Miracle-dz/UniFAR-FTUs huggingface dataset:
A 260-GHz Four-Way Phase Compensated CMOS Frequency Multiplier Chain

A novel × 6 frequency multiplier chain with a center frequency of 260 GHz is developed in 40 nm CMOS and measured through this work. The multiplication is accomplished through an × 3 frequency multiplier followed by a doubler successive stage. A four-way signal combiner is employed to enhance the output power, whereas phase shifters are dedicated for compensating the possible phase deviations between the different combined ways, and consequently maintain the combining efficiency. For further output power boosting, the output matching network of 260-GHz frequency doubler is optimized, and a stacked amplifier with 11.5 dBm is employed as a driving amplifier. The multiplier has been fabricated and a peak output power of 3.0 dBm is measured at 260 GHz with a 3-dB bandwidth of 17 GHz.
Calibrating the baryon oscillation ruler for matter and halos

We characterize the nonlinear evolution of the baryon acoustic feature as traced by the dark matter and halos, using a combination of perturbation theory and N-body simulations. We confirm that the acoustic peak traced by the dark matter is both broadened and shifted as structure forms, and that this shift is well described by second-order perturbation theory. These shifts persist for dark matter halos, and are a simple function of halo bias, with the shift (mostly) increasing with increasing bias. Extending our perturbation theory results to halos with simple two parameter bias models (both in Lagrangian and Eulerian space) quantitatively explains the observed shifts. In particular, we demonstrate that there are additional terms that contribute to the shift that are absent for the matter. At z = 0 for currently favored cosmologies, the matter shows shifts of ~0.5%, b = 1 halos shift the acoustic scale by ~0.2%, while b = 2 halos shift it by ~0.5%; these shifts decrease by the square of the growth factor D(z) at higher redshifts. These results are easily generalized to galaxies within the halo model, where we show that simple galaxy models show marginally larger shifts than the correspondingly biased halos, due to the contribution of satellites in high mass halos. While our focus here is on real space, our results make specific predictions for redshift space. For currently favored cosmological models, we find that the shifts for halos at z = 0 increase by ~0.3%; at high z, they increase by ~0.5%D 2 . Our results demonstrate that these theoretical systematics are smaller than the statistical precision of upcoming surveys, even if one ignored the corrections discussed here. Simple modeling, along the lines discussed here, has the potential to reduce these systematics to below the levels of cosmic variance limited surveys.
The YSZ,Planck – YSZ,XMM scaling relation and its difference between cool-core and non-cool-core clusters

We construct a sample of 70 clusters using data from XMM-Newton and Planck to investigate the YSZ,Planck – YSZ,XMM scaling relation and the cool-core influences on this relation. YSZ,XMM is calculated by accurately de-projected temperature and electron number density profiles derived from XMM-Newton. YSZ,Planck is the latest Planck data restricted to our precise X-ray cluster size θ500. To study the cool-core influences on the YSZ,Planck – YSZ,XMM scaling relation, we apply two criteria, namely the limits of central cooling time and classic mass deposition rate, to distinguish cool-core clusters (CCCs) from non-cool-core clusters (NCCCs). We also use YSZ,Planck from other papers, which are derived from different methods, to confirm our results. The intercept and slope of the YSZ,Planck – YSZ,XMM scaling relation are A = –0.86 ± 0.30 and B = 0.83 ± 0.06 respectively. The intrinsic scatter is σins = 0.14 ± 0.03. The ratio of YSZ,Planck/YSZ,XMM is 1.03 ± 0.05, which is in excellent statistical agreement with unity. Discrepancies in the YSZ,Planck – YSZ,XMM scaling relation between CCCs and NCCCs are found in the observation. They are independent of the cool-core classification criteria and YSZ,Planck calculation methods, although the discrepancies are more significant under the classification criteria of classic mass deposition rate. The intrinsic scatter of CCCs (0.04) is quite small compared to that of NCCCs (0.27). The ratio of YSZ,Planck/YSZ,XMM for CCCs is 0.89 ± 0.05, suggesting that CCCs’ YSZ,XMM may overestimate the Sunyaev-Zel’dovich (SZ) signal. By contrast, the ratio of YSZ,Planck/YSZ,XMM for NCCCs is 1.14 ± 0.12, which indicates that NCCCs’ YSZ,XMM may underestimate the SZ signal.
Activity, diffusion, and correlations in a two-dimensional conserved stochastic sandpile

