Table 9: A compilation of luminosities and abundances for a sample of nearby dwarf star-forming galaxies. The abundances listed in Col. 6 have been taken from the publication the number of which is given in Col. 8 and have been computed with the method identified in Col. 7: 1 = direct method but temperature not computed, assumed $T_{{\rm e}}=10~000~{\rm K}$ ; 2 = direct method; 3 = unknown. The publication numbers correspond to the following papers: (1) Hunter & Hoffman 1999; (2) Hidalgo-Gàmez & Olofsson (2002); (3) Vigroux et al. (1987); (4) Storchi-Bergmann et al. (1994); (5) Martin (1997); (6) Kobulnicky & Skillman (1998); (7) average $\pm 1\sigma$ of abundances from the following papers: Izotov & Thuan (2004), Hunter & Hoffman (1999), Thuan & Izotov (2005a,b), Alloin et al. (1979), Shi et al. (2005); (8) Izotov & Thuan (1998); (9) Shi et al. (2005); (10) Thuan & Izotov (2005a,b); (11) van Zee et al. (1997); (12) Izotov & Thuan (1998); (13) Izotov & Thuan (1997). Most distances were taken from Hunter & Elmegreen (2006; HE06): in Col. 10 the label ``h'' means that these authors computed the distance from the recession velocity, while a number identifies their source publication for the distance. If no distance is given in HE06, then we derived it using the NED velocity and $H_{\circ}=72~{\rm km}~{\rm s}^{-1}~{\rm Mpc}^{-1}$ . Finally the DDO 43 distance is from Sharina (2004, private communication; cited in Karachentsev et al. 2004).
Name Alt. name RA Dec $v_{{\rm r}}$ (NED) $12+\log~({\rm O/H})$ M Ref. D source ${\it A}_{{\rm tot}}$ ${\it H}_{{\rm tot}}$

J2000 [km s^-1] [Mpc] of D [mag] [mag]

MRK 600 02:51:04.6 +04:27:14 $1008\pm1$ $7.83\pm0.01$ 2 12 15.7 h 0.038 $14.38\pm0.19$

NGG 1156 02:59:42.2 +25:14:14 $375\pm1$ 8.23 $\pm$ ... 3 3 7.8 25 0.129 $9.83\pm0.01$

NGG 1569 04:30:49.0 +64:50:53 $-104\pm4$ 8.37 $\pm$ ... 2 4 2.5 41 0.403 $9.40\pm0.02$

DDO 43 UGC 03860 07:28:17.4 +40:46:11 $354\pm1$ $8.30\pm0.09$ 1 1 7.8 rg 0.034 $13.00\pm0.17$

Haro 23 UGCA 201 10:06:18.1 +28:56:40 1 $363\pm7$ 8.35 $\pm$ ... 2 7 20.2 h 0.014 $11.77\pm0.13$

MRK 33 UGC 05720 10:32:31.9 +54:24:04 $1430\pm4$ 8.35 $\pm$ ... 2 9 ... n 0.007 $10.70\pm0.04$

$10.84\pm0.03$

Haro 3 NGG 3353 10:45:22.4 +55:57:37 $944\pm5$ $8.3\pm0.10$ 2 7 15.5 h 0.004 $10.71\pm0.03$

$10.83\pm0.02$

$10.74\pm0.06$

Haro 4 UGCA 225 11:04:58.5 +29:08:22 $646\pm5$ $7.81\pm0.02$ 2 8 9.5 h 0.017 $14.03\pm0.03$

$13.75\pm0.36$

MRK 178 UGC 06541 11:33:28.9 +49:14:14 $250\pm1$ $7.93\pm0.02$ 2 10 3.9 27 0.010 $12.47\pm0.15$

NGG 3738 11:35:48.8 +54:31:26 $229\pm4$ $8.23\pm0.01$ 2 5 4.9 27 0.006 $9.63\pm0.04$

MRK 1307 UGC 06850 11:52:37.3 -02:28:10 $1055\pm12$ $7.95\pm0.01$ 2 8 ... n 0.011 $12.87\pm0.02$

