bluuebunny/crossref_metadata_2025_split huggingface dataset:
Developing Assistive Technologies for Persons with Alzheimer’s Disease and Their Carers
Authors: Mahoney Diane Feeney 
Published: January 2020

Abstract
This chapter examines the ethical principles applicable to gerontechnology research and development for in-home monitoring of persons with neurocognitive impairments. Principles addressed include respect for persons, autonomy, beneficence, justice, nonabandonment, nonmalfeasance, and privacy. Key issues for designers, developers, end-users, and reviewers are highlighted by uniquely drawing from real-world research examples. Studies indicate that among stakeholders there remains an emotional tension between “high tech” and “high touch” interventions for older adults with dementia. At the extremes, technophobic humanists dismiss technology as universally inferior to human assistance, while techno-proponents view it as the solution to care problems resulting from human limitations. “Benevolent” geriatric protectionism from technology is paternalistic and stifles innovation, while pushing technology without input from geriatric end-users results in products mismatched to their needs. Society will be better served if both viewpoints thoughtfully consider the ethical foundation of their beliefs informed by research findings to foster approaches that do good, not harm.
The ALMaQUEST Survey – II. What drives central starbursts at z ∼ 0?
Authors: Ellison Sara L , Thorp Mallory D , Pan Hsi-An , Lin Lihwai , Scudder Jillian M , Bluck Asa F L , Sánchez Sebastian F , Sargent Mark 
Published: January 2020

ABSTRACT
Starburst galaxies have elevated star formation rates (SFRs) for their stellar mass. In Ellison et al., we used integral field unit maps of SFR surface density (ΣSFR) and stellar mass surface density (Σ⋆) to show that starburst galaxies in the local universe are driven by SFRs that are preferentially boosted in their central regions. Here, we present molecular gas maps obtained with the Atacama Large Millimeter Array (ALMA) observatory for 12 central starburst galaxies at z ∼ 0 drawn from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey. The ALMA and MaNGA data are well matched in spatial resolution, such that the ALMA maps of molecular gas surface density ($\Sigma _{\rm H_2}$) can be directly compared with MaNGA maps at kpc-scale resolution. The combination of $\Sigma _{\rm H_2}$, Σ⋆ and ΣSFR at the same resolution allow us to investigate whether central starbursts are driven primarily by enhancements in star formation efficiency (SFE) or by increased gas fractions. By computing offsets from the resolved Kennicutt-Schmidt relation ($\Sigma _{\rm H_2}$ versus ΣSFR) and the molecular gas main sequence (Σ⋆ versus $\Sigma _{\rm H_2}$), we conclude that the primary driver of the central starburst is an elevated SFE. We also show that the enhancement in ΣSFR is accompanied by a dilution in O/H, consistent with a triggering that is induced by metal poor gas inflow. These observational signatures are found in both undisturbed (9/12 galaxies in our sample) and recently merged galaxies, indicating that both interactions and secular mechanisms contribute to central starbursts.
Detecting double neutron stars with LISA
Authors: Lau Mike Y M , Mandel Ilya , Vigna-Gómez Alejandro , Neijssel Coenraad J , Stevenson Simon , Sesana Alberto 
Published: January 2020

ABSTRACT
We estimate the properties of the double neutron star (DNS) population that will be observable by the planned space-based interferometer Laser Interferometer Space Antenna (LISA). By following the gravitational radiation-driven evolution of DNSs generated from rapid population synthesis of massive binary stars, we estimate that around 35 DNSs will accumulate a signal-to-noise ratio above 8 over a 4-yr LISA mission. The observed population mainly comprises Galactic DNSs (94 per cent), but detections in the LMC (5 per cent) and SMC (1 per cent) may also be expected. The median orbital frequency of detected DNSs is expected to be 0.8 mHz, and many of them will be eccentric (median eccentricity of 0.11). LISA is expected to localize these DNSs to a typical angular resolution of 2°. We expect the best-constrained DNSs to have eccentricities known to a few parts in a thousand, chirp masses measured to better than 1 per cent fractional uncertainty, and sky localization at the level of a few arcminutes. The orbital properties will provide insights into DNS progenitors and formation channels. The localizations may allow neutron star natal kick magnitudes to be constrained through the Galactic distribution of DNSs, and make it possible to follow up the sources with radio pulsar searches. LISA is also expected to resolve ∼104 Galactic double white dwarfs, many of which may have binary parameters that resemble DNSs; we discuss how the combined measurement of binary eccentricity, chirp mass, and sky location may aid the identification of a DNS.
The nuclear region of NGC 613 – I. Multiwavelength analysis
Authors: da Silva Patrícia , Menezes R B , Steiner J E 
Published: January 2020

