bluuebunny/crossref_metadata_2025_split huggingface dataset:
Rapid estimation of earthquake locations using waveform traveltimes
Authors: Vasco D W , Nakagawa Seiji , Petrov Petr , Newman Greg 
Published: March 2019

SUMMARYWe introduce a new approach for locating earthquakes using arrival times derived from waveforms. The most costly computational step of the algorithm scales as the number of stations in the active seismographic network. In this approach, a variation on existing grid search methods, a series of full waveform simulations are conducted for all receiver locations, with sources positioned successively at each station. The traveltime field over the region of interest is calculated by applying a phase picking algorithm to the numerical wavefields produced from each simulation. An event is located by subtracting the stored traveltime field from the arrival time at each station. This provides a shifted and time-reversed traveltime field for each station. The shifted and time-reversed fields all approach the origin time of the event at the source location. The mean or median value at the source location thus approximates the event origin time. Measures of dispersion about this mean or median time at each grid point, such as the sample standard error and the average deviation, are minimized at the correct source position. Uncertainty in the event position is provided by the contours of standard error defined over the grid. An application of this technique to a synthetic data set indicates that the approach provides stable locations even when the traveltimes are contaminated by additive random noise containing a significant number of outliers and velocity model errors. It is found that the waveform-based method out-performs one based upon the eikonal equation for a velocity model with rapid spatial variations in properties due to layering. A comparison with conventional location algorithms in both a laboratory and field setting demonstrates that the technique performs at least as well as existing techniques.
Responsible innovation in human germline gene editing. Background document to the recommendations of ESHG and ESHRE†‡
Authors: de Wert Guido , Heindryckx Björn , Pennings Guido , Clarke Angus , Eichenlaub-Ritter Ursula , van El Carla G , Forzano Francesca , Goddijn Mariëtte , Howard Heidi C , Radojkovic Dragica , Rial-Sebbag Emmanuelle , Dondorp Wybo , Tarlatzis Basil C , Cornel Martina C ,   on behalf of the European Society of Human Genetics and the European Society of Human Reproduction and Embryology
Published: March 2019

AbstractTechnological developments in gene editing raise high expectations for clinical applications, including editing of the germline. The European Society of Human Reproduction and Embryology (ESHRE) and the European Society of Human Genetics (ESHG) together developed a Background document and Recommendations to inform and stimulate ongoing societal debates. This document provides the background to the Recommendations. Germline gene editing is currently not allowed in many countries. This makes clinical applications in these countries impossible now, even if germline gene editing would become safe and effective. What were the arguments behind this legislation, and are they still convincing? If a technique could help to avoid serious genetic disorders, in a safe and effective way, would this be a reason to reconsider earlier standpoints? This Background document summarizes the scientific developments and expectations regarding germline gene editing, legal regulations at the European level, and ethics for three different settings (basic research, pre-clinical research and clinical applications). In ethical terms, we argue that the deontological objections (e.g. gene editing goes against nature) do not seem convincing while consequentialist objections (e.g. safety for the children thus conceived and following generations) require research, not all of which is allowed in the current legal situation in European countries. Development of this Background document and Recommendations reflects the responsibility to help society understand and debate the full range of possible implications of the new technologies, and to contribute to regulations that are adapted to the dynamics of the field while taking account of ethical considerations and societal concerns.
Amplifier linearity accounts for discrepancies in echo-integration measurements from two widely used echosounders
Authors: De Robertis Alex , Bassett Christopher , Andersen Lars Nonboe , Wangen Ivar , Furnish Scott , Levine Michael 
Published: March 2019

