The blue to red supergiant ratio in young clusters at various metallicities

Details The blue to red supergiant ratio in young clusters at various metallicities The blue to red supergiant ratio in young clusters at various metallicities

2002-02-26

arxiv.org/abs/astro-ph/0202478v1

Astronomy and Astrophysics

Astrophysics

7 pages, 2 figures. accepted for publication in A&A

Scientific paper

10.1051/0004-6361:20020262

We present new determinations of the blue to red supergiant ratio ($B/R$) in young open clusters at various metallicities. For this purpose, we examine the HR diagrams of 45 clusters in the Galaxy and of 4 clusters in the Magellanic Clouds. The identification of supergiants is based on spectroscopic measurements (with photometric counts to check the results). The new counts confirm the increase of the $B/R$ ratio when the metallicity increases with the following normalized relation : $\frac{B/R}{(B/R)_{\odot}} \cong 0.05\cdot e^{3 \frac{Z}{Z_{\odot}}}$, where $Z_{\odot}=0.02$ and $(B/R)_{\odot}$ is the value of $B/R$ at $Z_{\odot}$ which depends on the definition of $B$ and $R$ and on the age interval considered (e.g. for spectroscopic counts including clusters with $\log age$ between 6.8 and 7.5, $(B/R)_{\odot}\cong3$ when $B$ includes O, B and A supergiants).

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