bluuebunny/crossref_metadata_2025_split huggingface dataset:
A MicroRNA Expression Signature as Prognostic Marker for Oropharyngeal Squamous Cell Carcinoma
Authors: Liu Xinyi , Liu Ping , Chernock Rebecca D , Yang Zhenming , Lang Kuhs Krystle A , Lewis James S. , Luo Jingqin , Li Hua , Gay Hiram A , Thorstad Wade L , Wang Xiaowei 
Published: September 2020

Abstract

Background
Improved prognostication of oropharyngeal squamous cell carcinoma (OPSCC) may facilitate individualized patient management. The goal of this study was to develop and validate a prognostic signature based on microRNA sequencing (miRNA-seq) analysis.

Methods
We collected tumor specimens for miRNA-seq analysis from OPSCC patients treated at Washington University in St Louis (n = 324) and Vanderbilt University (n = 130). OPSCC patients (n = 79) from The Cancer Genome Atlas Program were also included for independent validation. Univariate and multivariable Cox regression analyses were performed to identify miRNAs associated with disease outcomes. All statistical tests were 2-sided.

Results
By miRNA-seq profiling analysis, we identified a 26-miRNA signature. Based on computed risk scores of the signature, we classified the patients into low- and high-risk groups. In the training cohort, the high-risk group had much shorter overall survival compared with the low-risk group (hazard ratio [HR] = 3.80, 95% confidence interval [CI] = 2.37 to 6.10, P &lt; .001). Subgroup analysis further revealed that the signature was prognostic for HPV-positive OPSCCs (HR = 3.07, 95% CI = 1.65 to 5.71, P &lt; .001). Multivariable analysis indicated that the signature was independent of common clinicopathologic factors for OPSCCs. Importantly, the miRNA signature was a statistically significant predictor of overall survival in independent validation cohorts (The Cancer Genome Atlas Program cohort: HR = 6.05, 95% CI = 2.10 to 17.37, P &lt; .001; Vanderbilt cohort: HR = 7.98, 95% CI = 3.99 to 15.97, P &lt; .001; Vanderbilt HPV-positive cohort: HR = 8.71, 95% CI = 2.70 to 28.14, P &lt; .001).

Conclusions
The miRNA signature is a robust and independent prognostic tool for risk stratification of OPSCCs including HPV-positive OPSCCs.
Capacity of proton beams in preserving normal liver tissue during proton beam therapy for hepatocellular carcinoma
Authors: Tsai Yu-Lun , Takei Hideyuki , Iizumi Takashi , Okumura Toshiyuki , Sekino Yuta , Numajiri Haruko , Ishikawa Hitoshi , Sakae Takeji , Sakurai Hideyuki 
Published: September 2020

Abstract
Unirradiated liver volume (ULV) preservation rate is an important factor associated with radiation-induced liver disease (RILD) in patients with hepatocellular carcinoma (HCC) undergoing proton beam therapy (PBT). The purpose of this study is to identify the predictors for ULV preservation and quantify the capacity of proton beams in normal liver sparing during PBT. We reviewed planning data of 92 patients with single intrahepatic HCC tumors undergoing PBT. The potential clinical and planning factors that may affect ULV preservation were involved in multiple linear regression for ULV preservation rate. The significant factors were determined to be predictors and their influences were quantified. The median ULV preservation rate was 62.08%. All the assessed clinical factors showed significant effects on ULV preservation rate: clinical target volume (CTV), P &lt; 0.001; portal vein tumor thrombosis (PVTT), P = 0.010; left lobe tumor, P = 0.010. In contrast, none of the planning factors demonstrated significance. The coefficients of significant factors in multiple linear regression were 60.85 for intercept, −0.02 for CTV, −9.01 for PVTT and 8.31 for left lobe tumors. The capacity of proton beams to spare normal liver tissue during PBT for HCC is mainly affected by clinical factors. The baseline of the ULV preservation rate is 60.85%, decreasing 0.02% with each milliliter of CTV increase and 9.01% for tumors with PVTT, and increasing 8.31% for tumors limited to the left lobe. Further clinical studies should be carried out to correlate our dosimetric findings with clinical outcomes.
Robot-assisted resection of GIST in the proximal jejunum
Authors: Oh Myeong Hun , Lee Byoung Chul 
Published: September 2020

