NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-06-18 T00:11:10 PDT
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Notes for object NGC 3489

12 note(s) found in NED.


1. 2006MNRAS.369..497K
Re:NGC 3489
This dusty galaxy shows a fast-rotating central component and a complex
morphology of the odd higher order kinematic moment h_3_ (see Paper III). The
H{beta} absorption strength is globally high (see also Kuntschner et al. 2001;
Rampazzo et al. 2005), with a sharp central (2 arcsec) enhancement, also evident
with OASIS (McDermid et al. 2004).

2. 2006MNRAS.366.1151S
Re:NGC 3489
Similarly to NGC 3156, this dusty galaxy also features a complex [O III]
distribution with filamentary structures and, despite this, a fairly regular
velocity field and very narrow lines. It also shows a more uniform distribution
for the H{alpha} emission, which explains the resemblance between the maps for
the [O III]/H{beta} ratio and the EW of the [O III]{lambda}5007 line.

3. 2005MNRAS.364..283E
Re:NGC 3489
NGC 3489. Bar measurements are from an unpublished William Herschel Telescope
(WHT)-Isaac Newton Group Red Imaging Device H-band image, due to strong dust
extinction in the optical.

4. 2004MNRAS.352..721E
Re:NGC 3489
NGC 3489: The photometry is perturbed by dust extinction. The effect is
not evident in the kinematic maps although it may explain the local
increase in the dispersion map at about 15 arcsec west from the centre
(Caon, Macchetto & Pastoriza 2000). Inside 4 arcsec, the opening angle
of the isovelocities decreases, indicating a fast rotating structure.
h_3_ decreases inwards, with a turnover at a radius of about 4 arcsec,
inside of which it shows a small increase.

5. 2002ApJS..142..223F
Re:NGC 3489
NGC 3489. NVSS did not detect this source. Other 1.4 GHz observations at
moderate resolution quote an upper limit of 10 mJy (Hummel & Kotanyi
1982; Fabbiano et al. 1987) to any radio emission; 5" resolution, 5 GHz
observations of Wrobel & Heeschen (1991) give an upper limit of 0.5
mJy.

6. 1999A&AS..136..269F
Re:NGC 3489
This is an S0/Sa type galaxy. It has a very complex absorption pattern
which has the form of patches (in the E side) and extended filamentary
structure (in the W side). The dust absorption is observed also in the
V image of the galaxy, producing box shaped isophotes in the central 20"
of the galaxy (see the V isophotes map in Fig. 5). The ionized gas
distribution in the form of filaments is rather regular in the inner
20", in which some patches of absorption can be seen.

7. 1995ApJS...98..477H
Re:NGC 3489
Multiple velocity components are responsible for the ``boxy'' structure
of the emission lines of NGC 3489.

8. 1994CAG1..B...0000S
Re:NGC 3489
S0_3_/Sa
(E,I,3/4)
H-1020-H
Jan 11/12, 1929
E40
60 min
NGC 3489 is similar to NGC 4429 at the
left but is of later type. (The dust in the disk is
more intricate and spreads over more of the
area.) Dust lanes, not visible in this print because
of the high intensity of the bulge, cut across the
bulge. From the structure of the lanes in
silhouette against the bulge, it is clear that the dust
is in the disk, not the bulge. The type is partly Sa
from (1) the absence of knots (HII regions), (2)
no sign of lumpiness in the disk due to star
associations, and (3) the large bulge. The absence
of a true spiral pattern and the prominent,
high-surface-brightness disk arc both characteristic
of S0 types.

9. 1976RC2...C...0000d
Re:NGC 3489
Leo I Cloud.
Photometry (5 Color):
A.J., 73, 313, 1968.

10. 1973UGC...C...0000N
Re:UGC 06082
SAB(rs)0+ (de Vaucouleurs)

11. 1964RC1...C...0000d
Re:NGC 3489
Very small, very bright nucleus in a bright inner lens: 0.37 arcmin x
0.17 arcmin. Pseudo (r) with a dark lane: 0.6 arcmin x 0.3 arcmin. Pseudo
(R): 1.4 arcmin x 0.45 arcmin.
Lund 9 and Heidelberg Veroff. Vol. 9, 1926 dimensions are for the bright
part only.
In the Leo Group.
Photograph:
Stockholm Ann., 14, No.3, 1942.

12. 1918PLicO..13....9C
Re:NGC 3489
2.5' x 1' in p.a. 70^deg^; very bright center with an almost stellar nucleus;
the whorls are rather indistinct; are most prominent at the ends of the minor
axis, and fade out at the ends of the major axis.


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