Date and Time of the Query: 2019-03-18 T16:29:55 PDT
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Notes for object NGC 1317

12 note(s) found in NED.

1. 2006AJ....132.2634L
Re:NGC 1317
NGC 1317 has been previously reported to be a double-barred galaxy, both in the
optical (Schweizer 1980; Wozniak et al. 1995) and in the near-infrared (Mulchaey
et al. 1997). The galaxy also has a nuclear ring, which is actually a double
ring/pseudoring evident particularly in blue light (Schweizer 1980; Papovich et
al. 2003) and in H{alpha} (Crocker et al. 1996). The galaxy is nearly in face-on
orientation. For the disk, RC3 gives a larger ellipticity than is found in this
study, most probably because the outer isophotes are elongated toward the nearby
companion. The secondary bar is clearly visible in our K_s_-band image, and the
double nuclear ring is now detected for the first time also in the
near-infrared. The outer structure is dominated by a large oval with no clear
sign of a primary bar. However, after subtracting the exponential disk a very
weak classical bar becomes visible (see Fig. 5). Previous evidence for the
primary bar comes from the {epsilon}-profiles, which are largely associated with
the large oval. The secondary bar lies within a bright nuclear lens (first
noticed by Schweizer 1980) and is completely detached from the nuclear
ring/pseudoring. Together, the secondary bar and its lens appear as a bump in
the radial surface brightness profile. In the decomposition only one primary
component was fitted. For the complex structure of this galaxy the decomposition
was made in small steps. The parameters for the disk and the main bar/oval were
found first, after which they were fixed. Then the secondary bar was found and
fixed, and finally the bulge component was found. In the central part of the
galaxy the secondary bar dominates the central oval, and therefore it is the
component that the fitting procedure found. In the final solution all components
(except the shape parameter of the bar) were left free for fitting. The solution
we find is reasonable, although it leaves some residuals, mainly because the
bars and ovals cannot be fitted separately. The double nuclear ring in the J -
K_s_ color map shows the presence of dust, which is consistent with the
observation that the ring is currently forming stars. The ring and the secondary
bar are also clearly visible in the K_s_-band image after subtracting the bulge
(Fig. 5). The ring has a patchy morphology, possibly indicating the presence of
red supergiants. Also, there are dust lanes in the central regions of the galaxy
that are not aligned with the secondary bar.

2. 2004A&A...415..941E
Re:NGC 1317
NGC 1317: Schweizer (1980). Outer-bar measurements are from the
publically available R-band image of Marcum et al. (2001); inner-bar
measurements are from the publically available K-band image of Mulchaey
et al. (1997), except that L_bar_ is from size of the inner H{alpha}
nuclear ring. The outer-disk inclination is from the axis ratio quoted
in Buta & Crocker (1993); the distance is a default value for the Fornax
Cluster, from the HST Key Project study of Freedman et al. (2001).

3. 2003ApJ...598..827P
Re:NGC 1317
NGC 1317 (Fornax B).-The optical morphology of NGC 1317 is dominated by
the bulge/disk system. The UV images indicate a prominent nuclear ring
of star formation (viith radius ~1 kpc), which is also observed in
H{alpha} (Marcum et al. 2001). This ring dominates the total UV emission
and drives the internal color dispersion and morphological K-correction
between the UV and optical images.

4. 2002ApJS..143...73E
Re:NGC 1317
NGC 1317.---SB0 (type example---see Fig. 3a): Nuclear point source
embedded in a nuclear bar. Inner isophotes of the bulge are elliptical
with the same major axis as the bar, but much less flat. At lower
intensity the bulge becomes circular. At lower intensity still, the
isophotes become elliptical again, but the major axis is roughly
perpendicular to the major axis of the nuclear region. This appears to
extend into a second, very faint, large-scale bar (again roughly
perpendicular to the inner bar). The disk is of quite low surface
brightness and has a faint inner ring at the radius where the outer
bar fades away.

