Twenty-three infants with neonatal cholestasis were examined laparoscopically. The differential diagnosis between biliary atresia and neonatal hepatitis was not established by-clinical and laboratory ...investigations. In 10 out of 23 cases the transcutaneous-transhepatic-cholangiography, performed with laparoscopy demonstrated the permeability of the biliary tree in children that are not suffering from the atresia. The hepatic biopsy by laparoscopic view allowed to complete the investigation in these cases, avoiding unnecessary laparotomy. In infants suffering from biliary atresia the surgery indication was early and exact.
An industrial microorganism, Streptomyces avermitilis, which is a producer of anthelmintic macrocyclic lactones, avermectins, has been constructed as a versatile model host for heterologous ...expression of genes encoding secondary metabolite biosynthesis. Twenty of the entire biosynthetic gene clusters for secondary metabolites were successively cloned and introduced into a versatile model host S. avermitilis SUKA17 or 22. Almost all S. avermitilis transformants carrying the entire gene cluster produced metabolites as a result of the expression of biosynthetic gene clusters introduced. A few transformants were unable to produce metabolites, but their production was restored by the expression of biosynthetic genes using an alternative promoter or the expression of a regulatory gene in the gene cluster that controls the expression of biosynthetic genes in the cluster using an alternative promoter. Production of metabolites in some transformants of the versatile host was higher than that of the original producers, and cryptic biosynthetic gene clusters in the original producer were also expressed in a versatile host.
"Vamos apresentar um caderninho com todas as mudancas, todas as prioridades, todas as linhas de credito que se beneficiarao de uma reducao do spread. E sao muitas", anunciou ontem o presidente do ...banco, Guido Mantega. De acordo com ele, trata-se de "um momento proprio" da instituicao, que quer estimular areas prioritarias para o desenvolvimento do Pais, seguindo a tendencia da reducao da Taxa de Juros de Longo Prazo (TJLP), usada como referencia para os emprestimos do banco e que recuou de 9,75% para 9% ao ano, no mes passado).
Astrophys.J.Suppl.148:175-194,2003 WMAP precision data enables accurate testing of cosmological models. We find
that the emerging standard model of cosmology, a flat Lambda-dominated universe
seeded ...by nearly scale-invariant adiabatic Gaussian fluctuations, fits the WMAP
data. With parameters fixed only by WMAP data, we can fit finer scale CMB
measurements and measurements of large scle structure (galaxy surveys and the
Lyman alpha forest). This simple model is also consistent with a host of other
astronomical measurements. We then fit the model parameters to a combination of
WMAP data with other finer scale CMB experiments (ACBAR and CBI), 2dFGRS
measurements and Lyman alpha forest data to find the model's best fit
cosmological parameters: h=0.71+0.04-0.03, Omega_b h^2=0.0224+-0.0009, Omega_m
h^2=0.135+0.008-0.009, tau=0.17+-0.06, n_s(0.05/Mpc)=0.93+-0.03, and
sigma_8=0.84+-0.04. WMAP's best determination of tau=0.17+-0.04 arises directly
from the TE data and not from this model fit, but they are consistent. These
parameters imply that the age of the universe is 13.7+-0.2 Gyr. The data favors
but does not require a slowly varying spectral index. By combining WMAP data
with other astronomical data sets, we constrain the geometry of the universe,
Omega_tot = 1.02 +- 0.02, the equation of state of the dark energy w < -0.78
(95% confidence limit assuming w >= -1), and the energy density in stable
neutrinos, Omega_nu h^2 < 0.0076 (95% confidence limit). For 3 degenerate
neutrino species, this limit implies that their mass is less than 0.23 eV (95%
confidence limit). The WMAP detection of early reionization rules out warm dark
matter.
Astrophys.J.Suppl.148:1,2003 We present full sky microwave maps in five bands (23 to 94 GHz) from the WMAP
first year sky survey. Calibration errors are <0.5% and the low systematic
error level is ...well specified. The 2<l<900 anisotropy power spectrum is cosmic
variance limited for l<354 with a signal-to-noise ratio >1 per mode to l=658.
