Date and Time of the Query: 2019-05-25 T23:23:44 PDT
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Notes for object NGC 1316

26 note(s) found in NED.

1. 2007ApJ...668..130C
Re:NGC 1316
NGC 1316.-A Z ~ 0.01 is found from models, with age t > 8 Gyr. The inner annuli
seem to be populated by a rather old (t ~ 13) stellar system with respect to the
outer annuli (t ~ 8). Such radial change of the stellar age would be also
supported by the fact that this galaxy is a known merger remnant (Goudfrooij et
al. 2001).

2. 2006MNRAS.371.1912B
Re:NGC 1316
5.1.1 NGC 1316 (Fornax A) - For this well-known merger remnant, Fig. 2 reveals
generally good agreement with the published results, although the new data reach
to very much larger radii. The new data indicate a rather higher dispersion than
the points at the largest radii of the previous measurements, but since these
points were derived from the lowest S/N data in the older observations, the
conflict is probably not significant. The more extended velocity dispersion
profile from the new data for the first time reveals a seemingly distinct
feature of enhanced dispersion within the central 15 arcsec. In this galaxy, as
might be expected in a merger, random motions dominate out to large radii in the
new data, bringing into question whether this galaxy should really be classified
as a S0 system.

3. 2006AJ....131..114B
Re:MRC 0320-373
MRC B0320-373: Well-studied radio galaxy Fornax A,
identified with the nearby elliptical galaxy NGC 1316 ( Mills
1954). The optical position in Table 7 is that of the nucleus
(Schweizer 1981).

4. 2006A&A...447...97B
Re:NGC 1316
NGC 1316: Kim & Fabbiano (2003) detected a low luminosity X-ray AGN; the nuclear
spectrum is well reproduced by a power-law model {GAMMA} = 1.76 plus a MEKAL

5. 2005ApJS..157...59L
Re:NGC 1316
This peculiar S0 (lenticular) radio galaxy at a distance of 21.48 Mpc is a
member of the Fornax cluster and shows pronounced dusty patches/loops/shells
outside its D_25_ isophote, reminiscent of recent merger events and possibly
star-forming activities. ULX1 (IXO 11) and ULX2 (IXO 10) are within the
isophote. ULX2 is close to a faint point source with B2^7^ = 20.24 mag and R2^8^
= 19.90 mag. Assuming V ~ 20, the X-ray-to-optical ratio log(f_X_/F_v_) = log
f_X_(0.3-3.5 keV) + V/2.5 + 5.37 ~ -0.2, and indicates it might be a background
AGN (Stocke et al. 1991). However, due to the large uncertainties in the optical
magnitudes (up to 0.5 mag) and the X-ray spectral shape, this could be a red old
cluster with M_B2_ ~ -10 mag in NGC 1316, or a M dwarf in our Galaxy. Five ULXs
are on the dusty features outside the D_25_ isophote. ULX3 is IXO 12 in CP2002.
ULX4 is close to a faint point source with B2 = 20.25 mag and R2 = 19.52 mag.
ULX6 (IXO 13) is close to a faint point source with B2 = 21.56 mag and R2 =
19.93 mag. Multiple faint optical objects are found around ULX7.

6. 2005ApJ...635.1031B
Re:NGC 1316
NGC 1316.-This is also known as Fornax A, a radio galaxy in the Fornax Cluster,
and one of the optically most luminous galaxies in the cluster. It is also a
LINER with weak low-ionization emission lines, extended ionized and neutral
gas, and some evidence of dust. The system has a low Galactic extinction and
low Galactic H I column (1.9 x 10^20^ cm^-2^), so the absence of detectable
Galactic H_2_ is expected. The FUSE LiF1A spectrum (Fig. 2) shows emission from
the strong line of O VI ({lambda}1032). There is weaker emission from the O VI
({lambda}1038) line, also seen in the LiF2b channel. The sharp feature that is
coincident with Ly{beta} for NGC 1316 and the O VI ({lambda}1032) line from the
Milky Way is not confirmed in the LiF2b channel and may not be real (also, the
higher series Ly lines are not seen). In addition, there is emission from the C
III ({lambda}977) line at the redshift of NGC 1316 (SiC2a and SiC1a channels).
The two O VI lines and the C III line have the same FWHM of about 1.5 A (440
km s^-1^), which is comparable to the FWHM that one would infer from the
one-dimensional velocity dispersion of the stars in NGC 1316 (223 km s^-1^,
which would lead to a FWHM of 525 km s^-1^). The line ratio of the two O VI
lines is 2.7+/-1.0, consistent with the value of 2 expected for optically thin

7. 2005ApJ...622..235T
Re:NGC 1316
Evidence of recent merger in H{alpha}, dust; H_2_ detected in dust patches;
Fornax A (strong radio source); evidence of merger in Arp 15; 3 Gyr old merger
remnant; 0.5 Gyr old merger remnant.

