496 research outputs found
DISSOLUTION OF MARRIAGE: FUNCTIONAL APPROACH TO POLISH-ENGLISH TRANSLATION OF SELECTED COURT DOCUMENTS
W artykule zaprezentowano wyniki badań, których celem była analiza problemów właściwych dla tłumaczenia z języka polskiego na język angielski wybranych pism procesowych i orzeczeń sądowych w sprawach rozwodowych oraz w sprawach o orzeczenie separacji. W ramach badań przeprowadzono m.in. analizę tekstów paralelnych, zastosowano metody właściwe dla językoznawstwa korpusowego w celu ekstrakcji jednostek terminologicznych oraz komparastykę prawniczą w celu porównawczej analizy pojęć. Wyniki, w tym uwagi dotyczące konkretnych wyborów terminologicznych i frazeologicznych oraz rozwiązań na poziomie tekstu, a także krytyczną analizę wybranych powszechnie przyjętych ekwiwalentów, przedstawiono w formie tłumaczenia z komentarzem. W artykule ujęto także wyniki obserwacji dotyczących rodzajów oraz źródeł problemów tłumaczeniowych napotykanych przez początkujących oraz doświadczonych tłumaczy. Ponadto we wnioskach wskazano na potrzebę opracowania skuteczniejszej formy prezentowania wyników ukierunkowanych praktycznie badań w dziedzinie translatoryki, w szczególności w odniesieniu do tłumaczeń prawnych i prawniczych, która – w porównaniu do tradycyjnych słowników oraz baz terminologicznych – byłaby bogatsza pod względem merytorycznym oraz zawierała szersze informacje na temat kontekstu użycia poszczególnych terminów.The paper presents results of a study aimed at analysing problems that arise in Polish‑English translation of selected court documents in divorce and judicial separation cases, as well as the ways of solving such problems in the light of the functional approach to translation. The methodology used includes parallel texts analysis, corpus linguistics for term extraction and comparative legal research into concept comparison. The results, including comments on specific terminological, phraseological and textual choices and a critical analysis of certain established equivalents, are presented in the form of an annotated translation. The findings also include general observations on the types and the sources of common problems encountered by both beginner and experienced translators. Finally, a need is identified for developing a more effective form of presenting results of practice-oriented research in the field of translation studies, especially with reference to legal translation, which would account for a richer knowledge component and more extensive contextual information than traditional dictionaries and term‑bases
Dynamics of pairwise motions
We derive a simple closed-form expression, relating \vs(r) -- the mean
relative velocity of pairs of galaxies at fixed separation -- to the
two-point correlation function of mass density fluctuations, . We
compare our analytic model for \vs(r) with N-body simulations, and find
excellent agreement in the entire dynamical range probed by the simulations
(0.1 \lsim \xi \lsim 1000). Our results can be used to estimate the
cosmological density parameter, \Om, directly from redshift-distance surveys,
like Mark III.Comment: 10 pages 2 Figs., submitted to ApJ Let
Kurtosis of Large-Scale Cosmic Fields
An attractive and simple hypothesis for the formation of large-scale
structure is that it developed by gravitational instability from primordial
fluctuations with an initially Gaussian probability distribution. Non-linear
gravitational evolution drives the distribution away from the Gaussian form,
generating measurable skewness and kurtosis even when the variance of the
fluctuations is much smaller than unity. We use perturbation theory to compute
the kurtosis of the mass density field and the velocity divergence field that
arises during the weakly non-linear evolution of initially Gaussian
fluctuations. We adopt an Einstein--de~Sitter universe for the perturbative
calculations, and we discuss the generalization to a universe of arbitrary
. We obtain semi-analytic results for the case of scale-free, power-law
spectra of the initial fluctuations and final smoothing of cosmic fields with a
Gaussian filter. We also give an exact analytical formula for the dependence of
the skewness of these fields on the power spectrum index. We show that the
kurtosis decreases with the power spectrum index, and we compare our more
accurate results for the kurtosis to previous estimates from Monte Carlo
integrations. We also compare our results to values obtained from cosmological
N-body simulations with power-law initial spectra. Measurements of the skewness
and kurtosis parameters can be used to test the hypothesis that structure in
the universe formed by gravitational instability from Gaussian initial
conditions.Comment: 29 pp incl. 8 figs, uuencoded compressed postscript, submitted to
MNRAS, preprints CAMK/281, IASSNS-AST 94/3
Omega from the skewness of the cosmic velocity divergence
We propose a method for measuring the cosmological density parameter
from the statistics of the divergence field, , the
divergence of peculiar velocity, expressed in units of the Hubble constant, . The velocity field is spatially smoothed over to remove strongly nonlinear effects. Assuming weakly-nonlinear
gravitational evolution from Gaussian initial fluctuations, and using
second-order perturbative analysis, we show that \propto
-\Omega^{-0.6} ^2. The constant of proportionality depends on the
smoothing window. For a top-hat of radius R and volume-weighted smoothing, this
constant is , where . If the
power spectrum is a power law, , then . A Gaussian
window yields similar results. The resulting method for measuring is
independent of any assumed biasing relation between galaxies and mass.