NGG 4214 12:15:39.2 +36:19:37 $291\pm3$ $8.25\pm0.05$ 2 6 2.9 33 0.013 $8.26\pm0.03$

Haro 8 UGC 07354 12:19:09.9 +03:51:21 $1526\pm4$ 8.12 $\pm$ ... 2 9 22.2 h 0.010 $11.97\pm0.14$

Haro 29 UGCA 281 12:26:16.0 +48:29:37 $281\pm4$ $7.82\pm0.01$ 2 10 5.4 h 0.009 $13.54\pm0.22$

4.72 100

LeoI HH DDO 168 13:14:27.9 +45:55:09 $192\pm1$ $7.5\pm0.20$ 2 2 3.5 h 0.009 $11.91\pm0.12$

4.33 101

Haro 38 UGC 08578 13:35:35.6 +29:13:01 $853\pm7$ 8.02 $\pm$ ... 2 9 13.7 h 0.007 $14.03\pm0.17$

Haro 43 14:36:08.8 +28:26:59 $1912\pm10$ $8.17\pm0.10$ 2 11 30.5 h 0.011 $13.66\pm0.17$

MRK 829 UGC 09560 14:50:56.5 +35:34:18 $1180\pm2$ 7.69 $\pm$ ... 2 9 ... n 0.007 $13.07\pm0.08$

$13.05\pm0.04$

II Zw 71 UGC 09562 14:51:14.4s +35:32:32 $1292\pm18$ 8.24 $\pm$ ... 2 9 ... n 0.007 $11.89\pm0.05$

$12.14\pm0.03$

MRK 487 UGCA 410 15:37:04.2s +55:15:48 $665\pm7$ $8.10\pm0.04$ 2 13 ... n 0.008 $13.35\pm0.11$

$13.25\pm0.03$

MRK 297 NGC 6052 16:05:12.9s +20:32:32 $4716\pm4$ 8.34 $\pm$ ... 2 9 ... n 0.044 $10.92\pm0.06$

