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Date and Time of the Query: 2019-05-23 T12:23:59 PDT
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Notes for object NGC 7252

10 note(s) found in NED.


1. 2002ApJS..143...47D
Re:IRAS 22179-2455
IRAS 22179-2455 (NGC 7252).---This is the well-known "atoms for peace"
merger remnant galaxy and has been studied extensively (e.g.,
Schweizer 1982; Dupraz et al. 1990; Borne & Richstone 1991; Hibbard &
Mihos 1995; Whitmore et al. 1997). We observe strong tidal features
in the red continuum image as has been previously observed at many
wavelengths from X-ray to radio (e.g., Read & Ponman 1998; Whitmore et
al. 1997; Richter et al. 1994). The H{alpha} image, however, shows that
most of the star formation in this galaxy is strongly concentrated
toward the nucleus. Some diffuse H{alpha} emission can be seen
extending to the northeast of the galaxy, and two faint H{alpha} knots
appear in the east, corresponding to one of the tidal features
observed in the red continuum image. Spectrophotometry was obtained
for this galaxy by Young et al. (1995), revealing an H II region--like
spectrum with strong Balmer absorption and emission in the nucleus (4
kpc aperture). This is indicative of both an old stellar population and
a current star-forming population coexisting in the inner regions of
this galaxy, consistent with our observations of very strong H{alpha}
and red continuum emission from the nucleus.

2. 1998MNRAS.297..143R
Re:ARP 226
NGC 7252 (Arp 226), the `atoms for peace' galaxy, is the prototypical merger
remnant, and is the last system within the Toomre sequence. It has two equally
long, very faint tails emanating from a disturbed, double-motion spheroidal
body, the mean light distributon of which closely folows the de Vaucouleurs
r^1/4^ law, typical of ellipticals.

3. 1997AJ....114.1797W
Re:NGC 7252
NGC 7252 (Whitmore et al. 1993; Miller et al. 1997a): NGC 7252 is the "oldest"
(i.e., most advanced) merger of the 11 galaxies in the Toomre (1977) sequence.
A young population is present with a mean V-I=0.65 mag extending to M_V_=-16
mag. It is interesting to note that this is 3 mag brighter than in NGC 3921,
although the colors are very similar. However, there are only five clusters
brighter than M_V_=-13, and this may simply indicate that a few young clusters
are still being produced in NGC 7252 but not in NGC 3921. The old population of
globular clusters is clearly seen at V-I=1.00+/-0.1 mag (Miller et al. 1997a).
The CMD looks quite similar to the 0.5 Gyr simulation shown in Fig. 15. Our
estimated mean age for the clusters is 0.6+/-0.2 Gyr, in good agreement with
the value of ~0.7 Gyr based on previous estimates of the merger age.

4. 1994CAG1..B...0000S
Re:NGC 7252
Merger or S0_1_ pec
CD-1564-S/Br
Aug 9/10, 1980
103aO + GG385
45 min
NGC 7252, with its two principal long, thin
plumes and its many shorter plumes near the
main body, was originally suggested by Toomre
and Toomre (1972) to be the product of a
merger. Schweizer (1982, 1983) argued the case
for a merger of two disk galaxies using data on
surface brightness, spectroscopy, and internal
kinematic structure. Dynamical interaction
simulations by Borne and Richstone (1982,
1991) support this interpretation.
The heavy exposure in the top print with a
wide view shows the principal plumes. These
features are shown particularly well in the series
of images by Schweizer (1982). Star formation
(HII-region candidates) in each of the outer
plumes is also suggested there.

5. 1994CAG1..B...0000S
Re:NGC 7252
Merger or S0_1_ pec
CD-1564-S/Br
Aug 9/10, 1980
103aO + GG385
45 min
This light print is made from the same
original plate used for the heavy print above. The
inner image shows an S0-like luminosity distribution,
and the central core is clearly S0; there is
an apparent break in the gradient of the profile
two-thirds the way out the disk, giving the
two-zone look characteristic of the S0 class often
discussed in the S0 section.

6. 1994AJ....107...99R
Re:NGC 7252
D-35 = NGC 7252. This, the famous 'Atoms for Peace' galaxy studied by
Schweizer (1982), is the most optically-luminous and one of the more
infrared-luminous galaxies in our sample. The galaxy is an obvious
merger product, as evidenced by the remarkable optical loops and tidal
tails surrounding it. The GB 140' detects 4.5 x 10^9^ M_sun_ of HI, which
given the large blue luminosity of this galaxy, makes it gas-poor
compared to others in our sample. The linewidth of 200 km s^-1^ seems
surprisingly low given the disturbed optical morphology of the system.
VLA observations (Hibbard et al. 1993) show 3.6 x 10^9^ M_sun_ of H I in
NGC 7252, tails and all, and a further 1.4 x 10^9^ M_sun_ in an
uncatalogued companion, A2218-248, about 12' and 50 km s^-1^ away. The
sum of these two fluxes is within 15% of our measured value.

7. 1985SGC...C...0000C
Re:NGC 7252
Plate 4469r
Overexposed center, dist lens and corona with 2 plumes. Overall
dimensions: [10: x 5:].

8. 1982ESOU..C...0000L
Re:ESO 221758-2455.8
=ESO 533-IG 15
loops
filaments

9. 1976RC2...C...0000d
Re:NGC 7252
= Arp 226
Faint filaments and loops around main body of galaxy

10. 1964RC1...C...0000d
Re:NGC 7252
Extremely bright nucleus in a bright lens: 0.5 arcmin x 0.4 arcmin with traces
of (r): 0.3 arcmin x 0.3 arcmin. Traces of a faint (R): 2.0 arcmin x
1.4 arcmin.


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