bluuebunny/crossref_metadata_2025_split huggingface dataset:
GP attitudes to and expectations for providing personal genomic risk information to the public: a qualitative study
Authors: Smit Amelia K , Newson Ainsley J , Keogh Louise , Best Megan , Dunlop Kate , Vuong Kylie , Kirk Judy , Butow Phyllis , Trevena Lyndal , Cust Anne E 
Published: February 2019

BackgroundAs part of a pilot randomised controlled trial examining the impact of personal melanoma genomic risk information on behavioural and psychosocial outcomes, GPs were sent a booklet containing their patient’s genomic risk of melanoma.AimUsing this booklet as an example of genomic risk information that might be offered on a population-level in the future, this study explored GP attitudes towards communicating genomic risk information and resources needed to support this process.Design & settingSemi-structured interviews were conducted with 22 Australian GPs.MethodThe interviews were recorded and transcribed, and data were analysed thematically.ResultsGPs in this sample believed that communicating genomic risk may become a responsibility within primary care and they recommended a shared decisionmaking approach to guide the testing process. Factors were identified that may influence how and when GPs communicate genomic risk information. GPs view genomics-based risk as one of many disease risk factors and feel that this type of information could be applied in practice in the context of overall risk assessment for diseases for which prevention and early detection strategies are available. They believe it is important to ensure that patients understand their genomic risk and do not experience long-term adverse psychological responses. GPs desire clinical practice guidelines that specify recommendations for genomic risk assessment and patient management, point-of-care resources, and risk prediction tools that include genomic and traditional risk factors.ConclusionThese findings will inform the development of resources for preparing GPs to manage and implement genomic risk information in practice.
Atmospheric Structure and Radiation Pattern for Neutron-star Polar Caps Heated by Magnetospheric Return Currents
Authors: Bauböck Michi , Psaltis Dimitrios , Özel Feryal 
Published: February 2019

Abstract
The Neutron-star Interior Composition ExploreR (NICER) is collecting data to measure the radii of neutron stars by observing the pulsed emission from their surfaces. The primary targets are isolated, rotation-powered pulsars, in which the surface polar caps are heated by bombardment from magnetospheric currents of electrons and positrons. We investigate various stopping mechanisms for the beams of particles that bombard the atmosphere and calculate the heat deposition, the atmospheric temperature profiles, and the energy spectra and beaming of the emerging radiation. We find that low-energy particles with γ ∼ 2–10 deposit most of their energy in the upper regions of the atmosphere, at low optical depth, resulting in beaming patterns that are substantially different from those of deep-heated, radiative equilibrium models. Only particles with energies γ ≳ 50 penetrate to high optical depths and fulfill the conditions necessary for a deep-heating approximation. We discuss the implications of our work for modeling the pulse profiles from rotation-powered pulsars and for the inference of their radii with NICER observations.
Survey Observations to Study Chemical Evolution from High-mass Starless Cores to High-mass Protostellar Objects. II. HC3N and N2H+
Authors: Taniguchi Kotomi , Saito Masao , Sridharan T. K. , Minamidani Tetsuhiro 
Published: February 2019

Abstract
We have carried out survey observations of molecular emission lines from HC3N, N2H+, CCS, and cyclic-C3H2 in the 81–94 GHz band toward 17 high-mass starless cores (HMSCs) and 28 high-mass prorostellar objects (HMPOs) with the Nobeyama 45 m radio telescope. We have detected N2H+ in all of the target sources except one and HC3N in 14 HMSCs and in 26 HMPOs. We investigate the N(N2H+)/N(HC3N) column density ratio as a chemical evolutionary indicator of massive cores. Using the Kolmogorov–Smirnov (K-S) test and Welch’s t test, we confirm that the N(N2H+)/N(HC3N) ratio decreases from HMSCs to HMPOs. This tendency in high-mass star-forming regions is opposite to that in low-mass star-forming regions. Furthermore, we find that the detection rates of carbon-chain species (HC3N, HC5N, and CCS) in HMPOs are different from those in low-mass protostars. The detection rates of cyanopolyynes (HC3N and HC5N) are higher and that of CCS is lower in high-mass protostars, compared to low-mass protostars. We discuss a possible interpretation for these differences.
Type Ib/Ic Supernovae: Effect of Nickel Mixing on the Early-time Color Evolution and Implications for the Progenitors
Authors: Yoon Sung-Chul , Chun Wonseok , Tolstov Alexey , Blinnikov Sergey , Dessart Luc 
Published: February 2019

