4 The list

Thus, all H$\alpha$ excess objects were divided into sequences on the basis of their morphological features: stellar (s), diffuse (d), bubble-type (b). Faint and compact objects that remained unclassified were labeled by c. Besides this, there were objects for which it turned out to be impossible to determine the size because of their closeness to bright HII regions. As a rule, in H$\alpha$ images, these objects are seen as a hump near a large nebula, i.e. they are located on a steep background gradient. In the methods we used, their size would often be underestimated or formally equal to zero. We denote such objects as zs. As a result there were isolated 81 stars, 154 diffuse nebulae, 180 bubbles, 117 objects of type c and 17 zs objects. The division between s and d, d and b objects have to be considered as an average, but not precise, because there are some objects located between the sequences and the objects may obviously have not a simple ${\rm H}\alpha$ morphology.

   

Table 1: Selected emission objects

n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type	n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type
1	8	18.80	3.7	3.0	b	41	208	17.00	10.6		s
2	11	18.50	6.6		c	42	210	18.47	6.0	4.0	d
3	18	18.40	5.7	2.8	d	43	211	17.97	4.6	3.2	b
4	22	18.60	2.9	3.2	b	44	215	18.60	13.4	3.1	d
5	42	18.70	52		s	45	216	18.81	42	6.0	b
6	60	19.10	34	4.6	d	46	222	17.70	5.9	3.0	d
7	61	19.20	68	6.9	b	47	227	18.90	2.5	3.9	b
8	65	16.67	7.5		s	48	228	18.35	5.8	4.2	b
9	68	19.30	10.0	5.4	b	49	240	17.20	32	4.4	d
10	71	19.00	5.2	3.2	b	50	246	18.70	2.1	5.5	b
11	72	18.65	23	3.7	d	51	248	18.39	2.6		c
12	87	18.00	6.4	3.1	d	52	263	17.81	13.5	3.7	d
13	90	18.31	3.2		c	53	268	17.30	42	6.7	d
14	99	18.58	3.2	2.7	b	54	272	18.10	4.8	3.3	b
15	101	18.24	6.5		c	55	276	16.80	7.4	3.9	d
16	104	18.70	3.2		c	56	282	19.10	8.7		c
17	109	18.80	14.3		s	57	284	19.19	7.1	3.0	b
18	116	18.20	16.2		s	58	285	19.42	6.0		c
19	119	18.60	12.9	3.1	d	59	298	18.60	24		s
20	120	18.70	5.8		c	60	301	16.40	4.0	4.1	d
21	125	19.22	12.5		s	61	329	18.80	1.9		c
22	131	17.80	61	5.6	d	62	337	19.10	2.0		c
23	136	19.50	11.6	3.3	d	63	341	19.40	6.2		c
24	137	17.79	390		zs	64	343	17.83	6.5	5.7	b
25	139	17.70	10.8		s	65	344	18.90	12.4	3.8	d
26	140	18.70	3.6	3.8	b	66	350	19.02	3.0	2.7	b
27	141	18.80	8.4	2.6	d	67	352	19.30	83	9.0	d
28	143	18.40	5.8		c	68	361	19.00	18.6		s
29	147	18.40	1.9	3.5	b	69	366	18.40	2.9	4.0	b
30	156	19.48	2.8	3.1	b	70	368	17.80	15.9		s
31	162	18.91	5.4	4.5	b	71	369	19.38	17.7	3.7	d
32	168	18.40	13.2	4.8	b	72	372	19.10	7.8		s
33	169	17.71	5.6	2.9	d	73	374	17.12	11.0		s
34	172	19.00	2.1	2.8	b	74	382	18.33	11.2	4.4	b
35	174	18.79	6.7	4.8	b	75	383	19.19	4.6		c
36	188	17.70	2.9		c	76	386	17.30	8.3		s
37	192	17.61	10.0		s	77	392	19.30	7.3		c
38	200	19.48	3.8	4.9	b	78	401	17.70	2.6	3.0	d
39	202	19.27	82	6.2	d	79	403	19.47	40	5.3	d
40	205	19.49	2.5	4.1	b	80	404	16.90	14.1		s

