Modeling of Far-IR Emission From G34.3+0.2

Details Modeling of Far-IR Emission From G34.3+0.2 Modeling of Far-IR Emission From G34.3+0.2

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...198.5903c&link_type=abstract

American Astronomical Society, 198th AAS Meeting, #59.03; Bulletin of the American Astronomical Society, Vol. 33, p.871

Astronomy and Astrophysics

Astronomy

Scientific paper

Photometric scans at 47 and 95 μ m made on the KAO of the bright source centered on G34.3+0.2 are presented and analyzed. The 47 and 95 μ m scans are similar, showing sharp central peaks and very similar diffuse extended emission wings. Maximum entropy method deconvolutions indicate that the peaks are quite compact with FWHM values of 11 by 14 \arcsec and 18 by 20 \arcsec at 47 and 95 μ m respectively. The Egan, Leung, & Spagna (1988) radiative transfer code has been used to model the emission from the central peak at 47 and 95 μ m as Draine and Lee (1985) dust surrounding the O star(s) which ionize the ultracompact HII regions A, B, and C. The emission optical depth in the far-ir model is comparable to the amount of dust assumed to be in absorption in the models of mid-ir emission from G34.3+02C presented by Campbell et al. (2000). This work was supported by NASA Grants 2-67 & 2-546 and by Colby College. Campbell, M.F. et al. 2000, ApJ, 536, 816 Draine, B.T. & Lee, H.M. 1984, ApJ, 289, 89 Egan, M.P., Leung, C.M., & Spagna, G.F. 1988, CPC, 48, 271

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