploring universality in neutron star mergers
Authors: Chakravarti Kabir , Andersson Nils 
Published: August 2020

ABSTRACT
We explore the correlation between the pre-merger tidal deformability and the post-merger remnant oscillations seen in numerical simulations of neutron star binaries, with the aim of understanding to what extent the physics support the existence of such a relation. We consider the impact of thermal and rotational effects and argue that the proposed relation does, indeed, make sense and provide simple arguments that help explain the result.
Solution to the debris disc mass problem: planetesimals are born small?
Authors: Krivov Alexander V , Wyatt Mark C 
Published: August 2020

ABSTRACTDebris belts on the periphery of planetary systems, encompassing the region occupied by planetary orbits, are massive analogues of the Solar system’s Kuiper belt. They are detected by thermal emission of dust released in collisions amongst directly unobservable larger bodies that carry most of the debris disc mass. We estimate the total mass of the discs by extrapolating up the mass of emitting dust with the help of collisional cascade models. The resulting mass of bright debris discs appears to be unrealistically large, exceeding the mass of solids available in the systems at the preceding protoplanetary stage. We discuss this ‘mass problem’ in detail and investigate possible solutions to it. These include uncertainties in the dust opacity and planetesimal strength, variation of the bulk density with size, steepening of the size distribution by damping processes, the role of the unknown ‘collisional age’ of the discs, and dust production in recent giant impacts. While we cannot rule out the possibility that a combination of these might help, we argue that the easiest solution would be to assume that planetesimals in systems with bright debris discs were ‘born small’, with sizes in the kilometre range, especially at large distances from the stars. This conclusion would necessitate revisions to the existing planetesimal formation models, and may have a range of implications for planet formation. We also discuss potential tests to constrain the largest planetesimal sizes and debris disc masses.
Validating N-body code chrono for granular DEM simulations in reduced-gravity environments
Authors: Sunday Cecily , Murdoch Naomi , Tardivel Simon , Schwartz Stephen R , Michel Patrick 
Published: August 2020

ABSTRACT
The Discrete Element Method (DEM) is frequently used to model complex granular systems and to augment the knowledge that we obtain through theory, experimentation, and real-world observations. Numerical simulations are a particularly powerful tool for studying the regolith-covered surfaces of asteroids, comets, and small moons, where reduced-gravity environments produce ill-defined flow behaviours. In this work, we present a method for validating soft-sphere DEM codes for both terrestrial and small-body granular environments. The open-source code chrono is modified and evaluated first with a series of simple two-body-collision tests, and then, with a set of piling and tumbler tests. In the piling tests, we vary the coefficient of rolling friction to calibrate the simulations against experiments with 1 mm glass beads. Then, we use the friction coefficient to model the flow of 1 mm glass beads in a rotating drum, using a drum configuration from a previous experimental study. We measure the dynamic angle of repose, the flowing layer thickness, and the flowing layer velocity for tests with different particle sizes, contact force models, coefficients of rolling friction, cohesion levels, drum rotation speeds, and gravity levels. The tests show that the same flow patterns can be observed at the Earth and reduced-gravity levels if the drum rotation speed and the gravity level are set according to the dimensionless parameter known as the Froude number. chrono is successfully validated against known flow behaviours at different gravity and cohesion levels, and will be used to study small-body regolith dynamics in future works.
The dynamical state of Abell 2399: a bullet-like cluster
Authors: Lourenço Ana C C , Lopes P A A , Laganá T F , Nascimento R S , Machado R E G , Moura M T , Jaffé Y L , Ribeiro A L , Vulcani B , Moretti A , Riguccini L A 
Published: August 2020

ABSTRACT
While there are many ways to identify substructures in galaxy clusters using different wavelengths, each technique has its own caveat. In this paper, we conduct a detailed substructure search and dynamical state characterization of Abell 2399, a galaxy cluster in the local Universe (z ∼ 0.0579), by performing a multiwavelength analysis and testing the results through hydrodynamical simulations. In particular, we apply a Gaussian mixture model to the spectroscopic data from SDSS, WINGS, and OmegaWINGS Surveys to identify substructures. We further use public XMM–Newton data to investigate the intracluster medium (ICM) thermal properties, creating temperature, metallicity, entropy, and pressure maps. Finally, we run hydrodynamical simulations to constrain the merger stage of this system. The ICM is very asymmetrical and has regions of temperature and pressure enhancement that evidence a recent merging process. The optical substructure analysis retrieves the two main X-ray concentrations. The temperature, entropy, and pressure are smaller in the secondary clump than in the main clump. On the other hand, its metallicity is considerably higher. This result can be explained by the scenario found by the hydrodynamical simulations where the secondary clump passed very near to the centre of the main cluster possibly causing the galaxies of that region to release more metals through the increase of ram-pressure stripping.
Are the spiral arms in the MWC 758 protoplanetary disc driven by a companion inside the cavity?
Authors: Calcino Josh , Christiaens Valentin , Price Daniel J , Pinte Christophe , Davis Tamara M , van der Marel Nienke , Cuello Nicolás 
Published: August 2020

