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G.H. Rieke, E.T. Young, P.A.R. Ade, A. Alonso-Herrero, C. Beichman, H. Dole, E. Egami, C. Engelbracht, T.N. Gautier, K.D. Gordon, T. deGraauw, E.E. Haller, D. Hines, D. Kelly, C. Lada, W. Latter, F.J. Low, K. Misselt, J. Morrison, J. Mould, J. Muzerolle, G.X. Neugebauer, C. Papovich, P.L. Richards, M.J. Rieke, G. Rivlis, J. Stansberry, K. Stapelfeldt, K. Y. Su, M.W. Werner (MIPS Team)
The GTO program for the MIPS team is concentrated in two areas. First, the evolution of planetary debris disks will be traced from their formation at less than one million years old, to the stable disks around old stars. To do so, we will make maps from 3 to 200 microns (in collaboration with the IRAC team) of regions where young stars are forming, to characterize thoroughly the circumstellar excess emission. We will include clusters representing a range of density and age. We will also observe a selection of isolated evolved stars in the MIPS photometric bands at 24, 70, and 160 microns. These observations will catalog the debris disk excesses as a function of stellar mass, age, binarity, and the presence of planetary companions. Second, we will explore the evolution of infrared galaxies and AGNs. This program has two components. In collaboration with both the IRAC and IRS teams, we will map at moderate depth 9 square degrees of sky, and in collaboration with IRAC will make deeper maps of about 2 square degrees. The latter regions have been selected to overlap with very deep xray surveys to aid in identification of AGNs and study of their evolution. We will extend the results of the deep maps by observations of 18 massive galaxy clusters in the redshift range 0.2 < z < 0.4. These clusters will image about 50 square arcmin of the background Universe, raising sources out of the confusion that will limit the sensitivity of the other deep surveys.
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The author(s) of this abstract have provided an email address for comments about the abstract: grieke@as.arizona.edu