Hubble Space Telescope Imaging of Central Stars of High-Excitation Planetary Nebulae with WFC and WFPC2

Details Hubble Space Telescope Imaging of Central Stars of High-Excitation Planetary Nebulae with WFC and WFPC2 Hubble Space Telescope Imaging of Central Stars of High-Excitation Planetary Nebulae with WFC and WFPC2

Jan 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aj....119..302w&link_type=abstract

The Astronomical Journal, Volume 119, Issue 1, pp. 302-314.

Astronomy and Astrophysics

Astronomy

14

Planetary Nebulae: Individual (Ic 2165, Me 2-1, Ngc 2440, Ngc 7027), Ism: Planetary Nebulae: General, Stars: Evolution

Scientific paper

We present observations of four high excitation planetary nebulae (IC 2165, Me 2-1, NGC 2440, NGC 7027) taken with the Wide Field Camera and the Wide Field Planetary Camera 2 on board the Hubble Space Telescope. The high angular resolution of the instruments allows for the unambiguous identification of the central star, which was not found to be the case in most previous studies. In addition, the panchromatic nature of the data, which include several ultraviolet bandpasses, permits us to directly determine the amount of dust extinction present along the sight line to the central star. The combination of these two characteristics make it possible to delineate the spectral energy distribution of the central stars. Assuming a Planck function spectrum and a standard interstellar extinction law with RV=3.1, the adopted EB-V values are 0.40 (IC 2165), 0.15 (Me 2-1), 0.15 (NGC 2440), and 1.10 (NGC 7027). The wavelength coverage of our measurements is not particularly sensitive to temperature values in the range 150,000-400,000 K. However, we do find that 200,000 K produces the best fits. Again using a Planck function to represent the wavelength dependence of the stellar flux, we determine V magnitudes of 17.47+/-0.06 (IC 2165), 18.40+/-0.05 (Me 2-1), 17.63+/-0.16 (NGC 2440), and 16.04+/-0.04 (NGC 7027). Combining these results with literature values for the emission-line fluxes and distances, we derive the Zanstra temperature, crossover magnitude, radius, and luminosities for each object. The implications of these measurements for the mass and the evolutionary state of each object is briefly discussed.

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