Far-IR Emission Surrounding G34.3+0.2

Details Far-IR Emission Surrounding G34.3+0.2 Far-IR Emission Surrounding G34.3+0.2

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...198.5904c&link_type=abstract

American Astronomical Society, 198th AAS Meeting, #59.04; Bulletin of the American Astronomical Society, Vol. 33, p.872

Astronomy and Astrophysics

Astronomy

Scientific paper

The complex of radio sources G34.3+0.2 A, B, C (the "cometary'' UC HII region), and D are associated with one of the brightest IRAS sources, IRAS 18507+1110. The IRAS PSC position is offset 26 \arcsec SE of component C, towards component D. In contrast, we have observed peaks at 47 and 95 μ m from the KAO which are consistent with the position of C, within their accuracy. IRAS HIRES images show that the 12 and 25 μ m peaks are centered on D, while the 60 and 100 μ m peaks are on centered C, with extended emission covering D. Our KAO maps at 47 and 95 μ m show sharp central peaks with extended emission surrounding them. The extended emission at 47 μ m is similiar in extent to that at 95 μ m, which is unusual. A mid-ir spectrum from the ISO Archive in a 24 \arcsec beam centered on the PSC position shows PAH features. In contrast, Faison et al. (1998) presented a spectrum in a 9 \arcsec beam centered on C which shows very deep silicate absorption. Campbell et al. (2000) modeled mid-ir emission in narrowband images from C as due to hot dust surrounded by a cooler silicate absorbing cloud. We propose that the IRAS 12 and 25 μ m emissions, and part of the IRAS 60 μ m emission are due to PAHs and small grains. The sharp emission peaks at 47 and 95 μ m are due to silicate dust grains, perhaps the same grains which are seen in absorption in the models of Campbell et al. for mid-ir emission from component C. The nature of the extended emission seen on the KAO at 47 and 95 μ m is unclear. This work was supported by NASA Grants 2-67 and 2-546 and by Colby College. Campbell, M.F. et al. 2000, ApJ, 536, 816 Faison, M. et al. 1998, ApJ, 500, 280

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