Miracle-dz/UniFAR-FTUs huggingface dataset:
PROBING MILLISECOND PULSAR EMISSION GEOMETRY USING LIGHT CURVES FROM THE FERMI/LARGE AREA TELESCOPE

An interesting new high-energy pulsar sub-population is emerging following early discoveries of gamma-ray millisecond pulsars (MSPs) by the Fermi Large Area Telescope (LAT). We present results from three-dimensional emission modeling, including the special relativistic effects of aberration and time-of-flight delays and also rotational sweepback of B-field lines, in the geometric context of polar cap (PC), outer gap (OG), and two-pole caustic (TPC) pulsar models. In contrast to the general belief that these very old, rapidly rotating neutron stars (NSs) should have largely pair-starved magnetospheres due to the absence of significant pair production, we find that most of the light curves are best fit by TPC and OG models, which indicates the presence of narrow accelerating gaps limited by robust pair production—even in these pulsars with very low spin-down luminosities. The gamma-ray pulse shapes and relative phase lags with respect to the radio pulses point to high-altitude emission being dominant for all geometries. We also find exclusive differentiation of the current gamma-ray MSP population into two MSP sub-classes: light curve shapes and lags across wavebands impose either pair-starved PC (PSPC) or TPC/OG-type geometries. In the first case, the radio pulse has a small lag with respect to the single gamma-ray pulse, while the (first) gamma-ray peak usually trails the radio by a large phase offset in the latter case. Finally, we find that the flux correction factor as a function of magnetic inclination and observer angles is typically of order unity for all models. Our calculation of light curves and flux correction factor for the case of MSPs is therefore complementary to the “ATLAS paper” of Watters et al. for younger pulsars.
Measurement of $T_{\rm CMB}$ evolution from Sunyaev-Zel'dovich effect

In the standard hot cosmological model, the black-body temperature of the Cosmic Microwave Background (CMB), $T_{\rm CMB}$, increases linearly with redshift. Across the line of sight CMB photons interact with the hot ($\sim10^{7-8}$ K) and diffuse gas of electrons from galaxy clusters. This interaction leads to the well known thermal Sunyaev-Zel'dovich effect (tSZ), which produces a distortion of the black-body emission law, depending on $T_{\rm CMB}$. Using tSZ data from the ${\it Planck}$ satellite it is possible to constrain $T_{\rm CMB}$ below z=1. Focusing on the redshift dependance of $T_{\rm CMB}$ we obtain $T_{\rm CMB}(z)=(2.726\pm0.001)\times (1+z)^{1-\beta}$ K with $\beta=0.009\pm0.017$, improving previous constraints. Combined with measurements of molecular species absorptions, we derive $\beta=0.006\pm0.013$. These constraints are consistent with the standard (i.e. adiabatic, $\beta=0$) Big-Bang model.
Cosmic ray electron and positron excesses from a fourth generation heavy Majorana neutrino

Unexpected features in the energy spectra of cosmic rays electrons and positrons have been recently observed by PAMELA and Fermi-LAT satellite experiments, opening to the exciting possibility of an indirect manifestation of new physics. A TeV-scale fourth lepton family is a natural extension of the Standard Model leptonic sector (also linked to the hierarchy problem in Minimal Walking Technicolor models). The heavy Majorana neutrino of this setup mixes with Standard Model charged leptons through a weak charged current interaction. Here, we first study analytically the energy spectrum of the electrons and positrons originated in the heavy Majorana neutrino decay modes, also including polarization effects. We then compare the prediction of this model with the experimental data, exploiting both the standard direct method and our recently proposed Sum Rules method. We find that the decay modes involving the tau and/or the muon charged leptons as primary decay products fit well the PAMELA and Fermi-LAT lepton excesses while there is tension with respect to the antiproton to proton fraction constrained by PAMELA.
γ-ray emission region located in the parsec scale jet of OJ287

