Miracle-dz/UniFAR-FTUs huggingface dataset:
Merging binary black holes formed through chemically homogeneous evolution in short-period stellar binaries

We explore a newly proposed channel to create binary black holes of stellar origin. This scenario applies to massive, tight binaries where mixing induced by rotation and tides transports the products of hydrogen burning throughout the stellar envelopes. This slowly enriches the entire star with helium, preventing the build-up of an internal chemical gradient. The stars remain compact as they evolve nearly chemically homogeneously, eventually forming two black holes, which we estimate typically merge 4–11 Gyr after formation. Like other proposed channels, this evolutionary pathway suffers from significant theoretical uncertainties, but could be constrained in the near future by data from advanced ground-based gravitational-wave detectors. We perform Monte Carlo simulations of the expected merger rate over cosmic time to explore the implications and uncertainties. Our default model for this channel yields a local binary black hole merger rate of about 10 Gpc−3 yr−1 at redshift z = 0, peaking at twice this rate at z = 0.5. This means that this channel is competitive, in terms of expected rates, with the conventional formation scenarios that involve a common-envelope phase during isolated binary evolution or dynamical interaction in a dense cluster. The events from this channel may be distinguished by the preference for nearly equal-mass components and high masses, with typical total masses between 50 and 110 M⊙. Unlike the conventional isolated binary evolution scenario that involves shrinkage of the orbit during a common-envelope phase, short time delays are unlikely for this channel, implying that we do not expect mergers at high redshift.
GMC evolution in a barred spiral galaxy with star formation and thermal feedback

We explore the impact of star formation and thermal stellar feedback on the giant molecular cloud (GMC) population forming in a M83-type barred spiral galaxy. We compare three high-resolution simulations (1.5 pc cell size) with different star formation/feedback models: one with no star formation, one with star formation but no feedback, and one with star formation and thermal energy injection. We analyze the resulting population of clouds, finding that we can identify the same population of massive, virialized clouds and transient, low-surface density clouds found in our previous work (that did not include star formation or feedback). Star formation and feedback can affect the mix of clouds we identify. In particular, star formation alone simply converts dense cloud gas into stars with only a small change to the cloud populations, principally resulting in a slight decrease in the transient population. Feedback, however, has a stronger impact: while it is not generally sufficient to entirely destroy the clouds, it does eject gas out of them, increasing the gas density in the inter-cloud region. This decreases the number of massive clouds, but substantially increases the transient cloud population. We also find that feedback tends to drive a net radial inflow of massive clouds, leading to an increase in the star formation rate in the bar region. We examine a number of possible reasons for this and conclude that it is possible that the drag force from the enhanced intercloud density could be responsible.
Superconducting hair on charged black string background

Behavior of Dirac fermions in the background of a charged black string penetrated by an Abelian Higgs vortex is elaborated. One finds evidence that the system under consideration can support fermion fields acting like a superconducting cosmic string in the sense that a nontrivial Dirac fermion field can be carried by the system in question. Nonextremal and extremal black string vortex systems were considered. The influence of electric and Higgs charge, the winding number, and the fermion mass on the fermion localization near the black string event horizon were studied. It turned out that the extreme charged black string expelled fermion fields more violently comparing to the nonextremal one.
Situating climate change adaptation within plural worlds: The role of Indigenous and local knowledge in Pentecost Island, Vanuatu

