Miracle-dz/UniFAR-FTUs huggingface dataset:
The metal contents of two groups of galaxies

Context. The hot gas in clusters and groups of galaxies is continuously being enriched with metals from supernovae and stars. It is well established that the enrichment of the gas with elements from oxygen to iron is mainly caused by supernova explosions. The origins of nitrogen and carbon are still being debated. Possible candidates include massive, metal-rich stars, early generations of massive stars, intermediate- or low-mass stars and asymptotic giant branch (AGB) stars. Aims. In this paper we accurately determine the metal abundances of the gas in the groups of galaxies NGC 5044 and NGC 5813, and discuss the nature of the objects that create these metals. We mainly focus on carbon and nitrogen. Methods. We use spatially-resolved high-resolution X-ray spectroscopy from XMM-Newton. For the spectral fitting, multitemperature hot gas models are used. Results. The abundance ratios of carbon over oxygen and nitrogen over oxygen that we find are high compared to the ratios in the stars in the disk of our Galaxy. The oxygen and nitrogen abundances we derive are similar to what has been found in earlier work on other giant ellipticals in comparable environments. We show that the iron abundances in both our sources have a gradient along the cross-dispersion direction of the reflection grating spectrometer (RGS). Conclusions. We conclude that it is unlikely that the creation of nitrogen and carbon takes place in massive stars, which end their lives as core-collapse supernovae, enriching the medium with oxygen because oxygen should then also be enhanced. Therefore we favour low- and intermediate-mass stars as sources of these elements. The abundances in the hot gas can be explained best by a 30‐40% contribution of type Ia supernovae based on the measured oxygen and iron abundances and under the assumption of a Salpeter initial mass function (IMF).
Probability in Banach Spaces: Isoperimetry and Processes

Notation. - 0. Isoperimetric Background and Generalities. - 1. Isoperimetric Inequalities and the Concentration of Measure Phenomenon. - 2. Generalities on Banach Space Valued Random Variables and Random Processes. - I. Banach Space Valued Random Variables and Their Strong Limiting Properties. - 3. Gaussian Random Variables. - 4. Rademacher Averages. - 5. Stable Random Variables. - 6 Sums of Independent Random Variables. - 7. The Strong Law of Large Numbers. - 8. The Law of the Iterated Logarithm. - II. Tightness of Vector Valued Random Variables and Regularity of Random Processes. - 9. Type and Cotype of Banach Spaces. - 10. The Central Limit Theorem. - 11. Regularity of Random Processes. - 12. Regularity of Gaussian and Stable Processes. - 13. Stationary Processes and Random Fourier Series. - 14. Empirical Process Methods in Probability in Banach Spaces. - 15. Applications to Banach Space Theory. - References.
The Statistical Analyses of the White-Light Flares: Two Main Results About Flare Behaviours

We present two main results, based on the models and the statistical analyses of 1672 U-band flares. We also discuss the behaviours of the white-light flares. In addition, the parameters of the flares detected from two years of observations on CR Dra are presented. By comparing with the flare parameters obtained from other UV Ceti type stars, we examine the behaviour of optical flare processes along the spectral types. Moreover, we aimed, using large white-light flare data,to analyse the flare time-scales in respect to some results obtained from the X-ray observations. Using the SPSS V17.0 and the GraphPad Prism V5.02 software, the flares detected from CR Dra were modelled with the OPEA function and analysed with t-Test method to compare similar flare events in other stars. In addition, using some regression calculations in order to derive the best histograms, the time-scales of the white-light flares were analysed. Firstly, CR Dra flares have revealed that the white-light flares behave in a similar way as their counterparts observed in X-rays. As seen in X-ray observations, the electron density seems to be a dominant parameter in white-light flare process, too. Secondly, the distributions of the flare time-scales demonstrate that the number of observed flares gets a maximum value in some particular ratios, which are 0.5 or its multiples, and especially positive integers. The thermal processes might be dominant for these white-light flares, while non-thermal processes might be dominant in the others. To reach better results for the behaviour of the white-light flare process along the spectral types, much more stars in a wide spectral range, from the spectral type dK5e to dM6e, must be observed in the white-light flare patrols.
Using dwarf satellite proper motions to determine their origin

