bluuebunny/crossref_metadata_2025_split huggingface dataset:
Temperature response of wheat affects final height and the timing of stem elongation under field conditions
Authors: Kronenberg Lukas , Yates Steven , Boer Martin P , Kirchgessner Norbert , Walter Achim , Hund Andreas 
Published: October 2020

Abstract
In wheat, temperature affects the timing and intensity of stem elongation. Genetic variation for this process is therefore important for adaptation. This study investigates the genetic response to temperature fluctuations during stem elongation and its relationship to phenology and height. Canopy height of 315 wheat genotypes (GABI wheat panel) was scanned twice weekly in the field phenotyping platform (FIP) of ETH Zurich using a LIDAR. Temperature response was modelled using linear regressions between stem elongation and mean temperature in each measurement interval. This led to a temperature-responsive (slope) and a temperature-irresponsive (intercept) component. The temperature response was highly heritable (H2=0.81) and positively related to a later start and end of stem elongation as well as final height. Genome-wide association mapping revealed three temperature-responsive and four temperature-irresponsive quantitative trait loci (QTLs). Furthermore, putative candidate genes for temperature-responsive QTLs were frequently related to the flowering pathway in Arabidopsis thaliana, whereas temperature-irresponsive QTLs corresponded to growth and reduced height genes. In combination with Rht and Ppd alleles, these loci, together with the loci for the timing of stem elongation, accounted for 71% of the variability in height. This demonstrates how high-throughput field phenotyping combined with environmental covariates can contribute to a smarter selection of climate-resilient crops.
Practice Variation in Regional Anesthesia Utilization by Current and Former U.S. Military Anesthesiology Residents
Authors: Jaffe Edward , Patzkowski Michael S , Hodgson John A , Foerschler Derek L , Gonzalez Sara C , Giordano Nicholas A , Scott-Richardson Maya P , Highland Krista B 
Published: October 2020

ABSTRACT

Introduction
Per Joint Trauma System guidelines, military anesthesiologists are expected to be ready to lead an Acute Pain Service with regional anesthesia in combat casualty care. However, regional anesthesia practice volume has not been assessed in the military. The objective of this study was to assess regional anesthesia utilization among current residents and graduates of U.S. military anesthesiology residency programs.

Materials and Methods
All current and former active duty military anesthesiology program residents, trained at any of the four military anesthesiology residency programs between 2013 and 2019, were anonymously surveyed about their regional anesthesia practice. Bivariate statistics described the total single-injection and catheter block techniques utilized in the last month. Cluster analysis assessed for the presence of distinct practice groups within the sample. Follow-up analyses explored potential associations between cluster membership and other variables (e.g., residency training site, residency graduation year, overall confidence in performing regional anesthesia, etc.). This protocol received exemption determination separately from each site’s institutional review board.

Results
Current and former residents reported broad variation in regional anesthesia practice and clustered into four distinct practice groups. Less than half of respondents utilized a moderate to high number of different single-injection and catheter blocks.

Conclusions
These findings highlight the need for creative solutions to increase regional anesthesia training in military anesthesiology programs and continued ability to implement skills, such that all military anesthesiologists have adequate practice for deployed responsibilities.
Melon with a Twist: A Case of Nicotine Overdose After Ingestion and Aspiration of Vape Liquid
Authors: Jude Joseph , Hiller Hugh , Miller Joel 
Published: October 2020

ABSTRACT
We present the case of an active duty 21-year-old male with severe hypoxic respiratory failure after accidentally ingesting, and subsequently aspirating, vaping liquid while intoxicated. Because of the increasing prevalence of vaping devices, this case highlights a unique risk of vape liquids with concentrated nicotine levels and appetizing labels and aromas. Vaping-associated pulmonary injury has been previously described in multiple publications, but unlike those patients with pathology after inhaling vaping products, our patient ingested and subsequently aspirated the highly nicotinic substance. Most vape liquid products have enough nicotine to result in significant toxicity, which most concerningly can lead to nicotine-induced respiratory failure. This patient’s hypoxia appeared to be multifactorial as a result of both nicotine toxicity and aspiration, but ultimately treatment of both focused on supportive measures.In addition to understanding nicotine toxicity, this patient’s hypoxia secondary to agitation and aspiration requiring emergent airway management illustrates the importance of understanding the technique of Delayed Sequence Intubation and its proper application in the critical airway algorithm. By treating preoxygenation as a procedure, the patient received adequate oxygenation resulting in successful intubation without harmful desaturation during the procedure.Given the prevalence of tobacco use in the military as well as the increasing popularity of vaping devices, future military providers have a responsibility to their patients to be prepared for similar case presentations. Fortunately, this case demonstrates that when managed properly, otherwise healthy patients without comorbidities often recover without significant long-term sequelae.
Abundance measurements of H2O and carbon-bearing species in the atmosphere of WASP-127b confirm its supersolar metallicity
Authors: Spake Jessica J , Sing David K , Wakeford Hannah R , Nikolov Nikolay , Mikal-Evans Thomas , Deming Drake , Barstow Joanna K , Anderson David R , Carter Aarynn L , Gillon Michael , Goyal Jayesh M , Hebrard Guillaume , Hellier Coel , Kataria Tiffany , Lam Kristine W F , Triaud A H M J , Wheatley Peter J 
Published: October 2020

