A Listing of Everything That Has to Be Done Before MWRSGs can be submitted:
   ---or---
Dwarfs We Know and Love


   Who   What                              Status

1)  PM Add in the rest of the authors      DONE

2)  PM Make editing pass through ms        in progress

3)      Make paper conform to ApJ FASTTRACK: naming of files, include 
        figures in text, etc               wait for final figures
        i.e., manuscript is "ms.tex"
              tables embedded in text
              figures and figure captions
              figures named "f1.eps", "f2.eps", "f3a.eps, f3b.eps", etc.


4)      Reopen the log g question: is -0.5 the right choice?  
    PM a) ALMOST DONE: log g = 0.0 is probably a better choice, but maybe
         wait until Bertrand responds.  His definition of "log g" may not
         be the same as my AY 21 one.

	SEE ITEM 18 BELOW 

   E.M.? b) Need to also see how log g =0.0 compares with sample spectra vs
        log g = -0.5.  E.L. offered to do this.

5) PM? Decide on color vs bw for figures.  If color, how?  Talk to Laura?
        Talked to Laura.  She believes that the color that you see on a
        24-bit screen should be "real", and that if there wasn't color on
        the postscript file, probably the program lacked a /device,color
        or some such.
        STILL NEED TO DECIDE WHAT WE SHOULD DO.  MAYBE COLOR FOR NOW?


6)        Table 1:
        a) Check coordinates of all stars
        b) Move E(B-V)'s to results table
        c) Check photometry and give references; fill in the blanks
        d) Add space between spectral subtype and luminosity class
        e) Add cluster/association membership
        f) Add in the K's and new spectral types [need to get list from Emily!]
           EMILY HAS PROVIDED LIST.  SEE ITEM 11 BELOW

       E.L. - I can take care of this

7)     Table 2: check but looks OK....make units conform to ApJ standards
       (A mm^-1 rather than A/mm; also if units are given, don't repeat
       (eliminate "/um on entries under slit width.  Will deal with this as
       part of 2 above.

      E.L. - I can take care of this (and any other corrections
             as they come up)

8)      Add table giving adopted distances of the OB associations listed
        in Table 1.

      E.L. - I'll have a couple questions (do the Mbols in Table 1 now
             reflect use of the new distance moduli?) but I can do this

9)        Results Table (currently Table 3):
       a) Add E(B-V), filling in the blanks where they are missing from table 1.
       b) Add M_V [V - 3.1E(B-V) - dm, with dm from new table
  PM   c) Compute new BCs from models and compute new Mbols
           HOW?   Not really sure!  Need to spend some time understanding the
           zeropoint of the Mbol system!   DONE!
     d) Add these to the table, so that we have Mbols.

     E.L. - I can take care of this

10) PM?    Using the new Mbols
        make new HR diagram.  What evolutionary tracks to use?  Phil to
        write to Maeder.  DONE.  Still need to understand and get the
        tracks!

11)   Get warmer models from Bertrand and run remaining stars (Ks).
  EL   a) Need to get a list of the stars that we want to include (Emily!)
          DONE
  PM?  b) Need to CLASSIFY the K's
       c) Need to compare to models
       d) Make plots  (see 4 and 18)
       e) Add to all tables

12)    Remake the final Teff plot with the K I's included

    E.L. - Since I wrote the putzy little program that makes the plot,
           I'll do this as soon as the data becomes available!

13) PM   Somehow address Nat's "brilliant idea" of developing some photometric
       index of TiO band strength vs Teff.  Think we should do this strictly
       from the models, and then relate that to the spectral types determined
       from our stars.  This is a project all in itself (and one might argue
       doesn't really belong in this paper).  Get Nat to help?  Not much 
       chance.  I'm guessing this is going to be a couple of days, and
       may require PM.

14)   Finish the manuscript and then pass around to to the kids

15)   Include comments from Bertrand, Maeder, etc.  
 
16)   Figure showing agreement CTIO/KPNO

    E.L. - I can at least go digginf for a star to use.

17)   Understand what is happening in the blue (<4200A)
   PM a) Write to Bertrand DONE
   PM b) In the cases where the blue TURNS UP, the problem is presumably
         OBSERVATIONAL.  Check this against the actual data! 
      c) Remake the figures using 3800A cut-off?  Need to think about this!
          See 18.

18) Remake the spectral figures:
   PM  a) Decide on color vs b&w
       b) If color, how?  Phil talked to Laura Woodney, who thinks it's
          simple: need 24-bit monitor to make the screen appear right,
          and then must include /device,color.  Looked at Emily's code,
          and that IS actually there.  So, now I'm puzzeled.
       c) Cut off low wavelength part of spectrum? (3800)
       d) Use log g = 0.0 instead?  Depends upon result of Emily's test


19) SUBMIT!