Miracle-dz/UniFAR-FTUs huggingface dataset:
Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). II. Discovery of 32 quasars and luminous galaxies at 5.7 < z ≤ 6.8

We present spectroscopic identification of 32 new quasars and luminous galaxies discovered at 5.7<z<6.8. This is the second in a series of papers presenting the results of the Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs) project, which exploits the deep multi-band imaging data produced by the Hyper Suprime-Cam (HSC) Subaru Strategic Program survey. The photometric candidates were selected by a Bayesian probabilistic algorithm, and then observed with spectrographs on the Gran Telescopio Canarias and the Subaru Telescope. Combined with the sample presented in the previous paper, we have now identified 64 HSC sources over about 430 deg2, which include 33 high-z quasars, 14 high-z luminous galaxies, 2 [O III] emitters at z ~ 0.8, and 15 Galactic brown dwarfs. The new quasars have considerably lower luminosity (M1450 ~ -25 to -22 mag) than most of the previously known high-z quasars. Several of these quasars have luminous (>10^(43) erg/s) and narrow (<500 km/s) Ly alpha lines, and also a possible mini broad absorption line system of N V 1240 in the composite spectrum, which clearly separate them from typical quasars. On the other hand, the high-z galaxies have extremely high luminosity (M1450 ~ -24 to -22 mag) compared to other galaxies found at similar redshift. With the discovery of these new classes of objects, we are opening up new parameter spaces in the high-z Universe. Further survey observations and follow-up studies of the identified objects, including the construction of the quasar luminosity function at z ~ 6, are ongoing.
of Animal Science and Technology) Insect peptide CopA3 promotes proliferation and PAX7 and expression in porcine muscle satellite cells promotes proliferation of satellite cells.

Insects are a valuable natural source that can produce a variety of bioactive compounds due to their increasing 11 species diversity. CopA3 is an antimicrobial peptide derived from Copris tripartitus (i.e., the dung beetle). It is known to increase the proliferation of colonic epithelial and neuronal stem cells by regulating cell cycle. This 13 research hypothesized that CopA3 can promote the proliferation of porcine muscle satellite cells (MSCs). The 14 effects of CopA3 on porcine MSCs, which are important for muscle growth and regeneration, remain unclear. Here, we investigated the effects of CopA3 on porcine MSCs. According to viability results, we designed four 16 groups: control (without CopA3) and three treatment groups (treated with 5,10, and 25 μg/mL of CopA3). At a 17 CopA3 concentration of 5 μg/mL and 10 μg/mL, the proliferation of MSCs increased more than that observed in 18 the control group. Furthermore, compared to that in the control, CopA3 treatment increased the S phase but 19 decreased the G0/G1 phase ratio. Additionally, early and late apoptotic cells were found to be decreased in the 5 20 μg/mL group. The expressions of the myogenesis-related transcription factor PAX7 and MYOD proteins were 21 significantly upregulated in the 5 μg/mL and 10 μg/mL groups, whereas the MYOG protein remained undetected 22 in all group. This study suggested that CopA3 promotes muscle cell proliferation by regulating the cell cycle of 23 MSCs and can regulate the activity of MSCs by increasing the expressions of PAX7 and MYOD. ×g, supernatant lysates protein assay kit electrophoresed 12% acrylamide polyvinylidene fluoride (PVDF) showed that the addition of CopA3 to a growth medium at concentrations of 5 and 10 μg/mL increased both cell viability and the proliferation rate of MSCs. These results were similar to those of a previous study reporting the increased proliferation and cell viability of mouse neuronal stem cells [28] and human colonic epithelial cells [29] following 10 and 20 μg/mL treatment respectively. Some studies have reported that CopA3 selectively reduces the survival rate of cancer cell lines [10, 27]; for example, when CopA3 was treated with 25 μg/mL in gastric cancer cells, cell viability decreased, and the proportion of necrosis and apoptosis increased [10]. In this study, treatment with 5 μg/mL CopA3 decreased the ratio of early and late apoptotic cells, and the addition of 25 μg/mL CopA3 did not increase the number of apoptotic cells. This could be due to the cell type-specific effects of CopA3.
Hybridation par méthode de décomposition de bord appliquée à l'étude des ondes acoustiques et électromagnétiques : résultats théoriques et numériques

