bluuebunny/crossref_metadata_2025_split huggingface dataset:
Membrane-type I matrix metalloproteinase (MT1-MMP), lipid metabolism, and therapeutic implications
Authors: Xia Xiao-Dan , Alabi Adekunle , Wang Maggie , Gu Hong-Mei , Yang Rui Zhe , Wang Gui-Qing , Zhang Da-Wei 
Published: July 2021

AbstractLipids exert many essential physiological functions, such as serving as a structural component of biological membranes, storing energy, and regulating cell signal transduction. Dysregulation of lipid metabolism can lead to dyslipidemia related to various human diseases, such as obesity, diabetes, and cardiovascular disease. Therefore, lipid metabolism is strictly regulated through multiple mechanisms at different levels, including the extracellular matrix. Membrane-type I matrix metalloproteinase (MT1-MMP), a zinc-dependent endopeptidase, proteolytically cleaves extracellular matrix components, and non-matrix proteins, thereby regulating many physiological and pathophysiological processes. Emerging evidence supports the vital role of MT1-MMP in lipid metabolism. For example, MT1-MMP mediates ectodomain shedding of low-density lipoprotein receptor and increases plasma low-density lipoprotein cholesterol levels and the development of atherosclerosis. It also increases the vulnerability of atherosclerotic plaque by promoting collagen cleavage. Furthermore, it can cleave the extracellular matrix of adipocytes, affecting adipogenesis and the development of obesity. Therefore, the activity of MT1-MMP is strictly regulated by multiple mechanisms, such as autocatalytic cleavage, endocytosis and exocytosis, and post-translational modifications. Here, we summarize the latest advances in MT1-MMP, mainly focusing on its role in lipid metabolism, the molecular mechanisms regulating the function and expression of MT1-MMP, and their pharmacotherapeutic implications.
Sleep Patterns Related to Emotion Dysregulation Among Adolescents and Young Adults
Authors: Fisher Rachel S , Dattilo Taylor M , Sharkey Christina M , Traino Katherine A , Espeleta Hannah C , Krietsch Kendra N , Chaney John M , Mullins Larry L 
Published: July 2021

Abstract

Objective
Adolescents and young adults in the college setting often report poor sleep hygiene and quality. These sleep difficulties may be related to emotion dysregulation, which is highly relevant to broader adjustment. The current study aimed to empirically identify latent groups of healthy college students with distinct subjective sleep patterns and examine differences in emotion dysregulation between subgroups.

Methods
College students (N = 476; Mage=19.38) completed the Adolescent Sleep–Wake Scale—Revised, Adolescent Sleep Hygiene Scale—Revised, and Difficulties in Emotion Dysregulation Scale. Most participants were White (78%), non-Hispanic/Latinx (85%), and female (77%). Latent profile analysis identified patterns of sleep with maximum likelihood estimation. Bolck–Croon–Hagenaars procedure evaluated differences in emotion dysregulation by class.

Results
A three-class model had optimal fit, Bayesian information criterion = 11,577.001, Bootstrapped Parametric Likelihood Ratio Test = −5,763.042, p &lt; .001, entropy = .815. The three profiles identified were good sleep (overall high sleep quality and hygiene; n = 219), moderate sleep (low sleep quality with mix of low and high sleep hygiene; n = 221), and poor sleep (very low sleep quality and hygiene; n = 36). Those in the good sleep group (M = 68.06, SE = 1.5) reported significantly less emotion dysregulation than the moderate sleep group (M = 92.12, SE = 1.67; X2(2) = 98.34, p = .001) and the poor sleep group (M = 99.51, SE = 4.10; p &lt; .001). The moderate and poor sleep groups did not significantly differ, X2(2) = 2.60, p = .11.

Conclusions
Emotion dysregulation differed across three sleep profiles, with participants classified in the good sleep group reporting, on average, the lowest emotion dysregulation, compared to the moderate and poor sleep groups. These findings highlight contextual factors of sleep that may be clinically targeted to promote emotion regulation.
Analysis on the accuracy of CT-guided radioactive I-125 seed implantation with 3D printing template assistance in the treatment of thoracic malignant tumors
Authors: Ji Zhe , Sun Haitao , Jiang Yuliang , Chen Yi , Guo Fuxin , Fan Jinghong , Wang Junjie 
Published: July 2021

