Date and Time of the Query: 2019-06-24 T19:28:37 PDT
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Notes for object NGC 5532

8 note(s) found in NED.

1. 2008ApJS..177..148F
Re:3C 296
4.1.11. 3C 296; z = 0.025; 3C 296 is hosted by an extremely boxy elliptical
galaxy. It has a double-lobed jet with clear radio emission along the jet axis
(FR I). The WFPC2 image (Martel et al. 1999) shows a truncated edge-on disk
embedded in the galaxy, similar to that seen in NGC 4261. The disk is aligned
with the major axis of the elliptical galaxy, with the jet perpendicular to the
disk. The nucleus is seen in both WFPC2 image (although faint) and in the NICMOS
image (brighter). X-ray and radio observations of this galaxy are discussed in
Hardcastle et al. (2005).

2. 2006ApJ...642...96E
Re:3C 296
Several simple one-component models were fitted to the nuclear spectrum, but we
found that the first acceptable fit was achieved with a model consisting of an
absorbed [N_H_ = (1.5+/-0.9) x 10^22^ atoms cm^-2^] power law of photon index
1.77^+0.60^_-0.52_ accompanied by thermal emission (kT = 0.8^+0.3^_-0.5_ keV,
abundance 0.3 of solar, and normalization 1.16^+0.42^_-0.45_ x 10^-5^). The fit
was good: {chi}^2^ = 9.3 for 21 dof. However, an acceptable fit was also
achieved with the combination of an absorbed power law with N_H_ =
2.1^+1.5^_-1.7_ x 10^22^ atoms cm^-2^, photon index {GAMMA}= 1.9, and a second
unabsorbed power law with a photon index frozen at 2. A subsequent radial
profile analysis shows that the number of extended counts measured spectrally
and spatially agree for the first model, and so we adopt this model. We
performed a comparison between our spectral analysis and previously published
Chandra results (Hardcastle et al. 2005b). The measured values of the intrinsic
absorption, power-law photon index, and 1 keV flux densities are consistent, as
are the parameters of the thermal component.

3. 2005ApJ...618..635G
Re:3C 296
1414+11 (3C 296) (Fig.11)
This symmetric FR I radio galaxy shows two-sided emission in our VLBI
image, as well as in the VLA images (Leahy & Perley 1991). From
polarization observations (Garrington et al. 1996), the southern lobe
appears to be the more distant one (because of the Laing-Garrington
effect). This agrees with the evidence that the brighter,
kiloparsec-scale jet points to the north and with the brightness
asymmetry in our VLBI image even if the low jet-counterjet ratio
suggests an orientation close to the plane of the sky. A second-epoch
observation did not show any visible proper motion in this smooth
radio jet.

4. 2002ApJS..139..411A
Re:3C 296
3C296.-The UV image of this galaxy, Figure 20a, shows a well-defined,
smooth dust disk. The southeast side of the dust disk is apparent in the
UV image as extinction against the background galaxy emission.

5. 2000ApJS..129...33D
Re:3C 296
3C 296 (NGC 5532), z = 0.0237. - The absorption map (Fig. 23) shows
a sharp, well defined edge-on disk, similar in shape to the one seen in
3C 270, only on a smaller linear scale. The radio map shows a
double-sided jet that remains straight over the full size of the source.
The lobes are more extended toward the southeast of the jet axis.

6. 1999ApJS..122...81M
Re:3C 296
3C 296 (NGC 5532). - This boxy elliptical galaxy hosts a sub-kiloparsec,
elongated, and sharp dusty structure centered on its nucleus and at a
P.A. of ~ 163^deg^. It is very reminiscent of the dust disk in 3C 270
(NGC 4261) but viewed from a more edge-on direction (i ~ 78^deg^). The
northwest portion of the dust feature appears slightly warped, and its
tip points toward the north. There is enhanced emission immediately
northeast of the nucleus, along the minor axis of the dust structure and
extending out to the edge. Its morphology is roughly conelike. A very
weak, possibly pointlike nucleus is detected at the center of the disk.
The radio jet points in a direction roughly orthogonal to the major axis
of the dusty feature. Several globular clusters are detected in the
outer halo. A small spiral galaxy is located 21" (10 kpc) to the east,
while a massive lenticular galaxy lies only 34" (16 kpc) to the south.

7. 1998ApJS..114..177Z
Re:3C 296
3C 296.--This galaxy is a relatively normal elliptical galaxy of FR I
morphology. The F702W image shows a close neighbor at a distance of ~30";
however, no isophotal twists, arms or bridges are visible, which may imply that
these galaxies are only close in projection. The image of the inner regions,
however, show some peculiarities, which may suggest that 3C 296 also has a gas
and dust disk. Again, as mentioned previously, nuclear disks of gas and dust
may play a central role in the feeding massive black hole at the center of the
AGN. No UV flux was detected after 900 s integration with the F220W filter
(this yields a maximum magnitude of 19.22).

8. 1976RC2...C...0000d
Re:NGC 5532
= 3C 296
= 4C 10.39
Brightest in a group.
Often misidentified as IC 5532.
P.A.S.P., 80, 129, 1968.
Photometry (UBVR):
Ap. J., 145, 1, 1966.
Ap. J., 178, 25, 1972.
Ap.J., 183, 731, 1973.
Ap. J., 145, 1, 1966.

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