Abstract
The Simrad EK60 echosounder is widely used in acoustic-trawl surveys. It has recently been replaced by the EK80, which can be configured to operate in a manner similar to the EK60. To examine whether EK80s can be substituted for EK60s, the echosounders were configured to alternate transmissions from common transducers at four frequencies during three acoustic-trawl surveys. Significant differences between echo-integration measurements of fish were observed at 18, 38, and 70 kHz. EK80 measurements were 3–12% lower than those from EK60. At 120 kHz EK80/EK60 ratios were less than, but not statistically different from one. The EK80/EK60 discrepancy increased with range. The observed discrepancies were identified to be related to slight over-amplification of low-power signals (&lt;−90 dB re 1 W) by EK60. EK80 amplified signals linearly over a wider range of measured powers. After accounting for over-amplification of weak signals by the EK60, the range dependence was removed and both echosounders produced equivalent results. The impact of over-amplification by the EK60 will be relatively small for surveys of strong scatters (fishes with swimbladders) at short ranges, but has the potential to be greater for surveys of weak scatterers and/or long observation ranges.
Perioperative ischaemic reperfusion injury and allograft function in the early post-transplantation period
Authors: Nakamura Yuki , Saito Shunsuke , Miyagawa Shigeru , Yoshikawa Yasushi , Hata Hiroki , Yoshioka Daisuke , Toda Koichi , Sawa Yoshiki 
Published: March 2019

Abstract

OBJECTIVES
Ischaemic reperfusion injury (IRI) is an inevitable complication of heart transplantation (HTX) and is observed as a pathological finding in biopsies from transplanted allografts. The aim of this study was to evaluate the severity of IRI and determine the clinical outcomes of HTX in patients with severe IRI.

METHODS
We enrolled 74 consecutive patients who had undergone HTX since 2007. Endomyocardial biopsy samples were obtained from the right ventricle of the transplanted heart. IRI was graded as ‘trivial’, ‘mild’, ‘moderate’ or ‘severe’ according to the extent of IRI-specific findings in the samples. The cohort was divided into a moderate-to-severe IRI group with 21 patients [IRI(+)] and a low-grade group with 53 patients [IRI(−)].

RESULTS
The frequency of mechanical circulatory support and duration of catecholamine dependence in the early postoperative period were significantly higher in the IRI(+) group compared to the IRI(−) group. However, overall survival after HTX and mid-term cardiac allograft function were not significantly different between the groups. Among perioperative factors, cardiac ischaemic time was significantly different between the groups [IRI(−) vs IRI(+), 199 ± 38 min vs 239 ± 39 min; P < 0.001]. Incremental increases in cardiac ischaemic time were correlated with increases in IRI severity. Serum troponin T levels 3 h after donor heart reperfusion was significantly correlated with cardiac ischaemic time (r = 0.418, P = 0.0007).

CONCLUSIONS
IRI is associated with a complicated clinical course in the early post-HTX period due to temporary deterioration of allograft function. This may be attributable to myocardial stunning caused by long donor heart ischaemic time during HTX.
Total arterial myocardial revascularization using bilateral internal mammary arteries and the role of postoperative sternal stabilization to reduce wound infections in a large cohort study
Authors: Albert Marc , Nagib Ragi , Ursulescu Adrian , Franke Ulrich F W 
Published: March 2019

Abstract

OBJECTIVES
Total arterial myocardial revascularization using bilateral internal mammary arteries shows improved results for mortality, long-term survival and superior graft patency. It has become the standard technique according to recent guidelines. However, these patients may have an increased risk of developing sternal wound infections, especially obese patients or those with diabetes. One reason for the wound complications may be early sternum instability. This situation could be avoided by using a thorax support vest (e.g. Posthorax® vest). This retrospective study compared the wound complications after bilateral internal mammary artery grafting including the use of a Posthorax vest.

METHODS
Between April 2015 and May 2017, 1613 patients received total arterial myocardial revascularization using bilateral internal mammary artery via a median sternotomy. The Posthorax support vest was used from the second postoperative day. We compared those patients with 1667 patients operated on via the same access in the preceding 26 months. The end points were the incidence of wound infections, when the wound infection occurred and how many wound revisions were needed until wound closure.

RESULTS
The demographic data of both groups were similar. A significant advantage for the use of a thorax support vest could be seen regarding the incidence of wound infections (P = 0.036) and the length of hospital stay when a wound complication did occur (P = 0.018).

