Figure 1.
Distance in parsecs from the center of the galaxy to the
brightest HII regions plotted as a function of the distance
in parsecs to the rotation curve turnover. Four of the galaxies have
two rotation curve turnovers plotted. The closed circle or
triangle represents the point
where the rotation velocity reaches a maximum and the open square
represents the point where the slope in the rotation curve changes as it
is still rising. The triangles represent giant HII regions.
The dashed line represents the line where the distance to the brightest
HII regions is equal to the distance to the rotation curve turnover.
(Funded by NSF through grant AST-9802193 to DAH.
Work by EWR was funded by NSF through the
Research Experiences for Undergraduates program,
under grant number 9423921 to Northern Arizona University.)
Figure 2.
Distance in parsecs to the furthest HII regions
plotted as a function of the distance in parsecs to the rotation curve
turnover. The closed circles represent the points where the
rotation velocity reaches a maximum and the open squares represent
the point where the slope in the rotation curve changes as it is still
rising. The dashed line represents the line where the distance to the
furthest HII regions is equal to the distance to the rotation
curve turnover. The two galaxies falling furthest above this line
are NGC 4214 and NGC 2366.
(Funded by NSF through grant AST-9802193 to DAH.
Work by EWR was funded by NSF through the
Research Experiences for Undergraduates program,
under grant number 9423921 to Northern Arizona University.)
Figure 4.
Distances in parsecs to all the HII complexes
in the galaxies
plotted as a function of the distances in parsecs to the rotation curve
turnover. The dashed line represents the line where the distance to
the HII complexes is equal to the distance to the rotation
curve turnover.
(Funded by NSF through grant AST-9802193 to DAH.
Work by EWR was funded by NSF through the
Research Experiences for Undergraduates program,
under grant number 9423921 to Northern Arizona University.)
Figure 5.
Star formation rate (SFR) plotted as
a fuction of V_{rot,max} for those galaxies
with rotation information. Right--pointing arrows extending from
some of the points indicate lower limits to the V_{rot,max} because
the rotation curves do not flatten out.
Upper limits to the rotation velocity are shown for galaxies with
no measureable rotation.
(Funded by NSF through grant AST-9802193 to DAH.
Work by EWR was funded by NSF through the
Research Experiences for Undergraduates program,
under grant number 9423921 to Northern Arizona University.)
Figure 2.
Distance in parsecs to the furthest HII regions
plotted as a function of the distance in parsecs to the rotation curve
turnover. The closed circles represent the points where the
rotation velocity reaches a maximum and the open squares represent
the point where the slope in the rotation curve changes as it is still
rising. The dashed line represents the line where the distance to the
furthest HII regions is equal to the distance to the rotation
curve turnover. The two galaxies falling furthest above this line
are NGC 4214 and NGC 2366.
(Funded by NSF through grant AST-9802193 to DAH.
Work by EWR was funded by NSF through the
Research Experiences for Undergraduates program,
under grant number 9423921 to Northern Arizona University.)
Figure 4.
Distances in parsecs to all the HII complexes
in the galaxies
plotted as a function of the distances in parsecs to the rotation curve
turnover. The dashed line represents the line where the distance to
the HII complexes is equal to the distance to the rotation
curve turnover.
(Funded by NSF through grant AST-9802193 to DAH.
Work by EWR was funded by NSF through the
Research Experiences for Undergraduates program,
under grant number 9423921 to Northern Arizona University.)
Figure 5.
Star formation rate (SFR) plotted as
a fuction of V_{rot,max} for those galaxies
with rotation information. Right--pointing arrows extending from
some of the points indicate lower limits to the V_{rot,max} because
the rotation curves do not flatten out.
Upper limits to the rotation velocity are shown for galaxies with
no measureable rotation.
(Funded by NSF through grant AST-9802193 to DAH.
Work by EWR was funded by NSF through the
Research Experiences for Undergraduates program,
under grant number 9423921 to Northern Arizona University.)