3 The list of dwarf galaxy candidates

To detect new dwarf galaxies we used J and R film copies of the Second Palomar Sky Survey, POSS-II. The high angular resolution of new photographic emulsions and their sensitivity to low contrast details permit the detection and classification with confidence of galaxies of small angular dimensions, especially of low surface brightness objects. Following the method described earlier (Karachentseva & Karachentsev 1998 = Survey I), we searched for dwarf galaxies with angular diameters more than about 0.5 arcmin in a wide region limited to RA = [14.0, 23.5]$^{\rm h}$, $D = [-3,\;+63$]$\hbox{$^\circ$}$.Because in the previous Survey-I we searched for very nearby dwarf galaxies with V₀ < 500 km s^-1, i.e. about 3 times lower than in the present survey, we relaxed slightly our criterion, not requiring signs of possible resolution of into stars.

We found 78 dwarf galaxy candidates, which are presented in Table 1. Here Col. 1 gives the object number indicating the POSS-II field number; Col. 2 contain the equatorial coordinates (epoch 1950.0); Col. 3 gives the major and minor angular diameters in arcmin measured on the blue and red films, respectively; Col. 4 gives the morphological type in the usual designations ("d" as a "dwarf" was omitted); Col. 5 gives a rough estimate of surface brightness: H-high (equal or brighter than for a normal spiral galaxy), L -- low, VL -- very low, EL -- extremely low, i.e. invisible on POSS-I (this means a mean SB brighter than about 26 mag/$\ifmmode\hbox{\rlap{$\sqcap$}$\sqcup$}\else{\unskip\nobreak\hfil \penalty50\hsk... ...up$} \parfillskip=0pt\finalhyphendemerits=0\endgraf}\fi\hbox{$^{\prime\prime}$}$); Col. 6 gives the cross-identification with other lists (D or F -- Schombert et al. 1992, BCh, 83 -- Balkowski & Chamaraux 1983); Col. 7 gives the galaxy morphology description, or the heliocentric radial velocity and magnitude estimated from NED.

The distribution of the 78 galaxies from Table 1 is presented in Fig. 3 by diamonds. Obviously, the detected new objects are distributed more or less regularly over the whole studied area. This picture gives no indication of the Local Void. However, only redshift measurements for the new objects can show, if they fill the Local Void volume or not. A HI survey of the objects from Table 1 is presently in progress at the 100-m Effelsberg radio telescope. (Huchtmeier 1998).

 

Figure 3: Distribution of new dwarf galaxy candidates in the same area (diamonds)

 

Table 1: List of new dwarf galaxy candidates towards the Local Void

 

Table 1: continued

 

Table 1: continued