ABSTRACT
In this paper, we report a detailed study with a variety of data from optical, near-infrared, X-ray, and radio telescopes of the nuclear region of the galaxy NGC 613 with the aim of understanding its complexity. We detected an extended stellar emission in the nucleus that, at first, appears to be, in the optical band, two stellar nuclei separated by a stream of dust. The active galactic nucleus (AGN) is identified as a variable point-like source between these two stellar components. There is a central hard X-ray emission and an extended soft X-ray emission that closely coincides with the ionization cone, as seen in the [O iii]λ5007 emission. The centroid of the [O i]λ6300 emission does not coincide with the AGN, being shifted by 0.24 arcsec towards the ionization cone; this shift is probably caused by a combination of differential dust extinction together with emission and reflection in the ionization cone. The optical spectra extracted from the central region are typical of low-ionization nuclear emission-line regions. We also identify 10 H ii regions, eight of them in a star-forming ring that is visible in Br γ, [Fe ii]λ16436, and molecular CO(3-2) images observed in previous studies. Such a ring also presents weak hard X-ray emission, probably associated with supernova remnants, not detected in other studies. The position of the AGN coincides with the centre of a nuclear spiral (detected in previous works) that brings gas and dust from the bar to the nucleus, causing the high extinction in this area.
The Cluster AgeS Experiment (CASE) – VIII. Age and distance of the Globular Cluster 47 Tuc from the analysis of two detached eclipsing binaries
Authors: Thompson I B , Udalski A , Dotter A , Rozyczka M , Schwarzenberg-Czerny A , Pych W , Beletsky Y , Burley G S , Marshall J L , McWilliam A , Morrell N , Osip D , Monson A , Persson S E , Szymański M K , Soszyński I , Poleski R , Ulaczyk K , Wyrzykowski Ł , Kozłowski S , Mróz P , Pietrukowicz P , Skowron J 
Published: January 2020

ABSTRACT
We use photometric and spectroscopic observations of the eclipsing binary E32 in the globular cluster 47 Tuc to derive the masses, radii, and luminosities of the component stars. The system has an orbital period of 40.9 d, a markedly eccentric orbit with e = 0.24, and is shown to be a member of or a recent escaper from the cluster. We obtain $M_{\rm p} = 0.862\pm 0.005 \, \mathrm{M}_\odot$, $R_{\rm p} = 1.183\pm 0.003 \, \mathrm{R}_\odot$, $L_{\rm p} = 1.65\pm 0.05 \, \mathrm{L}_\odot$ for the primary and $M_{\rm s} = 0.827\pm 0.005 \, \mathrm{M}_\odot$, $R_{\rm s} = 1.004\pm 0.004 \, \mathrm{R}_\odot$, $L_{\rm s} = 1.14\pm 0.04\, \mathrm{L}_\odot$ for the secondary. Based on these data and on an earlier analysis of the binary V69 in 47 Tuc, we measure the distance to the cluster from the distance moduli of the component stars, and, independently, from a colour – surface brightness calibration. We obtain 4.55 ± 0.03 and 4.50 ± 0.07 kpc, respectively – values compatible within 1$\, \sigma$ with recent estimates based on Gaia DR2 parallaxes. By comparing the M–R diagram of the two binaries and the colour–magnitude diagram of 47 Tuc to Dartmouth model isochrones we estimate the age of the cluster to be 12.0 ± 0.5 Gyr, and the helium abundance of the cluster to be Y ≈ 0.25.
X-ray detected AGN in SDSS dwarf galaxies
Authors: Birchall Keir L , Watson M G , Aird J 
Published: January 2020