Abstract
Gastrointestinal stromal tumors (GISTs) are rare. Although most commonly found in the stomach, GISTs in the jejunum are among the rarest subtypes. A 46-year-old woman presented to the surgical department with proximal jejunal mass found in the examinations after abdominal pain and melena. Computed tomography imaging showed a 2.3 cm sized well-defined heterogenous enhancing mass in the proximal jejunum, and GIST was strongly suspected. The jejunal mass was identified 5 cm below the ligament of Treitz intraoperatively. She underwent robotic-assisted jejunal resection with intracorporeal robot-sewn anastomosis. The patient’s postoperative course was uneventful, and she was discharged on the seventh postoperative day. A robotic approach for GIST in the proximal jejunum is a safe and feasible procedure with good surgical outcomes.
On the relation between mini-halos and AGN feedback in clusters of galaxies
Authors: Richard-Laferrière A , Hlavacek-Larrondo J , Nemmen R S , Rhea C L , Taylor G B , Prasow-Émond M , Gendron-Marsolais M , Latulippe M , Edge A C , Fabian A C , Sanders J S , Hogan M T , Demontigny G 
Published: September 2020

ABSTRACT
A variety of large-scale diffuse radio structures have been identified in many clusters with the advent of new state-of-the-art facilities in radio astronomy. Among these diffuse radio structures, radio mini-halos are found in the central regions of cool core clusters. Their origin is still unknown and they are challenging to discover; less than 30 have been published to date. Based on new VLA observations, we confirmed the mini-halo in the massive strong cool core cluster PKS 0745−191 (z = 0.1028) and discovered one in the massive cool core cluster MACS J1447.4+0827 (z = 0.3755). Furthermore, using a detailed analysis of all known mini-halos, we explore the relation between mini-halos and active galactic nucleus (AGN) feedback processes from the central galaxy. We find evidence of strong, previously unknown correlations between mini-halo radio power and X-ray cavity power, and between mini-halo and the central galaxy radio power related to the relativistic jets when spectrally decomposing the AGN radio emission into a component for past outbursts and one for ongoing accretion. Overall, our study indicates that mini-halos are directly connected to the central AGN in clusters, following previous suppositions. We hypothesize that AGN feedback may be one of the dominant mechanisms giving rise to mini-halos by injecting energy into the intra-cluster medium and reaccelerating an old population of particles, while sloshing motion may drive the overall shape of mini-halos inside cold fronts. AGN feedback may therefore not only play a vital role in offsetting cooling in cool core clusters, but may also play a fundamental role in re-energizing non-thermal particles in clusters.
The brown dwarf population in the star-forming region NGC 2264
Authors: Pearson Samuel , Scholz Aleks , Teixeira Paula S , Mužić Koraljka , Eislöffel Jochen 
Published: September 2020

ABSTRACT
The brown dwarf population in the canonical star-forming region NGC 2264 is so far poorly explored. We present a deep, multiwavelength, multiepoch survey of the star-forming cluster NGC 2264, aimed to identify young brown dwarf candidates in this region. Using criteria including optical/near-infrared (IR) colours, variability, Spitzer mid-IR colour excess, extinction, and Gaia parallax and proper motion (in order of relevance), we select 902 faint red sources with indicators of youth. Within this sample, we identify 429 brown dwarf candidates based on their IR colours. The brown dwarf candidates are estimated to span a mass range from 0.01 to 0.08 M⊙. We find rotation periods for 44 sources, 15 of which are brown dwarf candidates, ranging from 3.6 h to 6.5 d. A subset of 38 brown dwarf candidates show high-level irregular variability indicative of ongoing disc accretion, similar to the behaviour of young stars.
The dynamics of the broad-line region in NGC 3227
Authors: Devereux Nick 
Published: September 2020

