Date and Time of the Query: 2019-04-23 T16:05:24 PDT
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Notes for object IC 4296

20 note(s) found in NED.

1. 2009ApJ...703.1034Y
Re:IC 4296
The 0.3-10 keV X-ray spectrum of this source consists of two components, a power
law that dominates above 1 keV with photon index {GAMMA} = 1.48^+0.42^_-0.34_
and soft thermal emission with kT = 0.56^+0.03^_-0.03_ keV that dominates below
1 keV. Since the thermal component likely comes from the host galaxy background,
we only adopt the hard power-law component. The accretion rate required in our
model is roughly consistent with the Bondi accretion rate derived by Pellegrini
et al. (2003b).

2. 2006ApJ...639..136H
Re:IC 4296
IC 4296. We extracted the spectrum from a 1.5' (22 kpc) aperture, omitting
data from the vicinity of the central LLAGN. We found that the addition of
an extra hot gas component significantly (delta chi^2^ = 11) improved the
fit. The gas components had kT = 0.7 and 1.3 keV. Our results are in
excellent agreement with Z_Fe_ derived from ASCA (Buote & Fabian 1998).

3. 2006A&A...447...97B
Re:IC 4296
IC 4296: Pellegrini et al. (2003) found point-like and hard X-ray emission, well
described by a moderately absorbed (N_H_ = 1.1 x 10^22^ cm^-2^) power-law with
{GAMMA} = 1.48.

4. 2005A&A...440...73C
Re:IC 4296
IC 4296: the circum-nuclear dusty disk seen in the optical HST images (Laine et
al. 2003) affects only marginally the NICMOS image used by us. The central 0.4"
are flagged due to the presence of a point source.

5. 2004MNRAS.347..771W
Re:PKS 1333-33
3.4.12 1333-33 (IC 4296) There is no obvious UV excess detected in this
source. The best fit to the continuum is achieved with just an old
stellar population (12.5 Gyr, {chi}^2^ = 0.939). The fit is not improved
with the addition of a young stellar component. Only the [O II] line is

6. 2001ApJ...550..503J
Re:IC 4296
Abell 3565 (IC 4296). - IC 4296 has a compact dust ring close to the
nucleus, but no sign of dust outside of a radius of 1.5". Very small
residual spatial variance corrections (P_g_) bring the annuli into nearly
perfect agreement. The S/N of this measurement is high and the GC
correction small.

7. 2001AJ....121..808C
Re:IC 4296
IC 4296. - The color map reveals large dust patches around the center
and some indication of a disk. IC 4296, an FR I radio galaxy, was detected
by IRAS at 60 and 100 microns (Knapp et al. 1989).

8. 2001A&A...380..471B
Re:IC 4296
1333-337 - IC 4296, our value of sigma is lower than the mean value quoted
by Hypercat (340 km s^-1^). The agreement is better with the measure of
Franx et al. (1989). From our spectrum, taken at PA = 60^deg^ we measure a
rotation of ~71 km s^-1^ in agreement with data taken at the same position
angle by Saglia et al. (1993).

9. 2000A&AS..143..369G
Re:PKS 1333-33
1333-337: A regular elliptical galaxy located at the center of cluster
Abell 3565. Optical emission lines were detected within few arcsec of
the nucleus (Goudfrooij et al. 1994).

10. 1994CAG1..B...0000S
Re:IC 4296
IC 4296 Group
April 6/7, 1981
75 min
IC 4296 is the brightest galaxy of a loose group having more than
ten possible members. The mean redshift of the known members is
= 3648 km/s. Coordinates and individual redshifts for some of the
members are given elsewhere (Sandage 1978).

11. 1994A&AS..105..341G
Re:IC 4296
H{alpha}+[NII] emission detected in the inner 5". No obvious dust
absorption. Detected by IRAS at 60 and 100 microns. Bright, extended
radio source. X-ray emission.

12. 1994A&AS..105..211S
Re:[KWP81] 1333-33
The lobes of the radio source 1333-337 (IC 4296, Killeen et al. 1986),
which had previously been listed as the individual sources 1332-33 and
1334-33 (Kuehr et al. 1981a), have been removed from the 1 Jy

13. 1994A&AS..104..179G
Re:IC 4296
Regular elliptical from the surface photometry. Note its constant PA in
view of its low ellipticity. Detected by IRAS at 60 & 100 microns. Bright,
extended radio source. X-ray emission.

14. 1993MNRAS.263.1023M
Re:IC 4296
1333-33 (IC 4296). This radio galaxy has aspects of both FR I and FR II:
bright symmetric jets but lobes with 'warm' rather than 'hot' spots.

15. 1993MNRAS.263..999T
Re:PKS 1333-33
1333-33 (IC 4296). Weak H{alpha} + [N II] is detected, but no [O III]
{lambda}5007 or [O II] {lambda}3727. The continuum spectrum is typical of
early-type galaxies.

16. 1992ApJS...80..137J
Re:MRC 1333-337
MRC 1332-336*1333-337*1334-339
All merged in a complex source,
showing a strong slightly-bent bridge or jet between two diffuse lobes.
The bridge shows double structure (inner lobes) near the centre, but
not a distinct core. The lobes are edge-brightened although it is
an intrinsically weak radio source. Mapped by Gardner
& Whiteoak (1971), SM, Goss et al. (1977), Slee (1977), Swarup (1984),
Killeen et al. (1986) and Ekers et al. (1989).
Galaxy 11.0 m, IC 4296, at 13 33 47.52 -33 42 42.4,
between the two inner radio peaks and 45 arcsec from the centroid, see
Mills et al. (1960). z = 0.0124, Sandage (1978).
In cluster A 3565 (ACO).

17. 1985SGC...C...0000C
Re:IC 4296
Plate 1375
Overexposed. Trace of structure? Optical pair at 6.2 with IC 4299.
Brightest (or superposed on) cluster.
Plate 1449
Brightest in cluster. Optical pair with IC 4299 6' south-south-following.

18. 1982ESOU..C...0000L
Re:ESO 133347-3342.7
=ESO 383- G 39
in cluster

19. 1976RC2...C...0000d
Re:IC 4296
= PKS 1333-33
Brightest of a group.
P.A.S.P., 80, 129, 1968.
Photometry (UBV):
A.J., 74, 335, 1969.
Ap. J., 178, 1, 1972.
Magnitude and colors reduced using dimensions on POSS:
(3.9 arcmin x 3.9 arcmin).

20. 1964RC1...C...0000d
Re:IC 4296
H.A. 88,2 dimensions: 0.6 arcmin x 0.6 arcmin (series a').
M.N.R.A.S., 112, 606, 1952.

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