bluuebunny/crossref_metadata_2025_split huggingface dataset:
Determination of the Cross-Reactivity of the Biological Metabolite (–)-trans-Δ9-Tetrahydrocannabinol-Carboxylic Acid-Glucuronide (THC-COOH-Gluc) for Cannabinoid Immunoassays
Authors: Grafinger Katharina Elisabeth , Weinmann Wolfgang 
Published: June 2020

Abstract
The highest concentrated metabolite of (−)-trans-Δ9-tetrahydrocannabinol (THC) in urine, the main psychoactive constituent of Cannabis sativa, is 11-nor-9-carboxy-(−)-trans-Δ9-tetrahydrocannabinol-β-D-glucuronide [(−)-trans-THC-COOH-Gluc]. Even though reference standards for THC, 11-hydroxy-THC (11-OH-THC) and THC-COOH are commercially available as the biological (−)-trans-stereoisomers, the reference standard of THC-COOH-Gluc is only available as the racemic 11-nor-9-carboxy-(±)-cis-Δ9-tetrahydrocannabinol-β-D-glucuronide. This poses the problem for immunoassays, because different stereoisomers may have different cross-reactivity (CR). The aim of the current study was to extract the biological stereoisomer (−)-trans-THC-COOH-Gluc from a urine sample of two marihuana consumers by solid-phase extraction with a Chromabond® C18 cartridge. The cannabinoids in the obtained extract were quantified by Liquid-chromatography coupled to tandem mass spectrometry (LC–MS-MS) and used after dilution for further testing of the CR of (−)-trans-THC-COOH-Gluc with a homogenous enzyme immunoassay assay (hEIA) (Urine HEIA® Cannabinoids (THC), Immunalysis™, Pomona, CA, USA). The CR was determined as the measured HEIA® signal (ng/mL) per THC-COOH-Gluc concentration (ng/mL) in percentage. Results showed that the CR (determined in concentration ratios) is concentration dependent and is 72–87% in the calibration range (20–50 ng/mL). At the cut-off of the hEIA (40 ng/mL), the CR was determined to be 75%. With a molecular weight quotient of 1.51 (MWTHC-COOH-Gluc/MWTHC-COOH = 520.568 g/mol/344.451 g/mol), this means that CR (in molar ratios) is 106–131%. This finding is important, since the major metabolite of THC in urine is (−)-trans-THC-COOH-Gluc and not (−)-trans-THC-COOH, which is used for calibration and no hydrolysis is performed during the determination by hEIA.
De novo evolved gene product NCYM in the pathogenesis and clinical outcome of human neuroblastomas and other cancers
Authors: Suenaga Yusuke , Nakatani Kazuma , Nakagawara Akira 
Published: June 2020

Abstract
NCYM is an antisense transcript of MYCN oncogene and promotes tumor progression. NCYM encodes a de novo protein whose open reading frame evolved from noncoding genomic regions in the ancestor of Homininae. Because of its topology, NCYM is always co-amplified with MYCN oncogene, and the mutual regulations between NCYM and MYCN maintain their expressions at high levels in MYCN-amplified tumors. NCYM stabilizes MYCN by inhibiting GSK3β, whereas MYCN stimulates transcription of both NCYM and MYCN. NCYM mRNA and its noncoding transcript variants MYCNOS have been shown to stimulate MYCN expression via direct binding to MYCN promoter, indicating that both coding and noncoding transcripts of NCYM induce MYCN expression. In contrast to the noncoding functions of NCYM, NCYM protein also promotes calpain-mediated cleavage of c-MYC. The cleaved product called Myc-nick inhibits cell death and promotes cancer cell migration. Furthermore, NCYM-mediated inhibition of GSK3β results in the stabilization of β-catenin, which promotes aggressiveness of bladder cancers. These MYCN-independent functions of NCYM showed their clinical significance in MYCN-non-amplified tumors, including adult tumors. This year is the 30th anniversary of the identification of NCYM/MYCNOS gene. On this special occasion, we summarize the current understanding of molecular functions and the clinical significance of NCYM and discuss future directions to achieve therapeutic strategies targeting NCYM.
Whither mammalian ecology?
Authors: Krebs Charles J 
Published: June 2020

