Miracle-dz/UniFAR-FTUs huggingface dataset:
The LABOCA survey of the Extended Chandra Deep Field-South: clustering of submillimetre galaxies

We present a measurement of the spatial clustering of submillimetre galaxies (SMGs) at z= 1-3. Using data from the 870μm Large APEX Bolometer Camera (LABOCA) submillimetre survey of the Extended Chandra Deep Field-South, we employ a novel technique to measure the cross-correlation between SMGs and galaxies, accounting for the full probability distributions for photometric redshifts of the galaxies. From the observed projected two-point cross-correlation function we derive the linear bias and characteristic dark matter halo masses for the SMGs. We detect clustering in the cross-correlation between SMGs and galaxies at the >4σ level. Accounting for the clustering of galaxies from their autocorrelation function, we estimate an autocorrelation length for SMGs of r o = 7.7 -2.3 +1.8 h -1 Mpc assuming a power-law slope γ= 1.8, and derive a corresponding dark matter halo mass of log(M halo[h -1M ⊙]) = 12.8 -0.5 +0.3. Based on the evolution of dark matter haloes derived from simulations, we show that that the z= 0 descendants of SMGs are typically massive (~2-3L *) elliptical galaxies residing in moderate- to high-mass groups (log(M halo[h -1M ⊙]) = 13.3 -0.5 +0.3). From the observed clustering we estimate an SMG lifetime of ~100Myr, consistent with lifetimes derived from gas consumption times and star formation time-scales, although with considerable uncertainties. The clustering of SMGs at z~ 2 is consistent with measurements for optically selected quasi-stellar objects (QSOs), supporting evolutionary scenarios in which powerful starbursts and QSOs occur in the same systems. Given that SMGs reside in haloes of characteristic mass ~6 × 10 12h -1M ⊙, we demonstrate that the redshift distribution of SMGs can be described remarkably well by the combination of two effects: the cosmological growth of structure and the evolution of the molecular gas fraction in galaxies. We conclude that the powerful starbursts in SMGs likely represent a short-lived but universal phase in massive galaxy evolution, associated with the transition between cold gas-rich, star-forming galaxies and passively evolving systems.
Exploring Occlusion-Sensitive Deep Network for Single-View 3D Face Reconstruction

Recovering 3D geometry from a single-view 2D face image is an ill-posed task full of various challenges, especially under occlusion conditions commonly seen with large poses, while partial facial information missing makes the burden much heavier. Although existing methods could solve this problem in the end-to-end fashion, they still have limited performance in the occluded scenes. It is intuitively for many methods to depress the influence of those occluded regions for reconstruction. But we propose an occlusion-sensitive weighting mechanism for balancing the contributions among occluded and non-occluded regions. Meanwhile, considering no dataset contains various occlusions for learning, the data augmentation technique is exploited to expand the training dataset, which further facilitates the learning of the occlusion-sensitive deep network. Extensive experiments on two challenging datasets validate the advanced performance of our method for both 3D face reconstruction and face alignment.1
An Imbalance-Status-Enabled Autonomous Global Power-Sharing Scheme for Solid-State Transformer Interconnected Hybrid AC/DC Microgrids

This paper proposes a novel imbalance-status (IS)-enabled autonomous global power-sharing scheme for a solid-state transformer (SST) interconnected hybrid AC / DC microgrid system. Firstly, the proposed scheme globally estimates instantaneous active power imbalances according to the existing droop regulation characteristics of each sub-microgrid, and normalizes these imbalances by introducing the definition of IS. Next, three novel IS-enabled controllers are designed for the SST’s three core converters, to autonomously share the power imbalances in the entire system. Then, the control parameters of the proposed scheme are optimized through small-signal analysis. The control effectiveness and flexibility of the proposed scheme in realizing global power-sharing function are verified by controller hardware-in-loop experiments in RT-LAB platform.
Complementary Observables and Non-Boolean Logic Outside Quantum Physics

