This paper explores the nature of creative composition particularly as it applies to dance, and describes the development of interactive computer based tools to assist the composer. The hierarchical nature of the composition process calls for an interface which allows the composer the flexibility to move back and forth between alternate views and conceptual levels of abstraction.COMPOSE, an interactive system for the composition of dance has been implemented on Silicon Graphics and Apple workstations. The user visually composes in space and in time using menus of postures and sequences. Paths can be edited and an animation of the dance composition allows the final result to be evaluated.
We present WALLABY pilot data release 1, the first public release of H i pilot survey data from the Wide-field ASKAP L-band Legacy All-sky Blind Survey (WALLABY) on the Australian Square Kilometre Array Pathfinder. Phase 1 of the WALLABY pilot survey targeted three
$60\,\mathrm{deg}^{2}$
regions on the sky in the direction of the Hydra and Norma galaxy clusters and the NGC 4636 galaxy group, covering the redshift range of
$z \lesssim 0.08$
. The source catalogue, images and spectra of nearly 600 extragalactic H i detections and kinematic models for 109 spatially resolved galaxies are available. As the pilot survey targeted regions containing nearby group and cluster environments, the median redshift of the sample of
$z \approx 0.014$
is relatively low compared to the full WALLABY survey. The median galaxy H i mass is
$2.3 \times 10^{9}\,{\rm M}_{{\odot}}$
. The target noise level of
$1.6\,\mathrm{mJy}$
per 30′′ beam and
$18.5\,\mathrm{kHz}$
channel translates into a
$5 \sigma$
H i mass sensitivity for point sources of about
$5.2 \times 10^{8} \, (D_{\rm L} / \mathrm{100\,Mpc})^{2} \, {\rm M}_{{\odot}}$
across 50 spectral channels (
${\approx} 200\,\mathrm{km \, s}^{-1}$
) and a
$5 \sigma$
H i column density sensitivity of about
$8.6 \times 10^{19} \, (1 + z)^{4}\,\mathrm{cm}^{-2}$
across 5 channels (
${\approx} 20\,\mathrm{km \, s}^{-1}$
) for emission filling the 30′′ beam. As expected for a pilot survey, several technical issues and artefacts are still affecting the data quality. Most notably, there are systematic flux errors of up to several 10% caused by uncertainties about the exact size and shape of each of the primary beams as well as the presence of sidelobes due to the finite deconvolution threshold. In addition, artefacts such as residual continuum emission and bandpass ripples have affected some of the data. The pilot survey has been highly successful in uncovering such technical problems, most of which are expected to be addressed and rectified before the start of the full WALLABY survey.
We present, as a case study, a description of the partnership between an observatory (JCMT) and a data centre (CADC) that led to the development of the JCMT Science Archive (JSA). The JSA is a successful example of a service designed to use Virtual Observatory (VO) technologies from the start. We describe the motivation, process and lessons learned from this approach.
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