Abstract
We investigate the effect of mixing of radioactive nickel (56Ni) on the early-time color evolution of Type Ib and Ic supernovae (SNe Ib/Ic) using multigroup radiation hydrodynamics simulations. We consider both helium-rich and helium-poor progenitors. Mixing of 56Ni is parameterized using a Gaussian distribution function. We find that the early-time color evolution with a weak 56Ni mixing is characterized by three different phases: initial rapid reddening, blueward evolution due to the delayed effect of 56Ni heating, and redward evolution thereafter until the transition to the nebular phase. With a strong 56Ni mixing, the color evolution is characterized by a monotonic reddening. We compare our models with the early-time color evolution of several SNe Ib/Ic (SN 1999ex, SN 2008D, SN 2009jf, iPTF13bvn, SN 1994I, SN 2007gr, SN 2013ge, and 2017ein) and find signatures of relatively weak and strong 56Ni mixing for SNe Ib and SNe Ic, respectively. This suggests that SNe Ib progenitors are distinct from SN Ic progenitors in terms of helium content and that 56Ni mixing is generally stronger in the carbon–oxygen core and weaker in the helium-rich envelope. We conclude that the early-time color evolution is a powerful probe of 56Ni mixing in SNe Ib/Ic.
Sharp Gap Edges in Dense Planetary Rings: An Axisymmetric Diffusion Model
Authors: Grätz Fabio , Seiß Martin , Schmidt Jürgen , Colwell Joshua , Spahn Frank 
Published: February 2019

Abstract
One of the most intriguing facets of Saturn’s rings are the sharp edges of gaps in the rings where the surface density abruptly drops to zero. This is despite of the fact that the range over which a moon transfers angular momentum onto the ring material is much larger. Recent UVIS-scans of the edges of the Encke and Keeler gap show that this drop occurs over a range approximately equal to the rings’ thickness. Borderies et al. show that this striking feature is likely related to the local reversal of the usually outward directed viscous transport of angular momentum in strongly perturbed regions. In this article we revise the Borderies et al. model using a granular flow model to define the shear and bulk viscosities, ν and ζ, and incorporate the angular momentum flux reversal effect into the axisymmetric diffusion model we developed for gaps in dense planetary rings. Finally, we apply our model to the Encke and Keeler division in order to estimate the shear and bulk viscosities in the vicinity of both gaps.
The Streams of the Gaping Abyss: A Population of Entangled Stellar Streams Surrounding the Inner Galaxy
Authors: Ibata Rodrigo A. , Malhan Khyati , Martin Nicolas F. 
Published: February 2019

Abstract
We present the discovery of a large population of stellar streams that surround the inner Galaxy, found in the Gaia DR2 catalog using the new STREAMFINDER algorithm. Here we focus on the properties of eight new high-significance structures found at heliocentric distances between 1 and 10 kpc and at Galactic latitudes

, named Slidr, Sylgr, Ylgr, Fimbulthul, Svöl, Fjörm, Gjöll, and Leiptr. Spectroscopic measurements of seven of the streams confirm the detections, which are based on Gaia astrometry and photometry alone, and show that these streams are predominantly metal-poor. The sample possesses diverse orbital properties, although most of the streams appear to be debris of inner-halo globular clusters. Many more candidate streams are visible in our maps but require follow-up spectroscopy to confirm their nature. We also explain in detail the workings of the algorithm and gauge the incidence of false detections by running the algorithm on a smooth model of the Gaia catalog.
Weighing Black Holes Using Tidal Disruption Events
Authors: Mockler Brenna , Guillochon James , Ramirez-Ruiz Enrico 
Published: February 2019

Abstract
While once rare, observations of stars being tidally disrupted by supermassive black holes are quickly becoming commonplace. To continue to learn from these events, it is necessary to robustly and systematically compare our growing number of observations with theory. We present a tidal disruption module for the Modular Open Source Fitter for Transients (MOSFiT) and the results from fitting 14 tidal disruption events (TDEs). Our model uses FLASH simulations of TDEs to generate bolometric luminosities and passes these luminosities through viscosity and reprocessing transformation functions to create multiwavelength light curves. It then uses an MCMC fitting routine to compare these theoretical light curves with observations. We find that none of the events show evidence for viscous delays exceeding a few days, supporting the theory that our current observing strategies in the optical/UV are missing a significant number of viscously delayed flares. We find that the events have black hole masses of 106–108
M
⊙ and that the masses we predict are as reliable as those based on bulk galaxy properties. We also find that there is a preference for stars with mass <1 M
⊙, as expected when low-mass stars greatly outnumber high-mass stars.
Star Formation Rates of Massive Molecular Clouds in the Central Molecular Zone
Authors: Lu 吕 Xing 行 , Zhang Qizhou , Kauffmann Jens , Pillai Thushara , Ginsburg Adam , Mills Elisabeth A. C. , Diederik Kruijssen J. M. , Longmore Steven N. , Battersby Cara , Baobab Liu Hauyu , Gu Qiusheng 
Published: February 2019