Abstract
This article analyzes the accuracy of needle track and dose of a 3-dimensional printing template (3DPT) in the treatment of thoracic tumor with radioactive I-125 seed implantation (RISI). A total of 28 patients were included. The technical process included: (i) preoperative CT positioning, (ii) preoperative planning design, (iii) 3DPT design and printing, (iv) 3DPT alignment, (v) puncture and seed implantation. The errors of needle position and dosimetric parameters were analyzed. A total of 318 needles were used. The mean errors in needle depth, needle insertion point, needle tip and needle angle were 0.52 ± 0.48 cm, 3.4 ± 1.7 mm, 4.4 ± 2.9 mm and 2.8 ± 1.7°, respectively. The differences between actual needle insertion angle and needle depth and those designed in the preoperative were statistically significant (p &lt; 0.05). The mean values of all the errors of the chest wall cases were smaller than those of the lungs, and the differences were statistically significant (p &lt; 0.05). There was no significant difference between the D90 calculated in the postoperative plan and those designed in the preoperative and intraoperative plans (p &gt; 0.05). Some dosimetric parameters of preoperative plans such as V100, V200, CI and HI were not consistent with that of preoperative plans, and the difference was statistically significant (p &lt; 0.05). However, there were no statistical difference in the dosimetric parameters between the postoperative plans and intraoperative plans (p &gt; 0.05). We conclude that for thoracic tumors, even under the guidance of 3DPT, there will be errors. The plan should be optimized in real time during the operation.
Radon inhalation decreases DNA damage induced by oxidative stress in mouse organs via the activation of antioxidative functions
Authors: Kataoka Takahiro , Shuto Hina , Naoe Shota , Yano Junki , Kanzaki Norie , Sakoda Akihiro , Tanaka Hiroshi , Hanamoto Katsumi , Mitsunobu Fumihiro , Terato Hiroaki , Yamaoka Kiyonori 
Published: July 2021

Abstract
Radon inhalation decreases the level of lipid peroxide (LPO); this is attributed to the activation of antioxidative functions. This activation contributes to the beneficial effects of radon therapy, but there are no studies on the risks of radon therapy, such as DNA damage. We evaluated the effect of radon inhalation on DNA damage caused by oxidative stress and explored the underlying mechanisms. Mice were exposed to radon inhalation at concentrations of 2 or 20 kBq/m3 (for one, three, or 10 days). The 8-hydroxy-2′-deoxyguanosine (8-OHdG) levels decreased in the brains of mice that inhaled 20 kBq/m3 radon for three days and in the kidneys of mice that inhaled 2 or 20 kBq/m3 radon for one, three or 10 days. The 8-OHdG levels in the small intestine decreased by approximately 20–40% (2 kBq/m3 for three days or 20 kBq/m3 for one, three or 10 days), but there were no significant differences in the 8-OHdG levels between mice that inhaled a sham treatment and those that inhaled radon. There was no significant change in the levels of 8-oxoguanine DNA glycosylase, which plays an important role in DNA repair. However, the level of Mn-superoxide dismutase (SOD) increased by 15–60% and 15–45% in the small intestine and kidney, respectively, following radon inhalation. These results suggest that Mn-SOD probably plays an important role in the inhibition of oxidative DNA damage.
Automatic contour segmentation of cervical cancer using artificial intelligence
Authors: Kano Yosuke , Ikushima Hitoshi , Sasaki Motoharu , Haga Akihiro 
Published: July 2021

Abstract
In cervical cancer treatment, radiation therapy is selected based on the degree of tumor progression, and radiation oncologists are required to delineate tumor contours. To reduce the burden on radiation oncologists, an automatic segmentation of the tumor contours would prove useful. To the best of our knowledge, automatic tumor contour segmentation has rarely been applied to cervical cancer treatment. In this study, diffusion-weighted images (DWI) of 98 patients with cervical cancer were acquired. We trained an automatic tumor contour segmentation model using 2D U-Net and 3D U-Net to investigate the possibility of applying such a model to clinical practice. A total of 98 cases were employed for the training, and they were then predicted by swapping the training and test images. To predict tumor contours, six prediction images were obtained after six training sessions for one case. The six images were then summed and binarized to output a final image through automatic contour segmentation. For the evaluation, the Dice similarity coefficient (DSC) and Hausdorff distance (HD) was applied to analyze the difference between tumor contour delineation by radiation oncologists and the output image. The DSC ranged from 0.13 to 0.93 (median 0.83, mean 0.77). The cases with DSC &lt;0.65 included tumors with a maximum diameter &lt; 40 mm and heterogeneous intracavitary concentration due to necrosis. The HD ranged from 2.7 to 9.6 mm (median 4.7 mm). Thus, the study confirmed that the tumor contours of cervical cancer can be automatically segmented with high accuracy.
Risk scorecard to minimize impact of COVID-19 when reopening
Authors: Lim Shin B , Pung Rachael , Tan Kellie , Lang Jocelyn H S , Yong Dominique Z X , Teh Shi-Hua , Quah Elizabeth , Sun Yinxiaohe , Ma Stefan , Lee Vernon J M 
Published: July 2021

Abstract

Background
We present a novel approach for exiting coronavirus disease 2019 (COVID-19) lockdowns using a ‘risk scorecard’ to prioritize activities to resume whilst allowing safe reopening.

