Date and Time of the Query: 2019-03-26 T17:44:27 PDT
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Notes for object NGC 3256

13 note(s) found in NED.

1. 2008A&A...484..341R
Re:NGC 3256
Our image (not presented here) of this IR-luminous merger system shows an
unresolved core, In contrast to Siebenmorgen et al. (2004) who present a
resolved, yet featureless image, taken with shorter exposure time. The
difference may be explained by a change in seeing between the calibrator, from
which the PSF is determined, and NGC 3256.

2. 2004A&A...419..501F
Re:NGC 3256
NGC 3256 - The MIR emission can be separated into two components of
different sizes, a core of {approx}8" superposed onto a source of
{approx}20". Therefore, a single Gaussian does not provide a good fit to
the surface brightness profile. We adopt the size of the larger source
as our aperture. Kawara et al. (1987) report a Br{gamma} flux of 14.8 x
10^-17^ W m^-2^ in a smaller aperture of 9" x 18", almost identical to
the total Br{gamma} flux of 15 x 10^-17^ W m^-2^ measured by Moorwood &
Oliva (1994) in a field of view of 34" x 34". We derive the extinction
in the central 3.5" x 3.5" from the Pa{beta}/Br{gamma} ratio of Doyon et
al. (1994) and assume that it does not vary inside our larger aperture.

3. 1998AJ....116.2682C
Re:IRAS 10257-4338
NGC 3256. Optical position from Wamsteker et al. (1985). Radio core
resolved in 4" resolution 4.86 GHz VLA map (Smith & Kassim 1993).

4. 1996ApJS..103...81C
Re:NGC 3256
NGC 3256.--VLA CnB-configuration map at 4.86 GHz in Smith & Kassim (1993).

5. 1994CAG1..B...0000S
Re:NGC 3256
Sb(s) pec
Feb 7/8, 1978
103aO + GG385
45 min
The two views of NGC 3256 are shown on
the facing panel, printed to different scales and
different contrast gray scales.
The galaxy is in the complex Hydra-Centaurus
Supercluster region, about 9^deg^ south of the
concentrated Antlia Cluster (Hopp and Materne
1985; Ferguson and Sandage 1990) whose redshift
is = 2500 km/s. The redshift of NGC 3256
is v_o = 2517 km/s.
The extended luminous streamer, visible in
the image on the left, extends nearly to the right-hand
border of the print. A very-low-surface-brightness
luminous wisp exists at the position
three-quarters of the way to the left-hand
border; it may or may not be associated with the
galaxy. This wisp is real, visible on a second
NGC 3256 has been said to be a galaxy in
collision or in a merger encounter (de
Vaucouleurs 1956a, 1963; Toomre 1977 in the
discussion) based on the plume and the nature of
the central regions (de Vaucouleurs 1956a),
shown best at the right. This description is
challenged at the right.

6. 1994CAG1..B...0000S
Re:NGC 3256
Sb(s) pec
Feb 7/8, 1978
103aO + GG385
45 min
The orientation of NGC 3256 in these
prints is south at the top, east to the right, given
here to identify the features described by de
Vaucouleurs (1956a) as fragments and the nuclei
of two colliding galaxies. He describes "2 or 3
nuclei in contact forming a very bright mass 0.6'
x 0.3' with fragment 0.5' x 0.15' at 0.3' south
These features in the print to the right are
the bright central bulge, partially burned out
here, and the high-surface-brightness area at the
base of the smooth "plume" encircling the top of
the main body. Neither of these features were
resolved on the Mount Stromlo plate material,
and neither of them can be described on the
present material as the nuclei of two colliding
The luminosity pattern is chaotic, but it is
unclear if the pattern is due to collision, to a
possible merger, or is an apparent pattern caused
by dust lanes. The central region on the available
Las Campanas 100-inch plates appears to be that
of a single, albeit disturbed, galaxy with dust
lanes that cut the bright bulge, giving the
appearance of separate components on low-resolution
images. Of course, by their presence the
plumes have suggested, by themselves, a merger
event (Toomre 1977; Schweizer 1982, 1983,
1986), but the nuclei as described by de
Vaucouleurs do not exist.

7. 1993ApJS...86....5K
Re:NGC 3256
NGC 3256; Sb(s) pec, starburst.
This galaxy contains a very bright star-forming region spanning over 4
kpc and called by Joseph & Wright (1985) a "super-starburst." NGC 3256 is
also ultraluminous in the infrared (Kawara, Nishida, & Gregory 1990).
Tidal tails evident in the optical photographs of Joseph & Wright signal
a merger. The short- wavelength UV spectrum shows a flux decreasing
toward short wavelengths with very strong, deep absorption features.
while the deep broad absorption features reveal the presence of young,
hot stars, the overall slope is probably due to dust [E(B - V) = 0.13

8. 1985SGC...C...0000C
Re:NGC 3256
Plate 1447
Colliding pair at 0.45, loops and plumes (included in dimensions).

9. 1982ESOU..C...0000L
Re:ESO 102543-4339.0
=ESO 263-IG 38
in cluster
*2 long arms disturbed
*star superimposed

10. 1979AJ.....84..472S
Re:NGC 3256
= VV 065
Much dust in broken spiral patterns silhouetted against
a high surface brightness disk.
Very high-surface-brightness central region
and two inner spiral arms that are lumpy.
Two smooth outer plumes of low surface brightness, as if by encounter.
Three galaxies of unknown redshift exist within about 20 diameters,
listed as NGC 3526A, NGC 3526B and NGC 3526C
by Sulentic and Tifft (1973) in their Revised NGC.

11. 1976RC2...C...0000d
Re:NGC 3256
= VV 065
In Klemola Group No. 12
A.J., 74, 804, 1969
Atlas Gal. Australis, 1968.
Photometry: (I.R.: 1-3.5 microns)
M.N.R.A.S., 164, 155, 1973. 168, 27P, 1974.
Spectrum: (possible variability)
M.N.R.A.S., 168, 27P, 1974.
Radio Observations:
M.N.R.A.S., 167, 251, 1974.

12. 1964RC1...C...0000d
Re:NGC 3256
Colliding system includes 2 or 3 nuclei in contact forming a very bright mass:
0.6 arcmin x 0.3 arcmin with a fragment 0.5 arcmin x 0.15 arcmin at 0.3 arcmin
south-preceding. Very faint streamers up to 4 arcmin from nucleus. Overall
extent: 7.5 arcmin x 2.5 arcmin:
Photograph and Photometry:
Zeit. fur Ap, 47, 9, 1959. Magnitude: 11.85 (pg).
Mem. R.A.S., 68, 69, 1961.

13. 1959VV....C...0000V
Re:VV 065
= NGC 3256
Upper photograph is from Sersic:
(Zeit. fur Astrophys., 47, 9, 1959)
Lower picture is from de Vaucouleurs:
(Sky & Telescope, 16, No. 12)
2 (two) or 3 (three) nuclei
(de Vaucouleurs, G., Mem. Commonwealth Obs., No.13, 1956)

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