We report on the location of the γ-ray emission region in flares of the BL Lacertae object OJ287 at > 14 pc from the central supermassive black hole. We employ data from multi-spectral range (total flux and linear polarization) monitoring programs combined with sequences of ultra-high-resolution 7 mm VLBA images. The correlation between the brightest γ-ray and mm flares is found to be statistically significant. The two γ-ray peaks, detected by Fermi-LAT, that we report here happened at the rising phase of two exceptionally bright mm flares accompanied by sharp linear polarization peaks. The VLBA images show that these mm flares in total flux and polarization degree occurred in a jet region at > 14 pc from the innermost jet region. The time coincidence of the brighter γ-ray flare and its corresponding mm linear polarization peak evidences that both the γ-ray and mm outbursts occur > 14 pc from the central black hole. We find two sharp optical flares occurring at the peak times of the two reported γ-ray flares. This is interpreted as the γ-ray flares being produced by synchrotron self-Compton scattering of optical photons from the flares triggered by the interaction of moving knots with a stationary conical shock in the jet.
Using the XMM-Newton Optical Monitor to Study Cluster Galaxy Evolution

We explore the application of XMM-Newton Optical Monitor (XMM-OM) ultraviolet (UV) data to study galaxy evolution. Our sample is constructed as the intersection of all Abell clusters with z < 0.05 and having archival XMM-OM data in either the UVM2 or UVW1 filters, plus optical and UV photometry from the Sloan Digital Sky Survey and GALEX, respectively. The 11 resulting clusters include 726 galaxies with measured redshifts, 520 of which have redshifts placing them within their parent Abell clusters. We develop procedures for manipulating the XMM-OM images and measuring galaxy photometry from them, and we confirm our results via comparison with published catalogs. Color-magnitude diagrams (CMDs) constructed using the XMM-OM data along with SDSS optical data show promise for evolutionary studies, with good separation between red and blue sequences and real variation in the width of the red sequence that is likely indicative of differences in star formation history. This is particularly true for UVW1 data, as the relative abundance of data collected using this filter and its depth make it an attractive choice. Available tools that use stellar synthesis libraries to fit the UV and optical photometric data may also be used, thereby better describing star formation history within the past billion years and providing estimates of total stellar mass that include contributions from young stars. Finally, color-color diagrams that include XMM-OM UV data appear useful to the photometric identification of both extragalactic and stellar sources.
Creation of a Functional Cotton Headcover (turban/bonnet) via Lac and Turmeric Natural dyes

: Functional textiles and clothes have attracted increasing attention in recent years. Apparel possessing antibacterial and antioxidant functions can offer health care effects. Cotton head covers with antioxidant and antibacterial functional properties were created by using a sustainable approach in the current study. The sustainability was applied through using microwave dyeing for knitted cotton fabric with lac and turmeric natural dyes as well as chitosan bio- mordanting. The microwave dyeing was optimized by studying the dyeing time (3-11 min), the microwave power (100 - 900 W), salt concentration (0-10 %) for both lac and turmeric dyes, and the pH of the dyeing bath (2-6) for lac dye and (4-8) for turmeric dye. The deposition of chitosan on cotton fabric was confirmed by scanning electron microscopy for the cotton surface. The color strength of cotton fabric reached 11 and 8.3 for lac and turmeric dyes, respectively with no salt dyeing after chitosan treatment. This result was obtained at 450 W, 7 min, and pH 3 for lac dye and 100 W, 3 min, and pH 7 for turmeric dye. both perspiration and washing fastness (the staining on cotton) properties of lac dyed cotton fabrics were enhanced in the case of chitosan treatment. But in the case of turmeric dye, the fastness properties to wash and light were improved after chitosan treatment. The functional properties of antioxidant and antibacterial were evaluated for both lac and turmeric dyed cotton fabric. The antioxidant activity for turmeric and lac dyed cotton fabrics reached 61.25% and 11% respectively. The antibacterial activity against three strains of bacteria (Bacillus cereus, Staphylococcus aureus, and Escherichia coli) was evaluated using the turbidity method and both lac and turmeric dyes showed antibacterial activity.
CONNECTING THE DOTS: TRACKING GALAXY EVOLUTION USING CONSTANT CUMULATIVE NUMBER DENSITY AT 3 ≤ z ≤ 7

