2 The data

From our sample of 250 ELGs we selected for analysis only objects from a region North of the Slice of the Universe(de Lapparent et al. 1986), which is dominated by very well defined nearby voids. This subsample consists of 90 ELGs, most of them being distributed in the sheets and filaments that surround the voids, and with a few ELGs within some nearby voids or at the rim of the voids. No rich cluster of galaxies was included in the survey.

Most of the galaxies from this sample were observed twice. The objects were first observed in a snap-shot mode (Popescu et al. 1997), in order to check the selection criteria and to measure redshifts. In these campaigns we mostly did not have photometric conditions, therefore no reliable absolute fluxes could have been derived. Also a slit width of 2 $^{\prime\prime}$ was used, which did not provide a total coverage of the galaxies. The observing campaign from May 1997 (see Table 1 for the details of the observations) was

 

 

Table 1: The details of the spectroscopic observations from May 1996

Detector	Lor-80
Pixel Size ($\mu$)	15
Slit width ( ${\prime\prime}$)	4
PA	90.
Pixel number	1024 $\times$ 1024
Grism	9
Dispersion (Å/pixel)	5.6
Resolution (Å)	17
Spectral Range (Å)	3600-9000

dedicated to the spectrophotometry of our objects, but it also completed the observations of selected candidates. These latter observations were done in good photometric conditions, with a slit width of 4 $^{\prime\prime}$. For the small projected sizes of our dwarf galaxies, such an aperture is large enough to encompass most of their line emission. For the purpose of estimating the fraction of the line emission included in the slit we list in all the relevant tables of the paper the seeing-corrected angular sizes of the star-forming HII regions ( $r_{{\rm HII}}$). The comparison between the angular sizes of the emitting regions and the aperture sizes lead to the conclusion that the fluxes measured in the campaign from May 1996 represent accurate measurements of the total integrated fluxes of our galaxies. The large aperture used to obtain total fluxes reduces the resolution of our spectra, therefore any deblending of the emission lines was performed on the spectra taken in the previous campaigns. For the few galaxies observed only in the May 1997 observing campaign, no deblending was performed on the lines. Also, for the galaxies observed only in non-photometric conditions, no fluxes were assigned, only relative line ratios.

 

 

Table 2:

error	emission line flux or equivalent width
5$\%$	H${\beta }$, [OIII]${\lambda}$4959, [OIII]${\lambda}$5007, H$\alpha$,
	W([OIII]), W(H$\alpha$)
10$\%$	[OII]${\lambda}$3727, H$\gamma$, HeI${\lambda}$5876, W(H${\beta }$)
15$\%$	H$\delta$, [SII]${\lambda}$6717, 6731
20$\%$	[OI]${\lambda}$6300, HeI${\lambda}$6678, HeII${\lambda}$4686,
	W([SII])
25$\%$	HeI${\lambda}$7065, [AIII]${\lambda}$7136
30$\%$	[OI]${\lambda}$6364

The data were reduced using the MIDAS routines (as described by Popescu et al. 1996, 1998). The photometric calibrations of the spectra taken in the May 97 observing run were done using the standard stars: HZ 21, HZ 44 and BD +33$^{\circ}$2642 (Oke 1990) and the absolute fluxes are accurate to about 10$\%$. For one observing night the accuracy of the photometry was as good as 5$\%$. Fluxes and equivalent widths of the emission lines were measured interactively using the integrate/line routine in MIDAS. The errors in the measurements were derived from repeated observations of the lines, and the errors of the fluxes and equivalent widths W for different lines are given in Table 2.

For all the galaxies with a strong underlying continuum emission (relative to the H${\beta }$ line emission, W(H $\beta) < 20$Å) we corrected the H${\beta }$ fluxes for underlying stellar absorption with an assumed constant equivalent width of 2 Å (McCall et al. 1985). The H${\beta }$ fluxes were afterwards corrected for reddening due to dust in our own Galaxy and in the galaxy being observed. We used the reddening coefficient c(H${\beta }$), derived from the observed H$\alpha$/H${\beta }$ Balmer line ratios. From Eq. (7.6) of Osterbrock (1974), the intrinsic ratio I(H$\alpha$)/I(H${\beta }$) is related to the observed ratio via

$$\frac {F({\rm H}{\alpha})}{F({\rm H}{\beta})} = \frac {I({\rm H}{... ...ta})}\times 10^{-c}({\rm H}{\beta})[f({\rm H}{\alpha})-f({\rm H} {\beta})]\cdot$$ (1)

For the extinction in our Galaxy, f(H ${\alpha})-f({\rm H}{\beta})$ is the standard Galactic reddening law (Whitford 1958), with the extinction values taken from Burstein & Heiles (1984). For the external extinction f(H ${\alpha})-f({\rm H}{\beta})$ is the reddening law given by Howarth (1983), which should be closer to the average reddening law for the dwarf galaxies in our sample than the standard galactic one. We assumed that the intrinsic Balmer-line ratios are equal to the case B recombination values of Brocklehurst (1971) for an electron temperature of 10⁴K and an electron density of 100cm^-3.

