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SPITZER 24 μm IMAGES OF PLANETARY NEBULAE

2009; Institute of Physics; Volume: 138; Issue: 2 Linguagem: Inglês

10.1088/0004-6256/138/2/691

1538-3881

You‐Hua Chu, R. A. Gruendl, M. A. Guerrero, K. Y. L. Su, Jana Bilíková, Martin Cohen, Q. A. Parker, Kevin Volk, A. Caulet, Wenping Chen, Joseph L. Hora, T. Rauch,

Astronomy and Astrophysical Research

Spitzer MIPS 24 um 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 um emission is detected in 28 of these PNe. The eight non-detections are angularly large PNe with very low H-alpha surface brightnesses. We find three types of correspondence between the 24 um emission and H-alpha line emission of these PNe: six show 24 um emission more extended than H-alpha emission, nine have a similar extent at 24 um and H-alpha, and 13 show diffuse 24 um emission near the center of the H-alpha shell. The sizes and surface brightnesses of these three groups of PNe and the non-detections suggest an evolutionary sequence, with the youngest ones being brightest and the most evolved ones undetected. The 24 um band emission from these PNe is attributed to [O IV] 25.9 um and [Ne V] 24.3 um 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.