Miracle-dz/UniFAR-FTUs huggingface dataset:
THE PRESSURE PROFILES OF HOT GAS IN LOCAL GALAXY GROUPS

Recent measurements of the Sunyaev–Zel'dovich (SZ) angular power spectrum from the South Pole Telescope and the Atacama Cosmology Telescope demonstrate the importance of understanding baryon physics when using the SZ power spectrum to constrain cosmology. This is challenging since roughly half of the SZ power at ℓ = 3000 is from low-mass systems with 1013 h−1 M☉ < M500 < 1.5 × 1014 h−1 M☉, which are more difficult to study than systems of higher mass. We present a study of the thermal pressure content for a sample of local galaxy groups from Sun et al. The group Ysph,500–M500 relation agrees with the one for clusters derived by Arnaud et al. The group median pressure profile also agrees with the universal pressure profile for clusters derived by Arnaud et al. With this in mind, we briefly discuss several ways to alleviate the tension between the measured low SZ power and the predictions from SZ templates.
A SYSTEMATIC STUDY OF CARBON–OXYGEN WHITE DWARF MERGERS: MASS COMBINATIONS FOR TYPE Ia SUPERNOVAE

Mergers of two carbon–oxygen (CO) white dwarfs (WDs) have been considered to be progenitors of Type Ia supernovae (SNe Ia). Based on smoothed particle hydrodynamics (SPH) simulations, previous studies have claimed that mergers of CO WDs lead to SN Ia explosions either in the dynamical merger phase or the stationary rotating merger remnant phase. However, the mass range of CO WDs that lead to SNe Ia has not yet been clearly identified. In the present work, we perform systematic SPH merger simulations for the WD masses ranging from 0.5 M ⊙ ? > to 1.1 M ⊙ ? > with higher resolutions than the previous systematic surveys and examine whether or not carbon burning occurs dynamically or quiescently in each phase. We further study the possibility of SNe Ia explosions and estimate the mass range of CO WDs that lead to SNe Ia. We found that when both WDs are massive, i.e., in the mass range of 0.9 M ⊙ ≤ M 1,2 ≤ 1.1 M ⊙ ? > , they can explode as an SN Ia in the merger phase. On the other hand, when the more massive WD is in the range of 0.7 M ⊙ ≤ M 1 ≤ 0.9 M ⊙ ? > and the total mass exceeds 1.38 M ⊙ ? > , they can finally explode in the stationary rotating merger remnant phase. We estimate the contribution of CO WD mergers to the entire SN Ia rate in our galaxy to be of ≲ 9 % ? > . Thus, it might be difficult to explain all galactic SNe Ia with CO WD mergers.
Enhanced Candidate Selection Algorithm for Analog Circuit Verification

In latest years, the complexity and applicability of modern Integrated Circuits (ICs) grew exponentially, hence the high-pressure to deliver IC designs faster on the market. For safety, a design meeting its specification under any allowed operating condition and fabrication variation is a prerequisite. Therefore, pre-Silicon (pre-Si) analog IC verification is an extremely important task, as in certain regions of this large parameter space, the device exhibits degraded performance, or it fails completely. During verification, a designer must find these regions of the input parameter space where the circuit fails. Ideally this must be done during pre-Si phase, to avoid potential huge re-design delays during prototyping or production. In this context, this paper presents a Machine Learning (ML) approach, where we sample the input space to offer good initial coverage of the operating conditions (OCs) hyperspace, with a small number of simulations. We denote one input of a circuit as an Operating Condition. We then leverage a ML-surrogate model of the circuit instead of time-consuming simulations to propose, during a candidate selection phase, new circuit worst cases, where the circuit fails. After updating the candidate proposal algorithm to include a Gradient Descent (GD) step, we highlight the performance improvement of this new method on synthetic circuits, where we obtain relative absolute verification errors below 1%, while using less simulations than other classical approaches.
A UNIVERSAL LAW FOR SOLAR-WIND TURBULENCE AT ELECTRON SCALES