We perform large-scale simulations of a two-dimensional restricted height conserved stochastic sandpile, focusing on particle diffusion and mobility, and spatial correlations. Quasistationary (QS) simulations yield the critical particle density to high precision [pc = 0.7112687(2)], and show that the diffusion constant scales in the same manner as the activity density, as found previously in the one-dimensional case. Short-time scaling is characterized by subdiffusive behavior (mean-square displacement ∼ tγ with γ < 1), which is easily understood as a consequence of the initial decay of activity, ρ(t) ∼ t−δ, with γ = 1 − δ. We verify that at criticality, the activity-activity correlation function C(r)∼r−β/ν⊥ ? >, as expected at an absorbing-state phase transition. Our results for critical exponents are consistent with, and somewhat more precise than, predictions derived from the Langevin equation for stochastic sandpiles in two dimensions.
F4, E6 and G2 exceptional gauge groups in the vacuum domain structure model

Using vacuum domain structure model, trivial static potentials in various representations of $F_4$, $E_6$ and $G_2$ exceptional groups are calculated by means of the unit center element. Due to the absence of the non-trivial center elements, the potential of every representation is screened at far distances. However, the linear part is observed at intermediate quark separations which is investigated by the decomposition of the exceptional group to its maximal subgroups. Comparing the group factor of the super-group with the corresponding one obtained from the non-trivial center elements of $SU(3)$ subgroup, shows that $SU(3)$ is not the direct cause of temporary confinement in any of the exceptional groups. However, the trivial potential obtained from the group decomposition to the $SU(3)$ subgroup is the same as the potential of the super-group itself. In addition, any regular or singular decomposition to the $SU(2)$ subgroup which produces the Cartan generator with the same elements as $h_1$, in any exceptional group, leads to the linear intermediate potential of the exceptional gauge groups. The other $SU(2)$ decompositions with the Cartan generator different from $h_1$, are still able to describe the linear potential if the number of $SU(2)$ non-trivial center element which emerge in the decompositions is the same. As a result, it is the center vortices quantized in terms of non-trivial center element of the $SU(2)$ subgroup which give rise to the intermediate confinement in the static potentials.
1D Classical Density Functional Theory of a Tethered Polymer Layer

A simple application of classical density functional theory is derived and applied to a system of polymers grafted to a plane. The system is assumed to have symmetry in directions parallel to the grafting plane hence it being a '1-dimensional' problem. A quick introduction to using propagators in the theory of chains in the presence of external fields and a numerical algorithm for solving the modified diffusion (or Fokker-Planck) equation are presented. Density profiles are found for hard-sphere chains which agree with results in the literature (see Murat,., Milner,., Muhukumar and others) and align with physical expectations of brush formation due to excluded volume. The linear scaling $h \approx (\sigma)^{1/3} N$, of brush height with polymerisation $N$, is reproduced here.
FIRST DYNAMIC COMPUTATIONS OF SYNCHROTRON EMISSION FROM THE CYGNUS A RADIO CAVITY: EVIDENCE FOR ELECTRON PAIR PLASMA IN CAVITY

Cosmic rays, thermal gas and magnetic fields in FRII radio cavities are assumed to come entirely from winds flowing from just behind the jet shocks. Combining analytic and computational methods, it is shown that the computed radio-electron energy distribution and synchrotron emissivity spectra everywhere in the Cygnus A radio cavity agree with radio observations of the Cygnus A lobes. The magnetic field energy density is small everywhere and evolves passively in the post-shock wind. Most synchrotron emission arises in recent post-shock material as it flows back along the radio cavity wall. Because it experienced less adiabatic expansion, the magnetic field in this young backflow is larger than elsewhere in the radio lobe, explaining the observed radio synchrotron limb-brightening. The boundary backflow decelerates due to small cavity pressure gradients, causing large-scale fields perpendicular to the backflow (and synchrotron emission) to grow exponentially unlike observations. However, if the field is random on subgrid (sub-kpc) scales, the computed field reproduces both the magnitude and slowly decreasing radio synchrotron emissivity observed along the backflow. The radio synchrotron spectrum and image computed with a small-scale random field agree with Very Large Array observations. The total relativistic energy density in the post-jet shock region required in computations to inflate the radio cavity matches the energy density of relativistic electrons observed in the post-shock region of Cygnus A. This indicates that the component in the jet and cavity that dominates the dynamical evolution is a relativistic pair plasma.
Discovery of a Magnetic White Dwarf with Unusual Short-period Variability