The concept of complementarity in combination with a non-Boolean calculus of propositions refers to a pivotal feature of quantum systems which has long been regarded as a key to their distinction from classical systems. But a non-Boolean logic of complementary features may also apply to classical systems, if their states and observables are defined by partitions of a classical state space. If these partitions do not satisfy certain stability criteria, complementary observables and non-Boolean propositional lattices may be the consequence. This is especially the case for non-generating partitions of nonlinear dynamical systems. We show how this can be understood in more detail and indicate some challenging consequences for systems outside quantum physics, including mental processes.
Universal short-time quantum critical dynamics in imaginary time

We propose a scaling theory for the universal imaginary-time quantum critical dynamics for both short times and long times. We discover that there exists a universal critical initial slip related to a small initial order parameter $M_0$. In this stage, the order parameter $M$ increases with the imaginary time $\tau$ as $M\propto M_0\tau^\theta$ with a universal initial slip exponent $\theta$. For the one-dimensional transverse-field Ising model, we estimate $\theta$ to be $0.373$, which is markedly distinct from its classical counterpart. Apart from the local order parameter, we also show that the entanglement entropy exhibits universal behavior in the short-time region. As the critical exponents in the early stage and in equilibrium are identical, we apply the short-time dynamics method to determine quantum critical properties. The method is generally applicable in both the Landau-Ginzburg-Wilson paradigm and topological phase transitions.
Power spectra in the eikonal approximation with adiabatic and nonadiabatic modes

We use the so-called eikonal approximation, recently introduced in the context of cosmological perturbation theory, to compute power spectra for multicomponent fluids. We demonstrate that, at any given order in standard perturbation theory, multipoint power spectra do not depend on the large-scale adiabatic modes. Moreover, we employ perturbation theories to decipher how nonadiabatic modes, such as a relative velocity between two different components, damp the small-scale matter power spectrum, a mechanism recently described in the literature. In particular, we do an explicit calculation at one-loop order of this effect. While the one-loop result eventually breaks down, we show how the damping effect can be fully captured by the help of the eikonal approximation. A relative velocity not only induces mode damping but also creates large-scale anisotropic modulations of the matter power spectrum amplitude. We illustrate this for the Local Group environment.
Halo shapes from weak lensing: the impact of galaxy–halo misalignment

We analyse the impact of galaxy–halo misalignment on the ability of weak lensing studies to constrain the shape of dark matter haloes, using a combination of the Millennium dark matter N-body simulation and different semi-analytic galaxy formation models, as well as simpler Monte Carlo tests. Since the distribution of galaxy–halo alignments is not known in detail, we test various alignment models, together with different methods of determining the halo shape. In addition to alignment, we examine the interplay of halo mass and shape, and galaxy colour and morphology with the resulting stacked projected halo shape. We find that only in the case where significant numbers of galaxy and halo minor axes are parallel does the stacked, projected halo axis ratio fall below 0.95. When using broader misalignment distributions, such as those found in recent simulations of galaxy formation, the halo ellipticity signal is washed out and would be extremely difficult to measure observationally. It is important to note that the spread in stacked halo axis ratio due to theoretical unknowns (differences between semi-analytic models and between alignment models) are much bigger than any statistical uncertainty. It is naive to assume that, simply because Λ cold dark matter (ΛCDM) predicts aspherical haloes, the stacked projected shape will be elliptical. In fact, there is no robust ΛCDM prediction yet for this procedure, and the interpretation of any such elliptical halo signal from lensing in terms of physical halo properties will be extremely difficult.
STAR FORMATION FEEDBACK AND METAL-ENRICHMENT HISTORY OF THE INTERGALACTIC MEDIUM

