bluuebunny/crossref_metadata_2025_split huggingface dataset:
Melanoma Incidence Among Non-Hispanic Whites in All 50 US States From 2001 Through 2015
Authors: Thrift Aaron P , Gudenkauf Franciska J 
Published: July 2019

Abstract

Background
The United States has large regional variation in primary prevention campaigns for skin cancer. We collected data from all 50 states to examine changes in melanoma incidence and performed age-period-cohort analyses to describe the simultaneous effects of age, period, and cohort on incidence rates.

Methods
Annual melanoma incidence rates for non-Hispanic whites from 2001 to 2015 were extracted from the US Cancer Statistics registry. Secular trends were examined overall and by sex and state. We used joinpoint regression to compute annual percent change and average annual percent change and corresponding 95% confidence intervals (CIs). We also analyzed incidence trends by 5-year age group and birth cohort using incidence rate ratios and age-period-cohort modeling.

Results
Melanoma incidence increased from 20.7 per 100 000 (95% CI = 20.5 to 20.9) in 2001 to 28.2 per 100 000 (95% CI = 28.0 to 28.5) in 2015, increasing by 3.90% (95% CI = 2.36% to 5.48%) annually between 2001 and 2005 and 1.68% (95% CI = 1.37% to 1.99%) annually from 2005 through 2015. The average annual percent change in melanoma incidence rates were similar for men (2.34%, 95% CI = 1.91 to 2.78) and women (2.25%, 95% CI = 1.60 to 2.91). Age-specific relative risk by birth cohort increased from circa 1921 to 1981 before decreasing. Compared with adults born circa 1956, those born circa 1991 had lower melanoma risk (incidence rate ratio  = 0.85; 95% CI = 0.77 to 0.94). Geographic variation was observed; some states still have melanoma rates trending upwards in all birth cohorts.

Conclusions
The continued increase in melanoma incidence among non-Hispanic whites, particularly in states where rates continue to rise among recent and current birth cohorts, underscores the need for increased public health campaigns aimed at reducing sun exposure.
Signatures of circumstellar interaction in the unusual transient AT 2018cow
Authors: Fox Ori D , Smith Nathan 
Published: July 2019

ABSTRACT
AT 2018cow is a unique transient that stands out due to its relatively fast light curve, high peak bolometric luminosity, and blue colour. These properties distinguish it from typical radioactively powered core-collapse supernovae (SNe). Instead, the characteristics are more similar to a growing sample of Fast Blue Optical Transients (FBOTs). Mostly discovered at hundreds of Mpc, FBOT follow-up is usually limited to several photometry points and low signal-to-noise spectra. At only ∼60 Mpc, AT 2018cow offers an opportunity for detailed follow-up. Studies of this object published to date propose a number of interpretations for AT 2018cow, but none of these specifically consider the interacting Type Ibn SN subclass. We point out that while narrow lines do not dominate the spectrum of AT 2018cow, as narrow Balmer lines typically do in SNe IIn, the narrow lines in AT 2018cow may nevertheless include emission from pre-shock CSM. In particular, the He i lines in AT 2018cow are broader than H ii region lines in the same spectrum, and they closely resemble He i lines in some examples of SNe Ibn or transitional SNe Ibn/IIn objects. We compare AT 2018cow to interacting SNe Ibn and IIn and find a number of noteworthy similarities, including light-curve rise and fall times, peak magnitude, X-ray light curves, and spectroscopic properties. We therefore explore the hypothesis that CSM interaction in a relatively H-poor system might help explain some observed properties of AT 2018cow, and we go on to consider progenitor implications for AT 2018cow, FBOTs, and SNe Ibn.
Axion core–halo mass and the black hole–halo mass relation: constraints on a few parsec scales
Authors: Desjacques Vincent , Nusser Adi 
Published: July 2019

ABSTRACT
If the dark matter is made of ultralight axions, stable solitonic cores form at the centres of virialized haloes. In some range for the mass m of the axion particle, these cores are sufficiently compact and can mimic supermassive black holes (SMBH) residing at galactic nuclei. We use the solitonic core–halo mass relation, validated in numerical simulations, to constrain a new range of allowed axion mass from measurements of the SMBH mass in (pseudo)bulge and bulgeless galaxies. These limits are based on observations of galactic nuclei on scales smaller than 10 pc. Our analysis suggests that $m\lesssim 10^{-18}\, {\rm eV}$ is ruled out by the data. We briefly discuss whether an attractive self-interaction among axions could alleviate this constraint.
X-ray study of spatial structures in Tycho’s supernova remnant using unsupervised deep learning
Authors: Iwasaki Hiroyoshi , Ichinohe Yuto , Uchiyama Yasunobu 
Published: July 2019

