A Near Infrared Study of the NS 14 Bipolar Nebula

Details A Near Infrared Study of the NS 14 Bipolar Nebula A Near Infrared Study of the NS 14 Bipolar Nebula

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...186.0910h&link_type=abstract

American Astronomical Society, 186th AAS Meeting, #09.10; Bulletin of the American Astronomical Society, Vol. 27, p.825

Astronomy and Astrophysics

Astronomy

Scientific paper

As part of a study of high mass star formation in the near (1-5 microns) infrared (NIR), we have imaged the bipolar nebula NS 14 at J (1.23 microns), H (1.65 microns), and K (2.23 microns) broadband NIR wavelengths. We have also obtained 3.29 microns dust feature emission and Brgamma (n = 7->4, 2.166 microns) hydrogen recombination line emission images of this region. The broadband reflection nebulosity, surrounding a central `trapezium' of stars, forms a bipolar structure that is also seen in the 3.29 microns dust feature emission. The 3.29 microns emission is limb brightened, indicating that small dust grains in the central regions of the bipolar structure have been evacuated. The unresolved Brgamma emission in the vicinity of the hottest star (star A) in the trapezium is too high for what is expected from case B recombination based on radio measurements and previous estimates of extinction to the region. We have modeled this region with two components, an ionizing wind source and traditional nebular case B recombination in order to match the observations. A study of the stellar population of the cluster centered on the nebular emission has also been made.

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