Miracle-dz/UniFAR-FTUs huggingface dataset:
Genesis of the Sinongduo Carbonate‐hosted Pb‐Zn‐Ag Deposit in the Central Lhasa Terrane, Tibet

The Sinongduo mining region includes two types of mineralizations: the epithermal and the carbonate‐hosted Pb‐Zn‐Ag deposits. Despite being studied for many years, the ore formation process and genesis of the carbonate‐hosted Pb‐Zn‐Ag deposits remain poorly understood. The Pb‐Zn‐Ag ore bodies occur as veins and are hosted by limestone and dolostone of the Permian Xiala Formation. Three sulfide mineralization substages have been identified at the Sinongduo carbonate‐hosted deposit. Indium coupled with Cu, Co and Sn was incorporated into sphalerite as substitutions: 2Zn2+ ↔ Cu+ + In3+, (3n/2 + 1)Zn2+ ↔ Co2+ + nIn3+ or (2n + 1)Zn2+ ↔ Co2+ + n(Cu+ + In3+) (n > 1) and 4Zn2+ ↔ Sn2+ + 2In3+. Sphalerite and pyrite in the mineralization stage display δ34S values in a narrow range of +5.7‰ to +11.3‰, which are similar to those of Palaeocene igneous rocks, indicative of a magmatic source of sulfur. We present systematic carbon‐hydrogen‐oxygen isotope results that further support a magmatic source for the ore‐forming fluids that were influenced by meteoric water. Furthermore, the Pb isotope compositions of sulfide minerals in the Sinongduo carbonate‐hosted deposit overlap with the values of coeval Linzizong volcanic rocks and are similar to those of Indian Ocean sediments, indicating upper crustal sources of metals. We conclude that the Sinongduo carbonate‐hosted Pb‐Zn‐Ag deposit is a medium‐ to low‐temperature magmatic‐hydrothermal deposit related to Linzizong magmatism.
LOCAL INTERSTELLAR HYDROGEN'S DISAPPEARANCE AT 1 AU: FOUR YEARS OF IBEX IN THE RISING SOLAR CYCLE

NASA's Interstellar Boundary Explorer (IBEX) mission has recently opened a new window on the interstellar medium (ISM) by imaging neutral atoms. One “bright” feature in the sky is the interstellar wind flowing into the solar system. Composed of remnants of stellar explosions as well as primordial gas and plasma, the ISM is by no means uniform. The interaction of the local ISM with the solar wind shapes our heliospheric environment with hydrogen being the dominant component of the very local ISM. In this paper, we report on direct sampling of the neutral hydrogen of the local ISM over four years of IBEX observations. The hydrogen wind observed at 1 AU has decreased and nearly disappeared as the solar activity has increased over the last four years; the signal at 1 AU has dropped off in 2012 by a factor of ∼8 to near background levels. The longitudinal offset has also increased with time presumably due to greater radiation pressure deflecting the interstellar wind. We present longitudinal and latitudinal arrival direction measurements of the bulk flow as measured over four years beginning at near solar minimum conditions. The H distribution we observe at 1 AU is expected to be different from that outside the heliopause due to ionization, photon pressure, gravity, and filtration by interactions with heliospheric plasma populations. These observations provide an important benchmark for modeling of the global heliospheric interaction. Based on these observations we suggest a further course of scientific action to observe neutral hydrogen over a full solar cycle with IBEX.
Curvature-Free Margulis Lemma for Gromov-Hyperbolic Spaces

We prove curvature-free versions of the celebrated Margulis Lemma. We are interested by both the algebraic aspects and the geometric ones, with however an emphasis on the second and we aim at giving quantitative (computable) estimates of some important invariants. Our goal is to get rid of the pointwise curvature assumptions in order to extend the results to more general spaces such as certain metric spaces. Essentially the upper bound on the curvature is replaced by the assumption that the space is _ $\delta$-hyperbolic in the sense of Gromov and the lower bound of the curvature by an upper bound on the entropy which we recall the definition.
The SUSY Yang-Mills plasma in a $T$-matrix approach

