2 Observations

2.1 The sample

The UCM sample of galaxies is divided into two lists. Galaxies of List I (Zamorano et al. [1994]) and List II (Zamorano et al. [1996]) were found in fields in a region of the sky from right ascension 12$^{\rm h}$ to 16$^{\rm h}$ and from 22$^{\rm h}$ to 2$^{\rm h}$, respectively. The surveyed region covered a 10 $\hbox{$^\circ$ }$ width strip centered at declination 20 $\hbox{$^\circ$ }$ for both lists. A summary of the main features of each galaxy is listed in Table 1, including the names, redshifts, morphological and spectral types, Gunn r magnitudes and B-V colour excesses as obtained from the Balmer decrements.

 

Table 1: The sample of galaxies in the UCM survey Lists I and II

UCM name	z	MphT	SpT	$m_{\rm r}$	E(B-V)	UCM name	z	MphT	SpT	$m_{\rm r}$	E(B-V)
(1)	(2)	(3)	(4)	(5)	(6)	(1)	(2)	(3)	(4)	(5)	(6)
0000+2140	0.0238	-	HIIH	-	1.204	1255+2734	0.0234	Irr	SBN	15.99	0.715
0003+2200	0.0224	Sc+	DANS	16.16	0.867	1256+2717	0.0273	-	DHIIH	-	0.447
0003+2215	0.0223	-	SBN	-	1.008	1256+2732	0.0234	S0	SBN	15.40	-
0003+1955	0.0278	-	Sy1	-	-	1256+2701	0.0247	Irr	HIIH	16.32	0.220
0005+1802	0.0187	-	SBN	-	1.244	1256+2910	0.0279	Sb	SBN	15.10	-
0006+2332	0.0159	-	HIIH	-	0.644	1256+2823	0.0307	Sb	SBN	15.11	0.644
0013+1942	0.0272	Sc+	HIIH	16.39	0.276	1256+2754	0.0172	-	SBN	-	0.645
0014+1829	0.0182	Sa	HIIH	16.01	1.473	1256+2722	0.0287	Sc+	DANS	16.05	0.928
0014+1748	0.0182	SBb	SBN	14.13	0.806	1257+2808	0.0181	Sa	SBN	15.45	1.344
0015+2212	0.0198	Sa	HIIH	15.59	0.215	1258+2754	0.0253	Sb	SBN	15.38	1.020
0017+1942	0.0281	Sc+	HIIH	15.34	0.357	1259+2934	0.0239	Sb	Sy2	14.18	0.984
0017+2148	0.0189	-	HIIH	-	0.575	1259+3011	0.0307	Sa	SBN	15.36	0.682
0018+2216	0.0169	Sb	DANS	15.82	0.136	1259+2755	0.0235	Sa	SBN	14.45	0.913
0018+2218	0.0220	-	SBN	-	-	1300+2907	0.0219	Sb	HIIH	16.69	0.620
0019+2201	0.0191	Sc+	DANS	15.54	0.438	1301+2904	0.0266	Sb	HIIH	15.18	0.207
0022+2049	0.0185	Sb	HIIH	14.45	0.901	1302+2853	0.0237	Sa	DHIIH	15.77	0.621
0023+1908	0.0251	-	HIIH	-	0.409	1302+3032	0.0342	-	HIIH	-	0.595
0034+2119	0.0315	-	SBN	-	0.684	1303+2908	0.0261	Irr	HIIH	16.26	-
0037+2226	0.0204	-	SBN	-	0.615	1304+2808	0.0210	Sa	SBN	14.85	0.114
0038+2259	0.0464	Sa	SBN	15.07	0.810	1304+2830	0.0217	BCD	DHIIH	17.72	0.372
0039+0054	0.0191	-	SBN	-	-	1304+2907	0.0159	Irr	-	14.55	-
0040+0257	0.0367	Sc+	DANS	16.76	-	1304+2818	0.0244	Sc+	SBN	14.88	0.111
0040+2312	0.0254	-	SBN	-	-	1306+2938	0.0211	Sb	SBN	14.80	0.501
0040+0220	0.0173	Sb	DANS	16.39	0.378	1306+3111	0.0168	Sc+	DANS	15.32	-
0040-0023	0.0142	LINER	-	-	-	1307+2910	0.0183	SBb	SBN	13.05	0.970
0041+0134	0.0169	-	-	-	-	1308+2958	0.0223	Sc+	SBN	14.46	1.313
0043+0245	0.0180	-	HIIH	-	0.950	1308+2950	0.0246	SBb	SBN	13.92	1.381
0043-0159	0.0161	-	SBN	-	-	1310+3027	0.0234	Sa	DANS	15.70	-
0044+2246	0.0253	Sb	SBN	14.83	1.384	1312+3040	0.0210	SBa	SBN	14.67	0.474
