1,695 research outputs found
Produtividade econômica e componentes da produção de espigas verdes de milho em função da adubação nitrogenada.
Foi avaliado, durante dois anos, o efeito de doses de nitrogênio (N) na produtividade de espigas verdes de milho e em componentes da sua produção. Cinco doses de N (0, 60, 120, 180 e 240 kg ha-1) aplicadas em cobertura foram testadas num delineamento experimental de blocos casualizados, com quatro repetições. Foram avaliadas a produção e o número de espigas comerciais com palha por hectare, peso das espigas com e sem palha, comprimento e diâmetro de espigas sem palha e relação espiga com palha/palha. Aumentos na produtividade de espigas comerciais com palha com a aplicação de N foram encontrados, sendo estimadas as máximas produtividades de 13,52 t ha-1 com a dose de 157 kg ha-1 de N (primeiro ano) e de 14,86 t ha-1 com a dose de 177 kg ha-1 de N (segundo ano). Os aumentos na produtividade de espigas não foram devido aos aumentos do número de espigas por área e do comprimento destas, que não foram afetados pela adubação nitrogenada. Diferentemente da relação espiga/palha, o peso e o diâmetro das espigas foram influenciados pela elevação das doses de N. Foi proposta uma tabela de recomendação de adubação nitrogenada nos moldes de preços preestabelecidos de N e de espigas
Spectroscopic Observations of Optically Selected Clusters of Galaxies from the Palomar Distant Cluster Survey
We have conducted a redshift survey of sixteen cluster candidates from the
Palomar Distant Cluster Survey (PDCS) to determine both the density of PDCS
clusters and the accuracy of the estimated redshifts presented in the PDCS
catalog (Postman et. al. 1996). We find that the matched-filter redshift
estimate presented in the PDCS has an error sigma_z = 0.06 in the redshift
range 0.1 < z < 0.35 based on eight cluster candidates with three or more
concordant galaxy redshifts.
We measure the low redshift (0.1 < z < 0.35) space density of PDCS clusters
to be 31.3^{+30.5}_{-17.1} * E-06 h^3 Mpc^-3 (68% confidence limits for a
Poisson distribution) for Richness Class 1 systems. We find a tentative space
density of 10.4^{+23.4}_{-8.4}* E-06 h^3 Mpc^-3 for Richness Class 2 clusters.
These densities compare favorably with those found for the whole of the PDCS
and support the finding that the space density of clusters in the PDCS is a
factor of ~5 above that of clusters in the Abell catalog (Abell 1958; Abell,
Corwin, and Olowin 1989). These new space density measurements were derived as
independently as possible from the original PDCS analysis and therefore,
demonstrate the robustness of the original work. Based on our survey, we
conclude that the PDCS matched-filter algorithm is successful in detecting real
clusters and in estimating their true redshifts in the redshift range we
surveyed.Comment: 23 pages with 4 figures and 3 seperate tables. To be published in the
November Issue of the Astronomical Journa
A Serendipitous Galaxy Cluster Survey with XMM: Expected Catalogue Properties and Scientific Applications
This paper describes a serendipitous galaxy cluster survey that we plan to
conduct with the XMM X-ray satellite. We have modeled the expected properties
of such a survey for three different cosmological models, using an extended
Press-Schechter (Press & Schechter 1974) formalism, combined with a detailed
characterization of the expected capabilities of the EPIC camera on board XMM.
We estimate that, over the ten year design lifetime of XMM, the EPIC camera
will image a total of ~800 square degrees in fields suitable for the
serendipitous detection of clusters of galaxies. For the presently-favored
low-density model with a cosmological constant, our simulations predict that
this survey area would yield a catalogue of more than 8000 clusters, ranging
from poor to very rich systems, with around 750 detections above z=1. A
low-density open Universe yields similar numbers, though with a different
redshift distribution, while a critical-density Universe gives considerably
fewer clusters. This dependence of catalogue properties on cosmology means that
the proposed survey will place strong constraints on the values of Omega-Matter
and Omega-Lambda. The survey would also facilitate a variety of follow-up
projects, including the quantification of evolution in the cluster X-ray
luminosity-temperature relation, the study of high-redshift galaxies via
gravitational lensing, follow-up observations of the Sunyaev-Zel'dovich effect
and foreground analyses of cosmic microwave background maps.Comment: Accepted to ApJ. Minor changes, e.g. presentation of temperature
errors as a figure (rather than as a table). Latex (20 pages, 6 figures, uses
emulateapj.sty
Mass Profiles of the Typical Relaxed Galaxy Clusters A2199 and A496
We present maps and radial profiles of the gas temperature in the nearby
galaxy clusters A2199 and A496, which have the most accurate ASCA spectral data
for all hot clusters. These clusters are relaxed and can provide reliable X-ray
mass measurements under the assumption of hydrostatic equilibrium. The cluster
average temperatures corrected for the presence of cooling flows are 4.8+-0.2
keV and 4.7+-0.2 keV (90% errors), respectively. Outside the central cooling
flow regions, the radial temperature profiles are similar to those of the
majority of nearby relaxed clusters. They are accurately described by
polytropic models with gamma=1.17+-0.07 for A2199 and gamma=1.24+-0.09 for
A496. We use these polytropic models to derive accurate total mass profiles.
