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Notes for object NGC 4567

12 note(s) found in NED.

1. 2008ApJ...679.1094T
Re:NGC 4567
Both NGC 4567 and NGC 4568 are Sbc galaxies that form an optically overlapping
pair with comparable optical redshifts. In this way, NGC 4567/NGC 4568 resemble
UGC 3995/UGC 3995A in the active galaxy sample. Both NGC 4567 and NGC 4568 are
included in our control sample. There are no other cataloged galaxies at a
comparable optical redshift within 15^'^ of the galaxy. Despite their apparent
proximity and similar redshifts, as in the case of UGC 3995/UGC 3995A we detect
noH I disturbances at a spatial resolution of ~20 kpc, nor at a spatial
resolution of ~10 kpc (Fig. 20), in either NGC 4567 or NGC 4568. Indeed, in a
much deeperH I observation at an angular resolution of ~20^'^, Iono et al.
(2005) detected no extended tidal features in this pair of galaxies.

2. 2006MNRAS.366..812C
Re:NGC 4567
This galaxy is part of a pair with NGC 4568. The morphology and the velocity
field do not show signs of disturbance.

3. 2001A&A...379...54H
Re:KPG 347A
KPG347A. The components in this pair show an apparent overlapping but
similar morphological types. The galaxy is classified as SA(rs)bc. Our
sharp/filtered and (B-I) images show a prominent bulge region and wrapped
spiral arms that resemble an inner ring. Blue knotty features are seen
along the arms. We classify this galaxy as SA(r)bc. The (B-V)_T_^0^ colour
is representative of Sa types. Our EE class is 12.

4. 2000ApJ...542..761W
Re:NGC 4567
The Sbc pair NGC 4567/8 (UGC 7777/6) is another case in which the
analysis is limited by the general lack of symmetry (see Figs. 5a and 5b
for B and B-I images). Here we concentrate on the dark lane in the upper
left of Figure 5a that cuts across a brighter background galaxy arm. The
comparison region for the foreground arm is taken from a region along
the arm but beyond the projected bulk of the background galaxy (farther
to the upper left in Fig. 5a); the comparison region for the background
arm is along the background arm, just away from where it is blocked by
the foreground galaxy. The foreground galaxy (NGC 4568/UGC 7776) has an
axial ratio of 2.29, implying an inclination of 64^deg^. The assessed
region in the foreground galaxy samples, in projection, a range of radii
spanning 0.5-0.85 R_25_^B^. We calculate face-on extinctions of
A_B_ ~ 1.2 and A_I_ = 0.69 for this region (see Table 3).
The interpretation of the light seen beyond the strong dust lane in
NGC 4568 (to the lower left of the region analyzed above) as coming from
the background galaxy rather than the foreground structure hinges on
whether any similarly bright areas are found at comparable projected
radius in NGC 4568 and on the rather symmetric shape of NGC 4567 as seen
in the less obscured I band. Inspection of archival Hubble Space
Telescope (HST) "snapshot" images obtained in the F606W filter (WFPC2
data sets U29R4H01/2; PI G. Illingworth) shows that most of the excess
light in this area comes from distinct bright clusters and associations,
brighter than any others seen in the foreground object at comparable
radius but quite comparable to the (systematically brighter)
star-forming regions in the background system (see Fig. 5c). This
somewhat strengthens our interpretation of the excess light as indeed
shining through a more transparent interarm medium.
The WFPC2 data also show that the darkest absorbing clouds in this
pair, with a measured extinction of A_606_ ~ 1.5, are two irregular
resolved features about 7" (0.5 kpc) in extent but narrow
enough (<1") that they are not prominent in our ground-based
images. Both are located well beyond the spiral arms (and other dust
features) in NGC 4568 (as marked in Fig. 5c). Their low residual
intensity requires that they be in the foreground, not part of NGC 4567
in the background. Either they are isolated in the outer disk or are
located several kiloparsecs from the disk plane (either of which might
be attributed to the effects of interactions between these two
galaxies). We cannot immediately exclude the possibility that they are
in the extreme foreground of the Milky Way itself, though the surface
density of such clouds could not be very large without violating
constraints from the number not seen in HST imagery of elliptical
galaxies and the intensity of high-latitude IR cirrus emission.

5. 1995AJ....109.1608R
Re:NGC 4567
NGC 4567 and NGC 4568
The principal question here is whether or not these galaxies are
interacting. There are numerous H{alpha} regions spread out across the
surfaces of both NGC 4567 and NGC 4568. However, the general lack of
tidal tails, x-ray emission, or discernible tidal signatures in the
nuclear regions all argue that the galaxies are not interacting.

6. 1994CAG1..B...0000S
Re:NGC 4567
VCC 1673
Karachentsev 347 [with NGC 4568]
Feb2/3, 1979
VV 219
103aO + Wr2c
45 min
The redshifts of the components of this pair
are v_o(4567) = 2136 km/s and v_o(4568) = 2199 km/s.
The separation of centers is 1.3'. If the
pair is in the Virgo Cluster at a distance of
21.9 Mpc, the projected linear separation is
small at 8 kpc.
A most interesting aspect of the combined
morphology is the lack of evidence for tidal
distortion in either member of the pair. Each galaxy
has the morphology of a normal Sc galaxy of
intermediate luminosity class. Each has a small
nucleus and well-developed multiple spiral arm
fragments of the NGC 488 type. Either the
separation is large in the line of sight or the
orbital circumstances of the encounter are
unfavorable for tidal plumes (orbital angular
momentum could be opposite to the direction of
the individual spin angular momenta).

7. 1976RC2...C...0000d
Re:NGC 4567
= Holm 427b
In VV 219 = Kara[72] 347.
Interacting pair with NGC 4568 at 1.2 arcmin.
Radio Observations:
Australian J. Phys., 21, 193, 1968.

8. 1973UGC...C...0000N
Re:UGC 07777
VV 219b
SA(rs)bc (de Vaucouleurs), Sc- (Holmberg)
See UGC 07776

9. 1964RC1...C...0000d
Re:NGC 4567
= Holm 427b
Very bright, diffuse nucleus? Pseudo (r): 0.55 arcmin x 0.4 arcmin. Many
bright knotty, branching arms in a lens. Smooth faint (R).
Interacting(?) pair with NGC 4568 at 1.2 arcmin.
Misidentified as NGC 4568 in Uppsala 21.
Lund 9 and Uppsala 21 dimensions are for the bright part only.
Handbuch der Ap., 5, 2, 1933.
Handbuch der Ap., 5, 843, 1933.
Ap. J., 116, 66, 1952.
I.A.U. Symp., No. 5, 1958 = Lick Contr. II, 81, 1958.
Medd. Lund II, 128, 1950.

10. 1959VV....C...0000V
Re:VV 219b
NGC 4567
V = +2,284 km/sec
V = +2,158 from H{alpha}, [NII]
(Page, T., Ap. J., 116, 63, 1952)
Yerkes Type: fS4

11. 1956AJ.....61...97H
Re:NGC 4567
HMS Note No. 144
Slit simultaneously on both nebulae: NGC 4567 and NGC 4568

12. 1918PLicO..13....9C
Re:NGC 4567
NGC 4567 and NGC 4568
Two rather faint spirals so close together that they overlap slightly. The
centers are 1.2' apart in p.a. 165^deg^. The northern nebula is 2' x 1'; the
southern 3' x 1'. The northern nebula has a very bright, almost stellar nucleus;
that of the southern nebula is double. Both are rather open spirals with many
almost stellar condensations .. There is apparently a. slight amount of
occulting effect, due to overlapping. See Abs. Eff. 42 s.n.

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