Abstract

We present an 8–13 μm spectrum of the planetary nebula IC 2165. In addition to a bright [S IV] emission line, we identify weak emission from the [A III] and [Cl IV] fine structure lines and the H7–6 hydrogen recombination line. These lines are used to derive ionic abundances which are in agreement with those expected from the known excitation of the nebula. The rather weak continuum is attributed to free–free emission near 8 μm, but with increasing contributions from dust emission with increasing wavelength. From the presence of emission from silicon carbide dust, we infer that the emitting dust grains were formed in a carbon-rich environment, in accord with abundance determinations from optical and ultraviolet line emission.

Talk to us

Join us for a 30 min session where you can share your feedback and ask us any queries you have

Schedule a call

Disclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.