The highly organised distribution of satellite galaxies su rrounding the Milky Way is a serious challenge to the concordance cosmological model. Perhaps the only remaining solution, in this framework, is that the dwarf satellite galaxies fall in to the Milky Way’s potential along one or two filaments, which may or may not plausibly reproduce the observed distribution. Here we test this scenario by making use of the proper motions of the Fornax, Sculptor, Ursa Minor and Carina dwarf spheroidals, and trace their orbits back through several variations of the Milky Way’s potential and account for dynamical frict ion. The key parameters are the proper motions and total masses of the dwarf galaxies. Using a simple model we find no tenable set of parameters that can allow Fornax to be consistent with filamentary infall, mainly because the 1σ error on its proper motion is relatively small. The other thr ee must walk a tightrope between requiring a small pericentre (less than 20 kpc) to lose enough orbital energy to dynamical friction and avoiding being tidally disrupted. We then employed a more realistic model with host halo mass accretion, and found that the four dwarf galaxies must have fallen in at least 5 Gyrs ago. This time interval is longe r than organised distribution is expected to last before being erased by the randomisation of the satellite orbits.
Positive Semidefiniteness and Global Well-Posedness of Solutions to the Gross-Pitaevskii Hierarchy

We study the cubic defocusing Gross-Pitaevskii (GP) hierarchy in ${\mathbb R}^3$. In a first step, we derive the GP hierarchy from a bosonic $N$-particle system in GP scaling as $N\rightarrow\infty$, in the strong topology corresponding to the spaces used by Klainerman and Machedon in \cite{KM}. In particular, our approach removes a condition on the regularity of initial data used in \cite{CPBBGKY}. Furthermore, we prove that positive semidefiniteness of marginal density matrices is preserved over time; so far, this property has been known only for special cases. This, combined with previous results in \cite{CPHE}, implies the global well-posedness of solutions.
DISCOVERY OF A 7 mHz X-RAY QUASI-PERIODIC OSCILLATION FROM THE MOST MASSIVE STELLAR-MASS BLACK HOLE IC 10 X-1

We report the discovery with XMM-Newton of an ≈7 mHz X-ray (0.3–10.0 keV) quasi-periodic oscillation (QPO) from the eclipsing, high-inclination black hole binary IC 10 X-1. The QPO is significant at >4. 33σ confidence level and has a fractional amplitude (% rms) and a quality factor, Q ≡ ν/Δν, of ≈11 and 4, respectively. The overall X-ray (0.3–10.0 keV) power spectrum in the frequency range 0.0001–0.1 Hz can be described by a power-law with an index of ≈ − 2, and a QPO at 7 mHz. At frequencies ≳0.02 Hz there is no evidence for significant variability. The fractional amplitude (rms) of the QPO is roughly energy-independent in the energy range of 0.3–1.5 keV. Above 1.5 keV the low signal-to-noise ratio of the data does not allow us to detect the QPO. By directly comparing these properties with the wide range of QPOs currently known from accreting black hole and neutron stars, we suggest that the 7 mHz QPO of IC 10 X-1 may be linked to one of the following three categories of QPOs: (1) the “heartbeat” mHz QPOs of the black hole sources GRS 1915+105 and IGR J17091−3624, or (2) the 0.6–2.4 Hz “dipper QPOs” of high-inclination neutron star systems, or (3) the mHz QPOs of Cygnus X-3.
MEASURING X-RAY VARIABILITY IN FAINT/SPARSELY SAMPLED ACTIVE GALACTIC NUCLEI