ABSTRACT
Archival Hubble Space Telescope (HST) observations of the Seyfert 1 nucleus of NGC 3227 obtained with the Space Telescope Imaging Spectrograph (STIS) are re-examined in order to constrain a viable photoionization model for the broad-line region (BLR). The results imply that the BLR is a partially ionized, dust-free, spherical shell that is collapsing, supersonically, at the free-fall velocity due to its proximity to a supermassive black hole. The BLR is ionization bounded at the outer radius, coincident with the dust reverberation radius, and transforms into an X-ray emitting plasma inside the Balmer reverberation radius as the central UV–X-ray source is approached. Only 40 M⊙ of Hydrogen are required to explain the Balmer emission-line luminosity, but it is compressed by gravity into a column measuring 5.5 × 1024 atoms cm−2. Assuming radiatively inefficient accretion, the X-ray luminosity requires ∼10−2 M⊙ yr−1. However, the mass inflow rate required to explain the luminosity of the broad H α emission line is ∼1 M⊙ yr−1. The very large disparity between these two estimates indicates that 99 per cent of the inflowing gas must be re-directed into an outflow, and on a very short time-scale corresponding to ∼40 yr. Alternatively, the radiative efficiency of the inflow has been overestimated, or the X-ray luminosity has been underestimated, a distinct possibility if the BLR is indeed Compton-thick.
Pre-selection of the candidate fields for deep imaging of the epoch of reionization with SKA1-low
Authors: Zheng Qian , Wu Xiang-Ping , Guo Quan , Johnston-Hollitt Melanie , Shan Huanyuan , Duchesne Stefan W , Li Weitian 
Published: September 2020

ABSTRACT
The Square Kilometre Array (SKA) will be the first low-frequency instrument with the capability to directly image the structures of the epoch of reionization (EoR). Indeed, deep imaging of the EoR over five targeted fields of 20 sq deg each has been selected as the highest priority science objective for SKA1. Aiming at preparing for this highly challenging observation, we perform an extensive pre-selection of the ‘quietest’ and ‘cleanest’ candidate fields in the southern sky to be suited for deep imaging of the EoR using existing catalogues and observations over a broad frequency range. The candidate fields should meet a number of strict criteria to avoid contaminations from foreground structures and sources. The candidate fields should also exhibit both the lowest average surface brightness and smallest variance to ensure uniformity and high-quality deep imaging over the fields. Our selection eventually yields a sample of 7 ‘ideal’ fields of 20 sq deg in the southern sky that could be targeted for deep imaging of the EoR. Finally, these selected fields are convolved with the synthesized beam of SKA1-low stations to ensure that the effect of sidelobes from the far-field bright sources is also weak.
Bi-directional streaming of particles accelerated at the STEREO-A shock on 2008 March 9
Authors: Fraschetti F , Giacalone J 
Published: September 2020

ABSTRACT
We present an interpretation of anisotropy and intensity of supra-thermal ions near a fast quasi-perpendicular reverse shock measured by Solar Terrestrial Relations Observatory Ahead (ST-A) on 2008 March 9. The measured intensity profiles of the supra-thermal particles exhibit an enhancement, or ‘spike’, at the time of the shock arrival and pitch-angle anisotropies before the shock arrival are bi-modal, jointly suggesting trapping of near-scatter-free ions along magnetic field lines that intersect the shock at two locations. We run test-particle simulations with pre-existing upstream magnetostatic fluctuations advected across the shock. The measured bi-modal upstream anisotropy, the nearly field-aligned anisotropies up to ∼15 min upstream of the shock, as well as the ‘pancake-like’ anisotropies up to ∼10 min downstream of the shock are well reproduced by the simulations. These results, in agreement with earlier works, suggest a dominant role of the large-scale structure (100s of supra-thermal proton gyroradii) of the magnetic field in forging the early-on particle acceleration at shocks.
Unfolding the X-ray spectral curvature of Mkn 421 for further clues
Authors: Goswami Pranjupriya , Sahayanathan Sunder , Sinha Atreyee , Gogoi Rupjyoti 
Published: September 2020

ABSTRACT
The X-ray observations of Mkn 421 show significant spectral curvature that can be reproduced by a log-parabola function. The spectra can also be fitted by an analytical model considering synchrotron emission from an electron distribution that is accelerated at a shock front with an energy-dependent diffusion (EDD model). The spectral fit of NuSTAR and Swift-XRT observations using EDD model during different flux states reveals that the model parameters are strongly correlated. We perform a detailed investigation of this correlation to decipher the information hidden underneath. The model predicts the synchrotron peak energy to be correlated with the peak spectral curvature, which is consistent with the case of Mkn 421. Expressing the energy dependence of the diffusion in terms of the magnetohydrodynamic turbulence energy index, it appears that the turbulence shifts from Kolmogorov/Kraichnan type to Bohm limit during high flux states. Further, the correlation between the best-fitting parameters of EDD model lets us derive an expression for the product of source magnetic field(B) and jet Doppler factor(δ) in terms of synchrotron and Compton peak energies. The synchrotron peak energy is obtained using the simultaneous Swift-XRT–NuSTAR observations, whereas the Compton peak energy is estimated by performing a linear regression analysis of the archival spectral peaks. The deduced δB varies over a wide range; however, it satisfies reasonably well with the values estimated solely from the spectral peak energies independent of the EDD model. This highlights the plausible connection between the microscopic description of the electron diffusion with the macroscopic quantities deciding the broad-band spectrum of Mkn 421.
The radio structure of the narrow-line Seyfert 1 Mrk 783 with VLBA and e-MERLIN
Authors: Congiu E , Kharb P , Tarchi A , Berton M , Caccianiga A , Chen S , Crepaldi L , Di Mille F , Järvelä E , Jarvis M E , La Mura G , Vietri A 
Published: September 2020