AbstractThe critical agenda for mammalian ecologists over this century is to obtain a synthetic and predictive understanding of the factors that limit the distribution and abundance of mammals on Earth. During the last 100 years, a start has been made on this agenda, but only a start. Most mammal species have been described, but there still are tropical areas of undisclosed species richness. We have been measuring changes in distribution and abundance of many common mammals during the last century, and this monitoring agenda has become more critical as climate change has accelerated and habitat destruction has increased with human population growth. There are a small number of factors that can limit the distribution and abundance of mammals: weather, predation, food supplies, disease, and social behavior. Weather limits distribution and abundance mostly in an indirect manner by affecting food supplies, disease, and predation in the short term and habitat composition and structure in the longer term. A good starting point for all studies of mammals is to define them within a well-structured trophic web, and then quantify the major linkages within that web. We still are far from having data on enough model systems to develop a complete theory and understanding of how food webs are structured and constrained as climate shifts and humans disturb habitats. We have many of the bits and pieces for some of our major ecosystems but a poor understanding of the links and the resilience of our mammalian communities to changes in trophic webs driven by climate change and human disturbances.
Protective effect of trimetazidine in radiation-induced cardiac fibrosis in mice
Authors: Zhang Jinmeng , He Xinjia , Bai Xinya , Sun Yang , Jiang Peng , Wang Xiang , Li Wei , Zhang Yuliang 
Published: June 2020

Abstract
Radiation-induced heart damage is a serious side effect caused by radiotherapy, especially during the treatment of cancer near the chest. Trimetazidine is effective at reducing inflammation in the heart, but how it affects radiation-induced cardiac fibrosis (RICF) is unknown. To investigate the potential effect and molecular mechanism, we designed this project with a C57BL6 male mouse model supposing trimetazidine could inhibit RICF in mice. During the experiment, mice were randomly divided into six groups including a control group (Con), radiation-damaged model group (Mod) and four experimental groups receiving low-dose (10 mg/kg/day) or high-dose (20 mg/kg/day) trimetazidine before or after radiation treatment. Apart from the control group, all mice chests were exposed to 6 MV X-rays at a single dose of 20 Gy to induce RICF, and tissue analysis was done at 8 weeks after irradiation. Fibroblast or interstitial tissues and cardiac fibrosis-like characteristics were determined using haematoxylin and eosin and Masson staining, which can be used to assess myocardial fibrosis. Immunohistochemical analysis and RT-PCR were used to determine gene expression and study the molecular mechanism. As a result, this study suggests that trimetazidine inhibits RICF by reducing gene expression related to myocyte apoptosis and fibrosis formation, i.e. connective tissue growth factor (CTGF), transforming growth factor (TGF)-β1, smad2 and smad3. In conclusion, by regulating the CTGF/TGF-β1/Smad pathway, trimetazidine could be a prospective drug for clinical treatment of RICF.
Spectroscopic and photometric periods of six ultracompact accreting binaries
Authors: Green Matthew J , Marsh Thomas R , Carter Philip J , Steeghs Danny , Breedt Elmé , Dhillon V S , Littlefair S P , Parsons Steven G , Kerry Paul , Gentile Fusillo Nicola P , Ashley R P , Bours Madelon C P , Cunningham Tim , Dyer Martin J , Gänsicke Boris T , Izquierdo Paula , Pala Anna F , Pattama Chuangwit , Outmani Sabrina , Sahman David I , Sukaum Boonchoo , Wild James 
Published: June 2020

ABSTRACT
Ultracompact accreting binary systems each consist of a stellar remnant accreting helium-enriched material from a compact donor star. Such binaries include two related sub-classes, AM CVn-type binaries and helium cataclysmic variables, in both of which the central star is a white dwarf. We present a spectroscopic and photometric study of six accreting binaries with orbital periods in the range of 40–70 min, including phase-resolved VLT spectroscopy and high-speed ULTRACAM photometry. Four of these are AM CVn systems and two are helium cataclysmic variables. For four of these binaries we are able to identify orbital periods (of which three are spectroscopic). SDSS J1505+0659 has an orbital period of 67.8 min, significantly longer than previously believed, and longer than any other known AM CVn binary. We identify a Wide-field Infrared Survey Explorer (WISE) infrared excess in SDSS J1505+0659 that we believe to be the first direct detection of an AM CVn donor star in a non-direct impacting binary. The mass ratio of SDSS J1505+0659 is consistent with a white dwarf donor. CRTS J1028–0819 has an orbital period of 52.1 min, the shortest period of any helium cataclysmic variable. MOA 2010-BLG-087 is co-aligned with a K-class star that dominates its spectrum. ASASSN-14ei and ASASSN-14mv both show a remarkable number of echo outbursts following superoutbursts (13 and 10 echo outbursts respectively). ASASSN-14ei shows an increased outburst rate over the years following its superoutburst, perhaps resulting from an increased accretion rate.
Producing synthetic maps of dust polarization using a velocity channel gradient technique
Authors: Lu Zekun , Lazarian A , Pogosyan Dmitri 
Published: June 2020