Using the cosmological smoothed particle hydrodynamical code GADGET-3, we make a realistic assessment of the technique of using constant cumulative number density as a tracer of galaxy evolution at high redshift. We find that over a redshift range of 3 ≤ z ≤ 7 one can on average track the growth of the stellar mass of a population of galaxies selected from the same cumulative number density bin to within ∼0.20 dex. Over the stellar mass range that we probe ( 10 10.4 ≤ M s / M ⊙ ≤ 10 10.8 ? > at z = 3 and 10 8.5 ≤ M s / M ⊙ ≤ 10 9.6 ? > at z = 7), one can reduce this bias by selecting galaxies based on an evolving cumulative number density. We find that this cumulative number density evolution exhibits a trend toward higher values which can be quantified by simple linear formulations of −0.10Δz for descendants and 0. 12Δz for progenitors. Utilizing such an evolving cumulative number density increases the accuracy of descendant/progenitor tracking by a factor of ∼2. This result is in excellent agreement, within 0.10 dex, with abundance matching results over the same redshift range. However, we find that our more physically realistic cosmological hydrodynamic simulations produce a much larger scatter in descendant/progenitor stellar masses than previous studies, particularly when tracking progenitors. This large scatter makes the application of either the constant cumulative number density or evolving cumulative number density technique limited to average stellar masses of populations only, as the diverse mass assembly histories caused by stochastic physical processes such as gas accretion or mergers lead to an even larger scatter in other physical properties such as metallicity and star formation rate.
AN IN-DEPTH STUDY OF GRID-BASED ASTEROSEISMIC ANALYSIS

NASA's Kepler mission is providing basic asteroseismic data for hundreds of stars. One of the more common ways of determining stellar characteristics from these data is by the so-called grid-based modeling. We have made a detailed study of grid-based analysis techniques to study the errors (and error correlations) involved. As had been reported earlier, we find that it is relatively easy to get very precise values of stellar radii using grid-based techniques. However, we find that there are small, but significant, biases that can result because of the grid of models used. The biases can be minimized if metallicity is known. Masses cannot be determined as precisely as the radii and suffer from larger systematic effects. We also find that the errors in mass and radius are correlated. A positive consequence of this correlation is that log g can be determined both precisely and accurately with almost no systematic biases. Radii and log g can be determined with almost no model dependence to within 5% for realistic estimates of errors in asteroseismic and conventional observations. Errors in mass can be somewhat higher unless accurate metallicity estimates are available. Age estimates of individual stars are the most model dependent. The errors are larger, too. However, we find that for star clusters, it is possible to get a relatively precise age if one assumes that all stars in a given cluster have the same age.
Searching for transit timing variations in transiting exoplanet systems

Abstract Searching for transit timing variations in the known transiting exoplanet systems can reveal the presence of other bodies in the system. Here we report such searches for two transiting exoplanet systems, TrES-1 and WASP-2. Their new transits were observed with the 4.2m William Herschel Telescope located on La Palma, Spain. In a continuing programme, three consecutive transits were observed for TrES-1, and one for WASP-2 during September 2007. We used the Markov Chain Monte Carlo simulations to derive transit times and their uncertainties. The resulting transit times are consistent with the most recent ephemerides and no conclusive proof of additional bodies in either system was found.
THE BALMER-DOMINATED BOW SHOCK AND WIND NEBULA STRUCTURE OF γ-RAY PULSAR PSR J1741−2054

We have detected an Hα bow shock nebula around PSR J1741−2054, a pulsar discovered through its GeV γ-ray pulsations. The pulsar is only ∼1. ″5 behind the leading edge of the shock. Optical spectroscopy shows that the nebula is non-radiative, dominated by Balmer emission. The Hα images and spectra suggest that the pulsar wind momentum is equatorially concentrated and implies a pulsar space velocity ≈150 km s−1, directed 15° ± 10° out of the plane of the sky. The complex Hα profile indicates that different portions of the post-shock flow dominate line emission as gas moves along the nebula and provide an opportunity to study the structure of this unusual slow non-radiative shock under a variety of conditions. CXO ACIS observations reveal an X-ray pulsar wind nebula within this nebula, with a compact ∼2. ″5 equatorial structure and a trail extending several arcminutes behind. Together these data support a close (⩽0.5 kpc) distance, a spin geometry viewed edge-on, and highly efficient γ-ray production for this unusual, energetic pulsar.
A Study of Differential Resting-State Brain Functional Activity in Males and Females with Recurrent Depressive Disorder