ABSTRACT
The chemical abundances of exoplanet atmospheres may provide valuable information about the bulk compositions, formation pathways, and evolutionary histories of planets. Exoplanets with large, relatively cloud-free atmospheres, and which orbit bright stars provide the best opportunities for accurate abundance measurements. For this reason, we measured the transmission spectrum of the bright (V ∼ 10.2), large (1.37 RJ), sub-Saturn mass (0.19 MJ) exoplanet WASP-127b across the near-UV to near-infrared wavelength range (0.3–5 μm), using the Hubble and Spitzer Space Telescopes. Our results show a feature-rich transmission spectrum, with absorption from Na, H2O, and CO2, and wavelength-dependent scattering from small-particle condensates. We ran two types of atmospheric retrieval models: one enforcing chemical equilibrium, and the other which fit the abundances freely. Our retrieved abundances at chemical equilibrium for Na, O, and C are all supersolar, with abundances relative to solar values of 9$^{+15}_{-6}$, 16$^{+7}_{-5}$, and 26$^{+12}_{-9}$, respectively. Despite giving conflicting C/O ratios, both retrievals gave supersolar CO2 volume mixing ratios, which adds to the likelihood that WASP-127b’s bulk metallicity is supersolar, since CO2 abundance is highly sensitive to atmospheric metallicity. We detect water at a significance of 13.7σ. Our detection of Na is in agreement with previous ground-based detections, though we find a much lower abundance, and we also do not find evidence for Li or K despite increased sensitivity. In the future, spectroscopy with James Webb Space Telescope will be able to constrain WASP-127b’s C/O ratio, and may reveal the formation history of this metal-enriched, highly observable exoplanet.
Cooling of accretion disc coronae by Type I X-ray bursts
Authors: Speicher J , Ballantyne D R , Malzac J 
Published: October 2020

ABSTRACT
Although accretion disc coronae appear to be common in many accreting systems, their fundamental properties remain insufficiently understood. Recent work suggests that Type I X-ray bursts from accreting neutron stars provide an opportunity to probe the characteristics of coronae. Several studies have observed hard X-ray shortages from the accretion disc during an X-ray burst implying strong coronal cooling by burst photons. Here, we use the plasma emission code eqpair to study the impact of X-ray bursts on coronae, and how the coronal and burst properties affect the coronal electron temperatures and emitted spectra. Assuming a constant accretion rate during the burst, our simulations show that soft photons can cool coronal electrons by a factor of ≳ 10 and cause a reduction of emission in the 30–50 keV band to $\lesssim 1{{\ \rm per\ cent}}$ of the pre-burst emission. This hard X-ray drop is intensified when the coronal optical depth and aspect ratio is increased. In contrast, depending on the properties of the burst and corona, the emission in the 8–24 keV band can either increase, by a factor of ≳ 20, or decrease, down to $\lesssim 1{{\ \rm per\ cent}}$ of the pre-burst emission. An increasing accretion rate during the X-ray burst reduces the coronal cooling effects and the electron temperature drop can be mitigated by $\gtrsim 60{{\ \rm per\ cent}}$. These results indicate that changes of the hard X-ray flux during an X-ray burst probe the geometrical properties of the corona.
A bias in VLBI measurements of the core shift effect in AGN jets
Authors: Pashchenko I N , Plavin A V , Kutkin A M , Kovalev Y Y 
Published: October 2020