ABSTRACT
Spiral arms in protoplanetary discs are thought to be linked to the presence of companions. We test the hypothesis that the double spiral arm morphology observed in the transition disc MWC 758 can be generated by an ≈10MJup companion on an eccentric orbit internal to the spiral arms. Previous studies on MWC 758 have assumed an external companion. We compare simulated observations from three-dimensional hydrodynamics simulations of disc–companion interaction to scattered light, infrared and CO molecular line observations, taking into account observational biases. The inner companion hypothesis is found to explain the double spiral arms, as well as several additional features seen in MWC 758 – the arc in the north-west, substructures inside the spiral arms, the cavity in CO isotopologues, and the twist in the kinematics. Testable predictions include detection of fainter spiral structure, detection of a point source south-southeast of the primary, and proper motion of the spiral arms.
AGN and star formation properties of inside–out assembled galaxy candidates at z &lt; 0.1
Authors: Zewdie Dejene , Pović Mirjana , Aravena Manuel , Assef Roberto J , Gaulle Asrate 
Published: August 2020

ABSTRACT
We study a sample of 48 127 galaxies selected from the SDSS MPA-JHU catalogue, with log M⋆/M⊙ = 10.73−11.03 and z &lt; 0.1. Local galaxies in this stellar mass range have been shown to have systematically shorter assembly times within their inner regions (&lt;0.5 R50) when compared to that of the galaxy as a whole, contrary to lower or higher mass galaxies that show consistent assembly times at all radii. Hence, we refer to these galaxies as Inside-Out Assembled Galaxy (IOAG) candidates. We find that the majority of IOAG candidates with well-detected emission lines are classified as either active galactic nucleus (AGN; 40 per cent) or composite (40 per cent) in the BPT (Baldwin, Phillips & Terlevich) diagram. We also find that the majority of our sources are located below the main sequence of star formation, and within the green valley or red sequence. Most BPT-classified star-forming IOAG candidates have spiral morphologies and are in the main sequence, whereas Seyfert 2 and composites have mostly spiral morphologies but quiescent star formation rates (SFRs). We argue that a high fraction of IOAG candidates seem to be in the process of quenching, moving from the blue cloud to the red sequence. Those classified as AGN have systematically lower SFRs than star-forming galaxies, suggesting that AGN activity may be related to this quenching. However, the spiral morphology of these galaxies remains in place, suggesting that the central star formation is suppressed before the morphological transformation occurs.
What does FRB light-curve variability tell us about the emission mechanism?
Authors: Beniamini Paz , Kumar Pawan 
Published: August 2020

ABSTRACT
A few fast radio bursts’ (FRBs) light curves have exhibited large intrinsic modulations of their flux on extremely short ($t_{\rm r}\sim 10\, \mu$s) time-scales, compared to pulse durations (tFRB ∼ 1 ms). Light-curve variability time-scales, the small ratio of rise time of the flux to pulse duration, and the spectro-temporal correlations in the data constrain the compactness of the source and the mechanism responsible for the powerful radio emission. The constraints are strongest when radiation is produced far (≳1010 cm) from the compact object. We describe different physical set-ups that can account for the observed tr/tFRB ≪ 1 despite having large emission radii. The result is either a significant reduction in the radio production efficiency or distinct light-curve features that could be searched for in observed data. For the same class of models, we also show that due to high-latitude emission, if a flux f1(ν1) is observed at t1 then at a lower frequency ν2 &lt; ν1 the flux should be at least (ν2/ν1)2f1 at a slightly later time (t2 = t1ν1/ν2) independent of the duration and spectrum of the emission in the comoving frame. These features can be tested, once light-curve modulations due to scintillation are accounted for. We provide the time-scales and coherence bandwidths of the latter for a range of possibilities regarding the physical screens and the scintillation regime. Finally, if future highly resolved FRB light curves are shown to have intrinsic variability extending down to ${\sim}\mu$s time-scales, this will provide strong evidence in favour of magnetospheric models.
Proto-neutron stars with heavy baryons and universal relations
Authors: Raduta Adriana R , Oertel Micaela , Sedrakian Armen 
Published: August 2020