The interplanetary magnetic fluctuation spectrum obeys a Kolmogorovian power law at scales above the proton inertial length and gyroradius which is well regarded as an inertial range. Below these scales, a power-law index around −2.5 is often measured and associated with nonlinear dispersive processes. Recent observations reveal a third region at scales below the electron inertial length. This region is characterized by a steeper spectrum that some refer to as the dissipation range. We investigate this range of scales in the electron magnetohydrodynamic approximation and derive an exact and universal law for a third-order structure function. This law can predict a magnetic fluctuation spectrum with an index of −11/3 which is in agreement with the observed spectrum at the smallest scales. We conclude on the possible existence of a third turbulence regime in the solar wind instead of a dissipation range as recently postulated.
A FLARE OBSERVED IN CORONAL, TRANSITION REGION, AND HELIUM I 10830 Å EMISSIONS

On 2012 June 17, we observed the evolution of a C-class flare associated with the eruption of a filament near a large sunspot in the active region NOAA 11504. We obtained high spatial resolution filtergrams using the 1.6 m New Solar Telescope at the Big Bear Solar Observatory in broadband TiO at 706 nm (bandpass: 10 Å) and He i 10830 Å narrow band (bandpass: 0.5 Å, centered 0.25 Å to the blue). We analyze the spatio-temporal behavior of the He i 10830 Å data, which were obtained over a 90″×90″ field of view with a cadence of 10 s. We also analyze simultaneous data from the Atmospheric Imaging Assembly and Extreme Ultraviolet Variability Experiment instruments on board the Solar Dynamics Observatory spacecraft, and data from the Reuven Ramaty High Energy Solar Spectroscopic Imager and GOES spacecrafts. Non-thermal effects are ignored in this analysis. Several quantitative aspects of the data, as well as models derived using the “0D” enthalpy-based thermal evolution of loops model code, indicate that the triplet states of the 10830 Å multiplet are populated by photoionization of chromospheric plasma followed by radiative recombination. Surprisingly, the He ii 304 Å line is reasonably well matched by standard emission measure calculations, along with the C iv emission which dominates the Atmosphere Imaging Assembly 1600 Å channel during flares. This work lends support to some of our previous work combining X-ray, EUV, and UV data of flares to build models of energy transport from corona to chromosphere.
THE HIGH-MASS STELLAR INITIAL MASS FUNCTION IN M31 CLUSTERS

We have undertaken the largest systematic study of the high-mass stellar initial mass function (IMF) to date using the optical color–magnitude diagrams (CMDs) of 85 resolved, young ( 4 Myr < t < 25 Myr ? > ), intermediate mass star clusters (103–104 M⊙), observed as part of the Panchromatic Hubble Andromeda Treasury program. We fit each cluster’s CMD to measure its mass function (MF) slope for stars ≳2 M⊙. By modeling the ensemble of clusters, we find the distribution of MF slopes is best described by Γ = + 1.45 − 0.06 + 0.03 ? > with a very small intrinsic scatter and no drastic outliers. This model allows the MF slope to depend on cluster mass, size, and age, but the data imply no significant dependencies within this regime of cluster properties. The lack of an age dependence suggests that the MF slope has not significantly evolved over the first ∼25 Myr and provides direct observational evidence that the measured MF represents the IMF. Taken together, this analysis—based on an unprecedented large sample of young clusters, homogeneously constructed CMDs, well-defined selection criteria, and consistent principled modeling—implies that the high-mass IMF slope in M31 clusters is universal. The IMF has a slope ( Γ = + 1.45 − 0.06 + 0.03 ? > ; statistical uncertainties) that is slightly steeper than the canonical Kroupa ( + 1.30 ? > ) and Salpeter ( + 1.35 ? > ) values, and our measurement of it represents a factor of ∼20 improvement in precision over the Kroupa IMF (+1.30 ± 0.7). Using our inference model on select Milky Way (MW) and LMC high-mass IMF studies from the literature, we find Γ MW ∼ + 1.15 ± 0.1 ? > and Γ LMC ∼ + 1.3 ± 0.1 ? > , both with intrinsic scatter of ∼0.3–0.4 dex. Thus, while the high-mass IMF in the Local Group may be universal, systematics in the literature of IMF studies preclude any definitive conclusions; homogenous investigations of the high-mass IMF in the local universe are needed to overcome this limitation. Consequently, the present study represents the most robust measurement of the high-mass IMF slope to date. To facilitate practical use over the full stellar mass spectrum, we have grafted the M31 high-mass IMF slope onto widely used sub-solar mass Kroupa and Chabrier IMFs. The increased steepness in the M31 high-mass IMF slope implies that commonly used UV- and Hα-based star formation rates should be increased by a factor of ∼1.3–1.5 and the number of stars with masses > 8 ? > M⊙ is ∼25% fewer than expected for a Salpeter/Kroupa IMF.
Flux Modulation from the Rossby Wave Instability in microquasars' accretion disks: toward a HFQPO model

