Date and Time of the Query: 2019-04-19 T01:55:14 PDT
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Notes for object NGC 1079

9 note(s) found in NED.

1. 2006AJ....132.2634L
Re:NGC 1079
NGC 1079: The morphology of NGC 1079 has been previously studied by Buta (1995),
Jungwiert et al. (1997), and SGA04, who also made a 2D decomposition for it, and
Knapen et al. (2006), who found a strong nuclear peak in H{alpha} surrounded by
rather faint circumnuclear patchy emission. Buta (1995) recognized NGC 1079 as a
galaxy showing one of the largest examples of a feature called R_1_R^'^_2_, a
double outer ring/pseudoring morphology linked to an outer Lindblad resonance
(Buta & Crocker 1991). This feature includes a well-defined outer ring from
which two conspicuous spiral arms emerge. Sandage & Brucato (1979) also
recognized NGC 1079 as an early-type spiral. The bar in NGC 1079 was recognized
by Jungwiert et al. as a large peak at r = 30" in the ellipticity profile, while
a smaller peak at r = 17" was attributed to a triaxial bulge. We see both peaks
in our {epsilon}-profile as well. The axis ratio of the disk (q = 0.59) deviates
from the axis ratio of the bulge (q = 0.68), confirming that they are separate
components. In our decomposition we first determined h_r_, which was then kept
fixed. Finally, the bulge, disk, and bar were fitted, but for the ansae-type
morphology of the bar the solution depends slightly on the parameters of the
bar: it is possible to use n > 2 or n = 2 together with a shape parameter that
deviates from purely elliptical isophotes. Depending on this choice, we found
B/T = 0.20-0.25. Our solution converges only if flattening of the bulge is taken
into account. The bar has a high surface brightness compared to that of the
underlying disk. Apparently, an inner ring surrounds the bar, seen as a residual
after subtracting the model image from the observed image.

2. 2006AJ....132.2634L
Re:NGC 1079
Our solution for this galaxy is very different from the 2D bulge/disk solution
obtained by SGA04. They found a large de Vaucouleurs-type bulge (B/T = 0.65, n =
3.82) dominating the whole surface brightness profile and a very weak
exponential inner disk extending to the radius of the bar. In their fit the disk
at the edge of the bar is about 5 mag weaker than the bulge. SGA04 made the
decomposition in the R band, which extends approximately to the same radial
distance as our Ks-band image. For comparison, we also made a 2D bulge-disk
decomposition (thus omitting the bar), which gives B/T = 0.57 (see Fig. 6, top
right). This is near the B/T ratio obtained by SGA04, except that the bulge is
more exponential (n = 2.7). However, we stress that in this solution the flux of
the bar goes erroneously to the bulge. A similar solution was found by us using
the 1D method. This resembles the solution by SGA04 even more, although the disk
we find is still several magnitudes brighter than that obtained by SGA04. It is
also possible to find a solution in which the surface brightness profile is
fitted by a single Sersic function with n = 3.3 (Fig. 6, top middle), but in
that case the fit is not good, and, in particular, the model image is very
different from the original image.

3. 2004A&A...415..941E
Re:NGC 1079
NGC 1079: Listed by Moiseev (2001), on the basis of an ellipse-fit feature in
Jungwiert et al. (1997). However, the ellipticity peak is very weak, and
Jungwiert et al. preferred to attribute it to "bulge triaxiality".

4. 1997A&AS..125..479J
Re:NGC 1079
NGC 1079 (RSAB0/a, 1"~82 pc, I=57.1^deg^)
The highest peak in ellipticity (e_max_=0.51 at a~32") is related to the
large-scale bar, however the shape of the profile can be deformed by the
presence of spiral arms at the end of the bar. There is a secondary maximum
(e_max_=0.32^s^ at a=17") that we attribute to the triaxiality of the bulge.

5. 1994CAG1..B...0000S
Re:NGC 1079
Sep 27/28, 1978
103aO + GG385
45 min
This and the print below show the outer and
the inner structures of NGC 1079 which have
high symmetry in the spiral patterns. There are
two principal outer arms that are tightly wound.
Each contains many knots, presumably small HII
regions, all unresolved at 1" resolution.
The outer arms have very low surface
brightness. As usual, the place where these arms
connect to the rim of the bulge cannot be traced
with certainty at the intensity level reached by
the plates. The intensity of the arms always drops
in the vicinity of the connections near the bulge.
The inner arms can be traced on this print into
the vicinity of the bulge at about 12 o'clock and
6 o'clock. The arms can then be traced outward
over an arc of about 270 deg, an unusually large
wrap except in a few of the most regular galaxies
such as NGC 7096 on the next panel.
The outer arm on the left side (at about 9
o'clock) is bifurcated. There is a suggestion that
the opposite arm is thickened at a position angle
of about 3 o'clock, again showing the high
symmetry of the image. This symmetry suggests a
grand design type.
The galaxy is isolated. The nearest bright
galaxy is NGC 1097 (RSBbc; panel 201 here;
Hubble Atlas, p. 46) separated by 1 deg 20'
southeast and at a much different redshift. There
are no obvious companions to NGC 1079. The
grand design features in NGC 1079 are not,
then, due to perturbative interaction.

6. 1994CAG1..B...0000S
Re:NGC 1079
Sep 27/28, 1978
103aO + GG385
45 min
The print of NGC 1079 here is from the
same plate as above, printed to show the
high-surface-brightness, smooth inner arms. These
attach to the bulge at about the same position angle
as the faint outer arms. A thin dust lane exists on
the inside of the bottom inner arm.
At least four arms exist in this galaxy - two
inner and two outer. The pattern is neither
filamentary nor simply two-armed of the usual
grand design type.

7. 1985SGC...C...0000C
Re:NGC 1079
Plate 1044
Very bright center, broken (r): 1.3 x 0.7, very faint outer arms. (R): 3.5 x 1.9

8. 1982ESOU..C...0000L
Re:ESO 024135-2912.9
=ESO 416- G 13
very faint outer arms

9. 1964RC1...C...0000d
Re:NGC 1079
Small, very bright nucleus.
Weak bar: 0.9 x 0.4 arcmin
Pseudo (r): 1.3 arcmin x 0.65 arcmin.
Outer arms form a very faint double (R): 4.3 arcmin x 2.7 arcmin.

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