For all the objects considered in this paper we also obtained B and Rframes. Most of the direct images were either obtained for the purpose of acquisition of the following spectroscopy or as a snap-shot survey to obtain total magnitudes. Dedicated deeper (600 s B and 300 s R) images were observed for all isolated ELGs. The photometry of the whole sample is discussed in details in Vennik et al. (1999). Based on their photometric parameters (absolute magnitudes, diameters) and the morphological appearance on the CCD images, the galaxies were classified into the morphological classes proposed by Salzer et al. (1989a,b), namely Star Burst Nucleus Galaxies (SBN), Dwarf Amorphous Nuclear Starburst Galaxies (DANS), HII Hotspot Galaxies (HIIH), Dwarf HII Hotspot Galaxies (DHIIH), Sargent-Searle Objects (SS), Magellanic Irregular (Im), and Interacting Pairs (IP). Nevertheless, an independent check was done using the line ratios of the emission-lines and their location in the diagnostic diagrams, and there is an overall good agreement between the morphological and spectroscopic classification.

 

 

Table 3:

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)
Galaxy	MB	z	c(H${\beta }$)	H${\beta }$	[OIII]	H$\alpha$	[SII]	F(H $\beta)_{{\rm obs}}$	$r_{{\rm HII}}$	type
				W[Å]	W[Å]	W[Å]	W[Å]	[ ${\rm erg}\,{\rm s}^{-1}\,{\rm cm}^{-2}$]	[ $^{\prime\prime}$]
HS 1222+3741	-17.67	0.0409	0.151	114	681	593	39	1.67e-14	0.6	Im/BCD
HS 1223+3938	-18.73	0.0360	0.474	15	91	101	14	6.88e-15	1.7	HIIH
HS 1232+3846	-19.70	0.0528	0.254	11	14	75	23	4.18e-15	2.0	SBN
HS 1232+3947	-17.16	0.0210	0.286	29	139	172	13	8.90e-15	1.7	DHIIH
HS 1232+3612	-19.77	0.0425	0.411	18	85	136	25	1.27e-14		IP
HS 1236+3821	-17.06	0.0073	0.602	4	23	37	9	7.72e-15	2.1	DHIIH
HS 1236+3937	-15.67	0.0184	0.081	112	506	521	56	5.72e-15	0.8	DHIIH/SS
HS 1240+3755	-21.1	0.0860	0.969	3	6	64	14	-		IP/SBNpec
HS 1244+3648	-18.82	0.0472	0.000	35	146	140	38	1.52e-14	0.8	HIIH
HS 1256+3505	-18.75	0.0342	0.448	20	55	155	32	1.60e-14	1.1	DANS
HS 1258+3438	-16.4	0.0248	0.380	36	209	189	15	4.39e-15		DHIIH
HS 1301+3312	-17.41	0.0371	0.391	31	125	177	40	5.90e-15	0.8	IP
HS 1301+3325	-16.96	0.0246	0.573	11	51	73	8	3.71e-15	1.3	DHIIH
HS 1301+3209	-17.06	0.0238	0.579	10	36	78	13	3.01e-15	2.2	HIIH
HS 1304+3529	-17.38	0.0165	0.013	118	570	617	76	4.82e-14	1.9	IP
HS 1306+3320	-18.32	0.0270	0.508	36	116	199	27	1.32e-14	1.9	HIIH