ABSTRACT
The Blandford and Königl model of active galactic nuclei (AGN) jets predicts that the position of the apparent opaque jet base – the core – changes with frequency. This effect is observed with radio interferometry and is widely used to infer parameters and structure of the innermost jet regions. The position of the radio core is typically estimated by fitting a Gaussian template to the interferometric visibilities. This results in a model approximation error, i.e. a bias that can be detected and evaluated through simulations of observations with a realistic jet model. To assess the bias, we construct an artificial sample of sources based on the AGN jet model evaluated on a grid of the parameters derived from a real VLBI flux-density-limited sample and create simulated VLBI data sets at 2.3, 8.1, and 15.4 GHz. We found that the core position shifts from the true jet apex are generally overestimated. The bias is typically comparable to the core shift random error and can reach a factor of 2 for jets with large apparent opening angles. This observational bias depends mostly on the ratio between the true core shift and the image resolution. This implies that the magnetic field, the core radial distance, and the jet speed inferred from the core shift measurements are overestimated. We present a method to account for the bias.
An extreme-mass ratio, short-period eclipsing binary consisting of a B dwarf primary and a pre-main-sequence M star companion discovered by KELT
Authors: Stevens Daniel J , Zhou George , Johnson Marshall C , Rizzuto Aaron C , Rodriguez Joseph E , Bieryla Allyson , Collins Karen A , Villanueva Steven , Wright Jason T , Gaudi B Scott , Latham David W , Beatty Thomas G , Lund Michael B , Siverd Robert J , Kraus Adam L , Wachiraphan Patcharapol , Berlind Perry , Calkins Michael L , Esquerdo Gilbert A , Kielkopf John F , Kuhn Rudolf B , Manner Mark , Pepper Joshua , Stassun Keivan G 
Published: October 2020

ABSTRACT
We present the discovery of KELT J072709 + 072007 (HD 58730), a very low mass ratio (q ≡ M2/M1 ≈ 0.07) eclipsing binary (EB) identified by the Kilodegree Extremely Little Telescope (KELT) survey. We present the discovery light curve and perform a global analysis of four high-precision ground-based light curves, the Transiting Exoplanets Survey Satellite (TESS) light curve, radial velocity (RV) measurements, Doppler Tomography (DT) measurements, and the broad-band spectral energy distribution. Results from the global analysis are consistent with a fully convective ($M_2 = 0.22 \pm 0.02\ \, \mathrm{M}_{\odot })$ M star transiting a late-B primary ($M_1 = 3.34^{+0.07}_{-0.09}\ \, \mathrm{M}_{\odot }\,\mathrm{ and}\,\ T_{\rm eff,1} = 11960^{+430}_{-520}\ {\rm K}$). We infer that the primary star is $183_{-30}^{+33}$ Myr old and that the companion star’s radius is inflated by $26 \pm 8{{\ \rm per\ cent}}$ relative to the predicted value from a low-mass isochrone of similar age. We separately and analytically fit for the variability in the out-of-eclipse TESS phase curve, finding good agreement between the resulting stellar parameters and those from the global fit. Such systems are valuable for testing theories of binary star formation and understanding how the environment of a star in a close-but-detached binary affects its physical properties. In particular, we examine how a star’s properties in such a binary might differ from the properties it would have in isolation.
Coupled day–night models of exoplanetary atmospheres
Authors: Gandhi Siddharth , Jermyn Adam S 
Published: October 2020

ABSTRACT
We provide a new framework to model the day side and night side atmospheres of irradiated exoplanets using 1D radiative transfer by incorporating a self-consistent heat flux carried by circulation currents (winds) between the two sides. The advantages of our model are its physical motivation and computational efficiency, which allows for an exploration of a wide range of atmospheric parameters. We use this forward model to explore the day and night side atmosphere of WASP-76 b, an ultrahot Jupiter which shows evidence for a thermal inversion and Fe condensation, and WASP-43 b, comparing our model against high precision phase curves and general circulation models. We are able to closely match the observations as well as prior theoretical predictions for both of these planets with our model. We also model a range of hot Jupiters with equilibrium temperatures between 1000 and 3000 K and reproduce the observed trend that the day–night temperature contrast increases with equilibrium temperature up to ∼2500 K beyond which the dissociation of H2 becomes significant and the relative temperature difference declines.
K2-111: an old system with two planets in near-resonance†
Authors: Mortier A , Zapatero Osorio M R , Malavolta L , Alibert Y , Rice K , Lillo-Box J , Vanderburg A , Oshagh M , Buchhave L , Adibekyan V , Delgado Mena E , Lopez-Morales M , Charbonneau D , Sousa S G , Lovis C , Affer L , Allende Prieto C , Barros S C C , Benatti S , Bonomo A S , Boschin W , Bouchy F , Cabral A , Collier Cameron A , Cosentino R , Cristiani S , Demangeon O D S , Di Marcantonio P , D’Odorico V , Dumusque X , Ehrenreich D , Figueira P , Fiorenzano A , Ghedina A , González Hernández J I , Haldemann J , Harutyunyan A , Haywood R D , Latham D W , Lavie B , Lo Curto G , Maldonado J , Manescau A , Martins C J A P , Mayor M , Mégevand D , Mehner A , Micela G , Molaro P , Molinari E , Nunes N J , Pepe F A , Palle E , Phillips D , Piotto G , Pinamonti M , Poretti E , Riva M , Rebolo R , Santos N C , Sasselov D , Sozzetti A , Suárez Mascareño A , Udry S , West R G , Watson C A , Wilson T G 
Published: October 2020