ABSTRACT
In modern cosmology, many efforts have been made to detect the primordial B-mode of cosmic microwave background polarization from gravitational waves generated during inflation. Considering the foreground dust contamination of microwave polarization maps, it is essential to obtain a precise prediction for polarization in dust emission. In this work, we show a new method to produce synthetic maps of dust polarization in the magnetized turbulent interstellar medium from more abundant high-resolution H i data. By using the velocity channel gradient technique, we are able to predict both the direction and degree of dust polarization by investigating spectroscopic H i information in position–position–velocity space. We apply our approach to the Galactic Arecibo L-band Feed Array H i data, and find a good correspondence between synthesized maps and Planck’s polarization measurements at 353 GHz.
The C-Band All-Sky Survey: total intensity point-source detection over the northern sky
Authors: Grumitt R D P , Taylor Angela C , Jew Luke , Jones Michael E , Dickinson C , Barr A , Cepeda-Arroita R , Chiang H C , Harper S E , Heilgendorff H M , Jonas J L , Leahy J P , Leech J , Pearson T J , Peel M W , Readhead A C S , Sievers J 
Published: June 2020

ABSTRACT
We present a point-source detection algorithm that employs the second-order Spherical Mexican Hat wavelet filter (SMHW2), and use it on C-Band All-Sky Survey (C-BASS) northern intensity data to produce a catalogue of point sources. This catalogue allows us to cross-check the C-BASS flux-density scale against existing source surveys, and provides the basis for a source mask that will be used in subsequent C-BASS and cosmic microwave background (CMB) analyses. The SMHW2 allows us to filter the entire sky at once, avoiding complications from edge effects arising when filtering small sky patches. The algorithm is validated against a set of Monte Carlo simulations, consisting of diffuse emission, instrumental noise, and various point-source populations. The simulated source populations are successfully recovered. The SMHW2 detection algorithm is used to produce a $4.76\, \mathrm{GHz}$ northern sky source catalogue in total intensity, containing 1784 sources and covering declinations δ ≥ −10°. The C-BASS catalogue is matched with the Green Bank 6 cm (GB6) and Parkes-MIT-NRAO (PMN) catalogues over their areas of common sky coverage. From this we estimate the 90 per cent completeness level to be approximately $610\, \mathrm{mJy}$, with a corresponding reliability of 98 per cent, when masking the brightest 30 per cent of the diffuse emission in the C-BASS northern sky map. We find the C-BASS and GB6 flux-density scales to be consistent with one another to within approximately 4 per cent.
Systematic opacity calculations for kilonovae
Authors: Tanaka Masaomi , Kato Daiji , Gaigalas Gediminas , Kawaguchi Kyohei 
Published: June 2020

ABSTRACTCoalescence of neutron stars (NSs) gives rise to kilonova, thermal emission powered by radioactive decays of freshly synthesized r-process nuclei. Although observational properties are largely affected by bound–bound opacities of r-process elements, available atomic data have been limited. In this paper, we study element-to-element variation of the opacities in the ejecta of NS mergers by performing systematic atomic structure calculations of r-process elements for the first time. We show that the distributions of energy levels tend to be higher as electron occupation increases for each electron shell due to the larger energy spacing caused by larger effects of spin–orbit and electron–electron interactions. As a result, elements with a fewer number of electrons in the outermost shells tend to give larger contributions to the bound–bound opacities. This implies that Fe is not representative for the opacities of light r-process elements. The average opacities for the mixture of r-process elements are found to be κ ∼ 20–30 cm2 g−1 for the electron fraction of Ye ≤ 0.20, κ ∼ 3–5 cm2 g−1 for Ye = 0.25–0.35, and κ ∼ 1 cm2 g−1 for Ye = 0.40 at $T = 5000\!-\!10\, 000$ K, and they steeply decrease at lower temperature. We show that, even with the same abundance or Ye, the opacity in the ejecta changes with time by one order of magnitude from 1 to 10 d after the merger. Our radiative transfer simulations with the new opacity data confirm that ejecta with a high electron fraction (Ye ≳ 0.25, with no lanthanide) are needed to explain the early, blue emission in GW170817/AT2017gfo while lanthanide-rich ejecta (with a mass fraction of lanthanides ∼5 × 10−3) reproduce the long-lasting near-infrared emission.
ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions – I. Survey description and a first look at G9.62+0.19
Authors: Liu Tie , Evans Neal J , Kim Kee-Tae , Goldsmith Paul F , Liu Sheng-Yuan , Zhang Qizhou , Tatematsu Ken’ichi , Wang Ke , Juvela Mika , Bronfman Leonardo , Cunningham Maria R , Garay Guido , Hirota Tomoya , Lee Jeong-Eun , Kang Sung-Ju , Li Di , Li Pak-Shing , Mardones Diego , Qin Sheng-Li , Ristorcelli Isabelle , Tej Anandmayee , Toth L Viktor , Wu Jing-Wen , Wu Yue-Fang , Yi Hee-weon , Yun Hyeong-Sik , Liu Hong-Li , Peng Ya-Ping , Li Juan , Li Shang-Huo , Lee Chang Won , Shen Zhi-Qiang , Baug Tapas , Wang Jun-Zhi , Zhang Yong , Issac Namitha , Zhu Feng-Yao , Luo Qiu-Yi , Soam Archana , Liu Xun-Chuan , Xu Feng-Wei , Wang Yu , Zhang Chao , Ren Zhiyuan , Zhang Chao 
Published: June 2020