Methods
We modelled cases generated in the community/week, incorporating parameters for social distancing, contact tracing and imported cases. We set thresholds for cases and analysed the effect of varying parameters. An online tool to facilitate country-specific use including the modification of parameters (https://sshsphdemos.shinyapps.io/covid_riskbudget/) enables visualization of effects of parameter changes and trade-offs. Local outbreak investigation data from Singapore illustrate this.

Results
Setting a threshold of 0.9 mean number of secondary cases arising from a case to keep R &lt; 1, we showed that opening all activities excluding high-risk ones (e.g. nightclubs) allows cases to remain within threshold; while opening high-risk activities would exceed the threshold and result in escalating cases. An 80% reduction in imported cases per week (141 to 29) reduced steady-state cases by 30% (295 to 205). One-off surges in cases (due to superspreading) had no effect on the steady state if the R remains &lt;1. Increasing the effectiveness of contact tracing (probability of a community case being isolated when infectious) by 33% (0.6 to 0.8) reduced cases by 22% (295 to 231). Cases grew exponentially if the product of the mean number of secondary cases arising from a case and (1—probability of case being isolated) was &gt;1.

Conclusions
Countries can utilize a ‘risk scorecard’ to balance relaxations for travel and domestic activity depending on factors that reduce disease impact, including hospital/ICU capacity, contact tracing, quarantine and vaccination. The tool enabled visualization of the combinations of imported cases and activity levels on the case numbers and the trade-offs required. For vaccination, a reduction factor should be applied both for likelihood of an infected case being present and a close contact getting infected.
Computational Errors and Suspension in a PWK Epistemic Agent
Authors: Carrara Massimiliano , Zhu Wei 
Published: July 2021

Abstract
In a computational program there can be two kinds of errors: (i) critical errors and (ii) non-critical errors. A critical error stops the program in a global way, which means the error cannot be fixed in the subsequent computation process. A non-critical error partially stops the computation program, and the error can be fixed in the subsequent computation process. We argue that two kinds of errors correspond to two kinds of suspension and can be modeled using Paraconsistent Weak Kleene ($ {\textsf{PWK}}$) belief revision theory, with the help of a new interpretation of the third value of $ {\textsf{PWK}}$, that is, off-topic. According to this new interpretation, if a proposition obtains the third value $\textbf{u}$, it means it is off-topic. Within our framework of $ {\textsf{PWK}}$ belief revision theory, we will show that a non-critical error corresponds to a non-critical suspension and that a critical error corresponds to a critical suspension.
High-redshift quasars at z ≥ 3 – I. Radio spectra
Authors: Sotnikova Yu , Mikhailov A , Mufakharov T , Mingaliev M , Bursov N , Semenova T , Stolyarov V , Udovitskiy R , Kudryashova A , Erkenov A 
Published: July 2021

ABSTRACT
We present the radio properties of optically selected quasars with z ≥ 3. The complete sample consists of 102 quasars with a flux density level S1.4 ≥ 100 mJy in a declination range −35° ≤ Dec. ≤ +49°. The observations were obtained in 2017–2020 using the radio telescope RATAN-600. We measured flux densities at six frequencies 1.2, 2.3, 4.7, 8.2, 11.2, and 22 GHz quasi-simultaneously with uncertainties of 9–31 per cent. The detection rate is 100, 89, and 46 per cent at 4.7, 11.2, and 22 GHz, respectively. We have analysed the averaged radio spectra of the quasars based on the RATAN and literature data. We classify 46 per cent of radio spectra as peaked-spectrum, 24 per cent as flat, and none as ultra-steep spectra (α ≤ −1.1). The multifrequency data reveal that a peaked spectral shape (PS) is a common feature for bright high-redshift quasars. This indicates the dominance of bright compact core emission and the insignificant contribution of extended optically thin kpc-scale components in observed radio spectra. Using these new radio data, the radio loudness log  R was estimated for 71 objects with a median value of 3.5, showing that the majority of the quasars are highly radio-loud with log  R &gt; 2.5. We have not found any significant correlation between z and α. Several new megahertz- peaked spectrum (MPS) and gigahertz- peaked spectrum (GPS) candidates are suggested. Further studies of their variability and additional low-frequency observations are needed to classify them precisely.
Binary evolution pathways of blue large-amplitude pulsators
Authors: Byrne C M , Stanway E R , Eldridge J J 
Published: July 2021