ABSTRACT
Recent rapid development of deep learning algorithms, which can implicitly capture structures in high-dimensional data, opens a new chapter in astronomical data analysis. We report here a new implementation of deep learning techniques for X-ray analysis. We apply a variational autoencoder (VAE) using a deep neural network for spatio-spectral analysis of data obtained by Chandra X-ray Observatory from Tycho’s supernova remnant (SNR). We established an unsupervised learning method combining the VAE and a Gaussian mixture model (GMM), where the dimensions of the observed spectral data are reduced by the VAE, and clustering in feature space is performed by the GMM. We found that some characteristic spatial structures, such as the iron knot on the eastern rim, can be automatically recognized by this method, which uses only spectral properties. This result shows that unsupervised machine learning can be useful for extracting characteristic spatial structures from spectral information in observational data (without detailed spectral analysis), which would reduce human-intensive preprocessing costs for understanding fine structures in diffuse astronomical objects, e.g. SNRs or galaxy clusters. Such data-driven analysis can be used to select regions from which to extract spectra for detailed analysis and help us make the best use of the large amount of spectral data available currently and arriving in the coming decades.
Swift UVOT observations of the 2015 outburst of V404 Cygni
Authors: Oates S R , Motta S , Beardmore A P , Russell D M , Gandhi P , Kuin N P M , De Pasquale M , Altamirano D , Breeveld A A , Castro-Tirado A J , Knigge C , Page M J , Steeghs D 
Published: July 2019

ABSTRACT
The black hole binary, V404 Cygni, went into outburst in 2015 June, after 26 years of X-ray quiescence. We observed the outburst with the Neil Gehrels Swift observatory. We present optical/UV observations taken with the Swift Ultra-violet Optical Telescope, and compare them with the X-ray observations obtained with the Swift X-ray Telescope. We find that dust extinction affecting the optical/UV does not correlate with absorption due to neutral hydrogen that affects the X-ray emission. We suggest there is a small inhomogeneous high-density absorber containing a negligible amount of dust, close to the black hole. Overall, temporal variations in the optical/UV appear to trace those in the X-rays. During some epochs we observe an optical time-lag of (15–35) s. For both the optical/UV and X-rays, the amplitude of the variations correlates with flux, but this correlation is less significant in the optical/UV. The variability in the light curves may be produced by a complex combination of processes. Some of the X-ray variability may be due to the presence of a local, inhomogeneous and dust-free absorber, while variability visible in both the X-ray and optical/UV may instead be driven by the accretion flow: the X-rays are produced in the inner accretion disc, some of which are reprocessed to the optical/UV; and/or the X-ray and optical/UV emission is produced within the jet.
Bondi–Hoyle–Lyttleton accretion in supergiant X-ray binaries: stability and disc formation
Authors: Xu Wenrui , Stone James M 
Published: July 2019

Abstract
We use 2D (axisymmetric) and 3D hydrodynamic simulations to study Bondi–Hoyle–Lyttleton accretion with and without transverse upstream gradients. We mainly focus on the regime of high (upstream) Mach number, weak upstream gradients, and small accretor size, which is relevant to neutron star accretion in wind-fed supergiant X-ray binaries (SgXBs). We present a systematic exploration of the flow in this regime. When there are no upstream gradients, the flow is always stable regardless of accretor size or Mach number. For finite upstream gradients, there are three main types of behaviour: stable flow (small upstream gradient), turbulent unstable flow without a disc (intermediate upstream gradient), and turbulent flow with a disc-like structure (relatively large upstream gradient). When the accretion flow is turbulent, the accretion rate decreases non-convergently as the accretor size decreases. The flow is more prone to instability and the disc is less likely to form than previously expected; the parameters of most observed SgXBs place them in the regime of a turbulent, disc-less accretion flow. Among the SgXBs with relatively well-determined parameters, we find OAO 1657−415 to be the only one that is likely to host a persistent disc (or disc-like structure); this finding is consistent with observations.
Constraining the initial planetary population in the gravitational instability model
Authors: Humphries J , Vazan A , Bonavita M , Helled R , Nayakshin S 
Published: July 2019

