A Star Formation Scenario for the Explanation of Seyfert Type 2 Activity: MK 348
In the frame of the VSF scenario, a young star cluster a few Myr old contributing about 8% to the total light at Hβ is required in order to reproduce the observed emission line spectrum of Mk 348 (García-Vargas et al 1989). This cluster should dominate the light shortward of 4000 Å. We have synthesized the SED of such a cluster using a homogeneous set of evolutionary tracks for stars of solar composition with masses between 1 and 120 M⊙ (Maeder 1987 and private communication). The most massive of these stars (m ≥ 60 M⊙) evolve to the left of the HR diagram and are identified with the “warmers” (Terlevich &, Melnick 1985). Emergent stellar fluxes have been taken from the model atmospheres by Clegg et al (1987) for stars with T eff ≥ 50000 K and Kurucz (1979) for stars with 5000 K ≤ T eff ≤ 50000 K. For stars of T eff ≤ 5000 K the stellar atlas by Jacobi et al (1984) has been used. The cluster is assumed to form in a burst with an IMF with a Salpeter slope. The computed spectrum is shown in Fig. 1 (solid line) in a logv logF v , scale.
KeywordsStar Formation Star Formation Region Evolutionary Track Royal Greenwich Observatory Small Magellanic Cloud
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