Optical spectrum of the planetary nebula M 2-24

Abstract

We have obtained medium-resolution, deep optical long-slit spectra of the bulge planetary nebula (PN) M 2-24. The spectrum covers the wavelength range from 3610--7330 A. Over two hundred emission lines have been detected. The spectra show a variety of optical recombination lines (ORLs) from C, N, O and Ne ions. The diagnostic diagram shows significant density and temperature variations across the nebula. Our analysis suggests that the nebula has a dense central emission core. The nebula was thus studied by dividing it into two regions: 1) an high ionization region characterized by an electron temperature of T_e=16,300K and a density of logN_e(cm^{-3})=6.3; and 2) a low ionization region represented by T_e=11,400K and logN_e(cm^{-3})=3.7. A large number of ORLs from C, N, O and Ne ions have been used to determine the abundances of these elements relative to hydrogen. In general, the resultant abundances are found to be higher than the corresponding values deduced from collisionally excited lines (CELs). This bulge PN is found to have large enhancements in two {alpha}-elements, magnesium and neon.

arXiv comment16 pages, 7 figures; accepted for publication in A&A

References in corpus (3)

• Improving Predictions for Helium Emission Lines
• Radiative Transfer Effects in He I Emission Lines
• Evidence for binarity in the bipolar planetary nebulae A79, He2-428 and M1-91

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