ABSTRACT
Direct imaging (DI) surveys suggest that gas giants beyond 20 au are rare around FGK stars. However, it is not clear what this means for the formation frequency of gravitational instability (GI) protoplanets due to uncertainties in gap opening and migration efficiency. Here we combine state-of-the-art calculations of homogeneous planet contraction with a population synthesis code. We find DI constraints to be satisfied if protoplanet formation by GI occurs in tens of per cent of systems if protoplanets ‘supermigrate’ to small separations. In contrast, GI may occur in only a few per cent of systems if protoplanets remain stranded at wide orbits because their migration is ‘quenched’ by efficient gap opening. We then use the frequency of massive giants in radial velocity surveys inside 5 au to break this degeneracy – observations recently showed that this population does not correlate with the host star metallicity and is therefore suspected to have formed via GI followed by inward migration. We find that only the supermigration scenario can sufficiently explain this population while simultaneously satisfying the DI constraints and producing the right mass spectrum of planets inside 5 au. If massive gas giants inside 5 au formed via GI, then our models imply that migration must be efficient and that the formation of GI protoplanets occurs in at least tens of per cent of systems.
The luminosity function and formation rate of a complete sample of long gamma-ray bursts
Authors: Lan Guang-Xuan , Zeng Hou-Dun , Wei Jun-Jie , Wu Xue-Feng 
Published: July 2019

ABSTRACT
We study the luminosity function and formation rate of long gamma-ray bursts (GRBs) by using a maximum likelihood method. This is the first time this method is applied to a well-defined sample of GRBs that is complete in redshift. The sample is composed of 99 bursts detected by the Swift satellite, 81 of them with measured redshift and luminosity for a completeness level of $82\, {\rm per\, cent}$. We confirm that a strong redshift evolution in luminosity (with an evolution index of $\delta =2.22^{+0.32}_{-0.31}$) or in density ($\delta =1.92^{+0.20}_{-0.21}$) is needed in order to reproduce the observations well. But since the predicted redshift and luminosity distributions in the two scenarios are very similar, it is difficult to distinguish between these two kinds of evolutions only on the basis of the current sample. Furthermore, we also consider an empirical density case in which the GRB rate density is directly described as a broken power-law function and the luminosity function is taken to be non-evolving. In this case, we find that the GRB formation rate rises like $(1+z)^{3.85^{+0.48}_{-0.45}}$ for $z\lesssim 2$ and is proportional to $(1+z)^{-1.07^{+0.98}_{-1.12}}$ for $z\gtrsim 2$. The local GRB rate is $1.49^{+0.63}_{-0.64}$ Gpc−3 yr−1. The GRB rate may be consistent with the cosmic star formation rate (SFR) at $z\lesssim 2$, but shows an enhancement compared to the SFR at $z\gtrsim 2$.
Bolometric correction factors for active galactic nuclei
Authors: Netzer Hagai 
Published: July 2019

ABSTRACT
The bolometric luminosity of active galactic nuclei (AGNs) is difficult to determine, and various approximations have been used to calibrate it against different observed properties. Here, I combine theoretical calculations of optically thick, geometrically thin accretion discs, and observed X-ray properties of AGN, to provide new bolometric correction factors (kBOL) over a large range of black hole (BH) mass, accretion rate, and spin. This is particularly important in cases where the mass accretion rate cannot be determined from the observed spectral energy distribution, and in cases where luminosity-independent correction factors have been used. Simple power-law approximations of kBOL are provided for L(5100 Å), L(3000 Å), L(1400 Å), L(2–10 keV), and L(narrow Hβ). In all cases, the uncertainties are large mostly due to the unknown BH spin. Prior knowledge of the BH mass reduces the uncertainty considerably.
Pseudo-evolution of galaxies in Λ CDM cosmology
Authors: Balakrishna Subramani Vasanth , Kroupa Pavel , Shenavar Hossein , Muralidhara Vyoma 
Published: July 2019