On propose, dans ce document, une methode iterative, appelee methode de decomposition de bord, adaptee a la resolution de l'equation de helmholtz et du systeme d'equations de maxwell dans le complementaire d'un obstacle constitue d'une reunion de composantes disjointes. En faisant l'hypothese que la distance separant les composantes est minoree par une quantite dependant exponentiellement du nombre d'onde, on prouve la convergence de l'algorithme dans le cas de l'equation de helmholtz avec condition aux limites de type dirichlet. On montre que cette hypothese peut etre assouplie lorsque toutes les composantes ont la propriete d'etre etoilees. Encourage par la qualite des resultats numeriques observee pour des configurations n'entrant pas dans le cadre de la preuve precedente, on propose une extension, non demontree, de cette methode a la resolution de l'equation de helmholtz et du systeme d'equations de maxwell dans le complementaire d'une reunion de composantes jointives. Les caracteristiques de la methode de decomposition de bord en font un outil adapte a la realisation de calculs d'hybridation couplant methodes integrale et asymptotique. L'introduction de cette technique dans le domaine de la simulation numerique de phenomenes electromagnetiques permet d'ameliorer significativement la resolution des problemes multi-echelles.
Gradient of the Casimir force between Au surfaces of a sphere and a plate measured using an atomic force microscope in a frequency-shift technique

We present measurement results for the gradient of the Casimir force between an Au-coated sphere and an Au-coated plate obtained by means of an atomic force microscope operated in a frequency shift technique. This experiment was performed at a pressure of 3x10^{-8} Torr with hollow glass sphere of 41.3 mcm radius. Special attention is paid to electrostatic calibrations including the problem of electrostatic patches. All calibration parameters are shown to be separation-independent after the corrections for mechanical drift are included. The gradient of the Casimir force was measured in two ways with applied compensating voltage to the plate and with different applied voltages and subsequent subtraction of electric forces. The obtained mean gradients are shown to be in mutual agreement and in agreement with previous experiments performed using a micromachined oscillator. The obtained data are compared with theoretical predictions of the Lifshitz theory including corrections beyond the proximity force approximation. An independent comparison with no fitting parameters demonstrated that the Drude model approach is excluded by the data at a 67% confidence level over the separation region from 235 to 420 nm. The theoretical approach using the generalized plasma-like model is shown to be consistent with the data over the entire measurement range. Corrections due to the nonlinearity of oscillator are calculated and the application region of the linear regime is determined. A conclusion is made that the results of several performed experiments call for a thorough analysis of the basics of the theory of dispersion forces.
Effect of richness on AGN and star formation activities in SDSS galaxy groups

Based on a large sample of 254 220 galaxies in 81 089 groups, which are selected from the spectroscopic galaxy sample of the SDSS DR12, we investigate the radial distribution of incidences, morphologies, environmental densities, and star formation properties of the active galactic nucleus (AGN) host galaxies and star-forming galaxies (SFGs) in the groups at z 10.7$) galaxies, and the mean SFG fraction is about 6 times as that of AGNs in the late-type galaxies with lower masses at larger radius. The distribution of environmental luminosity densities shows that the AGNs are likely to be reside in a denser environment relative to the SFGs. Compared with the SFGs in groups, the group AGNs are found to have a higher mean stellar mass, a lower mean star formation rate, and an older mean stellar age.
A NEW CEPHEID DISTANCE MEASUREMENT AND METHOD FOR NGC 6822

We present a revised distance to the nearby galaxy NGC 6822 using a new multi-band fit to both previously published and new optical, near-, and mid-infrared data for Cepheid variables. The new data presented in this study include multi-epoch observations obtained in 3.6 μm and 4.5 μm with the Spitzer Space Telescope taken for the Carnegie Hubble Program. We also present new observations in J, H, and Ks with FourStar on the Magellan Baade Telescope at Las Campanas Observatory. We determine mean magnitudes and present new period–luminosity relations in V, I, J, H, Ks, Infrared Array Camera 3.6 μm, and 4.5 μm. In addition to using the multi-band distance moduli to calculate extinction and a true distance, we present a new method for determining an extinction-corrected distance modulus from multi-band data with varying sample sizes. We combine the distance moduli and extinction for individual stars to determine E(B − V) = 0.35 ± 0.04 and a true distance modulus μo = 23.38 ± 0.02stat ± 0.04sys.
Multiphysics CFD modelling of incompressible flows at Low and Moderate Reynolds Numbers