8. 2005A&A...440...73C
Re:NGC 1316
NGC 1316: despite the presence of extended patches of dust, the brightness
profile is remarkably smooth and well fitted by a Nuker law.

9. 2004A&A...416...41X
Re:NGC 1316
NGC 1316. This is a giant elliptical galaxy in the Fornax cluster
showing evidence of recent merging events (e.g. dust patches, H{alpha}
filaments, ripples and loops; see, e.g. Schweizer 1980). Observations of
atomic and molecular gas indicate an absence of neutral atomic gas in
the galaxy (except for four bright HII regions) while there was a
significant amount of molecular gas (~5 x 10^8^M_{sun}_) which is mainly
associated with the dust patches which are oriented along the minor axis
(Horellou et al. 2001). ROSAT observations have shown that the X-ray
emission is extended and flattened along the major axis of the galaxy
which indicates the presence of a hot gas component (Kim et al. 1998).
The 15 micron emission is oriented along the minor axis of the galaxy
and traces the dust patches quite well in the outer parts (see Fig. 2).

10. 2003ApJ...598..827P
Re:NGC 1316
NGC 1316 (Fornax A).-The optical morphology of NGC 1316 displays
prominent dust lanes (see also Schweizer 1980). No measurable FUV-MUV
internal color dispersion is apparent, but it is not excluded because of
the low S/N of the UIT/FUV image. The essentially nonexistent {xi}(MUV, B)
value argues that the stars contributing to the MUV and optical light
are generally cospatial.

11. 2001ApJS..132..129M
Re:NGC 1316
NGC 1316 (Fornax A, Arp 154). - A member of the Fornax cluster, this
peculiar elliptical or S0 galaxy is at a distance of 19 Mpc. A system of
dust filaments cross the minor axis, and there are numerous indications for
the infall of material (Schweizer 1980). At MUV wavelengths, a central
source is observed embedded in diffuse light from the prominent galactic
bulge (Fig. 10a). The galaxy is only barely detected in the FUV. The
diffuse extension to the southwest on the MUV image is spurious, produced
by residual phosphorescence from a preceding exposure of the planet
Jupiter. This artifact has been masked out of our photometry.

12. 2000ApJS..131...95F
Re:VSOP J0322-3712
J0322-3712 (For A). - No detection: not surprising in view of the very
low flux density of the compact core of this source, less than 4 mJy, from
the observation by Morganti et al. (1997) using the 275 km
Parkes-Tidbinbilla interferometer at 2.3 GHz.

13. 1998AJ....116.2682C
Re:IRAS 03208-3723
NGC 1316, Fornax A, LINER spectrum.

14. 1998A&AS..130..267L
Re:NGC 1316
Schweizer (1981) studied the optical properties of the NGC 1316 core
obtaining an estimate of the central velocity dispersion of 248 +/- 6 km
s^-1^. Both this value and the average one in the literature (250 km
s ^-1^, PS96) are in agreement with our measure.

15. 1994CAG1..B...0000S
Re:NGC 1316
FCC 21
Sa pec (ripples)
Feb 1/2, 1979
103aO + Wr2
45 min
NGC 1316 is the radio source Fornax A,
located close to or associated with the Fornax
Cluster. The galaxy is outside the classification
sequence. The type assigned here is done simply
to force it into the classification by considering
some features and ignoring others.
The print shows only the region of
intermediate intensity. Neither the small nucleus
(Schweizer 1981) nor the outer envelope with its
loops and filaments (Schweizer 1980) is visible,
but both these are well seen in the reproductions
in Schweizer (1980, 1981).
NGC 1316 is neither an S0 nor an Sb. It is
classed here as Sa pec on the basis of (1) the large
bulge, (2) the dust patches that have spiral
segments, and (3) the loops in the outer filaments.
Schweizer calls the galaxy a cD but the outer
filaments belie this because of the peculiarities of
the outer plumes which may be tidal signatures of
a merger.
Schweizer's (1980, Fig. 1) deep print shows
the faint-surface-brightness outer structures that
led to the compromise type, Sa pec, given here.

