The availability of high-quality Sky Surveys, POSS-II and ESO/SERC, made on new photographic emulsions stimulated strongly the present search. The high angular resolution and the sensitivity to low contrast details permit the detection and classification with confidence of galaxies of small angular dimensions, especially low surface brightness objects. Using our previous experience of searching for low surface brightness objects on the POSS-I prints (Karachentseva 1968, 1972, 1973), we undertook analogous searches based on new observational material. Due to the different morphology of dwarf galaxies there are no distinct criteria to distinguish them from a normal distant galaxy of the same angular diameter (or from a part of a reflecting nebula). Typical cases of such visual misclassification were described by Karachentseva et al. (1985). Indeed, a search for the nearby dwarf galaxy candidates seems to be a rather delicate subject. To complete the KKT- sample with new very nearby galaxies we used the following strategy:
1. Dwarf companions of the known nearby galaxies were assumed to
be the main supplier of new objects for the Local Volume (=LV). Following
this idea we searched on the POSS-II or ESO/SERC two-colour films for
dwarf galaxies down to the limiting angular diameter 0.5 arcmin around
each of 215 LV galaxies with V0 < 500 km/s from the list by
Karachentsev
(1994), which is an up-dated version of the KKT-sample.
The diameter of the inspected area around each of the LV galaxies was
chosen equal to 50 times its diameter. So, for a normal galaxy 20 kpc
in diameter the survey area corresponds to a 1 Mpc diameter circle and
exceeds the crossing length for the satellite during a cosmological time
of 1/H. Because of the present incompleteness of the POSS-II survey we used in 
%
of the cases the POSS-I prints too.
2. In addition to the inspected neighbourhood of individual galaxies we
carried out a total visual examination of wide regions of the well-known nearby
galaxy groups: the M 31, M 81, M 101, IC 342/Maffei, Sculptor, Centaurus and
the Canes Venatici cloud, indicated in the Nearby Galaxy Catalog of
Tully (1988).
In case of CnV the survey area was limited to
, 
], 
, 
].
3. Using the POSS-II and ESO/SERC films we revised the images of dwarf galaxies from the catalogues of Karachentseva & Sharina (1988), and Arp & Madore (1989). The objects with signs of possible resolution into stars have been included, as a rule, in the candidate list.
4. To fill in the empty cone evoked by excluding all galaxies in
the Virgo cluster direction, we inspected the galaxy images of the angular
diameter 
arcmin within the boundaries , 
],
, 
]. As an example, we considered the dwarf system GR 8
(Reaves 1983) situated in front of the Virgo cluster.
5. Into our list of the LV candidates there were included also
galaxies with recent radial velocity determinations, mainly from the HI
surveys
(Huchtmeier & Richter 1989b;
Shombert et al. 1992;
Kraan-Korteweg et al. 1994;
Garcia et al. 1994;
Gallagher et al. 1995;
Huchtmeier et al. 1995;
Mattews et al. 1995;
Huchtmeier & van Driel 1996;
Mattews & Gallagher 1996) when their corrected velocities did not exceed 500 km/s. Note that due
to the influence of Galactic hydrogen, the low signal-to-noise ratio or other
reasons the small value of galaxy radial velocity would often seem doubtful.
That is why our decision to include a galaxy in the list took into
account the visual impression about its structure. We used also the available
version of the ZCAT (Huchra 1995) which contains 386 objects with 
.
Of them 215 are in the Karachentsev (1994) list, and 97 objects are
members of the Virgo cluster. The remaining 74 ones formed a set of strange
cases. Note some typical examples: