Be Stars in and Around Young Clusters in the Magellanic Clouds

S. C. Keller; P. R. Wood; M. S. Bessell

doi:10.1051/aas:1999151

Be Stars in and Around Young Clusters in the Magellanic Clouds

S. C. Keller^*, P. R. Wood, M. S. Bessell

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

77 Citations (Scopus)

Abstract

We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band Hα CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing Hα emission strength.

Original language	English
Pages (from-to)	489-503
Number of pages	15
Journal	Astronomy and Astrophysics Supplement Series
Volume	134
Issue number	3
DOIs	https://doi.org/10.1051/aas:1999151
Publication status	Published - 1999

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@article{078aabb302ce4134ba1ccca174610851,

title = "Be Stars in and Around Young Clusters in the Magellanic Clouds",

abstract = "We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band Hα CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing Hα emission strength.",

keywords = "Galaxies: Magellanic Clouds, Galaxies: clusters, Stars: Be, Stars: emission-line",

author = "Keller, {S. C.} and Wood, {P. R.} and Bessell, {M. S.}",

year = "1999",

doi = "10.1051/aas:1999151",

language = "English",

volume = "134",

pages = "489--503",

journal = "Astronomy and Astrophysics Supplement Series",

issn = "0365-0138",

publisher = "EDP Sciences",

number = "3",

}

TY - JOUR

T1 - Be Stars in and Around Young Clusters in the Magellanic Clouds

AU - Keller, S. C.

AU - Wood, P. R.

AU - Bessell, M. S.

PY - 1999

Y1 - 1999

N2 - We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band Hα CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing Hα emission strength.

AB - We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band Hα CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing Hα emission strength.

KW - Galaxies: Magellanic Clouds

KW - Galaxies: clusters

KW - Stars: Be

KW - Stars: emission-line

UR - http://www.scopus.com/inward/record.url?scp=33746996623&partnerID=8YFLogxK

U2 - 10.1051/aas:1999151

DO - 10.1051/aas:1999151

M3 - Article

SN - 0365-0138

VL - 134

SP - 489

EP - 503

JO - Astronomy and Astrophysics Supplement Series

JF - Astronomy and Astrophysics Supplement Series

IS - 3

ER -

Be Stars in and Around Young Clusters in the Magellanic Clouds

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