Scholars, practitioners, and decision-makers are increasingly recognising that Indigenous knowledge can play a significant role in facilitating adaptation to climate change. Yet, adaptation theorising and practises remain overwhelmingly situated within Euromodern ontologies, and there remains limited space, at present, for plural ontologies or alternative ways of being and knowing. In this paper, and using the Pacific as our case study, we present an argument for the inclusion of multiple ontologies within adaptation policymaking. Pacific adaptation policies and interventions frequently privilege Western scientific knowledge and focus on addressing individual climate risks through technical fixes directed by foreign experts and funding agencies. They are also rooted in a policy architecture that is an artefact of colonisation in the region. Despite these obstacles, Pacific Islander responses to climate change are dynamic, and inclusive of the multiple and competing ontologies they work within, offering insights into how Euromodern and Pacific islander world views could coalesce to builds adaptive capacity and consolidate community resilience into the future. Highlights • Indigenous Knowledge plays a critical role in enabling resilience and facilitating climate change adaptation in some parts of Vanuatu • Ni-Vanuatu people employ dynamic responses to climate risks incorporating multiple knowledge systems and practises • Co-existence of different knowledge systems provide insights into factors that enable adaptive capacity and consolidate community resilience • Diverse worldviews, knowledge systems and practises with Pacific Island cultures highlights the importance of thinking about ontological pluralism within adaptation • Climate adaptation is principally founded on Western ontologies, but there is a need consider non-Western ontologies and epistemologies.
Quantitative detection of anti-PLA2R antibodies targeting different epitopes and its clinical application in primary membranous nephropathy

Abstract Objectives This study aimed to establish time-resolved fluorescence immunoassays to quantitatively detect the autoantibodies targeting different epitopes of M-type phospholipase A2 receptor (PLA2R) and evaluate its clinical application in primary membranous nephropathy (PMN). Methods PLA2R and its reactive epitope-specific IgG/IgG4 time-resolved fluorescence immunoassays (TRFIAs) were established using europium-labeled anti-human IgG/IgG4 antibodies, recombinant proteins, and patient serum. The levels of IgG/IgG4 targeting PLA2R and its epitopes in PMN patient serum were detected, and the relationship between epitope spreading of PLA2R and the severity of patients with PMN was evaluated. Results The TRFIAs established in this study could quantitatively detect PLA2R and its epitope-specific IgG and IgG4. Sera from 59 patients with PMN were subjected to detection using anti-PLA2R IgG and anti-PLA2R IgG4. Among them, 46 and 54 patients were found positive for PLA2R antibodies, respectively. Moreover, the levels of PLA2R antibodies were strongly correlated with the severity of patients with PMN. Patients who were detected to have two or more epitopes had more serious renal injury. Conclusions PLA2R domain-specific IgG/IgG4 TRFIAs were established in this study, and detection with anti-PLA2R IgG4 could more sensitively screen the reactivity of patients to the PLA2R domain. Moreover, detection epitope spreading of PLA2R was confirmed which is related to the severity of patients with PMN.
MODERATE-LUMINOSITY GROWING BLACK HOLES FROM 1.25 < z < 2.7: VARIED ACCRETION IN DISK-DOMINATED HOSTS

We compute black hole masses and bolometric luminosities for 57 active galactic nuclei (AGNs) in the redshift range 1.25 ⩽ z ⩽ 2.67, selected from the GOODS-South deep multi-wavelength survey field via their X-ray emission. We determine host galaxy morphological parameters by separating the galaxies from their central point sources in deep Hubble Space Telescope images, and host stellar masses and colors by multi-wavelength spectral energy distribution fitting. Of GOODS AGNs at these redshifts, 90% have detected rest-frame optical nuclear point sources; bolometric luminosities range from 2 × 1043 to 2 × 1046 erg s−1. The black holes are growing at a range of accretion rates, with ≳ 50% of the sample having L/LEdd < 0.1. Of the host galaxies, 70% have stellar masses M* > 1010 M☉, with a range of colors suggesting a complex star formation history. We find no evolution of AGN bolometric luminosity within the sample, and no correlation between AGN bolometric luminosity and host stellar mass, color, or morphology. Fully half the sample of host galaxies are disk-dominated, with another 25% having strong disk components. Fewer than 15% of the systems appear to be at some stage of a major merger. These moderate-luminosity AGN hosts are therefore inconsistent with a dynamical history dominated by mergers strong enough to destroy disks, indicating that minor mergers or secular processes dominate the coevolution of galaxies and their central black holes at z ∼ 2.
Discovery of Kilohertz Quasi-Periodic Oscillations and State Transitions in the Low-Mass X-Ray Binary 1E 1724–3045 (Terzan 2)

