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Notes for object NGC 1326

11 note(s) found in NED.


1. 2006AJ....132.2634L
Re:NGC 1326
This is a well-studied galaxy previously reported to have a primary bar, a
possible nuclear bar, and inner and outer rings. The outer ring is an
exceptionally bright example of the outer Lindblad resonance subclass R_1_,
characterized by an approximate alignment perpendicular to the bar and by slight
dimpling in its shape near the bar axis (Buta & Crocker 1991). The nuclear ring
is also an exceptional star-forming feature that has been well studied from both
ground and space (Buta & Crocker 1991; Garcia-Barreto et al. 1991;
Storchi-Bergman et al. 1996; Cid Fernandes et al. 1998; Buta et al. 2000). The
inner bar and the inner and outer rings are visible in our K_s_-band image, and
the nuclear ring is evident in the J - K_s_ color map. We detect a faint
secondary bar inside the nuclear ring, which is most visible in the K_s_-band
image after subtracting the bulge model (Fig. 5). The possible double-barred
nature of NGC 1326 was previously discussed by de Vaucouleurs (1974), Buta &
Crocker (1991), Wozniak et al. (1995), and Erwin (2004), but it has been
difficult to verify owing to strong extinction inside the nuclear ring. The best
evidence presented previously was by Erwin (2004), but the resolution in our
K_s_-band image is sufficient now to confirm it. The J - K_s_ color index map in
Figure 1 shows that dust still has some impact in the near-infrared bands inside
the nuclear ring. The ring is red in this map, which suggests the presence of
red supergiants. In our decomposition for NGC 1326, in addition to the bulge and
the disk we also fitted two bars. This solution converges only if the flattening
of the bulge is taken into account. Models for the individual components were
found in small steps, and finally all components were fitted simultaneously. The
bulge in this galaxy was found to be quite prominent (B/T = 0.34, n = 3.0) but
much less luminous than argued by SGA04. They found a very weak extended disk
embedded inside a large de Vaucouleurs type bulge dominating the whole surface
brightness profile, leading to B/T = 0.63 and n = 4.9. For comparison, we also
made bulge-disk-bar and bulge-disk decompositions, the former leading to B/T =
0.42 and the latter to B/T = 0.58 (and n = 3.1) (see also Fig. 6). However, in
the bulge-disk decomposition the flux of the bar/oval goes erroneously to the
bulge. It is also worth noting that the B/T in the bulge-disk-bar decomposition
is somewhat larger than in the decomposition in which two bars were fitted (B/T
= 0.42 vs. 0.34), which means that in this case even the bar/oval (visible as a
bump at r = 5" - 10" in the {MU}-profile) affects the solution.

2. 2004A&A...415..941E
Re:NGC 1326
NGC 1326: This is one of two double-barred galaxies originally discussed by de
Vaucouleurs (1974); it has also been reported by Buta & Crocker (1993) and
Wozniak et al. (1995). Inspection of WFPC2 F814W images shows very strong dust
lanes inside a dusty, star-forming nuclear ring, which combine to produce the
illusion of an inner bar. Near-IR images are needed to determine if there might
still be an inner bar inside the nuclear ring.

3. 2002MNRAS.337..641W
Re:HIPASS J0323-36
J0323-36 The central (arrowed) emission in this spectrum is from NGC 1326.
Emissions from the nearby interacting galaxies J0325-36a (NGC 1326A, 1836
km s^-1^) and J0325-36b (NGC 1326B, 1006 km s^-1^) are also seen in this
spectrum but have been masked out in measurements.

4. 1998MNRAS.297..579C
Re:NGC 1326
NGC 1326. Storchi-Bergmann et al. (1996b) obtained narrow-band [O III] and
H{alpha} images, which reveal a circumnuclear ring at |r|~6 arcsec. As for
NGC 1097 and other galaxies containing star-forming rings, the Ws and colour
profiles of this galaxy (Fig. 35) confirm the presence of a ring. The radial
behaviour of the Ws and continuum ratios does not suggest the presence of an FC
in the nucleus. The Ws have values typical of an S3 template at the nucleus, S6
at the ring and S2-S3 farther out. The continuum ratios indicate an S1 template
at the nucleus (redder than the one indicated by the Ws), S6 at the ring, and
S3-S4 farther out.

5. 1996ApJS..105..353C
Re:NGC 1326
NGC 1326 (Fig. 2, middle).--The inner and outer rings in this object are
exceptionally clear examples. The object has only a weak bar, however. The
outer H{alpha} structure does not follow the outer ring. The H II regions near
and beyond the outer ring, which is type R_1_ in the notation of Buta & Crocker
(1991), begin nearly along the bar line and lead it slightly. The H{alpha}
spiral arms also end slightly ahead of the bar; they stay mostly outside the
R_1_ and go well beyond this feature. The appearance of the outer H{alpha} arms
is consistent with the R'_2_ morphology illustrated in Buta & Crocker (1991),
but only 180^deg^ of each arm is populated with clear H II regions. The
continuum image is dominated by the R_1_ component of an R_1_R'_2_ morphology.
A bright H II region is located at the southern dimple of the R_1_ component.
The galaxy is located in the Fornax Cluster, so the slight asymmetry of the
outer arms may be due to some weak interaction.
In the inner regions, the emission is very bright and mostly ringlike (see Fig.
12). Discrete H II regions line this nuclear ring, which is also detectable in
blue light (Buta & Crocker 1991). The ring is asymmetrically bright and may be
affected by extinction. A detailed multiwavelength study of this ring is given
by Garcia-Barreto et al. (1991). In the bar region, there is one bright H II
region at the south end. A few other very faint H II regions are scattered in
the inner lens region, and the inner ring is not prominent at all in H{alpha}.