The thermodynamic properties of ${\cal N}=1$ supersymmetric Yang-Mills theory with an arbitrary gauge group are investigated. In the confined range, we show that identifying the bound state spectrum with a Hagedorn one coming from non-critical closed superstring theory leads to a prediction for the value of the deconfining temperature $T_c$ that agrees with recent lattice data. The deconfined phase is studied by resorting to a $T$-matrix formulation of statistical mechanics in which the medium under study is seen as a gas of quasigluons and quasigluinos interacting nonperturbatively. Emphasis is put on the temperature range (1-5)~$T_c$, where the interaction are expected to be strong enough to generate bound states. Binary bound states of gluons and gluinos are indeed found to be bound up to 1.4 $T_c$ for any gauge group. The equation of state is then computed numerically for SU($N$) and $G_2$, and discussed in the case of an arbitrary gauge group. It is found to be nearly independent of the gauge group and very close to that of non-supersymmetric Yang-Mills when normalized to the Stefan-Boltzmann pressure and expressed as a function of $T/T_c$.
Effect of reduced graphene oxide, multi-walled carbon nanotubes and their mixtures on the electrical conductivity and mechanical properties of a polymer composite with a segregated structure

The development of new electrically conductive polymer composites is one of the most important research areas of composite materials science community nowadays. This work is devoted to the preparation and study of electrically conductive polymer composites with a segregated network structure with mixtures of reduced graphene oxide/multi-walled carbon nanotubes (rGO/MWCNTs) in various ratios. At a fixed value of the total mass fraction of rGO/MWCNTs (1 wt.%), the set of samples with different rGO/MWCNTs ratio was obtained and examined via scanning electron microscopy, wide range dielectric spectroscopy and tested under compression. We have shown that the use of graphene oxide in a mixture with MWCNTs makes it possible to significantly improve the uniformity of MWCNTs distribution during the formation of a filler layer on polymer particles, which leads to an increase in the electrical conductivity of the composites in comparison with samples containing only rGO or MWCNTs. It was also shown adding 1 wt. % of rGO to the polymer increases the elastic modulus by 18% compared to the pure polymer. In turn, adding of MWCNTs, there is a drop in the elastic modulus by a quarter. It was found that fillers do not affect the plastic flow initiation stress of the material, which is 21 ± 1 MPa. Graphical Abstract
Corrective effect of many-body interactions in dynamical friction

Dynamical friction is a fundamental and important phenomenon in astrophysics. The Chandrasekhar formula is a well-known analytical estimation of the effect. However, current astrophysicists have realized that the formula is not correct in some cases because of several approximations used in the formulation and/or complex non-linearities in the real Universe. For example, it has been indicated that dynamical friction does not work in cored density profiles (constant density in the central region) despite the Chandrasekhar formula predicting drag force even for constant densities. In the first half of this paper, I show by N-body simulations that many-body interactions are also important in actual dynamical friction though derivation of the Chandrasekhar formula is based on the assumption of two-body interaction. In the simulation, the many-body interactions are caused by a very small number of field particles corotating with a perturber. However, the contribution from the many-body interactions accounts for a non-negligible fraction of the actual dynamical friction. In the second half of the paper, I discuss why the cored profiles suppress the dynamical friction. One possible explanation is that the corrective effect of the many-body interactions drives orbital motion of the perturber. The cessation of dynamical friction by this corrective effect would be feasible even in shallow cusp density profiles although the shallow cusp may evolve into a constant density.
Do we need another coffee house? The amenity space and the evolution of neighborhoods

Neighborhoods populated by amenities, such as restaurants, cafes, and libraries, are considered to be a key property of desirable cities. Yet, despite the global enthusiasm for amenity-rich neighborhoods, little is known about the empirical laws governing the colocation of amenities at the neighborhood scale. Here, we contribute to our understanding of the naturally occurring neighborhood-scale agglomerations of amenities observed in cities by using a dataset summarizing the precise location of millions of amenities. We use this dataset to build the network of co-location of amenities, or Amenity Space, by first introducing a clustering algorithm to identify neighborhoods, and then using the identified neighborhoods to map the probability that two amenities will be co-located in one of them. Finally, we use the Amenity Space to build a recommender system that identifies the amenities that are missing in a neighborhood given its current pattern of specialization. This opens the door for the construction of amenity recommendation algorithms that can be used to evaluate neighborhoods and inform their improvement and development.
Alignment of brightest cluster galaxies with their host clusters

