**Table A.1:** Parameters for the brightest stellar members of Tr 14. Values include: luminosity^a (L); effective temperature^a ( $T_{{\rm eff}}$ ); FUV luminosity^b ( $L_{{\rm FUV}}$ ); ionizing photon flux per second^b ( $N_{\rm L}$ ), stellar wind terminal velocity^c ( $v_{\infty }$ ); stellar wind mass-loss rate^d ( M) and the mechanical luminosity (L_W) given by $0.5 \times Mv_{\infty }^2$ .
Star^a	Spectral^a	L	$T_{{\rm eff}}$	$L_{{\rm FUV}}$	$N_{\rm L}$	$v_{\infty }$	M	L_W
	Type	10⁵ $L_{\odot}$	10⁴ K	10⁵ $L_{\odot}$	10⁴⁷ s^-1	km s^-1	10^-7 $M_\odot$ yr^-1	10⁴³ erg yr^-1
HD93129A	O3I	47.9	4.7	22.4	594	3000	533	477
HD93160	O6III	9.1	4.0	5.5	90	2500	23	14
HD93161W	O6.5V	5.5	4.0	3.3	55	2600	11	8
HD93161E	O6.5V	10.0	4.3	4.7	163	2600	27	19
HD93128	O3V	15.5	5.3	5.6	214	3200	48	49
HD93129B	O3V	13.5	5.3	4.9	186	3200	40	41
7	O6.5V	2.4	4.0	1.4	24	2600	3.8	2.6
8	O6V	3.9	4.1	2.3	35	2600	7.5	5.0
11	O8V	2.0	3.6	1.3	12	1900	3.6	1.3
13	O9V	0.72	3.3	0.5	6	1500	1.1	0.25
15	O9V	1.0	3.3	0.6	8	1500	1.6	0.36
23	09V	0.22	3.3	0.7	2	1500	0.2	0.05
25	09V	0.3	3.3	0.2	2	1500	0.3	0.06
Total		$\sim$ 110		$\sim$ 50	$\sim$ 1400			$\sim$ 600

^a Taken from Vázquez et al. (1996).
^b Derived using stellar models of Kurucz (1997).
^c Taken from Table 1 in Kudritzki & Puls (2000).
^d According to the wind-momentum luminosity relation given in Eq. (10) by Kudritzki & Puls (2000).

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