2 The sample

   

Table 1: The target galaxies.

VCC	NGC/IC	UGC	RA(1950)	Dec	a	b	Vel	Clust	Dist	$\theta$	Type	$m_{\rm pg}$	$B_{\rm T}^0$	$H_{\rm T}$
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)	(13)	(14)	(15)
24	-	-	120802.5	120220.0	1.00	0.37	1289	M	32	4.99	BCD	14.95	15.79	12.68
144	-	-	121245.0	60220.0	0.63	0.32	2014	W	32	7.66	BCD	15.31	15.18	12.95
213	3094	7305	121423.4	135413.0	0.93	0.71	-162	N	17	3.60	dS/BCD	14.26	14.74	11.52
324	-	7354	121636.5	40758.0	1.35	1.15	1524	S	17	9.01	BCD	14.78	14.30	11.83
404	-	7387	121743.8	42844.0	1.71	0.21	1733	S	17	8.60	Scd	15.00	13.90	-
428	-	-	121807.9	140959.0	0.39	0.11	794	A	17	2.89	BCD	17.50	-	-
459	-	-	121839.6	175457.0	0.84	0.36	2108	A	17	5.74	BCD	14.95	-	12.72
513	-	-	121924.0	23718.0	0.73	0.61	1832	S	17	10.28	BCD	15.10	-	12.33
655	4344	7468	122105.8	174906.0	1.55	1.55	1147	A	17	5.44	Spec/BCD	13.21	13.58	10.66
787	4376	7498	122245.1	60104.0	1.84	1.07	1136	B	23	6.79	Scd	13.69	13.38	11.08
793	-	-	122249.8	132060.0	0.47	0.34	1906	A	17	1.50	Im	16.74	17.26	14.85
802	-	-	122257.0	134624.0	0.64	0.21	-215	A	17	1.71	BCD	17.40	17.61	14.64
810	-	-	122301.8	133006.0	0.77	0.77	-340	A	17	1.53	dE	16.95	17.06	14.04
815	-	-	122305.4	132512.0	0.66	0.53	-700	A	17	1.47	dE	16.10	16.59	-
846	-	-	122318.0	132818.0	0.89	0.80	-730	A	17	1.46	dE	16.20	16.58	-
848	-	-	122319.8	60506.0	1.16	0.98	1537	B	23	6.70	Im/BCD	14.72	15.18	13.35
873	4402	7528	122335.3	132320.0	3.95	1.16	234	A	17	1.36	Sc	12.56	11.74	8.58
1297	-	-	122800.0	124600.0	0.51	0.45	1486	A	17	0.12	E	14.33	14.42	10.25
1313	-	-	122816.6	121916.0	0.45	0.20	1254	A	17	0.35	BCD	17.15	17.30	15.60
1316	4486	7654	122817.6	124002.0	11.00	11.00	1292	A	17	0.00	E	9.58	9.82	6.21
1369	-	-	122901.2	122024.0	0.50	0.20	1022	A	17	0.37	dE	17.30	-	-
1437	-	-	123001.2	92658.0	0.59	0.45	1160	S	17	3.25	BCD	15.12	-	12.21
1488	3487	-	123041.4	94030.0	1.26	0.53	1157	S	17	3.05	E	14.76	-	-
1725	-	-	123509.4	85001.0	1.55	0.97	1068	S	17	4.19	Sm/BCD	14.51	14.61	12.13
1804	-	-	123708.4	94024.0	0.75	0.20	1898	E	17	3.70	Im/BCD	15.63	16.30	13.31
1955	4641	7889	124036.5	121928.0	1.36	1.07	2012	E	17	3.02	Spec/BCD	14.32	-	11.16
2007	3716	-	124215.6	82254.0	0.78	0.41	1857	E	17	5.49	Im/BCD	15.20	-	13.33
2033	-	-	124333.0	84454.0	0.73	0.73	1486	E	17	5.42	BCD	14.65	15.60	13.06
2034	-	-	124336.6	102612.0	0.78	0.52	1500	E	17	4.36	Im	15.82	16.24	13.23
2037	-	-	124343.8	102848.0	0.88	0.38	1142	E	17	4.37	Im/BCD	15.92	16.20	12.55
2045	-	-	124424.0	102724.0	1.29	0.43	-	E	17	4.52	dE	16.33	-	-

Galaxies observed in this work have been selected from the Virgo Cluster Catalogue (VCC) of Binggeli et al. (1985), which is complete to the optical B magnitude $m_{\rm pg} = 18.0$. We selected all BCD galaxies (BCD, Im/BCD, Sm/BCD) classified as cluster members, possible members or belonging to the W, W', M clouds or to the southern extension (Binggeli et al. 1985, 1993).

Among the 67 BCD Virgo cluster members matching these criteria, 34 objects (51%) either included in the present work or in Paper I have an H$\alpha$ measurement. If limited to the ISO sample described in Boselli et al. (1997), 16 out 18 BCD galaxies (89%) have H$\alpha$ data.

Given the large field of view of the WFC at the INT, some galaxies not matching the selection criteria were serendipitously observed in the fields of other targets.

The target galaxies, as well as the serendipitously observed objects, are listed in Table 1, arranged as follow:

• Column 1: VCC designation, from Binggeli et al. (1985);
• Column 2: NGC or IC name;
• Column 3: UGC name (Nilson 1973);
• Columns 4 and 5: (B1950.0) celestial coordinates, from NED;
• Columns 6 and 7: major an minor optical diameters measured on the du Pont plates at the faintest detectable isophote;
• Column 8: heliocentric velocity, in kms^-1, from the VCC;
• Column 9: cluster membership as defined in Gavazzi et al. (1999);
• Column 10: distance, in Mpc. Distances to the various substructures of Virgo are as given in Gavazzi et al. (1999);
• Column 11: angular distance from the cluster centre, in degrees;
• Column 12: morphological type as given in the VCC;
• Column 13: photographic magnitude from the VCC;
• Column 14: optical magnitude determined and corrected for dust extinction as described in Gavazzi & Boselli (1996);
• Column 15: total extrapolated H band magnitude, uncorrected for extinction, determined as described in Gavazzi et al. (2000a). For galaxies observed in the K band (Boselli et al. 1997), H magnitudes are determined using the observed colour index H-K when available, or assuming an average H-K=0.25.