HST PC and FOS Observations of Planetary Nebulae in the Magellanic Clouds

Details HST PC and FOS Observations of Planetary Nebulae in the Magellanic Clouds HST PC and FOS Observations of Planetary Nebulae in the Magellanic Clouds

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...183.5109v&link_type=abstract

American Astronomical Society, 183rd AAS Meeting, #51.09; Bulletin of the American Astronomical Society, Vol. 25, p.1371

Astronomy and Astrophysics

Astronomy

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Scientific paper

A sample of 15 planetary nebulae are selected from the catalogue of Sanduleak, MacConnell, & Philip (1978, SMP), and are observed using the planetary camera (PC) and faint object spectrograph (FOS) onboard the Hubble Space Telescope (HST). Selection of the targets for this program are based upon the need to cover as large a range as possible in nebular excitation class and Hβ flux within the allotted spacecraft time. The objects selected in the Large Magellanic Cloud are LMC-SMP 2, 8, 20, 35, 40, 47, 72, 76, 85, 87, 96, and those in the Small Cloud are SMC-SMP 1, 3, 6, and 28. The PC images are obtained through the F502N narrow band filter, which is centered upon the relatively strong nebular emission line of [OIII] lambda 5007 Angstroms. Image restoration was performed using 100 iterations of the Richarson-Lucy (RL) method in all cases. Nebular structure reminiscent of Galactic PNs is seen in the restored images, with type I PNs having the largest and most complex structures. Tests of the RL method indicate PN structure can be resolved up to the point where the surface brightness profile begins to fall as radius(-4) . The FOS observations of the PN sample are obtained using the G130H, G190H, and PRISM spectral elements. The two gratings, G130H and G190H, give a spectral coverage of lambda lambda 1150-2250 Angstroms at ~ 1.3 Angstroms resolution. The PRISM observations are used to link the UV FOS observations with the ground-based optical spectrophotometry available in the literature. This work is conducted under General Observer program numbers 2266, 3441, and 4040. Initial results for LMC-SMP85 can be found in Dopita et al. (1994, ApJ, in press).

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