Near-infrared spectroscopy of the planetary nebula NGC 6572

Details Near-infrared spectroscopy of the planetary nebula NGC 6572 Near-infrared spectroscopy of the planetary nebula NGC 6572

Feb 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...368..468r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 368, Feb. 20, 1991, p. 468-473. Research supported by the Aerospace Corp.

Astronomy and Astrophysics

Astrophysics

15

Infrared Spectroscopy, Planetary Nebulae, Stellar Spectra, Emission Spectra, Line Spectra, Near Infrared Radiation, Oxygen, Phosphorus, Sulfur

Scientific paper

Spectroscopy of the PN NGC 6572 in the wavelength region 0.77-1.33 micron is presented. The measurement of line fluxes in regions of high telluric absorption is discussed, and an error in the wavelengths of forbidden P II reported in the literature is pointed out. The NGC 6572 continuum is well-matched by bound-free, free-free, and two-photon components at a temperature of 10,500 K. No significant contribution from the exciting star or hot dust is seen. The primary generation mechanism for the O I lines is fluorescent excitation by the stellar continuum. A sulfur abundance of 6.53 is derived, and N(P+)/N(S+) = 0.11 is found. This is much greater than the solar value and is probably due to the underabundance of S.

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