There are two mutually incompatible optical radial velocity
measurements for Phoenix, -52 +/- 6 (Gallart et al. 2001) and
-13 +/- 9 (Irwin & Tolstoy 2002). There is no obvious explanation for
the difference between them, nor any clear reason to choose either. I
have (somewhat arbitrarily) used the latter.
Although this galaxy is too far south for the LDS, it has been mapped
previously by Carignan, Demers, & Cote (1991), Young & Lo (1997), and
St-Germain et al. (1999). Because this galaxy lies close to the main
emission from the Milky Way, and its optical velocity has not yet been
measured, it is unclear which of two relatively compact velocity
components, if either, is associated with the galaxy. The H I properties
listed in Table 1 are from St-Germain et al. (1999). They cite evidence
suggesting that the lower mass (i.e., 2 x 10^5^ M_sun_) H I component is
associated with the galaxy, in part because they find the larger mass
component implausibly large. We follow their suggestion and use the
lower value in Figure 4 below. Without a reliable single-dish map,
however, it is unclear whether the interferometer recovers all of the
flux associated with the galaxy. Thus the mass quoted by St-Germain et
al. (1999) should be considered a lower limit.
Phoenix. Van de Rydt (1991). This is an intermediate-type dwarf galaxy that
apparently exhibits few blue supergiants and many red giants. The LF method, as
the brightest-star method, is inapplicable in such cases.
Well-resolved Phoenix dwarf. No knots.
=ESO 245- G 07
*associated? with ESO 245- G 05