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## (from tabmap V6.0 (2016-08-18)) 2024-04-28T21:01:20 #--------------------------------------------------------------------------- #-- J/MNRAS/353/601 2dF survey of the Small Magellanic Cloud (Evans+, 2004) #-------------------------------------------------------------------------- #---Table: J/MNRAS/353/601/./notes.dat Detailed classification notes very kindly provided by R.O. Gray (44 records) # Name I4 --- 2DF designation # Note A75 --- Text of the note -------------------------------------------------------------------------------- Name|Note ----|--------------------------------------------------------------------------- 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. --------------------------------------------------------------------------------