Date and Time of the Query: 2019-05-25 T02:11:38 PDT
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Notes for object NGC 4589

14 note(s) found in NED.

1. 2008A&A...488..523H
Re:NGC 4589
NGC 4589. According to the ASC and NED this is an E2 galaxy. Our images do show
a surface brightness distribution resembling an elliptical galaxy. According to
Theureau et al. (2007) it is a strong 21 cm HI source. In a study of the gas and
stellar kinematics of this galaxy, Ravindranath et al. (2001) concluded that it
is a merger remnant (see also Moellenhoff & Bender 1989) with LINER-type nuclear
activity (Larkin et al. 1998). Studies by Michard & Marchal (1994), Carollo et
al. (1997) and Lauer et al. (2005) show the existence of large, chaotic, and
disorganized opaque dust patches (in and outside of 4" fields), forming
asymmetric patterns, which might indicate a disk. Summarizing above data we
conclude that this galaxy is a merger remnant with an outer structure similar to
an elliptical galaxy. The object is a source of 1.4 GHz continuum radio emission
(Condon et al. 1998). SN2005cz is a type Ib SN (Leonard 2005) 17" far from the
nucleus. The peculiarities in the central regions of this galaxy (and reaching
out to the location of the SN) are possibly associated with star formation
(e.g., Kauffmann et al. 2003).

2. 2004ApJ...607..810M
Re:NGC 4589
NGC 4589. There is a dwarf galaxy, [HS98] 162, about 5' to the northwest
(Fig. 7). It is a prime candidate for being a physical companion and for
a follow-up radial velocity measurement.

3. 2001AJ....122..653R
Re:NGC 4589
NGC 4589: The complex gas and stellar kinematics of NGC 4589 suggest
that it is a merger remnant (Mollenhoff & Bender 1989). The dust filaments
that traverse the center of the optical image (Tomita et al. 2000;
Quillen et al. 2000) are also visible in our NIR residual map. The light
distribution beyond ~5" deviates from the Nuker profile, and we confined
our fit to the region interior to this radius.

4. 2000A&AS..144...53K
Re:NGC 4589
We used photometry from Goudfrooij et al. (1994) and extrapolated the
profile towards the center; the fitted slope is -0.50.

5. 1998ApJS..114...59L
Re:NGC 4589
NGC 4589.--This is classified as a LINER based on only the [O II] to [O III]
ratio. This is the most featureless of the LINERs in the infrared, showing no
emission or absorption lines, except possibly weak Pa{beta} absorption.
Mollenhoff & Bender (1989) showed that NGC 4589 had a peculiar velocity field
with evidence for large streaming motions and a warped dust lane. They argued
that NGC 4589 was the result of a recent merger.

6. 1997ApJ...481..710C
Re:NGC 4589
Large-scale patchy and filamentary dust perturbs the appearance of the
galaxy all across the PC chip. The major dust lane runs almost north-
south (i.e., parallel to the minor axis) out to ~10" and spatially
coincides with the position angle at which Mollenhof & Bender (1989)
observed the highest gas rotation velocity (+/-200 km s^-1^; see also F95
and references therein). This lane passes close (~0.1") to the apparent
center, which is located in a local minimum of extinction. Around the
nucleus and to its west, a more irregular dust distribution is seen,
including a crosslike feature (~9" away). The large amount of dust
affects the morphological analysis, which shows a drop in ellipticity in
the range 0.1" - 4", and relatively large values for the higher
coefficients. All these features are much reduced in the fit to the dust-
improved I frame.

7. 1995A&A...297..643W
Re:NGC 4589
NGC 4589. This E2 galaxy is part of a small group. It has a dusty disk
which rotates around the major axis (Mollenhoff & Bender 1989). It is
reported to be an X-ray source (Roberts et al. 1991). We did not detect
any CO emission from this galaxy, with an inferred upper limit of
2 x 10^8^ M_sun_. Sofue & Wakamatsu (1993) have reported a marginal
detection with an inferred H_2_ mass of 7 x 10^7^ M_sun_, using the
Nobeyama 45-m telescope. However, Wang et al. (1992) used the same
telescope and got an upper limit with a similar noise rms. For the moment
we consider NGC 4589 as undetected.

8. 1994CAG1..B...0000S
Re:NGC 4589
April 2/3, 1940
60 min
A classical E2 morphology is evident from this Mount Wilson 60-inch plate.

9. 1994A&AS..105..481M
Re:NGC 4589
NGC 4589: The e_4_ coefficient is near zero except in a dust affected
region. There are however important asymmetric patterns in this galaxy,
which might indicate a disk.

10. 1994A&AS..105..341G
Re:NGC 4589
The B-I and H{alpha}+[NII] images reveal a prominent dust lane with
associated ionized gas extending ~20" along P.A. 173^deg^ which is close
to that of the minor axis (see also Mollenhoff & Bender 1989). The
ionized gas shows a LINER type spectrum. Detected by IRAS at 60 and 100
microns. This galaxy has been detected in the ^12^CO(J=1-0) line (Sofue &
Wakamatsu 1993). X-ray source with compact radio source.

11. 1994A&AS..104..179G
Re:NGC 4589
Residual images reveal prominent dust lane extending ~ 20" along P.A.
173^deg^ which is close to that of the minor axis. The Fourier terms in
the dust lane region are strongest in B as expected from dust
absorption. C4 ~ +0.01 at larger radii. Detected by IRAS at 60
& 100 microns. Radio and X-ray source.

12. 1976RC2...C...0000d
Re:NGC 4589
Non-interacting pair with NGC 4572 at 7.5 arcmin.
NGC 4648 at 22 arcmin.

13. 1973UGC...C...0000N
Re:UGC 07797
E2 (de Vaucouleurs)
See UGC 07775

14. 1964RC1...C...0000d
Re:NGC 4589
Bright diffuse nucleus. Smooth nebulosity.
Non-interacting pair with NGC 4572 at 7.5 arcmin.
NGC 4648 at 22 arcmin.
Heidelberg Veroff. Vol. 9, 1926 dimensions are for the bright part only.
Ap. J., 85, 325, 1937.

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