We examine the alignment between brightest cluster galaxies (BCGs) and their host clusters in a sample of 7031 clusters with 0.08 0.65 mag brighter than the mean of the second- and third-ranked galaxies) show stronger alignment than do clusters with less dominant BCGs at the 4. 4σ level. Rich clusters show a stronger alignment than do poor clusters at the 2. 3σ level. Low-redshift clusters (z 0.26) clusters, with a difference significant at the 3. 0σ level. Our results do not depend on the algorithm used to select the cluster sample, suggesting that they are not biased by systematics of either algorithm. The correlation between BCG dominance and cluster alignment may be a consequence of the hierarchical merging process which forms the cluster. The observed redshift evolution may follow from secondary infall at late redshifts.
Determinants of survival time among HIV-infected patients receiving care at antiretroviral therapy (art) clinic of a public hospital, Ethiopia

Introduction: Even if there are different barriers to HIV testing in developing countries, timely access to care and early diagnosis improves the clinical course of the disease, reduces the transmission rates, and prolongs the survival time of patients. Objectives: This study aimed to investigate the potential predictors of survival time in a cohort of HIV-infected patients on ART using the parametric survival model perspective. Data and Methods: A hospital-based retrospective cohort charts-review study design was conducted on 647 patients from a public referral hospital in North-Central Ethiopia from July 2012 to January 2017. Log-rank and Wilcoxon tests, and an Accelerated Failure time (AFT) parametric statistical model were used. Results: A mean of 22.13months (SD=13.16) and a median of 21.47months (IQR: 11.55-33.30) were found. The median age, baselineCD4 count, and BMI of patients at baseline were 30years (IQR: 25-38years), 247cells/µl (IQR: 120-375cells/µl) and 19.75kg/m2 (IQR: 17.5-22kg/m2); respectively. At baseline, the patients CD4 count values ranged from 11 to 1764 (mean=289, SD= 233). The study revealed that 192(29.68%) events occurred, while 455(70.32%) were censored. The Gamma model was selected as the best-fit parametric model for the data. The estimated shape parameter of the fitted Gamma model is 1.9983 with 95%CI (1.3426, 2.9741) indicating that significantly determined as the survival time increases over time. Conclusion: The fitted AFT parametric model (Gamma distribution), the factors such as: higher BMI, higher current CD4 count, being married, starting on AZT-3TC-EFV regimen class significantly increased the survival time of HIV-positive patients attending ART treatment, while; baseline CD4 count and ambulatory functional status reduces the survival time of HIV patients. Moreover, using ART treatment significantly improves the survival time of patients.
Study of a homogeneous QSO sample: relations between the QSO and its host galaxy

We analyse a sample of 69 quasi-stellar objects (QSOs) which have been randomly selected in a complete sample of 104 QSOs (R ≤ 18,0.142 < z < 0.198,δ < 10°). 60 have been observed with the NTT/SUSI2 at La Silla, through two filters in the optical band (WB 655 and V 812), and the remaining nine are taken from archive data bases. The filter V 812 contains the redshifted H,β and forbidden [O III] emission lines, while WB 655 covers a spectral region devoid of emission lines, thus measuring the QSO and stellar continua. The contributions of the QSO and the host are separated thanks to the MCS deconvolution algorithm, allowing a morphological classification of the host, and the computation of several parameters such as the host and nucleus absolute V magnitude, distance between the luminosity centre of the host and the QSO and colour of the host and nucleus. We define a new asymmetry coefficient, independent of any galaxy models and well suited for QSO host studies. The main results from this study are (i) 25 per cent of the total number of QSO hosts are spirals, 51 per cent are ellipticals and 60 per cent show signs of interaction, (ii) highly asymmetric systems tend to have a higher gas ionization level and (iii) elliptical hosts contain a substantial amount of ionized gas and some show off-nuclear activity. These results agree with hierarchical models merger driven evolution.
THE EXTENDED HUBBLE SPACE TELESCOPE SUPERNOVA SURVEY: THE RATE OF CORE COLLAPSE SUPERNOVAE TO z ∼ 1

