A International Centre for Radio Astronomy Research, M468, University of Western Australia, Crawley, WA 6009, Australia B Australian Astronomical Observatory, P.O. Box 296, Epping NSW 1710, Australia C CSIRO Astronomy & Space Sciences, Australia Telescope National Facility, P.O. Box 76, Epping NSW 1710, Australia D Sydney Institute for Astronomy, School of Physics, The University of Sydney, NSW...

Astronomical images have some rather unusual characteristics that make many existing image compression techniques either ine ective or inapplicable. A typical image consists of a nearly at background sprinkled with point sources and occasional extended sources. The images are often noisy, so that lossless compression does not work very well; furthermore, the images are usually subjected to stri...

The Large Synoptic Survey Telescope (LSST) will catalog billions of astronomical objects and trillions of sources, all of which will be stored and managed by a database management system. One of the main challenges is real-time alert generation. To generate alerts, up to 100K new difference detections have to be cross-correlated with the huge historical catalogs, and then further processed to p...

For off-zenith observations with ground-based astronomical telescopes, the effect of atmospheric dispersion relative to diffraction on image size increases with telescope diameter. Correction of atmospheric dispersion in extremely large telescopes (ELTs) might become critical. A common solution for ELTs is to use linear atmospheric dispersion correctors (ADCs). In spite of their simplicity, the...

We report on the first astronomical observations with a photon counting pixel detector that provides arrival time-(δt = 100ns) and energy-(δE γ ≤ 0.15 eV) resolved measurements from the near IR through the near UV. Our test observations were performed by coupling this Transition Edge Sensor (TES) device to a 0.6m telescope; we have obtained the first simultaneous optical near-IR phase-resolved ...

Large gravitational wave interferometric detectors, like Virgo and LIGO, demonstrated the capability to reach their design sensitivity, but to transform these machines into an effective observational instrument for gravitational wave astronomy a large improvement in sensitivity is required. Advanced detectors in the near future and third-generation observatories in more than one decade will ope...

The Infrared Astronomical Satellite (IRAS) was successfully launched on 25 January 1983 and terminated science data acquisition on 22 November 1983. The in -orbit performance of the telescope has been described in two previous papers in these proceedings.1'2 A previous description of very preliminary scientific results from the mission has been given in these proceedings3, while far more extens...

We report the first observations of an astronomical object using a superconducting tunnel junction (STJ) device, a pixel detector with intrinsic energy resolution in the optical wavelength range. The Crab pulsar was observed using a 6 × 6 array of Tantalum STJs at the 4.2-m William Herschel Telescope on La Palma. Each array element provides photon counting capability recording up to ∼ 10 3 phot...

Abstract CASA, the Common Astronomy Software Applications, is primary data processing software for Atacama Large Millimeter/submillimeter Array (ALMA) and Karl G. Jansky Very (VLA), frequently used also other radio telescopes. The CASA can handle from single-dish, aperture-synthesis, Long Baseline Interferometery (VLBI) One of its core functionalities to support calibration imaging pipelines AL...

This paper considers the problem of change detection using local distributed eigen monitoring algorithms for next generation of astronomy petascale data pipelines such as the Large Synoptic Survey Telescopes (LSST). This telescope will take repeat images of the night sky every 20 seconds, thereby generating 30 terabytes of calibrated imagery every night that will need to be coanalyzed with othe...