Using the state-of-the-art cosmological hydrodynamic simulations of the standard cold dark matter model with star formation feedback strength normalized to match the observed star formation history of the universe at z= 0–6, we compute the metal-enrichment history of the intergalactic medium (IGM). Overall we show that galactic superwind (GSW) feedback from star formation can transport metals to the IGM and that the properties of simulated metal absorbers match current observations. The distance of influence of GSW from galaxies is typically limited to about ⩽0.5 Mpc and within regions of overdensity δ ⩾ 10. Most C iv and O vi absorbers are located within shocked regions of elevated temperature (T ⩾ 2 × 104 K), overdensity (δ ⩾ 10), and metallicity ([Z/ Z☉] = [ − 2.5, − 0.5]), enclosed by double shocks propagating outward. O vi absorbers have typically higher metallicity, lower density, and higher temperature than C iv absorbers. For O vi absorbers, collisional ionization dominates over the entire redshift range z= 0–6, whereas for C iv absorbers the transition occurs at moderate redshift z ∼ 3 from collisionally dominated to photoionization dominated. We find that the observed column density distributions for C iv and O vi in the range log N cm2=12–15 are reasonably reproduced by the simulations. The evolution of mass densities contained in C iv and O vi lines, ΩC iv and ΩO vi, is also in good agreement with observations, which shows a near constancy at low redshifts and an exponential drop beyond redshift z= 3–4. For both C iv and O vi, most absorbers are transient and the amount of metals probed by C iv and O vi lines of column log N cm2=12–15 is only ∼2% of total metal density at any epoch. While gravitational shocks from large-scale structure formation dominate the energy budget (80%–90%) for turning about 50% of the IGM to the warm–hot intergalactic medium (WHIM) by z = 0, GSW feedback shocks are energetically dominant over gravitational shocks at z⩾1–2. Most of the so-called missing metals at z= 2–3 are hidden in a warm–hot (T = 104.5–107 K) gaseous phase, heated up by GSW feedback shocks. Their mass distribution is broadly peaked at δ=1–10 in the IGM, outside virialized halos. Approximately 37%, 46%, 10%, and 7% of the total metals at z = 0 are in stars, WHIM, X-ray gas, and cold gas, respectively; the distributions stand at 23%, 57%, 2%, and 18% and 14%, 51%, 4%, and 31% at z = 2 and z = 4, respectively.
Current methods for analyzing light curves of solar-like stars

CoRoT has allowed a quantitative leap for the solar-like-star seismology thanks to 5-month-long uninterrupted timeseries of high-precision photometric data. Kepler is also starting to deliver similar data. Now, several F and G main-sequence stars have been analyzed. The techniques developed to interpret light curves directly inherit from the experience got on the Sun with helioseismology. I describe in this review the methods currently used to analyze these light curves. First, these data provide an accurate determination of the stellar rotation rate. This is possible thanks to the magnetic activity of stars. The power spectra of light curves put also constraints on the stellar granulation, which can be directly compared to 3-D stellar atmosphere models; this shows still unexplained discrepancies. I then detailed a standard method for extracting p-mode characteristics (frequency, amplitude and lifetime). CoRoT has revealed unexpected short life times for F stars. Last, I also discuss errors and biases of mode frequencies, especially the ones due to the simplified description of the rotation generally used (© 2010 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
HUBUNGAN TINGKAT PENGETAHUAN, SIKAP DAN PRAKTIK MASYARAKAT DALAM UPAYA PENCEGAHAN DEMAM BERDARAH DENGUE (DBD) DI PUSKESMAS PARONGPONG