We use a sample of 45 core collapse supernovae detected with the Advanced Camera for Surveys on board the Hubble Space Telescope to derive the core collapse supernova rate in the redshift range 0.1 < z < 1.3. In redshift bins centered on 〈z〉 = 0.39, 〈z〉 = 0.73, and 〈z〉 = 1.11, we find rates of 3.00+1.28− 0.94+1.04− 0.57, 7.39+1.86− 1.52+3.20− 1.60, and 9.57+3.76− 2.80+4.96− 2.80, respectively, given in units of yr−1 Mpc−3 10−4 h370. The rates have been corrected for host galaxy extinction, including supernovae missed in highly dust-enshrouded environments in infrared bright galaxies. The first errors are statistical while the second ones are the estimated systematic errors. We perform a detailed discussion of possible sources of systematic errors and note that these start to dominate over statistical errors at z > 0.5, emphasizing the need to better control the systematic effects. For example, a better understanding of the amount of dust extinction in the host galaxies and knowledge of the supernova luminosity function, in particular the fraction of faint M ≳ −15 supernovae, is needed to better constrain the rates. When comparing our results with the core collapse supernova rate based on the star formation rate, we find a good agreement, consistent with the supernova rate following the star formation rate, as expected.
LoCuSS: Hydrostatic mass measurements of the high-LX cluster sample - cross-calibration of Chandra and XMM-Newton

We present a consistent analysis of Chandra and XMM-Newton observations of an approximately mass-selected sample of 50 galaxy clusters at 0.15 < z < 0.3 -the 'LoCuSS high-L-X sample'. We apply the same analysis methods to data from both satellites, including newly developed analytic background models that predict the spatial variation of the Chandra and XMM-Newton backgrounds to < 2 and < 5 per cent precision, respectively. To verify the cross-calibration of Chandra-and XMM-Newton-based cluster mass measurements, we derive the mass profiles of the 21 clusters that have been observed with both satellites, extracting surface brightness and temperature profiles from identical regions of the respective data sets. We obtain consistent results for the gas and total hydrostatic cluster masses: the average ratio of Chandra-to XMM-Newton-based measurements of M-gas and M-X at r(500) are 0.99 +/- 0.02 and 1.02 +/- 0.05, respectively, with an intrinsic scatter of similar to 3 per cent for gas masses and similar to 8 per cent for hydrostatic masses. Comparison of our hydrostatic mass measurements at r(500) with the latest Local Cluster Substructure Survey (LoCuSS) weak-lensing results indicate that the data are consistent with non-thermal pressure support at this radius of similar to 7 per cent. We also investigate the scaling relation between our hydrostatic cluster masses and published integrated Compton parameter Y-sph measurements from the Sunyaev-Zel'dovich Array. We measure a scatter in mass at fixed Y-sph of similar to 16 per cent at Delta = 500, which is consistent with theoretical predictions of similar to 10-15 per cent scatter.
Low-frequency radio observations of Seyfert galaxies: A test of the unification scheme

Aims. We present low-frequency radio imaging and spectral properties of a well defined sample of Seyfert galaxies using GMRT 240/610 MHz dual frequency observations. Radio spectra of Seyfert galaxies over 240 MHz to 5.0 GHz are investigated using 240 MHz, 610 MHz flux densities derived from GMRT, and 1.4 GHz and 5.0 GHz flux densities mainly from published VLA data. We test the predictions of Seyfert unification scheme by comparing the radio properties of Seyfert type 1s and type 2s. Methods. We choose a sample such that the two Seyfert subtypes have matched distributions in parameters that are independent to the orientation of AGN, obscuring torus and the host galaxy. Our sample selection criteria allow us to assume that the two Seyfert subtypes are intrinsically similar within the framework of the unification scheme. Results. The new observations at 240/610 MHz, together with archival observations at 1.4 GHz, 5.0 GHz show that type 1s and type 2s have statistically similar radio luminosity distributions at 240 MHz, 610 MHz, 1.4 GHz and 5.0 GHz. The spectral indices at selected frequency intervals as well as index measured over 240 MHz to 5.0 GHz for the two Seyfert subtypes have similar distributions with median spectral index $/sim$ -0.7, consistent with the synchrotron emission from optically thin plasma. In our snap-shot 240/610 MHz GMRT observations, most of the Seyfert galaxies show primarily an unresolved central radio component, except a few sources in which faint kpc-scale extended emission is apparent at 610 MHz. Our results on the statistical comparison of the multifrequency radio properties of our sample Seyfert galaxies are in agreement with the predictions of the Seyfert unification scheme.
Southern class I methanol masers at 36 and 44 GHz