Within r=0.5/h Mpc, which corresponds to a radius of overdensity 1000, the
total mass values are 1.45+-0.15 10^14 /h Msun and 1.55+-0.15 10^14 /h Msun.
These values are 10% lower than those obtained assuming constant temperature.
The values inside a gas core radius (0.07-0.13/h Mpc) are a factor of >1.5
higher than the isothermal values. The gas mass fraction increases with radius
(by a factor of 3 between the X-ray core radius and r_1000) and at r_1000
reaches values of 0.057+-0.005 and 0.056+-0.006 h^-3/2 for the two clusters,
respectively. Our mass profiles within r_1000 are remarkably well approximated
by the NFW "universal" profile. Since A2199 and A496 are typical relaxed
clusters, the above findings should be relevant for most such systems. In
particular, the similarity of the temperature profiles in nearby clusters
appears to reflect the underlying "universal" dark matter profile. The upward
revision of mass at small radii will resolve most of the discrepancy between
the X-ray and strong lensing mass estimates. (Abridged)Comment: Latex, 9 pages, 6 figures, uses emulateapj.sty. Submitted to Ap
Inflationary cosmology with scalar field and radiation
We present a simple, exact and self-consistent cosmology with a
phenomenological model of quantum creation of radiation due to decay of the
scalar field. The decay drives a non-isentropic inflationary epoch, which exits
smoothly to the radiation era, without reheating. The initial vacuum for
radiation is a regular Minkowski vacuum. The created radiation obeys standard
thermodynamic laws, and the total entropy produced is consistent with the
accepted value. We analyze the difference between the present model and a model
with decaying cosmological constant previously considered.Comment: 13 pages Latex; to appear Gen. Rel. Gra
The WARPS survey: III. The discovery of an X-ray luminous galaxy cluster at z=0.833 and the impact of X-ray substructure on cluster abundance measurements
The WARPS team reviews the properties and history of discovery of
ClJ0152.7-1357, an X-ray luminous, rich cluster of galaxies at z=0.833. At L_X
= 8 x 10^44 h^(-2) erg/s (0.5-2.0 keV) ClJ0152.7-1357 is the most X-ray
luminous cluster known at redshifts z>0.55. The high X-ray luminosity of the
system suggests that massive clusters may begin to form at redshifts
considerably greater than unity. This scenario is supported by the high degree
of optical and X-ray substructure in ClJ0152.7-1357, which is similarly complex
as that of other X-ray selected distant clusters and consistent with the
picture of cluster formation by mass infall along large-scale filaments. X-ray
emission from ClJ0152.7-1357 was detected already in 1980 with the EINSTEIN
IPC. However, because the complex morphology of the emission caused its
significance to be underestimated, the corresponding source was not included in
the EMSS cluster sample and hence not previously identified. Simulations of the
EMSS source detection and selection procedure suggest a general bias of the
EMSS against X-ray luminous clusters with pronounced substructure. If highly
unrelaxed, merging clusters are common at high redshift, they could create a
bias in some samples as the morphological complexity of mergers may cause them
to fall below the flux limit of surveys that assume a unimodal spatial source
geometry. Conversely, the enhanced X-ray luminosity of mergers might cause them
to, temporarily, rise above the flux limit. Either effect could lead to
erroneous conclusions about the evolution of the comoving cluster space
density. A high fraction of morphologically complex clusters at high redshift
would also call into question the validity of cosmological studies that assume
that the systems under investigation are virialized.Comment: 17 pages, 7 figures; revised to focus on possible detection biases
caused by substructure in clusters; accepted for publication in ApJ; uses
emulateapj.sty; eps files of figures 1 and 2 can be obtained from
ftp://hubble.ifa.hawaii.edu/pub/ebeling/warp
Controlling and monitoring water stress in contrasting environment for drought tolerance phenotyping of cereals and legumes.
Time scale separation and heterogeneous off-equilibrium dynamics in spin models over random graphs
We study analytically and numerically the statics and the off-equilibrium
dynamics of spin models over finitely connected random graphs. We identify a
threshold value for the connectivity beyond which the loop structure of the
graph becomes thermodynamically relevant. Glauber dynamics simulations show
that this loop structure is responsible for the onset of dynamical features of
a local character (dynamical heterogeneities and spontaneous time scale
separation), consistently with previous (experimental and numerical) studies of
glasses and spin glasses in their approach to the low temperature phase.Comment: 5 pages, latex, 2 postscript figure
Observational Constraints on Open Inflation Models
We discuss observational constraints on models of open inflation. Current
data from large-scale structure and the cosmic microwave background prefer
models with blue spectra and/or Omega_0 >= 0.3--0.5. Models with minimal
anisotropy at large angles are strongly preferred.Comment: 4 pages, RevTeX, with 2 postscript figures included. Second Figure
correcte
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