Obscured clusters - III. Follow-up observations of Mercer 23

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Volume 516 (June-July 2010)

A&A, 516 (2010) A35

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Table 3:

Physical parameters of spectroscopically analyzed stars in Mercer 23.
Star	Sp Typ	$\log L$	$\dot{\cal M}$ ^a	$T_{\rm eff}$	$\log g$	E(J-K_S)	( $K_{\rm S}$ - $M_{K_{\rm S}})_0$
		[ $L_\odot$ ]	[ ${\cal M_\odot}{\rm yr}^{-1}$ ]	[K]
Obj1	O5.5 I	6.21	$1.5\times 10^{-5}$	35 000	3.25	1.30	14.20
Obj2	WNL7-8	6.56	$2.4\times 10^{-5}$	38 000	3.00
Obj3	B1/2	4.39		32 500	4.25	1.29	13.64
Obj4	O9/B0	4.65		32 500	4.25	1.32	14.55
Obj5	B3/4					1.38	14.49
Obj6	O6 If	5.86	$2.1\times 10^{-5}$	34 000	3.25	1.38	13.67
Obj7	B3/4					1.35	13.84
Obj9	B1/2	4.33		30 000	4.25	1.37	13.59
Obj10	O9/B0	4.72		30 000	4.25	1.39	14.46
Obj11	O9/B0	4.64		30 000	4.25	1.36	14.36

Notes. ^(a) Only objects 1, 2 and 6 had a modeled wind component providing a mass loss rate The value given in the table corresponds to a smooth wind. H/He ratio, $\beta$ parameter, clumping factor (f) and $V_{\infty}$ , needed for the wind models and errors, are given in Sect. 4.4.

Source LaTeX | All tables | In the text

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