6. 1996AJ....111.1566P
Re:NGC 1326
NGC 1326--This is a well-known "nuclear-ring" galaxy (Garcia-Barreto et at.
1991), and the circumnuclear starforming regions are clearly visible in our
image. The overall appearance is quite similar to that of M100 (Gallagher et
at. 1994; Freedman et at. 1994; see http://www.stsci.edu/pubinfo/ERO.html).
Spiral dust lanes in the inner regions are quite prominent, yet curiously are
seen across only one-half of the region interior to the circumnuclear ring.
The light distribution near the nucleus is asymmetric and fan-shaped, opening
toward the NW at around P.A. 330; the morphology is suggestive of light
scattered off the walls of a cavity or "bubble" of the kind found in
"superwind" galaxies (e.g. Heckman et at. 1990) such as NGC 3079 (ibid.) and
NGC 1808 (e.g., Phillips 1993a). The nucleus itself appears to be marginally
resolved.

7. 1994CAG1..B...0000S
Re:NGC 1326
FCC 29
RSBa
(E,L/I,1/8)
CD-719-S
Feb 1/2, 1979
103aO + Wr2c
45 min
NGC 1326 insert
CD-1667-S
Dec 31/Jan 1, 1980/1981
103aO
75 min
As in NGC 3081 on the preceding panel, the morphology of NGC 1326
is complex, having internal structures nested within structures near
the center. The morphology of the central region is so similar to that
in NGC 3081 that much of the latter's description applies here as
well.
A low-surface-brightness, ill-defined bar exists, containing the
central bulge. The position angle of the bar is 2 and 8 o'clock in the
insert print. The bar terminates on a very-high-surface brightness
broken ring that itself is the overlapping of two very tightly wound
spiral fragments, which start from the ends of the bar and overlap
after each unwinds by a half turn. Because of its high surface
brightness, as in NGC 3081, this broken ring would be the only feature
visible on incompletely exposed plates similar to the insert print.
Again, as in NGC 3081, a faint set of outer arms exist that start
tangent to the inner broken ring and form a spiral pattern that
overlaps to form an apparent outer ring, similar to the double-gamma
pattern of NGC 7702 (Sa; panel 66), NGC 6684 (SBa; panel 97), and IC
5240 (SBa; panel 99). As seen in the high-contrast negative print
here, this outer ring has yet a position angle for its major axis
different from the angles of the central bulge, the bar, and the inner
ring. The outer arms begin on the inner broken ring near where the bar
attaches to it (position angles 2 and 8 o'clock).
The prototype pattern of the outer arms is the morphology of NGC
210 (Hubble Atlas, p. 22; panel 124 here), mentioned before in the
descriptions of NGC 2962 (panel 93) and NGC 5377 (panel 96). The form
is described more completely in the Hubble Atlas, p. 22, where NGC
0023, NGC 1964, and NGC 0615 are also said to possess the pattern,
although seen at different inclination angles. Two sets of arms exist
- one tightly wound interior set and the outer, more-open outer
set. The combination produces the NGC 210 look. The outer pattern if
seen nearly face on would be similar to the outer arms of NGC 5701
(middle below) and others like it on this and the following panels
(NGC 1291, NGC 1358, NGC 1543, and NGC 5101).
In addition to the complex outer structure in NGC 1326, there is
internal structure, mentioned above, in the bulge as well. The bulge
is elongated (major axis at about 5 and 11 o'clock in the insert
print), with a suggestion of high-surface-brightness, smooth, massive
spiral stubs at about 12 and 6 o'clock. As in NGC 3081 (preceding
panel), a bright center exists in the bulge.

8. 1985SGC...C...0000C
Re:NGC 1326
Plate 1050r
Overexposed center, bright bar and (r): 1.1 x 0.8, lens 1.3 x 1.1,
(R): 2.5 x 1.6.
Plate 2770
Many extremely faint knots in arms.

9. 1982ESOU..C...0000L
Re:ESO 032201-3638.4
=ESO 357- G 26
in ESO 357- G 22 group

10. 1976RC2...C...0000d
Re:NGC 1326
In the Fornax I Cluster

11. 1964RC1...C...0000d
Re:NGC 1326
In the Fornax I Cluster.
Very bright nucleus.
Smooth narrow bar: 0.85 arcmin x 0.2 arcmin
Smooth (r): 1.0 arcmin x 0.85 arcmin
Very faint (R): 2.6 arcmin x 2.0 arcmin.


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