 

Table 1: continued

n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type	n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type
81	406	19.36	5.6	3.9	b	121	548	16.80	15.3		s
82	408	19.10	9.3		c	122	550	19.20	84		s
83	409	18.68	26	5.2	b	123	555	18.80	2.2	3.3	b
84	411	18.00	10.3	3.4	d	124	559	17.72	5.3		s
85	412	18.60	29	5.1	d	125	561	17.69	5.0		s
86	417	19.21	3.3	3.1	b	126	571	17.58	19.9		s
87	420	19.42	4.5		c	127	574	19.16	6.1		c
88	422	19.01	25		s	128	578	19.10	9.2	4.4	d
89	424	19.00	68	7.1	d	129	584	18.97	3.1	3.1	b
90	425	19.34	8.9	4.2	d	130	589	18.22	20.0	5.8	d
91	426	17.20	5.9	3.2	d	131	592	18.60	24.8	5.1	d
92	431	17.99	2.3		c	132	607	19.42	4.7		c
93	432	19.21	3.2		c	133	609	18.66	5.6	5.5	b
94	435	17.60	6.8	3.5	d	134	611	17.00	8.9	5.3	d
95	442	18.50	2.1	3.3	b	135	614	17.20	9.3		s
96	444	17.28	9.8		s	136	619	17.40	9.3	4.1	d
97	449	18.78	4.9	4.8	b	137	629	19.40	36	7.3	d
98	452	19.17	4.1	4.3	b	138	630	18.70	6.7	3.6	d
99	454	18.90	2.8	5.3	b	139	633	19.30	117	10.5	d
100	455	18.39	31	7.4	b	140	637	18.75	4.4	3.6	b
101	465	18.68	2.1	3.4	b	141	639	18.40	13.7	4.9	d
102	466	19.33	22.9	5.5	b	142	644	17.90	4.2	4.1	b
103	467	18.40	2.8		c	143	646	19.11	7.3	3.5	d
104	471	19.10	170		zs	144	648	18.10	2.7	3.5	b
105	482	18.96	28	5.7	b	145	651	19.17	3.9	3.2	b
106	488	19.20	61	6.5	d	146	653	18.90	11.7		s
107	490	18.22	2.2		c	147	656	19.42	7.5		c
108	492	18.95	5.4	5.2	b	148	663	19.46	2.8	3.1	b
109	493	19.40	18.6	7.7	b	149	664	18.50	20.3	5.9	d
110	500	18.10	2.7	3.2	b	150	666	19.34	30		s
111	505	18.15	3.1		c	151	667	19.00	4.1	4.5	b
112	511	18.70	13.2	4.5	d	152	669	17.70	4.2		c
113	515	16.50	2.1	4.0	d	153	675	19.40	11.4		s
114	526	18.70	4.9	3.6	b	154	676	18.50	2.6		c
115	527	18.62	2.6		c	155	677	19.50	4.4		c
116	532	18.85	14.0	7.7	b	156	678	18.70	42	9.3	b
117	533	18.60	250		zs	157	689	19.20	2.8		c
118	536	19.43	2.4		c	158	697	18.17	2.7	3.8	b
119	537	18.60	7.7	4.3	b	159	699	18.00	17.4	4.9	b
120	544	17.90	8.2	4.2	d	160	701	16.99	34	4.9	d

 