0045+2206	0.0203	-	HIIH	-	0.493	1312+2954	0.0230	Sc+	SBN	15.14	1.087
0047+2051	0.0577	Sc+	SBN	16.00	0.598	1313+2938	0.0380	Sa	HIIH	16.14	-
0047-0213	0.0144	Sa	DHIIH	14.82	0.857	1314+2827	0.0253	Sa	SBN	15.54	0.749
0047+2413	0.0347	Sa	SBN	14.69	1.059	1320+2727	0.0247	Sb	DHIIH	16.79	0.205
0047+2414	0.0347	-	SBN	-	0.592	1324+2926	0.0172	BCD	BCD	16.85	0.022
0049-0006	0.0377	BCD	BCD	18.22	0.006	1324+2651	0.0249	S0	SBN	14.27	0.628
0049+0017	0.0140	Sc+	DHIIH	16.48	0.088	1331+2900	0.0356	BCD	BCD	18.49	0.013
0049-0045	0.0048	-	HIIH	-	0.416	1428+2727	0.0149	Sc+	HIIH	14.38	0.150
0050+0005	0.0346	Sa	HIIH	15.72	0.438	1429+2645	0.0328	Sc+	DHIIH	16.91	0.105
0050+2114	0.0245	Sa	SBN	14.66	0.813	1430+2947	0.0290	S0	HIIH	15.95	0.308
0051+2430	0.0173	-	SBN	-	1.040	1431+2854	0.0310	Sb	SBN	14.83	-
0054-0133	0.0512	-	SBN	-	-	1431+2702	0.0384	Sb	HIIH	16.41	0.271
0054+2337	0.0164	-	HIIH	-	0.667	1431+2947	0.0219	BCD	BCD	17.40	-
0056+0044	0.0183	Irr	DHIIH	16.58	0.079	1431+2814	0.0320	Sa	DANS	15.85	-
0056+0043	0.0189	Sc+	DHIIH	16.07	0.331	1432+2645	0.0307	SBb	SBN	14.59	0.914
0119+2156	0.0583	Sc+	Sy2	15.44	-	1440+2521S	0.0314	Sb	SBN	16.16	0.292
0121+2137	0.0345	Sc+	SBN	15.41	0.703	1440+2511	0.0333	Sb	SBN	15.87	1.018
0129+2109	0.0344	-	LINER	-	-	1440+2521N	0.0315	Sa	SBN	15.74	0.773
0134+2257	0.0353	-	SBN	-	0.892	1442+2845	0.0110	Sb	SBN	14.66	0.681
0135+2242	0.0363	S0	DANS	16.05	0.976	1443+2714	0.0290	Sa	Sy2	14.75	1.008
0138+2216	0.0591	-	-	-	-	1443+2844	0.0279	SBc	SBN	14.91	-
0141+2220	0.0174	Sb	DANS	15.67	0.742	1443+2548	0.0351	Sc+	SBN	15.12	0.726
0142+2137	0.0362	SBb	Sy2	14.19	0.537	1444+2923	0.0281	S0	DANS	15.77	0.785
0144+2519	0.0414	SB(r)	SBN	14.78	1.033	1452+2754	0.0339	Sb	SBN	15.43	0.733
0147+2309	0.0194	Sa	HIIH	15.82	0.486	1506+1922	0.0205	Sb	HIIH	14.87	0.453
0148+2124	0.0169	BCD	BCD	16.32	0.174	1513+2012	0.0369	S0	SBN	14.96	0.540
0150+2032	0.0323	Sc+	HIIH	16.28	0.085	1537+2506N	0.0231	SBb	HIIH	14.36	0.225
0156+2410	0.0134	Sc+	DANS	14.55	0.702	1537+2506S	0.0231	SBa	HIIH	15.50	0.357
0157+2413	0.0177	Sc+	Sy2	13.65	0.725	1557+1423	0.0275	Sb	SBN	15.82	0.374
0157+2102	0.0106	Sb	HIIH	14.39	0.474	1612+1308	0.0114	BCD	BCD	17.48	0.031
0159+2326	0.0178	Sc+	DANS	14.72	-	1646+2725	0.0339	Sc+	DHIIH	17.87	0.288
0159+2354	0.0170	Sa	HIIH	16.07	0.565	1647+2950	0.0290	SBc+	SBN	14.68	0.736
1246+2727	0.0199	-	HIIH	-	0.775	1647+2729	0.0366	Sb	SBN	15.22	0.895
1247+2701	0.0231	Sc+	DANS	15.97	0.515	1647+2727	0.0369	Sa	SBN	16.29	0.678
1248+2912	0.0217	-	SBN	-	0.715	1648+2855	0.0308	Sa	HIIH	14.98	0.247
1253+2756	0.0165	Sa	HIIH	15.09	-	1653+2644	0.0393	-	SBN	-	-
1254+2741	0.0172	Sb	SBN	15.81	0.645	1654+2812	0.0348	Sc+	DHIIH	17.26	0.313
1254+2802	0.0253	Sc+	DANS	15.76	-	1655+2755	0.0349	Sb	Sy2	14.55	0.583
1255+2819	0.0273	Sb	SBN	15.01	0.651	1656+2744	0.0330	Sa	SBN	16.37	0.578
1255+3125	0.0258	Sa	HIIH	15.07	0.409	1657+2901	0.0317	Sc+	DANS	16.42	0.561

