BEGINNING WITH SERENA's OUTLINE FOR FIRST 70um PAPER AND MODIFYING FOR ADDITIONAL SOURCES 



Formation and Evolution of Planetary Systems: Additional Cold Outer Disks 

- Lead authors: Hillenbrand (??), Kim 
- Suggested Co-Authors:  ?????
			 Backman, Meyer, Carpenter, Moro-Martin
			 Silverstone, Bouwman, Hines 

0.   ABSTRACT

   In this paper we present 3.6 - 70 um IRAC, IRS, and MIPS photometry and
   spectrophotometry from the Spitzer Space Telescope of 15-20 new cold debris 
   disk systems associated with solar-type stars. The sources show infrared 
   excesses only at 70um, and not shortward of 33um, indicating
   large inner evacuated regions in the dust distribution.  
   The age of the parent stars indicates the dust is debris dust, which 
   may be associated with the presence of planetary bodies orbiting the stars.  


I.   Introduction  

     This paper is part of a sequence from the Spitzer Legacy Program
     ``Formation and Evolution of Planetary Systems".  Previous contributions
     have highlighted 
	- initial results including one debris disk discovery and one confirmation (Meyer et al. 2004)
        - dissipation of terrestrial zone dust at ages <30 Myr (Silverstone et al. 2005)
        - constraints on gas mass in young and intermediate age dusty disks (Hollenbach et al. 2005; Pascucci et al. 2006)
	- an unusual 30 Myr old warm asteroidal debris system (Hines et al 2005)
	- the prevelance of debris disks at 120 Myr of age (Stauffer et al. 2005)
	- evolution of debris dust in clusters from 5-600 Myr (Carpenter et al. 2006)
	- new cold, old debris disks (Kim et al. 2005)
	.
     This paper is similar to the Kim et al. paper in presenting new debris
     disks which are detected with sensitive Spitzer observations with only
     the MIPS 70um channel, and not shortward of the IRS long wavelength
     regime (33 um).


II.  Data
 
     A. Sub-Sample of Newly Presented FEPS targets with 70um-only excess.
	Could be as many as 15-20 sources.  Detailed checks still needed.
         
         Table of stellar properties 
         ============================================================
            target       Sp.         Age     d (pc)   Note              
         ------------------------------------------------------------


         ------------------------------------------------------------


     B. Observations and Data Reduction

        Brief description of IRAC, IRS, and MIPS observation modes and
             data reduction (heavy reference to previous papers)

        Measured fluxes, uncertainties, and excesses above photospheres in a table.  


III. Results 
  
      A. Spectral Energy Distribution

        i.  Photospheric models (reference Carpenter et al.)
	    described. Excesses defined.

        ii. SEDs of all sources presented in Figure with
	    simple models overplotted. 

      B. Modeling and Interpretation 

            i. Disk properties (inner and outer radii, dust masses)
           ii. Comparison of the best fit models for individual 
               sources with Solar System Toy Models? (are they  
               consistent? or different? If different, how different?) 

      C. Statistics
	    i. Simple statistics e.g., age bin vs. fraction of 70um only 
		excesses  (Nexcess/Ntot) compared to age bin vs. fraction 
		of excesses at shorter wavelengths (24um or 33um??). 
           ii. Reference to planet scenario; specific discussion 
		of 70um excess sources which have claimed rv planets


IV. Discussion

V.  Summary 

VI. Conclusions


Acknowledgements

REFERENCES