Figure 1.
Positions that were observed within and near the optical
part of the galaxy
are shown superposed on
an HI map of NGC 4449. The size of the circles represents the average FWHM
of the beam. The larger circles are millimeter observations obtained
with the NRAO 12 m telescope; the smaller one near the center is a
submillimeter observation obtained with the SMTO.
The integrated HI map is from Hunter, van Woerden, & Gallagher (1999).
The synthesized beam width in the HI map is 9.8 arcsec X 7.8 arcsec.
(Funded by the Lowell Research Fund and NSF through grant AST-9616940 to DAH.}
Figure 2.
Positions that were observed in the outer part of the galaxy's
HI are shown superposed on
an HI map of NGC 4449. The size of the circles represents the average FWHM
of the beam of the
NRAO 12 m telescope.
The integrated HI map is from Hunter et al. (1998).
The synthesized beam width in the HI map is
62 arcsecX54 arcsec.
(Funded by the Lowell Research Fund and NSF through grant AST-9616940 to DAH.}
Figure 6.
Molecular mass estimated from the CO observations
plotted against various properties of the HI gas mass included
in the beam of the CO observations.
(Funded by the Lowell Research Fund and NSF through grant AST-9616940 to DAH.}
Figure 7.
Positions of CO observations are shown superposed on an
Halpha image of NGC 4449 (Hunter et al. 1999).
(Funded by the Lowell Research Fund and NSF through grant AST-9616940 to DAH.}
Figure 8.
Several properties of the CO observations compared to
properties of the Halpha.
L_Halpha is measured for each of the CO positions
by summing the flux in an Halpha image over a square whose
length is the diameter of the HPBW of the CO observations.
An L_Halpha of 0 is plotted at log L_Halpha=0 in order
to show the regions without star formation.
(Funded by the Lowell Research Fund and NSF through grant AST-9616940 to DAH.}
Figure 9.
Properties of the CO observations plotted
as a function of radius from the center of the galaxy.
The distance in the plane of the galaxy has been determined
using an inclination and position angle appropriate for
the extended gas in NGC 4449, which is really only
appropriate beyond about 2 kpc.
(Funded by the Lowell Research Fund and NSF through grant AST-9616940 to DAH.}
Figure 2.
Positions that were observed in the outer part of the galaxy's
HI are shown superposed on
an HI map of NGC 4449. The size of the circles represents the average FWHM
of the beam of the
NRAO 12 m telescope.
The integrated HI map is from Hunter et al. (1998).
The synthesized beam width in the HI map is
62 arcsecX54 arcsec.
(Funded by the Lowell Research Fund and NSF through grant AST-9616940 to DAH.}
Figure 6.
Molecular mass estimated from the CO observations
plotted against various properties of the HI gas mass included
in the beam of the CO observations.
(Funded by the Lowell Research Fund and NSF through grant AST-9616940 to DAH.}
Figure 7.
Positions of CO observations are shown superposed on an
Halpha image of NGC 4449 (Hunter et al. 1999).
(Funded by the Lowell Research Fund and NSF through grant AST-9616940 to DAH.}
Figure 8.
Several properties of the CO observations compared to
properties of the Halpha.
L_Halpha is measured for each of the CO positions
by summing the flux in an Halpha image over a square whose
length is the diameter of the HPBW of the CO observations.
An L_Halpha of 0 is plotted at log L_Halpha=0 in order
to show the regions without star formation.
(Funded by the Lowell Research Fund and NSF through grant AST-9616940 to DAH.}
Figure 9.
Properties of the CO observations plotted
as a function of radius from the center of the galaxy.
The distance in the plane of the galaxy has been determined
using an inclination and position angle appropriate for
the extended gas in NGC 4449, which is really only
appropriate beyond about 2 kpc.
(Funded by the Lowell Research Fund and NSF through grant AST-9616940 to DAH.}