We have studied the rapid X-ray time variability in 99 pointed observations with the Rossi X-Ray Timing Explorer (RXTE) Proportional Counter Array of the low-mass X-ray binary 1E 1724–3045, including, for the first time, observations of this source in its island and banana states, confirming the atoll nature of this source. We report the discovery of kilohertz quasi-periodic oscillations (kHz QPOs). Although we have five detections of the lower kHz QPO and one detection of the upper kHz QPO, in none of the observations we detect both QPOs simultaneously. By comparing the dependence of the rms amplitude with energy of kHz QPOs in different atoll sources, we conclude that this information cannot be use to unambiguously identify the kilohertz QPOs as was previously thought. We find that Terzan 2 in its different states shows timing behavior similar to that seen in other neutron-star low-mass X-ray binaries (LMXBs). We studied the flux transitions observed between 2004 February and 2005 October and conclude that they are due to changes in the accretion rate.
ANALYZING THE LARGEST SPECTROSCOPIC DATA SET OF STRIPPED SUPERNOVAE TO IMPROVE THEIR IDENTIFICATIONS AND CONSTRAIN THEIR PROGENITORS

Using the largest spectroscopic data set of stripped-envelope core-collapse supernovae (stripped SNe), we present a systematic investigation of spectral properties of Type IIb SNe (SNe IIb), Type Ib SNe (SNe Ib), and Type Ic SNe (SNe Ic). Prior studies have been based on individual objects or small samples. Here, we analyze 242 spectra of 14 SNe IIb, 262 spectra of 21 SNe Ib, and 207 spectra of 17 SNe Ic based on the stripped SN data set of Modjaz et al. and other published spectra of individual SNe. Each SN in our sample has a secure spectroscopic ID, a date of V-band maximum light, and most have multiple spectra at different phases. We analyze these spectra as a function of subtype and phase in order to improve the SN identification scheme and constrain the progenitors of different kinds of stripped SNe. By comparing spectra of SNe IIb with those of SNe Ib, we find that the strength of Hα can be used to quantitatively differentiate between these two subtypes at all epochs. Moreover, we find a continuum in observational properties between SNe IIb and Ib. We address the question of hidden He in SNe Ic by comparing our observations with predictions from various models that either include hidden He or in which He has been burnt. Our results favor the He-free progenitor models for SNe Ic. Finally, we construct continuum-divided average spectra as a function of subtype and phase to quantify the spectral diversity of the different types of stripped SNe.
Multi-stage Citrus Detection based on Improved Yolov4

At present, the research of Citrus recognition is basically aimed at the detection of Citrus in mature stage. This paper proposes a citrus detection algorithm based on improved yolov4, which can detect citrus in each growth stage. Based on yolov4, Introducing CBAM attention mechanism to improve the feature extraction ability of backbone networks; Increase the 22nd layer output of feature extraction network to improve the small target detection rate; A short connection feature fusion method is designed to increase the utilization of shallow feature information; Add a detection head with a scale of 152 * 152 for small-scale targets. It is proved by experiments on the self-built citrus data set, the improved CBAM-F-YOLOv4 can effectively detect citrus in each stage, and the mean Average Precision (mAP) is 6.2 percentage points higher than the original algorithm, reaching 87.3%. The detection results show that the improved algorithm greatly improves the detection ability of occlusion、 overlap and small-scale citrus.
THE ROLE OF DARK MATTER INTERACTION IN GALAXY CLUSTERS

We consider a toy model to analyze the consequences of dark matter interaction with a dark energy background on the overall rotation of galaxy clusters and the misalignment between their dark matter and baryon distributions when compared to ΛCDM predictions. The interaction parameters are found via a genetic algorithm search. The results obtained suggest that interaction is a basic phenomenon whose effects are detectable even in simple models of galactic dynamics.
MPTbreeze: a fast renormalized perturbative scheme

