Date and Time of the Query: 2019-05-22 T14:48:54 PDT
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Notes for object NGC 3169

11 note(s) found in NED.

1. 2005ApJ...627..674A
Re:NGC 3169
NGC 3169.Falcke et al. (2000) found a peak flux density of 6.2 mJy beam^-1^ in
their 5.0 GHz VLBA observations from 1997 June 16, while Nagar et al. (2000)
found 6.8 mJy beam^-1^ in their 15 GHz VLA A-configuration image. Our VLBA
image had a peak of 8.6 mJy with a peak-to-rms-noise ratio of ~200, giving a 3
{sigma} upper limit to the size of the unresolved core of 0.65 mas. The
variability seen in our VLA observations has some features that correlate with
the phase calibrator behavior, and we classify this galaxy as possibly

2. 2002ApJS..143...73E
Re:NGC 3169
NGC 3169.---S0/a: Very bright, flattened nucleus, with evidence for a
weak bar, embedded in a luminous elliptical bulge. Outer bulge
isophotes appear slightly boxy. There is a LSB disk with patchy,
flocculent spiral features. No clear arm pattern. Although the disk is
not HSB, it is large---perhaps overfilling the field of view. The
optical types for this galaxy are SA(s)a pec (RC3), Sb(r)I--II tides
(CAG), and Sb (OSU B). The substantially earlier type in the near-IR
is due to the enhanced prominence of the bulge in the H band compared
to the optical and the lack of any visible spiral structure in the H

3. 2002ApJ...573..306E
Re:NGC 3169
NGC 3169
The first source in the list has a position that is coincident with the
central regions of NGC 3169. The emission is probably associated with
the center of the galaxy.

4. 2001A&A...368...16M
Re:NGC 3169
17. NGC 3169 is an Sb spiral of medium inclination, it forms a pair with
NGC 3166 at 7.7' angular distance. There exist signs of interaction (warps;
Sandage & Bedke 1994). The strong dust lane is still visible in the J
image, especially in the residuum (Fig. 4 in on-line version).

5. 2000ApJ...542..186N
Re:NGC 3169
NGC 3169.-Hummel et al. (1987) find a core flux density of 8.2 mJy in
the central 2" of their 1.2" resolution, 20 cm map and also extended
emission in P.A. 120^deg^, more or less along the minor axis of the host
galaxy. Combining their 20 cm peak flux density with our measured 2 cm
peak flux densities of 6.8 and 10 mJy beam^-1^ at resolutions of 0.15"
and 5", respectively, results in a nonsimultaneous spectral index,
{alpha}_2_^20^ between -0.1 and 0.1, for the radio emission within the
central 2".

6. 1997ApJS..108..155G
Re:NGC 3169
The continuum image shows many dust filaments following the spiral
pattern. We measure 67 H II regions in the disk, with some of them
arranged in a shell-like structure. The nucleus is extended 15" (1 kpc)
at P.A. = 95^deg^, almost perpendicular to the plane of the galaxy. To
the east the H{alpha} emission opens in a fanlike structure (see expanded
plot in Fig. 11b). The radio continuum map shows a jet structure extended
12" and aligned at P.A. = 115^deg^. This radio structure is cospatial
with the circumnuclear gas detected in this object. This alignment
between the ionized gas and the radio continuum emission has been
detected in other LINERs, e.g., M51 (Ford et al. 1985; Cecil 1988) and
NGC 2665 (Keel & Hummel 1988).

7. 1994CAG1..B...0000S
Re:NGC 3169
March 14/15, 1980
103aO + GG385
45 min
NGC 3169 forms a pair with NGC 3166 (Sa; panel 77), 7.7'
distant. The galaxies have closely similar redshifts, v_o(3166) = 1166
km/s and v_o(3169) = 1067 km/s. At the redshift distance of 22 Mpc (H
= 50) the projected linear separation is small, at 49 kpc.
The warped plane of NGC 3169 and the peculiar morphology of the
disk of NGC 3166 almost certainly verify that tides from a close
encounter have occurred, producing the warped plane evident here.
The dust lanes are multiple, seen well in silhouette against the
large central bulge. The spiral pattern is of the filamentary type.
HII regions are evident, particularly in the bright arm on the
near side. Very faint outer arms exist of such low surface brightness
that they are only hinted at in the print here. However, bright HII
regions exist in these outer arms, especially in the faint outer arm
on the near side where the largest resolves at a diameter of 4",
corresponding to a linear diameter of 425 pc, consistent with the
calibration of HII-region linear sizes as a function of galaxy
luminosity class (Sandage and Tammann 1974a).

8. 1976RC2...C...0000d
Re:NGC 3169
= Holm 173b
= Kara[72] 228b
In the NGC 3166 Group.
Interacting pair with NGC 3166 at 7.7 arcmin.
Rotation Curve and Systemic Velocity:
Astr. Ap., 8, 364, 1970.

9. 1973UGC...C...0000N
Re:UGC 05525
SA(s)a pec (de Vaucouleurs), Sa (Holmberg)
Extremely faint corona visible to approximately 8. x 6., disturbed on
following side
See UGC 05516

10. 1964RC1...C...0000d
Re:NGC 3169
= Holm 173b
Small, very bright nucleus in abright bulge, with a dark lane on one side.
Some distortion in outer partially caused by NGC 3166.
In the NGC 3166 Group.
Interacting pair with NGC 3166 at 7.7 arcmin.
Lund 6 dimensions for bright part only.
IAU Symp. 5, 1858 = Lick Cont.II, No.81, 1958.
Ap. J., 97, 117, 1943.

11. 1918PLicO..13....9C
Re:NGC 3169
Rather irregular, patchy spiral 4' x 1.7' in p.a. 55^deg^. "Nuclear portion oval
and quite bright. An absorption lane on the s.e. See Abs. Eff.

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