The temperature-polarization cross-power spectrum reveals both acoustic
features and a large angle correlation from reionization. The optical depth of
reionization is 0.17 +/- 0.04, which implies a reionization epoch of 180+220-80
Myr (95% CL) after the Big Bang at a redshift of 20+10-9 (95% CL) for a range
of ionization scenarios. This early reionization is incompatible with the
presence of a significant warm dark matter density. The age of the best-fit
universe is 13.7 +/- 0.2 Gyr old. Decoupling was 379+8-7 kyr after the Big Bang
at a redshift of 1089 +/- 1. The thickness of the decoupling surface was dz=195
+/- 2. The matter density is Omega_m h^2 = 0.135 +0.008 -0.009, the baryon
density is Omega_b h^2 = 0.0224 +/- 0.0009, and the total mass-energy of the
universe is Omega_tot = 1.02 +/- 0.02. The spectral index of scalar
fluctuations is fit as n_s = 0.93 +/- 0.03 at wavenumber k_0 = 0.05 Mpc^-1,
with a running index slope of dn_s/d ln k = -0.031 +0.016 -0.018 in the
best-fit model. This flat universe model is composed of 4.4% baryons, 22% dark
matter and 73% dark energy. The dark energy equation of state is limited to
w<-0.78 (95% CL). Inflation theory is supported with n_s~1, Omega_tot~1,
Gaussian random phases of the CMB anisotropy, and superhorizon fluctuations. An
admixture of isocurvature modes does not improve the fit. The tensor-to-scalar
ratio is r(k_0=0.002 Mpc^-1)<0.90 (95% CL).
The Wilkinson Microwave Anisotropy Probe WMAP has mapped the entire sky in five frequency bands between 23 and 94 GHz with polarization sensitive radiometers. We present three-year full-sky maps of ...the polarization and analyze them for foreground emission and cosmological implications. These observations open up a new window for understanding the universe. WMAP observes significant levels of polarized foreground emission due to both Galactic synchrotron radiation and thermal dust emission. The least contaminated channel is at 61 GHz. Informed by a model of the Galactic foreground emission, we subtract the foreground emission from the maps. In the foreground corrected maps, for l=2-6, we detect l(l+1) C_l^{EE} / (2 pi) = 0.086 +-0.029 microkelvin^2. This is interpreted as the result of rescattering of the CMB by free electrons released during reionization and corresponds to an optical depth of tau = 0.10 +- 0.03. We see no evidence for B-modes, limiting them to l(l+1) C_l^{BB} / (2 pi) = -0.04 +- 0.03 microkelvin^2. We find that the limit from the polarization signals alone is r<2.2 (95% CL) corresponding to a limit on the cosmic density of gravitational waves of Omega_{GW}h^2 < 5 times 10^{-12}. From the full WMAP analysis, we find r<0.55 (95% CL) corresponding to a limit of Omega_{GW}h^2 < 10^{-12} (95% CL).
The WMAP satellite has completed 3 years of observations of the cosmic microwave background radiation. The 3-year data products include several sets of full sky maps of the Stokes I, Q and U ...parameters in 5 frequency bands, spanning 23 to 94 GHz, and supporting items, such as beam window functions and noise covariance matrices. The processing used to produce the current sky maps and supporting products represents a significant advancement over the first year analysis, and is described herein. Improvements to the pointing reconstruction, radiometer gain modeling, window function determination and radiometer spectral noise parametrization are presented. A detailed description of the updated data processing that produces maximum likelihood sky map estimates is presented, along with the methods used to produce reduced resolution maps and corresponding noise covariance matrices. Finally two methods used to evaluate the noise of the full resolution sky maps are presented along with several representative year-to-year null tests, demonstrating that sky maps produced from data from different observational epochs are consistent.
We present new full-sky temperature maps in five frequency bands from 23 to 94 GHz, based on the first three years of the WMAP sky survey. The new maps, which are consistent with the first-year maps ...and more sensitive, incorporate improvements in data processing made possible by the additional years of data and by a more complete analysis of the polarization signal. These include refinements in the gain calibration and beam response models. We employ two forms of multi-frequency analysis to separate astrophysical foreground signals from the CMB, each of which improves on our first-year analyses. First, we form an improved 'Internal Linear Combination' map, based solely on WMAP data, by adding a bias correction step and by quantifying residual uncertainties in the resulting map. Second, we fit and subtract new spatial templates that trace Galactic emission; in particular, we now use low-frequency WMAP data to trace synchrotron emission. The WMAP point source catalog is updated to include 115 new sources. We derive the angular power spectrum of the temperature anisotropy using a hybrid approach that combines a maximum likelihood estimate at low l (large angular scales) with a quadratic cross-power estimate for l>30. Our best estimate of the CMB power spectrum is derived by averaging cross-power spectra from 153 statistically independent channel pairs. The combined spectrum is cosmic variance limited to l=400, and the signal-to-noise ratio per l-mode exceeds unity up to l=850. The first two acoustic peaks are seen at l=220.8 +- 0.7 and l=530.9 +- 3.8, respectively, while the first two troughs are seen at l=412.4 +- 1.9 and l=675.1 +- 11.1, respectively. The rise to the third peak is unambiguous; when the WMAP data are combined with higher resolution CMB measurements, the existence of a third acoustic peak is well established.
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