 

Table 1: continued

UCM name	z	MphT	SpT	$m_{\rm r}$	E(B-V)	UCM name	z	MphT	SpT	$m_{\rm r}$	E(B-V)
(1)	(2)	(3)	(4)	(5)	(6)	(1)	(2)	(3)	(4)	(5)	(6)
1659+2928	0.0369	SB0	Sy1	14.91	0.528	2313+2517	0.0273	-	SBN	-	-
1701+3131	0.0345	S0	Sy1	14.44	1.904	2315+1923	0.0385	Sa	HIIH	16.81	0.495
2238+2308	0.0240	Sa	SBN	14.00	1.051	2316+2457	0.0277	SBa	SBN	13.45	1.172
2239+1959	0.0258	S0	HIIH	14.17	0.537	2316+2459	0.0274	Sc+	SBN	15.00	0.894
2249+2149	0.0462	Sa	SBN	14.88	-	2316+2028	0.0263	Sc+	DANS	16.57	0.755
2250+2427	0.0429	Sa	SBN	14.78	0.773	2317+2356	0.0334	Sa	SBN	13.20	-
2251+2352	0.0267	Sc+	DANS	15.71	0.184	2319+2234	0.0364	Sc+	SBN	15.89	0.588
2253+2219	0.0242	Sa	SBN	15.41	0.537	2319+2243	0.0313	S0	SBN	14.75	-
2255+1930S	0.0203	Sb	SBN	15.42	0.493	2320+2428	0.0328	Sa	DANS	14.45	-
2255+1930N	0.0198	Sb	SBN	14.69	0.699	2321+2149	0.0374	Sc+	SBN	15.85	0.559
2255+1926	0.0193	Sc+	HIIH	16.11	0.366	2321+2506	0.0331	Sc+	SBN	15.26	-
2255+1654	0.0388	Sc+	SBN	15.37	1.473	2322+2218	0.0249	Sc+	SBN	16.47	0.676
2256+2001	0.0242	Sc+	DANS	14.60	-	2324+2448	0.0123	Sc+	SBN	12.75	1.300
2257+2438	0.0345	S0	Sy1	15.88	0.540	2325+2318	0.0122	-	HIIH	-	-
2257+1606	0.0339	-	SBN	-	0.807	2325+2208	0.0130	SBc+	SBN	12.09	-
2258+1920	0.0220	Sc+	DANS	15.42	0.348	2326+2435	0.0174	Sa	DHIIH	15.87	0.278
2300+2015	0.0346	Sb	SBN	15.60	0.326	2327+2515N	0.0206	Sb	HIIH	15.59	0.474
2302+2053W	0.0328	Sb	HIIH	16.87	0.457	2327+2515S	0.0206	S0	HIIH	15.25	0.364
2302+2053E	0.0328	Sb	SBN	14.69	1.301	2329+2427	0.0200	Sb	DANS	14.70	-
2303+1856	0.0276	Sa	SBN	14.73	1.199	2329+2500	0.0305	S(r)	Sy1	15.16	-
2303+1702	0.0428	Sc+	Sy2	16.19	0.416	2329+2512	0.0133	Sa	DHIIH	16.02	0.453
2304+1640	0.0179	BCD	BCD	17.15	0.333	2331+2214	0.0352	Sb	SBN	16.44	0.892
2304+1621	0.0384	Sa	DANS	15.40	0.397	2333+2248	0.0399	Sc+	HIIH	16.37	0.383
2307+1947	0.0271	Sb	DANS	15.56	0.453	2333+2359	0.0395	S0	Sy1	15.84	0.197
2310+1800	0.0363	Sc+	SBN	15.64	0.904	2348+2407	0.0359	Sa	SBN	16.29	0.517
2312+2204	0.0327	-	SBN	-	0.864	2351+2321	0.0273	Sb	HIIH	16.39	-
2313+1841	0.0300	Sb	SBN	16.26	0.914