ABSTRACT
The ATOMS, standing for ALMA Three-millimeter Observations of Massive Star-forming regions, survey has observed 146 active star-forming regions with ALMA band 3, aiming to systematically investigate the spatial distribution of various dense gas tracers in a large sample of Galactic massive clumps, to study the roles of stellar feedback in star formation, and to characterize filamentary structures inside massive clumps. In this work, the observations, data analysis, and example science of the ATOMS survey are presented, using a case study for the G9.62+0.19 complex. Toward this source, some transitions, commonly assumed to trace dense gas, including CS J = 2−1, HCO+J = 1−0, and HCN J = 1−0, are found to show extended gas emission in low-density regions within the clump; less than 25 per cent of their emission is from dense cores. SO, CH3OH, H13CN, and HC3N show similar morphologies in their spatial distributions and reveal well the dense cores. Widespread narrow SiO emission is present (over ∼1 pc), which may be caused by slow shocks from large–scale colliding flows or H ii regions. Stellar feedback from an expanding H ii region has greatly reshaped the natal clump, significantly changed the spatial distribution of gas, and may also account for the sequential high-mass star formation in the G9.62+0.19 complex. The ATOMS survey data can be jointly analysed with other survey data, e.g. MALT90, Orion B, EMPIRE, ALMA_IMF, and ALMAGAL, to deepen our understandings of ‘dense gas’ star formation scaling relations and massive protocluster formation.
Prospects for cosmic magnification measurements using H i
intensity mapping
Authors: Witzemann Amadeus , Pourtsidou Alkistis , Santos Mario G 
Published: June 2020

ABSTRACT
We investigate the prospects of measuring the cosmic magnification effect by cross-correlating neutral hydrogen intensity mapping (H i IM) maps with background optical galaxies. We forecast the signal-to-noise ratio for H i IM data from SKA1-MID and HIRAX, combined with LSST photometric galaxy samples. We find that, thanks to their different resolutions, SKA1-MID and HIRAX are highly complementary in such an analysis. We predict that SKA1-MID can achieve a detection with a signal-to-noise ratio of ∼15 on a multipole range of ℓ ≲ 200, while HIRAX can reach a signal-to-noise ratio of ∼50 on 200 &lt; ℓ &lt; 2000. We conclude that measurements of the cosmic magnification signal will be possible on a wide redshift range with foreground H i intensity maps up to z ≲ 2, while optimal results are obtained when 0.6 ≲ z ≲ 1.3. Finally, we perform a signal to noise analysis that shows how these measurements can constrain the H i parameters across a wide redshift range.
Anisotropic separate universe simulations
Authors: Masaki Shogo , Nishimichi Takahiro , Takada Masahiro 
Published: June 2020

ABSTRACT
The long-wavelength coherent overdensity and tidal force, which are not direct observables for a finite-volume survey, affect time evolution of cosmic structure formation and therefore clustering observables through the mode coupling. In this paper, we develop an ‘anisotropic’ separate universe (SU) simulation technique to simulate large-scale structure formation taking into account the effect of large-scale tidal force into the anisotropic expansion of local background. We modify the treepmN-body simulation code to implement the anisotropic SU simulations, and then study the ‘response’ function of matter power spectrum that describes how the matter power spectrum responds to the large-scale tidal effect as a function of wavenumber and redshift for a given global cosmology. We test and validate the SU simulation results from the comparison with the perturbation theory predictions and the results from high-resolution particle-mesh simulations. We find that the response function displays characteristic scale dependencies over the range of scales down to non-linear scales, up to k ≃ 6 h Mpc−1.
Inverse Compton signatures of gamma-ray burst afterglows
Authors: Zhang H , Christie I M , Petropoulou M , Rueda-Becerril J M , Giannios D 
Published: June 2020