ABSTRACT
Our knowledge about galaxy evolution comes from transforming observed galaxy properties at different redshifts to comoving physical scales. This transformation depends on using a cosmological model. Here, the effects of unintentional mixing of two different cosmological models on the size evolution of galaxies is studied. As a gedanken experiment, a galaxy of fixed proper size and luminosity is moved across different redshifts. The apparent size of this galaxy is then interpreted with a cosmological model presumed by the observer, which is different compared to the cosmology exhibited by the Universe. In such a case, a spurious size evolution of the galaxy is observed. A galaxy behaving according to the Rh = ct and Neumann’s cosmology, when interpreted with the Λ cold dark matter (ΛCDM) cosmological model, shows an increase in size by a factor of 1.1 and 1.3 from $z$ = 7.5 to ≈ 0, respectively. The apparent size of a galaxy in a static Euclidean cosmology, when interpreted in the ΛCDM model, shows a factor of 23.8 increase in size between $z$ = 7.5 to ≈ 0. This is in close agreement with the observational data with a size increase of a factor of 6.8 between $z$ = 3.2 to ≈ 0. Furthermore, using the apparent size data, it is shown that the difference between the derived proper sizes in Rh = ct, Neumann’s and ΛCDM cosmological models are minimal.
An accurate low-redshift measurement of the cosmic neutral hydrogen density
Authors: Hu Wenkai , Hoppmann Laura , Staveley-Smith Lister , Geréb Katinka , Oosterloo Tom , Morganti Raffaella , Catinella Barbara , Cortese Luca , Lagos Claudia del P , Meyer Martin 
Published: July 2019

ABSTRACT
Using a spectral stacking technique, we measure the neutral hydrogen (H i) properties of a sample of galaxies at z < 0.11 across 35 pointings of the Westerbork Synthesis Radio Telescope. The radio data contain 1895 galaxies with redshifts and positions known from the Sloan Digital Sky Survey. We carefully quantified the effects of sample bias, aperture used to extract spectra, sidelobes and weighting technique and use our data to provide a new estimate for the cosmic H i mass density. We find a cosmic H i mass density of $\Omega _{\rm H\,{\small I}} = (4.02 \pm 0.26)\times 10^{-4} h_{70}^{-1}$ at 〈z〉 = 0.066, consistent with measurements from blind H i surveys and other H i stacking experiments at low redshifts. The combination of the small interferometer beam size and the large survey volume makes our result highly robust against systematic effects due to confusion at small scales and cosmic variance at large scales. Splitting into three sub-samples with 〈z〉 = 0.038, 0.067, and 0.093 shows no significant evolution of the H i gas content at low redshift.
Energy of a quantum Coulomb liquid
Authors: Baiko D A 
Published: July 2019

ABSTRACT
Using the Metropolis method to compute path integrals, the energy of a quantum strongly coupled Coulomb liquid (1 ≤ Γ ≤ 175), composed of distinguishable atomic nuclei and a uniform incompressible electron background, is calculated from first principles. The range of temperatures and densities considered represents fully ionized layers of white dwarfs and neutron stars. In particular, the results allow one to determine reliably the heat capacity of ions in dense fluid stellar matter, which is a crucial ingredient for modelling the thermal evolution of compact degenerate stars.
Effects of infall and outflow on massive star-forming regions
Authors: Li Qiang , Zhou Jianjun , Esimbek Jarken , He Yuxin , Baan Willem , Li Dalei , Wu Gang , Tang Xindi , Ji Weiguang , Komesh Toktarkhan , Sailanbek Serikbek 
Published: July 2019

ABSTRACT
A total of 188 high-mass outflows have been identified from a sample of 694 clumps from the Millimetre Astronomy Legacy Team 90 GHz survey, representing a detection rate of approximately 27 per cent. The detection rate of outflows increases from the proto-stellar stage to the H ii stage, but decreases again at the photodissociation (PDR) stage suggesting that outflows are being switched off during the PDR stage. An intimate relationship is found between outflow action and the presence of masers, and water masers appear together with 6.7 GHz methanol masers. Comparing the infall detection rate of clumps with and without outflows, we find that outflow candidates have a lower infall detection rate. Finally, we find that outflow action has some influence on the local environment and the clump itself, and this influence decreases with increasing evolutionary time as the outflow action ceases.
Molecular envelope around the HII region RCW 120
Authors: Kirsanova M S , Pavlyuchenkov Ya N , Wiebe D S , Boley P A , Salii S V , Kalenskii S V , Sobolev A M , Anderson L D 
Published: July 2019

