bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Design, Construction and Maintenance of a SuDS management Train to Address Surface water Flows by Engaging the Community: Gawilan Refugee Camp, Ninewah Governate, Kurdistan Region of Iraq
Authors: Charlesworth Susanne M. , Mctough Mitchell , Adam-Bradford Andrew 
Published: September 2019

AbstractRefugee camps are set up under crisis conditions in the Kurdistan Region of Iraq by the United Nations High Commissioner for Refugees (UNHCR) with Water, Sanitation and Hygiene (WASH) installed as a matter of course. However, in general, little account is taken of surface-water drainage or greywater management until the camp floods or greywater streams become an environmental or health issue. This article reports on the construction of a sustainable drainage systems (SuDS) management train in a refugee camp with the community and local non-governmental organizations to address excess surface water and lack of greywater management in this most challenging of environments. There is thus potential to influence policy, at the first stages of planning, to encourage the installation of drainage as well as WASH. SuDS mimic nature by percolating water into the ground, storing it and allowing slow conveyance to reduce the storm peak, improve water quality and provide space for amenity for residents and for biodiversity. By encouraging the water to infiltrate, polluted standing water between dwellings and on the street is reduced, so that human and environmental health is improved, with the potential to address nuisance-insect-breeding sites. Site walkovers, workshops and meetings engaged residents in the design process from the very beginning. The design produced by the community was professionally drawn up and passed to the UNHCR and local management engineers for comment and approval; this article describes the process of designing and constructing the first SuDS-management train to be built in a humanitarian setting.
Towards a Neo-cosmetic Humanitarianism: Refugee Self-reliance as a Social-cohesion Regime in Lebanon’s Halba
Authors: Carpi Estella 
Published: September 2019

AbstractThis article focuses on Syrian-refugee self-reliance and humanitarian efforts meant to foster it in Halba, northern Lebanon. I argue that humanitarian livelihood programming is ‘neo-cosmetic’, as the skills refugees acquire through humanitarian programmes turn out to be little more than a cosmetic accessory. While the humanitarian apparatus deliberately limits its action in order not to challenge host economies, the acquired skills do not practically enhance refugees’ possibility to be employed. Instead, refugee self-reliance is reconfigured as the ‘inter-ethnic promotion of host stability’. Relatedly, I propose that the aim of implementing social cohesion in multi-ethnic areas reveals a new ethnicization of care within the humanitarian system. Within this framework, the citizen practice of running hardware stores on a permanent basis coexists with the temporariness of refugee livelihood practices. Lastly, I rethink social membership in a refugee–host setting by adopting a practice-based approach to the research subjects in an effort to challenge the ethnic definitions of social groups and other pre-established forms of belonging.
Chronic constrictive pericarditis complicated with huge right atrial thrombus in a child with abdominal tuberculosis: a rare life-threatening condition
Authors: Kumar Rupesh , Raja Javid , Rawat Sanjib , Srivastava Ayush , Thingnam Shyam Kumar Singh 
Published: September 2019

Abstract
Chronic constrictive pericarditis (CCP) is the most common pericardial pathology. CCP complicating with intracardiac thrombus is a rare entity, the detection of thrombus preoperatively is life-saving in avoiding the risk of pulmonary thromboembolism during anterior pericardiectomy. Transesophageal echocardiography has been shown to have better sensitivity in detecting atrial thrombus than transthoracic echocardiography. Surgical removal of right atrial thrombus under cardiopulmonary bypass should be considered.
The Rationally Supererogatory
Authors: Benn Claire , Bales Adam 
Published: September 2019

AbstractThe notion of supererogation—going above and beyond the call of duty—is typically discussed in a moral context. However, in this paper we argue for the existence of rationally supererogatory actions: that is, actions that go above and beyond the call of rational duty. In order to establish the existence of such actions, we first need to overcome the so-called paradox of supererogation: we need to provide some explanation for why, if some act is rationally optimal, it is not the case that we are rationally required to carry out that act. We argue that a response to this ‘paradox’ can be found by reflecting on normative conflicts: cases where what is best according to some normative domain is different from what is best according to some other normative domain.
Synchrocurvature modelling of the multifrequency non-thermal emission of pulsars
Authors: Torres Diego F , Viganò Daniele , Coti Zelati Francesco , Li Jian 
Published: September 2019