Table 1: continued

n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type	n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type
161	705	19.00	19.8	4.5	d	201	821	19.00	7.8	4.1	d
162	710	19.00	10.7	4.9	d	202	823	18.80	10.7	4.9	b
163	712	17.68	63	7.2	d	203	825	18.10	6.4	4.3	b
164	714	18.84	3.7	3.4	d	204	830	19.10	5.1		zs
165	718	18.40	8.5	3.9	d	205	836	19.00	6.9	4.4	b
166	719	16.90	9.8	4.8	d	206	837	18.90	8.2		zs
167	727	16.80	16.2		s	207	839	16.70	3.6		zs
168	730	18.70	13.5	4.9	d	208	842	18.80	13.1		zs
169	734	18.40	6.0		c	209	844	19.20	3.6		c
170	735	19.00	61	7.9	d	210	853	19.30	9.7	4.5	d
171	736	16.40	15.5	5.9	d	211	856	17.90	8.8	3.3	d
172	740	18.80	6.9	4.2	b	212	861	18.90	53	8.5	d
173	743	15.87	3.2		s	213	863	18.60	4.0	2.9	d
174	747	19.36	60	8.7	d	214	867	18.84	3.9		c
175	749	19.30	7.6		zs	215	868	18.30	12.0	4.4	d
176	750	16.77	6.7		s	216	870	19.00	36.3	8.9	b
177	751	19.40	7.3		c	217	874	18.66	8.9	4.3	d
178	755	17.84	3.0	3.5	b	218	875	18.90	8.7	5.0	b
179	757	17.20	9.7	4.8	d	219	878	18.10	5.7		s
180	760	18.70	2.0		c	220	879	18.60	2.4	3.5	b
181	761	18.20	2.2		c	221	884	18.22	16.8	4.7	d
182	771	18.10	2.8		c	222	895	18.48	3.1		c
183	772	19.01	38	6.4	d	223	905	18.60	6.6	4.4	b
184	774	18.90	8.5	4.6	b	224	910	19.30	14.9	5.3	d
185	775	19.10	2.4		c	225	913	19.20	2.7	3.4	b
186	779	18.20	6.0		c	226	920	17.50	11.9	5.0	d
187	780	18.60	6.3	5.0	b	227	923	18.40	9.7	4.0	d
188	781	18.91	4.0	3.5	b	228	926	18.30	240	9.3	d
189	783	19.40	2.1		c	229	933	19.20	6.2		zs
190	784	18.80	3.3	3.2	b	230	935	19.20	15.6		s
191	786	18.30	6.3		c	231	936	19.10	2.9		c
192	789	19.20	27.5	6.2	d	232	938	17.50	7.0	4.0	d
193	790	18.85	2.1		c	233	948	18.38	6.0		s
194	791	18.80	5.2		zs	234	953	19.40	3.7		c
195	795	18.50	3.3		c	235	956	17.90	10.6		s
196	799	19.00	57.8	7.6	d	236	965	19.31	2.4		c
197	803	19.13	2.3		c	237	976	18.30	6.1	4.2	b
198	805	17.10	33.2		s	238	987	19.29	7.7	4.4	b
199	815	19.00	6.0	4.1	b	239	990	19.00	48		s
200	818	19.20	5.0	3.3	d	240	994	19.43	3.2	3.8	b

 