ABSTRACT
The H ii region RCW 120 is a well-known object, which is often considered as a target to verify theoretical models of gas and dust dynamics in the interstellar medium. However, the exact geometry of RCW 120 is still a matter of debate. In this work, we analyse observational data on molecular emission in RCW 120 and show that 13CO(2–1) and C18O(2–1) lines are fitted by a 2D model representing a ring-like face-on structure. The changing of the C18O(3–2) line profile from double-peaked to single-peaked from the dense molecular Condensation 1 might be a signature of stalled expansion in this direction. In order to explain a self-absorption dip of the 13CO(2–1) and 13CO(3–2) lines, we suggest that RCW 120 is surrounded by a diffuse molecular cloud, and find confirmation of this cloud on a map of interstellar extinction. Optically thick 13CO(2–1) emission and the infrared 8 $\mu$m PAH band form a neutral envelope of the H ii region resembling a ring, while the envelope breaks into separate clumps on images made with optically thin C18O(2–1) line and far-infrared dust emission.
Population Gene Introgression and High Genome Plasticity for the Zoonotic Pathogen Streptococcus agalactiae
Authors: Richards Vincent P , Velsko Irina M , Alam Md Tauqeer , Zadoks Ruth N , Manning Shannon D , Pavinski Bitar Paulina D , Hassler Hayley B , Crestani Chiara , Springer Garrett H , Probert Brett M , Town Christopher D , Stanhope Michael J 
Published: July 2019

AbstractThe influence that bacterial adaptation (or niche partitioning) within species has on gene spillover and transmission among bacterial populations occupying different niches is not well understood. Streptococcus agalactiae is an important bacterial pathogen that has a taxonomically diverse host range making it an excellent model system to study these processes. Here, we analyze a global set of 901 genome sequences from nine diverse host species to advance our understanding of these processes. Bayesian clustering analysis delineated 12 major populations that closely aligned with niches. Comparative genomics revealed extensive gene gain/loss among populations and a large pan genome of 9,527 genes, which remained open and was strongly partitioned among niches. As a result, the biochemical characteristics of 11 populations were highly distinctive (significantly enriched). Positive selection was detected and biochemical characteristics of the dispensable genes under selection were enriched in ten populations. Despite the strong gene partitioning, phylogenomics detected gene spillover. In particular, tetracycline resistance (which likely evolved in the human-associated population) from humans to bovine, canines, seals, and fish, demonstrating how a gene selected in one host can ultimately be transmitted into another, and biased transmission from humans to bovines was confirmed with a Bayesian migration analysis. Our findings show high bacterial genome plasticity acting in balance with selection pressure from distinct functional requirements of niches that is associated with an extensive and highly partitioned dispensable genome, likely facilitating continued and expansive adaptation.
Utility of a Quantitative Approach Using Diffusion Tensor Imaging for Prognostication Regarding Motor and Functional Outcomes in Patients With Surgically Resected Deep Intracranial Cavernous Malformations
Authors: Abhinav Kumar , Nielsen Troels H , Singh Rhea , Weng Yingjie , Han Summer S , Iv Michael , Steinberg Gary K 
Published: July 2019

Abstract

BACKGROUND
Resection of deep intracranial cavernous malformations (CMs) is associated with a higher risk of neurological deterioration and uncertainty regarding clinical outcomes.

OBJECTIVE
To examine diffusion tractography imaging (DTI) data evaluating the corticospinal tract (CST) in relation to motor and functional outcomes in patients with surgically resected deep CMs.

METHODS
Perilesional CST was characterized as disrupted, displaced, or normal. Mean fractional anisotropy (FA) values were obtained for whole ipsilateral CST and in 3 regions: subcortical (proximal), perilesional, and distally. Mean FA values in anatomically equivalent regions in the contralateral CST were obtained. Clinical and radiological data were collected independently. Multivariable regression analysis was used for statistical analysis.

RESULTS
A total of 18 patients [brainstem (15) and thalamus/basal ganglia (3); median follow-up: 270 d] were identified over 2 yr. The CST was identified preoperatively as disrupted (6), displaced (8), and normal (4). Five of 6 patients with disruption had weakness. Higher preoperative mean FA values for distal ipsilateral CST segment were associated with better preoperative lower (P < .001), upper limb (P = .004), postoperative lower (P = .005), and upper limb (P < .001) motor examination. Preoperative mean FA values for distal ipsilateral CST segment (P = .001) and contralateral perilesional CST segment (P < .001) were negatively associated with postoperative modified Rankin scale scores.

CONCLUSION
Lower preoperative mean FA values for overall and defined CST segments corresponded to worse patient pre- and postoperative motor examination and/or functional status. FA value for the distal ipsilateral CST segment has prognostic potential with respect to clinical outcomes.