SCIENTIFIC ABSTRACT The IRAS discovery of far-infrared excesses among seemingly normal main-sequence star motivates this proposal. These have been interpreted in terms of disks of cold material. The aim of this proposal is to establish the true frequency for far-infrared excesses in a volume-limited sample of main sequence and related stars using PHT-P, PHT-C, CAM and SWS measurements, in order to address the success or failure of single stars in processes related to the forming of planetary systems. For brighter sources, more extensive wavelength coverage and spatial resolution will be attempted, with PHT-P, PHT-C, PHT-S and SWS. Finally, observations of Kuiper Belt objects will be attempted. OBSERVATION SUMMARY This proposal is split into three parts: this is PART 1 It is planned to obtain more accurate coordinates for sources in this proposal, beyond the SIMBAD information used so far. Annual proper motions, where available, are listed. For a volume-limited sample of main sequence and related stars, PHT03 measurements at 3.6, 11.5, 20 and 60 microns will be obtained, using a 120 arcsec aperture in all cases to eliminate possible companion confusion with differing apertures. For the M dwarfs, 100 micron observations will also be obtained. Rectangular chopping will be used for sources above and below 10 degrees galactic or ecliptic latitude; triangular chopping otherwise, with a throw of 120 arcsec. For selected bright stars, CAM01 observations using microscans with 5 second exposures and 6 arcsec pfov and 6 arcsec steps, for 10 linear steps using the LW3 filter are planned. The signal to noise ratios are predicted, from the PHOT Cookbook to be in excess of 1000 for 32 second observations of sources brighter than 0.7 Jy at 3.6 microns, decreasing to 300 at 11.5 and 20 microns and declining to 2.5 at 60 microns, even at the ecliptic equator. Therefore the minimum 32 sec for each PHT-P filter will be sufficient for the continuum measurements at 3.6, 11.5 and 20 microns, and 64 seconds for the 60 micron observations. The 100 micron observations for the M stars will require chopping and a minimum of 128 sec to obtain S/N of >2. Total time per star is therefore (3 * 32 s + 64 s (+128 s)) * 2 for chopping, + 180 s acquisition + 155s other overheads = 655s (921s). PHT-S, CAM and SWS observations are more exploratory, with S/N in excess of 3 are based on comparisons with Central Programme estimates. PART 2: Concerns spatial mapping and spectra of selected brighter far IR sources. PART 3: Concerns local Kuiper Belt observations. LINKED OBSERVATIONS: No FIXED TIME OBSERVATIONS: No CONCATENATION: Yes - several AOTs on some sources.