3 The data

Optical data of our galaxies are given in Table 1. The kkr-number is given in Col. 1, RA and Dec. (1950) follow in Cols. 2 and 3. The optical diameters a and b in the Holmberg (D_26.5) system follow in Cols. 4 and 5, the morphological type in Col. 6 where we use the following coding:

Im - irregular blue object with bright knot(s);

Ir - irregular without knots or with amorphous condensations, the colour is neutral or bluish;

Sm - disturbed spiral or irregular with signs of spiral structure;

Sph - spheroidal, with very low brightness gradient or without any, the color is neutral or redish. The estimated optical surface brightness: high - H (22 - 23 mag/sq. arcsec), low - L (24 mag/sq. arcsec), very low - VL (25 mag/sq. arcsec), and extremely low - EL (26 mag/sq. arcsec) in Col. 7 is averaged over the visible galaxy ( $\sim D_{26.5}$). The total blue magnitude $B_{\rm t}$ and its reference follow in Cols. 8 and 9. "NED'' - data are from the NASA/ Extragalactic Database, "IK'' - visual estimates from POSS (typical error is about 0.4 mag) by I. Karachentsev. The Galactic extinction (Schlegel et al. 1998) follows in Col. 10. Other names (identifications) are listed in Col. 11.

 

 

Table 1: List of new local void dwarf candidates: optical data

KKR	RA (1950.0) Dec.		a	b	Type	S.B.	$B_{\rm t}$	Ref.(B)	$A_{\rm b}$	Identification
	h m s	$\hbox{$^\circ$ }\ \ \$$^\prime$ $\ \ \ \hbox{$^{\prime\prime}$ }$	arcmin
1	2	3	4	5	6	7	8	9	10	11
1	13 55 16.8	+08 04 51	0.50	0.30	Ir	L				D 721-17
2	14 03 58.2	+09 35 43	0.85	0.25	Im	L	16.8	IK	0.12	D 721-07
3	14 05 01.5	+35 17 47	1.10	0.65	Ir	VL	16.9	IK	0
4	14 13 57.0	+14 06 24	1.10	1.10	PN?	VL				F650-01
5	14 14 26.1	+04 03 55	1.00	0.65	Ir	L	16.6	IK	0.13	BCh(83)
6	14 14 28.9	-01 16 24	1.00	0.50	Ir	L	16.9	IK	0.22
7	14 14 44.3	+13 54 59	0.60	0.50	Ir	L
8	14 16 45.4	+03 21 08	1.30	0.80	Ir?	L				BCh(83)
9	14 24 47.9	+22 54 51	0.90	0.60	Sph?	VL
10	14 30 10.3	+31 43 45	0.65	0.50	Ir	L
11	14 43 14.7	+55 47 56	0.80	0.55	Ir	L	16.9	IK	0.07
12	14 44 01.3	+14 25 18	1.20	0.75	Ir	L	16.6	IK	0.09	F651-2
13	14 46 50.0	+34 54 58	1.10	0.90	Sm?	L	16.4	IK	0.09	U 9540
14	14 52 09.8	+01 21 50	0.50	0.30	Ir	L	17.8	NED	0.13
15	15 01 22.7	+00 37 25	0.50	0.35	Ir	L	17.6	IK	0.26
16	15 01 58.2	-02 23 35	1.00	0.70	Ir	H	16.5	IK	0.39
17	15 08 46.1	+11 13 13	0.45	0.30	Ir	L
18	15 15 35.5	+16 29 27	0.50	0.45	Ir	H	15.9	IK	0.14	MCG3-39-9
19	15 20 44.7	+57 29 17	0.90	0.60	Ir	VL
20	15 28 36.0	+03 59 58	1.30	0.90	Sm	L	16.5	IK	0.21
21	15 34 47.4	+20 57 31	1.1:	0.8:	SB?	L	16.8	IK	0.23	F583-2
22	15 43 27.7	+17 28 04	1.50	1.00	SB?	L	16.6	IK	0.16	F583-5
23	16 11 05.1	+17 19 07	1.40	0.90	Sm	L	16.0	IK	0.25	UGC 10281
24	16 11 25.5	+02 39 20	0.70	0.50	Ir	L
25	16 12 37.3	+54 29 46	1.10	0.65	Ir	L	17.0	IK	0.04
26	16 14 28.2	+16 12 30	0.45	0.40	Ir	L	17.1	IK	0.20
27	16 38 47.8	+22 00 45	0.40	0.20	Ir?	L
28	16 43 30.2	+02 44 39	1.00	0.30	Ir?	VL
29	16 46 13.8	+22 25 27	0.70	0.35	SB?	L
30	16 54 13.8	+08 04 34	1.10	0.85	Sm?	VL	17.0	IK	0.56
31	16 56 27.4	+23 16 50	0.70	0.35	Ir	L
32	16 59 25.4	+21 07 55	0.45	0.40	Ir	L
33	17 07 31.2	+07 50 55	2.10	0.90	Sm	L	16.7	IK	0.56
34	17 10 24.5	+13 57 58	0.50	0.30	Ir	L	17.8	IK	0.65
35	17 28 26.6	+06 22 25	0.45	0.30	Ir	L
36	17 43 45.0	+02 08 04	1.10	0.75	Sm?	L
37	17 44 57.1	+22 21 47	0.70	0.40	Ir	L
38	17 46 40.7	+26 13 01	0.80	0.45	Ir	L				F520-3
39	17 56 53.7	+21 51 02	0.60	0.35	Ir	VL	18.1	IK	0.46
40	18 03 01.7	+23 08 12	1.30	0.90	Ir	L	16.5	IK	0.49
41	18 06 14.5	+00 22 10	-	-	PN?	EL
42	18 09 09.0	+37 14 09	0.45	0.40	Ir	L	17.7	IK	0.21
43	18 14 54.8	+09 58 04	0.70	0.60	Sm?	L
44	18 33 48.0	+31 02 18	0.70	0.60	Ir	L
45	19 30 40.0	-00 43 45	1.00	0.90	Ir	L	17.5	IK	1.07	CGMW 3-4255

