Determining the Physical Parameters of Massive Stars in the SMC and LMC

Details Determining the Physical Parameters of Massive Stars in the SMC and LMC Determining the Physical Parameters of Massive Stars in the SMC and LMC

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21542709n&link_type=abstract

American Astronomical Society, AAS Meeting #215, #427.09; Bulletin of the American Astronomical Society, Vol. 42, p.344

Astronomy and Astrophysics

Astronomy

1

Scientific paper

There are currently two main programs used to model the optical spectra of O stars: FASTWIND (Puls et al. 2005) and CMFGEN (Hillier et al. 2003). Both do an adequate job of matching the observed spectra but the modeling has never been done on the same spectra and the results compared. By modeling six stars in the SMC and LMC using CMFGEN that had previously been modeled by Massey et al. (2004, 2005, 2009) using FASTWIND, we were able to make direct comparisons between the results of the two modeling programs. The agreement we have found are usually within the uncertainties of our determination, and both FASTWIND and CMFGEN generally did an exemplary job at fitting the spectra. No systematics have been found in the effective temperatures, although in some individual cases the differences are larger than we expect, as much as 6%. There may be a small (0.1-0.15 dex) systematic difference in the derived surface gravities, with the CMFGEN values larger, and we are investigating possible causes. Additional tests are ongoing and will be described.
This work was partially supported by NASA through grant AR-11270 from the Space Telescope Science Institute, and by the National Science Foundation REU grant AST-0453611.

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