Table 2: Empirical population synthesis results of percentage contributions from stars of all ages and metallicities to $F_{\lambda 5870}$ , for two sample galaxies. The "evolutionary paths'' favored by the analysis are highlighted (see text).
a) Mrk 385 Age (yr) [ $Z/Z_{\odot}$ ] b) I Zw 97 Age (yr) [ $Z/Z_{\odot}$ ]

HII E7 5E7 E8 5E8 E9 5E9 E10 HII E7 5E7 E8 5E8 E9 5E9 E10

2.0 1.8 2.1 .3 .2 .2 .5 0.6 .3 1.6 2.6 1.7 .3 .2 .1 0.6

2.1 2.3 2.9 .5 .3 .3 .6 0.3 .4 1.9 3.3 3.0 .6 .3 .1 0.3

1.5 3.3 3.9 .8 .5 .5 .8 0.0 8.0 .8 5.9 9.8 5.9 1.7 .6 .2 0.0

8.8 4.0 6.0 6.9 11.7 1.7 1.5 1.8 -0.5 .5 1.9 3.3 1.8 2.8 1.2 .7 -0.5

4.5 3.4 3.4 -1.0 4.7 1.9 1.5 -1.0

5.5 5.4 -1.5 6.9 7.0 -1.5

8.1 -2.0 16.7 -2.0

**Table 2:** Empirical population synthesis results of percentage contributions from stars of all ages and metallicities to $F_{\lambda 5870}$ , for two sample galaxies. The "evolutionary paths'' favored by the analysis are highlighted (see text).
a) Mrk 385 Age (yr)	[ $Z/Z_{\odot}$ ]		b) I Zw 97 Age (yr)	[ $Z/Z_{\odot}$ ]
HII	E7	5E7	E8	5E8	E9	5E9	E10		HII	E7	5E7	E8	5E8	E9	5E9	E10
	2.0	1.8	2.1	.3	.2	.2	.5	0.6		.3	1.6	2.6	1.7	.3	.2	.1	0.6
	2.1	2.3	2.9	.5	.3	.3	.6	0.3		.4	1.9	3.3	3.0	.6	.3	.1	0.3
	1.5	3.3	3.9	.8	.5	.5	.8	0.0	8.0	.8	5.9	9.8	5.9	1.7	.6	.2	0.0
8.8	4.0	6.0	6.9	11.7	1.7	1.5	1.8	-0.5		.5	1.9	3.3	1.8	2.8	1.2	.7	-0.5
					4.5	3.4	3.4	-1.0						4.7	1.9	1.5	-1.0
						5.5	5.4	-1.5							6.9	7.0	-1.5
							8.1	-2.0								16.7	-2.0

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