Context. There has been a long string of efforts to understand the source of the variability observed in microquasars, especially concerning the elusive high-frequency quasi-periodic oscillation. These oscillations are among the fastest phenomena that affect matter in the vicinity of stellar black holes and therefore could be used as probes of strong-field general relativity. Nevertheless, no model has yet gained wide acceptance. Aims. The aim of this article is to investigate the model derived from the occurrence of the Rossby wave instability at the inner edge of the accretion disk. In particular, our goal here is to demonstrate the capacity of this instability to modulate the observed flux in agreement with the observed results. Methods. We used the AMRVAC hydrodynamical code to model the instability in a 3D optically thin disk. The GYOTO ray-tracing code was then used to compute the associated light curve. Results. We show that the 3D Rossby wave instability is able to modulate the flux well within the observed limits. We highlight that 2D simulations allow us to obtain the same general characteristics of the light curve as 3D calculations. With the time resolution we adopted in this work, 3D simulations do not give rise to any new observable features that could be detected by current instrumentation or archive data.
Ultralow loss single-mode silica tapers manufactured by a microheater

Using a ceramic thermoelectric heater, we show highly reproducible fabrication of single-mode subwavelength silica tapers with an ultralow loss level. The reproducibility of the process is studied statistically, leading to an average taper transmission of 94%. The best tapers have a transmission superior to 99%, above the level commonly reached by other fabrication methods. The taper profile is inspected along its length and closely follows the exponential profile predicted by the model of Birks and Li. This high degree of control over the taper shape allows a detailed analysis of the transition to the single-mode regime during tapering. As an application of this fabrication method, we present a microlooped taper probe for evanescent coupling experiments requiring fine spatial selectivity.
A MULTIPLICITY CENSUS OF INTERMEDIATE-MASS STARS IN SCORPIUS–CENTAURUS

Stellar multiplicity properties have been studied for the lowest and the highest stellar masses, but intermediate-mass stars from F-type to late A-type have received relatively little attention. Here, we report on a Gemini/NICI snapshot imaging survey of 138 such stars in the young Scorpius–Centaurus (Sco–Cen) region, for the purpose of studying multiplicity with sensitivity down to planetary masses at wide separations. In addition to two brown dwarfs and a companion straddling the hydrogen-burning limit which we reported previously, here we present 26 new stellar companions and determine a multiplicity fraction within 0. ″1–5. ″0 of 21% ± 4%. Depending on the adopted semimajor axis distribution, our results imply a total multiplicity in the range of ∼60%–80%, which further supports the known trend of a smooth continuous increase in the multiplicity fraction as a function of primary stellar mass. A surprising feature in the sample is a distinct lack of nearly equal-mass binaries, for which we discuss possible reasons. The survey yielded no additional companions below or near the deuterium-burning limit, implying that their frequency at >200 AU separations is not quite as high as might be inferred from previous detections of such objects within the Sco–Cen region.
INTERSTELLAR EXTINCTION LAW TOWARD THE GALACTIC CENTER III: J, H, KS BANDS IN THE 2MASS AND THE MKO SYSTEMS, AND 3.6, 4.5, 5.8, 8.0 μm IN THE SPITZER/IRAC SYSTEM