ABSTRACT
We use covariant density functional theory to obtain the equation of state (EoS) of matter in compact stars at non-zero temperature, including the full baryon octet as well as the Δ(1232) resonance states. Global properties of hot Δ-admixed hypernuclear stars are computed for fixed values of entropy per baryon (S/A) and lepton fraction (YL). Universal relations between the moment of inertia, quadrupole moment, tidal deformability, and compactness of compact stars are established for fixed values of S/A and YL that are analogous to those known for cold catalyzed compact stars. We also verify that the I–Love–Q relations hold at finite temperature for constant values of S/A and YL.
A catalogue of Locus Algorithm pointings for optimal differential photometry for 23 779 quasars
Authors: Creaner Oisín , Nolan Kevin , Smith Niall , Grennan David , Hickey Eugene 
Published: August 2020

ABSTRACT
This paper presents a catalogue of optimized pointings for differential photometry of 23 779 quasars extracted from the Sloan Digital Sky Survey (SDSS) Catalogue and a Score for each indicating the quality of the Field of View (FoV) associated with that pointing. Observation of millimagnitude variability on a time-scale of minutes typically requires differential observations with reference to an ensemble of reference stars. For optimal performance, these reference stars should have similar colour and magnitude to the target quasar. In addition, the greatest quantity and quality of suitable reference stars may be found by using a telescope pointing which offsets the target object from the centre of the FoV. By comparing each quasar with the stars which appear close to it on the sky in the SDSS Catalogue, an optimum pointing can be calculated, and a figure of merit, referred to as the ‘Score’ is calculated for that pointing. Highly flexible software has been developed to enable this process to be automated and implemented in a distributed computing paradigm, which enables the creation of catalogues of pointings given a set of input targets. Applying this technique to a sample of 40 000 targets from the fourth SDSS quasar catalogue resulted in the production of pointings and Scores for 23 779 quasars based on their magnitudes in the SDSS r-band. This catalogue is a useful resource for observers planning differential photometry studies and surveys of quasars to select those which have many suitable celestial neighbours for differential photometry.
Unravelling the complex magnetosphere of the B star HD 133880 via wideband observation of coherent radio emission
Authors: Das Barnali , Chandra Poonam , Wade Gregg A 
Published: August 2020

ABSTRACT
HD 133880 is one of the six hot magnetic stars known to produce coherent pulsed radio emission by the process of electron cyclotron maser emission (ECME). In this paper, we present observations of ECME from this star over a wide frequency range, covering nearly 300–4000 MHz with the Giant Metrewave Radio Telescope (GMRT) and the Karl G. Jansky Very Large Array (VLA). This study, which is the first of its kind, has led to the discovery of several interesting characteristics of the phenomenon and also of the host star. We find that the observable properties of ECME pulses, e.g. the time lag between right and left circularly polarized pulses, the amplitudes of the pulses, and their upper cut-off frequencies, appear to be dependent on the stellar orientation with respect to the line of sight. We suggest that all these phenomena, which are beyond the ideal picture, can be attributed to a highly azimuthally asymmetric matter distribution in the magnetosphere about the magnetic field axis, which is a consequence of both the high obliquity (the angle between rotation axis and the magnetic field axis) of the star and the deviation of the stellar magnetic field from a dipolar topology.
Heavy-metal Jupiters by major mergers: metallicity versus mass for giant planets
Authors: Ginzburg Sivan , Chiang Eugene 
Published: August 2020

ABSTRACT
Some Jupiter-mass exoplanets contain ${\sim}100\, {\rm M}_{\hbox{$\oplus $}}$ of metals, well above the ${\sim}10\, {\rm M}_{\hbox{$\oplus $}}$ typically needed in a solid core to trigger giant planet formation by runaway gas accretion. We demonstrate that such ‘heavy-metal Jupiters’ can result from planetary mergers near ∼10 au. Multiple cores accreting gas at runaway rates gravitationally perturb one another on to crossing orbits such that the average merger rate equals the gas accretion rate. Concurrent mergers and gas accretion implies the core mass scales with the total planet mass as Mcore ∝ M1/5 – heavier planets harbour heavier cores, in agreement with the observed relation between total mass and metal mass. While the average gas giant merges about once to double its core, others may merge multiple times, as merger trees grow chaotically. We show that the dispersion of outcomes inherent in mergers can reproduce the large scatter in observed planet metallicities, assuming $3{-}30\, {\rm M}_{\hbox{$\oplus $}}$ pre-runaway cores. Mergers potentially correlate metallicity, eccentricity, and spin.
CBTRUS Statistical Report: Primary Brain and Other Central Nervous System Tumors Diagnosed in the United States in 2013–2017
Authors: Ostrom Quinn T , Patil Nirav , Cioffi Gino , Waite Kristin , Kruchko Carol , Barnholtz-Sloan Jill S 
Published: August 2020

