Date and Time of the Query: 2019-08-25 T17:42:54 PDT
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Notes for object NGC 5297

8 note(s) found in NED.

1. 2008MNRAS.388..500E
Re:UGC 08709
UGC 8709 (NGC 5297). It is the large companion of NGC 5296. H{alpha} emission is
detected in the northern arm but only in the beginning of the southern tidal
arm, in agreement with Rossa & Dettmar (2003). The clear signature of a bar can
be seen at the centre of the H{alpha} velocity field. From the kinematics, we
find an inclination (76^deg^+/- 1^deg^) slightly smaller than the photometric
one (82^deg^+/- 3^deg^). It seems that the photometric inclination has been
computed from the axial ratio of the disc including the tidal arms. The width of
the H I profile at 20 per cent (418 km s^-1^ from van Driel et al. 2001, 413 km
s^-1^ from Bottinelli et al. 1990) is in agreement with our H{alpha} velocity
field amplitude. The H I velocity field has been observed by WHISP (website) and
is consistent with ours. The H I position-velocity diagram shows a slightly
decreasing plateau beyond 1 arcmin, in agreement with our H{alpha} rotation
curve. The long-slit rotation curve observed by Rampazzo et al .(1995) also
shows a decreasing trend in the outer parts. No CO has been detected in this
galaxy (Elfhag et al. 1996).

2. 2003A&A...406..505R
Re:NGC 5297
NGC 5297 Another northern edge-on spiral, NGC 5297 forms a binary
galaxy with NGC 5296 (Turner 1976), which is separated by about 1.5'
from NGC 5297, and has a velocity difference of {DELTA}_v_{approx} 360
km s^-1^. Another interesting source is also located in the direct
vicinity, a quasar of V=19.3 mag (Arp 1976). This quasar ([HB89]
1342+440), which has a redshift of z=0.963, is located 2.5' to the SW.
Arp reports on a luminous extension from NGC 5236 pointing at the QSO,
which Sharp (1990) did not confirm. However, Sharp (1990) did comment
on the unusually bright off-center secondary nucleus of NGC 5296. The
QSO is marked by a circle in our R-band image in Fig. 41. The outer
spiral arms of NGC 5297 show evidence of perturbation by the S0
companion, as reported by (Rampazzo et al. 1995).
Radio continuum observations of NGC 5297 have been performed (Irwin et
al. 2000; Hummel et al. 1985; Irwin et al. 1999). While Irwin et al.
(1999) claims extended radio continuum emission from NGC 5297, still,
higher resolution observations show only very weak emission (Irwin et
al. 2000). Our H{alpha} image does not reveal any extraplanar emission.
Thus, we do not see enhanced SF activity due to the interaction with
the companion galaxy in this case. The L_FIR_/D^2^_25_ ratio is
moderate. We also note, that this galaxy actually is not perfectly

3. 2000AJ....119.1592I
Re:NGC 5297
This galaxy, in the group LGG-358 (Garcia 1993), is apparently
interacting with its companion, NGC 5296, which is situated 1.5' to the
southwest (Sharp 1990). Broadband and H{alpha} CCD images by Sharp
(1990) reveal some extended material, presumably related to this
interaction. Previous low-resolution radio continuum images can be seen
in Pooley (1978), Hummel et al. (1985), and Paper I. The high-resolution
radio emission from this galaxy is very weak, showing only a few weak
components, the strongest of which is at the 7{sigma} level.

4. 1995A&AS..110..131R
Re:NGC 5297
NGC 5297: The outer spiral arms of the giant member of this pair show
evidence of perturbation by the S0 companion (Arp 1976). The SE arm shows
an unusual pitch angle although there is no clear connection to the
companion. The major axis rotation curve for NGC 5297 (Fig. 2) is well
defined out to r = 100 arcsec and is almost flat up to the last observed
point. The centroid velocities of the stars and gas agree well with
previous HI determinations. The gas appears to show a systematically very
slightly higher velocity than the stars. The velocity dispersion is
constant (169+/-73 km s^-1^ )within the inner 10 arcsec. Bonfanti (1994)
obtained a weighted average for the three central values of the velocity
dispersion of 104+/-5 km s^-1^.
The velocity curve along the axis connecting the two members (Fig. 3),
which is near the minor axis of the galaxy, reveals evidence for an
apparent counter rotating gas core in the inner 6 arcsec centered on the
nucleus. This feature could be connected with the presence of inner
structure, possibly a small bar. A similar case has been detected in the
lenticular galaxy NGC 4684 by Bettoni et al. (1993) and attributed to a
bar visible in the image. The same region shows a reversal of the
[N II] /H{alpha} ratio. In Fig. 12 this region is indicated as NGC 5297
center and lies in the area characteristic of low level nuclear activity.
Among possible interpretations of K 394, we may be observing either a
very slow encounter or a stable system with parent and satellite galaxy:
both dynamical situations would explain the strongly twisted isophotes of
NGC 5296, which are expected when the relative velocity does not exceed
the internal velocity dispersion. The slowness of the encounter enhances
also the possibility that gas could be acquired from the gas-rich spiral.

5. 1994CAG1..B...0000S
Re:NGC 5297
Karachentsev 394 [with NGC 5296]
Feb 6/7, 1981
12 min
Racine wedge
NGC 5297 forms a close physical pair with
[NGC 5296] (S0 pec) at an angular
separation of 88". The redshift from the RSA is
v_o = 2654 km/s. Karachentsev (1987) lists
v_o = 2755 km/s for the S0 companion. At the
redshift distance of 53 Mpc, the projected linear
separation of the pair is very small at 23 kpc.
The multiple arms in NGC 5297 are thin
and well defined but the pattern is mostly hidden
by the high inclination.

6. 1976RC2...C...0000d
Re:NGC 5297
= Kara[72] 394
Interacting (?) pair with NGC 5296 at 1.6 arcmin.

7. 1973UGC...C...0000N
Re:UGC 08709
SAB(s)b: (de Vaucouleurs)
Paired with 13 44.2 +44 05 = NGC 5296 at 1.5, 215, 0.9 x 0.5, S0
(de Vaucouleurs), m=15.0

8. 1964RC1...C...0000d
Re:NGC 5297
Very small, bright nucleus. Bright lens with several narrow knotty arms and
dark lanes. 2 faint outer smooth arms.
Lund 9 dimensions are for the bright part only.
Interacting? pair with NGC 5296 at 1.6 arcmin.

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