Be-Star Surveys with CCD Photometry - Part One - NGC330 and its High Be-Star Content

Details Be-Star Surveys with CCD Photometry - Part One - NGC330 and its High Be-Star Content Be-Star Surveys with CCD Photometry - Part One - NGC330 and its High Be-Star Content

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...254l...5g&link_type=abstract

Astronomy and Astrophysics, Vol.254, NO. FEB(I), P. L5, 1992

Astronomy and Astrophysics

Astrophysics

56

Clusters: Globular, Galaxies: Magellanic Clouds, Observing Methods, Ccd Photometry, Stars: Be, Stars: Classification

Scientific paper

We present a photometric method for identifying Be stars that is particularly suitable for work in star clusters. Our method uses three filters: Hα, and Strömgren b and y. Be stars are distinguished from normal B stars by their location in the two-colour diagram (b-y), (Hα-y).
Testing this method in the young SMC cluster NGC 330, we strengthen the spectroscopic result of Feast. We find that the majority of the B stars in NGC 330 are in fact Be stars. NGC 330 turns out to be the cluster richest known in Be stars.

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