Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.8206h&link_type=abstract
American Astronomical Society, 185th AAS Meeting, #82.06; Bulletin of the American Astronomical Society, Vol. 26, p.1453
Astronomy and Astrophysics
Astronomy
Scientific paper
In an ongoing study of star formation regions in the near (1-5microns) infrared, we present J (1.2microns, H (1.65microns), K (2.23microns), and 3.3microns broadband images as well as Brgamma (n = 7->4, 2.166microns) and Bralpha (n = 5->4, 4.052microns) hydrogen recombination line images, H_2 (1-0 S(1), 2.122microns) line images, and 3.29microns unidentified dust feature emission images of the triple HII region S255-2, at a plate scale of ~ 0.33'' per pixel. The Bralpha and Brgamma emission is larger than that predicted by the radio emission from the ~ 20'' region around the 3 compact sources for case B recombination. The {Bralpha / Brgamma } ratio is unusually large for a ~ 5'' region surrounding the western source. The 3.29microns emission and the H_2 is found in a bubble like region that overlaps and extends beyond the Bralpha and Brgamma emission into the photodisociation region (PDR). Excess hydrogen line emission may be due to accretion, stellar winds giving rise to extended atmospheres, high density and optical depth, a core-halo structure supported by the sub-Lyman continuum, or some combination of effects.
Forrest William John
Howard Eric M.
Pipher Judith L.
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