(Aug. 1 2004 - JSK) * Title: TBA (30% MIPS result from FEPS Legacy Program ??) * Authors: J. Serena Kim, Murray D. Silverstone, Dean C. Hines, Michael R. Meyer, Dana Backman, John M. Carpenter, Lynne A. Hillenbrand, E. Stobie, Jeroen Bouwman, Debbie Padgett, ?? * Brief Description of the Paper This paper outline is based on an assumption that we will be using 30% MIPS data. Note that other possibilities for the direction of this paper have been discussed. This paper will present 30% of MIPS data and SEDs including 3 MIPS bands (24um, 70um, and 160um when possible) together with optical and near IR fluxes. We will measure 24um, 70um, and 160um excesses using observed fluxes and Carpenter et al.'s best fit photospheric models convolved with the MIPS response function curves. Excesses vs. age bins will be presented and the implication will be discussed. For 70um and 160um non-detections, we will coadd measured fluxes (and images time permits) per age bin to give better upper limits or to see if we could see a source. Using Backman et al.'s models for Solar-analog systems, we will do simple analysis using 30% data to answer questions of FEPS programs: e.g., Is our Solar System common or rare in the Solar neighborhood? ============================= Outline of the MIPS 30% paper ============================= I. Introduction A. Some general questions and literature studies about disk evolution/planet formation will be addressed linking to the FEPS science goals. Questions that we can explore and answer using our 30% of MIPS data will follow those general questions. It will be a short about two paragraph introduction (reference: Meyer et al.'s paper about FEPS program.) II. Data acquisition & analysis A. Targets - Short introduction and a table will contain all the targets and some properties, such as spectral types, ages, and distances. We will reference other FEPS papers (e.g., Hillenbrand et al.). B. MIPS data i. Brief description of MIPS observation mode and our data will be described in the first paragraph. ii. Data reduction using DAT pipeline (DAT paper written by MIPS team will be referenced) C. Analysis (photometry, SED, definition of excesses) i. Short description of HOW we did photometry, including aperture sizes, aperture corrections, etc, will be written here. IDP3 will be referenced. ii. We will define excesses of 24um, 70um, and 160um here: we convolve photospheric model with MIPS response curves, and these fluxes will be subtracted from observed fluxes. (e.g., 24um excess = 24um_measured - 24um_photosphere_model) Since we may be dealing with only MIPS data in this paper it may be a good idea to define excess per band (24um, 70um, and 160um separately). iii. All the measured fluxes and excesses will be listed in a table. III. Results A. Excesses vs. age: All excesses will be plotted against age bins. Would we find a particular age bin showing significantly more number of stars having excesses? OR Would the excesses be randomly distributed over all the age bins? This section will contain the results involving only observational results and very simple interpretation of what the data might imply not involving models. For example, if there is an age bin that deviates significantly from other age bins, i.e., it has more number of excess sources than other age bins, might this age bin an era that planetesimals undergo more vigorous collisions to form excess dusts in Sun-like systems? B. Non-detections: upper limits (fluxes) of non-detections will be coadded by age bin weighted by sigma of each image. This can yield either better upper limits, or any detection from coadded flux per age bin for 70um and 160um. IV. Models and Interpretation A. We will give some constraints for tau, dust mass, and disk sizes for all 30% targets. Table in the section II can include these parameters as well. B. Dana Backman's toy models: we will have a short description of Dana's toy model (referencing Backman & Paresce 1993), and the grid of models we use in this paper. C. Using the fluxes predicted from the Toy models (Solar analog), We will compare observed distribution of excesses vs. age and the prediction from Toy models. Q.1: Is there any pattern in difference or in similarity between observed results and prediction by models? Q.2: If different, what are the differences, and how different are they? What astrophysics can we infer from these differences? (e.g., evolution of Kuiper Belt of the Solar System from the Toy model and results from this study) D. Should the upper limits for non-detection become useful to be used with Toy models, we will describe this following secton IV.C. If the coadded flux of non-detections per age bin (section III.B) turn out to be a meaningful number, we will describe the implication we can draw from Toy models about such systems. V. Discussion A. What have we learned from 30% data of FEPS MIPS data? B. Caveats in our interpretation and degeneracy of certain parameters will be addressed. C. Future follow-up observations helpful or needed can be mentioned. VI. Appendix A. Simple comments on some individual interesting sources will be made, e.g., just to COMMENT that which systems contain radial velocity planets, number of companions, or very strong activities, that are known from other literatures, etc. This comments will be a short and simple ones that do not involve any detail or time-consuming analysis. Other FEPS up-coming papers regarding these notes can be referenced. If IRAC or IRS results shows something very interesting for certain systems we could reference Silverstone et al. or Bouwman et al.'s paper with a short notes about what the interesting features are. (discussion needed for this matter?)