39 research outputs found
Theory and Simulations of Refractive Substructure in Resolved Scatter-Broadened Images
At radio wavelengths, scattering in the interstellar medium distorts the
appearance of astronomical sources. Averaged over a scattering ensemble, the
result is a blurred image of the source. However, Narayan & Goodman (1989) and
Goodman & Narayan (1989) showed that for an incomplete average, scattering
introduces refractive substructure in the image of a point source that is both
persistent and wideband. We show that this substructure is quenched but not
smoothed by an extended source. As a result, when the scatter-broadening is
comparable to or exceeds the unscattered source size, the scattering can
introduce spurious compact features into images. In addition, we derive
efficient strategies to numerically compute realistic scattered images, and we
present characteristic examples from simulations. Our results show that
refractive substructure is an important consideration for ongoing missions at
the highest angular resolutions, and we discuss specific implications for
RadioAstron and the Event Horizon Telescope.Comment: Equation numbering in appendix now matches published version. Two
minor typos correcte
Sub-Microarcsecond Astrometry and New Horizons in Relativistic Gravitational Physics
Attaining the limit of sub-microarcsecond optical resolution will completely
revolutionize fundamental astrometry by merging it with relativistic
gravitational physics. Beyond the sub-microarcsecond threshold, one will meet
in the sky a new population of physical phenomena caused by primordial
gravitational waves from early universe and/or different localized astronomical
sources, space-time topological defects, moving gravitational lenses, time
variability of gravitational fields of the solar system and binary stars, and
many others. Adequate physical interpretation of these yet undetectable
sub-microarcsecond phenomena can not be achieved on the ground of the
"standard" post-Newtonian approach (PNA), which is valid only in the near-zone
of astronomical objects having a time-dependent gravitational field. We
describe a new, post-Minkowskian relativistic approach for modeling astrometric
observations having sub-microarcsecond precision and briefly discuss the
light-propagation effects caused by gravitational waves and other phenomena
related to time-dependent gravitational fields. The domain of applicability of
the PNA in relativistic space astrometry is explicitly outlined.Comment: 5 pages, the talk given at the IAU Colloquium 180 "Towards Models and
Constants for Sub-Microarcsecond Astrometry", Washington DC, March 26 - April
2, 200
Optimal Correlation Estimators for Quantized Signals
Using a maximum-likelihood criterion, we derive optimal correlation
strategies for signals with and without digitization. We assume that the
signals are drawn from zero-mean Gaussian distributions, as is expected in
radio-astronomical applications, and we present correlation estimators both
with and without a priori knowledge of the signal variances. We demonstrate
that traditional estimators of correlation, which rely on averaging products,
exhibit large and paradoxical noise when the correlation is strong. However, we
also show that these estimators are fully optimal in the limit of vanishing
correlation. We calculate the bias and noise in each of these estimators and
discuss their suitability for implementation in modern digital correlators.Comment: 8 Pages, 3 Figures, Submitted to Ap
The Multi-Component Nature of the Vela Pulsar Nonthermal X-ray Spectrum
We report on our analysis of a 274 ks observation of the Vela pulsar with the
Rossi X-Ray Timing Explorer (RXTE). The double-peaked, pulsed emission at 2 -
30 keV, which we had previously detected during a 93 ks observation, is
confirmed with much improved statistics. There is now clear evidence, both in
the spectrum and the light curve, that the emission in the RXTE band is a blend
of two separate non-thermal components. The spectrum of the harder component
connects smoothly with the OSSE, COMPTEL and EGRET spectrum and the peaks in
the light curve are in phase coincidence with those of the high-energy light
curve. The spectrum of the softer component is consistent with an extrapolation
to the pulsed optical flux, and the second RXTE pulse is in phase coincidence
with the second optical peak. In addition, we see a peak in the 2-8 keV RXTE
pulse profile at the radio phase.Comment: 12 pages, 3 figures, accepted for publication in Astrophysical
Journa
Gravitational Radiation and Very Long Baseline Interferometry
Gravitational waves affect the observed direction of light from distant
sources. At telescopes, this change in direction appears as periodic variations
in the apparent positions of these sources on the sky; that is, as proper
motion. A wave of a given phase, traveling in a given direction, produces a
characteristic pattern of proper motions over the sky. Comparison of observed
proper motions with this pattern serves to test for the presence of
gravitational waves. A stochastic background of waves induces apparent proper
motions with specific statistical properties, and so, may also be sought. In
this paper we consider the effects of a cosmological background of
gravitational radiation on astrometric observations. We derive an equation for
the time delay measured by two antennae observing the same source in an
Einstein-de Sitter spacetime containing gravitational radiation. We also show
how to obtain similar expressions for curved Friedmann-Robertson-Walker
spacetimes.Comment: 31 pages plus 3 separate figures, plain TeX, submitted to Ap