NGC 1744 (SBd, 1"~36 pc, I=64.4^deg^)
The galaxy is inclined at I~65^deg^ and, moreover, our image is noisy: the
ellipse fitting is not reliable. No clear evidence for twist is found.
March 14/15, 1980
103aO + GG385
Brightest stars begin to resolve in abundance
in NGC 1744 about 1 mag above the plate
limit, which is near B = 23. The very brightest
star may have B = 20.5, but the numerous HII
regions must be separated from the stellar
candidates before the brightest-star data are secure.
Star-formation and HII regions exist over the
central oval and inner disk.
The redshift is v_o = 639 km/s. The resolution
into stars is not as pronounced as in NGC 45
(two panels back), which has a smaller redshift
by a factor of 1.2. If the redshift-distance relation
were noiseless, the magnitude difference between
the brightest stars in NGC 1744 and NGC 45
would be 0.4 mag. However, the observed
difference in the resolution level of the brightest
stars is about 1 mag, suggesting noise in the
velocity field of about +/-100 km/s. Such a
random velocity about the Hubble flow is, of
course, small. This method has important
promise and can be used out to distances of about
three-fourths the distance to the Virgo Cluster.
At this late type [SB(s)d] and high inclination, the spiral arms are
becoming difficult to trace. H II regions can be seen right across the
bar, and out into the northern and western arms, but the short
southeastern arm contains only a single giant H II region. Even the wispy
arm running south from the north end of the bar is found to harbor at
least three active star-forming regions.
Bright bar, faint arms with many knots. Near calibration cutout;
dimensions may be too small.
Narrow, knotty, bright bar: 1.3 arcmin x 0.3 arcmin.
Several partially resolved filamentary arms.
Very low surface brightness.
HMS Note No. 031
Slit on central bar.