5. 2001ApJS..132..129M
Re:NGC 1317
NGC 1317. - This early-type barred spiral (SAB(r)a) is located 6' north
of NGC 1316. The UV images (Fig. 11a) show a bright, broken, elliptical
ring of UV knots ~17" in diameter (~2.1 kpc at the adopted distance),
roughly coincident with the H{alpha} ring. The UV morphology is very
different from the optical continuum morphology, which shows only traces
of the knotty ring. These strong differences in morphology are found to be
most pronounced for early-type disk systems. NGC 4736, observed during
Astro-2, is another example of an early-type spiral, (SA(r)ab), with a
strong, UV-bright central ring. Lacking multiwavelength imagery, NGC 1317
might be erroneously classified as a "ring" galaxy based solely on the UV
morphology. Ring galaxies which have undergone a central penetrating
collision (Marcum, Appleton, & Higdon 1992) are extremely rare systems;
however, circumnuclear rings of massive star formation are much more common
(Crocker, Baugus, & Buta 1996).

6. 1997ApJS..110..299M
Re:NGC 1317
Double bar visible in the ellipse fits. While the inner bar is also
clearly seen in the image, the outer bar is much more difficult to
discern at the contrast level of Figure 1. Unbarred in the RSA, but
double bar seen in the optical images of Wozniak et al. (1995).

7. 1996ApJS..105..353C
Re:NGC 1317
NGC 1317 (Fig. 2, top).--This is a face-on peculiar spiral near Fornax A
(NGC 1316). H{alpha} emission is concentrated in a double nuclear
ring/pseudoring morphology which is best illustrated in the close-up in Figure
12. The inner nuclear ring is oval and is aligned nearly perpendicular to the
fat primary bar (see section 4.5). There is a bright nuclear bar inside this
ring; it is not visible in the continuum image in Figure 2, but it is well
illustrated by Schweizer (1980). The outer nuclear pseudoring is nearly
circular. There is bright central emission, and there is faint diffuse emission
inside the inner nuclear ring. Only a few much fainter H II regions are
detected outside the nuclear rings. These are near the boundary of the inner
lens recognized in the CSRG.

8. 1994CAG1..B...0000S
Re:NGC 1317
FCC 22
Feb 1/2, 1979
103aO + Wr2
45 min
NGC 1317 is a companion to NGC 1316 in
or near the Fornax Cluster. The inner spiral
pattern is formed by dust; the character of the
arms is closer to the MAS type than to a
two-armed symmetrical pattern of the grand design
type. Spiral patterns can be traced throughout
the faint outer envelope. There is a suggestion
that part of this outer spiral pattern, just visible
in this print when viewed from a distance, is due
to dust. The wide-field reproduction in Schweizer
(1980) shows the relation of this galaxy to NGC
1316 and to other members of the Fornax

9. 1985SGC...C...0000C
Re:NGC 1317
= NGC 1318
Plate 1050r
Overexposed center, star 0.9 north-preceding.
Plate 2765
Overexposed elongated nucleus, (r'): 1.6 x 1.6, dist (R'): 3.4: x 3.0:.
In corona of NGC 1316 and interacting pair at 6.1.

10. 1982ESOU..C...0000L
Re:ESO 032050-3716.8
=ESO 357- G 23
in ESO 357- G 22 group

11. 1976RC2...C...0000d
Re:NGC 1317
= NGC 1318
In the Fornax I Cluster.
Non-interacting pair with NGC 1316 at 6.3 arcmin south-preceding.
Atlas Gal. Australis, 1968.

12. 1964RC1...C...0000d
Re:NGC 1317
= NGC 1318
In the Fornax I Cluster.
Non-interacting pair with NGC 1316 at 6.3 arcmin.
Extremely bright nucleus
in pseudo (r): 0.45 arcmin x 0.35 arcmin,
Weak diffuse bar.
Very faint outer whorls form
a faint (R): 1.9 arcmin x 1.8 arcmin.
HA 88, 2 dimensions (series a)
(0.7 arcmin x 0.6 arcmin) rejected, nucleus only.

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