In this Ph.D. thesis, a novel high-resolution Godunov-type numerical procedure has been developed for solving the unsteady, incompressible Navier-Stokes equations for constant and variable density flows. The proposed FSAC-PP approach encompasses both artificial compressibility (AC) and fractional step (FS) pressure-projection (PP) methods of Chorin [3, 4] in a unified solution concept. To take advantage of different computational strategies, the FS and AC methods have been coupled (FSAC formulation), and further a PP step has been employed at each pseudo-time step. To provide time-accurate solutions, the dual-time stepping procedure is utilized. Taking the advantage of the hyperbolic nature of the inviscid part of the AC formulation, high-resolution characteristics-based (CB) Godunov-type scheme is employed to discretize the non-linear advective fluxes. Highorder of accuracy is achieved by using from firstup to ninth-order interpolation schemes. Time integration is obtained from a fourth-order Runge-Kutta scheme. A non-linear fullmultigrid, full-approximation storage (FMG-FAS) acceleration technique has been further extended to the FSAC-PP solution method to increase the efficiency and decrease the computational cost of the developed method and simulations. The AC method has major value for solving stationary flow problems, but for unsteady and/or low Reynolds number flows, the stability condition of the dual-time stepping procedure and the choice of the AC parameter may become too restrictive, which could lead to slow convergence rates [5]. To overcome this problem of stiffness, the key motivation for developing the FSAC-PP method is to improve the stability, efficiency and decrease the computational cost of the classical AC method at both (very) low and moderate Reynolds numbers. Most of the mircofluidic industrial applications under the continuum hypothesis are complex multiphysics problems occurring at low Reynolds numbers. In these cases, the typical Reynolds number is from 10−1 up to 102 [6], where the classical AC method could fail. Therefore, the main goal of this thesis is to develop, analyse and validate a new efficient high-resolution method based software package for modelling multiphysics problems. The proposed FSAC-PP solver based software tool, called HIRECOM-MULTIPHYSICS Unified Code v1.0, might be a bridge between the market leader packages and the daily engineering demand in the design of microfluidic devices. Numerical validation test cases and examples have been presented in this thesis. In
Thermal condensation in a turbulent atomic hydrogen flow

We present a numerical and analytical study of the thermal fragmentation of a turbulent flow of interstellar hydrogen. We first present the different dynamical processes and the large range of spatial (and temporal) scales that need to be adequately represented in numerical simulations. Next, we present bidimensional simulations of turbulent converging flows which induce the dynamical condensation of the warm neutral phase into the cold phase. We then analyse the cold structures and the fraction of unstable gas in each simulation, paying particular attention to the influence of the degree of turbulence. When the flow is very turbulent a large fraction of the gas remains in the thermally unstable domain. This unstable gas forms a filamentary network. We show that the fraction of thermally unstable gas is strongly correlated with the level of turbulence of the flow. We then develop a semi-analytical model to explain the origin of this unstable gas. This simple model is able to quantitatively reproduce the fraction of unstable gas observed in the simulations and its correlation with turbulence. Finally, we stress the fact that even when the flow is very turbulent and in spite of the fact that a large fraction of the gas is maintained dynamically in the thermally unstable domain, the classical picture of a 2-phase medium with stiff thermal fronts and local pressure equilibrium turns out to be still relevant in the vicinity of the cold structures.
Morphological Classification of Galaxies Using Photometric Parameters: The Concentration Index versus the Coarseness Parameter