In this study, we observed the sex differences in functional brain activity in patients with recurrent depressive disorder (RDE) and assessed the correlation between abnormal functional brain activity changes and clinical symptoms. A total of 40 patients with RDE (19 male and 21 female) and 42 healthy controls (HCs) (20 male and 22 female) met the inclusion criteria. Analysis of images using regional homogeneity (ReHo) and further analysis of the correlation between abnormal brain areas and clinical symptoms of the different sexes with RDE groups were carried out. For the main effects of sex (male vs. female), there were statistically significant differences in ReHo among the four groups in the right middle temporal gyrus, right thalamus, and left posterior cerebellar lobe. For the effects of the sex-by-group interaction, there were statistically significant differences in ReHo among the four groups in the left middle frontal gyrus, left precentral gyrus, and right insula. Post hoc analyses showed that compared with the female RDE group, the male RDE group had decreased ReHo in the left middle frontal gyrus and right insula. In the female RDE group, the ReHo values of the left middle frontal gyrus were positively correlated with the 17-item Hamilton Rating Scale for Depression (HAMD-17) scores. This study provides new insights into the clinical targeting of different sexes for RDE.
A search for radius inflation among active M-dwarfs in Praesepe

Rotation periods from Kepler K2 are combined with projected rotation velocities from the WIYN 3.5-m telescope, to determine projected radii for fast-rotating, low-mass ($0.15 \leq M/M_{\odot} \leq 0.6$) members of the Praesepe cluster. A maximum likelihood analysis that accounts for observational uncertainties, binarity and censored data, yields marginal evidence for radius inflation -- the average radius of these stars is $6\pm4$ per cent larger at a given luminosity than predicted by commonly-used evolutionary models. This over-radius is smaller (at 2-sigma confidence) than was found for similar stars in the younger Pleiades using a similar analysis; any decline appears due to changes occurring in higher mass ($>0.25 M_{\odot}$) stars. Models incorporating magnetic inhibition of convection predict an over-radius, but do not reproduce this mass dependence unless super-equipartition surface magnetic fields are present at lower masses. Models incorporating flux-blocking by starspots can explain the mass dependence but there is no evidence that spot coverage diminishes between the Pleiades and Praesepe samples to accompany the decline in over-radius. The fastest rotating stars in both Praesepe and the Pleiades are significantly smaller than the slowest rotators for which a projected radius can be measured. This may be a selection effect caused by more efficient angular momentum loss in larger stars leading to their progressive exclusion from the analysed samples. Our analyses assume random spin-axis orientations; any alignment in Praesepe, as suggested by Kovacs (2018), is strongly disfavoured by the broad distribution of projected radii.
Improved measurements of turbulence in the hot gaseous atmospheres of nearby giant elliptical galaxies

We present significantly improved measurements of turbulent velocities in the hot gaseous haloes of nearby giant elliptical galaxies. Using deep XMM-Newton Reflection Grating Spectrometer (RGS) observations and a combination of resonance scattering and direct line broadening methods, we obtain well bounded constraints for 13 galaxies. Assuming that the turbulence is isotropic, we obtain a best-fitting mean 1D turbulent velocity of similar to 110 km s(-1). This implies a typical 3D Mach number similar to 0.45 and a typical non-thermal pressure contribution of similar to 6 per cent in the cores of nearby massive galaxies. The intrinsic scatter around these values is modest-consistent with zero, albeit with large statistical uncertainty-hinting at a common and quasi-continuous mechanism sourcing the velocity structure in these objects. Using conservative estimates of the spatial scales associated with the observed turbulent motions, we find that turbulent heating can be sufficient to offset radiative cooling in the inner regions of these galaxies (< 10 kpc, typically 2-3 kpc). The full potential of our analysis methods will be enabled by future X-ray micro-calorimeter observations.
The Electromagnetic Green's Function for Layered Topological Insulators

