Title: Formation and Evolution of Planetary Systems: Cold Outer Disks - Lead authors: Kim, Hines - Suggested Co-Authors: Silverstone, Bouwman, Backman, Meyer, Carpenter, Hillenbrand, Wolf, Malhotra, Moro-Martin, Stobie, and other interested FEPSers - Brief Description of the paper outline In this paper, we present 3.6 - 70 um IRAC and MIPS photometry, and 5 - 35um IRS spectra of 4 new cold debris disk systems with log(age) > 7.5 of which excesses are detected only in 70um. HD_13974, which shows photosphere up to 70um (or possible tiny excess at 70um), will also be included. We can place simple limits on the dust excess in ways that will be different from all the non-detections at 70 um. We will determine excesses using Carpenter et al.'s best fit photosphere models. Modeling will be done using Toy models by Backman et al., and the DDS tool by Wolf and Hillenbrand to constrain disk properties of cold outer disks of these debris disk systems. 0. ABSTRACT I. Introduction We start with asking few fundamental questions about debris disks and planet formation (few sentences), and more specific questions that are related to this paper's science will follow. Literature studies about disk evolution/planet formation will be addressed linking to the FEPS science goals. (The first FEPS (ApJS) paper will be cited with few sentences of summary of that paper.) II. Data A. Samples - Short introduction and a table will contain all the targets and some properties, such as spectral types, ages, and distances. e.g. A table of stellar properties ============================================================ target Sp. Age d (pd) Note ------------------------------------------------------------ HD_8907 F8 8-8.5 34 HD_145229 G0 8.83 33 HD_6963 K0 9.02 27 HD_13974 G0V 9.19 11 nearby source NO or tiny 70um excess HD_122652 F8 9.29 37 ------------------------------------------------------------ (age: reference Hillenbrand et al.) B. Observations and Data Reduction i. Brief description of IRAC, IRS, and MIPS observation modes and our data will be described in the first paragraph. - Murray: IRAC few sentences (reference Silverstone et al.) - Jeroen: IRS few sentences (reference Bouwman et al.) - Serena: MIPS in a paragraph (in more detail) ii. Data reduction (reference the first FEPS paper) - Murray: IRAC a paragraph (reference Silverstone et al.) - Jeroen: IRS a paragraph? (reference Bouwman et al.) - Serena: In-depth description about MIPS data reduction iii. Short description of how we did photometry, including aperture sizes, aperture corrections, etc. IDP3 will be referenced. - Murray: IRAC a short paragraph or few sentences? (reference Silverstone et al.) - Serena: More in-depth for MIPS photometry (a table of aperture size, aperture corrections) iv. All the measured fluxes, uncertainties, (and excesses?) will be listed in a table. III. Results (We will follow the first FEPS paper (HD 105 and HD 150706) as a template.) A. Spectral Energy Distribution i. Photospheric models will be described in short paragraph (reference Carpenter et al.). Excesses will be defined following description of photospheric models. ii. SEDs of all 5 sources will be presented in a Figure(s) with best fit model overplotted. IRAC points and IRS spectra will also be used as well as other photometric points from the database. B. Modeling and Interpretation Goals: i. Given these stellar parameters and excesses what are the disk properties (inner and outer radii, dust masses)? ii. Can we compare the best fit models for individual sources with Solar System Toy Models? (are they consistent? or different? If different, how different?) iii. Is there any hint of planet formation? (inner gap?) First, we explain what modelings will done, and briefly describe each model (Toy model and DDS, give references, Backman et al. Wolf and Hillenbrand 2003). We address assumptions Toy model and DDS make. We will discuss a range of possible modeling results using toy models (Backman et al.), then the best results from using DDS (Wolf and Hillenbrand 2003) models. - A table of best range of results will be presented - Figures of AGES vs. EXCESSES for 5 targets AGES vs. R_inner range (if just scatter plot, do we want to include? maybe or maybe not. We can also include HD 105 and HD 150706 in this plot if we think we see an interesting trend. It would also be interesting to have comparison of these sources against other known debris disk systems like our samples.) Q. Dana and others: Could you help identifying similar "other" systems with debris disks that we can compare in this figure with our sources? ----------------------- (Detailed timeline is at the end of this outline) Q. Dana: Would you run Toy Models for all 5 systems, and get a range of possible fits? (please see the timeline) Q. Sebastian and Lynne: Would you run (and/or help me running) DDS models for these systems? (please see the timeline) Q. Renu and Amaya: Planetary architecture (Would you like to spectulate planetary architecture of these systems?) Q. A question to all of you: Do we need both modeling exercises? If you think YES, what would you suggest to construct a crystal clear structure of this section to avoid any confusion and/or redundancy that readers might have? If you think NO, what modeling excercise, you think, should be used, and why would you suggest so? (Your quick feedback will be very helpful!) Q. 2nd question to Dana, Lynne, Sebastian, (and Renu, Amaya?): If we are presenting the results from your models in this paper, could you contribute a short paragraph describing your model(s) and paragraphs about the best results? I will put your contributed paragraphs together in this section, and I'd very much appreciate your inputs. IV. Discussion This discussion section will contain more creative and spectuative interpretations. Some caveats can also be address here. V. Summary Summary of our paper with bullets or numbers. VI. Conclusions Acknowledgements REFERENCES =================== TIMELINE =================== If you see questions (Q.) asked to you, would you please send me your response by the date I specify below? October 27 (Wed): This outline is emailed to core team members of this paper (before Noon MST) MIPS Photometry and SED will be sent to the core team (tonight) Q. Murray: Would you let me know how long it would take for you to do photometry of these 5 sources? Q. Jeroen: (I've already asked you about the spectra of these sources) I'd appreciate if you could send me the IRAC photometry and Spectra by the end of this week. October 28 (Thu): Q. Dana, Lynne, Sebastian: Please let me know when you could start running models for sources I send you MIPS Photometry. Sorry about rushing... but it will be great to have modeling results asap. October 29 (Fri): Q. Core team members: Would you send your feedback by Friday (noon) about this outline? Q. Lynne: could you post this outline to the science plan page before Monday? October 31 (Sun): I will send out this outline to the whole team for feedback and to hear their intention of participation in this paper November 2 (Tue): Q. Dana, Lynne, Sebastian: would it be possible to have **some** modeling results by this day? How many sources out of 5 do you think we can have some results? It would be great if we can have some preliminary results for all, ... because... November 3 (Wed): I will report new results that I have at Steward Internal Symposium. I plan to include HD 105 and HD 150706. Please let me know if you have any suggestions. November 4 (Thu): Q. Dana, Lynne, Sebastian: Can we have modeling results of all 5 sources by this day? I'd like to have them if possible, for the poster to be presented at the New Views meeting at Pasadena. November 5 (Fri): I will circulate draft poster to authors, and will ask for quick feedback. November 8 - 12 (M-F): New Views Meeting at Pasadena ---- Novemner 29 (Mon): Circulate the First draft of the paper among the authors? December 3 (Fri): Feeback from authors December 10 (Fri): Next draft of the paper and circulate to the authors? December 17 (Fri): Feeback from authors December 22 (Wed): 3rd draft? December 30 (Thu): Submit the paper!!!!!!! PLEASE send me your comments, concerns, suggestions! THANK YOU VERY MUCH FOR YOUR COLLABORATION!! -- Serena