Power Spectrum Analysis of the Stromlo-APM Redshift Survey

We test estimators of the galaxy power spectrum $P(k)$ against simulated galaxy catalogues constructed from N-body simulations and we derive formulae to correct for biases. These estimators are then applied to compute the power spectrum of galaxies in the Stromlo-APM redshift survey. We test whether the amplitude of $P(k)$ depends on galaxy luminosity, but find no significant luminosity dependence except at absolute magnitudes brighter than M_{\bj} = -20.3, (H_{0} = 100 \kms) where there is some evidence for a rise in the amplitude of $P(k)$. By comparing the redshift space power spectrum of the Stromlo-APM survey with the real space power spectrum determined from the parent APM Galaxy Survey, we attempt to measure the distortion in the shape of $P(k)$ caused by galaxy peculiar motions. We find some evidence for an effect, but the errors are large and do not exclude a value of $\beta = \Omega^{0.6}/b = 1$, where $\Omega$ is the cosmological density parameter and $b$ is the linear biasing parameter relating galaxy fluctuations to those in the mass, $\left(\delta \rho/\rho\right)_{gal} = b \left(\delta \rho/\rho\right)_{m}$. The shape of the Stromlo-APM power spectrum is consistent with that determined from the CfA-2 survey, but has a slightly higher amplitude by a factor of about 1.4 than the power spectrum of IRAS galaxies.Comment: 14 pages, gziped and uuencoded postscript file. Submitted to MNRA

The impact of E-Services on the performance of AL- Balqa Applied University

The study aimed to uncover the extent of the quality of electronic services in the Al Balqa Applied University, as seen by faculty and administrative members. the study revealed the impact of electronic services on the performance, and detected if there are differences in the estimation of members of the study about the quality of e-services and the impact on the performance. The study population consisted of (1475) faculty members, (3057) administrative members, a simple random sample consisting of (162) faculty members, and (227) administrative members has been taken. The quality of electronic services resulted in (medium degree), and the impact of electronic services on the performance resulted in (high degree). The statistical significance of differences attributable to the impact of job title came in favor of the administrative body. In light of this study, a set of recommendations has been formulated to benefit the concern of the study. Keywords: e-services, e-government, e-administration, performance, Al Balqa Applied University

Determination of trace elements in triglycine sulfate solutions

Ten elements were divided into 2 groups. The elements in the first group included iron, nickel, chromium, manganese, copper, and gold. The elements in the second group included zinc, cobalt, lead, cadmium, and gold. Five ppm of each element in each group was spiked in a 1 percent triglycine sulfate (TGS) solution. Glycine was removed with 1-naphthyl isocyanate in ether medium. The glycine derivative 1-naphthyl isocyanate glycine was removed by filtration, and the filtrates were analyzed for the different elements. Analysis of these elements was performed by using the 5100 Perkin-Elmer Atomic Absorption Spectrophotometer. The result of these experiments was the observation that there was a decrease in the concentration of chromium and gold, which was interpreted to be due to the chelation of these elements by the derivative 1-naphthyl isocyanate glycine. Further research is needed to determine the concentration of other elements in triglycine sulfate (TGS) solutions. These elements will include lithium, sodium, rubidium, magnesium, calcium, strontium, barium, aluminum, and silicon. These are the most likely elements to be found in the sulfuric acid used in manufacturing the TGS crystal. Moreover, we will extend our research to investigate the structural formula of the violet colored chelated compounds, which had been formed by interaction of the derivative 1-naphthyl isocyanate glycine with the different elements, such as gold, chromium