The method has been successfully tested with numerical simulations. A
preliminary application to real data, provided by the POTENT recovery procedure
from observed velocities favors . However, because of an
uncertain sampling error, this result should be treated as an assessment of the
feasibility of our method rather than a definitive measurement of .Comment: 16 pages + 2 figures, uuencoded postscript file, also available by
anonymous ftp from ftp.cita.utoronto.ca in directory
/cita/francis/div_skewness, CITA 94-1
Transients from Zel'dovich initial conditions
We investigate the error implied by the use of the Zel'dovich approximation
to set up the initial conditions at a finite redshift zi in numerical
simulations. Using a steepest-descent method developed in a previous work we
derive the probability distribution P(delta_R) of the density contrast in the
quasi-linear regime. This also provides its dependence on the redshift zi at
which the simulation is started. Thus, we find that the discrepancy with the
exact pdf (defined by the limit zi->infinity) is negligible after the scale
factor has grown by a factor a/a_i>5, for scales which were initially within
the linear regime with sigma_i>0.1. This shows that the use of the Zel'dovich
approximation to implement the initial conditions is sufficient for practical
purposes since these are not very severe constraints.Comment: 6 pages, final version published in A&
The Real and Redshift Space Density Distribution Function for Large-Scale Structure in the Spherical Collapse Approximation
We use the spherical collapse (SC) approximation to derive expressions for
the smoothed redshift-space probability distribution function (PDF), as well as
the -order hierarchical amplitudes , in both real and redshift space.
We compare our results with numerical simulations, focusing on the
standard CDM model, where redshift distortions are strongest. We find good
agreement between the SC predictions and the numerical PDF in real space even
for \sigma_L \simgt 1, where is the linearly-evolved rms
fluctuation on the smoothing scale. In redshift space, reasonable agreement is
possible only for \sigma_L \simlt 0.4. Numerical simulations also yield a
simple empirical relation between the real-space PDF and redshift-space PDF: we
find that for \sigma \simlt 1, the redshift space PDF, P[\delta_z], is, to a
good approximation, a simple rescaling of the real space PDF, P[\delta], i.e.,
P[\delta/\sigma] d[\delta/\sigma] = P[\delta_z/\sigma_z] d[\delta_z/\sigma_z],
where and \sigma_z are the real-space and redshift-space rms
fluctuations, respectively. This result applies well beyond the validity of
linear perturbation theory, and it is a good fit for both the standard CDM
model and the Lambda-CDM model. It breaks down for SCDM at ,
but provides a good fit to the \Lambda-CDM models for as large as 0.8.Comment: 9 pages, latex, 12 figures added (26 total), minor changes to
conclusions, to appear in MNRA
Streaming velocities as a dynamical estimator of Omega
It is well known that estimating the pairwise velocity of galaxies, v_{12},
from the redshift space galaxy correlation function is difficult because this
method is highly sensitive to the assumed model of the pairwise velocity
dispersion. Here we propose an alternative method to estimate v_{12} directly
from peculiar velocity samples, which contain redshift-independent distances as
well as galaxy redshifts. In contrast to other dynamical measures which
determine beta = sigma_8 x Omega^{0.6}, our method can provide an estimate of
(sigma_8)^2 x Omega^{0.6} for a range of sigma_8 (here Omega is the
cosmological mass density parameter while sigma_8 is the standard normalization
parameter for the spectrum of matter density fluctuations). We demonstrate how
to measure this quantity from realistic catalogues.Comment: 8 pages of text, 4 figures Subject headings: Cosmology: theory -
observation - peculiar velocities: large scale flows Last name of one of the
authors was misspelled. It is now corrected. Otherwise the manuscript is
identical to its original versio
On the streaming motions of haloes and galaxies
A simple model of how objects of different masses stream towards each other
as they cluster gravitationally is described. The model shows how the mean
streaming velocity of dark matter particles is related to the motions of the
parent dark matter haloes. It also provides a reasonably accurate description
of how the pairwise velocity dispersion of dark matter particles differs from
that of the parent haloes. The analysis is then extended to describe the
streaming motions of galaxies. This shows explicitly that the streaming motions
measured in a given galaxy sample depend on how the sample was selected, and
shows how to account for this dependence on sample selection. In addition,we
show that the pairwise dispersion should also depend on sample type. Our model
predicts that, on small scales, redshift space distortions should affect red
galaxies more strongly than blue.Comment: 10 pages, submitted to MNRA
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