HS 1308+3044	-17.92	0.0209	0.564	4	13	40	8	4.55e-15	2.5	DANS
HS 1311+3628	-16.84	0.0031	0.160	301	1550	1834	139	-		DHIIH
HS 1312+3847	-18.77	0.0515	0.037	74	337	392	58	1.53e-14	1.4	HIIH
HS 1312+3508	-16.26	0.0035	0.164	254	1466	1463	179	1.02e-13		DHIIH
HS 1315+3132	-16.46	0.0315	0.476	36	136	175	28	4.14e-15	0.8	DHIIH
HS 1318+3239	-17.22	0.0435	0.186	79	464	394	32	5.75e-15	1.2	IP
HS 1319+3224	-15.3	0.0182	0.208	49	241	237	12	-	0.8	SS/DHIIH
HS 1325+3225	-17.9	0.0504	0.542	39	102	208	31	-		DHIIH/HIIH
HS 1325+3255	-15.92	0.0263	0.146	74	412	340	14	4.38e-15	0.8	DHIIH/SS
HS 1327+3126	-18.07	0.0568	0.192	91	514	484	42	1.07e-14	0.6	DHIIH
HS 1328+3424	-17.79	0.0227	0.503	8	18	54	4	2.15e-15		HIIH
HS 1329+3703	-19.11	0.0557	0.214	7	9	54	15	-	1.9	HIIH/DANS
HS 1330+3651	-17.15	0.0167	0.147	72	387	371	45	2.62e-14		DHIIH
HS 1332+3426	-16.14	0.0220	0.444	35	167	195	17	4.27e-15	1.4	DHIIH
HS 1334+3957	-15.32	0.0083	0.000	71	351	334	26	-	1.8	DHIIH
HS 1336+3114	-17.94	0.0158	0.000	5	11	29	14	-	3.9	HIIH
HS 1340+3307	-16.63	0.0158	0.539	20	108	128	23	9.73e-15	1.6	DHIIH
HS 1341+3409	-16.35	0.0171	0.480	15	59	85	19	5.34e-15	1.2	DHIIH
HS 1347+3811	-15.30	0.0103	0.243	64	363	290	33	8.62e-15	4.9	DHIIH
HS 1349+3942	-15.16	0.0054	0.337	13	45	85	23	1.05e-14	1.8	DHIIH
HS 1354+3634	-17.10	0.0167	0.513	19	50	123	26	1.12e-14	1.2	DANS
HS 1354+3635	-17.81	0.0171	0.507	21	76	124	25	2.04e-14	3.3	HIIH
HS 1402+3650	-18.81	0.0347	0.561	26	85	192	43	1.36e-14	1.6	HIIH
HS 1410+3627	-18.11	0.0338	0.311	15	55	97	28	5.16e-15		HIIH
HS 1413+4402	-19.67	0.0698	0.607	10	5	99	13	-	1.3	SBN
HS 1416+3554	-16.94	0.0103	0.328	14	49	91	24	7.70e-15	3.4	HIIH/DHIIH
HS 1420+3437	-16.75	0.0246	0.448	27	56	149	17	7.53e-15	0.6	DHIIH
HS 1422+3325	-17.30	0.0341	0.337	20	50	119	30	4.69e-15	0.8	HIIH
HS 1422+3339	-16.4	0.0114	0.350	17	58	95	20	1.12e-14	1.8	DHIIH
HS 1424+3836	-16.06	0.0218	0.195	104	579	545	24	1.00e-14	1.4	DHIIH?
HS 1425+3835	-17.80	0.0223	0.099	12	24	64	9	-	1.8	HIIH
HS 1429+4511	-17.40	0.0321	0.307	15	2	96	32	-	1.0	DANS
HS 1429+3154	-16.73	0.0117	0.143	34	144	162	26	2.06e-14	2.6	DHIIH
HS 1438+3147	-17.88	0.0443	0.308	35	188	198	30	6.54e-15	1.2	DANS
HS 1440+4302	-15.07	0.0085	0.336	44	269	238	31	1.13e-14	1.2	DHIIH/SS
HS 1440+3120	-17.4	0.0525	0.221	152	925	845	62	9.60e-15	0.7	DHIIH
HS 1440+3805	-18.80	0.0322	0.263	7	14	46	17	-	2.9	HIIH

 