We devise improved photometric parameters for the morphological classification of galaxies using a bright sample from the First Data Release of the Sloan Digital Sky Survey. In addition to using an elliptical aperture concentration index for classification, we introduce a new texture parameter, coarseness, which quantifies deviations from smooth galaxy isophotes. The elliptical aperture concentration index produces morphological classifications that are in appreciably better agreement with visual classifications than those based on circular apertures. With the addition of the coarseness parameter, the success rate of classifying galaxies into early and late types increases to ≃88% with respect to the reference visual classification. A reasonably high success rate (≃68%) is also attained in classifying galaxies into three types, early-type galaxies (E+S0) and early-type (Sa+Sb) and late-type (Sc+Sdm+Im) spiral galaxies.
Determining the local dark matter density with LAMOST data

Measurement of the local dark matter density plays an important role in both Galactic dynamics and dark matter direct detection experiments. However, the estimated values from previous works are far from agreeing with each other. In this work, we provide a well-defined observed sample with 1427 G \& K type main-sequence stars from the LAMOST spectroscopic survey, taking into account selection effects, volume completeness, and the stellar populations. We apply a vertical Jeans equation method containing a single exponential stellar disk, a razor thin gas disk, and a constant dark matter density distribution to the sample, and obtain a total surface mass density of $\rm {78.7 ^{+3.9}_{-4.7}\ M_{\odot}\ pc^{-2}}$ up to 1 kpc and a local dark matter density of $0.0159^{+0.0047}_{-0.0057}\,\rm M_{\odot}\,\rm pc^{-3}$. We find that the sampling density (i.e. number of stars per unit volume) of the spectroscopic data contributes to about two-thirds of the uncertainty in the estimated values. We discuss the effect of the tilt term in the Jeans equation and find it has little impact on our measurement. Other issues, such as a non-equilibrium component due to perturbations and contamination by the thick disk population, are also discussed.
The Interrelationship Between N-policy M/G/1/K and F-policy G/M/1/K Queues with Startup Time

Abstract This paper studies the interrelationship between the N-policy M/G/1/K queue and the F-policy G/M/1/K queue. The N- policy queuing problem investigates the most common issue of controlling service. The F- policy queuing problem deals with the most common issue of controlling arrivals. We provide a recursive method, using the supplementary variable technique and treating the supplementary variable as the remaining service time, to develop the solution algorithm for the N- policy M/G/1/K queue with startup time. We have demonstrated that the N-policy M/G/1/K queue with startup time has been effectively used to derive the solution algorithm to the F- policy G/M/1/K queue with startup time. The interrelationship between the N- policy and the F — policy queueing problems are illustrated analytically for 3-stage Erlang (service or interarrival) time distribution.
Hubble Space Telescope Trigonometric Parallax of Polaris B, Companion of the Nearest Cepheid

Polaris, the nearest and brightest Cepheid, is a potential anchor point for the Leavitt period–luminosity relation. However, its distance is a matter of contention, with recent advocacy for a parallax of ∼10 mas, in contrast with the Hipparcos measurement of 7.54 ± 0.11 mas. We report an independent trigonometric parallax determination, using the Fine Guidance Sensors (FGS) on the Hubble Space Telescope. Polaris itself is too bright for FGS, so we measured its eighth-magnitude companion Polaris B, relative to a network of background reference stars. We converted the FGS relative parallax to absolute, using estimated distances to the reference stars from ground-based photometry and spectral classification. Our result, 6.26 ± 0.24 mas, is even smaller than that found by Hipparcos. We note other objects for which Hipparcos appears to have overestimated parallaxes, including the well-established case of the Pleiades. We consider possible sources of systematic error in the FGS parallax, but find no evidence they are significant. If our “long” distance is correct, the high luminosity of Polaris indicates that it is pulsating in the second overtone of its fundamental mode. Our results raise several puzzles, including a long pulsation period for Polaris compared to second-overtone pulsators in the Magellanic Clouds, and a conflict between the isochrone age of Polaris B (∼2.1 Gyr) and the much younger age of Polaris A. We discuss possibilities that B is not a physical companion of A, in spite of the strong evidence that it is, or that one of the stars is a merger remnant. These issues may be resolved when Gaia provides parallaxes for both stars.
Dark soliton states of Bose-Einstein condensates in anisotropic traps,