We report the discovery of a magnetic white dwarf which shows periodic variability with P=110 min, color-dependent amplitudes and a transient phase shift in the blue compared to the red lightcurve - a previously unknown type of variability for this type of object. We attribute the variations either to a close ultracool (thus far undetected) companion or, more likely, to magnetic spots with unusual temperature structure.
Red clump stars of the Milky Way - laboratories of extra-mixing

In this work we present the main atmospheric parameters, carbon, nitrogen and oxygen abundances, and 12 C/ 13 C ratios determined in a sample of 28 Galactic clump stars. Abundances of carbon were studied using the C2 band at 5086.2 u The wavelength interval 7980–8130 u with strong CN features was analysed in order to determine nitrogen abundances and 12 C/ 13 C isotope ratios. The oxygen abundances were determined from the [Oi] line at 6300 u The mean abundances of C, N and O abundances in the investigated clump stars support our previous estimations that, compared to the Sun and dwarf stars of the Galactic disk, carbon is depleted by about 0.2 dex, nitrogen is enhanced by 0.2 dex and oxygen is close to abundances in dwarfs. The 12 C/ 13 C and C/N ratios for galactic red clump stars analysed were compared to the evolutionary models of extra-mixing. The steeper drop of 12 C/ 13 C ratio in the model of thermohaline mixing by Charbonnel & Lagarde better reflects the observational data at low stellar masses than the more shallow model of cool bottom processing by Boothroyd & Sackman. For stars of about 2 M⊙ masses a modelling of rotationally induced mixing should be considered with rotation of about 250kms −1 at the time when a star was at the hydrogen-core-burning stage.
Yukawa unification in SUSY SO(10) in light of the LHC Higgs data

The status of top-bottom-tau Yukawa coupling unification in supersymmetric SO(10) models is reviewed with a particular emphasis on the implications of the Higgs boson mass in the vicinity of 125 GeV, as suggested by the LHC Higgs data. In addition, the recently proposed model with negative \mu, D-term splitting of the soft scalar masses and non-universal gaugino masses generated by a non-zero F-term in a 24-dimensional representation of SU(5) \subset SO(10) is re-analysed in the context of the 125 GeV Higgs. The condition of top-bottom-tau Yukawa unification together with the Higgs mass of about 125 GeV impose strong lower mass limits on SUSY particles. Nevertheless, some of the MSSM particles may be within the reach of the LHC. In the case of models with positive \mu this is the gluino. While in the case of negative \mu these are the pseudoscalar Higgs, the lighter sbottom (sometimes strongly degenerate with the LSP leading to sbottom coannihilations), the right-handed down squark and the gluino.
ESS-IoT: The Smart Waste Management System for General Household
Shen Yuong Wong, Huashuo Han, Kin Meng Cheng, Ah Choo Koo and Salman Yussof