ABSTRACT
We apply a synchrocurvature spectral emission model based on characterizing the dynamics of magnetospheric particles to fit the phase-average spectra of the most extended data base for the non-thermal spectra of pulsars. We consider 36 pulsars with well-determined non-thermal spectra from X-rays to gamma-rays. The sample includes Crab and the Crab twin, for which the spectra extend even to the optical/ultraviolet and infrared energies. We find that the model – with just three physical parameters and a global scaling – can fit the observations well across eight orders of magnitude for 18 of the 36 pulsars studied. Additionally, we find a set of eight pulsars for which the model still provides arguably good fits and another set of 10 pulsars for which the model fails in reproducing the spectra. We discuss why, propose and provide physical interpretations for a simple model extension (related to the geometry of the accelerating system with regards to the observer) that allows dealing with all such cases, ultimately providing very good fits for all pulsars. The extended model is still austere, adding only two additional parameters to the former set, of the same kind of the ones previously used. We use these fits to discuss issues going from the observed spectral origin, to the extent of the dominance of synchrotron or curvature regimes, the use of a model as predictor for searching new non-thermal pulsars starting from gamma-ray surveys, and how the model offers a setting where phase shifts between X-ray and gamma-ray light curves would naturally arise.
Gaussian process modelling of granulation and oscillations in red giant stars
Authors: Pereira Filipe , Campante Tiago L , Cunha Margarida S , Faria João P , Santos Nuno C , Barros Susana C C , Demangeon Olivier , Kuszlewicz James S , Corsaro Enrico 
Published: September 2019

ABSTRACTThe analysis of photometric time series in the context of transiting planet surveys suffers from the presence of stellar signals, often dubbed ‘stellar noise’. These signals, caused by stellar oscillations and granulation, can usually be disregarded for main-sequence stars, as the stellar contributions average out when phase-folding the light curve. For evolved stars, however, the amplitudes of such signals are larger and the timescales similar to the transit duration of short-period planets, requiring that they be modelled alongside the transit. With the promise of TESS delivering of the order of ∼105 light curves for stars along the red giant branch, there is a need for a method capable of describing the ‘stellar noise’ while simultaneously modelling an exoplanet’s transit. In this work, a Gaussian process regression framework is used to model stellar light curves and the method validated by applying it to TESS-like artificial data. Furthermore, the method is used to characterize the stellar oscillations and granulation of a sample of well-studied Kepler low-luminosity red giant branch stars. The parameters determined are compared to equivalent ones obtained by modelling the power spectrum of the light curve. Results show that the method presented is capable of describing the stellar signals in the time domain and can also return an accurate and precise measurement of νmax, i.e. the frequency of maximum oscillation amplitude. Preliminary results show that using the method in transit modelling improves the precision and accuracy of the ratio between the planetary and stellar radius, Rp/R⋆. The method’s implementation is publicly available.1
Galaxy properties as revealed by MaNGA – I. Constraints on IMF and M*/L gradients in ellipticals
Authors: Domínguez Sánchez H , Bernardi M , Brownstein J R , Drory N , Sheth R K 
Published: September 2019

