NIR properties of Be stars in star clusters in the Magellanic Clouds

One of the many components of the software systems used to operate the Hubble Space Telescope (HST) are the applications packages for calibration and scientific data analysis. Although of great importance to the observer, data analysis is at the end of the line in this extensive system. Calibration is a more integral part of telescope operations, in that the STScI will provide all HST observers with nominally calibrated data. However, it is recognized that many observers will wish to verify or modify the calibration themselves, so that the calibration software is also an integral part of the data analysis system. STSDAS — the Space Telescope Science Data Analysis System — is the software tool kit that allows HST observers to calibrate, reduce, and analyze HST observations.

STSDAS: The Space Telescope Science Data Analysis System

Using neural networks for the detection, extraction and pre-classification of spectra in objective prism images

MIDAS will be the on-line image processing system used at ESO’s Very large Telescope (VLT). As the first step on its way to the telescopes, MIDAS will soon replace the IHAP system at ESO’s New Technology Telescope (NTT) when the NTT will be used also under remote control from ESO Headquarters in Garching. Observers will then have all utilities of a modern astronomical data analysis system at their finger tips, at the telescope.

MIDAS on-Line at the Telescope

Spectral types of stars for an extended area (1200 sq arcmin) of the SMC, containing the associations NGC456, NGC460 a, b and NGC465 have been derived here. High-quality UJ and YJ film copies of objective prism plates taken with the 1.2-m UK Schmidt telescope were used. The medium dispersion spectral (830 A/mm) were digitized with a PDS microdensitometer and spectra types of stars were obtained down to about 16.5 mag. A computer interactive method of reduction has been developed, and the spectral types obtained are accurate to 0.3 spectral subtypes. Spectral classification for the low (2440 A/mm) dispersion spectra down to 18.5 mag was carried out visually using a binocular microscope. The frequency distributions of stars in the associations region, after subtracting the field stars, have revealed that only blue main sequence stars are their members.

Spectral types of stars in the SMC associations NGC456, NGC460a, b and NGC465

An image display interface for astronomical image processing

The aim of this paper is to study the distribution of spectral types of the stellar content in an outlying region (wing) of the Small Magellanic Cloud (SMC) which contains the brightest early type stars and therefore the most massive in this galaxy.

An Age Estimate for the NGC456, 460 and 465 SMC Constellation

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Spectral types of stars in the SMC associations NGC456, NGC460a, b and NGC465

An image display interface for astronomical image processing

An Age Estimate for the NGC456, 460 and 465 SMC Constellation