ABSTRACT
In this work we present a robust quantification of X-ray selected AGN in local (z ≤ 0.25) dwarf galaxies ($M_\mathrm{*} \le 3 \times 10^9 \, \mathrm{M_\odot }$). We define a parent sample of 4331 dwarf galaxies found within the footprint of both the MPA-JHU galaxy catalogue (based on SDSS DR8) and 3XMM DR7, performed a careful review of the data to remove misidentifications and produced a sample of 61 dwarf galaxies that exhibit nuclear X-ray activity indicative of an AGN. We examine the optical emission line ratios of our X-ray selected sample and find that optical AGN diagnostics fail to identify 85 per cent of the sources. We then calculated the growth rates of the black holes powering our AGN in terms of their specific accretion rates (∝ LX/M*, an approximate tracer of the Eddington ratio). Within our observed sample, we found a wide range of specific accretion rates. After correcting the observed sample for the varying sensitivity of 3XMM, we found further evidence for a wide range of X-ray luminosities and specific accretion rates, described by a power law. Using this corrected AGN sample we also define an AGN fraction describing their relative incidence within the parent sample. We found the AGN fraction increases with host galaxy mass (up to ≈6 per cent) for galaxies with X-ray luminosities between $10^{39} \, $ and $10^{42} \, \mathrm{erg\, s^{-1}}$, and by extrapolating the power law to higher luminosities, we found evidence to suggest the fraction of luminous AGN ($L_\mathrm{X} \ge 10^{42.4} \, \mathrm{erg\, s^{-1}}$) is constant out to z ≈ 0.7.
The [C ii]–SFR correlation in dwarf galaxies across cosmic time
Authors: Lupi Alessandro , Bovino Stefano 
Published: January 2020

ABSTRACT
Current galaxy observations suggest that a roughly linear correlation exists between the [C ii] emission and the star formation rate, either as spatially resolved or integrated quantities. Observationally, this correlation seems to be independent of metallicity, but the very large scatter does not allow to properly assess whether this is true. On the other hand, theoretical models tend to suggest a metallicity dependence of the correlation. In this study, we investigate the metallicity evolution of the correlation via a high-resolution zoom-in cosmological simulation of a dwarf galaxy employing state-of-the-art sub-grid modelling for gas cooling, star formation, and stellar feedback, and that self-consistently evolves the abundances of metal elements out of equilibrium. Our results suggest that the correlation should evolve with metallicity, in agreement with theoretical predictions, but also that this evolution can be hardly detected in observations, because of the large scatter. We also find that most of the [C ii] emission is associated with neutral gas at low-intermediate densities, whereas the highest emissivity is produced by the densest regions around star-forming regions.
A search for Centaurus A-like features in the spectra of Fermi-LAT detected radio galaxies
Authors: Rulten Cameron B , Brown Anthony M , Chadwick Paula M 
Published: January 2020

ABSTRACT
Motivated by the detection of a hardening in the γ-ray spectrum of the radio galaxy Centaurus A, we have analysed $\mathord {\sim }10$ yr of Fermi-Large Area Telescope (LAT) observations of 26 radio galaxies to search for similar spectral features. We find that the majority of the radio galaxies’ γ-ray spectral energy distributions are best fitted with a simple power-law model, and no spectral hardening similar to that found in Centaurus A was detected. We show that, had there been any such spectral features present in our sample of radio galaxies, they would have been seen, but note that seven of the radio galaxies (3C 111, 3C 120, 3C 264, IC 4516, NGC 1218, NGC 2892, and PKS 0625−35) show evidence for flux variability on 6-month time-scales, which makes the detection of any steady spectral features difficult. We find a strong positive correlation (r = 0.9) between the core radio power at 5 GHz and the γ-ray luminosity and, using a simple extrapolation to TeV energies, we expect around half of the radio galaxies studied will be detectable with the forthcoming Cherenkov Telescope Array.
Geometric properties of galactic discs with clumpy episodes
Authors: Beraldo e Silva Leandro , Debattista Victor P , Khachaturyants Tigran , Nidever David 
Published: January 2020

ABSTRACT
A scenario for the formation of the bi-modality in the chemical space [α/Fe] versus [Fe/H] of the Milky Way was recently proposed in which α-enhanced stars are produced early and quickly in clumps. Besides accelerating the enrichment of the medium with α-elements, these clumps scatter the old stars, converting in-plane to vertical motion, forming a geometric thick disc. In this paper, by means of a detailed analysis of the data from smooth particle hydrodynamical simulations, we investigate the geometric properties (in particular of the chemical thick disc) produced in this scenario. For mono-age populations we show that the surface radial density profiles of high-[α/Fe] stars are well described by single exponentials, while that of low-[α/Fe] stars require broken exponentials. This break is sharp for young populations and broadens for older ones. The position of the break does not depend significantly on age. The vertical density profiles of mono-age populations are characterized by single exponentials, which flare significantly for low-[α/Fe] stars but only weakly (or not at all) for high-[α/Fe] stars. For low-[α/Fe] stars, the flaring level decreases with age, while for high-[α/Fe] stars it weakly increases with age (although with large uncertainties). All these properties are in agreement with observational results recently reported for the Milky Way, making this a plausible scenario for the formation of the Galactic thick disc.
NuSTAR observation of Ark 564 reveals the variation of coronal temperature with flux
Authors: Barua Samuzal , Jithesh V , Misra Ranjeev , Dewangan Gulab C , Sarma Rathin , Pathak Amit 
Published: January 2020