Table 3: continued

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)
Galaxy	MB	z	c(H${\beta }$)	H${\beta }$	[OIII]	H$\alpha$	[SII]	F(H $\beta)_{{\rm obs}}$	$r_{{\rm HII}}$	type
				W[Å]	W[Å]	W[Å]	W[Å]	[ ${\rm erg}\,{\rm s}^{-1}\,{\rm cm}^{-2}$]	[ $^{\prime\prime}$]
HS 1442+4250	-14.73	0.0025	0.081	113	550	574	17	2.95e-14		SS
HS 1444+3114	-19.02	0.0297	0.413	26	60	174	38	2.78e-14	1.7	DANS
HS 1502+4152	-16.66	0.0164	0.515	7	39	55	21	2.22e-15		DHIIH
HS 1507+3743	-17.58	0.0322	0.114	232	1374	1307	68	3.45e-14	1.0	DHIIH
HS 1529+4512	-17.05	0.0231	0.222	16	99	102	12	2.95e-15	1.7	HIIH/DHIIH
HS 1544+4736	-17.11	0.0195	0.025	32	154	162	30	1.00e-14	2.6	DHIIH
HS 1546+4755	-17.78	0.0377	0.485	35	181	204	27	7.77e-15	0.7	DHIIH
HS 1609+4827	-17.6	0.0096	0.381	12	40	86	20	1.91e-14	2.5	HIIH
HS 1610+4539	-17.2	0.0196	0.480	26	106	152	24	1.41e-14	1.3	DHIIH/HIIH
HS 1614+4709	-13.6	0.0026	0.100	140	880	915	55	6.62e-14	1.6	SS
HS 1633+4703	-15.93	0.0086	0.364	15	55	83	19	1.34e-14	1.1	DHIIH
HS 1640+5136	-19.59	0.0308	0.443	21	55	167	34	2.42e-14	2.0	SBN/HIIH
HS 1641+5053	-19.05	0.0292	0.574	15	65	110	21	2.11e-14		HIIH
HS 1645+5155	-19.11	0.0286	0.330	47	191	265	45	1.53e-14	5.5	HIIH
HS 1657+5735	-20.60	0.0505	0.455	43	167	253	46	5.43e-14	1.2	SBN
HS 1723+5631A	-18.70	0.0286	0.341	23	100	121	20	1.13e-14		IP
HS 1723+5631B	-18.70	0.0286	0.337	32	140	188	32	1.16e-14		IP
HS 1728+5655	-16.38	0.0160	0.094	106	514	522	36	2.39e-14	0.9	DHIIH

 

 

Table 4:

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)	(13)	(14)	(15)	(16)	(17)	(18)
Galaxy	[OII]	[NeIII]	H$\delta$	H$\gamma$	[OIII]	[OIII]	[OIII]	HeI	[OI]	[OI]	[NII]	HeI	[SII]	HeI	[AIII]	[OII]	[AIII]
	3727	3869	4102	4340	4363	4959	5007	5876	6300	6364	6584	6678	6717	7065	7136	7320	7751
													6731			7330
HS 1222+3741	168	68	22	45	15	185	556	10	4	-	-	-	16	-	5	-	-
HS 1223+3938	379	75	-	36	-	177	509	17	-	-	-	-	38	-	3	-	-
HS 1232+3846	334	-	-	32	-	38	103	-	-	-	68	-	109	-	-	-	-
HS 1232+3947	256	-	-	34	-	140	427	14	16	-	5	9	21	-	-	-	-
HS 1232+3612	428	69	-	43	-	132	399	9	13	-	27	7	56	-	4	-	-
HS 1236+3821	849	-	-	-	-	127	380	11	8	-	19	-	73	-	-	-	-
HS 1236+3937	116	78	27	51	14	152	445	13	-	-	-	-	26	-	-	-	-
HS 1240+3755	659	-	-	-	-	76	94	-	-	-	179	-	96	-	-	-	-
HS 1244+3648	292	55	-	41	-	135	406	15	16	7	-	-	72	-	5	-	-
HS 1256+3505	467	-	-	60	-	87	251	15	7	-	63	-	73	-	9	-	-
HS 1258+3438	222	43	23	48	2	193	534	10	-	-	-	-	22	-	-	-	-
HS 1301+3312	439	-	-	44	-	131	393	9	17	-	-	-	58	-	-	-	-
HS 1301+3325	508	-	-	-	-	125	350	-	-	-	-	-	28	-	-	-	-
HS 1301+3209	912	-	-	-	-	99	287	-	19	-	10	-	52	-	-	-	-
HS 1304+3529	185	55	24	46	10	152	451	10	9	-	10	1	33	-	6	-	-
HS 1306+3320	354	53	-	50	-	108	320	11	7	-	-	-	37	-	8	-	-
HS 1308+3044	577	-	-	-	-	70	198	-	-	-	59	-	68	-	-	-	-
HS 1311+3628	216	29	30	54	-	176	492	11	4	-	13	3	28	-	9	3	-
HS 1312+3847	242	64	18	46	5	153	445	18	6	-	10	-	47	-	7	-	-
HS 1312+3508	261	64	29	53	7	170	492	12	5	3	11	5	30	4	11	5	4
HS 1315+3132	410	20	24	50	5	123	356	11	10	-	-	-	42	-	8	-	-
HS 1318+3239	156	63	27	44	12	198	577	13	-	-	-	3	23	-	6	-	-
HS 1319+3224	124	63	26	48	13	163	503	10	-	-	-	-	14	-	-	-	-
HS 1325+3225	353	-	-	44	-	84	250	10	-	-	-	3	40	-	-	-	-
HS 1325+3255	126	57	22	49	8	187	548	9	6	-	-	-	12	-	-	-	-
HS 1327+3126	199	56	26	46	7	182	536	12	5	4	-	3	25	3	5	3	2
HS 1328+3424	434	-	-	-	-	84	183	-	-	-	34	-	25	-	-	-	-
HS 1329+3703	366	-	-	-	-	35	102	-	-	-	85	-	111	-	-	-	-
HS 1330+3651	186	48	25	43	9	164	490	15	8	-	9	-	35	-	4	-	-
HS 1332+3426	359	74	-	53	-	162	455	14	11	-	-	-	23	-	6	2	-
HS 1334+3957	288	48	33	55	-	178	519	17	-	-	5	-	24	-	7	-	-

