2945 kF0hF2mF2 (III) This may be a mild Am star. The Ca II K-line is a bit weak
2945  (although this may be due to noise), but the Ca I 4226 line is clearly 
2945  weak.  Otherwise, the star looks normal, and there is no clear indication 
2945  it is a composite.
2145 F6 III Fe-1.0 Again, I don't think that this is a composite star. The 
2145  Ca II H line is clearly too deep, and is probably due to a noise spike or 
2145  some other processing error. The Ca II K-line is okay. The hydrogen lines 
2145  are a good match with an F6 III star, and, bearing in mind that the star 
2145  is metal-weak, the luminosity indicators, Sr II 4077 & Fe II, Ti II 4172-8
2145  indicate III or possibly as luminous as II. The general metallic line 
2145  strength is like that of the F0 III standard, which yields the above 
2145  metallicity index. Note that this does not imply that [Fe/H]=-1.0. 
2145  My experience suggests that Fe-1.0 suggests closer to [Fe/H]=-0.5, with 
2145  some considerable uncertainty.
0833 Quite similar to 2145, and has a very similar classification. I believe it 
0833  is normal as well, and that the unusually deep Ca II H-line is due to a 
0833  noise spike or processing error.
1875 F2 III: composite?? This star really has me scratching my head; I can come
1875  up with no solution yet. The problem is that the hydrogen lines have wings
1875  which match quite well at F2-F5 III, but their depths are only about 
1875  one-half what they should be! The Ca II K&H lines are shallow as well, but
1875  nearly equally shallow, which puts the kibosh on this star being an early 
1875  F-giant in a binary with a, say, dwarf B-star. If that were the case, the 
1875  K-line would be much weaker than the Ca II H-line, somewhat like 3114, 
1875  which presents similar problems (see its H-lines). Rotation does not help 
1875  as the metal lines look quite sharp. The only way that I can possibly 
1875  understand this star is if there is some source of continuum radiation 
1875  (say an accretion disk around a WD in the system), but I would expect to 
1875  see hydrogen emission lines in such a system. Another possibility is some 
1875  sort of processing error. Is that possible? I can roughly approximate the 
1875  appearance of this star by adding 50% scattered light to an F-type star, 
1875  but the Ca II K and H lines turn out too shallow. Could this be a 
1875  hydrogen-deficient star - maybe a post-AGB star???
3114 F2 V + sdOB? This star has similar problems to 1875 - fairly broad hydrogen
3114  wings (about F2), but much too shallow. However, 3114 has a truncated 
3114  K-line, which almost certainly means that it is a composite. I call this 
3114  star a dwarf because the luminosity indicators (Sr II 4077, Fe II, 
3114  Ti II 4172-8) all suggest a dwarf. Also, the weaker metal lines point to 
3114  the lower microturbulent velocity we might expect in a dwarf. However, it 
3114  does appear that the entire spectrum is "veiled" probably with a hot 
3114  companion with weak hydrogen lines (a subdwarf OB star suggests itself 
3114  here - especially a helium-weak one - see work by John Drilling on the 
3114  classification of sdOB stars). I expect that this star is in our halo and 
3114  not in the SMC at all. But I can't explain the velocity.