**Table 9:** A compilation of luminosities and abundances for a sample of nearby dwarf star-forming galaxies. The abundances listed in Col. 6 have been taken from the publication the number of which is given in Col. 8 and have been computed with the method identified in Col. 7: 1 = direct method but temperature not computed, assumed $T_{{\rm e}}=10~000~{\rm K}$ ; 2 = direct method; 3 = unknown. The publication numbers correspond to the following papers: (1) Hunter & Hoffman 1999; (2) Hidalgo-Gàmez & Olofsson (2002); (3) Vigroux et al. (1987); (4) Storchi-Bergmann et al. (1994); (5) Martin (1997); (6) Kobulnicky & Skillman (1998); (7) average $\pm 1\sigma$ of abundances from the following papers: Izotov & Thuan (2004), Hunter & Hoffman (1999), Thuan & Izotov (2005a,b), Alloin et al. (1979), Shi et al. (2005); (8) Izotov & Thuan (1998); (9) Shi et al. (2005); (10) Thuan & Izotov (2005a,b); (11) van Zee et al. (1997); (12) Izotov & Thuan (1998); (13) Izotov & Thuan (1997). Most distances were taken from Hunter & Elmegreen (2006; HE06): in Col. 10 the label ``h'' means that these authors computed the distance from the recession velocity, while a number identifies their source publication for the distance. If no distance is given in HE06, then we derived it using the NED velocity and $H_{\circ}=72~{\rm km}~{\rm s}^{-1}~{\rm Mpc}^{-1}$ . Finally the DDO 43 distance is from Sharina (2004, private communication; cited in Karachentsev et al. 2004).
Name	Alt. name	RA	Dec	$v_{{\rm r}}$ (NED)	$12+\log~({\rm O/H})$	M	Ref.	D	source	${\it A}_{{\rm tot}}$	${\it H}_{{\rm tot}}$
		J2000	[km s^-1]				[Mpc]	of D	[mag]	[mag]
MRK 600		02:51:04.6	+04:27:14	$1008\pm1$	$7.83\pm0.01$	2	12	15.7	h	0.038	$14.38\pm0.19$
NGG 1156		02:59:42.2	+25:14:14	$375\pm1$	8.23 $\pm$ ...	3	3	7.8	25	0.129	$9.83\pm0.01$
NGG 1569		04:30:49.0	+64:50:53	$-104\pm4$	8.37 $\pm$ ...	2	4	2.5	41	0.403	$9.40\pm0.02$
DDO 43	UGC 03860	07:28:17.4	+40:46:11	$354\pm1$	$8.30\pm0.09$	1	1	7.8	rg	0.034	$13.00\pm0.17$
Haro 23	UGCA 201	10:06:18.1	+28:56:40	1 $363\pm7$	8.35 $\pm$ ...	2	7	20.2	h	0.014	$11.77\pm0.13$
MRK 33	UGC 05720	10:32:31.9	+54:24:04	$1430\pm4$	8.35 $\pm$ ...	2	9	...	n	0.007	$10.70\pm0.04$
											$10.84\pm0.03$
Haro 3	NGG 3353	10:45:22.4	+55:57:37	$944\pm5$	$8.3\pm0.10$	2	7	15.5	h	0.004	$10.71\pm0.03$
											$10.83\pm0.02$
											$10.74\pm0.06$
Haro 4	UGCA 225	11:04:58.5	+29:08:22	$646\pm5$	$7.81\pm0.02$	2	8	9.5	h	0.017	$14.03\pm0.03$
											$13.75\pm0.36$
MRK 178	UGC 06541	11:33:28.9	+49:14:14	$250\pm1$	$7.93\pm0.02$	2	10	3.9	27	0.010	$12.47\pm0.15$
NGG 3738		11:35:48.8	+54:31:26	$229\pm4$	$8.23\pm0.01$	2	5	4.9	27	0.006	$9.63\pm0.04$
MRK 1307	UGC 06850	11:52:37.3	-02:28:10	$1055\pm12$	$7.95\pm0.01$	2	8	...	n	0.011	$12.87\pm0.02$
NGG 4214		12:15:39.2	+36:19:37	$291\pm3$	$8.25\pm0.05$	2	6	2.9	33	0.013	$8.26\pm0.03$
Haro 8	UGC 07354	12:19:09.9	+03:51:21	$1526\pm4$	8.12 $\pm$ ...	2	9	22.2	h	0.010	$11.97\pm0.14$
Haro 29	UGCA 281	12:26:16.0	+48:29:37	$281\pm4$	$7.82\pm0.01$	2	10	5.4	h	0.009	$13.54\pm0.22$
								4.72	100
LeoI HH	DDO 168	13:14:27.9	+45:55:09	$192\pm1$	$7.5\pm0.20$	2	2	3.5	h	0.009	$11.91\pm0.12$
								4.33	101
Haro 38	UGC 08578	13:35:35.6	+29:13:01	$853\pm7$	8.02 $\pm$ ...	2	9	13.7	h	0.007	$14.03\pm0.17$
Haro 43		14:36:08.8	+28:26:59	$1912\pm10$	$8.17\pm0.10$	2	11	30.5	h	0.011	$13.66\pm0.17$
MRK 829	UGC 09560	14:50:56.5	+35:34:18	$1180\pm2$	7.69 $\pm$ ...	2	9	...	n	0.007	$13.07\pm0.08$
											$13.05\pm0.04$
II Zw 71	UGC 09562	14:51:14.4s	+35:32:32	$1292\pm18$	8.24 $\pm$ ...	2	9	...	n	0.007	$11.89\pm0.05$
											$12.14\pm0.03$
MRK 487	UGCA 410	15:37:04.2s	+55:15:48	$665\pm7$	$8.10\pm0.04$	2	13	...	n	0.008	$13.35\pm0.11$
											$13.25\pm0.03$
MRK 297	NGC 6052	16:05:12.9s	+20:32:32	$4716\pm4$	8.34 $\pm$ ...	2	9	...	n	0.044	$10.92\pm0.06$

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