CONCLUSIONS
As seen in this retrospective study, the early perioperative use of a thorax stabilization vest, such as the Posthorax vest, can reduce the incidence of sternal wound complications significantly. Furthermore, when a wound infection occurred, and the patient returned to the hospital for wound revision, patients who were given the Posthorax vest postoperatively had a significantly shorter length of stay until wound closure.
Varicella Zoster Virus Alters Expression of Cell Adhesion Proteins in Human Perineurial Cells via Interleukin 6
Authors: Blackmon Anna M , Como Christina N , Bubak Andrew N , Mescher Teresa , Jones Dallas , Nagel Maria A 
Published: March 2019

AbstractBackgroundIn temporal arteries (TAs) from patients with giant cell arteritis, varicella zoster virus (VZV) is seen in perineurial cells that surround adventitial nerve bundles and form the peripheral nerve-extrafascicular tissue barrier (perineurium). We hypothesized that during VZV reactivation from ganglia, virus travels transaxonally and disrupts the perineurium to infect surrounding cells.MethodsMock- and VZV-infected primary human perineurial cells (HPNCs) were examined for alterations in claudin-1, E-cadherin, and N-cadherin. Conditioned supernatant was analyzed for a soluble factor(s) mediating these alterations and for the ability to increase cell migration. To corroborate in vitro findings, a VZV-infected TA was examined.ResultsIn VZV-infected HPNCs, claudin-1 redistributed to the nucleus; E-cadherin was lost and N-cadherin gained, with similar changes seen in VZV-infected perineurial cells in a TA. VZV-conditioned supernatant contained increased interleukin 6 (IL-6) that induced E-cadherin loss and N-cadherin gain and increased cell migration when added to uninfected HPNCs; anti-IL-6 receptor antibody prevented these changes.ConclusionsIL-6 secreted from VZV-infected HPNCs facilitated changes in E- and N-cadherin expression and cell migration, reminiscent of an epithelial-to-mesenchymal cell transition, potentially contributing to loss of perineurial cell barrier integrity and viral spread. Importantly, an anti-IL-6 receptor antibody prevented virus-induced perineurial cell disruption.
TNF receptor signalling in autoinflammatory diseases
Authors: Jarosz-Griffiths Heledd H , Holbrook Jonathan , Lara-Reyna Samuel , McDermott Michael F 
Published: March 2019

Abstract
Autoinflammatory syndromes are a group of disorders characterized by recurring episodes of inflammation as a result of specific defects in the innate immune system. Patients with autoinflammatory disease present with recurrent outbreaks of chronic systemic inflammation that are mediated by innate immune cells, for the most part. A number of these diseases arise from defects in the tumour necrosis factor receptor (TNFR) signalling pathway leading to elevated levels of inflammatory cytokines. Elucidation of the molecular mechanisms of these recently defined autoinflammatory diseases has led to a greater understanding of the mechanisms of action of key molecules involved in TNFR signalling, particularly those involved in ubiquitination, as found in haploinsufficiency of A20 (HA20), otulipenia/OTULIN-related autoinflammatory syndrome (ORAS) and linear ubiquitin chain assembly complex (LUBAC) deficiency. In this review, we also address other TNFR signalling disorders such as TNFR-associated periodic syndrome (TRAPS), RELA haploinsufficiency, RIPK1-associated immunodeficiency and autoinflammation, X-linked ectodermal dysplasia and immunodeficiency (X-EDA-ID) and we review the most recent advances surrounding these diseases and therapeutic approaches currently used to target these diseases. Finally, we explore therapeutic advances in TNF-related immune-based therapies and explore new approaches to target disease-specific modulation of autoinflammatory diseases.
Close-up view of an ongoing merger between the NGC 4839 group and the Coma cluster – a post-merger scenario
Authors: Lyskova N , Churazov E , Zhang C , Forman W , Jones C , Dolag K , Roediger E , Sheardown A 
Published: March 2019

ABSTRACT
We study a merger of the NGC 4839 group with the Coma cluster using X-ray observations from the XMM–Newton and Chandra telescopes. X-ray data show two prominent features: (i) a long (∼600 kpc in projection) and bent tail of cool gas trailing (towards south-west) the optical centre of NGC 4839, and (ii) a ‘sheath’ region of enhanced X-ray surface brightness enveloping the group, which is due to hotter gas. While at first glance the X-ray images suggest that we are witnessing the first infall of NGC 4839 into the Coma cluster core, we argue that a post-merger scenario provides a better explanation of the observed features and illustrate this with a series of numerical simulations. In this scenario, the tail is formed when the group, initially moving to the south-west, reverses its radial velocity after crossing the apocenter, the ram pressure ceases and the ram pressure-displaced gas falls back towards the centre of the group and overshoots it. Shortly after the apocenter passage, the optical galaxy, dark matter, and gaseous core move in a north-east direction, while the displaced gas continues moving to the south-west. The ‘sheath’ is explained as being due to interaction of the re-infalling group with its own tail of stripped gas mixed with the Coma gas. In this scenario, the shock, driven by the group before reaching the apocenter, has already detached from the group and would be located close to the famous relic to the south-west of the Coma cluster.
The role of convection in determining the ejection efficiency of common envelope interactions
Authors: Wilson E C , Nordhaus J 
Published: March 2019

