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Date and Time of the Query: 2018-11-15 T03:00:47 PST
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Notes for object NGC 7727

7 note(s) found in NED.


1. 2002ApJS..143...73E
Re:NGC 7727
NGC 7727.---S pec (early): Elliptical nuclear source embedded in a
boxy (rhomboid) bulge. Bulge is very large. Four faint, broad,
irregular arms emerge from the bulge. These arms have differing pitch
angles and extents. Some can be followed through more than 90deg of
winding. Some stop very quickly. Several large-scale LSB features are
visible. Merger remnant?

2. 1994CAG1..B...0000S
Re:NGC 7727
Sa pec
(VE,L,1/2)
PH-7692-S
Sep 26/27, 1979
IIIaJ
75 min
Racine wedge
The two prints of NGC 7727 here were
made from the same original plate but with
different contrast control in the darkroom. The
properties of such prints for assessing
absolute-surface-brightness levels are discussed on
the preceding page.
NGC 7727 has similar features in its inner
and outer plumes to galaxies such as NGC 7252
(panel 340), which are said to be results of
recent mergers (Toomre 1977; Schweizer 1977,
1982, 1983), although NGC 7727 was not
included in the list of 11 thought by Toomre to
define the class. Other members of the class in
this atlas are NGC 520 (panel 340), NGC 3256
(panel 147), NGC 4038/4039 (panel 280), and
NGC 7252 (panel 340).
The plumes in NGC 7727 in the left panel
are similar to those in NGC 7252 (Schweizer
1982).
Note that the plate was made with a Racine
wedge that produced secondary images to the
bright stars separated from the primary by 18"
in the south-southeast direction (toward the left
and slightly up on the print here). The magnitude
difference between the primary and secondary
images is 5.0 mag.

3. 1994CAG1..B...0000S
Re:NGC 7727
Sa pec
(VE,L,1/2)
PH-7692-S
Sep 26/27, 1979
IIIaJ
75 min
Racine wedge
The pattern of plumes and near edges to
plumes (Quinn 1984) continues into the center of
NGC 7727.
The merger hypothesis for NGC 7727 is
strengthened by the presence of two nuclei near
the center of the image seen on short-exposure
Mount Wilson 100-inch plates taken by Duncan
in 1925 and 1938 and by Hubble in 1946. One
of these nuclei is at the center of the bulge plus
inner disk of the parent galaxy. The other
unresolved bright nucleus is well separated from the
primary nucleus by 3". However, at 0.8" resolution
for the seeing disk, it is not possible to decide
if the secondary nucleus is a superposed star or
is the nucleus of a proposed, nearly merged
previous companion.

4. 1976RC2...C...0000d
Re:NGC 7727
= Arp 222
= VV 067
Very faint smooth outer arms.
Non-interacting pair with NGC 7724, SB(s)ab, at 12 arcmin

5. 1968MCG4..C...0000V
Re:MCG -02-60-008
Inside L (or N_n_) is some kind of structure
but the trail of SAB not visible.
Possibly, these are overlapping galaxies.
Photo: Arp 222.
Its photograph as VV 067 is classified as possibly interacting.
Type:
Sand - Sa
vdB - Snn(t?)
Morg - Sp
deV - SAB(s)ap
Redshift = +1,943 km/sec
G8e
Cp' = 0.85.

6. 1964RC1...C...0000d
Re:NGC 7727
Very small, bright, diffuse nucleus in a smooth inner lens: 0.3 arcmin x
0.1 arcmin. There is a star or bright knot superimposed. Very faint, smooth
whorls or arms.
Non-interacting pair with NGC 7724, an SB(s)ab at 12 arcmin.
Heidelberg Veroff. Vol. 9, 1926 dimensions are for the bright part only.

7. 1959VV....C...0000V
Re:VV 067
= NGC 7727
G8
V = +1,943 km/sec Mount Wilson,
V = +1,982 km/sec Lick Obs.
Similar to VV 073?


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