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Date and Time of the Query: 2022-01-25 T00:30:07 PST
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Notes for object NGC 1602

8 note(s) found in NED.


1. 1994CAG1..B...0000S
Re:NGC 1602
Pair [with NGC 1596]
SBm
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).

2. 1994CAG1..B...0000S
Re:NGC 1602
Pair [with NGC 1596]
SBm
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.

3. 1994CAG1..B...0000S
Re:NGC 1602
Pair [with NGC 1596]
Not in RSA
SBm
CD-676-Br
Jan 25/26, 1979
IIaO + GG385
180 min
NGC 1602 is the highly resolved companion
to the S0_1_(7) galaxy NGC 1596 (panel 51). The
redshifts are v_o(1569) = 1324 km/s and
v_o(1602) = 1382 km/s. The near-equality of
the redshifts and the proximity of the components
at an angular separation of 3.1', suggest
a binary pair. At the mean redshift distance of
27 Mpc, the projected linear separation of the pair
would be small at 24 kpc.
NGC 1602 is resolved into many HII
regions. There is a complex of six such regions
(unresolved in the print here) near the end of the
major axis. The envelope of this complex has an
angular diameter of 10", which, at the distance
of 27 Mpc, is a linear diameter of 1300 psc,
similar to the diameter of the complex in
NGC 4861 on the preceding panel. At higher spatial
resolution, this complex would presumably appear
as an association of early-type stars and HII
regions.
The NGC 1596/1602 pair is of particular
interest because of the large difference in
morphological type. The S0 and Im types span the
total range of the classification sequence (see the
diagram of the dwarf classification sequence in
Chapter II here). Pairs with such diverse types
are of obvious importance in studies of the meaning
of the Hubble sequence for galaxy formation
and possible evolution within the sequence. Does
one morphological type change into the other
with time or with the type of environment, or are
the morphological types of individual galaxies
stable over most of a Hubble time, as suggested
by the calculations of Roberts (1963) and of
Sandage (1986d)? These central points are
discussed in Chapter IV here, "The Meaning of the
Classification."

4. 1985SGC...C...0000C
Re:NGC 1602
Plate 1893
Pretty faint bar, several faint knots; very bright knot 0.6 south-
preceding-preceding.

5. 1982ESOU..C...0000L
Re:ESO 042648-5510.0
=ESO 157- G 32
in group with ESO 157- G 31
cz=1900:200(9C) (A)
cz=1519:200(9C) (B)
knotty structure in west part

6. 1979AJ.....84..472S
Re:NGC 1602
Short exposure 103a-D plate centered on NGC 1596 shows
a large (presumably) HII region of diameter about 4 arcsec,
indicating possibility of useful resolution into stars.
This galaxy is not in the Shapley-Ames Catalog.

7. 1976RC2...C...0000d
Re:NGC 1602
Pair with NGC 1596 at 3.0 arcmin.

8. 1964RC1...C...0000d
Re:NGC 1602
Bright middle, no bright nucleus.
(r): 0.95: arcmin x 0.7 arcmin.
Paired with NGC 1596 at 3.0 arcmin.
See also M.N.R.A.S., 81, 601, 1921.


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