Date and Time of the Query: 2019-03-24 T17:14:59 PDT
Help | Comment | NED Home

Notes for object NGC 4274

10 note(s) found in NED.

1. 2012ApJ...754...67F
Re:NGC 4274
NGC 4274 RSBR2..-Double barred galaxy (Shaw et al. 1995; Erwin 2004). It is
classified as pseudobulge with a Sersic index of 1.60 +/- 0.35 by (Fisher &
Drory 2010). The bulge hosts a prominent nuclear spiral including strong dust
lanes and a nuclear ring. The ring is seen as a fast-rotating, low-dispersion
component in SAURON velocity and dispersion maps (Falcon-Barroso et al. 2006).
It also appears in their ionized gas maps through increased H{beta} emission and
lowered [O III]/H{beta} ratios which indicates star formation. The major axis
rotational velocity rises quickly with increasing radius and starts flattening
out at about 4", well within the bulge radius of 11.3". The velocity dispersion
profile shows a strong depression inside the bulge with values of about 100 km
s^-1^. Outside the bulge the dispersion rises to values exceeding 130 km s^-1^.
The h_3_ moments are well anti-correlated with velocity in the radial range that
is covered by our data. They reach values of up to +/-0.14 at about the same ra
dius where the rotational velocity starts to flatten out. This is accompanied by
peaks in the h_4_ moments with values of up to 0.14.

2. 2006MNRAS.369..529F
Re:NGC 4274
NGC 4274 is a double barred galaxy (Shaw et al. 1995; Erwin 2004) with
significant amounts of dust in the inner parts. Despite the dust, the stellar
kinematic maps show regular rotation on the main disc component of the galaxy,
and also the presence of an inner fast-rotating ring (detected in the V and
{sigma} maps). As in NGC 4245, the signatures of the star-forming ring are
easily identifiable in the ionized-gas maps. An H{alpha} image is presented in
Hameed & Devereux (2005).

3. 2004A&A...415..941E
Re:NGC 4274
NGC 4274: Suggested as double-barred by Shaw et al. (1995). Their near-IR image
strongly suggests an inner bar, almost perpendicular to the outer bar, but no
measurements are available. Unfortunately, the available WFPC2 images (F555W)
show that the central region is extremely dusty, so near-IR images are required
for measurement of the inner bar.

4. 1994CAG1..B...0000S
Re:NGC 4274
Hubble Atlas, p. 12
Feb 9/10, 1954
103aO + WG2
30 min
From poor plate material, NGC 4274 would
probably be described as having an external ring.
However, the pattern is similar to that described
for NGC 7702 in the print on the left. The ring
is broken. As in NGC 7702, it is composed of two
spiral arms that nearly overlap. The aspect of the
line of sight relative to the position angle of one
of the arms as it emerges from the inner disk at
the edge of the bulge allows the arm overlap to be
seen on the near side of the image at the bottom
on this print. The overlap of the two arms on the
far side is much less visible because of the
overriding luminosity of the bulge and the smaller
effect of the dust lanes in separating the arms in
the visual impression. (Dust lanes are always
more visible on the near side.) The silhouette of
the inner dust lanes on the near side against the
bulge is striking here.
The bright luminous inner arms with their
associated dust are well seen here. The arms
begin near the edge of the bulge; the spiral
subtype is (s) (see discussion under NGC 7742 on
this page). A set of fainter outer arms exist,
continuing outward from the rim of the broken
near-ring; the subtype of this feature is (r). These
faint outer arms are well shown in the negative
print on the Sa summary page, panel 88.
The galaxy has features both of the multiple-armed
spiral (MAS) and the grand design (GD)
type if only the two high-surface-brightness inner
near-ring arms are considered. These arms are
lumpy. NGC 4274 is later along the Sa sequence
than NGC 7702 at the left, although the basic
patterns are similar.
The positive print and the description in the
Hubble Atlas (p. 12) show the features described
here but with a different contrast.

5. 1994CAG1..B...0000S
Re:NGC 4274
Hubble Atlas, p. 12
Feb 9/10, 1954
103aO + WG2
30 min
NGC 4274 is of the same grand design type
as NGC 3358, above, but is later along the Sa
sequence because of the higher recent star-formation
rate evidenced by the more abundant HII
regions in the arms. The internal near-ring
impression due to the tightly wound spiral structure
is well seen here because of the large inclination

6. 1993A&AS...97..887B
Re:NGC 4274
NGC 4274 is a gas-poor Sa galaxy. PR obtained a CO(1-0) spectrum showing
emission from 750 to 1100 km/s, like the weak HI spectra. We detected
only the stronger redshifted side of PR's KP spectrum. The difference
could be due either to a difference in pointing centers or to an
asymmetric molecular gas distribution.

7. 1973UGC...C...0000N
Re:UGC 07377
(R)SB(r)ab (de Vaucouleurs), Sa (Holmberg)
Companions 2.5, 214, 0.4 x 0.3; and 3.2, 331, 0.5: x 0.4:, diffuse, dwarf

8. 1964RC1...C...0000d
Re:NGC 4274
Very bright nucleus in small bar seen almost end-on, with dark lanes.
Bright (r): 2.7 arcmin x 1.0 arcmin in a lens: 3.2 arcmin x 1.2 arcmin.
Faint outer arms form a pseudo (R): 5.8 arcmin x 1.55 arcmin.
Lick 13 and Uppsala 21 dimensions are for the bright part (lens) only.

9. 1961Hubbl.B...0000S
Re:NGC 4274
Feb. 9/10, 1954
103aO + WG2
30 min
Enlarged 3.5X
NGC 4274 is the type example of a special subgroup of
Sa within the NGC 4866 major group. On short-exposure
photographs, all galaxies of this subgroup appear to have
a complete narrow ring, separated from the nucleus, and
superposed on the faint background light of the lens.
Large-scale photographs, however, show that the ring is
not complete but is broken at diametrically opposite places,
the pieces having drifted outward to form a spiral pattern.
This feature is particularly well shown in NGC 4274.
The two bright spiral arms that make up the broken ring
are easily visible. Notice how the two arms almost touch
when the one sweeps through 180 degrees and passes near the
arm closer to the nucleus.
Two fainter arms are present in NGC 4274, winding
outward through an extended envelope on the outside of
the bright arms that form the "broken ring."

10. 1918PLicO..13....9C
Re:NGC 4274
The main whorl of this spiral forms an elliptical ring 3.5' x 1' in p.a.
951^deg^; exceedingly faint matter outside brings the total length to nearly 8'.
Bright, rather irregular matter in the vicinity of the nucleus, which is
elongated and shows well in a 5m exposure. See Abs. Eff. 17 s.n.

Back to NED Home