Table 1: (1) UCM Survey catalog name as denominated in Zamorano et al. ([1994] and [1996]) according to their B1950 coordinates. Objects are arranged in order of increasing right ascension. (2) Redshift extracted by Gallego et al. ([1996]) from emission lines; the mean error value is lower than $3\ 10^{-5}$. (3) Hubble morphological type assigned by Vitores et al. ([1996a]) using five different criteria involving bulge-disk ratios, concentration indexes and mean effective surface brightnesses in the Gunn r band. (4) Spectroscopic type assigned by Gallego et al. ([1996]) mainly from emission line ratios. (5) Gunn rmagnitude from Vitores et al. ([1996a]); the mean error is 0.08 magnitudes. (6) B-V excess calculated from the Balmer decrement as given by Gallego et al. ([1996]).

2.2 The observations

The whole sample was observed in six observing runs performed with three different telescopes. They were the 1.0 m Jacobus Kapteyn Telescope (JKT) at the Observatorio del Roque de los Muchachos in La Palma (Canary Islands, Spain), the 1.23 m telescope at the German-Spanish Observatory in Calar Alto (Almería, Spain) and the 1.52 meters Spanish Telescope in Calar Alto.

At the JKT we used a 1024 $\times$ 1024 CCD with a scale of 0.3 $\hbox{$^{\prime\prime}$ }$/pixel. The 1.52 m telescope in Calar Alto was equipped with a 1024 $\times$ 1024 CCD camera with a pixel size of $0\hbox{$.\!\!^{\prime\prime}$ }4$. Finally, the 1.23 meters telescope images were taken with a 1024 $\times$ 1024 CCD camera with a scale of $0.5\hbox{$^{\prime\prime}$ }$/pixel and also with a 2048 $\times$ 2048 CCD with a pixel size of $0\hbox{$.\!\!^{\prime\prime}$ }313$.

Typical exposure times in the first three campaigns were 600 s. Using this exposure time, the 24magarcsec^-2 level was reached at 1$\sigma$ of the sky brightness. We increased exposure times to 1800 s in order to obtain deeper images. In this case, 2$\sigma$ of the sky brightness corresponded to 25magarcsec^-2. Typical uncertainty (taking into account all sources of error) in the B magnitude was always lower than 0.1 mag in all campaigns.

All the objects were observed during photometric nights (most of them also dark) with seeing conditions ranging from $1\hbox{$.\!\!^{\prime\prime}$ }0-1\hbox{$.\!\!^{\prime\prime}$ }5$.

The main information of each observation campaign as well as the transformation equations that we will explain later are listed in Table 2.