Abstract
We investigate star formation at very early evolutionary phases in five massive clouds in the inner 500 pc of the Galaxy, the Central Molecular Zone (CMZ). Using interferometer observations of H2O masers and ultra-compact H ii regions, we find evidence of ongoing star formation embedded in cores of 0.2 pc scales and ≳105 cm−3 densities. Among the five clouds, Sgr C possesses a high (9%) fraction of gas mass in gravitationally bound and/or protostellar cores, and follows the dense (≳104 cm−3) gas star formation relation that is extrapolated from nearby clouds. The other four clouds have less than 1% of their cloud masses in gravitationally bound and/or protostellar cores, and star formation rates 10 times lower than predicted by the dense gas star formation relation. At the spatial scale of these cores, the star formation efficiency is comparable to that in Galactic disk sources. We suggest that the overall inactive star formation in these CMZ clouds could be because there is much less gas confined in gravitationally bound cores, which may be a result of the strong turbulence in this region and/or the very early evolutionary stage of the clouds when collapse has only recently started.
General Physical Properties of Gamma-Ray-emitting Narrow-line Seyfert 1 Galaxies
Authors: Paliya Vaidehi S. , Parker M. L. , Jiang J. , Fabian A. C. , Brenneman L. , Ajello M. , Hartmann D. 
Published: February 2019

Abstract
We present the results of a detailed multiwavelength study of a sample of 16 narrow-line Seyfert 1 (NLSy1) galaxies known in γ-rays so far. This includes a focused X-ray spectral analysis, to compare them with a more general NLSy1 population, and a broadband spectral energy distribution (SED) modeling considering the leptonic radiative processes to understand their similarity/dissimilarity with blazars. The X-ray spectra of γ-NLSy1 galaxies exhibit similarities to both typical NLSy1 sources below ≲2 keV and blazars at higher energies. We also find weak evidences of excess absorption in the soft X-ray spectra of three sources and a tentative detection of the Fe line in 1H 0323+342. A comparison of the broadband parameters derived from the SED modeling reveals the similarity of γ-NLSy1 objects to blazars, in particular to flat-spectrum radio quasars. The γ-NLS1 galaxies host relatively low power jets with small bulk Lorentz factors with respect to blazars, and this explains the paucity of such sources in the γ-ray catalogs and identification of even fewer parent population members. Many of the observed features of these intriguing objects suggest that they host low-mass black holes. The accretion rate in Eddington units can be considered as the driving factor to explain the physical properties of γ-NLSy1 sources, similar to that which is known for the general blazar population.
The NANOGrav 11 yr Data Set: Solar Wind Sounding through Pulsar Timing
Authors: Madison D. R. , Cordes J. M. , Arzoumanian Z. , Chatterjee S. , Crowter K. , DeCesar M. E. , Demorest P. B. , Dolch T. , Ellis J. A. , Ferdman R. D. , Ferrara E. C. , Fonseca E. , Gentile P. A. , Jones G. , Jones M. L. , Lam M. T. , Levin L. , Lorimer D. R. , Lynch R. S. , McLaughlin M. A. , Mingarelli C. M. F. , Ng C. , Nice D. J. , Pennucci T. T. , Ransom S. M. , Ray P. S. , Spiewak R. , Stairs I. H. , Stovall K. , Swiggum J. K. , Zhu W. W. 
Published: February 2019