ABSTRACT
The afterglow emission from gamma-ray bursts (GRBs) is believed to originate from a relativistic blast wave driven into the circumburst medium. Although the afterglow emission from radio up to X-ray frequencies is thought to originate from synchrotron radiation emitted by relativistic, non-thermal electrons accelerated by the blast wave, the origin of the emission at high energies (HE; ≳GeV) remains uncertain. The recent detection of sub-TeV emission from GRB 190114C by the Major Atmospheric Gamma Imaging Cherenkov Telescopes (MAGIC) raises further debate on what powers the very high energy (VHE; ≳300 GeV) emission. Here, we explore the inverse Compton scenario as a candidate for the HE and VHE emissions, considering two sources of seed photons for scattering: synchrotron photons from the blast wave (synchrotron self-Compton or SSC) and isotropic photon fields external to the blast wave (external Compton). For each case, we compute the multiwavelength afterglow spectra and light curves. We find that SSC will dominate particle cooling and the GeV emission, unless a dense ambient infrared photon field, typical of star-forming regions, is present. Additionally, considering the extragalactic background light attenuation, we discuss the detectability of VHE afterglows by existing and future gamma-ray instruments for a wide range of model parameters. Studying GRB 190114C, we find that its afterglow emission in the Fermi-Large Area Telescope (LAT) band is synchrotron dominated. The late-time Fermi-LAT measurement (i.e. t ∼ 104 s), and the MAGIC observation also set an upper limit on the energy density of a putative external infrared photon field (i.e. ${\lesssim} 3\times 10^{-9}\, {\rm erg\, cm^{-3}}$), making the inverse Compton dominant in the sub-TeV energies.
Physical Therapist Management of Total Knee Arthroplasty
Authors: Jette Diane U , Hunter Stephen J , Burkett Lynn , Langham Bud , Logerstedt David S , Piuzzi Nicolas S , Poirier Noreen M , Radach Linda J L , Ritter Jennifer E , Scalzitti David A , Stevens-Lapsley Jennifer E , Tompkins James , Zeni Jr Joseph ,   for the American Physical Therapy Association
Published: June 2020

Abstract
A clinical practice guideline on total knee arthroplasty was developed by an American Physical Therapy (APTA) volunteer guideline development group that consisted of physical therapists, an orthopedic surgeon, a nurse, and a consumer. The guideline was based on systematic reviews of current scientific and clinical information and accepted approaches to management of total knee arthroplasty.
Disease Control and Inequality Reduction: Evidence from a Tuberculosis Testing and Vaccination Campaign
Authors: Bütikofer Aline , Salvanes Kjell G 
Published: June 2020

AbstractThis article examines the economic impact of a tuberculosis control program launched in Norway in 1948. In the 1940s, Norway had one of the highest tuberculosis infection rates in Europe, affecting about 85% of the inhabitants. To lower the disease burden, the Norwegian government launched a large-scale tuberculosis testing and vaccination campaign that substantially reduced tuberculosis infection rates among children. We find that cohorts in school during and after the campaign in municipalities with high tuberculosis prevalence gained more in terms of education, earnings, longevity, and height following this public health intervention. Furthermore, the gains from the disease control program are not limited to the initially treated cohorts but also affect their children. The results also suggest that individuals from a low socioeconomic background benefited more from the intervention and we present new evidence that a narrowing of the gap in childhood health can lead to a reduction in socioeconomic inequalities in adulthood.
Sharing the Pain? Credit Supply and Real Effects of Bank Bail-ins
Authors: Beck Thorsten , Da-Rocha-Lopes Samuel , Silva André F 
Published: June 2020

AbstractWe analyze the credit supply and real effects of bank bail-ins by exploiting the unexpected failure and subsequent resolution of a major Portuguese bank. Using loan-level data, we show that while firms more exposed to the bail-in suffered a significant contraction of credit at the intensive margin, they were on average able to compensate for the supply-driven shock. However, affected SMEs experienced a binding reduction of funds available through credit lines, and those with lower internal liquidity increased precautionary cash holdings and reduced investment and employment. Our results highlight the trade-off policymakers face when considering this new bank resolution mechanism.