** file last updated 10 august 2007

REQUESTS CONCERNING 70um PAPER:
-------------------------------


1) READ AND COMMENT ON PAPER CONTENT
   http://www.astro.caltech.edu/~lah/feps/draft.hillenbrand70.pdf

   - any/all suggestions on any aspect of the paper are welcome
   - please send requested info in specific boldfaced areas


2) RESPOND TO THE FOLLOWING SPECIFIC AREAS WHERE INPUT IS DESIRED

  - i have included calibration uncertainty in identifying excess 
    but only internal uncertainty in identifying detections. right?

  - please comment on the use of Fexcess vs lambda as in Figure 2 of
    http://www.astro.caltech.edu/~lah/feps/060710/hillenbrand.html
    or lambda^4 Flambda vs lambda as is currently in the paper.  the former 
    "residual" plot has scaling difficulties while in the latter "observed" 
    plot is hard to see subtleties.  the point is: how do we demonstrate 
    the plausible need for extended dust structures.

  - i show LIR/L* vs Tdust and Rdust vs Tdust. 
    is Lir/L* vs Rdust a useful addition or replacement?


3) PLEASE CONFIRM IF YOU CAN TAKE CARE OF ASSIGNED ACTION ITEMS BELOW



WHO                 WHAT
-------------------------------------------------------------------------------------

**
hillenbrand      convert http://www.astro.caltech.edu/~jmc/feps/data/mips70/ 
or               to paper text.  include other updated data reduction as
carpenter        appropriate.  alternately, do we just reference carpenter 
		 et al. 2007

** 
carpenter        which/latest IRS data is in the database?
bouwmann         hd 191089 ahd hd72905 have neither hi res feps data
		 or low res GTO data present.

**
volunteer?       we still need to revisit consideration of errors on the irs 
		 photometry.  note in figure 4 that there is relatively wide 
		 scatter in the bottom two panels which show IRS33/MIPS24 
		 measured flux ratios, compared to the other panels.

**
hillenbrand      fix figure 6 (seds) 
		   1) a few rogue cases: hd 38529, hd 13974 
		   2) suppress fit for hd206374 with bad irs "phot" due to spike 
		   3) plot full IRS spectrophotometry ??

**
open              sections 3.2 and 3.3 move to appendix?


**
moro martin      investigate applicability of survival analysis for
		 understanding 70um detection limits wrt various 
		 dust parameters.  **stellar** parameters already done.

**
volunteer??      look at Lir/L* vs dist and age; we are likely missing a corner
		 of low lum and distant disks which will possibly help on
		 placing FEPS-approprite sensitivity limits on figure 8.
		 relate to 5x zodi goal of FEPS at 70um.

**
open             the 2-3 sigma sources.  current inclination is to leave them
		 in the tables and let people treat them as candidates.

**
open             need to address T(delta R) vs T(delta a) by calculating
		 grain size distribution that would mimic radial range

**
hillenbrand      compare to most recent jmc spectrophotometric values 
		 of Tdust and Ldust              

**
hillenbrand      in figure comparing to literature
		   1) change from LIR(upper limit) to LIR(minimum) when Tdust 
		      is inferred to be <50K.
                   2) for Tdust > 50K, plot both infered LIR(upper limit) 
		      and LIR(minimum) as bounds

**
hillenbrand      for literature comparison, replace my zs04 table with 
		 table2 from rhee et al. 2006 which appears to contain
                 more precise (accuracy unknown) dust values; note that 
		 there are just a few solar type stars that have been added 
		 since zs04.

                 make my two .sm scripts (FIELDSTARS/zs04plot.sm and 
		 sirtf/smgo.rdust_tdust) into single script....


**
volunteer ??     plot expected collisional and PR time scales vs 
		 1) disk radius for assumed 10um grains and various alpha 
		 2) grain radius for assumed R=50 AU and assumed alpha
                 (like figure 7 of besla and wu 2007 or chen_irs 2006 paper)


**
kim (thank you!) the dreaded, check references


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