Figure 3.
Global galaxy colors plotted against various other global
properties for galaxies in our samples.
The filled-circles are Im
galaxies, the "x" are Sm, and the open circles are BCD galaxies.
SB_25 is the surface brightness in magnitudes per arcsec^2
measured within the radius where the surface brightness declines to
25 magnitude per arcsec^2. The "SFR/area" is the star formation rate
in solar masses per year within the area defined by the 25 magnitude
per arcsec^2 surface brightness
contour in kpc^2. L_IR is the far-infrared
luminosity determined from observations at 60 and 100 microns
by the Infrared Astronomical Satellite.
M_gas is M_HI+M_H_2 where M_H_2 is estimated
as a fraction of the M_HI from observations of the Large and
Small Magellanic Clouds. M_tot is a dynamical mass estimated
from the FWHM of an integrated HI profile.
(Funded by NSF through grant AST-9802193 to DAH. Summer
fellowship to LH funded by the Friends of Lowell.)
Figure 4.
Reddenings internal to the HII regions
plotted against the global color of the galaxy.
The reddenings are galaxy averages when multiple HII
regions were observed. The (U-B)_0 colors
have been corrected for foreground reddening plus 0.05 in E(B-V)
to account for some small reddening of the stars.
(Funded by NSF through grant AST-9802193 to DAH. Summer
fellowship to LH funded by the Friends of Lowell.)
Figure 5.
Number distribution of BCD and Im galaxies in our sample
as a function of the O/H abundance.
Several Im and BCD galaxies have been added from the literature.
(Funded by NSF through grant AST-9802193 to DAH. Summer
fellowship to LH funded by the Friends of Lowell.)
Figure 6.
Galaxy-wide average oxygen abundance plotted against
various global properties of the galaxies in our samples.
The filled-circles are Im
galaxies, the "x" are Sm, and the open circles are BCD galaxies.
(Funded by NSF through grant AST-9802193 to DAH. Summer
fellowship to LH funded by the Friends of Lowell.)
Figure 7.
Galactic M_B plotted against the oxygen abundance.
Error bars are the dispersions around the mean of
the oxygen abundance determined in a galaxy with multiple HII
region measurements or the uncertainty in the measurement for
galaxies with only one measured HII region.
The solid line is the relationship
derived by Richer & McCall (1995) between M_B and O/H
for low luminosity galaxies. The dashed line in the middle panel
is the relationship seen in a sample of emission-line galaxies
by Salzer et al. (1989).
Im and Sm samples are plotted in the upper panel, the BCD sample in
the middle panel, and all of the galaxies along with spirals from
Zaritsky, Kennicutt, & Huchra (1994) in the bottom panel.
Except for the spirals,
galaxies are distinguished in the plots by the method used to
estimate O/H:
The label "4363" means that the determination of O/H was from use
of [OIII]4363 to determine T_e,
"McG" refers to the method of McGaugh(1991),
"EP" refers to the method of Edmunds & Pagel (1984),
and "lit" refers to values taken from the literature.
(Funded by NSF through grant AST-9802193 to DAH. Summer
fellowship to LH funded by the Friends of Lowell.)
Figure 4.
Reddenings internal to the HII regions
plotted against the global color of the galaxy.
The reddenings are galaxy averages when multiple HII
regions were observed. The (U-B)_0 colors
have been corrected for foreground reddening plus 0.05 in E(B-V)
to account for some small reddening of the stars.
(Funded by NSF through grant AST-9802193 to DAH. Summer
fellowship to LH funded by the Friends of Lowell.)
Figure 6.
Galaxy-wide average oxygen abundance plotted against
various global properties of the galaxies in our samples.
The filled-circles are Im
galaxies, the "x" are Sm, and the open circles are BCD galaxies.
(Funded by NSF through grant AST-9802193 to DAH. Summer
fellowship to LH funded by the Friends of Lowell.)
Figure 7.
Galactic M_B plotted against the oxygen abundance.
Error bars are the dispersions around the mean of
the oxygen abundance determined in a galaxy with multiple HII
region measurements or the uncertainty in the measurement for
galaxies with only one measured HII region.
The solid line is the relationship
derived by Richer & McCall (1995) between M_B and O/H
for low luminosity galaxies. The dashed line in the middle panel
is the relationship seen in a sample of emission-line galaxies
by Salzer et al. (1989).
Im and Sm samples are plotted in the upper panel, the BCD sample in
the middle panel, and all of the galaxies along with spirals from
Zaritsky, Kennicutt, & Huchra (1994) in the bottom panel.
Except for the spirals,
galaxies are distinguished in the plots by the method used to
estimate O/H:
The label "4363" means that the determination of O/H was from use
of [OIII]4363 to determine T_e,
"McG" refers to the method of McGaugh(1991),
"EP" refers to the method of Edmunds & Pagel (1984),
and "lit" refers to values taken from the literature.
(Funded by NSF through grant AST-9802193 to DAH. Summer
fellowship to LH funded by the Friends of Lowell.)