NGC 3275 (Fig. 8d, available in the online version). This is also an
example of a bar/ring system, but in this case there are also
large-scale spiral arms outside the bar. The Q_T_ profiles in NGC 5101
and 3275 have different shapes. The broad hump in the Q_T_ profile of
NGC 3275 is caused by the strong material condensations at the two ends
of the bar coinciding with the radius of the inner ring. It is not
clear in the direct image whether these blobs are part of the inner
ring or part of the large-scale spiral arms.
NGC 3275 (Fig. 8d, available in the online version). This is also an example of
a bar/ring system, but in this case there are also largescale spiral arms
outside the bar. The Q_T_ profles in NGC 5101 and 3275 have different shapes.
The broad hump in the Q_T_ profle of NGC 3275 is caused by the strong material
condensations at the two ends of the bar coinciding with the radius of the inner
ring. It is not clear in the direct image whether these blobs are part of the
inner ring or part of the large-scale spiral arms.
NGC 3504 (Fig. 8e, available in the online version; see also Fig. 2). This is
another example of a bar/ring system with prominent spiral arms, which are
forming a ring. This is a good example of galaxies showing a bar with two blobs
at the ends of the bar, manifesting also some spiral-like characteristics. The
amplitude profle also has two peaks in the bar region. In this case, the tiny
spiral arm segments are not related to the outer spiral arm structure, being
rather part of the bar/inner ring system. The Q_T_ profle is asymmetric, but in
the opposite direction than in NGC 5101. The outer pseudo-ring of NGC 3504 is
type R'_1_ (appendix 3 of RC3).
NGC 3275: Mulchaey et al. (1997). Outer-bar measurements are from the
publically available images of Mulchaey et al.; inner-bar measurements
are from a NICMOS3 F160W image, with L_bar_ based on the nuclear ring
NGC 3275.---SB(r)ab: Very bright nucleus embedded in an elliptical
bulge with a short bar. The bulge is embedded in a lens that extends
to the ends of the bar. Faint spiral arms emerge from bar ends. Arms
have no evidence for knots. At high surface brightness, the major disk
of the galaxy is aligned with the bar (P.A. is ~135deg), but at lower
surface brightness, the P.A. is closer to 0deg.
Primary bar is visible in both the K_S_image and the ellipse fits. A
secondary bar on the scales of several arcseconds is visible in the
Antlia Group #244
Jan 6/7, 1978
103aO + GG385
NGC 3275 is in the Antlia Group Catalog (Ferguson and Sandage
1990). Its morphological type is listed there as SBb from an
independent classification. The classification of SBab here is
arbitrarily earlier than SBb for the reason used in the RSA2 listing,
the thinness of the arms.
The arms do not spring from the ends of the bar, as in the
prototype SBb galaxy NGC 1300 (panels 154, S8), but rather start, as
in NGC 1389, at a position on the broad bar that is about 90^deg^ from
the ends of the bar. This is a common feature of SBa(r) subtypes, as
discussed in the SBa section.
The arms are tightly wound, each nearly touching one another
after unwinding by about half a revolution, as has often been
described (compare NGC 3081, NGC 3185, and IC 5240, all shown in the
SBa section, panel 99). This feature is often mistaken for an internal
ring but is almost always two nearly overlapping separate spiral arms
of the grand design type.
Overexposed center, dist bar and (r): 0.95 x 0.65, pretty smooth dist arms.
=ESO 375- G 50
Two characteristic straight dust lanes on outer edge on
either side of the weak bar (as in type examples of SBb).
Large, smooth (population II) central region.
Star arms begin with interesting detail on a ring,
but the two dust lanes spring from ends of the weak bar
as in the SB(s) types (NGC 1300).
Im portant example for studies of dust lane morphology.
Pair with NGC 3275A (S sp) 9.8 arcmin.
Small, bright nucleus. Weak bar. (r): 0.95 arcmin x 0.75 arcmin with
a faint star on it. There is another faint star 0.2 arcmin south-following
Pair with NGC 3275A S sp 0.85 arcmin x 0.2 arcmin at 9.8 arcmin.