We put forward and test a simple description of multipoint propagators (MP), which serve as building blocks to calculate the non-linear matter power spectrum. On large scales these propagators reduce to the well-known kernels in standard perturbation theory, while at smaller scales they are suppressed due to non-linear couplings. Through extensive testing with numerical simulations we find that this decay is characterized by the same damping scale for both two- and three-point propagators. In turn this transition can be well modelled with resummation results that exponentiate one-loop computations. For the first time, we measure the four components of the non-linear (two-point) propagator using dedicated simulations started from two independent random Gaussian fields for positions and velocities, verifying in detail the fundamentals of propagator resummation. We use these results to develop an implementation of the MP expansion for the non-linear power spectrum that only requires seconds to evaluate at baryon acoustic oscillations (BAO) scales. To test it we construct six suites of large numerical simulations with different cosmologies. From these and LasDamas runs we show that the non-linear power spectrum can be described at the ≲ 2 per cent level at BAO scales for redshifts in the range [0–2.5]. We make a public release of the MPTbreeze code with the hope that it can be useful to the community.
Mode density and frequency extraction in the δ Scuti star HD 50844

We consider the high mode density reported in the delta Scuti star HD 50844 observed by CoRoT. Using simulations, we find that extracting frequencies down to a given false alarm probability by means of successive prewhitening leads to a gross over-estimate of the number of frequencies in a star. This is due to blending of the peaks in the periodogram due to the finite duration of the time series. Prewhitening is equivalent to adding a frequency to the data which is carefully chosen to interfere destructively with a given frequency in the data. Since the frequency extracted from a blended peak is not quite correct, the interference is not destructive with the result that many additional fictitious frequencies are added to the data. In data with very high signal-to-noise, such as the CoRoT data, these spurious frequencies are highly significant. Continuous prewhitening thus causes a cascade of spurious frequencies which leads to a much larger estimate of the mode density than is actually the case. The results reported for HD 50844 are consistent with this effect. Direct comparison of the power in the raw periodogram in this star with that in delta Scuti stars observed by Kepler shows that HD 50844 has a typical mode density.
X-ray detections of submillimetre galaxies: active galactic nuclei versus starburst contribution

We present a large-scale study of the X-ray properties and near-IR-to-radio SEDs of submillimetre galaxies (SMGs) detected at 1.1mm with the AzTEC instrument across a ~1.2 square degree area of the sky. Combining deep 2-4 Ms Chandra data with Spitzer IRAC/MIPS and VLA data within the GOODS-N/S and COSMOS fields, we find evidence for AGN activity in ~14 percent of 271 AzTEC SMGs, ~28 percent considering only the two GOODS fields. Through X-ray spectral modeling and SED fitting using Monte Carlo Markov Chain techniques to Siebenmorgen et al. (2004) (AGN) and Efstathiou et al. (2000) (starburst) templates, we find that while star formation dominates the IR emission, with SFRs ~100-1000 M_sun/yr, the X-ray emission for most sources is almost exclusively from obscured AGNs, with column densities in excess of 10^23 cm^-2. Only for ~6 percent of our sources do we find an X-ray-derived SFR consistent with NIR-to-radio SED derived SFRs. Inclusion of the X-ray luminosities as a prior to the NIR-to-radio SED effectively sets the AGN luminosity and SFR, preventing significant contribution from the AGN template. Our SED modeling further shows that the AGN and starburst templates typically lack the required 1.1 mm emission necessary to match observations, arguing for an extended, cool dust component. The cross correlation function between the full samples of X-ray sources and SMGs in these fields does not indicate a strong correlation between the two populations at large scales, suggesting that SMGs and AGNs do not necessarily trace the same underlying large scale structure. Combined with the remaining X-ray-dim SMGs, this suggests that sub-mm bright sources may evolve along multiple tracks, with X-ray-detected SMGs representing transitionary objects between periods of high star formation and AGN activity while X-ray-faint SMGs represent a brief starburst phase of more normal galaxies.
Evidence of $\theta_{13}$>0 from global neutrino data analysis