 

Table 4: continued

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)	(13)	(14)	(15)	(16)	(17)	(18)
Galaxy	[OII]	[NeIII]	H$\delta$	H$\gamma$	[OIII]	[OIII]	[OIII]	HeI	[OI]	[OI]	[NII]	HeI	[SII]	HeI	[AIII]	[OII]	[AIII]
	3727	3869	4102	4340	4363	4959	5007	5876	6300	6364	6584	6678	6724	7065	7136	7320	7751
													6731			7330
HS 1336+3114	278	-	-	-	-	79	172	-	-	-	51	-	163	-	-	-	-
HS 1340+3307	503	153	-	66	-	174	485	16	-	-	7	-	49	-	-	-	-
HS 1341+3409	573	88	-	-	-	126	325	18	-	-	-	-	60	-	-	-	-
HS 1347+3811	229	90	28	54	7	189	546	13	8	-	-	-	33	3	8	-	-
HS 1349+3942	556	-	-	53	-	106	286	13	12	-	26	-	82	-	-	-	-
HS 1354+3634	467	-	-	48	-	91	255	10	18	-	44	-	71	-	-	-	-
HS 1354+3635	468	-	-	48	-	118	339	10	7	-	28	3	61	-	4	-	-
HS 1402+3650	483	85	-	49	-	96	294	12	13	-	20	4	63	-	-	-	-
HS 1410+3627	601	-	-	46	-	109	305	14	14	-	14	-	81	-	-	-	-
HS 1413+4402	214	-	-	-	-	26	45	-	-	-	150	-	62	-	-	-	-
HS 1416+3554	593	87	-	-	-	99	284	-	-	-	18	-	77	-	-	-	-
HS 1420+3437	484	-	-	49	-	79	196	11	-	-	22	-	34	-	-	-	-
HS 1422+3325	479	-	-	50	-	90	245	9	-	-	59	-	86	-	-	-	-
HS 1422+3339	466	-	-	40	-	105	289	-	-	-	21	-	65	-	-	-	-
HS 1424+3836	115	36	26	53	7	181	552	12	4	-	-	-	12	-	3	-	-
HS 1425+3835	586	-	-	-	-	59	200	-	-	-	40	-	51	-	-	-	-
HS 1429+4511	205	-	-	-	-	11	51	-	-	-	82	-	112	-	-	-	0
HS 1429+3154	392	-	-	46	-	142	419	6	6	-	19	-	49	-	7	-	-
HS 1438+3147	335	71	-	43	-	174	507	14	8	-	7	-	42	-	-	-	-
HS 1440+4302	530	94	26	60	14	191	558	10	6	-	11	-	36	-	7	-	-
HS 1440+3120	156	59	30	44	11	211	613	13	5	-	-	3	20	-	4	-	-
HS 1440+3805	397	-	-	-	-	78	159	13	23	-	50	-	118	-	-	-	-
HS 1442+4250	97	50	22	38	11	165	475	12	-	-	-	2	8	-	4	-	-
HS 1444+3114	492	30	-	50	-	75	220	9	9	5	43	-	71	-	6	-	-
HS 1502+4152	-	-	-	-	-	153	420	-	-	-	22	-	108	-	-	-	-
HS 1507+3743	87	66	29	52	12	217	658	10	3	-	-	2	13	4	4	4	-
HS 1529+4512	465	76	-	46	-	173	502	-	-	-	16	-	34	-	-	-	0
HS 1544+4736	104	-	-	62	-	147	456	15	7	-	14	-	52	-	7	-	-
HS 1546+4755	397	73	40	52	-	166	494	10	7	-	6	-	37	-	-	-	-