Abstract
The North American Nanohertz Observatory for Gravitational Waves (NANOGrav) has observed dozens of millisecond pulsars for over a decade. We have accrued a large collection of dispersion measure (DM) measurements sensitive to the total electron content between Earth and the pulsars at each observation. All lines of sight cross through the solar wind (SW), which produces correlated DM fluctuations in all pulsars. We develop and apply techniques for extracting the imprint of the SW from the full collection of DM measurements in the recently released NANOGrav 11 yr data set. We filter out long-timescale DM fluctuations attributable to structure in the interstellar medium and carry out a simultaneous analysis of all pulsars in our sample that can differentiate the correlated signature of the wind from signals unique to individual lines of sight. When treating the SW as spherically symmetric and constant in time, we find the electron number density at 1 au to be 7.9 ± 0.2 cm−3. We find our data to be insensitive to long-term variation in the density of the wind. We argue that our techniques paired with a high-cadence, low-radio-frequency observing campaign of near-ecliptic pulsars would be capable of mapping out large-scale latitudinal structure in the wind.
MACER Improved: AGN Feedback Computed in Rotating Early-type Galaxies at High Resolution
Authors: Gan Zhaoming , Ciotti Luca , Ostriker Jeremiah P. , Yuan Feng 
Published: February 2019

Abstract
Based on our previous modeling of active galactic nucleus (AGN) feedback in isolated elliptical galaxies using the MACER (Massive AGN Controlled Ellipticals Resolved) code, we extend and improve the model to include rotation, to facilitate angular momentum transfer via the Toomre instability in gaseous disks, to limit the star formation to regions of high density and low temperature, and to improve the treatment of hot-mode (low accretion rate) AGN feedback. The model galaxy now has an extended dark matter profile that matches with standard observations, but it has a resolution of parsecs in the inner region and resolves the Bondi radius. We find that the results agree reasonably well with a panoply of observations: (1) Both AGN activity and star formation are primarily in central cold gaseous disks, are bursty, and are mainly driven by the Toomre instability. (2) The AGN duty cycle agrees well with the Soltan argument, i.e., the AGN spends most of its lifetime when it is in low luminosity (half of the time with

), while emitting most of its energy when it is in high luminosity (half of radiant energy emitted with L/L
Edd > 0.06). (3) The total star formation is roughly a few percent of the initial stellar mass, occurring in the bursts that would be associated with the observed E+A phenomenon. Most of the star formation occurs in a circumnuclear disk of size ≤1 kpc, which is in agreement with recent observations. (4) The interstellar medium X-ray luminosity varies within a reasonable range (median

erg s−1), in agreement with observations.
Ionization Profiles of Galactic H ii Regions
Authors: Luisi Matteo , Anderson L. D. , Liu Bin , Roshi D. Anish , Churchwell Ed 
Published: February 2019

Abstract
Using Green Bank Telescope radio recombination line (RRL) data, we analyze the role of leaking radiation from H ii regions in maintaining the ionization of the interstellar medium (ISM). We observed a sample of eight Galactic H ii regions of various sizes, morphologies, and luminosities. For each region, the hydrogen RRL intensity decreases roughly as a power-law with the distance from the center of the region. This suggests that radiation leaking from the H ii region is responsible for the majority of surrounding ionized gas producing RRL emission. Our results further indicate that the hydrogen RRL intensity appears to be fundamentally related to the H ii region sizes traced by their photodissociation regions, such that physically smaller H ii regions show a steeper decrease in intensity with an increasing distance from the region centers. As a result, giant H ii regions may have a much larger effect in maintaining the ionization of the ISM. For six of the eight observed H ii regions, we find a decrease in the 4He+/H+ abundance ratio with an increasing distance, indicating that He-ionizing photons are being absorbed within the ionization front of the H ii region. There is enhanced carbon RRL emission toward directions with strong continuum background, suggesting that the carbon emission is amplified by stimulated emission.
The Single Nucleotide Polymorphism Mal-D96N Mice Provide New Insights into Functionality of Mal in TLR Immune Responses
Authors: Dowling Jennifer K. , Tate Michelle D. , Rosli Sarah , Bourke Nollaig M. , Bitto Natalie , Lauterbach Mario A. , Cheung Shane , Ve Thomas , Kobe Bostjan , Golenbock Douglas , Mansell Ashley 
Published: February 2019