Dengue hemorrhagic fever is still a public health problem in Indonesia. Prevention and eradication of dengue hemorrhagic fever (DHF) must be the responsibility of all communities. Behavior that includes knowledge, attitudes and practices about prevention is a factor that affects the increase in cases of dengue fever. The purpose of this study was to determine the relationship between the level of knowledge, attitudes and practices of the community in an effort to prevent dengue fever in the Parongpong Public Health Center area. This study used the descriptive correlation method and was conducted in July 2022 at the Parongpong Health Center. The sample of this study amounted to 100 respondents using simple random sampling technique. The statistical test used was the Spearman Rho test. The results showed that there was no significant relationship between knowledge and attitude (sig value 0.435 with p <0.05), there was no significant relationship between knowledge and practice (sig value 0.651 with p<0.05), and there is no significant relationship between attitude and practice (sig value is 0.736 with p<0.05), the results of this study are expected to be input and evaluation for health agencies in order to monitor preventive practices dengue fever in the community which is useful for reducing the incidence of dengue fever. Keywords: Dengue Hemorrhagic Fever, Prevention, Knowledge, Attitude, Practice Demam berdarah dengue masih menjadi masalah kesehatan masyarakat Indonesia. Pencegahan dan pemberantasan penyakit demam berdarah dengue (DBD) harus menjadi tanggung jawab semua komunitas. Perilaku yang meliputi pengetahuan, sikap dan praktik tentang pencegahan merupakan faktor yang mempengaruhi peningkatan kasus demam berdarah. Tujuan penelitian ini adalah untuk mengetahui hubungan tingkat pengetahuan, sikap dan praktik masyarakat dalam upaya pencegahan demam berdarah di wilayah puskesmas Parongpong. Penelitian ini menggunkan metode descriptive correlation dan dilakukan pada bulan bulan Juli 2022 di Puskesmas Parongpong. Sampel penelitian ini berjumlah 100 responden menggunakan teknik simple random sampling. Uji statistik yang digunakan adalah Uji Spearman Rho. Hasil penelitian menunjukkan tidak terdapat hubungan yang signifikan antara pengetahuan dan sikap dengan (nilai sig yaitu 0,435 dengan p<0,05), Tidak terdapat hubungan yang signifikan antara pengetahuan dan praktik (nilai sig yaitu 0,651 dengan p<0,05), dan Tidak terdapat hubungan yang signifikan antara sikap dan praktik (nilai sig yaitu 0,736 dengan p<0,05). Hasil penelitian ini diharapkan dapat menjadi masukkan dan evaluasi bagi instansi kesehatan agar dapat melakukan pengawasan terhadap praktik pencegahan demam berdarah di masyarakat yang berguna untuk menurunkan angka kejadian demam berdarah. Kata Kunci: Demam Berdarah Dengue, Pencegahan, Pengetahuan, Praktik, Sikap
Detection of distinct power spectra in soft and hard X-ray bands in the hard state of GRS 1915+105

The well-known black hole X-ray binary GRS 1915+105 is a unique source in the sense that it cannot be classified within the standard picture of black hole binary states. In this work, we study archival XMM-Newton observations taken between 2003 and 2004 of the chi variability class of GRS 1915+105, which corresponds to the hard state in the standard black hole X-ray binary state classification. The crucial point of our study is that by using XMM-Newton data, we can access the variability below 3 keV, an energy range that is not covered with RXTE. We focus on the study of the power spectral shape in the soft and hard X-ray band, in light of our work done with Swift on MAXI J1659-152. In the hard band (above 2.5 keV), power density spectra consist of band-limited noise and quasi-periodic oscillations, corresponding to the power spectral shape seen in the hard or intermediate state, while in the soft band the averaged power density spectrum is consistent with a power-law noise, corresponding to the power spectral shape usually seen in the soft state. The coexisting of two different power spectral shapes in the soft and hard band, where the soft-band power spectrum is dominated by a power-law noise, is consistent with MAXI J1659-152, and confirms the energy dependence of power spectral states. Our additional spectral analysis shows that the disc component does contribute to the soft-band flux. These findings support that the observed black hole power spectral state depends on which spectral component we are looking at, which implies that power spectral analysis is probably a more sensitive method than spectral modelling to trace the emergence of the disc component in the hard or intermediate state.
Optimal Hölder Continuity of SHE and SWE with Rough Fractional Noise

We mainly focus on the stochastic heat equation (SHE), i.e., L = ∂t − ∂xx, and the stochastic wave equation (SWE), i.e., L = ∂tt − ∂xx, with specified initial data. In the SHE case we impose u(0, x) = u0(x), while in the SWE case we further impose ut(0, x) = v0(x). There has been a widespread interest in Holder continuity result for random fields. This type of sample path regularity is a key property that is needed early
EXPANDED SEARCH FOR z ∼ 10 GALAXIES FROM HUDF09, ERS, AND CANDELS DATA: EVIDENCE FOR ACCELERATED EVOLUTION AT z > 8?