ABSTRACT
In this paper, we present the analysis of new radio and optical observations of the narrow-line Seyfert 1 galaxy Mrk 783. $1.6\, \mathrm{GHz}$ observations performed with the e-MERLIN interferometer confirm the presence of the diffuse emission previously observed. The Very Long Baseline Array (VLBA) also detects the nuclear source both at $1.6\, \mathrm{GHz}$ (L band) and $5\, \mathrm{GHz}$ (C band). While the L-band image shows only an unresolved core, the C-band image shows the presence of a partially resolved structure at a position angle of 60○. The brightness temperature of the emission in both bands (${\gt}10^6\, \mathrm{K}$) suggests that it is a pc-scale jet produced by the active galactic nucleus. The relatively steep VLBA spectral index (αVLBA = 0.63 ± 0.03) is consistent with the presence of optically thin emission on milliarcsecond scales. Finally, we investigated two possible scenarios that can result in the misalignment between the kpc and pc-scale radio structure detected in the galaxy. We also analysed the optical morphology of the galaxy, which suggests that Mrk 783 underwent a merging in relatively recent times.
Are Ly α emitters segregated in protoclusters regions?
Authors: Hough Tomás , Gurung-López Siddhartha , Orsi Álvaro , Cora Sofía A , Lacey Cedric G , Baugh Carlton M 
Published: September 2020

ABSTRACT
The presence of neutral hydrogen in the interstellar medium (ISM) and intergalactic medium (IGM) induces radiative transfer (RT) effects on $\rm {Ly}\,\alpha$ photons that affect the observability of Lyman alpha emitters (LAEs). We use the galform semi-analytic model of galaxy formation and evolution to analyse how these effects shape the spatial distribution of LAEs with respect to $\rm {H}\,\alpha$ emitters (HAEs) around high-density regions at high redshift. We find that when a large sample of protoclusters is considered, HAEs showing also $\rm {Ly}\,\alpha$ emission (HAEs + LAEs) populate the same regions as those that do not display the $\rm {Ly}\,\alpha$ line at $z$ = 2.2. We compare against the protocluster USS1558-003, one of the most massive protoclusters located at $z$ = 2.53. Our results indicate that the strong depletion of HAEs + LAEs present in the high-density regions of USS1558-003 may be due to cosmic variance. We find that at $z$ = 2.2 and $z$ = 3.0, RT of the ISM produces a strong decline (30–50 per cent) of the clustering amplitude of HAEs + LAEs with respect to HAEs towards the protoclusters centre. At $z$ = 5.7, given the early evolutionary state of protoclusters and galaxies, the clustering of HAEs + LAEs has a smaller variation (10–20 per cent) towards the protoclusters centre. Depending on the equivalent width and luminosity criteria of the emission-line galaxy sample, the IGM can have a mild or a null effect on galaxy properties and clustering in high-density regions.
Towards a realistic explosion landscape for binary population synthesis
Authors: Patton Rachel A , Sukhbold Tuguldur 
Published: September 2020

