Target Name (resolved by Sesame) or Position:	Target dimension:
NB: The epoch used for the query is the original epoch of the table(s)	Radius Box size

Full	Flag	Com
1	A	is for an entry that has been identified as a probable astrometric binary by
2	A	MK; this presumably has a long period, and so if the system is already known
3	A	to have a short period (from SB9, GCVS, or another source), we assume the
4	A	system is triple (at least). If this makes it a triple that is not in the
5	A	MSC, we write n= 3? rather than n= 3 . Quite often it is in the MSC,
6	A	however, because there is convincing additional evidence.
7	b	is for an entry of two or more stars that are (usually) intrinsically bright,
8	b	distant and not very close together. They are close enough together that
9	b	their juxtaposition is unlikely to be chance, yet far enough apart that one
10	b	can question whether they are in a long-lived orbit. It ends up as largely a
11	b	subjective matter whether one thinks these should be listed as one system, or
12	b	two or more systems. In some cases, they may be members of a cluster, and
13	b	(arguably) not much closer together than cluster stars usually are. We list
14	b	eight systems that we qualify with b.
15	C	is for an entry that comes from CHARA.
16	E	is for an entry identified in the GCVS as having an eclipsing, or eclipse
17	E	related, light curve. If a system merits both A and E we regard it as a
18	E	probable triple, since an orbit that gives eclipses will usually be too small
19	E	to also give an astrometric indication. Most but not all systems flagged E
20	E	from the GCVS have known periods, coinciding with SB9 periods, but those
21	E	without periods are presumably rather uncertain.
22	G	is for a system whose parameters are taken from the catalogue of
23	G	R.E.M. Griffin (to be published). These are mostly G/K giants plus B/A
24	G	dwarfs; but in a handful of cases, she concludes that the dwarf is itself in
25	G	a subbinary.
26	H	is for a system that we identify, through slightly discrepant proper motions,
27	H	as having an extra, unseen, component making the system at least triple.
28	H	There are six such systems; we assign their multiplicities as 3?, indicating
29	H	that we think that the probability of the extra body is over 50 per cent,
30	H	though nothing like certain enough for inclusion in the MSC.
31	h	is for a binary system where we suspect that large but uncertain discrepancies
32	h	in the HIP values of parallax and/or proper motion may be hinting very weakly
33	h	at a third body. We assign multiplicity 2?, and we identify 25 such systems.
34	L	is for a system where we have relied on the discussion by Lindroos (1985,
35	L	Cat. II/127) as to whether certain companions, usually rather distant, are
36	L	optical or physical, and arguably pre-main sequence if physical.
37	P	is for a system noted by Parsons (2004, Cat. J/AJ/127/2915) as containing a
38	R	hot component that may be two roughly equal components.
39	R	is for an entry identified as a probable or certain spectroscopic binary by
40	R	Famaey et al. (2005, Cat. J/A+A/430/165), Andersen & Nordstroem
41	R	(1983A&AS...52..471A, 1983A&AS...52..479A, Cat. III/127), Nordstrom &
42	R	Andersen (1985A&AS...61...53N, Cat. III/127) or Grenier et al. (1999,
43	R	Cat. J/A+AS/137/451, Cat. J/A+AS/135/503).
44	s	is for a specific reference which is given in the electronic version of the
45	s	table.

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