There are a few cases of high
values in Table 2.
Four of the five galaxies with
are actually found to be
confused by emission from nearby galaxies (see footnotes to Table2).
The present sample of galaxies as presented in Tables 1 and 2 will be discussed now in some detail with the help of global parameters. The distribution of radial velocity (v0, corrected for the rotation of our galaxy) is given in Fig.4. Apart from a few background objects most of the galaxies belong to the local supercluster, about 25% are within the Local Volume. From this situation it is clear that the great majority of the galaxies in the present sample are dwarfish in nature. This will be shown more convincingly below when we compare several other global parameters of these objects.
Next we will look at the optical linear diameter A0 (in kpc). The
histogram in Fig.5 presents the number of galaxies binned in intervals of
0.5 kpc width. The
distribution of the optical linear diameters of our galaxies extends from 0.2
kpc to 26 kpc, yet the great majority is smaller than 8 kpc in diameter
(in the de Vaucouleurs D25 system). Galaxies in the Local Volume
(indicated by shaded areas) are even smaller with a median value of
1.4
0.2 kpc.
Now we will use the correlation of two global parameters to compare
the present sample of galaxies with the previously known galaxies
in the Local Volume. In Fig.6 the total mass of neutral hydrogen
of
the galaxies is plotted versus their linear extent A0 for this
sample of galaxies.
The full line is the regression line for the
KKT sample (Huchtmeier & Richter 1988). This regression line seems to
be an excellent fit for the present sample, too.
The average HI mass of the galaxies in the Local Volume is 4.6 107
.
The HI masses in Fig.6 cover a range from 106 to 1010 solar masses. The HI luminosity function for galaxies has been studied with galaxies of 107 and more solar masses in HI so far. With the data of the new dwarf galaxies within the Local Volume we will be able in the end to discuss the HI luminosity function starting from 106 solar masses.
The galaxies in our sample have small line widths on the average. In Fig.7 we present the distribution of observed line widths in the upper panel and the (for inclination) corrected line widths in the lower panel. The optical axial ratio has been used here to derive the inclination. Galaxies within the Local Volume are indicated by the shaded areas. The peak of the line width distribution of the galaxies within the Local Volume is 39 kms-1 for the uncorrected and 47 kms-1 for the corrected line widths.
The three global parameters we have considered so far point
altogether toward the dwarfish character of the Local Volume objects in our
sample: the average linear diameter of
kpc (Fig. 5),
the mean total HI mass of 4.6 107
and the small line
width of less than 50 km s-1.
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Figure 8:
The pseudo column density of neutral hydrogen (
![]() ![]() ![]() |
Two more global parameters are shown in Fig.8, pseudo HI surface
density
and the relative HI content
.
The pseudo HI surface density is obtained by dividing the total HI mass
of the galaxy by the disk area of the galaxy as defined by its
optical diameter A0. This quantity is given in units of solar mass
per square parsec as well as in the usual HI column density
in
atoms cm-2. This quantity is plotted versus the relative HI content
.
Our galaxies fill the usual range in HI surface density
as well as in relative HI content as observed for normal galaxies (e.g.
HR).
The present sample of galaxies is relatively rich in HI. Some of the
scatter in the diagram is due to uncertainties in observed quantities,
especially the inclination which is used to correct the line width
which itself enters the total mass calculation by the square. The
optical diameters are uncertain for galaxies at low galactic latitudes
due to the high foreground extinction, e.g. Cas2, ESO 137-G27, BK12, ESO 558-11.
If we exclude the confused galaxies and those with heavy galactic
extinction all entries in Fig.8 with
100
pc-2 are gone. Low values of the HI surface density are
not only due to the uncertainties of observational data, the gas content
of dwarf galaxies is very sensitive to outside influences (tidal interactions)
due to their shallow gravitational potential.
Finally we plot the HI surface brightness versus the optical surface brightness (Fig.9). The surface brightness class (Table 1, Col. 7) has been coded from 4 to 1 from high SB to extremely low SB in steps of 1. The different errors of the mean values of each class essentially depend on the different population size of each SB class. However, there is a definite trend of the HI surface density to grow with increasing optical SB by a factor of 2 to 4 (e.g. van der Hulst et al. 1993; de Blok 1997).
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