 

Table 4: continued

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)	(13)	(14)	(15)	(16)	(17)	(18)
Galaxy	[OII]	[NeIII]	H$\delta$	H$\gamma$	[OIII]	[OIII]	[OIII]	HeI	[OI]	[OI]	[NII]	HeI	[SII]	HeI	[AIII]	[OII]	[AIII]
	3727	3869	4102	4340	4363	4959	5007	5876	6300	6364	6584	6678	6724	7065	7136	7320	7751
													6731			7330
HS 1609+4827	551	-	-	38	-	91	261	8	15	-	-	-	63	-	-	-	-
HS 1610+4539	390	-	31	47	9	136	374	10	10	-	-	4	42	-	4	-	-
HS 1614+4709	79	54	27	50	6	200	590	10	4	-	-	-	18	-	5	-	-
HS 1633+4703	596	86	-	48	-	116	309	15	10	-	19	9	67	-	7	-	-
HS 1640+5136	520	22	-	56	-	84	243	15	11	4	98	-	79	-	5	-	-
HS 1641+5053	582	94	-	33	-	121	339	11	11	-	-	-	50	-	-	-	-
HS 1645+5155	349	-	24	45	9	129	387	22	7	-	12	-	46	-	-	-	-
HS 1657+5735	349	39	22	47	3	117	355	10	7	1	-	2	47	-	3	-	2
HS 1723+5631A	425	-	-	61	-	140	412	15	14	6	23	-	49	-	-	-	-
HS 1723+5631B	352	-	-	54	-	144	419	13	9	-	23	-	50	-	-	-	-
HS 1728+5655	211	75	26	47	3	172	500	12	5	2	25	2	23	-	7	3	-

 

 

Table 5:

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)	(13)	(14)	(15)	(16)	(17)	(18)	(19)
Galaxy	MB	z	H${\beta }$	[OIII]	H$\alpha$	[SII]	F(H $\beta)_{{\rm obs}}$	[OII]	H$\gamma$	[OIII]	[OIII]	HeI	[OI]	H ${\alpha}^{*}$	HeI	[SII]	$r_{{\rm HII}}$	type
			W	W	W	W		3727	4340	4959	5007	5876	6300	6563	6678	6724
			[Å]	[Å]	[Å]	[Å]	[ ${\rm erg}\,{\rm s}^{-1}\,{\rm cm}^{-2}$]							6584		6731	[ $^{\prime\prime}$]
HS 1255+3506	-16.61	0.0155	10	31	66	19	4.70e-15	381	-	86	258	-	24	457	-	124	1.7	DHIIH?
HS 1318+3406	-18.65	0.0352	8	17	69	21	5.09e-15	414	-	74	178	-	-	526	-	152		HIIH?
HS 1327+3412	-	0.2510	11	7	111	11	-	87	-	13	52	-	-	376	-	37	0.7	-
HS 1333+3149	-18.61	0.0248	8	27	66	11	8.86e-15	387	-	101	267	-	-	470	-	77	2.3	HIIH
HS 1340+3207	-18.35	0.0365	18	105	127	23	6.92e-15	390	16	186	555	21	-	426	-	73	1.7	DANS
HS 1429+3154*	-16.73	0.0117	34	144	162	26	2.06e-14	347	39	143	424	6	7	344	-	55	2.6	DHIIH
HS 1442+4332	-20.05	0.0811	5	9	65	15	2.55e-15	361	-	57	116	15	43	616	14	126	1.5	SBN?
HS 1543+4525	-19.17	0.0389	10	15	92	27	6.90e-15	388	-	38	123	15	14	573	8	164	2.2	DANS?
HS 1627+5239*	-17.88	0.0288	14	37	95	16	7.61e-15	286	-	73	224	12	-	422	-	70	1.22	HIIH?
HS 1657+5033	-17.43	0.0102	7	29	60	14	1.19e-14	338	-	103	323	10	-	559	6	124	1.88	HIIH
The galaxies HS 1429+3154 and HS 1627+5239 have detected [AIII]${\lambda}$7136, with the line ratios relative to H${\beta }$ of 8 and 15, respectively.