Date and Time of the Query: 2019-05-20 T10:32:50 PDT
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Notes for object NGC 0474

13 note(s) found in NED.

1. 2007ApJ...668..130C
Re:NGC 0474
NGC 474.-The single measurement available for this galaxy agrees with a Z ~
0.01, old (t >~ 14 Gyr) stellar population, for all models considered. Lower
ages and slightly higher metallicity have been found using high S/N spectral
analysis (Howell 2006), although the spectral data refer to a smaller, more
centrally concentrated area compared to our measurements.

2. 2006MNRAS.369..497K
Re:NGC 0474
This galaxy (Arp 227), famous for its shell structures (e.g. Turnbull, Bridges &
Carter 1999), shows normal metal line strength gradients. The H{beta} map
appears relatively flat in the inner regions, while we observe rising H{beta}
strength towards larger radii.

3. 2006MNRAS.366.1151S
Re:NGC 0474
This well-known shell galaxy (Turnbull, Bridges & Carter 1999) displays a
peculiar ionized-gas distribution and kinematics. The [O III] distribution
follows a twisted pattern, along which the [O III] lines are stronger at the
northern side of the galaxy between 5 and 7 arcsec, whereas they become stronger
at the southern end at larger radii. Although the H{alpha} lines are much
fainter than the [O III] lines, they seem to follow a similar spatial
distribution and indeed escape detection on the northern side beyond 7 arcsec.
The gas velocity field is characterized by a central component and an outer
component with almost opposite angular momenta. In both cases, the gas
kinematics is decoupled from the stellar kinematics. The widths of the lines
appear to peak in the transition region between the inner and outer gas velocity
components, which can be explained as a bias introduced by fitting a single
Gaussian to what, in fact, in some spectra looks like a superposition of two
separate components with diff erent velocities. The absence of strong absorption
features is surprising given the considerable amount of gas emission.

4. 2004MNRAS.352..721E
Re:NGC 0474
NGC 474: This galaxy (Arp 227), famous for its shell structures
(e.g. Turnbull, Bridges & Carter 1999), is a clear case of a
non-axisymmetric object, with a strong misalignment between the
kinematic and photometric major axes (Hau, Balcells & Carter 1996).

5. 2001AJ....122..653R
Re:NGC 0474
NGC 474: Although NGC 474 is known to be a shell galaxy with obvious
signatures of a merger remnant at large radii (Turnbull, Bridges, & Carter
1999), the inner regions appear undisturbed, showing no evidence for
significant structure or dust, in either the V or H bands. The low-level
features in the residual image are due to a slightly mismatched PSF for
the nucleus and deviations from the Nuker-law fit.

6. 1994CAG1..B...0000S
Re:NGC 0474
Pair [with NGC 470]
Sep 5/6, 1980
150 min
Racine wedge
NGC 474 (RS0/a) forms a close double with
NGC 470 (Sbc; panel 189), partially cut off at
the top middle of the print here. The projected
separation of the pair is 313". The redshifts are
v_o(470) = 2643 km/s, and v_o(474) = 2548 km/s.
The mean of = 2596 km/s gives a
redshift distance of 52 Mpc (H = 50) and therefore
a projected linear separation of 80 kpc for
the pair.
The multiple rims at many distances from
the center of NGC 474 are similar to the
theoretical expectations of the effect of mergers
calculated by Quinn (1984; see also the diagram
due to Toomre in Schweizer 1983). However, the
circumstantial evidence is not that a merger has
occurred but rather that a close encounter is
taking place with NGC 470.
Short-exposure plates taken with the Mount
Wilson 100-inch by van Maanen in 1938 and by
Sandage in 1975 fail to show evidence for a
merged companion. However, the absence of a
double nucleus may not be of consequence; it is
claimed that direct evidence of a merger would
rapidly disappear (Toomre 1977 in the discussion).
The common feature in NGC 474 and NGC
7585, above, is the exceptionally high surface
brightness of the central, almost point-like,
nucleus. This feature is seen on the low-contrast
prints of both galaxies in the secondary images of
the nuclei from the Racine wedge.
The print has been made from the same
original plate used for the image on the left.

7. 1994CAG1..B...0000S
Re:NGC 0474
Pair [with NGC 470]
Sep 5/6, 1980
150 min
Racine wedge
The print has been made from the same
original plate used for the image on the left.
The sharp rimmed arcs continue farther
into the center than is visible on the more heavily
exposed print at the left. The well-defined,
closely circular central bulge appears featureless
on short-exposure Mount Wilson 100-inch
plates, but it is of exceptionally high surface
brightness. At the center is an almost unresolved,
very bright nucleus. As in NGC 7585, above, its
secondary image from the Racine wedge is visible
to the right of the bulge, slightly below the
centerline at what appears to be the edge of the
central region. To locate this secondary image
note the relative position of the many other
Racine wedge images for the bright stars in the field.

8. 1994AJ....108.2128C
Re:PGC 004801
PGC 004801 = NGC 474. Type = .LAS0..

9. 1976RC2...C...0000d
Re:NGC 0474
= Arp 227
Non-interacting pair with NGC 0470 at 5.5 arcmin
In a group with NGC 0467 and NGC 0470.

10. 1973UGC...C...0000N
Re:UGC 00864
Arp 227
E-type main body with extensive extremely faint corona, hints of several
concentric rings or arcs, strongest straight opposite UGC 00858,
`Very faint rings extend to diameter of 7.4' (Arp)
SA(s)0 (de Vaucouleurs)
See UGC 00848, UGC 00858

11. 1964RC1...C...0000d
Re:NGC 0474
Member of the NGC 0467-0470-0474 Group.
Non-interacting pair with NGC 0470 at 5.5 arcmin.
Small, very bright, diffuse nucleus
in a bright diffuse lens.
Very faint smooth arcs or whorls in envelope.
Lick 13 dimensions rejected; nucleus only.
Ap. J., 135, 2, 1962.
Radio Source: (possible identification)
Austral. J. Phys., 11, 360, 1958.

12. 1961AJ.....66..562V
Re:NGC 0474
Fuzzy nucleus surrounded by segments of nebulous ring. Interacting with
NGC 0470

13. 1918PLicO..13....9C
Re:NGC 0474
Round; 0.5' in diameter. Center very bright, with much fainter matter outside.
No spiral structure discernible. 28 s.n.

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