The neutrino mixing angle �13 is at the focus of current neutrino research. From a global analysis of the available oscillation data in a 3� framework, we previously reported [Phys. Rev. Lett. 101, 141801 (2008)] hints in favor of �13 > 0 at the 90% C.L. Such hints are consistent with the recent indications of �µ ! �e appearance in the T2K and MINOS long-baseline accelerator experiments. Our global analysis of all the available data currently provides > 3� evidence for nonzero �13, with 1� ranges sin 2 �13 = 0.021 ± 0.007 or 0.025 ± 0.007, depending on reactor neutrino flux systematics. Updated ranges are also reported for the other 3� oscillation parameters (�m 2 , sin 2 �12) and (�m 2 , sin 2 �23).
THE COMPACT, TIME-VARIABLE RADIO SOURCE PROJECTED INSIDE W3(OH): EVIDENCE FOR A PHOTOEVAPORATED DISK?

We present new Karl G. Jansky Very Large Array (VLA) observations of the compact (∼0.″05), time-variable radio source projected near the center of the ultracompact H ii region W3(OH). The analysis of our new data as well as of VLA archival observations confirms the variability of the source on timescales of years and for a given epoch indicates a spectral index of α = 1.3 ± 0.3 (Sν∝να). This spectral index and the brightness temperature of the source (∼6500 K) suggest that we are most likely detecting partially optically thick free–free radiation. The radio source is probably associated with the ionizing star of W3(OH), but an interpretation in terms of an ionized stellar wind fails because the detected flux densities are orders of magnitude larger than expected. We discuss several scenarios and tentatively propose that the radio emission could arise in a static ionized atmosphere around a fossil photoevaporated disk.
Multicolor photometry of the galaxy cluster A98: substructures and star formation properties

An optical photometric observation with the Beijing-Arizona-Taiwan- Connecticut (BATC) multicolor system is carried out for A98 (z =0 .104), a galaxy cluster with two large enhancements in X-ray surface brightness. Spectral energy dis- tributions (SEDs) covering15 intermediate bands are obtained for all sources detected down to V ∼ 20 mag in a field of 58 � × 58 � . After star-galaxy separation with color- color diagrams, a photometric redshift technique is applied to the galaxy sample for further membership determination. The color-magnitude relation is taken as a further restriction of the early-type cluster galaxies. As a result, a list of 198 faint member galaxies is achieved. Based on the newly generated sample of member galaxies, the dynamical substructures, A98N, A98S, and A98W, are investigated in detail. A sepa- rate galaxy group, A98X, is also found to the south of the main concentration of A98, which is gravitationally unbound to A98. For 74 spectroscopically confirmed member galaxies, the environmental effect on the star formation history is investigated. The bright galaxies in the core region are found to have shorter time scales of star forma- tion, longer mean stellar ages, and higher interstellar medium metallicities, which can be interpreted in the context of the hierarchical cosmological scenario.
A candidate circumbinary Keplerian disk in G35.20-0.74 N: A study with ALMA

We report on ALMA observations of continuum and molecular line emission with 0 ''. 4 resolution towards the high-mass star-forming region G35.20-0.74 N. Two dense cores are detected in typical hot-core tracers (e. g., CH3CN) that reveal velocity gradients. In one of these cores, the velocity field can be fitted with an almost edge-on Keplerian disk rotating about a central mass of similar to 18 M-circle dot. This finding is consistent with the results of a recent study of the CO first overtone bandhead emission at 2.3 mu m towards G35.20-0.74 N. The disk radius and mass are greater than or similar to 2500 au and similar to 3 M-circle dot. To reconcile the observed bolometric luminosity (similar to 3x10(4) L-circle dot) with the estimated stellar mass of 18 M-circle dot, we propose that the latter is the total mass of a binary system.
Flexoelectric effect in biaxial nematics

The flexoelectric (FE) effect provides a linear coupling between electric polarization and orientational deformation in liquid crystals. It influences many electrooptical phenomena and it is used in some bistable nematic devices. A statistical theory of dipole FE polarization in biaxial nematic liquid crystals is used to calculate temperature dependence of order parameters, elastic constants, and FE coefficients. The splitting of the two Meyer FE coefficients and the appearance of new FE coefficients is obtained at the uniaxial-biaxial nematic transition. The ordering of the splited FE coefficients corresponds to the ordering of the splited elastic constants.