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Date and Time of the Query: 2019-06-18 T16:07:44 PDT
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Notes for object Superantennae

6 note(s) found in NED.


1. 2004AJ....128..969D
Re:IRAS F19254-7245
F19254-7245: Extended at 1" spatial resolution. Bright and fainter
components at low frequency, fainter component undetected at high
frequency. Steep spectrum flattening toward lower frequency.

2. 2004AJ....128..955D
Re:IRAS F19254-7245
F19254-7245: This is the Superantennae. Our image covers the central 150
kpc; the low surface brightness tidal tails are not shown. No fit was
attempted for this galaxy.

3. 2003MNRAS.343..585F
Re:IRAS 19254-7245
19254-7245. This object is more commonly known as the Super-Antenna,
arid possesses a spectacular morphology. Two extremely long tail-like
features extend on either side of the central regions, with a total
length of 500 kpc. These features can be explained as a result of a
coplanar encounter between two massive disc galaxies (Melnick & Mirabel
1990). There are two optical nuclei in the central regions, one with a
Sy2 spectrum and the other with a starburst spectrum (Mirabel, Lutz &
Maza 1991). Further optical spectroscopy by Colina, Lipari & Macchetto
(1991) classify this source as an obscured AGN surrounded by
star-forming clouds. The mid-IR spectrum of this object classifies it as
an AGN (Lutz et al. 1999). X-ray observations (Pappa, Georgaritopoulos
& Stewart 2000) were inconclusive, but suggested an AGN was at least
present in this object. We compiled for this object an extra flux at 6.7
{microns} of 113 +- 23 mJy from Charmandaris et al. (2002). Of our
sample the SED fit for this object is of reasonable quality, but
deviates markedly from one point. We interpret this as being due to the
very large angular size of this object, which is much larger than any
other object in our sample. Whilst IRAS fluxes are likely to contain all
the flux from the object, it is feasible that other observations have
missed some flux. Our fit (Fig. 1) is a pure starburst, but the AGN
upper limit is weak.

4. 2003AJ....126.2237D
Re:IRAS F19254-7245
.
4.2. Seyfert Galaxies
.
The Superantennae (F19254-7245) is an infrared-luminous interacting
pair of galaxies [{nu}L_{nu}_(60 micron) = 10^12.05^L_solar]. It has a
small radio excess (u = 1.76) and moderate radio power [L_{nu}_(4.8
GHz) = 10^24.2^ W Hz^-1^]. The small radio excess is only just
sufficient to distinguish it from radio-quiet objects. The two
distinct nuclei have been classified as a Seyfert 2 (southern galaxy)
and a starburst/LINER (northern galaxy) based on optical spectroscopy
(Mirabel, Lutz, & Maza 1991). The Seyfert galaxy is the dominant radio
source (ATCA data) and is likely to be the FIR source (Mirabel et al.
1991). The radio source is smaller than our ATCA beam at 8.6 GHz, and
so must be less than 500 pc in extent.

5. 1997A&AS..124..533D
Re:IRAS 19254-7245
IRAS 19254-7245: This spectacular object, also known as "the Super-Antennae"
has been discussed in details by Mirabel et al.(1991) and Colina et al.(1991).

6. 1990A&A...231L..19M
Re:IRAS 19254-7245
IRAS 19254-7245 is a galaxy with remarkable narrow and elongated
features that stretch out beyond the limits of the picture shown in
Figure 1a. For H_0_ = 75 km s^-1^ the long slender features have a
total extent of 500 kpc. These tails are reminiscent of "The Antennae"
seen in NGC 4038/9 and, since in IRAS 19254-7245 they are a factor of 5
larger in size, we have named this galaxy the "Super-Antena", following
the spelling in the mother tongue of the authors. These spectacular
streamers are likely to be provoked by gravity during a flat encounter
of the same, equally massive disk galaxies (toomre and Toomre, 1972).
The image in Figure 1a show bright spots along the thin tails, which
may be localized bursts of star formation at distances in the range of
100-200 kpc from the main bodies of the merging galaxies. Two nuclei 9
arcsec (~10 kpc) apart in PA 160^deg^ are also apparent in that figure.
K band imaging by Djorgovski (1989) shows that the southern component
is semi-stellar and the northern fuzzy, the southern component being
considerably brighter, which could be consistent with it being a
"hidden" AGN.
Mirabel et al. (1990) find in the Super-antena 3x10^10^ solar masses
of molecular gas, namely 10 times the content of molecular gas in the
Galaxy. The results from a comprehensive study of this remarkable
system will be presented in a forthcoming paper.


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