 

Table 1: continued

KKR	RA (1950.0) Dec.		a	b	Type	S.B.	$B_{\rm t}$	Ref.(B)	$A_{\rm b}$	Identification
	h m s	$\hbox{$^\circ$ }\ \ \ \hbox{$^\prime$ }\ \ \ \hbox{$^{\prime\prime}$ }$	arcmin
1	2	3	4	5	6	7	8	9	10	11
46	19 35 28.2	+54 31 33	0.85	0.65	Ir	L	17.5	IK	0.46
47	19 55 54.0	+42 07 34	0.85	0.45	Ir	L
48	19 57 14.7	+62 29 09	0.90	0.45	Ir	L	17.5	IK	0.36
49	19 59 13.1	+42 09 05	0.70	0.35	Ir	L	17.7	IK	2.33
50	20 08 49.0	+10 46 42	0.60	0.40	Ir	L
51	20 19 52.6	+52 18 26	0.75	0.35	Ir	L
52	20 28 05.4	+10 35 56	0.80	0.20	Ir	VL
53	20 30 49.1	+01 23 35	0.65	0.30	Ir?	L
54	20 33 23.7	-01 29 25	0.75	0.30	Ir	L
55	20 44 15.2	+60 13 40	0.60	0.40	Ir	L	17.0	IK	2.94	comp. N6946?
56	20 47 11.5	+58 25 56	0.70	0.45	Ir	L	17.6	IK	3.14	comp. N6946?
57	20 46 36.5	+62 53 03	0.50	0.45	Ir	L
58	20 48 19.1	+57 55 04	2.10	0.20	Sm	VL	17.9	IK	3.58	RFGC3647
59	21 02 02.8	+57 05 17	2.30	1.40	Ir	VL	15.7	IK	3.86	comp. N6946
60	21 04 30.6	+57 00 15	0.70	0.50	Ir	VL
61	21 16 29.6	+26 04 56	1.00	0.65	Sm?	L	16.9	IK	0.47
62	21 29 04.3	+52 28 24	-	-	Ir?	VL				Dw095+1.0?
63	21 53 40.8	+40 14 05	0.60	0.35	Ir	L
64	21 58 05.5	+41 47 15	1.0:	0.6	Ir	VL
65	22 00 02.0	+41 54 27	0.60	0.40	Ir	L
66	22 04 08.9	+37 25 25	1.00	0.60	Ir?	VL
67	22 04 12.3	+37 06 31	0.45	0.30	Ir?	L
68	22 09 43.2	+45 21 45	2.00	1.40	Sm	L	16.3	IK	1.38
69	22 09 54.9	+45 25 12	0.70	0.40	Ir	L	17.9	IK	1.43
70	22 25 44.2	+23 07 08	0.65	0.55	Ir	L				F533-1
71	22 28 24.7	+38 28 30	1.2:	0.80	Ir	VL	17.3	IK	0.53
72	22 33 48.4	+23 27 02	0.75	0.55	Ir?	L	17.24	NED	0.14	F533-v1
73	22 33 17.5	+23 20 50	0.35	0.35	Sph?	VL
74	23 08 19.5	+12 58 01	1.10	0.65	Ir	VL
75	23 17 39.6	+10 20 57	0.60	0.35	Ir	L	18.0	IK	0.21
76	23 19 09.1	+25 49 55	0.65	0.45	Ir	L
77	23 22 46.2	+12 26 26	0.60	0.40	Ir	L	17.4	IK	0.25	F677-v4
78	23 28 31.1	+22 09 57	0.55	0.45	Ir	L

Results of the H I observations are summarized in Table 2.