ABSTRACT
Blue large-amplitude pulsators (BLAPs) are a recently discovered class of pulsating star, believed to be proto-white dwarfs, produced by mass stripping of a red giant when it has a small helium core. An outstanding question is why the stars in this class of pulsator seem to form two distinct groups by surface gravity, despite predictions that stars in the gap between them should also pulsate. We use a binary population synthesis model to identify potential evolutionary pathways that a star can take to become a BLAP. We find that BLAPs can be produced either through common envelope evolution or through Roche lobe overflow, with a main-sequence star or an evolved compact object being responsible for the envelope stripping. The mass distribution of the inferred population indicates that fewer stars would be expected in the range of masses intermediate to the two known groups of pulsators, suggesting that the lack of observational discoveries in this region may be a result of the underlying population of pre-white dwarf stars. We also consider metallicity variation and find evidence that BLAPs at Z = 0.010 (half-solar) would be pulsationally unstable and may also be more common. Based on this analysis, we expect the Milky Way to host around 12 000 BLAPs and we predict the number density of sources expected in future observations such as the Legacy Survey of Space and Time at the Vera Rubin Observatory.
Prospects of newly detecting nearby star-forming galaxies by the Cherenkov Telescope Array
Authors: Shimono Naoya , Totani Tomonori , Sudoh Takahiro 
Published: July 2021

ABSTRACT
Prospects of the Cherenkov Telescope Array (CTA) for the study of very high energy gamma-ray emission from nearby star-forming galaxies are investigated. In the previous work, we constructed a model to calculate luminosity and energy spectrum of pion-decay gamma-ray emission produced by cosmic ray interaction with the interstellar medium (ISM), from four physical quantities of galaxies [star formation rate (SFR), gas mass, stellar mass, and effective radius]. The model is in good agreement with the observed GeV–TeV emission of several nearby galaxies. Applying this model to nearby galaxies that are not yet detected in TeV (mainly from the KINGFISH catalogue), their hadronic gamma-ray luminosities and spectra are predicted. We identify galaxies of the highest chance of detection by CTA, including NGC 5236, M33, NGC 6946, and IC 342. Concerning gamma-ray spectra, NGC 1482 is particularly interesting because our model predicts that this galaxy is close to the calorimetric limit and its gamma-ray spectral index in GeV–TeV is close to that of cosmic ray protons injected into ISM. Therefore, this galaxy may be detectable by CTA even though its GeV flux is below the Fermi Large Area Telescope sensitivity limit. In the TeV regime, most galaxies are not in the calorimetric limit, and the predicted TeV flux is lower than that assuming a simple relation between the TeV luminosity and SFR of M82 and NGC 253, typically by a factor of 15. This means that a more sophisticated model beyond the calorimetric limit assumption is necessary to study TeV emission from star-forming galaxies.
SRG/eROSITA discovery of a large circular SNR candidate G116.6−26.1: SN Ia explosion probing the gas of the Milky Way halo?
Authors: Churazov E M , Khabibullin I I , Bykov A M , Chugai N N , Sunyaev R A , Zinchenko I I 
Published: July 2021

ABSTRACT
We report a discovery of a new X-ray-selected supernova remnant (SNR) candidate SRGe J0023+3625 = G116.6−26.1 found in the SRG/eROSITA all-sky survey. The source features a large angular extent (∼4° in diameter), nearly circular shape, and X-ray spectrum dominated by emission lines of helium- and hydrogen-like oxygen. It lacks bright counterparts of similar extent at other wavelengths which could be unequivocally associated with it. Given the relatively high Galactic latitude of the source, b ≈ −26°, we interpret these observational properties as an indication of the off-disc location of this SNR candidate. Namely, we propose that this object originated from a Type Ia supernotva which exploded some 40 000 yr ago in the low density ($\sim 10^{-3}\, {\rm cm^{-3}}$) and hot ($\sim (1{-}2)\times 10^6\, {\rm K}$) gas of the Milky Way halo at a distance of ∼3 kpc from the Sun. The low density of the halo gas implies that the cooling and collisional ionization equilibrium (CEI) time-scales downstream of the forward shock are much longer than the age of the SNR. This results in a relatively soft spectrum, reflecting pre-shock ionization state of the gas, and strong boost in the plasma emissivity (compared to CEI) due to enhanced collisional excitation through the increased electron temperature. If confirmed, such a rare object would provide us with a unique ‘in situ’ probe of physical conditions (density, temperature and metallicity) near the interface between the Milky Way’s disc and the halo.
Multiwavelength observations reveal a faint candidate black hole X-ray binary in IGR J17285−2922
Authors: Stoop M , van den Eijnden J , Degenaar N , Bahramian A , Swihart S J , Strader J , Jiménez-Ibarra F , Muñoz-Darias T , Armas Padilla M , Shaw A W , Maccarone T J , Wijnands R , Russell T D , Santisteban J V Hernández , Miller-Jones J C A , Russell D M , Maitra D , Heinke C O , Sivakoff G R , Lewis F , Bramich D M 
Published: July 2021

