Quantitative analysis of STIS spectra of NGC 2363-V1

Details Quantitative analysis of STIS spectra of NGC 2363-V1 Quantitative analysis of STIS spectra of NGC 2363-V1

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..332..157p&link_type=abstract

The Fate of the Most Massive Stars, ASP Conference Series, Vol. 332, Proceedings of the conference held 23-28 May, 2004 in Grand

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We obtained a spectroscopic follow-up of V1 with the Hubble Space Telescope, from 1997 to 2004. The data sets are composed of two spectra in the UV (with gratings G140L and G203L) and two in the visible (G430L, G750L). We also obtained medium resolution spectra around Hα (G750M) and around Hγ + HeI λ4471 (G430M; for 2001, 2003 and 2004 only). The data were processed with the standard HST pipeline. However, the highly non-uniform surrounding nebula contaminates the stellar spectrum. So, background subtraction was redone properly with standard IRAF tasks.
We used CMFGEN, the iterative, line-blanketed technique of Hillier & Miller (1998, ApJ, 496, 407). It solves the transfer equation in the co-moving frame subject to statistical and radiative equilibrium in an expanding, steady-state atmosphere. We relied on stellar continuum distribution, from which the stellar temperature and luminosity are derived, and Hα (plus Hγ/HeI 4471 when available), which is an excellent tracer of mass-loss rate and wind velocity. We used some fixed parameters; H/He=4 by number, Z=0.20Z&sun; and a clumping filling factor of 0.3. We calculated grids of models at different temperatures and mass loss rates and various E(B-V). The difficulty of fitting simultaneously the 2003 UV continuum and the Hα profile for low extinction suggests that E(B-V)=0.13 for V1, in rough agreement with other estimates for this region.

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