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Date and Time of the Query: 2019-05-21 T03:43:10 PDT
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Notes for object NGC 0596

7 note(s) found in NED.


1. 2002A&A...391..531R
Re:NGC 0596
Presents approximately circular isophotes ({eps}~0.1 ), for all radii.
The position angle of the external isophotes varies about 40^deg^
in relation to the central region.

2. 2002A&A...391..531R
Re:NGC 0596
Abrupt variations of position angle (more than 40^deg^) ocurred in the
galaxies NGC 596, NGC 636 and NGC 7626. The first presents very low
ellipticity, which means that, at least in part, the variation of the
position angle can be spurious. NGC 636 shows slightly disky isophotes.
In both objects, we can see strong and nonconstant variations in the
Fourier coefficients; Michard & Marchal (1994), through V photometry,
proposed for both objects a disk structure in the internal region. For
NGC 596, Goudfooij et al. (1994) found the same result.
Ferrari et al. (1999) found, for NGC 636, a conical axisymmetrical
distribution of dust. Ionized gas in the form of a small internal disk,
perpendicular to the orientation of the dust cone, was also found for
this galaxy (Macchetto et al. 1996).

3. 1994CAG1..B...0000S
Re:NGC 0596
Group
E0/S0_1_(disk)
PH-7943/7944-S
Nov 8/9, 1980
103aO
12 min
A very-low-surface-brightness thick disk
exists that can be seen by viewing the main print
here from a distance while moving the head and
eyes back and forth. The position angle of the
thick disk is from lower left to upper left in the
orientation of the print here.
The insert print also shows an apparent
two-zone intensity structure in the inner region
that is normal for S0 galaxies, but not for
ellipticals.
NGC 596 forms a wide pair with NGC 584
(S0_1_(3, 5); panel 32). These are the brightest two
members of a small group that also contains
several dE dwarf candidates. Other bright
members of the group include NGC 586, NGC 600,
NGC 607, and NGC 615 (Sb; panel 131).

4. 1994A&AS..105..481M
Re:NGC 0596
NGC 596: A complex PA profile, with a total twist of some 60^deg^ led
NBPS92 to propose a bar-like structure (see graphs in the quoted paper).
Indeed there is an abrupt variation of geometrical parameters occurring
near l = 20 arcsec: the contours change from faintly boxy to very disky,
while the axis-ratio q decreases from 0.91 to 0.76, and a twist occurs
from PA = 81^deg^ to 39^deg^ (further decreasing to 22^deg^ in the
envelope. The inner component itself presents a further twist of some
15^deg^ between l= 10 and 3 arcsec. This galaxy is interpreted as a two-
component object with a peculiar envelope, most likely a disk, and
classified as diEp. See also an image treated by "unsharp masking" in
Schweizer (1992).

5. 1994A&AS..104..179G
Re:NGC 0596
The residual images reveal a stellar disk along PA 40^deg^. Due to the
large PA twist of 70^deg^ this only results in a significant S4 and C4
coefficients at radii > 15". Shells.

6. 1994A&A...286..389H
Re:NGC 0596
NGC 596 - might be confused by a nearby dwarf galaxy (at 4'), no radial
velocity known.

7. 1976RC2...C...0000d
Re:NGC 0596
In a group with IC 0127, NGC 0584, and NGC 0586.
Distorted corona with faint "tail" to south-preceding.
Similar to NGC 7135.
Photometry: (B,Y)
Publ. Byurakan Obs. No. 42, 3, 1970.
Photometry: (10 Color)
Ap. J., 179, 731, 1973.


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