We search for z ∼ 10 galaxies over ∼160 arcmin2 of Wide-Field Camera 3 (WFC3)/IR data in the Chandra Deep Field South, using the public HUDF09, Early Release Science, and CANDELS surveys, that reach to 5σ depths ranging from 26.9 to 29.4 in H160 AB mag. z ≳ 9.5 galaxy candidates are identified via J125 − H160 > 1.2 colors and non-detections in any band blueward of J125. Spitzer Infrared Array Camera (IRAC) photometry is key for separating the genuine high-z candidates from intermediate-redshift (z ∼ 2–4) galaxies with evolved or heavily dust obscured stellar populations. After removing 16 sources of intermediate brightness (H160 ∼ 24–26 mag) with strong IRAC detections, we only find one plausible z ∼ 10 galaxy candidate in the whole data set, previously reported in Bouwens et al. The newer data cover a 3 × larger area and provide much stronger constraints on the evolution of the UV luminosity function (LF). If the evolution of the z ∼ 4–8 LFs is extrapolated to z ∼ 10, six z ∼ 10 galaxies are expected in our data. The detection of only one source suggests that the UV LF evolves at an accelerated rate before z ∼ 8. The luminosity density is found to increase by more than an order of magnitude in only 170 Myr from z ∼ 10 to z ∼ 8. This increase is ⩾4 × larger than expected from the lower redshift extrapolation of the UV LF. We are thus likely witnessing the first rapid buildup of galaxies in the heart of cosmic reionization. Future deep Hubble Space Telescope WFC3/IR data, reaching to well beyond 29 mag, can enable a more robust quantification of the accelerated evolution around z ∼ 10.
Dynamic Multi-Reference Generative Prediction for Face Video Compression

Face videos own abundant structured information and prior knowledge which can be utilized by generative neural networks to achieve ultra-low bitrate compression. However, generative neural network based face video compression suffers from large head motion which may easily result in deformed images. In this paper, the dynamic multi-reference prediction method is proposed for generative face video compression. Specifically, key map is extracted as the compact latent to represent the face image. The key maps of the current frame and multiple reference frames are used together to estimate multiple dense motion maps. The multiple motion maps are further applied to the corresponding reference frames to generate the final prediction of the current frame. Moreover, the reference frame can be dynamically refreshed during encoding to convert large head motion to relatively small motion. Experimental results show that the proposed method achieves superior compression performance compared to the state-of-the-art VVC standard as well as the latest generative face compression frameworks.
On high-order pressure-robust space discretisations, their advantages for incompressible high Reynolds number generalised Beltrami flows and beyond

An improved understanding of the divergence-free constraint for the incompressible Navier--Stokes equations leads to the observation that a semi-norm and corresponding equivalence classes of forces are fundamental for their nonlinear dynamics. The recent concept of {\em pressure-robustness} allows to distinguish between space discretisations that discretise these equivalence classes appropriately or not. This contribution compares the accuracy of pressure-robust and non-pressure-robust space discretisations for transient high Reynolds number flows, starting from the observation that in generalised Beltrami flows the nonlinear convection term is balanced by a strong pressure gradient. Then, pressure-robust methods are shown to outperform comparable non-pressure-robust space discretisations. Indeed, pressure-robust methods of formal order $k$ are comparably accurate than non-pressure-robust methods of formal order $2k$ on coarse meshes. Investigating the material derivative of incompressible Euler flows, it is conjectured that strong pressure gradients are typical for non-trivial high Reynolds number flows. Connections to vortex-dominated flows are established. Thus, pressure-robustness appears to be a prerequisite for accurate incompressible flow solvers at high Reynolds numbers. The arguments are supported by numerical analysis and numerical experiments.
Asteroseismology of binary stars and a compilation of core overshoot and rotational frequency values of OB stars

After a brief introduction into the asteroseismic modelling of stars, we provide a compilation of the current seismic estimates of the core overshooting parameter and of the rotational frequency of single and binary massive stars. These important stellar parameters have meanwhile become available for eleven OB-type stars, among which three spectroscopic pulsating binaries and one magnetic pulsator. We highlight the potential of ongoing and future analyses of eclipsing binary pulsators as essential laboraties to test stellar structure and evolution models of single and binary stars.