We study the statistical properties of the normalized excess variance of variability process characterized by a “red-noise” power spectral density (PSD), as in the case of active galactic nuclei (AGNs). We perform Monte Carlo simulations of light curves, assuming both a continuous and a sparse sampling pattern and various signal-to-noise ratios (S/Ns). We show that the normalized excess variance is a biased estimate of the variance even in the case of continuously sampled light curves. The bias depends on the PSD slope and on the sampling pattern, but not on the S/N. We provide a simple formula to account for the bias, which yields unbiased estimates with an accuracy better than 15%. We show that the normalized excess variance estimates based on single light curves (especially for sparse sampling and S/N < 3) are highly uncertain (even if corrected for bias) and we propose instead the use of an “ensemble estimate,” based on multiple light curves of the same object, or on the use of light curves of many objects. These estimates have symmetric distributions, known errors, and can also be corrected for biases. We use our results to estimate the ability to measure the intrinsic source variability in current data, and show that they could also be useful in the planning of the observing strategy of future surveys such as those provided by X-ray missions studying distant and/or faint AGN populations and, more in general, in the estimation of the variability amplitude of sources that will result from future surveys such as Pan-STARRS and LSST.
Correlation, Breit, and QED effects in spectra of Mg-like ions

We calculated spectra of the first six members of the Mg-like isoelectronic sequence using different approximations. The most accurate results were obtained with the configuration interaction + all order method (CI+AO), which provided relative accuracy for transition energies on the level of 0.1\%, or better. On this level of accuracy the Breit and QED corrections become important for the systems with nuclear charge $Z\gtrsim 20$. The retardation part of the Breit interaction and QED corrections for the partial waves with $l\ne 0$ are still too small to be important.
CGNet: Robotic Grasp Detection in Heavily Cluttered Scenes

Robotic grasp technology has been widely used. However, the robotic grasp in cluttered scene is still a challenging problem. In this regard, this article proposes a novel robotic grasp detection method cluttered grasp network (CGNet). First, to make the network fully focus on important features, this article proposes a novel attention module two branches squeeze-and-excitation residual network (TSE-ResNet) and uses it as the backbone to extract features. Then, to detect grasp rectangle more accurately, a novel grasp region proposal module is proposed, which can well utilize the multiscale features and refine the grasp region. Finally, a novel position focal loss is proposed to detect the rotation angle of the grasp rectangle, and can well solve the problem of discontinuous rotation angle. The CGNet is trained and tested on the GraspNet-1Billion dataset and Cornell dataset, achieving 87.9 and 97.9% accuracy, respectively. Moreover, to test the effectiveness, the CGNet is also tested on the Multiobject dataset and Clutter dataset. The detection results show that the CGNet can well detect the grasp rectangle when faces unseen objects. The ablation experiments are also performed to verify the performance of proposed modules. The experimental results show that the proposed modules can improve the detection accuracy in the cluttered scene. Finally, to evaluate the generalization of the CGNet, it is also evaluated in the real world, and applied to the grasp task of a real Baxter robot, and obtained a grasping success rate of 91.7%.
MODEL-INDEPENDENT ESTIMATIONS FOR THE CURVATURE FROM STANDARD CANDLES AND CLOCKS

Model-independent estimations for the spatial curvature of the universe not only provide a test for the fundamental assumption of the Copernican principle, but also can effectively break the degeneracy between curvature and dark-energy properties. In this paper, we propose to achieve model-independent constraints on the spatial curvature from observations of standard candles and standard clocks, without assuming any fiducial cosmology or other priors. We find that, for the popular Union2.1 observations of Type Ia supernovae (SNe Ia), the spatial curvature is constrained to be . For the latest joint light-curve analysis of SNe Ia observations, we obtain . It is suggested that these results are in excellent agreement with a spatially flat universe. Moreover, compared to other approaches aiming for model-independent estimations of spatial curvature, this method also achieves constraints with competitive precision.
The growth of the galaxy cluster Abell 85: mergers, shocks, stripping and seeding of clumping

