flames_table_README.txt

Ian Hunter February 2009

Only those stars which have been listed in the online tables of Dufton et al.
2006 and Hunter et al. 2007 (the Galactic and Magellanic CLoud vsini papers)
have been included in this table. Abundances have only been computed where
possible, see the forthcoming paper by Hunter et al. 2008.

This table has been created to be easily readable by IDL so all columns have
been made to be numerical. This has been a bit of a problem with spectral types
and luminosity classes but numbers have been assigned to represent the
characters. The IDL command to read one line of the file is given below and a
description of what is given on each line follows this. 
 
OPENR, table, 'flames_table.txt', /GET_LUN
READF, table, clus, starname, Btype, lum, be, sp, pe, mv, b_v, ebv,$
  temp, logg, vt, vsini, vsinilim, logteff, luminosity, mass, $
  bin, vel2, rad_dist, rad_vel, CII, CIIerr, CIIels, $
  NII, nlim, NIIerr, NIIels, OII, OIIerr, OIIels, $
  MgII, MgIIerr, MgIIels, SiIII, SiIIIerr, SiIIIels
FREE_LUN, out

1: clus - This is the name of the cluster

2: star - this is the star identifier for its cluster

3: Btype - is its spectral type as a Bstar. So a 1 is a B1
star, a 3 is a B3 star. O stars are negative in the sense that
a -4 will represent a O6 star. Stars with spectral type ranges
have just been given a value in the middle of the range, so
a B1-3 star will have a 2 in the Btype column
Stars with no spectral type are listed as -99

4: lum - indicates the luminosity class of the star and
1=Ia, 1.3=Iab, 1.7=Ib, 2=II, 3=III, 4=IV, 5=V. A zero in this
column indicates no luminosity class is given by Evans et al.

5: be - a 1 in this column indicates a Be-type star, otherwise 0 is given

6: sp - a 1 is listed in this column if there is some uncertainty in the
star's spectral type or luminosity class eg. its listed as B1-3

7: pc - a 1 is given in this column if there are any other pecularities
about the spectra type, e.g. B3 IIIn

8: mv - the visual magnitude as given by Evans et al.

9: b_v - the B-V color as given by Evans et al.

10: ebv - the E(B-V) value. This is from Dufton et al for the Galactic stars and
is assumed to be a standard value for each of the Magellanic Cloud clusters

11: temp - the effective temperature for the star. A negative number indicates that
no effective temperature was estimated

12: logg - the surface gravity of the star. A negative number indicates that no surface
gravity was estimated

13: vt - the microturblence computed to give a standard silicon abundance. A -9 means no
value was estimated, -1 indicated that no physical value could be determined and zero
was adopted to compute the abundances

14: vsini - the projected rotational velocity (profile fitting for most, Fourier method for supergiants)

15: vsinilim - indicates an upper limit to vsini value

16: logteff - log(temp) but for stars with no temperatures has been estimated from Btype
and Trundle et al, temperature scales in order to plot on HR diagram, -1 for no value

17: luminosity - luminosity estimated as discussed in papers, -1 for no value

18: mass - evolutionary mass from papers, -1 for no value

19: bin - binary indication. 0=apparently single star, 1=possible SB1 object, 2=possible SB2 object
a value of 2 is often given if some contaimation or assymmetry is observed

20: vel2 - vsini of secondary object in an SB2 system if measureable. -1 if no value

21: rad_dist - radial distance from cluster centre in arc minutes, -1 if no value

22: rad_vel - radial velocity of star. -999 if no value (e.g. binary)

23: CII - CII abundance

24: CIIerr - uncertainty in CII abundance

25: CIIels - number of lines used to calcualte CII abundance

26: NII - NII abundance

27: nlim - indicates if the NII abundance is an upper limit

28: NIIerr - uncertainty in NII abundance

29: NIIels - number of lines used to calcualte NII abundance

30: OII - OII abundance

31: OIIerr - uncertainty in OII abundance

32: OIIels - number of lines used to calcualte OII abundance

33: MgII - MgII abundance

34: MgIIerr - uncertainty in MgII abundance

35: MgIIels - number of lines used to calcualte MgII abundance

36: SiIII - SiIII abundance

37: SiIIIerr - uncertainty in SiIII abundance

38: SiIIIels - number of lines used to calcualte SiIII abundance