Table 1: continued

n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type	n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type
241	995	19.49	5.3		c	281	1130	19.20	3.3	4.5	b
242	999	16.46	2.1		s	282	1131	18.30	19.8	5.8	d
243	1001	18.73	11.5		s	283	1142	18.10	15.6		s
244	1002	16.20	2.9	4.2	d	284	1145	18.02	5.1	4.1	b
245	1003	18.20	2.5		c	285	1147	18.89	7.7	5.5	b
246	1004	16.40	6.2	5.3	d	286	1153	18.90	4.6		c
247	1005	19.10	9.4		s	287	1156	18.00	19.8	6.2	d
248	1006	17.60	5.6	3.5	d	288	1157	18.70	29	6.3	d
249	1010	19.38	2.4	3.1	b	289	1161	18.80	5.4	3.5	d
250	1011	19.20	2.7	2.9	b	290	1163	17.50	6.6	3.1	d
251	1013	19.20	19.6	5.7	d	291	1166	19.29	3.1		c
252	1018	18.40	3.1		c	292	1176	19.09	5.9		c
253	1020	17.90	25		s	293	1177	18.30	12.4	3.9	d
254	1022	18.80	2.8		c	294	1179	18.70	32	6.4	d
255	1024	17.70	28		s	295	1194	19.00	3.7	3.1	b
256	1026	16.60	17.5	5.5	d	296	1203	18.50	7.0	4.1	b
257	1030	19.30	5.1		c	297	1211	18.60	91	9.4	d
258	1031	19.30	9.0		zs	298	1212	19.00	5.5		c
259	1035	19.38	29	5.5	d	299	1215	19.50	14.9	4.7	d
260	1038	18.50	4.1		c	300	1216	18.30	3.3		c
261	1042	19.47	18.7		s	301	1219	18.50	10.1	3.9	d
262	1051	19.50	5.0		c	302	1222	19.23	33	4.4	d
263	1053	18.44	2.8	3.3	b	303	1228	18.70	6.5	4.5	b
264	1055	18.50	2.4	4.3	b	304	1242	18.39	3.7		c
265	1061	16.40	7.9		s	305	1248	19.40	9.8		c
266	1066	19.40	3.8		c	306	1249	18.00	7.7	5.8	b
267	1070	18.10	2.2	3.4	b	307	1254	17.71	5.8	3.7	d
268	1080	18.00	3.1		c	308	1263	19.50	13.8	4.8	d
269	1089	19.10	31		s	309	1265	17.81	7.1	3.8	d
270	1090	18.50	6.8		zs	310	1269	18.60	2.4	3.7	b
271	1097	18.20	17.6		s	311	1270	18.70	14.5	4.4	d
272	1101	18.50	3.7		c	312	1277	19.40	5.2	3.3	b
273	1102	19.20	20.8	5.7	d	313	1278	19.10	109	10.4	d
274	1104	19.20	4.1		c	314	1281	19.10	7.1	4.2	b
275	1105	19.50	9.7	4.7	b	315	1288	19.20	12.7		s
276	1106	18.80	7.8		s	316	1299	18.90	4.9	6.1	b
277	1112	19.10	2.3	3.2	b	317	1300	19.10	7.0	3.6	d
278	1122	18.20	3.0		c	318	1304	19.20	4.4	3.3	b
279	1123	19.40	4.9	3.5	b	319	1309	18.90	2.1		c
280	1129	18.50	3.0		zs	320	1314	16.90	10.6	4.0	d

 

Table 1: continued

n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type	n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type
321	1319	19.20	3.2		c	361	1473	17.70	4.8	5.4	b
322	1326	19.20	4.4		c	362	1474	17.70	9.1	4.9	b
323	1327	17.50	6.2	4.0	b	363	1475	19.00	3.2		c
324	1328	18.80	2.6	3.3	b	364	1480	18.80	4.5		c
325	1331	18.40	4.7	4.8	b	365	1487	18.50	9.2	4.3	d
326	1334	18.71	3.5	3.3	d	366	1504	18.93	3.4	3.3	b
327	1339	18.80	3.6		c	367	1507	19.40	4.3		c
328	1356	17.64	6.7	3.8	d	368	1508	19.10	64		zs
329	1358	18.50	8.2	4.1	d	369	1512	19.40	4.5	4.7	b
330	1363	19.30	35	4.5	d	370	1523	17.80	7.4		s
331	1368	19.07	28.3	5.4	d	371	1524	17.60	5.8	3.8	d
332	1381	19.00	36	6.8	d	372	1527	18.10	2.7		c
333	1383	18.90	3.3	5.7	b	373	1528	18.70	3.1		c
334	1386	18.60	6.7	3.9	d	374	1533	19.10	14.5		s
335	1389	18.90	3.7	3.9	b	375	1536	19.30	5.8		s
336	1393	19.20	3.8	3.2	b	376	1539	19.30	150	9.2	d
337	1396	19.20	2.5		c	377	1541	19.00	2.8	2.9	b
338	1400	19.00	39	10.7	b	378	1543	18.80	5.8	5.2	b
339	1402	18.70	84	9.1	d	379	1547	18.80	47	4.2	d
340	1404	17.50	7.1	3.2	d	380	1548	19.00	5.2	4.5	b
341	1405	19.40	100	9.9	d	381	1551	18.50	9.3	4.2	d
342	1406	18.61	119	10.2	d	382	1553	18.10	8.5	2.9	d
343	1408	19.41	2.4	4.2	b	383	1556	18.99	5.7	4.6	b
344	1413	17.20	11.9		s	384	1560	19.40	4.1	3.3	b
345	1414	18.10	3.9	3.4	d	385	1561	19.00	3.3	2.5	b
346	1422	18.70	3.5		c	386	1567	19.30	2.9	3.6	b
347	1426	18.90	7.9	4.6	b	387	1568	19.27	9.2		c
348	1427	17.90	3.5		c	388	1569	19.42	3.4	2.7	b
349	1431	18.09	7.5	4.5	d	389	1571	18.00	2.8	3.0	d
350	1434	18.65	4.3		c	390	1573	17.40	8.7	4.3	d
351	1436	19.40	2.5	2.9	b	391	1575	16.60	27	5.5	d
352	1440	19.00	2.1		c	392	1576	19.00	2.7	3.6	b
353	1448	18.60	2.0	3.4	b	393	1579	18.00	64		s
354	1451	18.40	2.2		c	394	1588	16.48	45	4.7	d
355	1453	18.40	5.6	4.4	b	395	1589	19.50	4.6	3.6	b
356	1460	18.99	5.3	3.5	d	396	1607	18.10	3.4		c
357	1463	18.40	3.5		zs	397	1613	19.30	5.0		s
358	1465	18.80	2.2		c	398	1617	18.31	2.6		c
359	1466	18.50	4.1	3.1	d	399	1625	18.79	4.0	2.9	b
360	1467	17.95	5.5		s	400	1630	19.10	2.6	2.5	b