ABSTRACTA crucial ingredient in population synthesis studies involving massive stars is the determination of whether they explode or implode in the end. While the final fate of a massive star is sensitive to its core structure at the onset of collapse, the existing binary population synthesis studies do not reach core collapse. Instead, they employ simple prescriptions to infer their final fates without knowing the pre-supernova core structure. We explore a potential solution to this problem by treating the carbon-oxygen (CO) core independently from the rest of the star. Using the implicit hydrodynamics code $\mathrm{\tt {KEPLER}}$, we have computed an extensive grid of 3496 CO-core models from a diverse range of initial conditions, each evolved from carbon ignition until core collapse. The final core structure, and thus the explodability, varies non-monotonically and depends sensitively on both the mass and initial composition of the CO core. Although bare CO cores are not perfect substitutes for cores embedded in massive stars, our models compare well both with $\mathrm{\tt {MESA}}$ and full hydrogenic and helium star calculations. Our results can be used to infer the pre-supernova core structures from population synthesis estimates of CO-core properties, thus to determine the final outcomes based on the results of modern neutrino-driven explosion simulations. A sample application is presented for a population of Type-IIb supernova progenitors.
Cross-Sectional Association Between Exclusive and Concurrent Use of Cigarettes, ENDS, and Cigars, the Three Most Popular Tobacco Products, and Wheezing Symptoms Among U.S. Adults
Authors: Schneller Liane M , Quiñones Tavárez Zahíra , Goniewicz Maciej L , Xie Zidian , McIntosh Scott , Rahman Irfan , O’Connor Richard J , Ossip Deborah J , Li Dongmei 
Published: September 2020

Abstract

Introduction
This study assessed the association of exclusive and concurrent use of cigarettes, electronic nicotine delivery systems (ENDS), and cigars with ever and past 12-month wheezing symptoms among a nationally representative sample of US adult current tobacco users.

Methods
Cross-sectional data from the Population Assessment of Tobacco and Health (PATH) Study Wave 3 (W3) were used. The weighted prevalence of self-reported ever and past 12-month wheezing symptoms for noncurrent users compared with users of cigarettes, ENDS, cigars, and any combination of these products (polytobacco use of these tobacco products) were presented for 28 082 adults. The cross-sectional association of tobacco use with self-reported wheezing symptoms was assessed using weighted multivariable and ordinal logistic regression with consideration of complex sampling design.

Results
Significantly higher odds of ever had wheezing or whistling in the chest at any time in the past were observed among current cigarette (adjusted odds ratio: 2.62, 95% confidence intervals [CI]: 2.35, 2.91), ENDS (1.49, 95% CI: 1.14, 1.95), and polytobacco users (2.67, 95% CI: 2.26, 3.16) compared with noncurrent users. No associations were seen for cigar use. Polytobacco use was associated with a higher odds of ever wheezing when compared with exclusive ENDS (1.61, 95% CI: 1.19, 2.17) and exclusive cigar use (2.87, 95% CI: 1.93, 4.26), but not exclusive use of cigarettes.

Conclusions
Ever wheezing is associated with the use of cigarettes, ENDS, and polytobacco use of cigarettes, ENDS, and/or cigars, but not cigar use. The association of polytobacco use and wheezing appears to be driven by cigarette use.

Implications
Cross-sectional associations with ever and past 12-month wheezing symptoms were found to be the strongest among cigarette users, exclusively or in combination. Future longitudinal research is needed to better understand how cigarette use interacts with other tobacco and nicotine products and contributes to respiratory symptoms.
Augmenting Markets with Mechanisms
Authors: Antill Samuel , Duffie Darrell 
Published: September 2020

Abstract
We explain how the common practice of size-discovery trade detracts from overall financial market efficiency. At each of a series of size-discovery sessions, traders report their desired trades, generating allocations of the asset and cash that rely on the most recent exchange price. Traders can thus mitigate exchange price impacts by waiting for size-discovery sessions. This waiting causes socially costly delays in the rebalancing of asset positions across traders. As the frequency of size-discovery sessions is increased, exchange market depth is further lowered by the traders’ reduced incentive to bid aggressively on the exchange, further delaying the rebalancing of positions, and more than offsetting the gains from trade that occur at each of the size-discovery sessions.
Impression Formation in the Human Infant Brain
Authors: Krol Kathleen M , Grossmann Tobias 
Published: September 2020

Abstract
Forming an impression of another person is an essential aspect of human social cognition linked to medial prefrontal cortex (mPFC) function in adults. The current study examined the neurodevelopmental origins of impression formation by testing the hypothesis that infants rely on processes localized in mPFC when forming impressions about individuals who appear friendly or threatening. Infants’ brain responses were measured using functional near-infrared spectroscopy while watching 4 different face identities displaying either smiles or frowns directed toward or away from them (N = 77). This was followed by a looking preference test for these face identities (now displaying a neutral expression) using eyetracking. Our results show that infants’ mPFC responses distinguish between smiling and frowning faces when directed at them and that these responses predicted their subsequent person preferences. This suggests that the mPFC is involved in impression formation in human infants, attesting to the early ontogenetic emergence of brain systems supporting person perception and adaptive behavior.