Miracle-dz/UniFAR-FTUs huggingface dataset:
Lightest CP-even Higgs boson mass in the testable flipped SU(5)×U(1)x models from F theory

We study the lightest CP-even Higgs boson mass in five kinds of testable flipped SU(5) x U(1)(X) models from F-theory. Two kinds of models have vectorlike particles around the TeV scale, while the other three kinds also have the vectorlike particles at the intermediate scale that can be considered as messenger fields in gauge-mediated supersymmetry breaking. We require that the Yukawa couplings for the TeV-scale vectorlike particles and the third family of the Standard Model (SM) fermions are smaller than three from the electroweak scale to the SU(3)(C) x SU(2)(L) unification scale. With the two-loop renormalization group equation running for the gauge couplings and Yukawa couplings, we obtain the maximal Yukawa couplings between the TeV-scale vectorlike particles and Higgs fields. To calculate the lightest CP-even Higgs boson mass upper bounds, we employ the renormalization group improved effective Higgs potential approach, and consider the two-loop leading contributions in the supersymmetric SM and one-loop contributions from the TeV-scale vectorlike particles. We assume maximal mixings between the stops and between the TeV-scale vectorlike scalars. The numerical results for these five kinds of models are roughly the same. In particular, we showthat the lightest CP-even Higgs boson can have mass up to 146 GeV naturally, which is the current upper bound from the CMS and ATLAS collaborations.
The AGN–Star Formation Connection: Future Prospects with JWST

The bulk of the stellar growth over cosmic time is dominated by IR-luminous galaxies at cosmic noon ( z = 1 – 2 ), many of which harbor a hidden active galactic nucleus (AGN). We use state-of-the-art infrared color diagnostics, combining Spitzer and Herschel observations, to separate dust-obscured AGNs from dusty star-forming galaxies (SFGs) in the CANDELS and COSMOS surveys. We calculate 24 μm counts of SFGs, AGN/star-forming “Composites,” and AGNs. AGNs and Composites dominate the counts above 0.8 mJy at 24 μm, and Composites form at least 25% of an IR sample even to faint detection limits. We develop methods to use the Mid-Infrared Instrument (MIRI) on JWST to identify dust-obscured AGNs and Composite galaxies from z ∼ 1 – 2 . With the sensitivity and spacing of MIRI filters, we will detect >4 times as many AGN hosts as with Spitzer/IRAC criteria. Any star formation rates based on the 7.7 μm PAH feature (likely to be applied to MIRI photometry) must be corrected for the contribution of the AGN, or the star formation rate will be overestimated by ∼35% for cases where the AGN provides half the IR luminosity and ∼50% when the AGN accounts for 90% of the luminosity. Finally, we demonstrate that our MIRI color technique can select AGNs with an Eddington ratio of λ Edd ∼ 0.01 and will identify AGN hosts with a higher specific star formation rate than X-ray techniques alone. JWST/MIRI will enable critical steps forward in identifying and understanding dust-obscured AGNs and the link to their host galaxies.
Conditional probabilities in the excursion set theory: generic barriers and non-Gaussian initial conditions

The excursion set theory, where density perturbations evolve stochastically with the smoothing scale, provides a method for computing the dark matter halo mass function. The computation of the mass function is mapped into the so-called first-passage time problem in the presence of a moving barrier. The excursion set theory is also a powerful formalism to study other properties of dark matter haloes such as halo bias, accretion rate, formation time, merging rate and the formation history of haloes. This is achieved by computing conditional probabilities with non-trivial initial conditions, and the conditional two-barrier first-crossing rate. In this paper we use the path integral formulation of the excursion set theory to calculate analytically these conditional probabilities in the presence of a generic moving barrier, including the one describing the ellipsoidal collapse, and for both Gaussian and non-Gaussian initial conditions. While most of our analysis associated with Gaussian initial conditions assumes Markovianity (top-hat in momentum space smoothing, rather than generic filters), the non-Markovianity of the random walks induced by non-Gaussianity is consistently accounted for. We compute, for a generic barrier, the first two scale-independent halo bias parameters, the conditional mass function and the halo formation time probability, including the effects of non-Gaussianities. We also provide the expression for the two-constant-barrier first-crossing rate when non-Markovian effects are induced by a top-hat filter function in real space.
M0.20–0.033: An Expanding Molecular Shell in the Galactic Center Radio Arc