ABSTRACT
IGR J17285−2922 is a known X-ray binary with a low peak 2–10 keV X-ray luminosity of ∼ 1036 erg s−1 during outburst. IGR J17285−2922 exhibited two outbursts in 2003 and 2010 and went into outburst again in 2019. We have monitored this ∼ 4-month long 2019 outburst with Swift in X-ray and the Very Large Array in radio. We have also obtained four optical spectra with the Gran Telescopio Canarias and Southern Astrophysical Research Telescope, three optical photometry measurements with the Las Cumbres Observatory, and one near-infrared spectrum with the Gemini South telescope. The ratio between its X-ray and radio luminosity is consistent with both samples of neutron star and black hole (BH) X-ray binaries, while the ratio between the X-ray and optical luminosity is consistent with BH X-ray binaries. Studying the evolution of its X-ray power-law index throughout the outburst, we find additional evidence for a BH as compact object. The four optical spectra show no H α emission and the nIR spectrum shows no Brγ emission, suggesting that the donor star could be hydrogen-poor and hence that IGR J17285−2922 might have an ultracompact binary orbit. The shape of the X-ray light curve is well described by an exponential, followed by a linear decay, from which we obtain a relation between the orbital period Porb and the binary mass ratio. We discuss how this relation is consistent with theoretical predictions and known ultracompact X-ray binaries. Lastly, we discuss how the observed properties are reminiscent of short-Porb BH X-ray binaries.
Optically detected galaxy cluster candidates in the AKARI North Ecliptic Pole field based on photometric redshift from the Subaru Hyper Suprime-Cam
Authors: Huang Ting-Chi , Matsuhara Hideo , Goto Tomotsugu , Santos Daryl Joe D , Ho Simon C-C , Kim Seong Jin , Hashimoto Tetsuya , Ikeda Hiroyuki , Oi Nagisa , Malkan Matthew A , Pearson William J , Pollo Agnieszka , Serjeant Stephen , Shim Hyunjin , Miyaji Takamitsu , Hwang Ho Seong , Durkalec Anna , Poliszczuk Artem , Greve Thomas R , Pearson Chris , Toba Yoshiki , Lee Dongseob , Kim Helen K , Toft Sune , Jeong Woong-Seob , Enokidani Umi 
Published: July 2021

ABSTRACT
Galaxy clusters provide an excellent probe in various research fields in astrophysics and cosmology. However, the number of galaxy clusters detected so far in the AKARI North Ecliptic Pole (NEP) field is limited. In this work, we provide galaxy cluster candidates in the AKARI NEP field with the minimum requisites based only on the coordinates and photometric redshift (photo-z) of galaxies. We used galaxies detected in five optical bands (g, r, i, z, and Y) by the Subaru Hyper Suprime-Cam (HSC), with additional data from the u band obtained from the Canada-France-Hawaii Telescope (CFHT) MegaPrime/MegaCam, and from the IRAC1 and IRAC2 bands from the Spitzer space telescope for photo-z estimation. We calculated the local density around every galaxy using the 10th-nearest neighbourhood. Cluster candidates were determined by applying the friends-of-friends algorithm to over-densities. A total of 88 cluster candidates containing 4390 member galaxies below redshift 1.1 in 5.4 deg2 were identified. The reliability of our method was examined through false-detection tests, redshift-uncertainty tests, and applications on the Cosmic Evolution Survey (COSMOS) data, giving false-detection rates of 0.01 to 0.05 and a recovery rate of 0.9 at high richness. Three X-ray clusters previously observed by ROSAT and Chandra were recovered. The cluster galaxies show a higher stellar mass and lower star formation rate compared with the field galaxies in two-sample Z-tests. These cluster candidates are useful for environmental studies of galaxy evolution and future astronomical surveys in the NEP, where AKARI has performed unique nine-band mid-infrared photometry for tens of thousands of galaxies.