With the urban population’s growth, unethical and unmanaged waste disposal may negatively impact the environment. In many cities, a massive flow of people in municipal buildings or offices has generated vast amounts of waste daily, which correlates to the enormous expenses of waste management. The critical issue for better waste management is waste collection and sorting. In this study, the Electronic Smart Sorting- Internet of Things (ESS-IoT) is proposed to assist people in better waste management. The ESS-IoT system uses Raspberry Pi 4b as the microcontroller with three modules, and it is designed with two main functions: waste collection and waste classification. The two main functions have been deployed separately in the literature, while this study has combined both functions to achieve a more comprehensive smart bin waste disposal solution. Waste collection is triggered by the overflow alarm mechanism that employs ultrasonic and tracker sensors. On the other hand, the waste classification is implemented using two classification algorithms: Random Forest (RF) prediction model and Convolutional Neural Network (CNN) prediction model. An experiment is conducted to evaluate the accuracy of the two classification algorithms in classifying various types of waste. The waste materials under investigation can be classified into four categories: kitchen waste, recyclables, hazardous waste, and other waste. The results show that CNN is the better classification algorithm between the two. Future work proposes the research extension by introducing an incentive mechanism to motivate the household communities using a cloud-based competition platform incorporated with the ESS-IoT system.
Z (4430) and a new paradigm for spin interactions in tetraquarks

Following the recent confirmation of the Z+(4430) resonance with J^{PG}=1^{++}, we have re-examined the model of S- and P-wave tetraquarks. We propose a `type-II' diquark-antidiquark model which shows to be very effective at producing a simple and comprehensive picture of the J^{PG}=1^{++} and 1^{--} sectors of the recently discovered charged tetraquarks and of the observed Y resonances. The model is still faced with the unresolved difficulty of explaining why some states seem to have incomplete isospin multiplets.
A TRANSIENT SUPERGIANT X-RAY BINARY IN IC 10: AN EXTRAGALACTIC SFXT?

We report the discovery of a large amplitude (factor of ∼100) X-ray transient (IC 10 X-2, CXOU J002020.99+591758.6) in the nearby dwarf starburst galaxy IC 10 during our Chandra monitoring project. Based on the X-ray timing and spectral properties, and an optical counterpart observed with Gemini, the system is a high-mass X-ray binary consisting of a luminous blue supergiant and a neutron star. The highest measured luminosity of the source was 1.8 × 1037 erg s−1during an outburst in 2003. Observations before, during, and after a second outburst in 2010 constrain the outburst duration to be less than 3 months (with no lower limit). The X-ray spectrum is a hard power law (Γ = 0.3) with fitted column density (NH = 6.3 × 1021 atom cm−2), consistent with the established absorption to sources in IC 10. The optical spectrum shows hydrogen Balmer lines strongly in emission at the correct blueshift (–340 km s−1) for IC 10. The N iii triplet emission feature is seen, accompanied by He ii [4686] weakly in emission. Together these features classify the star as a luminous blue supergiant of the OBN subclass, characterized by enhanced nitrogen abundance. Emission lines of He i are seen, at similar strength to Hβ. A complex of Fe ii permitted and forbidden emission lines are seen, as in B[e] stars. The system closely resembles galactic supergiant fast X-ray transients, in terms of its hard spectrum, variability amplitude, and blue supergiant primary.
Recent outburst activity of the symbiotic binary AG Draconis

The symbiotic binary AG Dra regularly undergoes quiescent and active stages which consist of several outbursts repeating with about 360d interval. The recent outburst activity of AG Dra started by the minor outburst in the late spring of 2015 and was definitely confirmed by the outbursts in April 2016 and May 2017. In the presented work, the photometric and spectroscopic behaviour of the recent outburst activity of AG Dra is presented in detail. Moreover, the temperature of the white dwarf in AG Dra is studied based on the behaviour of the prominent emission lines. We show that a disentanglement of particular effects in the observed changes of the emission lines is crucial to investigate the intrinsic white dwarf temperature variations related to outburst activity of this strongly interacting binary. We also report the effects of the low excitation lines orbital variations and of the H$_{\beta}$ absorption component on their equivalent widths as well as consequences of the approximations used in our previous works.
Black Hole Mass Scaling Relations for Spiral Galaxies. I. MBH–M*,sph