ABSTRACT
The hard X-ray spectral index of some active galactic nuclei (AGN) has been observed to steepen with the source flux. This has been interpreted in a Comptonization scenario, where an increase in the soft flux decreases the temperature of the corona, leading to steepening of the photon index. However, the variation of the coronal temperature with flux has been difficult to measure due to the presence of complex reflection component in the hard X-rays and the lack of high-quality data at that energy band. Recently, a 200 ks Nuclear Spectroscopic Telescope Array(NuSTAR) observation of Ark 564 in 3–50 keV band revealed the presence of one of the coolest coronae with temperature kTe ∼ 15 keV in the time-averaged spectrum. Here, we reanalyse the data and examined the spectra in four flux levels. Our analysis shows that the coronal temperature decreased from ∼17 to ∼14 keV as the flux increased. The high energy photon index Γ ∼ 2.3 varied by less than 0.1, implying that the optical depth of the corona increased by about 10 per cent as the flux increased. This first reporting of coronal temperature variation with flux shows that further long observation by NuSTAR of this and other sources would shed light on the geometry and dynamics of the inner regions of the accretion flow.
X-ray plateaus in gamma-ray bursts’ light curves from jets viewed slightly off-axis
Authors: Beniamini Paz , Duque Raphaël , Daigne Frédéric , Mochkovitch Robert 
Published: January 2020

ABSTRACT
Using multiple observational arguments, recent work has shown that cosmological gamma-ray bursts (GRBs) are typically viewed at angles within, or close to the cores of their relativistic jets. One of those arguments relied on the lack of tens-of-days-long periods of very shallow evolution that would be seen in the afterglow light curves of GRBs viewed at large angles. Motivated by these results, we consider that GRBs efficiently produce γ-rays only within a narrow region around the core. We show that, on these near-core lines of sight, structured jets naturally produce shallow phases in the X-ray afterglow of GRBs. These plateaus would be seen by a large fraction of observers and would last between 102–105 s. They naturally reproduce the observed distributions of time-scales and luminosities as well as the intercorrelations between plateau duration, plateau luminosity, and prompt γ-ray energy. An advantage of this interpretation is that it involves no late-time energy injection which would be both challenging from the point of view of the central engine and, as we show here, less natural given the observed correlations between plateau and prompt properties.
Markov Chain Monte Carlo population synthesis of single radio pulsars in the Galaxy
Authors: Cieślar Marek , Bulik Tomasz , Osłowski Stefan 
Published: January 2020

ABSTRACT
We present a model of evolution of solitary neutron stars, including spin parameters, magnetic field decay, motion in the Galactic potential, and birth inside spiral arms. We use two parametrizations of the radio-luminosity law and model the radio selection effects. Dispersion measure is estimated from the recent model of free electron distribution in the Galaxy (YMW16). Model parameters are optimized using the Markov Chain Monte Carlo technique. The preferred model has a short decay scale of the magnetic field of $4.27^{+0.4}_{-0.38}$ Myr. However, it has non-negligible correlation with parameters describing the pulsar radio luminosity. Based on the best-fitting model, we predict that the Square Kilometre Array surveys will increase the population of known single radio pulsars by between 23 and 137 per cent. The indri code used for simulations is publicly available to facilitate future population synthesis efforts.
Disentangling Population History and Character Evolution among Hybridizing Lineages
Authors: Mullen Sean P , VanKuren Nicholas W , Zhang Wei , Nallu Sumitha , Kristiansen Evan B , Wuyun Qiqige , Liu Kevin , Hill Ryan I , Briscoe Adriana D , Kronforst Marcus R 
Published: January 2020