 

 

Table 2: List of new local void dwarf candidates: HI data

KKR	H I-flux	$S_{\max}$	velocity	line width	distance	$M_{\rm Bt}$	H I mass	$M_{{\rm H\,{\sc I}}}/L_{B}$	Comments
No.	Jy kms-1	mJy	kms-1	kms-1	Mpc		$10^{7}M_{\odot}$
1	2	3	4	5	6	7	8	9	10
1		$\pm6$
2	1.26	$19\pm6.3$	$3260\pm3$	57 95 96	43.2	-17.14	55	0.5
3	2.1	$110\pm9.6$	$63\pm2$	18 27 28	1.9	-9.57	0.17	1.58
4		$\pm 6.8$
5	8.74	$74\pm4.2$	$1470\pm3$	93 106 109	19.2	-15.17	76	4.2
6	2.76	$61\pm6.8$	$1546\pm2$	34 73 74	19.9	-15.18	26	1.4
7		$\pm6.5$
8		$\pm5.8$
9		$\pm9$
10		$\pm10$
11	2.64	$75\pm9$	$590\pm3$	29 46 49	10.2	-13.41	6.5	1.8
12	4.10	$102\pm8$	$1793\pm3$	42 60 65	24.4	-15.67	58	2.0
13	4.83	$49\pm7.9$	$802\pm2$	39 44 47	12.2	-14.23	17	2.2
14		$\pm11$
15	1.44	$40\pm8.4$	$1588\pm4$	23 44 61	21.1	-14.47	15	1.6
16	2.67	$37\pm7.8$	$1616\pm3$	99 109 111	21.3	-15.72	29	0.95
17		$\pm8.1$
18	1.25	$44\pm7$	$722\pm2$	38 44 45	10.5	-14.40	3.3	0.36
19		$\pm9$
20	4.32	$46\pm8$	$1775\pm2$	80 106 108	24.1	-15.81	59	1.8
21	6.12	$57\pm5.7$	$1719\pm2$	82 93 94	24.3	-15.52	85	3.4
22	2.72	$151\pm10$	$3261\pm1$	19 25 27	44.7	-17.02	130	1.3
23	5.83	$66\pm6.5$	$1084\pm2$	103 114 116	16.0	-15.50	35	1.4
24		$\pm12$
25	2.20	$101\pm10$	$-135\pm2$	14 30 35					local H I
26	2.31	$59\pm7$	$2251\pm2$	60 71 72	31.6	-15.66	54	1.9
27		$\pm6.7$
28		$\pm8.1$
29		$\pm8.4$
30	4.90	$68\pm5.8$	$1484\pm2$	80 87 91	21.4	-15.35	53	2.5
31		$\pm11$
32		$\pm7.4$
33	8.06	$74\pm8$	$2596\pm2$	128 137 144	36.3	-17.10	250	2.3
34	4.17	$52\pm6$	$1504\pm5$	89 102 106	22.1	-14.84	48	3.6
35		$\pm7.2$
36		$\pm12$
37		$\pm13$
38		$\pm12$
39	2.58	$59\pm10$	$2043\pm4$	41 69 73	30.0	-15.03	55	3.4
40	3.75	$47\pm7.9$	$2492\pm3$	106 115 116	36.1	-16.97	120	1.2	confused
41		$\pm8$
42	0.84	$29\pm5$	$1510\pm7$	27 38 41	23.4	-14.42	11	1.2
43		$\pm12$
44		$\pm11$
45	5.31	$81\pm10$	$1435\pm2$	72 89 92	21.5	-15.29	58	2.8
kkr3 = kk230 (e.g. Huchtmeier et al. 2000).
kkr40: UGC11111 (at 3.3$^\prime$) and UGC11113 (at 3.8$^\prime$) with similar radial velocities.