Dark soliton states of Bose-Einstein condensates in harmonic traps are studied both analytically and computationally by the direct solution of the Gross-Pitaevskii equation in three dimensions. The ground and self-consistent excited states are found numerically by relaxation in imaginary time. The energy of a stationary soliton in a harmonic trap is shown to be independent of density and geometry for large numbers of atoms. Large-amplitude field modulation at a frequency resonant with the energy of a dark soliton is found to give rise to a state with multiple vortices. The Bogoliubov excitation spectrum of the soliton state contains complex frequencies, which disappear for sufficiently small numbers of atoms or large transverse confinement. The relationship between these complex modes and the snake instability is investigated numerically by propagation in real time.
COSMIC EVOLUTION OF SIZE AND VELOCITY DISPERSION FOR EARLY-TYPE GALAXIES

Massive (stellar mass M⋆ ≳ 3 × 1010 M☉), passively evolving galaxies at redshifts z ≳ 1 exhibit on average physical sizes smaller, by factors ≈3, than local early-type galaxies (ETGs) endowed with the same stellar mass. Small sizes are in fact expected on theoretical grounds, if dissipative collapse occurs. Recent results show that the size evolution at z ≲ 1 is limited to less than 40%, while most of the evolution occurs at z ≳ 1, where both compact and already extended galaxies are observed and the scatter in size is remarkably larger than it is locally. The presence at high redshift of a significant number of ETGs with the same size as their local counterparts, as well as ETGs with quite small size (≲1/10 of the local one), points to a timescale for reaching the new, expanded equilibrium configuration of less than the Hubble time tH(z). We demonstrate that the projected mass of compact, high-redshift galaxies and that of local ETGs within the same physical radius, the nominal half-luminosity radius of high-redshift ETGs, differ substantially in that the high-redshift ETGs are on average significantly denser. This result suggests that the physical mechanism responsible for the size increase should also remove mass from central galaxy regions (r ≲ 1 kpc). We propose that quasar activity, which peaks at redshift z ∼ 2, can remove large amounts of gas from central galaxy regions on a timescale shorter than the triggering a puffing up of the stellar component at constant stellar mass (or a timescale on the order of the dynamical one); in this case, the size increase goes together with a decrease in the central mass. The size evolution is expected to parallel that of the quasars and the inverse hierarchy, or downsizing, seen in the quasar evolution is mirrored in the size evolution. Exploiting the virial theorem, we derive the relation between the stellar velocity dispersion of ETGs and the characteristic velocity of their hosting halos at the time of formation and collapse. By combining this relation with the halo formation rate at z ≳ 1, we predict the local velocity dispersion distribution function. On comparing it to the observed one, we show that velocity dispersion evolution of massive ETGs is fully compatible with the observed average evolution in size at constant stellar mass. Less massive ETGs (with stellar masses M⋆ ≲ 3 × 1010 M☉) are expected to evolve less both in size and in velocity dispersion, because their evolution is essentially determined by supernova feedback, which cannot yield winds as powerful as those triggered by quasars. The differential evolution is expected to leave imprints in the size versus luminosity/mass, velocity dispersion versus luminosity/mass, and central black hole mass versus velocity dispersion relationships, as observed in local ETGs.
First observations of CN (2–1), HCO+ (3–2) and C2H (3–2) emission lines in the Perseus cluster: constraints on heating mechanisms in the cluster gas

We present the first observations of emission lines of CN (2-1), HCO+ (3-2) and C2H (3-2) in the Perseus cluster. We observed at two positions: directly at the central galaxy, NGC 1275, and also at a position about 20 arcsec to the east where associated filamentary structure has been shown to have strong CO emission. Clear detections in CN and HCO+ transitions and a weak detection of the C2H transition were made towards NGC 1275, while weak detections of CN and HCO+ were made towards the eastern filamentary structure. Crude estimates of the column densities and fractional abundances (mostly upper limits) as functions of an unknown rotational temperature were made to both sources. These observational data were compared with the outputs of thermal/chemical models previously published by Bayet et al. in an attempt to constrain the heating mechanisms in cluster gas. We find that models in which heating is caused mainly by cosmic rays while other sources of heating are unimportant can account for the molecular observations. This conclusion is consistent with that of Ferland et al. in their study of gas traced by optical and infrared radiation. The cosmic ray heating rate in the regions probed by molecular emissions is required to be at least two orders of magnitude larger than that in the Milky Way.