Abstract
The Central Brain Tumor Registry of the United States (CBTRUS), in collaboration with the Centers for Disease Control (CDC) and National Cancer Institute (NCI), is the largest population-based registry focused exclusively on primary brain and other central nervous system (CNS) tumors in the United States (US) and represents the entire US population. This report contains the most up-to-date population-based data on primary brain tumors (malignant and non-malignant) and supersedes all previous CBTRUS reports in terms of completeness and accuracy. All rates (incidence and mortality) are age-adjusted using the 2000 US standard population and presented per 100,000 population. The average annual age-adjusted incidence rate (AAAIR) of all malignant and non-malignant brain and other CNS tumors was 23.79 (Malignant AAAIR=7.08, non-Malignant AAAIR=16.71). This rate was higher in females compared to males (26.31 versus 21.09), Blacks compared to Whites (23.88 versus 23.83), and non-Hispanics compared to Hispanics (24.23 versus 21.48). The most commonly occurring malignant brain and other CNS tumor was glioblastoma (14.5% of all tumors), and the most common non-malignant tumor was meningioma (38.3% of all tumors). Glioblastoma was more common in males, and meningioma was more common in females. In children and adolescents (age 0-19 years), the incidence rate of all primary brain and other CNS tumors was 6.14. An estimated 83,830 new cases of malignant and non-malignant brain and other CNS tumors are expected to be diagnosed in the US in 2020 (24,970 malignant and 58,860 non-malignant). There were 81,246 deaths attributed to malignant brain and other CNS tumors between 2013 and 2017. This represents an average annual mortality rate of 4.42. The 5-year relative survival rate following diagnosis of a malignant brain and other CNS tumor was 23.5% and for a non-malignant brain and other CNS tumor was 82.4%.
Organizational Characteristics and Readiness for Tobacco-Free Workplace Program Implementation Moderates Changes in Clinician’s Delivery of Smoking Interventions within Behavioral Health Treatment Clinics
Authors: Nitturi Vijay , Chen Tzu-An , Kyburz Bryce , Martinez Leal Isabel , Correa-Fernandez Virmarie , O’Connor Daniel P , Williams Teresa , Garey Lorra , Stacey Tim , Wilson William T , Lam Cho , Reitzel Lorraine R 
Published: August 2020

AbstractBackgroundSmoking is elevated amongst individuals with behavioral health disorders, but not commonly addressed. Taking Texas Tobacco Free is an evidence-based, tobacco-free workplace program that addresses this, in-part, by providing clinician training to treat tobacco use in local mental health authorities (LMHAs). This study examined organizational moderators of change in intervention delivery from pre- to post-program implementation.MethodsLMHA leaders completed the Organizational Readiness for Implementing Change (ORIC) and provided organization demographics pre-implementation. Clinicians (N = 1237) were anonymously surveyed about their consistent use of the 5As (Asking about smoking; Advising clientele to quit; Assessing willingness to quit; Assisting them to quit; Arranging follow-up) pre- and post-program implementation. Adjusted generalized linear mixed models were used for analyses (responses nested within LMHAs), with interaction terms used to assess moderation effects.ResultsClinician delivery of 5As increased pre- to post-implementation (p &lt; .001). LMHAs with fewer employees (ref = ≤300) demonstrated greater increases in Asking, Assessing, and Assisting over time. LMHAs with fewer patients (ref = ≤10 000) evinced greater changes in Asking over time. Less initial ORIC Change Efficacy, Change Commitment, and Task Knowledge were each associated with greater pre- to post-implementation changes in Asking. Less initial Task Knowledge was associated with greater increases in Advising, Assessing, and Assisting. Finally, less initial Resource Availability was associated with greater increases in Assisting (all moderation term ps &lt; .025).ConclusionThe smallest and least ready LMHAs showed the largest gains in tobacco cessation intervention delivery; thus, low initial readiness was not a barrier for program implementation, particularly when efficacy-building training and resources are provided.ImplicationsThis study examined organizational moderators of increases in tobacco cessation treatment delivery over time following the implementation of a comprehensive tobacco-free workplace program within 20 of 39 LMHAs across Texas (hundreds of clinics; servicing &gt;50% of the state) from 2013 to 2018. Overall, LMHAs with fewer employees and patients, and that demonstrated the least initial readiness for change, evinced greater gains in intervention delivery. Findings add to dissemination and implementation science by supporting that low initial readiness was not a barrier for this aspect of tobacco-free workplace program implementation when resources and clinician training sessions were provided.