ABSTRACT
A widely used method for parametrizing the outcomes of common envelopes (CEs) involves defining an ejection efficiency, $\bar{\alpha }_{\mathrm{eff}}$, that represents the fraction of orbital energy used to unbind the envelope as the orbit decays. Given $\bar{\alpha }_{\mathrm{eff}}$, a prediction for the post-CE orbital separation is possible with knowledge of the energy required to unbind the primary’s envelope from its core. Unfortunately, placing observational constraints on $\bar{\alpha }_{\mathrm{eff}}$ is challenging as it requires knowledge of the primary’s structure at the onset of the CE phase. Numerical simulations have also had difficulties reproducing post-CE orbital configurations as they leave extended, but still bound, envelopes. Using detailed stellar interior profiles, we calculate $\bar{\alpha }_{\mathrm{eff}}$ values for a matrix of primary-companion mass pairs when the primary is at maximal extent in its evolution. We find that the ejection efficiency is most sensitive to the properties of the surface-contact convective region (SCCR). In this region, the convective transport time-scales are often short compared to orbital decay time-scales, thereby allowing the star to effectively radiate orbital energy and thus lower $\bar{\alpha }_{\mathrm{eff}}$. The inclusion of convection in numerical simulations of CEs may aid ejection without the need for additional energy sources as the orbit must shrink substantially further before the requisite energy can be tapped to drive ejection. Additionally, convection leads to predicted post-CE orbital periods of less than a day in many cases, an observational result that has been difficult to reproduce in population studies where $\bar{\alpha }_{\mathrm{eff}}$ is taken to be constant. Finally, we provide a simple method to calculate $\bar{\alpha }_{\mathrm{eff}}$ if the properties of the SCCR are known.
The ultracool helium-atmosphere white dwarf companion of PSR J0740+6620?
Authors: Beronya D M , Karpova A V , Kirichenko A Yu , Zharikov S V , Zyuzin D A , Shibanov Yu A , Cabrera-Lavers A 
Published: March 2019

ABSTRACT
We report detection of the likely companion of the binary millisecond pulsar (MSP) J0740+6620 with the Gran Telescopio Canarias in the r′ and i′ bands. The position of the detected starlike source coincides with the pulsar coordinates within the 1σ uncertainty of ≈0.2 arcsec. Its magnitudes are r′ = 26.51 ± 0.17 and i′ = 25.49 ± 0.15. Comparing the data with the white dwarf (WD) cooling tracks suggests that it can be an ultracool helium-atmosphere WD with the temperature ≲3500 K and cooling age ≳5 Gyr. The age is consistent with the pulsar characteristic age corrected for kinematic effects. This is the reddest source among known WD companions of MSPs. Detection of the source in other bands would be useful to clarify its properties and nature.
The black hole X-ray transient Swift J1357.2–0933 as seen with Swift and NuSTAR during its 2017 outburst
Authors: Beri Aru , Tetarenko B E , Bahramian A , Altamirano Diego , Gandhi Poshak , Sivakoff G R , Degenaar N , Middleton M J , Wijnands R , Hernándz Santisteban J V , Paice John A 
Published: March 2019

