Date and Time of the Query: 2019-06-17 T06:32:39 PDT
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Notes for object NGC 5693

5 note(s) found in NED.

1. 2008MNRAS.388..500E
Re:UGC 09406
UGC 9406 (NGC 5693). A short bright bar and an asymmetric disc (with one knotty
arm) are observed. This galaxy is paired with UGC 9399 (NGC 5689) at 11.8
arcmin, which may explain the presence of a single arm. Poor H{alpha} emission
is detected and our H{alpha} velocity field shows a strong dispersion, so that
it is difficult to draw any reliable rotation curve from our data. The
photometric inclination found in the literature varies from 33^deg^
(Vorontsov-Velyaminov & Krasnogorskaya 1994) to 51^deg^ (HyperLeda). Even
when adopting the lowest value of inclination, we find a maximum rotation
velocity which remains abnormally low considering the absolute magnitude of this
galaxy, suggesting that our H{alpha} velocity field is far from reaching the
maximum velocity amplitude. Indeed the width of the H I profile at 20 per cent
is 74 km s^-1^ (Bottinelli et al. 1990), whereas our H{alpha} velocity field
amplitude is smaller than 50 km s^-1^. No H I velocity map is available for this
galaxy in the litera ture.

2. 2006MNRAS.369..529F
Re:NGC 5693
NGC 5953 is a Seyfert 2 galaxy closely interacting with NGC 5954 (Reshetnikov
1993; Gonzalez Delgado & Perez 1996). The SAURON stellar kinematics display
large-scale rotation and a kinematically decoupled component in the central 10
arcsec. The [O III] ionized gas presents an elongated distribution towards NGC
5954 (i.e. northeast of NGC 5953 centre), which is associated with radio
emission (Jenkins 1984), whereas the H{beta} distribution is symmetric around
the galactic centre, and it is consistent with a dust ring seen in the
unsharp-masked image. The ionized-gas kinematics of the central component follow
that of the stars in the inner parts, and it is in good agreement with that of
Hernandez-Toledo et al. (2003) from Fabry-Perot observations of the [N II]
emission line. The [O III]/H{beta} ratio map exhibits very low values in the
location of the circumnuclear region, and it is enhanced in the very centre of
the galaxy. Our results are similar to those measured by Yoshida et al. (1993)
in the inner region (i.e. [O III]/H{beta}= 0.14-0.41), and are consistent with a
star-forming ring surrounding an active galactic nucleus. The combined
observations presented here suggest that we might be witnessing the early stages
in the formation of a kinematically decoupled component. Further analysis
including stellar populations is, however, necessary to confirm this hypothesis.

3. 1976RC2...C...0000d
Re:NGC 5693
Pair with NGC 5689 at 11.8 arcmin

4. 1973UGC...C...0000N
Re:UGC 09406
SB(rs)d (de Vaucouleurs)

5. 1964RC1...C...0000d
Re:NGC 5693
Short bright bar. One main, knotty arm. Strongly asymmetric.
Pair with NGC 5689 at 11.8 arcmin.

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