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Notes for object NGC 4568

15 note(s) found in NED.

1. 2008ApJ...679.1094T
Re:NGC 4568
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 4568
Here again, no clear signs of velocity disturbance are observed, except perhaps
in the external regions of the disc. Koopmann & Kenney (2004) claim that this
galaxy pair likely experiences RPS and a tidal interaction. It is however not
obvious that a tidal interaction is (or has) occurring (occurred) while
regarding the very mildly perturbed kinematics of the pair.

3. 2002ApJS..143...73E
Re:NGC 4568
NGC 4568.---Sbc: Interacting pair with NGC 4567. NGC 4568 is the
system to the SE. Small, moderately bright elliptical bulge, embedded
in an inner disk. Inner disk has structure, but no spiral arms. Arms
begin somewhat farther out and are narrow, well defined, and smooth.
There is a lot of interarm emission as well. There are fainter,
flocculent arm structures on the north side of the galaxy.

4. 2001A&A...379...54H
Re:KPG 347B
KPG347B. The galaxy is classified as SA(rs)bc. Our sharp/filtered and
(B-I) images show an inclined galaxy with a bright nucleus and knotty
features along multiple spiral arms. We classify this galaxy as Sc. The
estimated (B-V)_T_^0^ colour is representative of Sa types. The I/A class
for the pair is DI. Our EE class is 3.

5. 2000ApJ...542..761W
Re:NGC 4568
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.

6. 1996A&AS..115..439E
Re:NGC 4568
NGC 4568 is a Virgo cluster spiral galaxy in contact with NCC 4567.
High-resolution optical CCD spectra (Rubin et al. 1989) and VLA H I
observations (Guhathakurta et al. 1988) have revealed its optical and radio
rotation curves.

7. 1996A&AS..115..439E
Re:NGC 4568
NGC 4568 is a Sbc spiral which is in actual physical contact with its
neighbour NGC 4567, they are members of the Virgo cluster. Fabbiano et al.
(1992) have observed extended X-ray emission covering both galaxies and
NGC 4568 has a recent type Ib/c supernova (van Dyk 1992). Extended radio
emission has been observed by Condon (1987) at 1.49 GHz. Our CO data show
strong CO emission along the major axis and also along the minor axis away
from the companion. However, no CO is detected along the minor axis near the

8. 1995AJ....109.1608R
Re:NGC 4568
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.

9. 1994CAG1..B...0000S
Re:NGC 4568
VCC 1676
Karachentsev 347 [with NGC 4567]
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).

10. 1976RC2...C...0000d
Re:NGC 4568
= Holm 427a
In VV 219 = Kara[72] 347
Interacting pair with NGC 4567 at 1.2 arcmin

11. 1973UGC...C...0000N
Re:UGC 07776
VV 219a
SA(rs)bc (de Vaucouleurs), Sc- (Holmberg)
Paired with UGC 07777 at 1.4, 210, contact

12. 1964RC1...C...0000d
Re:NGC 4568
= Holm 427a
Very small, bright nucleus. Very many bright, knotty arms with dark lanes.
Pseudo (r): 0.8 arcmin x 0.3 arcmin.
Interacting pair with NGC 4567 at 1.2 arcmin.
Overlaps NGC 4567.
Misidentified as NGC 4567 in Uppsala 21.
Heidelberg Veroff. Vol. 9, 1926, Lund 6, Lund 10, 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.

13. 1959VV....C...0000V
Re:VV 219a
= NGC 4568
V = +2,413 km/sec.
V = +2,102 from H{alpha}, [NII]
(Page, T., Ap. J., 116, 63, 1952)
Yerkes Type: afS5

14. 1956AJ.....61...97H
Re:NGC 4568
HMS Note No. 144
Slit simultaneously on both nebulae: NGC 4567 and NGC 4568

15. 1918PLicO..13....9C
Re:NGC 4568
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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