We present high-frequency Karl G. Jansky Very Large Array (VLA) continuum and spectral line (NH3, H64α, and H63α) observations of the Galactic Center Radio Arc region, covering the Sickle H ii region, the Quintuplet cluster, and molecular clouds M0.20−0.033 and M0.10−0.08. These observations show that the two velocity components of M0.20−0.033 (∼25 and 80 km s−1), previously thought to be separate clouds along the same line-of-sight, are physically connected in position–velocity space via a third southern component around 50 km s−1. Further position–velocity analysis of the surrounding region, using lower-resolution survey observations taken with the Mopra and ATCA telescopes, indicates that both molecular components in M0.20−0.033 are physically connected to the M0.10−0.08 molecular cloud, which is suggested to be located on stream 1 in the Kruijssen et al. orbital model. The morphology and kinematics of the molecular gas in M0.20−0.033 indicate that the two velocity components in M0.20−0.033 constitute an expanding shell. Our observations suggest that the M0.20−0.033 expanding shell has an expansion velocity of 40 km s−1, with a systemic velocity of 53 km s−1, comparable to velocities detected in M0.10−0.08. The origin of the expanding shell is located near the Quintuplet cluster, suggesting that the energy and momentum output from this massive stellar cluster may have contributed to the expansion.
Nancy Cartwright and the Logic of Quantum Mechanics

This paper deals with Nancy Cartwright's views on the measurement problem in Quantum Mechanics, as exposed in her book {\it{How the Laws of Physics Lie}}. She does not accept the logic of Quantum Mechanics. It is argued that her proposals, which are at variance with many facts results and epistemics of Quantum Mechanics are the result of her choice of classical logic, which leads her to propose the transition rate as the fundamental object of Quantum Mechanics. I argue that this is incorrect. The positions which Nancy Cartwright defends on the reduction of the wave packet do not address the fundamental issue, i.e. the duality of a world where quantum and classical objects coexist and interact. I suggest that the main problem with Nancy Cartwright's positions is her difficulty in accepting that the contradiction at the basis of Quantum Mechanics, i.e. the simultaneous corpuscular and wave-like nature of quantum objects, is a fact of nature. Recent experiments, described in this paper, shed a new light on the foundations of Quantum Mechanics and on the topic of this paper. The limits of the no-contradiction principle are discussed; modern dialectical materialism is argued to offer a useful framework for the interplay between knowledge and reality.
Multi-scale energy injection: a new tool to generate intense homogeneous and isotropic turbulence for premixed combustion

Highly turbulent flow, generated by an original multi-scale device and nearly homogeneous and isotropic, is experimentally investigated. This multi-scale device is made of three perforated plates shifted in space such that the diameter of their holes and their blockage ratio increase with the downstream distance. The multi-scale turbulence injection (MuSTI) is compared with a mono-scale turbulence injection (MoSTI), the latter being only constituted of the last plate of the MuSTI. This comparison is done for both cold and reactive flows. For the cold flow the following are shown, in comparison with the classical mono-scale device, for the MuSTI device in the near-field: (i) The turbulent kinetic energy is larger, and the kinetic energy supply is distributed over the whole range of scales. This is emphasised by second- and third-order structure functions. (ii) The shear-stresses are enhanced. (iii) The homogeneity and isotropy are reached earlier (≈50%). (iv) The jet-merging distance is the relevant scalin.
Cosmological large-scale structures beyond linear theory in modified gravity