We have determined interstellar extinction law toward the Galactic center (GC) at the wavelength from 1.2 to 8.0 μm, using point sources detected in the IRSF/SIRIUS near-infrared (NIR) survey and those in the Two Micron All Sky Survey (2MASS) and Spitzer/IRAC/GLIMPSE II catalogs. The central region ∣l ∣ ≲3. °0 and ∣b ∣ ≲1. °0 has been surveyed in the J, H, and KS bands with the IRSF telescope and the SIRIUS camera whose filters are similar to the Mauna Kea Observatories (MKO) NIR photometric system. Combined with the GLIMPSE II point source catalog, we made KS versus KS − λ color–magnitude diagrams (CMDs) where λ=3.6, 4.5, 5.8, and 8.0 μm. The KS magnitudes of bulge red clump stars and the KS − λ colors of red giant branches are used as a tracer of the reddening vector in the CMDs. From these magnitudes and colors, we have obtained the ratios of total-to-selective extinction for the four IRAC bands. Combined with for the J and H bands derived by Nishiyama et al., we obtain AJ:AH::A[3.6]:A[4.5]:A[5.8]:A[8.0] = 3.02:1.73:1:0.50:0.39:0.36:0.43 for the line of sight toward the GC. This confirms the flattening of the extinction curve at λ ≳ 3 μm from a simple extrapolation of the power-law extinction at shorter wavelengths, in accordance with recent studies. The extinction law in the 2MASS J, H, and KS bands has also been calculated, and good agreement with that in the MKO system is found. Thus, it is established that the extinction in the wavelength range of J, H, and KS is well fitted by a power law of steep decrease Aλ ∝ λ−2.0 toward the GC. In nearby molecular clouds and diffuse interstellar medium, the lack of reliable measurements of the total-to-selective extinction ratios hampers unambiguous determination of the extinction law; however, observational results toward these lines of sight cannot be reconciled with a single extinction law.
SALT long-slit spectroscopy of quasar HE 0435-4312: fast displacement of the Mg II emission line

Context. The Mg II emission line is visible in the optical band for intermediate redshift quasars (0.4 We aim to determine the substructure and the variability of the Mg II line with the aim to identify which part of the line comes from a medium in Keplerian motion.Methods. Using the Southern African Large Telescope (SALT) with the Robert Stobie Spectrograph (RSS) we performed ten spectroscopic observations of quasar HE 0435-4312 (z = 1.2231) over a period of three years (Dec. 23/24, 2012 to Dec. 7/8, 2015). Results. Both the Mg II line and the Fe II pseudo-continuum increase with time. We clearly detect the systematic shift of the Mg II line with respect to the Fe II over the years, corresponding to the acceleration of 104 ± 14 km s-1 yr-1 in the quasar rest frame. The Mg II line shape is clearly non-Gaussian but single-component, and the increase in line equivalent width and line shift is not accompanied with significant evolution of the line shape. We analyse the conditions in the Mg II and Fe II formation region and we note that the very large difference in the covering factor and the turbulent velocity also support the conclusion that the two regions are spatially separated.Conclusions. The measured acceleration of the line systematic shift is too large to connect it with the orbital motion at a distance of the BLR in this source. It may imply a precessing inner disk illuminating the BLR. Further monitoring is still needed to better constrain the variability mechanism.
Calculation of Nucleon Electric Dipole Moments Induced by Quark Chromo-Electric Dipole Moments and the QCD $\theta$-term

Electric dipole moments (EDMs) of nucleons and nuclei, which are sought as evidence of CP violation, require lattice calculations to connect constraints from experiments to limits on the strong CP violation within QCD or CP violation introduced by new physics from beyond the standard model. Nucleon EDM calculations on a lattice are notoriously hard due to large statistical noise, chiral symmetry violating effects, and potential mixing of the EDM and the anomalous magnetic moment of the nucleon. In this report, details of ongoing lattice calculations of proton and neutron EDMs induced by the QCD $\theta$-term and the quark chromo-EDM, the lowest-dimension effective CP-violating quark-gluon interaction are presented. Our calculation employs chiral-symmetric fermion discretization. An assessment of feasibility of nucleon EDM calculations at the physical point is discussed.
Prediction of Maximum Temperatures by Time Series and Artificial Neural Networks (Case Study: Isfahan Station)

Due to climate changes, global warming, and the recent drought, forecasting, checking, and analyzing maximum temperatures as one of the foremost imperative climatic parameters allows planners to plan and provide the necessary arrangements. The main reasons for checking the temperature as a parameter influencing nature are agriculture, pests, diseases, melting ice and flooding, evaporation and transpiration, and drought. Today, artificial neural networks are used to predict time series like temperature because of their feature for understanding the random mechanism of fully nonlinear and complex series. This study used data from 1953 to 2005, two methods, and multi-layer perceptron artificial neural networks with the learning algorithm after the error propagation to analyze and check the monthly maximum temperature. This issue used an input layer, five hidden layers of TANSIG, and an output layer of the pure line for artificial neural networks. The mean squared error criterion was also used to assess the results. In the following study, 70% of the total data were used as training data (RMSE = 1.8622 and MSE = 3.4677); in order to avoid the phenomenon of the over-load network, 15% of the data were used for validation data (RMSE = 1.7667 and MSE = 3.1213). The remaining 15 percent has also been used to check and test data. (RMSE = 2.134 and MSE = 4.5538). A comparison of monthly maximum temperature forecast results for 1953 and 2005 with observed data shows good agreement of the model. The overall results indicate that approximately every 64 years will add a degree to the temperature.
On the evolution of the bi-modal distribution of galaxies in the plane of specific star formation rate versus stellar mass

