The Phonology And Morphology Of Yemeni Tihami Dialect: An Autosegmental Account

Tidak banyak kajian metodologi tentang dialek Arab, terutamanya dialek Arab Yemen (YAD) (Versteegh, 1997). Little methodological studies are available on Arabic dialectology particularly on Yemeni Arabic dialects (YADs) (Versteegh, 1997)

Kinematic Evolution of Simulated Star-Forming Galaxies

Recent observations have shown that star-forming galaxies like our own Milky Way evolve kinematically into ordered thin disks over the last ~8 billion years since z=1.2, undergoing a process of "disk settling." For the first time, we study the kinematic evolution of a suite of four state of the art "zoom in" hydrodynamic simulations of galaxy formation and evolution in a fully cosmological context and compare with these observations. Until now, robust measurements of the internal kinematics of simulated galaxies were lacking as the simulations suffered from low resolution, overproduction of stars, and overly massive bulges. The current generation of simulations has made great progress in overcoming these difficulties and is ready for a kinematic analysis. We show that simulated galaxies follow the same kinematic trends as real galaxies: they progressively decrease in disordered motions (sigma_g) and increase in ordered rotation (Vrot) with time. The slopes of the relations between both sigma_g and Vrot with redshift are consistent between the simulations and the observations. In addition, the morphologies of the simulated galaxies become less disturbed with time, also consistent with observations, and they both have similarly large scatter. This match between the simulated and observed trends is a significant success for the current generation of simulations, and a first step in determining the physical processes behind disk settling.Comment: ApJ accepted; 6 pages; A pdf with full resolution figures can be found at https://db.tt/8y4Vzaff (2.8M

Characterization of soil fertility in Coffee (Coffea spp.) production areas in Côte d'Ivoire

With the depletion of forest reserves, coffee growing based on extensive and shifting cultivation mode is no more reproductive. Thus, soils of different coffee growing areas were studied in order to diagnose the fertility level, their potential for productivity of new varieties of coffee (Coffea canephora Pierre, var. Robusta) and their sustainable managements. In total, 156 soil samples were collected and analyzed in the laboratory using standard methods to determine their physicochemical statutes. The results obtained show a low nitrogen content of less than 0.27% in all soil mapping units, a base saturation percentage lower than 60% for the vast majority of soils and crucial presence of organic matter on distribution of physicochemical properties. Clustering of results identified two main components, which accounted for 88.69% of the variability of the data and the grouping into three communities by similarity of features. In view of these results, a sustainable production of the coffee trees requires a fertilization program for the improvement of soils under coffee trees

The Epoch of Disk Formation: z is Approximately l to Today

We present data on galaxy kinematics, morphologies, and star-formation rates over 0.1 less than z less than 1.2 for approximately 500 blue galaxies. These data show how systems like our own Milky-Way have come into being. At redshifts around 1, about half the age of the Universe ago, Milky-Way mass galaxies were different beasts than today. They had a significant amount of disturbed motions, disturbed morphologies, shallower potential wells, higher specific star-formation rates, and likely higher gas fractions. Since redshift approximately 1, galaxies have decreased in disturbed motions, increased in rotation velocity and potential well depth, become more well-ordered morphologically, and decreased in specific star-formation rate. We find interrelationships between these measurements. Galaxy kinematics are correlated with morphology and specific star-formation rate such that galaxies with the fastest rotation velocities and the least amounts of disturbed motions have the most well-ordered morphologies and the lowest specific star-formation rates. The converse is true. Moreover, we find that the rate at which galaxies become more well-ordered kinematically (i.e., increased rotation velocity, decreased disturbed motions) and morphologically is directly proportional to their stellar mass

The Rise and Fall of Star Formation Histories of Blue Galaxies at Redshifts 0.2 < z < 1.4