We consider the effect of modified gravity on the growth of large-scale structures at second order in perturbation theory. We show that modified gravity models changing the linear growth rate of fluctuations are also bound to change, although mildly, the mode coupling amplitude in the density and reduced velocity fields. We present explicit formulae which describe this effect. We then focus on models of modified gravity involving a scalar field coupled to matter, in particular chameleons and dilatons, where it is shown that there exists a transition scale around which the existence of an extra scalar degree of freedom induces significant changes in the coupling properties of the cosmic fields. We obtain the amplitude of this effect for realistic dilaton models at the tree-order level for the bispectrum, finding them to be comparable in amplitude to those obtained in the DGP and f(R) models.
Hyperbolic theory of relativistic conformal dissipative fluids

We develop a complete description of the class of conformal relativistic dissipative fluids of divergence form, following the formalism carried out by Geroch, Lindblom and Pennisi. This type of theories is fully described in terms of evolution variables whose dynamics is governed by total divergence-type conservation laws. Specifically, we give a characterization of the whole family of conformal fluids in terms of a single master scalar function defined up to second order corrections in dissipative effects, which we explicitly find in general form. This allows us to identify the equilibrium states of the theory, as well as to derive constitutive relations and a Fourier-like law for the corresponding first-order theory heat flux. Finally, we show that among this class of theories-- and near equilibrium configurations-- there exist symmetric hyperbolic ones, implying that for them one can define well posed initial value problems.
Anderson localization in tight-binding models with flat bands

We consider the effect of weak disorder on eigenstates in a special class of tight-binding models. Models in this class have short-range hopping on periodic lattices; their defining feature is that the clean systems have some energy bands that are dispersionless throughout the Brillouin zone. We show that states derived from these flat bands are generically critical in the presence of weak disorder, being neither Anderson localised nor spatially extended. Further, we establish a mapping between this localisation problem and the one of resonances in random impedance networks, which previous work has suggested are also critical. Our conclusions are illustrated using numerical results for a two-dimensional lattice, known as the square lattice with crossings or the planar pyrochlore lattice.
Ripple field losses in direct current biased superconductors: Simulations and comparison with measurements

In several superconducting applications, as, for example, in some supercondcuting generators, motors, and power transmission cables, the superconductor experiences a changing magnetic field in a DC background. Simulating the losses caused by this AC ripple field is an important task from the application design point of view. In this work, we compare two formulations, the H-formulation and the minimum magnetic energy variation-formulation, based on the eddy current model (ECM) and the critical state model (CSM), respectively, for simulating ripple field losses in a DC biased coated conductor tape. Furthermore, we compare our simulation results with measurements. We investigate the frequency-dependence of the hysteresis loss predictions of the power law based ECM and verify by measurements, that in DC use, ECM clearly over-estimates the homogenization of the current density profile in the coated conductor tape: the relaxation of the local current density is not nearly as prominent in the measurement as it i.
Assessment of The pretreatment Efficiency with Dexamethasone VS Placebo on Post-operative Pain in teeth with Symptomatic Irreversible Pulpitis

This study aimed to assess the clinical efficiency of administrating one oral preoperative dose of dexamethasone vs placebo on post-operative pain which is a primary outcome demonstrated directly after the root canal treatment procedure, and also respectively after 6, 12, 24, 48 hours in teeth with symptomatic irreversible pulpitis. Methods: Thirty-two adults, with age range of 25-45 years old, complaining from symptomatic irreversible pulpitis were involved in our clinical study. Thorough clinical and radiographic diagnosis was performed, then the candidates were blindly assigned into 2 main equal groups with 16 patient in each group. The procedure of pain levels recording was properly discussed to the patients and they were asker to record the pain levels after applying a thermal pulp test (cold test) before proceeding in the root canal procedure utilizing the Numerical Rate Scale (NRS). Access cavity preparation followed by extirpating all the pulp tissues were performed. Pain records directly after the treatment is completed, then at 6, 12, 24, and 48 hours postoperatively. All demographic data and categorical scores were collected from the patients and statistically analysed. Results: it was shown that there was no statistically significance differences between the 2 main groups regarding pain records obtained pre-operatively, during access cavity preparation, extirpating the pulp tissue, immediate postoperative, after 6, 12, 24 and 48 hours.
Clinical and Prognostic Significance of Baseline Serum Vitamin D Levels in Hospitalized Egyptian Covid-19 Patients