The dyadic Green's function of the inhomogeneous vector Helmholtz equation describes the field pattern of a single frequency point source. It appears in the mathematical description of many areas of electromagnetism and optics including both classical and quantum, linear and nonlinear optics, dispersion forces (such as the Casimir and Casimir-Polder forces), and in the dynamics of trapped atoms and molecules. Here we compute the Green's function for a layered topological insulator. Via the magnetoelectric effect, topological insulators are able to mix the electric $\mathbf{E}$ and magnetic induction $\mathbf{B}$ fields and, hence, one finds that the TE and TM polarizations mix on reflection from or transmission through an interface. This leads to unusual field patterns close to the surface of a topological insulator.
Mid-infrared multi-wavelength imaging of Ophiuchus IRS 48 transitional disk

Transitional disks around the Herbig Ae/Be stars are fascinating targets in the contexts of disk evolution and also planet formation. Oph IRS 48 is one of such Herbig Ae stars, which shows an inner dust cavity and azimuthally lopsided large dust distribution. We present new images of Oph IRS 48 at eight mid-infrared (MIR) wavelengths from 8.59 to 24.6\,$\mu {\rm m}$ taken with the COMICS mounted on the 8.2\,m Subaru Telescope. The N-band (7 to 13\,$\mu {\rm m}$) images show that the flux distribution is centrally peaked with a slight spatial extent, while the Q-band (17 to 25\,$\mu {\rm m}$) images show asymmetric double peaks (east and west). Using 18.8 and 24.6\,$\mu$m images, we derived the dust temperature at both east and west peaks to be 135$\pm$22 K. Thus, the asymmetry may not be attributed to a difference in the temperature. % thus other reason is necessary to explain the asymmetry of east and west peaks in Q-band. Comparing our results with previous modeling works, we conclude that the inner disk is aligned to the outer disk. A shadow casted by the optically thick inner disk has a great influence on the morphology of MIR thermal emission from the outer disk.
A two-phase mixing layer between parallel gas and liquid streams: multiphase turbulence statistics and influence of interfacial instability

The two-phase mixing layer formed between parallel gas and liquid streams is an important fundamental problem in turbulent multiphase flows. The problem is relevant to many industrial applications and natural phenomena, such as air-blast atomizers in fuel injection systems and breaking waves in the ocean. The velocity difference between the gas and liquid streams triggers an interfacial instability which can be convective or absolute depending on the stream properties and injection parameters. In the present study, a direct numerical simulation of a two-phase gas–liquid mixing layer that lie in the absolute instability regime is conducted. A dominant frequency is observed in the simulation and the numerical result agrees well with the prediction from viscous stability theory. As the interfacial wave plays a critical role in turbulence transition and development, the temporal evolution of turbulent fluctuations (such as the enstrophy) also exhibits a similar frequency. To investigate the statistical response of the multiphase turbulence flow, the simulation has been run for a long physical time so that time-averaging can be performed to yield the statistically converged results for Reynolds stresses and the turbulent kinetic energy (TKE) budget. An extensive mesh refinement study using from 8 million to about 4 billions cells has been performed. The turbulent dissipation is shown to be highly demanding on mesh resolution compared with other terms in TKE budget. The results obtained with the finest mesh are shown to be close to converged results of turbulent dissipation which allow us to obtain estimations of the Kolmogorov and Hinze scales. The estimated Kolmogorov scale is found to be similar to the cell size of the finest mesh used here. The computed Hinze scale is significantly larger than the size of droplets observed and does not seem to be a relevant length scale to describe the smallest size of droplets formed in atomization.
Harmonic decomposition of three-particle azimuthal correlations at RHIC

We present measurements of three-particle correlations for various harmonics in Au+Au collisions at energies ranging from $\sqrt{s_{{\rm NN}}}=7.7$ to 200 GeV using the STAR detector. The quantity $\langle\cos(m\phi_1+n\phi_2-(m+n)\phi_3)\rangle$ is evaluated as a function of $\sqrt{s_{{\rm NN}}}$, collision centrality, transverse momentum, $p_T$, pseudo-rapidity difference, $\Delta\eta$, and harmonics ($m$ and $n$). These data provide detailed information on global event properties like the three-dimensional structure of the initial overlap region, the expansion dynamics of the matter produced in the collisions, and the transport properties of the medium. A strong dependence on $\Delta\eta$ is observed for most harmonic combinations consistent with breaking of longitudinal boost invariance. Data reveal changes with energy in the two-particle correlation functions relative to the second-harmonic event-plane and provide ways to constrain models of heavy-ion collisions over a wide range of collision energies.