 

Table 1: continued

n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type	n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type
401	1637	19.30	14		s	441	1779	18.40	23.1		s
402	1644	17.10	3.0	3.8	d	442	1780	18.82	205		zs
403	1648	18.50	3.1	3.9	b	443	1781	19.30	4.3		c
404	1650	19.30	6.5	4.1	b	444	1783	19.20	30	6.5	d
405	1660	18.20	9.6	3.6	d	445	1790	19.01	60	7.6	d
406	1661	19.37	4.4	3.7	b	446	1793	19.00	2.8		c
407	1665	19.38	21	6.2	d	447	1794	18.86	2.2	4.5	b
408	1667	19.11	7.8	4.7	b	448	1796	18.40	8.3	3.0	d
409	1670	19.50	2.8	2.9	b	449	1800	19.00	88	6.5	d
410	1671	18.90	5.4		c	450	1805	18.11	8.6	3.0	d
411	1677	19.01	3.4	3.3	b	451	1808	19.19	5.6	3.7	b
412	1685	19.20	4.6		c	452	1810	18.70	32	6.4	d
413	1686	19.16	5.0	3.3	b	453	1811	19.10	3.2	2.7	b
414	1700	19.20	4.6	2.5	b	454	1813	19.40	51	7.5	d
415	1701	18.40	8.2	5.4	b	455	1818	18.90	23		s
416	1704	18.51	2.3	3.9	b	456	1820	18.64	5.0	2.9	b
417	1707	19.20	3.5	3.7	b	457	1821	18.80	2.8	3.2	b
418	1708	18.90	30	3.9	d	458	1825	17.08	13.7		s
419	1714	19.00	37	4.9	d	459	1829	19.20	6.6	4.6	b
420	1720	18.90	4.6	3.8	b	460	1838	19.30	5.8		c
421	1728	19.10	16.8		s	461	1840	19.40	120	7.7	d
422	1731	18.10	16.1		s	462	1852	19.30	5.6	2.9	b
423	1733	16.70	10.6	5.0	d	463	1855	18.85	22		s
424	1734	19.18	4.7	3.8	b	464	1866	18.90	3.4		c
425	1735	16.40	430		zs	465	1867	18.50	13.1	3.8	d
426	1736	19.50	2.5		c	466	1870	19.35	6.0	3.1	b
427	1737	18.20	4.1	2.9	b	467	1875	19.10	4.5	3.2	b
428	1741	18.40	2.6	3.1	b	468	1878	19.10	2.2		c
429	1747	18.70	4.2		c	469	1895	18.34	7.7		c
430	1749	19.30	8.3	4.6	b	470	1897	19.20	2.7	3.5	b
431	1750	19.10	61		s	471	1900	18.10	3.4	3.6	b
432	1751	16.40	27		s	472	1904	19.00	6.6	4.1	b
433	1761	19.10	33		s	473	1909	19.48	3.0	3.4	b
434	1764	19.30	2.7	2.6	b	474	1913	18.66	46	5.1	d
435	1765	19.40	6.6		c	475	1914	18.96	11.5	3.3	d
436	1766	18.20	10.2	4.5	b	476	1915	19.40	130	6.7	d
437	1770	19.26	2.7		c	477	1922	18.80	2.3	2.4	b
438	1775	18.26	2.0		c	478	1923	18.80	2.3	2.8	b
439	1776	16.49	45	4.9	d	479	1925	19.00	8.2	2.7	d
440	1777	19.38	3.4	4.4	b	480	1930	19.19	4.2	3.0	b