 

Table 2: continued

KKR	H I-flux	$S_{\max}$	velocity	line width	distance	$M_{\rm Bt}$	H I mass	$M_{{\rm H\,{\sc I}}}/L_{B}$	Comment
No.	Jy$\,$km$\,$s-1	mJy	km$\,$s-1	km$\,$s-1	Mpc		$10^{7}M_{\odot}$
1	2	3	4	5	6	7	8	9	10
46	3.53	$36\pm8.4$	$3779\pm5$	50 127 130	54.2	-16.77	240	3.1
47		$\pm9.3$
48	1.88	$30\pm7$	$3158\pm3$	48 51 92	45.9	-16.53	94	1.5
49	3.57	$55\pm8.2$	$785\pm4$	72 91 99	14.4	-15.78	17	0.6
50		$\pm11$
51		$\pm12$
52		$\pm18$
53		$\pm12$
54		$\pm11$
55	$\ge1$:	68 $\pm9.3$	23:	$\ge44$:	5.4	-14.8	$\ge0.7$	$\ge0.07$	local H I?
56	5.6:	$470 \pm8.5$	-135:	10 22 24:	6.4	-14.4	5.4	$\ge0.56$	local H I
57		$\pm7.9$
58	16.04	$101\pm9.4$	$2756\pm2$	246 277 280	40.7	-19.95	630	0.42
59	$\ge36$	680 $\pm8$	$\le17$:	$\ge64$:	4.7	-17.0	$\ge18.8$	$\ge0.32$	local H I?
60		$\pm9.1$
61	6.35	$110\pm8$	$919\pm2$	74 81 90	16.0	-14.82	3.8	2.9
62		$\pm18$
63		$\pm8.1$
64		$\pm9.7$
65		$\pm10$
66		$\pm7.8$
67		$\pm14$
68	19.5	$291\pm7.4$	$1145\pm1$	72 86 90	19.2	-16.68	170	2.3	confused?
69	14.3	$190\pm8.5$	$1143\pm1$	74 90 94	19.2	-15.24	120	6.4	confused
70		$\pm11$
71	5.64	$191\pm14$	$693\pm2$	26 35 40	13.1	-14.03	23	3.6
72		$\pm6.1$
73		$\pm5.9$
74		$\pm6.4$
75	3.56	$38\pm4.3$	$1469\pm5$	97 124 128	22.4	-14.24	42	5.4
76		$\pm7$
77	0.45	$32\pm8.4$	$3665\pm2$	29 33 40	51.7	-16.63	28	0.4
78		$\pm6.9$
kkr55, kkr56, kkr59 are possible companions of NGC6946.
kkr69 within 4.1 arcmin from kkr68, confused.

The kkr-number is given in Col. 1, the H I flux [Jykms^-1] follows in Col. 2, the maximum emission and/or the rms noise [mJy] in Col. 3, the heliocentric radial velocity plus error in Col. 4, the line widths at the 50%, the 25%, and the 20% level of the peak emission in Col. 5. "Kinematic'' distances (Col. 6) have been derived via corrected radial velocities assuming a Hubble constant of 75 kms^-1 Mpc^-1. The absolute magnitude is given in Col. 7, the integrated H I mass (Col. 8) was calculated as (e.g. Roberts 1969)

$$\begin{eqnarray*}(M_{{\rm H\,{\sc I}}}/M_{\odot})= 2.355 \ 10^{5} \ D^{2} \ \int S_{v}{\rm d}v \end{eqnarray*}$$

where D is the distance of the galaxy in Mpc and $\int S_{v}{\rm d}v$ is the integrated H I flux in Jykms^-1. The relative H I content $M_{{\rm H\,{\sc I}}}/L_{B}$ (in solar units) follows in Col. 9. Finally, Col. 10 contains comments. Possible confusion is mentioned in the footnotes to Table 2.

During the observing session we noticed radio interferences at certain times which did not have a strong influence on the observations. Most of the interference spikes are situated outside the velocity range of the H I profiles (e.g. kkr21, kkr39). In two cases a spike hits the profile (kkr49, kkr61). Baseline ripples are visible in a few spectra (e.g. kkr2, kkr22, kkr77). None of these events really perturb the measurement of the line parameters of narrow emission lines as for these dwarf galaxies.

In the case of kkr59 the H I emission from this galaxy is confused by Local H I emission. Its H I parameters may only be guessed, i.e. we get an upper limit for the radial velocity and lower limits for the line widths and the H I flux in this case.

In a number of cases emission at negative radial velocities has been observed (kkr25, kkr55, kkr56). The Dwingeloo H I survey (Hartmann & Burton 1997) shows that in all these cases extended H I emission was found at negative radial velocities suggesting that we may observe high velocity clouds in our Galaxy in these directions.