NGC 5746 (UGC 9499). No previous X-ray data have been reported previously. Its
morphology shows a clearly compact, unresolved nuclear source (Fig. 5). Nagar et
al. (2002) detected a compact radio source suggesting the AGN nature of this
galaxy. Both the fitting and the position in the color-color diagrams indicate
considerable obscuration (see Table 6).
NGC 5746. NVSS reports a 19 mJy and FIRST a 1.2 mJy source. 1.4 GHz, 54"
resolution observations (Condon 1987) measure an uncertain 11 mJy (due
to confusion from a strong, unrelated northern source). The
high-resolution observations at 1.4 GHz of Hummel et al. (1987)
establish an upper limit of 0.8 mJy to the radio core emission.
A dark dust lane obscures most of the nucleus in this nearly edge-on
spiral, making the spectrum heavily reddened.
April 2/3, 1981
NGC 5746 is the brighter member of the
physical pair with NGC 5740 (Sb; panel 141).
It is seen nearly edge on; the bulge light is
visible below the near-side dust lane as well as
above it. For this to happen when the bulge is
moderately small requires the line of sight to be
within only a few degrees from exactly edge on.
= Kara 434b
Non-interacting pair with NGC 5740 at 18 arcmin
A.J., 72, 1032, 1967.
A.J., 72, 1032, 1967.
IAU Symp. No.58, 337, 1974.
Systemic Velocity Astr. Ap., 8, 364, 1970.
SAB(rs)b? (de Vaucouleurs), Sb- (Holmberg)
See UGC 09493
Very small, bright nucleus in a bright central bulge. Strong dark lane in
Non-interacting pair with NGC 5740 at 18 arcmin.
Photograph and Photometry:
B.A.N., 16, 1, 1961.
Orientation and Rotation:
Ap. J., 97, 117, 1943.
Ap. J., 127, 487, 1958.
The spheroidal component is very much reduced, but still
contributes a large fraction of the light.
The spiral pattern of bright and dark arms is well defined
(save for the projection foreshortening), regular and
still fairly smooth, although it begins to show some clumpiness.
Compare with NGC 7205 (Plate 18), and NGC 6753 (Plate 22).
A fine, nearly edgwise spiral 7' x 0.8' in p.a. 170^deg^; quite bright. Bright,
elongated nucleus. A broad dark lane runs along the spiral to the east of the
nucleus. Most of the nebular matter is to the west of this lane, there are no
prominent condensations other than the nucleus. See Abs. Eff. 18 s.n.