**Table 2:** Derived physical parameters for program stars.
Star	$T_{\rm eff}$	$\log g$	$\xi$	V_r (hel)	$V ({\it LSR})$
	(K)		$\rm (km~s^{-1})$	$\rm (km~s^{-1})$	$\rm (km~s^{-1})$
HD 10285	7750	1.5	3.5	-69.9	-64.2
HD 25291	7250	1.5	3.5	-19.2	-18.3
HD 27381	7500	1.0	4.0	-5.4	-11.4
HD 137569	12 500	3.0	8.0	-45.7	-30.2
HD 137569 $^\dag$	12 000	3.0	7.0	-55.2	-39.6
HD 172324^*	11 000	2.5	5.0	-126.1	-106.4
	11 500	2.5	7.5	-117.3	-97.5
	10 500	2.5	5.4	-139.0	-119.3
	10 500	2.5	6.8	-105.2	-85.7
				-152.1	-132.5⁺
HD 10132	5000	2.0	1.0	-70.2	-64.5
HD 12533	4250	2.0	1.8	-11.2	-10.9
HD 159251	4800	2.75	1.2	-39.2	-27.6

$\dag$ - From McDonald spectrum obtained in 2004. * - Four independent analyses carried out for different epochs are included. The first two are from Paper I. The second two are from the present work. + Radial velocity measured on a 17 000 resolution spectrum obtained at San Pedro Mártir Observatory on November 18, 2000.

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations and data reduction
	3 Derived elemental abundances
	4 Conclusions
	References