ABSTRACT
We estimate ages, metallicities, α-element abundance ratios, and stellar initial mass functions (IMFs) of elliptical (E) and S0 galaxies from the MaNGA-DR15 survey. We stack spectra and use a variety of single stellar population synthesis models to interpret the absorption line strengths in these spectra. We quantify how these properties vary across the population, as well as with galactocentric distance. This paper is the first of a series and is based on a sample of pure elliptical galaxies at z ≤ 0.08. We confirm previous work showing that IMFs in Es with the largest luminosity (Lr) and central velocity dispersion (σ0) appear to be increasingly bottom heavy towards their centres. For these galaxies the stellar mass-to-light ratio decreases at most by a factor of 2 from the central regions to Re. In contrast, for lower Lr and σ0 galaxies, the IMF is shallower and M*/Lr in the central regions is similar to the outskirts, although quantitative estimates depend on assumptions about element abundance gradients. Accounting self-consistently for these gradients when estimating both M* and Mdyn brings the two into good agreement: gradients reduce Mdyn by ∼0.2 dex while only slightly increasing the M* inferred using a Kroupa IMF. This is a different resolution of the M*–Mdyn discrepancy than has been followed in the recent literature where M* of massive galaxies is increased by adopting a Salpeter IMF throughout the galaxy while leaving Mdyn unchanged. A companion paper discusses how stellar population differences are even more pronounced if one separates slow from fast rotators.
Seeking edge-on galaxies with substantial extraplanar dust using a radiative transfer model: determination of the model parameter uncertainties for EON_10.477_41.954 (FGC 79)
Authors: Shinn Jong-Ho 
Published: September 2019

ABSTRACTWe have revisited the target EON_10.477_41.954 in order to determine more accurately the uncertainties in the model parameters that are important for target classification (i.e. galaxies with or without substantial extraplanar dust). We performed a Markov chain Monte Carlo (MCMC) analysis for the 15 parameters of the three-dimensional radiative-transfer galaxy model we used previously for target classification. To investigate the convergence of the MCMC sampling – which is usually neglected in the literature but should not be – we monitored the integrated autocorrelation time (τint), and we achieved effective sample sizes >5650 for all the model parameters. The confidence intervals are unstable at the beginning of the iterations where the values of τint are increasing, but they become stable in later iterations where those values are almost constant. The final confidence intervals are ∼5–100 times larger than the nominal uncertainties used in our previous study (the standard deviation of three best-fitting results). Thus, those nominal uncertainties are not good proxies for the model-parameter uncertainties. Although the position of EON_10.477_41.954 in the target-classification plot (the scale height to diameter ratio of dust versus that of light source) decreases by about 20–30 per cent when compared to our previous study, its membership in the ‘high-group’ – i.e. among galaxies with substantial extraplanar dust – nevertheless remains unchanged.
Secularly powered outflows from AGNs: the dominance of non-merger driven supermassive black hole growth
Authors: Smethurst R J , Simmons B D , Lintott C J , Shanahan J 
Published: September 2019

ABSTRACT
Recent observations and simulations have revealed the dominance of secular processes over mergers in driving the growth of both supermassive black holes (SMBHs) and galaxy evolution. Here, we obtain narrow-band imaging of AGN powered outflows in a sample of 12 galaxies with disc-dominated morphologies, whose history is assumed to be merger-free. We detect outflows in 10/12 sources in narrow-band imaging of the $\mathrm{[O\, \small {III}] }$ $5007~\mathring{\rm A}$ emission using filters on the Shane-3m telescope. We calculate a mean outflow rate for these AGNs of $0.95\pm 0.14~\rm {M}_{\odot }~\rm {yr}^{-1}$. This exceeds the mean accretion rate of their SMBHs ($0.054\pm 0.039~\rm {M}_{\odot }~\rm {yr}^{-1}$) by a factor of 18. Assuming that the galaxy must provide at least enough material to power both the AGN and outflow, this gives a lower limit on the average inflow rate of $1.01\pm 0.14~\rm {M}_{\odot }~\rm {yr}^{-1}$, a rate which simulations show can be achieved by bars, spiral arms, and cold accretion. We compare our disc-dominated sample to a sample of nearby AGNs with merger dominated histories and show that the black hole accretion rates in our sample are five times higher (4.2σ) and the outflow rates are five times lower (2.6σ). We suggest that this could be a result of the geometry of the smooth, planar inflow in a secular dominated system, which is both spinning up the black hole to increase accretion efficiency and less affected by feedback from the outflow, than in a merger-driven system with chaotic quasi-spherical inflows. This work provides further evidence that secular processes are sufficient to fuel SMBH growth.
Deep Learning Algorithms Applied to the Classification of Video Meteor Detections
Authors: Gural Peter S 
Published: September 2019

