Spitzer 24 μm Images of Planetary Nebulae

doi:10.1088/0004-6256/138/2/691

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You-Hua Chu et al. 2009 The Astronomical Journal 138 691 doi:10.1088/0004-6256/138/2/691

SPITZER 24 μm IMAGES OF PLANETARY NEBULAE

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You-Hua Chu¹, Robert A. Gruendl¹, Martin A. Guerrero², Kate Y. L. Su³, Jana Bilikova¹, Martin Cohen⁴, Quentin A. Parker⁵, Kevin Volk⁶, Adeline Caulet¹, Wen-Ping Chen⁷, Joseph L. Hora⁸ and Thomas Rauch⁹

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chu@astro.uiuc.edu

¹ Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 West Green Street, Urbana, IL 61801, USA
² Instituto de Astrofísica de Andalucía, CSIC. c/ Camino Bajo de Huétor 50, E-18008 Granada, Spain
³ Stewart Observatory, University of Arizona, Tucson, AZ 85721, USA
⁴ Radio Astronomy Laboratory, University of California, Berkeley, CA 94720, USA
⁵ Department of Physics, Macquarie University, Sydney, NSW 2109, Australia
⁶ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
⁷ Institute of Astronomy, National Central University, Chung-Li, Taiwan
⁸ Center for Astrophysics, 60 Garden Street, MS 65, Cambridge, MA 02138, USA
⁹ Institut für Astronomie und Astrophysik Tübingen (IAAT), Abteilung Astronomie, Sand 1, D-72076 Tübingen, Germany

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Abstract References Cited By

Spitzer MIPS 24 μm images were obtained for 36 Galactic planetary nebulae (PNe) whose central stars are hot white dwarfs (WDs) or pre-WDs with effective temperatures of ~100,000 K or higher. Diffuse 24 μm emission is detected in 28 of these PNe. The eight nondetections are angularly large PNe with very low Hα surface brightnesses. We find three types of correspondence between the 24 μm emission and Hα line emission of these PNe: six show 24 μm emission more extended than Hα emission, nine have a similar extent at 24 μm and Hα, and 13 show diffuse 24 μm emission near the center of the Hα shell. The sizes and surface brightnesses of these three groups of PNe and the nondetections suggest an evolutionary sequence, with the youngest ones being brightest and the most evolved ones undetected. The 24 μm band emission from these PNe is attributed to [O IV] 25.9 μm and [Ne V] 24.3 μm line emission and dust continuum emission, but the relative contributions of these three components depend on the temperature of the central star and the distribution of gas and dust in the nebula.

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SPITZER 24 μm IMAGES OF PLANETARY NEBULAE

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