Popular cosmological scenarios predict that galaxies form hierarchically from the merger of many progenitor, each with their own unique star formation history (SFH). We use the approach recently developed by Pacifici et al. to constrain the SFHs of 4517 blue (presumably star-forming) galaxies with spectroscopic redshifts in the range O.2 < z < 1:4 from the All-Wavelength Extended Groth Strip International Survey (AEGIS). This consists in the Bayesian analysis of the observed galaxy spectral ' energy distributions with a comprehensive library of synthetic spectra assembled using state-of-the-art models of star formation and chemical enrichment histories, stellar population synthesis, nebular emission and attenuation by dust. We constrain the SFH of each galaxy in our sample by comparing the observed fluxes in the B, R,l and K(sub s) bands and rest-frame optical emission-line luminosities with those of one million model spectral energy distributions. We explore the dependence of the resulting SFH on galaxy stellar mass and redshift. We find that the average SFHs of high-mass galaxies rise and fall in a roughly symmetric bell-shaped manner, while those of low-mass galaxies rise progressively in time, consistent with the typically stronger activity of star formation in low-mass compared to high-mass galaxies. For galaxies of all masses, the star formation activity rises more rapidly at high than at low redshift. These findings imply that the standard approximation of exponentially declining SFHs wIdely used to interpret observed galaxy spectral energy distributions is not appropriate to constrain the physical parameters of star-forming galaxies at intermediate redshifts

Mapping cacao fertiliser requirements in Côte d'Ivoire

In Côte d'Ivoire, soils in cacao plantations are depleted due to the absence or underuse of fertilisation. A digital map of 130 landunits was created from soil and climatic parameters. A soil diagnosis software was combined with GIS (geographical information system) to convert the current unique fertiliser “Engrais cacao” into a greater number of recommendations more adapted to local conditions, thus more actual. Cacao fertiliser requirements were calculated from soil samples taken in mature cacao plantations in each landunit. The relationships between nutrient requirements and soil chemical parameters enabled building a map of the actual cacao fertiliser recommendations. Soils with identical characteristics were compared regarding their cacao nutritional needs. Highly significant correlations between soil nutrients were found; particularly, Ca and Mg were highly correlated with K, making it possible to calculate the Ca and Mg amounts in fertiliser formulae as function of K (i.e. Ca = 8.5×K and Mg = 3×K). The final map contains 23 N-P-K-Ca-Mg fertiliser formulae. Among them, the currently recommended blanket fertiliser represents 16.5% of the cacao areas. The comparison of our results with a previous study, done 40 years ago, evidenced that the soil nutrients under cacao have significantly decreased over the period, reinforcing the need for fertilizers. (Résumé d'auteur

z~2: An Epoch of Disk Assembly

We explore the evolution of the internal gas kinematics of star-forming galaxies from the peak of cosmic star-formation at $z\sim2$ to today. Measurements of galaxy rotation velocity $V_{rot}$, which quantify ordered motions, and gas velocity dispersion $\sigma_g$, which quantify disordered motions, are adopted from the DEEP2 and SIGMA surveys. This sample covers a continuous baseline in redshift from $z=2.5$ to $z=0.1$, spanning 10 Gyrs. At low redshift, nearly all sufficiently massive star-forming galaxies are rotationally supported ($V_{rot}>\sigma_g$). By $z=2$, the percentage of galaxies with rotational support has declined to 50$\%$ at low stellar mass ($10^{9}-10^{10}\,M_{\odot}$) and 70$\%$ at high stellar mass ($10^{10}-10^{11}M_{\odot}$). For $V_{rot}\,>\,3\,\sigma_g$, the percentage drops below 35$\%$ for all masses. From $z\,=\,2$ to now, galaxies exhibit remarkably smooth kinematic evolution on average. All galaxies tend towards rotational support with time, and it is reached earlier in higher mass systems. This is mostly due to an average decline in $\sigma_g$ by a factor of 3 since a redshift of 2, which is independent of mass. Over the same time period, $V_{rot}$ increases by a factor of 1.5 for low mass systems, but does not evolve for high mass systems. These trends in $V_{rot}$ and $\sigma_g$ with time are at a fixed stellar mass and should not be interpreted as evolutionary tracks for galaxy populations. When galaxy populations are linked in time with abundance matching, not only does $\sigma_g$ decline with time as before, but $V_{rot}$ strongly increases with time for all galaxy masses. This enhances the evolution in $V_{rot}/\sigma_g$. These results indicate that $z\,=\,2$ is a period of disk assembly, during which the strong rotational support present in today's massive disk galaxies is only just beginning to emerge.Comment: 12 pages, 8 figures, submitted to Ap