Abstract
The application of a class of advanced machine learning techniques, namely deep learning, has been applied to automating the confirmation/classification of potential meteor tracks in video imagery. Deep learning is shown to perform remarkably well, even surpassing human performance, and will likely supplant the need for human visual inspection and review of collected meteor imagery. When applied to time series measurements of meteor track centroid positions and integrated intensities obtained from each video frame, a recurrent neural network (RNN) has achieved 98.1 per cent recall, which is defined as the number of true meteors properly classified as meteors. The RNN allowed only 2.1 per cent leakage, defined herein as the number of false positives that were incorrectly identified as meteors. The desire is to maximize recall to avoid missed orbit estimations, while also minimizing false alarms leaking through to the next processing stage of multi-site trajectory and orbit estimation. When two-dimensional spatial imagery is available or the temporal image sequence can be reconstructed, these results climb to 99.94 per cent recall and only 0.4 per cent leakage when employing a convolutional neural network (CNN). This has been further generalized from a baseline of interleaved analog video to modern progressive scan digital imagery with equivalent results. The trained CNN, nicknamed MeteorNet, will be used for post-detection automated screening of potential meteor tracks and explored in the future as a potential upstream meteor detector.
Testing the entropy calibration of the radii of cool stars: models of α Centauri A and B
Authors: Spada Federico , Demarque Pierre 
Published: September 2019

Abstract
We present models of α Centauri A and B implementing an entropy calibration of the mixing-length parameter αMLT, recently developed and successfully applied to the Sun (Spada et al. 2018, ApJ, 869, 135). In this technique the value of αMLT in the 1D stellar evolution code is calibrated to match the adiabatic specific entropy derived from 3D radiation-hydrodynamics simulations of stellar convective envelopes, whose effective temperature, surface gravity, and metallicity are selected consistently along the evolutionary track. The customary treatment of convection in stellar evolution models relies on a constant, solar-calibrated αMLT. There is, however, mounting evidence that this procedure does not reproduce the observed radii of cool stars satisfactorily. For instance, modelling α Cen A and B requires an ad-hoc tuning of αMLT to distinct, non-solar values. The entropy-calibrated models of α Cen A and B reproduce their observed radii within $1\%$ (or better) without externally adjusted parameters. The fit is of comparable quality to that of models with freely adjusted αMLT for α Cen B (within 1 σ), while it is less satisfactory for α Cen A (within ≈2.5 σ). This level of accuracy is consistent with the intrinsic uncertainties of the method. Our results demonstrate the capability of the entropy calibration method to produce stellar models with radii accurate within $1\%$. This is especially relevant in characterising exoplanet-host stars and their planetary systems accurately.
On the survivability of planets in young massive clusters and its implication of planet orbital architectures in globular clusters
Authors: Cai Maxwell X , Portegies Zwart S , Kouwenhoven M B N , Spurzem Rainer 
Published: September 2019