ABSTRACT
This paper reports on the detailed characterization of the K2-111 planetary system with K2, WASP, and ASAS-SN photometry, as well as high-resolution spectroscopic data from HARPS-N and ESPRESSO. The host, K2-111, is confirmed to be a mildly evolved (log g = 4.17), iron-poor ([Fe/H] = −0.46), but alpha-enhanced ([α/Fe]=0.27), chromospherically quiet, very old thick disc G2 star. A global fit, performed by using PyORBIT, shows that the transiting planet, K2-111 b, orbits with a period Pb = 5.3518 ± 0.0004 d and has a planet radius of $1.82^{+0.11}_{-0.09}$ R⊕ and a mass of $5.29^{+0.76}_{-0.77}$ M⊕, resulting in a bulk density slightly lower than that of the Earth. The stellar chemical composition and the planet properties are consistent with K2-111 b being a terrestrial planet with an iron core mass fraction lower than the Earth. We announce the existence of a second signal in the radial velocity data that we attribute to a non-transiting planet, K2-111 c, with an orbital period of 15.6785 ± 0.0064 d, orbiting in near-3:1 mean motion resonance with the transiting planet, and a minimum planet mass of 11.3 ± 1.1 M⊕. Both planet signals are independently detected in the HARPS-N and ESPRESSO data when fitted separately. There are potentially more planets in this resonant system, but more well-sampled data are required to confirm their presence and physical parameters.
What if the neutron star maximum mass is beyond ∼2.3 M⊙?
Authors: Wu X H , Du S , Xu R X 
Published: October 2020

ABSTRACT
By assuming the formation of a black hole soon after the merger event of GW170817, the maximum mass of non-rotating stable neutron star, MTOV ≃ 2.3 M⊙, is proposed by numerical relativity, but there is no solid evidence to rule out MTOV &gt; 2.3 M⊙ from the point of both microphysical and astrophysical views. It is naturally expected that the equation of state (EOS) would become stiffer beyond a specific density to explain massive pulsars. We consider the possibility of EOSs with MTOV &gt; 2.3 M⊙, investigating the stiffness and the transition density in a polytropic model, for two kinds of neutron stars (i.e. gravity-bound and strong-bound stars on surface). Only two parameters are input in both cases: (ρt, γ) for gravity-bound neutron stars, while (ρs, γ) for strong-bound strange stars, with ρt the transition density, ρs the surface density, and γ the polytropic exponent. In the matter of MTOV &gt; 2.3 M⊙ for the maximum mass and 70 ≤ Λ1.4 ≤ 580 for the tidal deformability, it is found that the smallest ρt and γ should be ∼0.50 ρ0 and ∼2.65 for neutron stars, respectively, whereas for strange star, we have γ &gt; 1.40 if ρs &gt; 1.0 ρ0 (ρ0 is the nuclear saturation density). These parametric results could guide further research of the real EOS with any foundation of microphysics if a pulsar mass higher than 2.3 M⊙ is measured in the future, especially for an essential comparison of allowed parameter space between gravity-bound and strong-bound compact stars.
Prospects for distinguishing galaxy evolution models with surveys at redshifts z ≳ 4
Authors: Mirocha Jordan 
Published: October 2020