We present the results of deep Chandra, XMM-Newton and Suzaku observations of the nearby galaxy cluster Abell 85, which is currently undergoing at least two mergers, and in addition shows evidence for gas sloshing which extends out to r ~ 600 kpc. One of the two infalling subclusters, to the south of the main cluster center, has a dense, X-ray bright cool core and a tail extending to the southeast. The northern edge of this tail is strikingly smooth and sharp (narrower than the Coulomb mean free path of the ambient gas) over a length of 200 kpc, while toward the southwest the boundary of the tail is blurred and bent, indicating a difference in the plasma transport properties between these two edges. The thermodynamic structure of the tail strongly supports an overall northwestward motion. We propose, that a sloshing-induced tangential, ambient, coherent gas flow is bending the tail eastward. The brightest galaxy of this subcluster is at the leading edge of the dense core, and is trailed by the tail of stripped gas, suggesting that the cool core of the subcluster has been almost completely destroyed by the time it reached its current radius of r ~ 500 kpc. The surface-brightness excess, likely associated with gas stripped from the infalling southern subcluster, extends toward the southeast out to at least r_500 of the main cluster, indicating that the stripping of infalling subclusters may seed gas inhomogeneities. The second merging subcluster appears to be a diffuse non-cool core system. Its merger is likely supersonic with a Mach number of ~ 1.4.
Chemoprevention of 4NQO-Induced Mouse Tongue Carcinogenesis by AKT Inhibitor through the MMP-9/RhoC Signaling Pathway and Autophagy

Oral cancer (OC), the most common cancer in the head and neck, which has a poor prognosis, histopathologically follows a stepwise pattern of hyperplasia, dysplasia, and cancer. Blocking the progression of OC in the precancer stage could greatly improve the survival and cure rates. AKT protein plays a critical role in the signal transduction of cancer cells, and we found that AKT was overexpressed in human OC samples through analysis of TCGA database. Therefore, this study is aimed at investigating the chemopreventive effect of an AKT inhibitor (MK2206 2HCl) on OC. In vivo, we established a 4-nitroquinoline-1-oxide- (4NQO-) induced mouse tongue carcinogenesis model to investigate the potential chemopreventive effect of MK2206 2HCl on mouse OC resulting from 4NQO. The results showed that MK2206 2HCl could significantly reduce the incidence rate and growth of OC, inhibit the transformation of dysplasia to cancer in the 4NQO-induced mouse tongue carcinogenesis model, and simultaneously markedly suppress cell proliferation, angiogenesis, and mast cell (MC) infiltration in 4NQO-induced mouse tongue cancers. In vitro, our results revealed that MK2206 2HCl could also inhibit oral squamous cell carcinoma (OSCC) cell malignant biological behaviors, including cell proliferation, colony formation, cell invasion, and migration, while promoting apoptosis. Mechanistic studies revealed that MK2206 2HCl suppressed matrix metalloproteinase 9 (MMP-9) and RhoC expression and promoted autophagy gene LC3 II expression. In summary, our findings demonstrated the chemopreventive effect of MK2206 2HCl on the 4NQO-induced mouse tongue carcinogenesis model, which likely has an underlying mechanism mediated by the MMP-9/RhoC signaling pathway and autophagy.
CEBI WORKING PAPER SERIES

This paper utilizes high-quality transaction data from the largest bank in Denmark to study what drives the demand for high-cost consumption loans. I investigate the extent to which adverse events drive loan demand, or if it is more likely to be explained by borrowers’ personality traits. I find no evidence suggesting that borrowers suffer expenditure, health or social shocks at the time of borrowing. There are indications that some borrowers suffer income shocks, but the magnitude is too modest for this to be an important determinant of aggregate loan demand. Instead, I find evidence pointing towards a dominant role for borrowers’ personality traits in explaining loan demand. Using paycheck sensitivity as a proxy, I show that high-cost borrowers appear to be significantly more present-biased than other consumers. I also document that high-cost borrowers are more prone to temptation spending as they spend much more on gambling than other consumers, both leading up to and when borrowing for the first time. Further, I find that high-cost borrowers persistently spend more than they earn and that this gap widens further as they approach the time of their first high-cost loan. Lastly, I document a large increase in non-essential spending around the time of borrowing. Taken together, the results indicate that high-cost borrowers have self-control problems and that high-cost loans are likely used to finance impulse spending or function as a way to prolong a credit-financed spell of overconsumption.
Periodically bursting edge states in plane Poiseuille flow

We investigate the laminar-turbulent boundary in plane Poiseuille flow by the method of edge tracking. In short and narrow computational domains we find for a wide range of Reynolds numbers that all states in the boundary converge to a periodic orbit with a period of the order of 10 3 ? > time units. The attracting states in these small domains are periodically extended in the spanwise and streamwise directions, but always localized to one side of the channel in the normal direction. In wider domains the edge states are localized in the spanwise direction as well. The periodic motion found in the small domains then induces a large variety of dynamical activity that is similar to that found in the asymptotic suction boundary layer.
THE MID-INFRARED LUMINOSITIES OF NORMAL GALAXIES OVER COSMIC TIME