We have compared the observed distribution of galaxies in the plane of specific star formation rate versus stellar mass with the predictions of the Garching semi-analytic model at redshifts 0, 1 and 2. The goal is to test whether the implementation of radio-mode active galactic nucleus feedback, which, in the simulation, is responsible for terminating the formation of stars in high-mass galaxies, provides an adequate match to current high-redshift observations. The fraction of quenched galaxies as a function of stellar mass in the models is in good agreement with data at z = 0 and 1. By z = 2, there are too few quenched galaxies with low stellar masses in the models. At z = 2, the population of galaxies with no ongoing star formation is clearly separated from the ‘main sequence’ of star-forming galaxies in the data. This is not found in the models, because z = 2 galaxies with stellar masses less than ∼1011 M⊙ are predicted to host black holes with relatively low masses (less than 108 M⊙). The current implementation of radio-mode feedback from such black holes reduces the cooling rates from the surrounding halo, but does not generate sufficient energy to stop star formation entirely. We suggest that the models may be brought into better agreement with the data if black hole growth is triggered by disc instabilities in addition to major mergers, and if feedback mechanisms associated with the formation of galactic bulges act to quench star formation in galaxies.
SOLAR MULTIPLE ERUPTIONS FROM A CONFINED MAGNETIC STRUCTURE

How eruption can recur from a confined magnetic structure is discussed based on the Solar Dynamics Observatory observations of the NOAA active region 11444, which produced three eruptions within 1.5 hr on 2012 March 27. The active region (AR) had the positive-polarity magnetic fields in the center surrounded by the negative-polarity fields around. Since such a distribution of magnetic polarity tends to form a dome-like magnetic fan structure confined over the AR, the multiple eruptions were puzzling. Our investigation reveals that this event exhibits several properties distinct from other eruptions associated with magnetic fan structures: (i) a long filament encircling the AR was present before the eruptions; (ii) expansion of the open–closed boundary (OCB) of the field lines after each eruption was suggestive of the growing fan-dome structure, and (iii) the ribbons inside the closed magnetic polarity inversion line evolved in response to the expanding OCB. It thus appears that in spite of multiple eruptions the fan-dome structure remained undamaged, and the closing back field lines after each eruption rather reinforced the fan-dome structure. We argue that the multiple eruptions could occur in this AR in spite of its confined magnetic structure because the filament encircling the AR was adequate for slipping through the magnetic separatrix to minimize the damage to its overlying fan-dome structure. The result of this study provides a new insight into the productivity of eruptions from a confined magnetic structure.
ANCIENT PLANETARY SYSTEMS ARE ORBITING A LARGE FRACTION OF WHITE DWARF STARS

Infrared studies have revealed debris likely related to planet formation in orbit around ∼30% of youthful, intermediate mass, main-sequence stars. We present evidence, based on atmospheric pollution by various elements heavier than helium, that a comparable fraction of the white dwarf descendants of such main-sequence stars are orbited by planetary systems. These systems have survived, at least in part, through all stages of stellar evolution that precede the white dwarf. During the time interval (∼200 million years) that a typical polluted white dwarf in our sample has been cooling it has accreted from its planetary system the mass of one of the largest asteroids in our solar system (e.g., Vesta or Ceres). Usually, this accreted mass will be only a fraction of the total mass of rocky material that orbits these white dwarfs; for plausible planetary system configurations we estimate that this total mass is likely to be at least equal to that of the Sun's asteroid belt, and perhaps much larger. We report abundances of a suite of eight elements detected in the little studied star G241-6 that we find to be among the most heavily polluted of all moderately bright white dwarfs.