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Date and Time of the Query: 2019-06-25 T07:17:52 PDT
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Notes for object IC 4769

4 note(s) found in NED.


1. 2002ApJS..143...47D
Re:IRAS 18429-6312
IRAS 18429-6312(IC 4769).---This object is in a galaxy cluster
(Lauberts 1982; Corwin et al. 1985) and is interacting with the small
galaxy to its west. It is a barred spiral galaxy, with strong H{alpha}
emission in its tidally distorted northern spiral arm. The strongest
H{alpha} emission occurs in the nucleus and at the ends of the bar.
This galaxy has been classified as a Sy2 using optical diagnostics
(Kewley et al. 2001b; Whittle 1985), but the AGN clearly does not
dominate the total H{alpha} emission from the galaxy. The companion
galaxy has distributed star formation across its disk.

2. 1995A&AS..113...35A
Re:DC 1842-630:[D80] 039
DC 39: Observed with DC 40 in 1992 with an interference filter cutting
the receding side, it was observed again in 1993 with a better centered
filter and a longer exposure time. The approaching side of the rotation
curve already obtained in 1992 was fully confirmed and the receding side
observed in good conditions.
The northeast arm (blueshifted side) is much brighter in the continuum
as well as H{alpha} light and looks very straight, as if it were an
edge-on companion galaxy. However the 2D velocity field leaves no doubt
that it is part of DC 39. But the velocity field is problematic in the
southwest arm, although its morphology appears much more normal. The
rotation curve rapidly reaches a plateau with good agreement on both
receding and approaching sides up to 50", at which point there is a
sudden and strong decrease for the receding side due to the velocity
points measured along the tip of the southwest arm. But since there are
only a few of them and they are far from the major axis, their weight is
small in the average rotation curve. This anomalous behaviour of the
southwest arm is likely a result of non-circular motions or a sudden
bending of the spiral arm out of the disk of the galaxy; these could be
the result of a recent encounter. DC 40, which is less than 3' to the
west and has a slightly higher velocity, could be the culprit. Two other
members of the cluster, DC 36 and DC 35, are found in the vicinity,
respectively 2' and 3' to the southeast, with velocities 3150 km s^-1^
and 4320 km s^-1^ (Fairall 1979). DC 35 could have interacted with DC 39
as well.
The plateau of our rotation curve exhibits a similar wavy shape as
found by RWF, however we find its velocity almost 100 km s^-1^ higher.
Strangely their first velocity point is in good agreement with our data
and our curve agrees with their synthetic predicted rotation curve. The
explanation comes from their choice of the PA of the major axis,
175^deg^, since when simulating a slit with that PA along our 2D velocity
field we find a rotation curve with a plateau below 100 km s^-1^,
although much more wary. The value of PA we find is 130^deg^, which is
significantly lower (note that RWF tried 175^deg^ and 126^deg^,
mentioning that the true value could be significantly lower than the
175^deg^ they chose). Since we go 35% farther out than RWF, there is no
problem in obtaining OG, even with the much higher value of R_25_ listed
by the RC3 (61.3" instead of 40.2" adopted by RWF).

3. 1985SGC...C...0000C
Re:IC 4769
Plate 887
Dist, bright center with structure, very faint arms, one with line of knots.
2nd largest in cluster. Possible foreground? A dozen objects within 5'.
Plate 2290
Overexposed center, extremely bright bar (with internal structure?) 0.7 x 0.35.
Ssp or extremely bright extension to north arm 0.8 north. At end of chain of
7 galaxies. IC 4771 (Sb pec) is 6th at 7.0 south-following.

4. 1982ESOU..C...0000L
Re:ESO 184300-6312.8
=ESO 104- G 11
in cluster


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