2-12.5\micron Imaging of \iras 21282+5050: The Structure of a Young Planetary Nebula

Details 2-12.5\micron Imaging of \iras 21282+5050: The Structure of a Young Planetary Nebula 2-12.5\micron Imaging of \iras 21282+5050: The Structure of a Young Planetary Nebula

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.5602m&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #56.02; Bulletin of the American Astronomical Society, Vol. 24, p.1213

Astronomy and Astrophysics

Astronomy

Scientific paper

We present 3.3, 8.5, 10.0, 11.3 and 12.5 \micron narrowband ({{Delta lambda }/ λ} ~ 3-10%) and K-band (2.2\micron) high resolution images of \iras 21282+5050 and a 6 cm flux density measurement. The new infrared images reveal a 4.\arcs 5times 6\arcs , P.A. 15(deg) nebula with two prominent emission peaks aligned almost E-W and separated by 1.\arcs 7-2.\arcs 1. Comparison of these images with CO 1-0 maps, and a 6cm continuum map reveals an ionization bounded planetary nebula whose structure may reflect the density inhomogeneities of the ejected Asymptotic Giant Branch (AGB) wind. From the 6cm flux density and the nebula size, we derive an electron density of 1.3times 10(3) cm(-3) for the central ionized region. Only slight spatial differences are discernible between the K-band and 10\micron ``dust'' continuum images and the 3.3, 11.3, and 12.5\micron unidentified infrared (UIR) emission bands images which have been attributed to polycyclic aromatic hydrocarbons (PAHs). This tight spatial correlation suggests that the K-band and 10\micron arises from the same molecular dust material as the UIR bands.

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