Modern population synthesis models estimate that 50% of the rest-frame K-band light is produced by thermally pulsing asymptotic giant branch (TP-AGB) stars during the first Gyr of a stellar population, with a substantial fraction continuing to be produced by the TP-AGB over a Hubble time. Between 0.2 and 1.5 Gyr, intermediate-mass stars evolve into TP-AGB C stars which, due to significant amounts of circumstellar dust, emit half their energy in the mid-IR. We combine these results using published mid-IR colors of Galactic TP-AGB M and C stars to construct simple models for exploring the contribution of the TP-AGB to 24 μm data as a function of stellar population age. We compare these empirical models with an ensemble of galaxies in the Chandra Deep Field South from z = 0 to z = 2, and with high-quality imaging in M81. Within the uncertainties, the TP-AGB appears responsible for a substantial fraction of the mid-IR luminosities of galaxies from z = 0 to z = 2, the maximum redshift to which we can test our hypothesis, while, at the same time, our models reproduce much of the detailed structure observed in mid-IR imaging of M81. The mid-IR is a good diagnostic of star formation over timescales of ∼1.5 Gyr, but this implies that ongoing star formation rates at z = 1 may be overestimated by factors of ∼1.5–6, depending on the nature of star formation events. Our results, if confirmed through subsequent work, have strong implications for the star formation rate density of the universe and the growth of stellar mass over time.
The Effectiveness and Safety of Abelmoschus manihot in Treating IgA Nephropathy: A Systematic Review and Meta-Analysis

Introduction IgA nephropathy (IgAN) is a common issue. In China, Abelmoschus manihot (AM) is widely used in the treatment of IgAN. However, their combined effectiveness and safety for this purpose have not yet been explored. AM is an effective medicine for treating IgAN. This meta-analysis aimed to evaluate the effectiveness of AM for IgAN. Materials and Methods The Cochrane Library, PubMed, EMBASE, Allied and Complementary Medicine Database (AMED), Chinese Biomedical Literature Database (CBM), Chinese National Knowledge Infrastructure Database (CNKI), Chinese Science and Technique Journals Database (VIP), and the Wanfang Database were searched from their inceptions to June 2021. Random clinical trials (RCTs) comparing the effects of AM treatment in patients with IgAN were included. The study evaluated the efficacy or effectiveness of AM for IgAN and had clear outcome data, such as total effectiveness rate or proteinuria. Results A total of 11 RCTs with 850 participants were included in this meta-analysis. The results of the meta-analysis showed that, compared with that of the conventional therapy alone, being combined with conventional treatment was significantly more effective for the total efficacy rate (OR = 4.33; 95% CI = 2.66, 7.04; P < 0.00001) and proteinuria (MD = −0.41 g/24 h; 95% CI = −0.44, −0.38; P < 0.00001) but had no effect on serum creatinine (Scr) (MD = −2.23 μmol/L; 95% CI = −5.90, 1.45; P=0.24), eGFR (MD = −0.45 mL/min·1.73 m2; 95% CI = −1.24, 2.13; P=0.60), Bun (MD = −0.22 mmol/L; 95% CI = −0.59, 0.14; P=0.23), systolic blood pressure (MD = −0.04 mmHg; 95% CI = −2.59, 2.51; P=0.98), diastolic blood pressure (MD = −0.34 mmHg, 95% CI = −1.65, 2.33; P=0.74), systolic blood pressure (MD = −0.04 mmHg, 95% CI = −2.59, 2.51; P=0.98), or serum albumin (MD = 1.70 g/L, 95% CI = −1.06, 4.45; P=0.23). Conclusions AM provided additional benefits to proteinuria individuals with IgAN. However, due to the high clinical heterogeneity and small sample size of the included trials, future studies should conduct more rigorous RCTs on the clinical efficacy and safety of AM and RCTs with a larger sample size involving multicenters.