AbstractUnderstanding the origin and maintenance of adaptive phenotypic novelty is a central goal of evolutionary biology. However, both hybridization and incomplete lineage sorting can lead to genealogical discordance between the regions of the genome underlying adaptive traits and the remainder of the genome, decoupling inferences about character evolution from population history. Here, to disentangle these effects, we investigated the evolutionary origins and maintenance of Batesian mimicry between North American admiral butterflies (Limenitis arthemis) and their chemically defended model (Battus philenor) using a combination of de novo genome sequencing, whole-genome resequencing, and statistical introgression mapping. Our results suggest that balancing selection, arising from geographic variation in the presence or absence of the unpalatable model, has maintained two deeply divergent color patterning haplotypes that have been repeatedly sieved among distinct mimetic and nonmimetic lineages of Limenitis via introgressive hybridization.
The Many Flavours of Regret
Authors: Price Carolyn 
Published: January 2020

AbstractRegret is a slippery phenomenon. Fundamental questions about its fittingness conditions and functions have yet to be settled. Here, I offer a diagnosis of regret’s slippery character. Extending a suggestion made by Daniel Kahneman (1995, 1998), I argue that regret comes in a range of emotional flavours, distinguished in the first instance by their phenomenology. While regret has received some attention from philosophers, its varied phenomenology has not been investigated. Yet the varied phenomenology of regret is significant: it reflects further variations in its cognitive and motivational effects. As a result, I argue, different flavours of regret have different fittingness conditions and contribute to our lives in different ways. In Section I, I offer a preliminary sketch of regret and introduce the questions that drive my discussion. In Section II, I introduce regret’s different flavours. In Section III, I investigate their contrasting cognitive and motivational effects, with a view to determining their functions. In Section IV, I investigate what this implies concerning regret’s fittingness conditions—and, in particular, what constitutes a regrettable action.
I’ll Show You: Spite as a Reactive Attitude
Authors: Thomason Krista K 
Published: January 2020

AbstractSpite is typically considered a vicious emotion that causes us to engage in petty, vindictive, and sometimes self-destructive behavior. Even though it has this bad reputation, I will argue that spite is a reactive attitude. Spite is emotional defiance of another’s command: to spite you, I will do something exactly because you told me not to. Our liability to feelings of spite presupposes that we recognize others as having practical authority, which is why it qualifies as a reactive attitude. I conclude by offering conditions under which spite can be justified and unjustified.
Cannabinoids in the Treatment of Back Pain
Authors: Kim Teddy E , Townsend Robert K , Branch Charles L , Romero-Sandoval Edgar A , Hsu Wesley 
Published: January 2020

Abstract
Marijuana is increasingly utilized for the treatment of multiple medical problems, including back pain, in the United States. Although there is strong preclinical evidence supporting the promise of cannabinoids in the treatment of back pain, there is a paucity of clinical data supporting their use in clinical practice. Opioids are an important medication for the treatment of acute and chronic back pain, but utilization of opioid-based regimens have likely contributed to the growing opioid epidemic. The significant risk of morbidity, mortality, and dependence secondary to opioid medications have increased the interest in nonopioid medications, including cannabinoid-based pain regimens, in treating back pain. This review will provide an overview on the pharmacology, drug delivery methods, clinical evidence, and safety considerations critical to understanding the potential role of cannabinoids in the treatment of back pain.
Maximizing organs for donation: the potential for ex situ normothermic machine perfusion
Authors: Griffiths C , Scott W E , Ali S , Fisher A J 
Published: January 2020

Abstract
Currently, there is a shortfall in the number of suitable organs available for transplant resulting in a high number of patients on the active transplant waiting lists worldwide. To address this shortfall and increase the utilization of donor organs, the acceptance criteria for donor organs is gradually expanding including increased use of organs from donation after circulatory death. Use of such extended criteria donors and exposure of organs to more prolonged periods of warm or cold ischaemia also increases the risk of primary graft dysfunction occurring. Normothermic machine perfusion (NMP) offers a unique opportunity to objectively assess donor organ function outside the donor body and potentially recondition those deemed unsuitable on initial evaluation prior to implantation in the recipient. Furthermore, NMP provides a platform to support the use of established and novel therapeutics delivered directly to the organ, without the need to worry about potential deleterious ‘off-target’ side effects typically considered when treating the whole patient. This review will explore some of the novel therapeutics currently being added to perfusion platforms during NMP experimentally in an attempt to improve organ function and post-transplant outcomes.