Background and Aim Vitamin D is a hormone with essential roles in both cellular metabolism and immunity. It controls calcium homeostasis and modulates innate and adaptive immune system responses. Many studies suggested an association between vitamin D deficiency and clinical outcomes of covid-19 infection, while others failed to document such a relation. The present study aimed to evaluate the clinical and prognostic significance of baseline vitamin D levels in hospitalized Egyptian covid-19 patients. Patients and Methods The present retrospective study included 300 hospitalized covid-19 patients. Patients were submitted to standard clinical, laboratory, and radiological assessment. According to vitamin D levels, patients were classified to have normal levels (≥30), insufficient levels (20–29) or deficient levels (<20). Results According to their vitamin D levels, patients were classified into those with normal vitamin D (n=135), others with vitamin D insufficiency (n=114), and a third group with vitamin D deficiency (n=51). Patients with normal vitamin D levels and vitamin D insufficiency are significantly younger [median (IQR): 49.0 (39.0–57.0) versus 51.0 (40.0–61.0) and 55.0 (43.0–62.0) years, respectively, p=0.012] and had less frequency of severe disease (24.4% versus 40.4% and 51.0%, respectively) when compared with those with vitamin D deficiency. Moreover, they had significantly lower levels of D dimer [median (IQR): 1.5 (0.9–2.5) versus 1.8 (0.9–3.1) and 2.0 (1.0–3.2)], CRP [median (IQR): 58.0 (30.0–120.0) versus 76.0 (42.5–160.0) and 105.0 (74.0–208.0), respectively, p<0.001], ferritin [median (IQR): 458.0 (240.0–759.0) versus 606.0 (433.8–897.8) and 820.0 (552.0–1087.0), respectively, p<0.001], and procalcitonin [median (IQR): 290.0 (152.0–394.0) versus 372.5 (227.0–530.5) and 443.0 (272.0–575.0), respectively, p<0.001]. Only lower vitamin D levels were significant predictors of mortality in multivariate analysis [OR (95% CI): 0.88 (0.84–0.92), p<0.001]. Conclusion Low vitamin D levels are related to exaggerated inflammatory response, disease severity, and poor clinical outcome in hospitalized covid-19 patients.
Cyg X-3: a low-mass black hole or a neutron star.

Cyg X-3 is a highly interesting accreting X-ray binary, emitting from the radio to high-energy gamma-rays. It consists of a compact object wind-fed by a Wolf-Rayet (WR) star, but the masses of the components and the mass-loss rate have been a subject of controversies. Here, we determine its masses, inclination, and the mass-loss rate using our derived relationship between the mass-loss rate and the mass for WR stars of the WN type, published infrared and X-ray data, and a relation between the mass-loss rate and the binary period derivative (observed to be >0 in Cyg X-3). Our obtained mass-loss rate is almost identical to that from two independent estimates and consistent with other ones, which strongly supports the validity of this solution. The found WR and compact object masses are 10. 3_{-2.8}^{+3.9}, 2. 4_{-1.1}^{+2.1} solar masses, respectively. Thus, our solution still allows for the presence of either a neutron star or a black hole, but the latter only with a low mass. However, the radio, infrared and X-ray properties of the system suggest that the compact object is a black hole. Such a low-mass black-hole could be formed via accretion-induced collapse or directly from a supernova.
New insights into the foreground analysis of the WMAP 5-year data using fastica