16. 1994AJ....108.2128C
Re:PGC 012651
PGC 012651 = NGC 1316. Type = .LXS0P. Type is uncertain; this is
probably a merger remnant (1980ApJ...237..303S).

17. 1994A&AS..106..199C
Re:NGC 1316
NGC 1316. It is the well-known radio source Fornax A. It displays tails
and filaments in the outer parts, `ripples', dust and gas in the inner
parts. These characteristics, together with the velocity dispersion
significantly lower than that of galaxies of similar luminosity, and the
peculiar structure of the radio emission, suggest that NGC 1316 is a
merger remnant.

18. 1993MNRAS.263.1023M
0320-37 (For A). One of the closest and most famous sources in the
Southern Hemisphere. The radio image shows two 'flat', low-brightness
lobes and a weak core in the middle. These lobes are extremely
filamentary at high resolution. It is presumably an FR I, but not very

19. 1993MNRAS.263..999T
Re:PKS 0320-37
0320-37 (Fornax A). No emission lines are detected. The continuum
appears to be typical of early-type galaxies.

20. 1992ApJS...80..137J
Re:MRC 0320-373
Fornax A, a complex source with a
compact core component and very large diffuse lobes showing much structure.
It is an edge-brightened double although
not a powerful radio source.
The MOST image has a negative `bowl'
due to the lack of short-spacing data and has not been CLEANed. Fornax A
has been extensively studied so only a few references are given here.
Mapped by Cameron (1971), Gardner &
Whiteoak (1971) and Ekers et al. (1983).
S0 Galaxy, 9.5 m,
NGC 1316 at 03 20 47 -37 23 12 (Lauberts 1982) coincident with
the central peak of the radio source. z = 0.0061, Palumbo et al. (1983).
This is a well-known ID, one of the earliest
extragalactic radio sources identified (Mills 1954).

21. 1985SGC...C...0000C
Re:NGC 1316
Plate 1050r
Lens 7.2 x 6.4, dimensions include faint corona.
Plate 2698
Near plate edge.
Plate 2765
Overexposed center, dist lens and corona; incomplete (R'): 15' x -.
Interacting pair with NGC 1317 6.1 north.

22. 1982ESOU..C...0000L
Re:ESO 032047-3723.2
=ESO 357- G 22
absorption regions
largest in group

23. 1976RC2...C...0000d
Re:NGC 1316
= Arp 154
= Fornax A
In Fornax I Cluster? Possibly foreground.
NGC 1317 at 6.3 arcmin north-following.
Description and Classification:
Ap. J., 140, 35, 1964.
Ap. J., 139, 1378, 1964.
140, 44, 1964.
"Periodic Orbits, Stability and Resonances", 314, 1970.
J.R.A.S. Canada, 68, 117, 1974.
Atlas Gal. Australis, 1968.
Photometry (UBV):
A.J., 74, 335, 1969.
Ap. J., 178, 1, 1972.
Photometry:(I.R. 1-3.5 microns)
M.N.R.A.S., 164, 155, 1973.
Rotation Curve:
Nature, 207, 1282, 1965.
Radio Observations:
Ap. J., 140, 44, 1964.
Ann. Ap., 28, 75, 1965.
Ann. Ap., 31, 153, 1968.
Proc. A.S. Australia, 1, 229, 1969.
M.N.R.A.S., 152, 439, 1971.

24. 1964RC1...C...0000d
Re:NGC 1316
In the Fornax I Cluster.
Very bright, diffuse center with dark clouds,
Smooth nebulosity.
Non-interacting pair with NGC 1317 at 6.3 arcmin.
Observatory, 74, 248, 1954.
Revista Ast., XXIX, No.13, 1957.
Mem. R.A.S., 68, 69, 1961.
Radio Emission: (Fornax A)
Observatory, 73, 252, 1953.
Observatory, 74, 248, 1954.
Ap. J., 125, 1, 1957.
Ap. J., 133, 322, 1961.
Austral. J. Phys., 11, 400, 1958.
Austral. J. Phys., 11, 517, 1958.
P.A.S.P., 72, 368, 1960.
Caltech. Rad. Obs., 5, 1960.

25. 1964ApJ...140...35M
Re:Fornax A
No. 13.-For A classified from a slightly enlarged positive copy of 48-inch
Schmidt plate by E. Herzog. Absorption in nuclear region (Burbidge et at. 1963).
Member of the Fornax I cluster of galaxies (Zwicky 1959), richness 1.

26. 1961AJ.....66..562V
Re:NGC 1316
1316 Dark patches and bright knots. Similar to NGC 1275 and NGC S128?

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