The Australia Telescope Compact Array (ATCA) has been used for high angular resolution imaging of 71 southern class I methanol maser sources quasi-simultaneously at 36 and 44 GHz. The data reveal a high level of morphological and kinematical complexity, and allow us to demonstrate associations, at arcsecond precision, of the class I maser emission with outflows, expanding H ɪɪ regions, dark clouds, shocks traced by the 4.5-μm emission and 8.0-μm filaments. More than 700 maser component features were found at each of the two methanol transitions, but with only 23 per cent recognizable at both transitions; the morphology of class emission is much better revealed by our survey of both transitions, compared with either one alone. We found that the number of masers falls exponentially with the projected linear distance from the associated class II 6.7-GHz methanol maser. This distribution has a scale of 263 ± 15 mpc, irrespective of the transition. The class I masers associated with OH masers were found to have a tendency to be more spread out, both spatially and in the velocity domain. This is consistent with the expectation that such sources are more evolved. Apart from a small number of high-velocity components (which are largely blueshifted and predominantly seen at 36 GHz), the velocity distribution was found to be Gaussian, peaking near the systemic velocity of the region, which had been estimated as the middle of the velocity interval of the associated class II methanol maser at 6.7 GHz. The mean indicated a small, but significant blueshift asymmetry of −0.57 km s −1 (uncertainties are 0.06 and 0.07 km s −1 for the 36- and 44-GHz masers, respectively) with respect to the 6.7-GHz masers. The standard deviation of the velocity distribution was found to be 3.65 ± 0.05 and 3.32 ± 0.07 km s −1 for the 36- and 44-GHz masers, respectively. We also suggest a refined rest frequency value of 36 169.238 ± 0.011 MHz for the 4 −1 -3 0 E methanol transition.
EVIDENCE FOR ENVIRONMENTAL DEPENDENCE OF THE UPPER STELLAR INITIAL MASS FUNCTION IN ORION A

We extend our previous study of the stellar population of L1641, the lower-density star-forming region of the Orion A cloud south of the dense Orion Nebula Cluster (ONC), with the goal of testing whether there is a statistically significant deficiency of high-mass stars in low-density regions. Previously, we compared the observed ratio of low-mass stars to high-mass stars with theoretical models of the stellar initial mass function (IMF) to infer a deficiency of the highest-mass stars in L1641. We expand our population study to identify the intermediate-mass (late B to G) L1641 members in an attempt to make a more direct comparison with the mass function of the nearby ONC. The spectral-type distribution and the K-band luminosity function of L1641 are similar to those of the ONC, but problems of incompleteness and contamination prevent us from making a detailed test for differences. We limit our analysis to statistical tests of the ratio of high-mass to low-mass stars, which indicate a probability of only 3% that the ONC and the southern region of L1641 were drawn from the same population, supporting the hypothesis that the upper-mass end of the IMF is dependent on environmental density.
A DIVERSITY OF PROGENITORS AND HISTORIES FOR ISOLATED SPIRAL GALAXIES

We analyze a suite of 33 cosmological simulations of the evolution of Milky-Way-mass galaxies in low-density environments. Our sample spans a broad range of Hubble types at z = 0, from nearly bulgeless disks to bulge-dominated galaxies. Despite the fact that a large fraction of the bulge is typically in place by z ∼ 1, we find no significant correlation between the morphology at z = 1 and at z = 0. The z = 1 progenitors of disk galaxies span a range of morphologies, including smooth disks, unstable disks, interacting galaxies, and bulge-dominated systems. By z ∼ 0.5, spiral arms and bars are largely in place and the progenitor morphology is correlated with the final morphology. We next focus on late-type galaxies with a bulge-to-total ratio (B/T) <0.3 at z = 0. These show a correlation between B/T at z = 0 and the mass ratio of the largest merger at z < 2, as well as with the gas accretion rate at z > 1. We find that the galaxies with the lowest B/T tend to have a quiet baryon input history, with no major mergers at z < 2, and with a low and constant gas accretion rate that keeps a stable angular-momentum direction. More violent merger or gas accretion histories lead to galaxies with more prominent bulges. Most disk galaxies have a bulge Sérsic index n ⩽ 2. The galaxies with the highest bulge Sérsic index tend to have histories of intense gas accretion and disk instability rather than active mergers.