99 research outputs found
A GPU based real-time software correlation system for the Murchison Widefield Array prototype
Modern graphics processing units (GPUs) are inexpensive commodity hardware
that offer Tflop/s theoretical computing capacity. GPUs are well suited to many
compute-intensive tasks including digital signal processing.
We describe the implementation and performance of a GPU-based digital
correlator for radio astronomy. The correlator is implemented using the NVIDIA
CUDA development environment. We evaluate three design options on two
generations of NVIDIA hardware. The different designs utilize the internal
registers, shared memory and multiprocessors in different ways. We find that
optimal performance is achieved with the design that minimizes global memory
reads on recent generations of hardware.
The GPU-based correlator outperforms a single-threaded CPU equivalent by a
factor of 60 for a 32 antenna array, and runs on commodity PC hardware. The
extra compute capability provided by the GPU maximises the correlation
capability of a PC while retaining the fast development time associated with
using standard hardware, networking and programming languages. In this way, a
GPU-based correlation system represents a middle ground in design space between
high performance, custom built hardware and pure CPU-based software
correlation.
The correlator was deployed at the Murchison Widefield Array 32 antenna
prototype system where it ran in real-time for extended periods. We briefly
describe the data capture, streaming and correlation system for the prototype
array.Comment: 11 pages, to appear in PAS
Lensview: Software for modelling resolved gravitational lens images
We have developed a new software tool, Lensview, for modelling resolved
gravitational lens images. Based on the LensMEM algorithm, the software finds
the best fitting lens mass model and source brightness distribution using a
maximum entropy constraint. The method can be used with any point spread
function or lens model. We review the algorithm and introduce some significant
improvements. We also investigate and discuss issues associated with the
statistical uncertainties of models and model parameters and the issues of
source plane size and source pixel size.
We test the software on simulated optical and radio data to evaluate how well
lens models can be recovered and with what accuracy. For optical data, lens
model parameters can typically be recovered with better than 1% accuracy and
the degeneracy between mass ellipticity and power law is reduced. For radio
data, we find that systematic errors associated with using processed radio
maps, rather than the visibilities, are of similar magnitude to the random
errors. Hence analysing radio data in image space is still useful and
meaningful.
The software is applied to the optical arc HST J15433+5352 and the radio ring
MG1549+3047 using a simple elliptical isothermal lens model. For HST
J15433+5352, the Einstein radius is 0.525" +/- 0.015 which probably includes a
substantial convergence contribution from a neighbouring galaxy. For
MG1549+3047, the model has Einstein radius 1.105" +/- 0.005 and core radius
0.16" 0.03. The total mass enclosed in the critical radius is 7.06 x 10^{10}
Solar masses for our best model.Comment: 21 pages, 24 figures, appearing in MNRAS. Software available from
http://www.cfa.harvard.edu/~rwayth/lensview/Lensview_Home.htm
The lens and source of the optical Einstein ring gravitational lens ER 0047-2808
(Abridged) We perform a detailed analysis of the optical gravitational lens
ER 0047-2808 imaged with WFPC2 on the Hubble Space Telescope. Using software
specifically designed for the analysis of resolved gravitational lens systems,
we focus on how the image alone can constrain the mass distribution in the lens
galaxy. We find the data are of sufficient quality to strongly constrain the
lens model with no a priori assumptions about the source. Using a variety of
mass models, we find statistically acceptable results for elliptical
isothermal-like models with an Einstein radius of 1.17''. An elliptical
power-law model (Sigma \propto R^-beta) for the surface mass density favours a
slope slightly steeper than isothermal with beta = 1.08 +/- 0.03. Other models
including a constant M/L, pure NFW halo and (surprisingly) an isothermal sphere
with external shear are ruled out by the data. We find the galaxy light profile
can only be fit with a Sersic plus point source model. The resulting total
M/L_B contained within the images is 4.7 h_65 +/-0.3. In addition, we find the
luminous matter is aligned with the total mass distribution within a few
degrees. The source, reconstructed by the software, is revealed to have two
bright regions, with an unresolved component inside the caustic and a resolved
component straddling a fold caustic. The angular size of the entire source is
approx. 0.1'' and its (unlensed) Lyman-alpha flux is 3 x 10^-17 erg/s/cm^2.Comment: 13 pages, 5 figures. Revised version accepted for publication in
MNRA
Direction-Dependent Polarised Primary Beams in Wide-Field Synthesis Imaging
The process of wide-field synthesis imaging is explored, with the aim of
understanding the implications of variable, polarised primary beams for
forthcoming Epoch of Reionisation experiments. These experiments seek to detect
weak signatures from redshifted 21cm emission in deep residual datasets, after
suppression and subtraction of foreground emission. Many subtraction algorithms
benefit from low side-lobes and polarisation leakage at the outset, and both of
these are intimately linked to how the polarised primary beams are handled.
