Massive Stars in the SGR 1806-20 Cluster

Details Massive Stars in the SGR 1806-20 Cluster Massive Stars in the SGR 1806-20 Cluster

2005-01-25

arxiv.org/abs/astro-ph/0501560v3

Astrophys.J. 622 (2005) L49-L52

Astronomy and Astrophysics

Astrophysics

ApJ Letters, accepted ScI Eprint #1640, added acknowledgement of Gaensler et al. (2005) http://arxiv.org/abs/astro-ph/0501563

Scientific paper

10.1086/429159

We report the discovery of additional hot and massive stars in the cluster surrounding the soft gamma repeater SGR 1806-20, based upon UKIRT and Keck near-infrared spectroscopy. Of the newly identified stars, three are Wolf-Rayet stars of types WC8, WN6, and WN7, and a fourth star is an OB supergiant. These three stars, along with four previously discovered, imply a cluster age of \~3.0-4.5 Myr, based on the presence of WC stars and the absence of red supergiants. Assuming coevality, this age suggests that the progenitor of SGR 1806-20 had an initial mass greater than ~50 Msun. This is consistent with the suggestion that SGRs are post-supernovae end states of massive progenitors, and may suggest that only massive stars evolve into magnetars that produce SGRs. It also suggests that very massive stars can evolve into neutron stars, not just black holes, as recently predicted by theory. The cluster age also provides constraints on the very high mass object, LBV 1806-20.

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