Intervalo hídrico ótimo e grau de compactação de um latossolo vermelho após 30 anos sob plantio direto

A qualidade física do solo é um dos fatores determinantes da sustentabilidade agronômica, econômica e ambiental no sistema plantio direto (SPD). A compactação do solo tem sido apontada como um dos fatores de redução da qualidade física em solos sob SPD. Contudo, com a utilização do SPD, pode haver o incremento de matéria orgânica do solo e o desenvolvimento de um sistema poroso contínuo e estável, que atenuam os impactos negativos da compactação. O objetivo deste trabalho foi avaliar a qualidade física de um Latossolo Vermelho distroférrico sob SPD durante 30 anos, utilizando o intervalo hídrico ótimo (IHO) e o grau de compactação do solo (GC). Em uma área comercial com histórico de altas produtividades sob SPD, foram coletadas amostras de solo com estrutura preservada e deformada, para determinação da densidade do solo (Ds), do IHO e do GC. As amostras com estrutura preservada foram obtidas em três posições, relativas às linhas (L), entrelinhas (E) e posição intermediária entre as linhas e entrelinhas (PI) da cultura do milho. Foram determinadas as curvas de retenção de água e resistência do solo à penetração, bem como a Ds. A amostra de solo com estrutura deformada foi usada para obter a curva de compactação, utilizando o teste de Proctor. A Dmax foi obtida a partir da curva de compactação, e o GC foi determinado pela razão entre a Ds e a Dmax. Independentemente dos limites críticos de resistência à penetração (RP), verifica-se redução do IHO com o aumento da Ds. Os maiores valores do IHO foram verificados na posição de amostragem L, e a utilização de RP crítica maior que 2,0 MPa resultou em IHO condizente com a qualidade física desse solo sob SPD de longo tempo. A Dmax foi de 1,52 kg dm-3, e o GC variou de 64 a 87 %, sendo os maiores valores obtidos nas posições E e PI. Os valores de IHO e GC obtidos neste estudo indicam que a qualidade física desse solo não é limitante à produção das culturas após 30 anos de utilização do SPD.

The globular cluster kinematics and galaxy dark matter content of NGC 3923

This paper presents further results from our spectroscopic study of the globular cluster (GC) system of the group elliptical NGC 3923. From observations made with the GMOS instrument on the Gemini South Telescope, an additional 50 GC and ultra-compact dwarf (UCD) candidates have been spectroscopically confirmed as members of the NGC 3923 system. When the recessional velocities of these GCs are combined with the 29 GC velocities reported previously, a total sample of 79 GC/UCD velocities is produced. This sample extends to over 6 arcmin (>6 R-e similar to 30 kpc) from the centre of NGC 3923 and is used to study the dynamics of the GC system and the dark matter content of NGC 3923. It is found that the GC system of NGC 3923 displays no appreciable rotation, and that the projected velocity dispersion is constant with radius within the uncertainties. The velocity dispersion profiles of the integrated light and GC system of NGC 3923 are indistinguishable over the region in which they overlap. We find some evidence that the diffuse light and GCs of NGC 3923 have radially biased orbits within similar to 130 arcsec. The application of axisymmetric orbit-based models to the GC and integrated light velocity dispersion profiles demonstrates that a significant increase in the mass-to-light ratio (from M/L-V = 8 to 26) at large galactocentric radii is required to explain this observation. We therefore confirm the presence of a dark matter halo in NGC 3923. We find that dark matter comprises 17.5(-4.5)(+7.3) per cent of the mass within 1 R-e, 41.2(-10.6)(+18.2) per cent within 2 R-e and 75.6(-16.8)(+15.4) per cent within the radius of our last kinematic tracer at 6.9 R-e. The total dynamical mass within this radius is found to be 1.5(-0.25)(+0.4) x 10(12) M-circle dot. In common with other studies of large ellipticals, we find that our derived dynamical mass profile is consistently higher than that derived by X-ray observations, by a factor of around 2.

The 6dF Galaxy Survey: stellar population trends across and through the Fundamental Plane

We present results from an analysis of stellar population parameters for 7132 galaxies in the 6dF Galaxy Survey Fundamental Plane (FP) sample. We bin the galaxies along the axes, v1, v2 and v3, of the tri-variate Gaussian to which we have fitted the galaxy distribution in effective radius, surface brightness and central velocity dispersion (FP space), and compute median values of stellar age, [Fe/H], [Z/H] and [a/Fe]. We determine the directions of the vectors in FP space along which each of the binned stellar population parameters vary most strongly. In contrast to previous work, we find stellar population trends not just with velocity dispersion and FP residual, but with radius and surface brightness as well. The most remarkable finding is that the stellar population parameters vary through the plane (v1 direction) and across the plane (v3 direction), but show no variation at all along the plane (v2 direction). The v2 direction in FP space roughly corresponds to luminosity density. We interpret a galaxys position along this vector as being closely tied to its merger history, such that early-type galaxies with lower luminosity density are more likely to have undergone major mergers. This conclusion is reinforced by an examination of the simulations of Kobayashi, which show clear trends of merger history with v2.

FINDING FOSSIL GROUPS: OPTICAL IDENTIFICATION AND X-RAY CONFIRMATION

We report the discovery of 12 new fossil groups (FGs) of galaxies, systems dominated by a single giant elliptical galaxy and cluster-scale gravitational potential, but lacking the population of bright galaxies typically seen in galaxy clusters. These FGs, selected from the maxBCG optical cluster catalog, were detected in snapshot observations with the Chandra X-ray Observatory. We detail the highly successful selection method, with an 80% success rate in identifying 12 FGs from our target sample of 15 candidates. For 11 of the systems, we determine the X-ray luminosity, temperature, and hydrostatic mass, which do not deviate significantly from expectations for normal systems, spanning a range typical of rich groups and poor clusters of galaxies. A small number of detected FGs are morphologically irregular, possibly due to past mergers, interaction of the intra-group medium with a central active galactic nucleus (AGN), or superposition of multiple massive halos. Two-thirds of the X-ray-detected FGs exhibit X-ray emission associated with the central brightest cluster galaxy (BCG), although we are unable to distinguish between AGN and extended thermal galaxy emission using the current data. This sample representing a large increase in the number of known FGs, will be invaluable for future planned observations to determine FG temperature, gas density, metal abundance, and mass distributions, and to compare to normal (non-fossil) systems. Finally, the presence of a population of galaxy-poor systems may bias mass function determinations that measure richness from galaxy counts. When used to constrain power spectrum normalization and Omega(m), these biased mass functions may in turn bias these results.