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Date and Time of the Query: 2022-01-20 T09:10:20 PST
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Notes for object NGC 1596

8 note(s) found in NED.


1. 2007MNRAS.378..594P
Re:NGC 1596
See Pohlen et al. (2004b) for additional notes. The face-on-equivalent profile
of NGC 1596 is classified as Type III, i.e. a break with an upbending profile
beyond. However, the profile is not well described by a simple broken
exponential. The whole disc profile (beyond R [IMAGE] +/-25 arcsec) appears to
be almost continuously upbending. One may argue for an extended, exponential
break region between breaks at R ~= 70 and ~=130 arcsec. Therefore, the exact
position of the break is unclear. Judging from the individually deprojected cuts
this structure is driven by the clear upbending breaks on the major axis and at
z = 8 arcsec at a radial distance of R ~= 110 arcsec. All cuts at larger
distance from the plane (z <~ 17 arcsec) are consistent with having no break.
We find an increase in scalelength by a factor of 3.6 from the major axis
(steepest) to a vertical scaleheight of 33 arcsec (flatter) in the inner region.

2. 1994CAG1..B...0000S
Re:NGC 1596
Pair [with NGC 1602]
S0_1_(7)
(P)
CD-676-Br
Jan 25/26, 1979
IIaO + GG385
180 min
These two galaxies form a physical pair of
greatly dissimilar types. NGC 1569 is a classical
S0_1_ with a boxy bulge and a well-defined,
high-surface-brightness disk. NGC 1602 is a
star-forming Sm galaxy having a knot of bright HII
regions. Because of the dissimilar types and their
undoubted physical relationship, the pair is
important in understanding that the formation of
S0 galaxies is generic to the classification
sequence; S0's are not secondary forms made from
what were once spirals by some process such as
gas sweeping; they are intrinsic to the sequence.
The angular separation of the pair is 3.1'.
The redshifts listed by Huchtmeier and Richter
(1989) and corrected to the centroid of the Local
Group are v_o(1596) = 1324 km/s and v_o(1602)
= 1382 km/s. The projected linear separation
is small at 24 kpc based on a redshift distance of
27 Mpc (H = 50).

3. 1994CAG1..B...0000S
Re:NGC 1596
Pair [with NGC 1602]
S0_1_(7)
(P)
Jan 5/6, 1979
103aO + GG385
10 min
The print here is made from a different Las
Campanas 100-inch du Pont plate from the one
used for the print above. The S0 morphology of
NGC 1596 is well seen by the existence of the
bright disk and the boxy bulge. The knot of HII
regions in NGC 1602 and the other evidence of
star formation over its face are well seen here.

4. 1985SGC...C...0000C
Re:NGC 1596
Plate 1893
Overexposed center, slightly flattened bulge. NGC 1602 3.0 south-following.

5. 1982ESOU..C...0000L
Re:ESO 042632-5508.2
=ESO 157- G 31
in group with ESO 157- G 32

6. 1979AJ.....84..472S
Re:NGC 1596
Strong central bulge with smooth thin disk.
The major axis of the bulge appears tilted approximately 5 degrees
to the plane of the disk (tidal distortion due to NGC 1602?).

7. 1976RC2...C...0000d
Re:NGC 1596
There is a star 0.6 arcmin preceding the nucleus.
Pair with NGC 1602 at 3.0 arcmin.

8. 1964RC1...C...0000d
Re:NGC 1596
Very bright nucleus.
There is a star 0.6 arcmin [preceding] the nucleus.
Paired with NGC 1602 at 3.0 arcmin.


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