V1233 Tau = HD 27989 = BU 1185 = vB 58
 Variable of BY Dra type, G4V
 BU 1185, P = 28y, a = 0.25", motion retrograde. Also SB Griffin et al. (1988).	
 Malkov et al. (2012) derived masses of 2.01, 2.00, and 0.98 Msun, respectively.
 prob_member = 1 (Perryman+ 1998)
----------------------------------------------------------------------------------------------
61 Tau = HD 27697 = Chr 262 = BUP 55 = vB 41
 SB (P=530d)/Occ. bin./RG (K0III) -> poss. resolved (Mason et al. 2012)
 The primary is a long-period spectroscopic and occultation binary. Aa,Ab: If real, this pair 
 could be the 530.1-d spectroscopic binary (Griffin 2012). If this additional component is 	 
 confirmed, vB41 will be the second K0 giant binary that has been resolved in the Hyades. 
 prob_member = 1 (Perryman+ 1998)
----------------------------------------------------------------------------------------------
54 Tau = HD 27371 = BLM 1 = WDS 04198+1538 = vB 28
 IB/SB/RG (G9.5IIIab) -> SB1 (ApJ 142) resolved by speckle interferometry (Mason et al. 2012)
 prob_member = 1 (Perryman+ 1998)
----------------------------------------------------------------------------------------------
V1099 Tau = 48 Tau =  HD 26911 = BUP 51 A (wide VDS) = vB 20
 Ellipsoidal variable, F6III -> unresolved (Hartkopf et al. 1984), Te=6624 K, log(g)=4.03
 v.sini= 50; prob_member = 1 (Perryman+ 1998)
----------------------------------------------------------------------------------------------
V696 Tau = 58 Tau = HD 27459 = vB 33
 DSCT (Jian-ning et al. 1996), A9IV; v.sini=82, Te=7982 K
 prob_member = 1 (Perryman+ 1998)
----------------------------------------------------------------------------------------------
V775 Tau = 60 Tau = HD 27628 = vB 38 = BUP 54 A (wide VDS)
 DSCT (Horan 1979)/SB1, P=2.1436d (Griffin 2012), A9IV/A3m ; v.sini=32, Te=7443 K
 prob_member = 1 (Perryman+ 1998)
----------------------------------------------------------------------------------------------
V483 Tau = 57 Tau = HD 27397 = vB 30
 DSCT (Jian-ning et al. 1996)/SB1, P=2.486 d (Kaye 1999) A/Fm; v.sini=102, Te=7525 K
 Paparo et al. (2000) identified 8 frequencies among 12 [7-25 c/d], of which 2 are found in the low 
 frequency domain. If the mass ratio is obtained from the binary motion, and the chemical composition 
 & distance based on the membership of Hyades are assumed, 57 Tau is a good candidate for modelling.
 prob_member = 1 (Perryman+ 1998)
----------------------------------------------------------------------------------------------
NB: The above 3 DSCT stars are in the paper by Suarez et al. A&A 390, 523-531 (2002) 
Star 		Mv 	B2-V1 	${A_{{\rm osc}}}$    ${{V}~\sin~i}$ 	Sp 	Weight 	Cluster
HD 27397 	2.33 	0.076 	0.018 	100 	F0V 	2 	Hyades
HD 27459 	1.87 	0.025 	0.010 	70 	A9V 	2 	Hyades
HD 27628 	2.45 	0.101 	0.010 	40 	Am 	2 	Hyades