 

Table 1: continued

n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type	n	n(IFM)	mV	S	${d(\hbox{$^{\prime\prime}$ })}$	Type
481	1931	19.44	13.9		s	521	385	19.40	2.1		c
482	1939	18.90	3.1		c	522	535	18.91	6.0		c
483	1942	19.40	6.1		c	523	638	19.30	6.7	4.2	b
484	1943	19.30	2.6	2.8	b	524	659	19.00	2.5		c
485	1946	19.20	4.7	3.3	b	525	669	19.20	2.2		c
486	1954	19.18	9.5	3.8	b	526	688	19.15	84		s
487	1964	18.80	38		s	527	781	18.70	4.7		c
488	1973	18.57	6.2	2.8	d	528	809	18.90	7.0		s
489	1974	19.24	12.2	3.9	b	529	836	18.60	4.2		c
490	1976	19.24	1.9		c	530	911	19.18	30	5.0	d
491	1979	18.00	9.9	3.9	b	531	920	17.70	6.6	3.8	d
492	1987	19.40	10.0	4.8	b	532	1090	19.40	5.3		s
493	1990	18.74	5.4	3.3	b	533	1127	19.50	21		c
494	1991	18.37	5.1	3.9	b	534	1270	18.20	18.1	4.9	d
495	1992	17.42	4.8		s	535	1273	17.00	2.8	3.7	d
496	2002	19.24	10.8	4.3	b	536	1285	19.18	3.1		c
497	2003	19.47	3.7	2.7	b	537	1294	18.40	16.8	6.4	b
498	2022	16.10	3.5	3.8	d	538	1332	18.40	36	5.6	d
499	2025	19.00	3.0	2.3	b	539	1517	18.80	5.0		s
500	2031	18.95	11.3		s	540	1591	17.89	3.7	3.5	d
501	2043	18.90	23	4.8	b	541	1624	19.00	5.7	4.1	b
502	2059	19.10	3.1	2.5	b	542	1647	18.60	4.0		c
503	2067	18.10	2.6		c	543	1662	18.70	3.8		c
504	2068	19.44	4.4		c	544	1763	18.80	22		s
505	2075	19.00	8.6		c	545	1879	17.76	2.1	3.3	b
506	2077	18.70	32	5.3	b	546	1880	17.20	17.4		s
507	2085	19.30	50		s	547	1908	18.70	6.5		s
508	2086	17.90	5.3	3.6	b	548	2004	19.30	120	7.2	d
509	2087	19.23	29		s	549	2143	18.04	21.3		s
510	2091	18.62	13.6		s
511	2102	18.10	2.9	4.1	b
512	2103	17.94	34		s
513	2107	18.00	6.6	2.8	d
514	2117	18.40	7.4		c
515	10	17.85	3.1	3.3	b
516	60	18.30	140	6.5	d
517	104	17.20	77		s
518	266	19.10	2.1	2.9	b
519	286	17.89	8.1	4.6	b
520	349	18.83	2.9	3.6	b

All isolated objects are listed in Table 1, where the columns present: 1) successive numbers n, 2) number from the original catalogue n(IFM). The last 35 objects are from the first unpublished version of the catalogue. Other columns are 3) stellar magnitudes V, 4) ${ S=(F-F_{\rm b})/\sigma_{\rm b}}$ -- flux excess over the flux of the basic (nonemission) star sequence, which is measured in standard deviations of stars composing this sequence, 5) object sizes in arcseconds (for objects of types b and d only), 6) morphological type. Finding charts could be found in IFM.