Building on previous contributions from a number of authors, in which
direction-dependent corrections are incorporated into visibility gridding
kernels, we consider the special characteristics of arrays of fixed dipole
antennas operating around 100-200 MHz, looking towards instruments such as the
Square Kilometre Array (SKA) and the Hydrogen Epoch of Reionization Arrays
(HERA). We show that integrating snapshots in the image domain can help to
produce compact gridding kernels, and also reduce the need to make complicated
polarised leakage corrections during gridding. We also investigate an
alternative form for the gridding kernel that can suppress variations in the
direction-dependent weighting of gridded visibilities by 10s of dB, while
maintaining compact support.Comment: 15 pages, 4 figures. Accepted for publication in JA
Spectral performance of Square Kilometre Array Antennas - II. Calibration performance
We test the bandpass smoothness performance of two prototype Square Kilometre Array (SKA) SKA1-Low log-periodic dipole antennas, SKALA2 and SKALA3 ('SKA Log-periodic Antenna'), and the current dipole from the Murchison Widefield Array (MWA) precursor telescope. Throughout this paper, we refer to the output complex-valued voltage response of an antenna when connected to a low-noise amplifier, as the dipole bandpass. In Paper I, the bandpass spectral response of the log-periodic antenna being developed for the SKA1-Low was estimated using numerical electromagnetic simulations and analysed using low-order polynomial fittings, and it was compared with the HERA antenna against the delay spectrum metric. In this work, realistic simulations of the SKA1-Low instrument, including frequencydependent primary beam shapes and array configuration, are used with a weighted leastsquares polynomial estimator to assess the ability of a given prototype antenna to perform the SKA Epoch of Reionisation (EoR) statistical experiments. This work complements the ideal estimator tolerances computed for the proposed EoR science experiments in Trott & Wayth, with the realized performance of an optimal and standard estimation (calibration) procedure. With a sufficient sky calibration model at higher frequencies, all antennas have bandpasses that are sufficiently smooth to meet the tolerances described in Trott & Wayth to perform the EoR statistical experiments, and these are primarily limited by an adequate sky calibration model and the thermal noise level in the calibration data. At frequencies of the Cosmic Dawn, which is of principal interest to SKA as one of the first next-generation telescopes capable of accessing higher redshifts, the MWA dipole and SKALA3 antenna have adequate performance, while the SKALA2 design will impede the ability to explore this era
H1517+656: the Birth of a BL Lac Object?
H1517+656 is an unusual source, even for a BL Lac object. It is one of the
most luminous BL Lacs known, with extreme emission properties at radio,
optical, and X-ray frequencies. Furthermore, in our WFPC2 snapshot survey we
discovered a series of peculiar arcs describing a 2.4 arcsec radius ring
surrounding the source. This paper describes follow-up observations with
additional WFPC2 bands and the STIS longpass filter, which have revealed this
structure to be the remnants of a very recent galaxy merger. Population
synthesis modelling has shown that regions of the arcs have stellar populations
with age < 20 Myrs. Additionally, the circularity of the arcs indicates that
the plane of the collision and hence accretion is very close to the plane of
the sky. Given that BL Lac jets are thought to be aligned with the line of
sight, this observation may provide a direct link between the transfer of
angular momentum in an interaction and the generation of a radio source.Comment: 29 pages, 9 figures, accepted for publication in Ap
Spectral calibration requirements of radio interferometers for epoch of reionisation science with the SKA
Spectral features introduced by instrumental chromaticity of radio interferometers have the potential to negatively impact the ability to perform Epoch of Reionisation and Cosmic Dawn (EoR/CD) science. We describe instrument calibration choices that influence the spectral characteristics of the science data, and assess their impact on EoR/CD statistical and tomographic experiments. Principally, we consider the intrinsic spectral response of the antennas, embedded within a complete frequency-dependent primary beam response, and instrument sampling. The analysis is applied to the proposed SKA1-Low EoR/CD experiments. We provide tolerances on the smoothness of the SKA station primary beam bandpass, to meet the scientific goals of statistical and tomographic (imaging) of EoR/CD programs. Two calibration strategies are tested: (1) fitting of each fine channel independently, and (2) fitting of an nth-order polynomial for each ~ 1 MHz coarse channel with (n+1)th-order residuals (n = 2, 3, 4). Strategy (1) leads to uncorrelated power in the 2D power spectrum proportional to the thermal noise power, thereby reducing the overall sensitivity. Strategy (2) leads to correlated residuals from the fitting, and residual signal power with (n+1)th-order curvature. For the residual power to be less than the thermal noise, the fractional amplitude of a fourth-order term in the bandpass across a single coarse channel must be <2.5% (50 MHz), <0.5% (150 MHz), <0.8% (200 MHz). The tomographic experiment places constraints on phase residuals in the bandpass. We find that the root-mean-square variability over all stations of the change in phase across any fine channel (4.578 kHz) should not exceed 0.2 degrees
Real-Time Adaptive Event Detection in Astronomical Data Streams
A new generation of observational science instruments is dramatically increasing collected data volumes in a range of fields. These instruments include the Square Kilometer Array (SKA), Large Synoptic Survey Telescope (LSST), terrestrial sensor networks, and NASA satellites participating in "decadal survey"' missions. Their unprecedented coverage and sensitivity will likely reveal wholly new categories of unexpected and transient events. Commensal methods passively analyze these data streams, recognizing anomalous events of scientific interest and reacting in real time. Here, the authors report on a case example: Very Long Baseline Array Fast Transients Experiment (V-FASTR), an ongoing commensal experiment at the Very Long Baseline Array (VLBA) that uses online adaptive pattern recognition to search for anomalous fast radio transients. V-FASTR triages a millisecond-resolution stream of data and promotes candidate anomalies for further offline analysis. It tunes detection parameters in real time, injecting synthetic events to continually retrain itself for optimum performance. This self-tuning approach retains sensitivity to weak signals while adapting to changing instrument configurations and noise conditions. The system has operated since July 2011, making it the longest-running real-time commensal radio transient experiment to date
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