ABSTRACT
Many semi-empirical galaxy formation models have recently emerged to interpret high-z galaxy luminosity functions and make predictions for future galaxy surveys. A common approach assumes a ‘universal’ star formation efficiency, f*, independent of cosmic time but strongly dependent on the masses of dark matter haloes. Though this class of models has been very successful in matching observations over much of cosmic history, simple stellar feedback models do predict redshift evolution in f* and are commonly used in semi-analytic models. In this work, we calibrate a set of universal f* and feedback-regulated models to the same set of rest-ultraviolet z ≳ 4 observations and find that a rapid, ∼(1 + z)−3/2 decline in both the efficiency of dust production and duty cycle of star formation are needed to reconcile feedback-regulated models with current observations. By construction, these models remain nearly identical to universal f* models in rest-ultraviolet luminosity functions (UVLFs) and colours. As a result, the only way to distinguish these competing scenarios is either via (i) improved constraints on the clustering of galaxies – universal and feedback-regulated models differ in predictions for the galaxy bias by 0.1 ≲ Δ〈b〉 ≲ 0.3 over 4 ≲ z ≲ 10 – or (ii) independent constraints on the dust contents and/or duty cycle of star formation. This suggests that improved constraints on the ‘dustiness’ and ‘burstiness’ of high-z galaxies will not merely add clarity to a given model of star formation in high-z galaxies, but rather fundamentally determine our ability to identify the correct model in the first place.
Discovery and development of novel DNA-PK inhibitors by targeting the unique Ku–DNA interaction
Authors: Gavande Navnath S , VanderVere-Carozza Pamela S , Pawelczak Katherine S , Mendoza-Munoz Pamela , Vernon Tyler L , Hanakahi Leslyn A , Summerlin Matthew , Dynlacht Joseph R , Farmer Annabelle H , Sears Catherine R , Nasrallah Nawar Al , Garrett Joy , Turchi John J 
Published: October 2020

Abstract
DNA-dependent protein kinase (DNA-PK) plays a critical role in the non-homologous end joining (NHEJ) repair pathway and the DNA damage response (DDR). DNA-PK has therefore been pursued for the development of anti-cancer therapeutics in combination with ionizing radiation (IR). We report the discovery of a new class of DNA-PK inhibitors that act via a novel mechanism of action, inhibition of the Ku–DNA interaction. We have developed a series of highly potent and specific Ku–DNA binding inhibitors (Ku-DBi’s) that block the Ku–DNA interaction and inhibit DNA-PK kinase activity. Ku-DBi’s directly interact with the Ku and inhibit in vitro NHEJ, cellular NHEJ, and potentiate the cellular activity of radiomimetic agents and IR. Analysis of Ku-null cells demonstrates that Ku-DBi’s cellular activity is a direct result of Ku inhibition, as Ku-null cells are insensitive to Ku-DBi’s. The utility of Ku-DBi’s was also revealed in a CRISPR gene-editing model where we demonstrate that the efficiency of gene insertion events was increased in cells pre-treated with Ku-DBi’s, consistent with inhibition of NHEJ and activation of homologous recombination to facilitate gene insertion. These data demonstrate the discovery and application of new series of compounds that modulate DNA repair pathways via a unique mechanism of action.
The catalytic activity of the translation termination factor methyltransferase Mtq2-Trm112 complex is required for large ribosomal subunit biogenesis
Authors: Lacoux Caroline , Wacheul Ludivine , Saraf Kritika , Pythoud Nicolas , Huvelle Emmeline , Figaro Sabine , Graille Marc , Carapito Christine , Lafontaine Denis L J , Heurgué-Hamard Valérie 
Published: October 2020

Abstract
The Mtq2-Trm112 methyltransferase modifies the eukaryotic translation termination factor eRF1 on the glutamine side chain of a universally conserved GGQ motif that is essential for release of newly synthesized peptides. Although this modification is found in the three domains of life, its exact role in eukaryotes remains unknown. As the deletion of MTQ2 leads to severe growth impairment in yeast, we have investigated its role further and tested its putative involvement in ribosome biogenesis. We found that Mtq2 is associated with nuclear 60S subunit precursors, and we demonstrate that its catalytic activity is required for nucleolar release of pre-60S and for efficient production of mature 5.8S and 25S rRNAs. Thus, we identify Mtq2 as a novel ribosome assembly factor important for large ribosomal subunit formation. We propose that Mtq2-Trm112 might modify eRF1 in the nucleus as part of a quality control mechanism aimed at proof-reading the peptidyl transferase center, where it will subsequently bind during translation termination.