Abstract
MyD88 adaptor-like (Mal) protein is the most polymorphic of the four key adaptor proteins involved in TLR signaling. TLRs play a critical role in the recognition and immune response to pathogens through activation of the prototypic inflammatory transcription factor NF-κB. The study of single nucleotide polymorphisms in TLRs, adaptors, and signaling mediators has provided key insights into the function of the corresponding genes but also into the susceptibility to infectious diseases in humans. In this study, we have analyzed the immune response of mice carrying the human Mal-D96N genetic variation that has previously been proposed to confer protection against septic shock. We have found that Mal-D96N macrophages display reduced cytokine expression in response to TLR4 and TLR2 ligand challenge. Mal-D96N macrophages also display reduced MAPK activation, NF-κB transactivation, and delayed NF-κB nuclear translocation, presumably via delayed kinetics of Mal interaction with MyD88 following LPS stimulation. Importantly, Mal-D96N genetic variation confers a physiological protective phenotype to in vivo models of LPS-, Escherichia coli–, and influenza A virus–induced hyperinflammatory disease in a gene dosage-dependent manner. Together, these results highlight the critical role Mal plays in regulating optimal TLR-induced inflammatory signaling pathways and suggest the potential therapeutic advantages of targeting the Mal D96 signaling nexus.
Aliphatic carbonyl compounds (C8–C26) in wintertime atmospheric aerosol in London, UK
Authors: Lyu Ruihe , Alam Mohammed S. , Stark Christopher , Xu Ruixin , Shi Zongbo , Feng Yinchang , Harrison Roy M. 
Published: February 2019

Abstract. Three groups of aliphatic carbonyl compounds, the n-alkanals
(C8–C20), n-alkan-2-ones (C8–C26), and
n-alkan-3-ones (C8–C19), were measured in both particulate
and vapour phases in air samples collected in London from January to
April 2017. Four sites were sampled including two rooftop background sites,
one ground-level urban background site, and a street canyon location on
Marylebone Road in central London. The n-alkanals showed the highest
concentrations, followed by the n-alkan-2-ones and the n-alkan-3-ones, the
latter having appreciably lower concentrations. It seems likely that all
compound groups have both primary and secondary sources and these are
considered in light of published laboratory work on the oxidation
products of high-molecular-weight n-alkanes. All compound groups show
a relatively low correlation with black carbon and NOx in the
background air of London, but in street canyon air heavily impacted by
vehicle emissions, stronger correlations emerge, especially for the
n-alkanals. It appears that vehicle exhaust is likely to be a major
contributor for concentrations of the n-alkanals, whereas it is a much smaller
contributor to the n-alkan-2-ones and n-alkan-3-ones. Other primary sources
such as cooking or wood burning may be contributors for the ketones but were
not directly evaluated. It seems likely that there is also a significant
contribution from the photo-oxidation of n-alkanes and this would be consistent
with the much higher abundance of n-alkan-2-ones relative to
n-alkan-3-ones if the formation mechanism were through the oxidation of
condensed-phase alkanes. Vapour–particle partitioning fitted the Pankow model
well for the n-alkan-2-ones but less well for the other compound groups,
although somewhat stronger relationships were seen at the Marylebone Road
site than at the background sites. The former observation gives support to
the n-alkane-2-ones being a predominantly secondary product, whereas primary
sources of the other groups are more prominent.
Remineralization rate of terrestrial DOC as inferred from CO2 supersaturated coastal waters
Authors: Fransner Filippa , Fransson Agneta , Humborg Christoph , Gustafsson Erik , Tedesco Letizia , Hordoir Robinson , Nycander Jonas 
Published: February 2019

Abstract. Coastal
seas receive large amounts of terrestrially derived organic carbon (OC). The
fate of this carbon, and its impact on the marine environment, is however
poorly understood. Here we combine underway CO2 partial pressure
(pCO2) measurements with coupled 3-D
hydrodynamical–biogeochemical modelling to investigate whether
remineralization of terrestrial dissolved organic carbon (tDOC) can explain
CO2 supersaturated surface waters in the Gulf of Bothnia, a subarctic
estuary. We find that a substantial remineralization of tDOC and a strong
tDOC-induced light attenuation dampening the primary production are required
to reproduce the observed CO2 supersaturated waters in the nearshore
areas. A removal rate of tDOC of the order of 1 year, estimated in a
previous modelling study in the same area, gives a good agreement between
modelled and observed pCO2. The remineralization rate is on
the same order as bacterial degradation rates calculated from published
incubation experiments, suggesting that bacteria has the potential to cause
this degradation. Furthermore, the observed high pCO2 values
during the ice-covered season argue against photochemical degradation as the
main removal mechanism. All of the remineralized tDOC is outgassed to the
atmosphere in the model, turning the northernmost part of the Gulf of Bothnia
into a source of CO2 to the atmosphere.