The (supermassive black hole mass, MBH)–(bulge stellar mass, ) relation is, obviously, derived using two quantities. We endeavor to provide accurate values for the latter via detailed multicomponent galaxy decompositions for the current full sample of 43 spiral galaxies having directly measured MBH values; 35 of these galaxies have been alleged to contain pseudobulges, 21 have water maser measurements, and three appear bulgeless. This more than doubles the previous sample size of spiral galaxies with a finessed image analysis. We have analyzed near-infrared images, accounting for not only the bulge, disk (exponential, truncated, or inclined), and bar but also spiral arms and rings and additional central components (active galactic nuclei (AGNs), etc.). A symmetric Bayesian analysis finds = / + (7.24 ± 0.12), with υ a stellar mass-to-light ratio term. The level of scatter equals that about the MBH–σ* relation. The nonlinear slope rules out the idea that many mergers, coupled with the central limit theorem, produced this scaling relation, and it corroborates previous observational studies and simulations, which have reported a near-quadratic slope at the low-mass end of the MBH– diagram. Furthermore, bulges with AGNs follow this relation; they are not offset by an order of magnitude, and models that have invoked AGN feedback to establish a linear MBH– relation need revisiting. We additionally present an updated MBH–(Sérsic index, nsph) relation for spiral galaxy bulges with a comparable level of scatter and a new –(spiral-arm pitch angle, ϕ) relation.
A deep XMM–Newton study of the hot gaseous halo around NGC 1961

We examine 11 XMM-Newton observations of the giant spiral galaxy NGC 1961, allowing us to study the hot gaseous halo of a spiral galaxy in unprecedented detail. We perform a spatial and a spectral analysis; with the former, the hot halo is detected to at least 80 kpc and with the latter its properties can be measured in detail up to 42 kpc. We find evidence for a negative gradient in the temperature profile as is common for elliptical galaxies. We measure a rough metallicity profile, which is consistent with being flat at $Z \sim 0.2 Z_{\odot}$. Converting to this metallicity, the deprojected density profile is consistent with previous parametric fits, with no evidence for a break within 42 kpc ($\sim$0.1R$_{\text{vir}}$). Extrapolating to the virial radius, we infer a hot halo mass comparable to the stellar mass of the galaxy, and a baryon fraction from the stars and hot gas of around 30%. The cooling time of the hot gas is orders of magnitude longer than the dynamical time, making the hot halo stable against cooling instabilities, and we argue that an extended stream of neutral Hydrogen seen to the NW of this galaxy is instead likely due to accretion from the intergalactic medium. The low metallicity of the hot halo suggests it too was likely accreted. We compare the hot halo of NGC 1961 to hot halos around isolated elliptical galaxies, and show that the total mass determines the hot halo properties better than the stellar mass.
THE NEXT GENERATION VIRGO CLUSTER SURVEY. V. MODELING THE DYNAMICS OF M87 WITH THE MADE-TO-MEASURE METHOD

We study the dynamics of the giant elliptical galaxy M87 from the central to the outermost regions with the made-to-measure (M2M) method. We use a new catalog of 922 globular cluster line-of-sight velocities extending to a projected radius of 180 kpc (equivalent to 25 M87 effective radii), and SAURON integral field unit data within the central 2.4 kpc. There are 263 globular clusters, mainly located beyond 40 kpc, newly observed by the Next Generation Virgo Survey. For the M2M modeling, the gravitational potential is taken as a combination of a luminous matter potential with a constant stellar mass-to-light ratio and a dark matter potential modeled as a logarithmic potential. Our best-fit dynamical model returns a stellar mass-to-light ratio in the I band of M/LI = 6.0 ± 0.3 with a dark matter potential scale velocity of 591 ± 50 km s−1 and scale radius of 42 ± 10 kpc. We determine the total mass of M87 within 180 kpc to be (1.5 ± 0.2) × 1013 M☉. The mass within 40 kpc is smaller than previous estimates determined using globular cluster kinematics that did not extend beyond ∼45 kpc. With our new globular cluster velocities at much larger radii, we see that globular clusters around 40 kpc show an anomalously large velocity dispersion which affected previous results. The mass we derive is in good agreement with that inferred from ROSAT X-ray observation out to 180 kpc. Within 30 kpc our mass is also consistent with that inferred from Chandra and XMM-Newton X-ray observations, while within 120 kpc it is about 20% smaller. The model velocity dispersion anisotropy β parameter for the globular clusters in M87 is small, varying from −0.2 at the center to 0.2 at ∼40 kpc, and gradually decreasing to zero at ∼120 kpc.