Table 1: Main data of the sample of 20 WR galaxies analyzed in this work.

Galaxy RA (2000) Dec (2000) $E_{\rm G} (B-V)^a$ m_B^b M_B^b d^c [O/H]^d Type^e Other

( $\rm h\ m\ s$ ) ( $^\circ\ '\ \hbox{$^{\prime\prime}$ }$ ) (Mpc) (dex) names

NGC 1741 05 01 38.4 -04 15 25 0.051 13.59 -20.01 52.5 8.22 pec HCG 31 AC, Mkn 1089, SBS 0459-043

Mkn 1087 04 49 44.4 +03 20 03 0.063 13.08 -22.14 110.6 8.57^* S0 pec II Zw 23

Haro 15 00 48 35.9 -12 43 07 0.023 13.82 -20.87 86.6 8.37^* (R)SB0 pec? Mkn 960

Mkn 1199 07 20 28.3 +33 32 21 0.054 12.98 -20.68 54.0 8.75^* Sc H II SBS 0720+335

Mkn 5 06 42 15.5 +75 37 33 0.084 14.83 -15.57 12.0 8.07 I? H II SBS 0635+756

IRAS 08208+2816 08 23 55.0 +28 06 14 0.032 15.10 -21.29 190.0 8.42^* Irr ...

IRAS 08339+6517 08 38 23.2 +65 07 15 0.092 12.94 -21.57 78.3 8.45^* Pec LIRG H II ...

POX 4 11 51 11.6 -20 36 02 0.039 14.56 -18.79 45.5 8.03 H II IRAS 11485-2018

UM 420 02 20 54.5 +00 33 24 0.036 17.32 -19.55 237.1 7.95 Compact SBS 0218+003

SBS 0926+606A 09 30 06.5 +60 26 52 0.031 16.45 -17.29 55.9 7.94 BCG, H II ...

SBS 0948+532 09 51 32.0 +52 59 36 0.013 17.93 -18.43 187.4 8.03 Sy ...

SBS 1054+365 10 57 47.0 +36 15 26 0.021 15.46 -14.06 8.0 8.00 NE ...

SBS 1211+540 12 14 02.5 +53 45 18 0.020 17.32 -13.27 13.1 7.65 BCG ...

SBS 1319+579 13 21 10.0 +57 39 41 0.014 15.32 -18.53 28.8 8.05^* H II ...

SBS 1415+437 14 17 01.7 +43 30 13 0.009 15.32 -14.52 9.3 7.58 BCG ...

III Zw 107 23 30 09.9 +25 31 58 0.060 14.36 -20.14 79.6 8.23 Im IV Zw 153, IRAS 23276+2515

Tol 9 10 34 38.7 -28 35 00 0.065 13.92 -19.26 43.3 8.58 E4: H II IRAS 10323-2819,ESO 435-42,Tol 1032-283

Tol 1457-262a 15 00 29.0 -26 26 49 0.158 14.44 -19.73 68.1 8.22^* H II IRAS 14575-2615, ESO 513-IG11

Arp 252 09 44 58.6 -19 43 32 0.049 16.22 -19.35 129.8 8.50^* Gpair pec ESO 566-7 + ESO 566-8

NGC 5253 13 39 55.9 -31 38 24 0.056 10.09 -17.92 4.0^f 8.28^* Im pec H II Haro 10

**Table 1:** Main data of the sample of 20 WR galaxies analyzed in this work.
Galaxy	RA (2000)	Dec (2000)	$E_{\rm G} (B-V)^a$	m_B^b	M_B^b	d^c	[O/H]^d	Type^e	Other
	( $\rm h\ m\ s$ )	( $^\circ\ '\ \hbox{$^{\prime\prime}$ }$ )				(Mpc)	(dex)		names
NGC 1741	05 01 38.4	-04 15 25	0.051	13.59	-20.01	52.5	8.22	pec	HCG 31 AC, Mkn 1089, SBS 0459-043
Mkn 1087	04 49 44.4	+03 20 03	0.063	13.08	-22.14	110.6	8.57^*	S0 pec	II Zw 23
Haro 15	00 48 35.9	-12 43 07	0.023	13.82	-20.87	86.6	8.37^*	(R)SB0 pec?	Mkn 960
Mkn 1199	07 20 28.3	+33 32 21	0.054	12.98	-20.68	54.0	8.75^*	Sc H II	SBS 0720+335
Mkn 5	06 42 15.5	+75 37 33	0.084	14.83	-15.57	12.0	8.07	I? H II	SBS 0635+756
IRAS 08208+2816	08 23 55.0	+28 06 14	0.032	15.10	-21.29	190.0	8.42^*	Irr	...
IRAS 08339+6517	08 38 23.2	+65 07 15	0.092	12.94	-21.57	78.3	8.45^*	Pec LIRG H II	...
POX 4	11 51 11.6	-20 36 02	0.039	14.56	-18.79	45.5	8.03	H II	IRAS 11485-2018
UM 420	02 20 54.5	+00 33 24	0.036	17.32	-19.55	237.1	7.95	Compact	SBS 0218+003
SBS 0926+606A	09 30 06.5	+60 26 52	0.031	16.45	-17.29	55.9	7.94	BCG, H II	...
SBS 0948+532	09 51 32.0	+52 59 36	0.013	17.93	-18.43	187.4	8.03	Sy	...
SBS 1054+365	10 57 47.0	+36 15 26	0.021	15.46	-14.06	8.0	8.00	NE	...
SBS 1211+540	12 14 02.5	+53 45 18	0.020	17.32	-13.27	13.1	7.65	BCG	...
SBS 1319+579	13 21 10.0	+57 39 41	0.014	15.32	-18.53	28.8	8.05^*	H II	...
SBS 1415+437	14 17 01.7	+43 30 13	0.009	15.32	-14.52	9.3	7.58	BCG	...
III Zw 107	23 30 09.9	+25 31 58	0.060	14.36	-20.14	79.6	8.23	Im	IV Zw 153, IRAS 23276+2515
Tol 9	10 34 38.7	-28 35 00	0.065	13.92	-19.26	43.3	8.58	E4: H II	IRAS 10323-2819,ESO 435-42,Tol 1032-283
Tol 1457-262a	15 00 29.0	-26 26 49	0.158	14.44	-19.73	68.1	8.22^*	H II	IRAS 14575-2615, ESO 513-IG11
Arp 252	09 44 58.6	-19 43 32	0.049	16.22	-19.35	129.8	8.50^*	Gpair pec	ESO 566-7 + ESO 566-8
NGC 5253	13 39 55.9	-31 38 24	0.056	10.09	-17.92	4.0^f	8.28^*	Im pec H II	Haro 10

^a Value of the Galactic extinction (Schlegel et al. 1998); ^b corrected for Galactic and internal extinction; ^c except for NGC 5253, the distances were estimated from our optical spectra and correcting for Galactic Standard of Rest (see Paper II); ^d oxygen abundance, in units of 12 + log(O/H), derived in this work for each galaxy (see Paper II). If several regions were analyzed in the same galaxy (indicated by a star), the highest oxygen abundance derived using $T_{\rm e}$ is shown; ^e morphological type as indicated by NED; ^f distance obtained by Karachentsev et al. (2004).

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