In this paper, we present a foreground analysis of the Wilkinson Microwave Anisotropy Probe (WMAP) 5-year data using the fastica algorithm, improving on the treatment of the WMAP 3-year data in Bottino et al. We determine coupling coefficients between the WMAP data and templates commonly used to trace the dominant foreground emissions, and use them to study the spectral properties of the diffuse emissions and subsequently to clean the data. We confirm the dependence of the values of these scaling factors on the extension of the mask used in the analysis and we again demonstrate some anomalies when the Kp0 mask is adopted that remain unexplained. We also revisit the nature of the free–free spectrum with the emphasis on attempting to confirm or otherwise the spectral feature claimed in Dobler et al. and explained in terms of spinning dust emission in the warm ionized medium. With the application of different Galactic cuts, the index is always flatter than the canonical value of 2.14 except for the Kp0 mask which is steeper. Irrespective of this, we cannot confirm the presence of any feature in the free–free spectrum. We experiment with a more extensive approach to the cleaning of the data, introduced in connection with the iterative application of fastica. We confirm the presence of a residual foreground whose spatial distribution is concentrated along the Galactic plane, with pronounced emission near the Galactic Centre. This is consistent with the WMAP haze detected in Finkbeiner et al. Finally, we attempted to perform the same analysis on full-sky (FS) maps. The code returns good results even for those regions where the cross-talk among the components is high. However, slightly better results in terms of the possibility of reconstructing an FS CMB map are achieved with a simultaneous analysis of both the five WMAP maps and foreground templates. None the less, some residuals are still present and detected in terms of an excess in the cosmic microwave background power spectrum, on small angular scales. Therefore, a minimal mask for the brightest regions of the plane is necessary, and has been defined.
Understanding students’ activities in Wi-Fi coffee shops in Aceh: A survey and narrative interview report

This study attempts to investigate and comprehend more in-depth information about students' daily lives in the Wi-Fi coffee shops, specifically in Aceh, a province of Indonesia. The study explores how the wireless Internet in coffee shops relates to college students' activities. The surveys of 619 students were conducted as a preliminary report. An in-depth phenomenological interview was employed to collect data from three university students who regularly spent many waking hours in coffee shops. Findings from the preliminary survey revealed that more male students visited coffee shops than women, with an average time of more than three hours daily. Accessing information through the Internet was not the primary purpose of visiting the coffee shops by most students instead of gaming, meeting up with friends for a chat, and enjoying the coffee. Qualitative interviews reported that students often visited coffee shops for various purposes, including completing homework, meetings with friends, and finding freelance online market jobs. Wi-Fi coffee shops are essential for those who do not have Internet access at home, particularly young people and recent transplants with low incomes but high educational capital. Although the Internet in coffee shops can have both negative and positive effects on students, if users or students can access these facilities rightly, they will acquire many benefits to support their education and future career. However, if misused, it may negatively affect their lives. Suppose the Internet in the coffee shop is used properly for educational purposes. In that case, it will push for greener and healthier information practices for students who may favor low-tech environments or lack personal infrastructure or resources.
Study of Superoutbursts and Superhumps in SU UMa Stars by the Kepler Light Curves of V344Lyrae and V1504 Cygni

We have studied the short-cadence Kepler public light curves of SU UMa stars, V344 Lyr and V1504 Cyg extending over a period of more than two years by using power spectral analysis. We determined the orbital period of V344 Lyr to be Porb=0.087903(1) d. We also reanalyzed the frequency variation of the negative superhump in a complete supercycle of V1504 Cyg with additional data of the O-C diagram, confirming that its characteristic variation is in accordance with the thermal-tidal instability model. We present a new two-dimensional period analysis based on a new method of a least absolute shrinkage and selection operator (Lasso). The new method gives very sharp peaks in the power spectra, and it is very useful for studying of the frequency variation in cataclysmic variable stars. We also analyzed simultaneous frequency variations of the positive and negative superhumps. If they are appropriately converted, it is found that they vary in unison, indicating that they represent a disk-radius variation. We have also studied the frequency (or period) variations of positive superhumps during superoutbursts. These variations can be understood in a qualitative way by combining of the disk radius variation and the variation of pressure effects during a superoutburst. A sudden excitation of oscillation with a frequency range near to the negative superhump (which we call "impulsive negative superhump") was observed in the descending branch of several outbursts of V344 Lyr. These events seem to have occurred just prior to the next superoutburst, and to act as a "lead" of the impending superoutburst.