emamajek on 30-Nov-2011 03:56:08 GMT about BD-18 4244
Concerning [MMG98] RX J1612.6-1859 "a" and "b" in Martin et al.
(1998;
1998MNRAS.300..733M
). This study did not include finder
charts, magnitudes for the companions, nor useful
cross-identifications, so disentangling which component is which is
not entirely straightforward. I will give you my interpretation.
Martin et al. (1998) lists the following properties for this binary:
RX J1612.6-1859a: K6, EW(Halpha)=-0.2A, EW(Li)=0.48+-0.06A, WTTS
RX J1612.6-1859b: M0, EW(Halpha)=-15A, EW(Li)=0.78+-0.07A, CTTS
WTTS = Weak-lined T Tauri star, CTTS = Classical T Tauri star, EW(Li)
= Equivalent width of Li I 6707 feature. So "a" is hotter, and is a
young star lacking accretion signatures. "b" is cooler, and is a
young star showing accretion signatures.
"a" seems to correspond to the bright young star ScoPMS 52 = Wa Oph 3,
a known weak-lined T Tauri star. 18" away from "a" is a common proper motion
companion which shows strong Halpha emission (as discovered by
The 1964, and unambiguously identified in their finder charts). So
I believe [T64] 6 = "b".
So I propose the following identifications:
Wa Oph 3 = [MMG98] RX J1612.6-1859a = 2MASS J16124051-1859282 = GSC 0620901316
[T64] 6 = [MMG98] RX J1612.6-1859b = 2MASS J16123916-1859284 = GSC 0620901312
Currently (11/28/2011), SIMBAD appears to have the "a" and "b"
components flipped. I suggest that they be reversed.
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