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Date and Time of the Query: 2019-04-23 T07:28:50 PDT
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Notes for object NGC 3800

6 note(s) found in NED.


1. 2005MNRAS.364.1253V
Re:NGC 3800
NGC 3799/3800. NGC 3799 and 3800 were observed in separate maps. NGC 3799
individually is not detected at the 3{sigma} level (although we measure flux at
the 2{sigma} level). For NGC 3800 (shown in Fig. 1) most of the integrations for
the bolometers to the S of the map were unusable, and consequently this part of
the map is very much noisier. Generally, this observation is very noisy, and
especially bad at 450 {mu}m; thus no 450-{mu}m flux is available. In fact only
the main region of submm emission at the centre of the map is in an area free
from noisy bolometers, and it is this region over which we have measured the
submm flux of the galaxy.
The S_850_ listed for NGC 3799/3800 in Table 2 is a conservative measurement
of the 850-{mu}m emission from the system, the sum of the separately measured
fluxes from each of the two component galaxies. In co-adding the two maps there
appears to be a 'bridge' of 850-{mu}m emission between the two galaxies,
consistent with emission seen in the optical (NGC 3799 is to the SW of NGC 3800
in Fig. 1). However, since this region of the map has several noisy bolometers
we only measure fluxes for the main optical extent of the galaxies.

2. 1997AJ....114...77N
Re:NGC 3800
5.4 NGC 3799-3800
The Gunn r image of the NGC 3799-3800 system shows two spiral galaxies
surrounded by a diffuse common envelope of stellar emission. NGC 3799, the
southern galaxy of the pair, has a bright central spiral "S" coupled with broad
outer spiral structures which bear more resemblance to tidal tails than to real
spiral arms.
Figure 7(a) shows the galaxies to lie in a common H I envelope (which may be
the result of beam smearing). There is also sizable tail extending to the east.
NGC 3799 is not detected in the uniform weight image (not shown). The velocity
field [Fig. 7(b)] shows "gear-like" rotation of the two galaxies. Although the
beam smearing makes it difficult to completely disentangle the emission of the
two galaxies, it is clear that the central velocity of NGC 3800 is higher (by
~30-50 km s^-1^) than that of NGC 3799, which implies that NGC 3800 is
undergoing a direct encounter.
A companion galaxy (which we call NGC 3800A) is also detected [Fig. 7(a) and
8(a)]. Despite being optically much fainter, NGC 3800A has a similar peak H I
flux to the entire close pair combined. Its H I disk is warped, not unexpected
for a galaxy with such a large H I halo in the presence of nearby companions.
The ratio of H I to optical major axes is 6.5 (although beam smearing
correction could reduce this to ~5). NGC 3800A is not listed in NED. From the
velocity field in Fig. 7(b), we have attempted to assign the gas from the
emission region (not including the tail) to a each member of the pair. Figure
8(b) shows the H I emission for NGC 3799 and 3800 as well as the total
emission.

3. 1976RC2...C...0000d
Re:NGC 3800
= Arp 083
= VV 350
= Kara[72] 296
Interacting pair with NGC 3799 at 1.2 arcmin

4. 1973UGC...C...0000N
Re:UGC 06634
VV 350a, Arp 83b
Sb (de Vaucouleurs)
See UGC 06630
"Some hazy material at juncture of two arms; high surface brightness,
S-shape inside companion" (Arp)

5. 1964RC1...C...0000d
Re:NGC 3800
Very close pair with NGC 3799.
Photograph and Spectrum:
Ap. J., 116, 65, 1952.

6. 1959VV....C...0000V
Re:VV 350a
= NGC 3800
V = +3,482 km/sec from H{alpha}, {lambda}3727
(Page, T., Ap. J., 116, 63, 1952)


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