ABSTRACT
As of 2019 August, among the more than 4000 confirmed exoplanets, only one has been detected in a globular cluster (GC) M4. The scarce of exoplanet detections motivates us to employ direct N-body simulations to investigate the dynamical stability of planets in young massive clusters (YMC), which are potentially the progenitors of GCs. In an N = 128 k cluster of virial radius 1.7 pc (comparable to Westerlund-1), our simulations show that most wide-orbit planets (a ≥ 20 au) will be ejected within a time-scale of 10 Myr. Interestingly, more than $70{{\ \rm per\ cent}}$ of planets with a < 5 au survive in the 100 Myr simulations. Ignoring planet–planet scattering and tidal damping, the survivability at t Myr as a function of initial semimajor axis a0 in au in such a YMC can be described as fsurv(a0, t) = −0.33log10(a0)(1 − e−0.0482t) + 1. Upon ejection, about $28.8{{\ \rm per\ cent}}$ of free-floating planets (FFPs) have sufficient speeds to escape from the host cluster at a crossing time-scale. The other FFPs will remain bound to the cluster potential, but the subsequent dynamical evolution of the stellar system can result in the delayed ejection of FFPs from the host cluster. Although a full investigation of planet population in GCs requires extending the simulations to multiGyr, our results suggest that wide-orbit planets and free-floating planets are unlikely to be found in GCs.
The aspherical explosion of the Type IIP SN 2017gmr
Authors: Nagao T , Cikota A , Patat F , Taubenberger S , Bulla M , Faran T , Sand D J , Valenti S , Andrews J E , Reichart D E 
Published: September 2019

ABSTRACT
Type IIP supernovae (SNe IIP), which represent the most common class of core-collapse (CC) SNe, show a rapid increase in continuum polarization just after entering the tail phase. This feature can be explained by a highly asymmetric helium core, which is exposed when the hydrogen envelope becomes transparent. Here we report the case of an SN IIP (SN 2017gmr) that shows an unusually early rise of the polarization, ≳30 d before the start of the tail phase. This implies that SN 2017gmr is an SN IIP that has very extended asphericity. The asymmetries are not confined to the helium core, but reach out to a significant part of the outer hydrogen envelope, hence clearly indicating a marked intrinsic diversity in the aspherical structure of CC explosions. These observations provide new constraints on the explosion mechanism, where viable models must be able to produce such extended deviations from spherical symmetry, and account for the observed geometrical diversity.
The discovery of secondary lobes in the Seyfert galaxy NGC 2639
Authors: Sebastian Biny , Kharb P , O’Dea C P , Gallimore J F , Baum S A 
Published: September 2019

ABSTRACT
We report the discovery of a secondary pair of radio lobes in the Seyfert galaxy NGC 2639 with polarization-sensitive observations with the Karl G. Jansky Very Large Array (VLA). The presence of these lobes, which are aligned nearly perpendicular to the known set of radio lobes observed in the east–west direction, has not been reported previously in the literature. The in-band rotation measure image shows gradients in both the lobes indicative of organized magnetic field structures on kpc-scales. The magnetic field structure is aligned with the jet/lobe direction in both the lobes. Based on the settled optical morphology of the host galaxy, it is likely that a minor merger that did not disrupt the host galaxy structure is responsible for the observed features in NGC 2639. This also explains the near 90° change in the jet direction; the current jet direction being the result of a new accretion disc formed by the minor merger, whose direction was a result of the angular momentum of the inflowing merger gas.
The fifth main-sequence magnetic B-type star showing coherent radio emission: Is this really a rare phenomenon?
Authors: Das Barnali , Chandra Poonam , Shultz Matt E , Wade Gregg A 
Published: September 2019

ABSTRACT
We report the discovery of intense, highly directional radio emission from the Bp star HD 35298, which we interpret as the consequence of Electron Cyclotron Maser Emission (ECME). The star was observed with the Giant Metrewave Radio Telescope near the rotational phases of both magnetic nulls in band 4 (550–750 MHz) and one of the nulls in band 5 (1060–1460 MHz). In band 4, we observed flux density enhancement in both circular polarizations near both magnetic nulls. The sequences of arrival of the left and right circularly polarized pulses are opposite near the two nulls. In band 5, we did not have circular polarization information and hence measured only the total intensity light curve, which also shows enhancement around the magnetic null. The observed sequence of the circular polarization signs in band 4, compared with the longitudinal magnetic field curve, is able to locate the hemisphere from which ECME arises. This observational evidence supports the scenario of ECME in the ordinary mode, arising in a magnetosphere shaped like an oblique dipole. HD 35298 is the most slowly rotating and most distant main-sequence magnetic star from which ECME has been observed.