From the examination of Table 1 it follows that the objects having a maximal excess in H$\alpha$ belong mostly to the diffuse nebulae sequence, while the objects with a minimal excess belong to the sequence of bubbles (see also Table 2). On the basis of the photometry data we may estimate H$\alpha$ line flux in units of stellar continuum flux. One may find a quantity ${W'_{\rm H\alpha}= \bigtriangleup\lambda \cdot((F-F_{\rm b})/F_{\rm b})}$, where $\bigtriangleup\lambda=35$ Å is a width of H$\alpha$ band used (Courtes et al. 1987). It is important to note that F is a total ${\rm H}\alpha$ band flux which is radiated both in a whole nebula and in a star's atmosphere, but the continuous emission ${ F_{\rm b}}$ is stellar. In a case of pure intrinsic stellar ${\rm H}\alpha$ emission it is the line equivalent width. In a case of nebula emission, ${W'_{\rm H\alpha}}$ is a direct function of the star UV luminosity beyond Lyman edge over that in V band, i.e. it is a function of the ionizing star's temperature. In general case ${W'_{\rm H\alpha}}$ depends on HII region size that surrounds the star, which in turn is determined by the star's temperature and luminosity, electron density and other parameters of the medium. The object sizes and the H$\alpha$ fluxes measured, may be of independent interest for study the isolated nebulae and their central stars parameters.

   

Table 2: The mean parameters and their rms of the emission objects

Type	n	V	U-B	B-V	${ V-\rm H{\alpha}}$	SB	S	d ( ${}^{\prime\prime}$)	${W'_{\rm H\alpha}}$ (Å)
s	81	18.23	-0.78	0.08	2.26	277	19.7		273
		0.10	0.04	0.03	0.11	9	2.0		38
d	154	18.35	-0.85	0.08	2.52	180	28.0	4.93	558
		0.07	0.03	0.02	0.11	5	2.9	0.14	82
b	180	18.83	-0.68	0.04	1.65	75	6.9	4.08	120
		0.03	0.02	0.02	0.05	2	0.6	0.09	11
c	117	18.85	-0.82	0.05	1.60	625	4.2		101
		0.04	0.03	0.02	0.05	218	0.2		8
zs	17	18.55	-0.98	0.01	3.14		93		824
		0.20	0.07	0.09	0.36		34		342

Calzetti et al. (1995) published results of a systematic search for SS 433-type candidates in the galaxy M33. To isolate candidates they used CCD images of M33 in a narrow H$\alpha$ band and in an adjacent continuum at about 6100 Å. They have estimated a limiting stellar magnitude as V $\approx 20$. The M33 field coverage by their images is approximately twice as small as the region we have studied. Calzetti et al. (1995) have isolated a total of 279 compact HII regions and 153 point-like emission sources (actually analysis of their images reveals that their samples contain 27 object repetitions). Their fields contain 311 objects from 549 objects we have selected. Comparing our Table 1 with the data of Calzetti et al. (1995), we found 42 common objects, 17 of them among HII regions and 25 from the point-like emission objects. The greater part of these HII regions belong to our sequence of diffuse nebulae. A half of these point-like H$\alpha$ sources are also among our diffuse nebulae, while the rest of the objects are of types s and c. The list of Calzetti et al. (1995) comprises 64$\%$ HII regions and 36$\%$ point-like objects. Our sample contains 63$\%$ d and b nebulae, 15$\%$ s and 22$\%$ c objects, i.e. 37$\%$ are star-like emission objects. The relative proportions of extended and star-like objects in these two lists are in agreement. The incomplete overlapping of the lists is likely to be due to the fact that Calzetti et al. (1995) have examined central regions of M33, where the great H$\alpha$ background inhibits the separation of emission objects in the photographic data we used. For this reason these two lists may be considered as complementing each other.