We make use of the the Lyon Extragalactic Cepheid Database (Lanoix et al. 1999b). In this database there are 32 galaxies with both V and I band photometry. 23 galaxies have Cepheid measurement from the HST and rest have groundbased measurements. The PL relation was calibrated using a sample of galactic Cepheids measured with the astrometric HIPPARCOS satellite (Lanoix et al. 1999a) and corrected for a Malmquist-like bias according to Lanoix et al. (1999c).

As we are interested in the very local velocity field we restricted our sample by requiring $R_{\rm gal}\le7{\rm\ Mpc}$ , where also the Virgo-centric flow correction is small. $R_{\rm gal}$ refers to the distance in Mpc measured from Galaxy. We were left with 14 galaxies. The Virgo flow at larger distances was studied with Cepheid-based distances in Ekholm et al. (1999a).

In Table 1 we present the data relevant for the present analysis. In Col. 1 we give the PGC number and in Col. 2 we give the name. In Col. 3 we give the distance in Mpc as calculated from the distance moduli provided in the Lyon Extragalactic Cepheid Database. In Col. 4 we give the distance in Mpc as seen from the barycentre of the Local Group. In Cols. 5-7 we give the velocities: $V_{\odot}$ is the mean heliocentric velocity extracted from LEDA (the Lyon-Meudon Extragalactic Database), $V_{\rm Yahil}$ is $V_{\odot}$ corrected for the centroid of the Local Group according to Yahil (1977) and $V_{\rm corr}$ is $V_{\rm Yahil}$ corrected for the virgocentric motion. We explain these corrections in the next section. As regards uncertainties in the parameters we note that the mean error for $V_{\odot}$ is 6.4 kms^-1. In Fig. 1 we plot the error bars reflecting the uncertainties in the Cepheid distances.

Finally we remind that LMC and NGC 6822 belong to the Milky Way subsystem and NGC 598 (M 33) is a member of the M 31 subsystem. The status of the irregular galaxy IC 1613 is unclear. Gurzadian et al. (1993) and Rauzy & Gurzadian (1998) link it with the Galaxy, but van den Bergh (1999) recognizes that IC 1613 may be a free-floating member of the Local Group. Thus it is wise to consider it as a special case in our diagrams.

Table 1: In this table we present the the crucial data for the 14 galaxies with extragalactic PL-distances. The entries are explained in the text
LEDA NAME $R_{\rm gal}$ $R_{\rm 2/3}$ $V_{\odot}$ $V_{\rm Yahil}$ $V_{\rm corr}$

3844 IC 1613 0.69 0.44 -231 -62 -72

45314 IC 4182 4.94 5.09 316 337 274

17223 LMC 0.05 0.61 317 81 82

2557 N224 0.87 0.29 -300 -13 -12.7

3238 N300 2.17 2.13 142 125 101

28630 N3031 3.37 3.18 -35 125 147

29128 N3109 1.02 1.53 404 130 131

34554 N3621 6.61 7.16 727 436 457

48334 N5253 3.16 3.73 403 155 153

50063 N5457 6.92 6.87 240 361 374

5818 N598 0.79 0.27 -180 69 66

63616 N6822 0.45 0.73 -56 8 11

29653 SEXA 1.45 1.88 325 118 110

28913 SEXB 1.39 1.76 302 139 131

LEDA	NAME	$R_{\rm gal}$	$R_{\rm 2/3}$	$V_{\odot}$	$V_{\rm Yahil}$	$V_{\rm corr}$
3844	IC 1613	0.69	0.44	-231	-62	-72
45314	IC 4182	4.94	5.09	316	337	274
17223	LMC	0.05	0.61	317	81	82
2557	N224	0.87	0.29	-300	-13	-12.7
3238	N300	2.17	2.13	142	125	101
28630	N3031	3.37	3.18	-35	125	147
29128	N3109	1.02	1.53	404	130	131
34554	N3621	6.61	7.16	727	436	457
48334	N5253	3.16	3.73	403	155	153
50063	N5457	6.92	6.87	240	361	374
5818	N598	0.79	0.27	-180	69	66
63616	N6822	0.45	0.73	-56	8	11
29653	SEXA	1.45	1.88	325	118	110
28913	SEXB	1.39	1.76	302	139	131

2 The sample