The Bispectrum of IRAS Galaxies

We compute the bispectrum for the galaxy distribution in the IRAS QDOT, 2Jy, and 1.2Jy redshift catalogs for wavenumbers 0.05<k<0.2 h/Mpc and compare the results with predictions from gravitational instability in perturbation theory. Taking into account redshift space distortions, nonlinear evolution, the survey selection function, and discreteness and finite volume effects, all three catalogs show evidence for the dependence of the bispectrum on configuration shape predicted by gravitational instability. Assuming Gaussian initial conditions and local biasing parametrized by linear and non-linear bias parameters b_1 and b_2, a likelihood analysis yields 1/b_1 = 1.32^{+0.36}_{-0.58}, 1.15^{+0.39}_{-0.39} and b_2/b_1^2=-0.57^{+0.45}_{-0.30}, -0.50^{+0.31}_{-0.51}, for the for the 2Jy and 1.2Jy samples, respectively. This implies that IRAS galaxies trace dark matter increasingly weakly as the density contrast increases, consistent with their being under-represented in clusters. In a model with chi^2 non-Gaussian initial conditions, the bispectrum displays an amplitude and scale dependence different than that found in the Gaussian case; if IRAS galaxies do not have bias b_1> 1 at large scales, \chi^2 non-Gaussian initial conditions are ruled out at the 95% confidence level. The IRAS data do not distinguish between Lagrangian or Eulerian local bias.Comment: 30 pages, 11 figure

Application of Data Compression Methods to the Redshift-space distortions of the PSCz galaxy catalogue

We apply a spherical harmonic analysis to the Point Source Redshift Survey (PSCz), to compute the real-space galaxy power spectrum and the degree of redshift distortion caused by peculiar velocities. We employ new parameter eigenvector and hierarchical data compression techniques, allowing a much larger number of harmonic modes to be included, and correspondingly smaller error bars. Using 4644 harmonic modes, compressed to 2278, we find that the IRAS redshift-space distortion parameter is $beta = 0.39 pm 0.12$ and the amplitude of galaxy clustering on a scale of $k=0.1 Mpch$ is $Delta_{ m gal}(0.1)=0.42 pm 0.02$. Combining these we find the amplitude of mass perturbations is $Delta_m(0.1)=(0.16pm0.04) Omega_m^{-0.6}$. A preliminary model fitting analysis combining the PSCz amplitudes with the CMB and abundance of clusters yields the cosmological matter density parameter $Omega_m=0.16pm 0.03$, the amplitude of primordial perturbations $Q=(8.4pm 3.8) times 10^{-5}$, and the IRAS bias parameter $b=0.84pm 0.28$

Sensitivity of Redshift Distortion Measurements to Cosmological Parameters

The multipole moments of the power spectrum of large scale structure, observed in redshift space, are calculated for a finite sample volume including the effects of both the linear velocity field and geometry. A variance calculation is also performed including the effects of shot noise. The sensitivity with which a survey with the depth and geometry of the Sloan Digital Sky Survey (SDSS) can measure cosmological parameters $\Omega_0$ and $b_0$ (the bias) or $\lambda_0$ (the cosmological constant) and $b_0$ is derived through fitting power spectrum moments to the large scale structure in the linear regime in a way which is independent of the evolution of the galaxy number density. We find that for surveys of the approximate depth of the SDSS no restrictions can be placed on $\Omega_0$ at the 99% confidence limit when a fiducial open, $\Omega_0 = 0.3$ model is assumed and bias is unconstrained. At the 95% limit, $\Omega_{0} < .85$ is ruled out. Furthermore, for this fiducial model, both flat (cosmological constant) and open models are expected to reasonably fit the data. For flat, cosmological constant models with a fiducial $\Omega_{0} = 0.3$, we find that models with $\Omega_{0} > 0.48$ are ruled out at the 95% confidence limit regardless of the choice of the bias parameter, and open models cannot fit the data even at the 99% confidence limit.Comment: We correct an error which which caused us to overestimate the cosmic variance of our statistics. We also include shot noise in the new variace calculation. In our fitting proceedure, we now include $\sigma$, the non-linear velocity dispersion, as a free parameter. Our conclusions are modifed as a result, with $\Omega_0=0.3$ open models now nominaly excluding $\Omega_0 = 1$ at the 95% but not 99% confidence limi