ABSTRACT
We report on observations of black hole Swift J1357.2–0933, a member of the modest population of very faint X-ray transients. This source has previously shown intense dips in the optical light curve, a phenomena that has been linked to the existence of a ‘unique toroidal structure’ in the inner region of the disc, seen at a high inclination. Our observations, carried out by the Neil Gehrels Swift and NuSTAR X-ray observatories, do not show the presence of intense dips in the optical light curves. We find that the X-ray light curves do not show any features that would straightforwardly support an edge-on configuration or high inclination configuration of the orbit. This is similar to what was seen in the X-ray observations of the source during its 2011 outburst. Moreover, the broad-band spectra were well described with an absorbed power-law model without any signatures of cut-off at energies above 10 keV, or any reflection from the disc or the putative torus. Thus, the X-ray data do not support the unique ‘obscuring torus’ scenario proposed for J1357. We also performed a multiwavelength study using the data of X-ray telescope and Ultraviolet/Optical Telescope aboard Swift, taken during the ∼4.5 months duration of the 2017 outburst. This is consistent with what was previously inferred for this source. We found a correlation between the simultaneous X-ray and ultraviolet/optical data and our study suggests that most of the reprocessed flux must be coming out in the ultraviolet.
Hidden IR structures in NGC 40: signpost of an ancient born-again event
Authors: Toalá J A , Ramos-Larios G , Guerrero M A , Todt H 
Published: March 2019

Abstract
We present the analysis of infrared (IR) observations of the planetary nebula NGC 40 together with spectral analysis of its [WC]-type central star HD 826. Spitzer IRS observations were used to produce spectral maps centred at polycyclic aromatic hydrocarbons (PAH) bands and ionic transitions to compare their spatial distribution. The ionic lines show a clumpy distribution of material around the main cavity of NGC 40, with the emission from [Ar ii] being the most extended, whilst the PAHs show a rather smooth spatial distribution. Analysis of ratio maps shows the presence of a toroidal structure mainly seen in PAH emission, but also detected in a Herschel PACS 70 $\mu$m image. We argue that the toroidal structure absorbs the UV flux from HD 826, preventing the nebula to exhibit lines of high-excitation levels as suggested by previous authors. We discuss the origin of this structure and the results from the spectral analysis of HD 826 under the scenario of a late thermal pulse.
WISDOM project – IV. A molecular gas dynamical measurement of the supermassive black hole mass in NGC 524
Authors: Smith Mark D , Bureau Martin , Davis Timothy A , Cappellari Michele , Liu Lijie , North Eve V , Onishi Kyoko , Iguchi Satoru , Sarzi Marc 
Published: March 2019

ABSTRACT
We present high angular resolution (0.3 arcsec or $37\, \mathrm{pc}$) Atacama Large Millimeter/submillimeter Array observations of the CO(2–1) line emission from a central disc in the early-type galaxy NGC 524. This disc is shown to be dynamically relaxed, exhibiting ordered rotation about a compact $1.3\, \mathrm{mm}$ continuum source, which we identify as emission from an active supermassive black hole (SMBH). There is a hole at the centre of the disc slightly larger than the SMBH sphere of influence. An azimuthal distortion of the observed velocity field is found to be due to either a position angle warp or radial gas flow over the inner 2${^{\prime\prime}_{.}}$5. By forward-modelling the observations, we obtain an estimate of the SMBH mass of $4.0^{+3.5}_{-2.0}\times 10^8\,$ M⊙, where the uncertainties are at the 3σ level. The uncertainties are dominated by the poorly constrained inclination and the stellar mass-to-light ratio of this galaxy, and our measurement is consistent with the established correlation between SMBH mass and stellar velocity dispersion. Our result is roughly half that of the previous stellar dynamical measurement, but is consistent within the uncertainties of both. We also present and apply a new tool for modelling complex molecular gas distributions.
Conflict
Authors: Shortland Neil D. , Alison Laurence J. , Moran Joseph M. 
Published: March 2019

Abstract
This book is about decisions in military conflict and the psychological conflict they cause. By drawing on interviews conducted with real soldiers about real situations they faced, the book explores how soldiers choose between seemingly impossible options for which all outcomes appear horrendous. Their vivid and sometimes upsetting stories were part of the experience of war and became part of their identity. This book describes the processes that make choice selection so difficult; the psychology of decisional conflict; and the immediate, short-term, and longer term behavioral consequences of these actions. Special attention is directed to the concept of “decision inertia”—one of several kinds of “failures to act” in which decision-makers are unable to calculate and/or commit to a least-worst course of action. By referring to many real cases, readers are invited to consider their own responses to choosing between difficult options in order to help them understand what it might feel like when faced with making a least-worst decision in war.