Date and Time of the Query: 2019-05-24 T04:31:18 PDT
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Notes for object 3C 321

14 note(s) found in NED.

1. 2008ApJS..175..423P
Re:3C 321
3C 321 (Figs. 44 and 45) has the ELR aligned with the radio source. Because of
the dust lane (noted in Martel et al. 1998) determining the proper center of the
host galaxy is problematic.

2. 2006ApJS..164..307M
Re:3C 321
This galaxy shows a clearly visible dust lane on our near-infrared image. A
companion in the process of merging (Roche & Eales 2000) is located 3.5" to
the northwest and is elongated toward the central source along the radio axis.
Bright knots of emission are present along the northern border of the dust lane
on the UV image (Allen et al. 2002).

3. 2006ApJ...642...96E
Re:3C 321
Single-component models provided poor fits to the spectrum, with noticeable
residuals at high and low energies, together with a residual at ~6 keV,
suggesting the presence of Fe K{alpha} line emission. The first moderately
acceptable fit ({chi}^2^ = 19.2 for 9 dof) was achieved with an absorbed [N_H_ =
(8.7+/-5.7) x 10^21^ atoms cm^-2^] power law, a Gaussian Fe K{alpha} emission
line, and a thermal component of temperature 0.57+/-0.04 keV. However, positive
residuals at energies >~4 keV were noticeable, suggesting the presence of
heavily absorbed emission. A model consisting of a heavily absorbed power law of
photon index frozen at 1.7, a strong Gaussian Fe K{alpha} line of equivalent
width ~1 keV, a second unabsorbed power law of photon index frozen at 2, and
thermal emission of temperature 0.49+/-0.15 keV and normalization
1.33^+0.53^_-0.4_ x 10^-6^ provided the best fit to the data ({chi}^2^ = 9.8 for
eight dof). Although the photon indices are frozen at their canonical values
(because of the relatively small number of bins [14] and large number of free
parameters), the parameter uncertainties are large.

4. 2005ApJ...618..635G
Re:3C 321
1529+24 (3C 321) (figure not included)
This narrow-line FR II radio galaxy shows two symmetric lobes with
hot spots and a faint jet in the northwestern direction. Only a
pointlike core is visible in our VLBA map. From the core dominance,
we find that high-velocity jets agree with observational data only if
{theta} is 45^deg^-70^deg^. This relatively large orientation angle
is consistent with the lack of a visible broad-line region.

5. 2002ApJS..139..411A
Re:3C 321
3C321.-The UV image of 3C 321 (Fig. 24a) is spectacular. UV emission
spans the entire region covered by the two galaxies seen in the optical
image (Fig. 24b) showing bright clumps and V-shaped structures. The
brightest UV emission occurs along the northern edge of the dust lane in
the southern galaxy, and the brightest knot is coincident with the
partially obscured nucleus. At least three bright knots can be
discerned in this arc of emission that outlines the edge of the dust
lane. UV emission blobs are detected curving up from the western end of
the dust lane toward the northern galaxy. From the UV image it is
impossible to clearly demark the object into two separate
galaxies. South of the dust there is a group of UV emission knots
embedded in a diffuse irregular ring feature. Some of the knots in this
structure have corresponding features in the optical image, but others
do not. (This feature is very suggestive of a three-dimensional cone
with its axis pointing out from the nucleus of the galaxy.) In contrast
to the relatively smooth and regular optical appearance of the
northern galaxy, the UV emission corresponding to the northern galaxy is
very irregular. The brightest region, centered on the northern galaxy
(northern nucleus), is V-shaped with the apex directed toward the
nucleus of the southern galaxy. Beyond the flare of the V-shaped
feature, there is more diffuse filamentary UV emission which has no
optical counterpart. At fainter levels the outline of the northern
optical isophotes of the southern galaxy is apparent in the UV image.
The radio jet emanates from the nucleus of the southern galaxy and
follows the P.A. which remarkably passes through the northern
neighbor. The spectroscopy of Robinson et al. (2000) shows that
redshifts of these galaxies are equal to within 200 km s^-1^, so these
systems are definitely physically related.

6. 2000MNRAS.317..120R
Re:3C 321
5.6 3C 321 (z=0.0961)
This blue, high surface brightness galaxy is detected by PISA as a
single source with a close alignment with the radio axis in both
passbands (ellipticity 0.255/0.281, PA 1469/1430 in VU respectively).
The double nucleus of 3C 321 (Fig. 10) can be split (by running
'PISAFIND' with DEBLEND and using a higher threshold) into two
components of V = 15.93 and 17.04, separated by 3.48 arcsec at PA 1255,
which is close to the radio axis. The two components are clearly
merging galaxies (the evidence for a merger-triggered starburst is
discussed in Section 9.3)
The radio source (Baum et al. 1988) is centred on the brighter
south-eastern nucleus, with hotspots ~ 150 arcsec on either side of the
galaxy, giving the second largest radio size in this sample. There is
also radio emission peaked at the north-western nucleus and extending in
a long jet ~ 35 arcsec beyond it. The jet direction is 11^deg^ clockwise
from the axis of the more distant hotspots and more closely aligned with
the two galaxy nuclei, implying that the north-western nucleus interacts
with, and slightly deflects, the radio jet.

7. 2000ApJS..129...33D
Re:3C 321
3C 321, z = 0.096. - The absorption map (Fig. 28) shows a disturbed
dust lane with some patches of emission at both far ends of the lane. At
the east the dust seems to divide itself up into three separate lanes.
The galaxy has a close companion to the northwest (distance ~ 5 kpc).
The radio source shows a radio jet of length 10". On larger scales, two
hotspots are seen, at a position angle differing by just over 10^deg^
from that of the radio jet.

8. 1999ApJS..122...81M
Re:3C 321
3C 321. - A beautiful, undulating dust lane bifurcates this galaxy at a
P.A. of ~ 60^deg^. Its total projected length is ~ 3.7" (6.8 kpc) and at
approximately 1.5" southwest of the nucleus, it breaks up into two
separate strands. A significant fraction of the light from the southern
regions of the galaxy is blocked by the dust, and the southern isophotes
are therefore more knotty and irregular than their northern
counterparts. A nearby companion galaxy is also visible 3.5" (6.4 kpc)
to the northwest. The radio jet is oriented at a nearly orthogonal angle
to the dust lane.

9. 1998ApJS..114..177Z
Re:3C 321
3C 321.--This peculiar galaxy has two nuclei (Heckman et al. 1986; Baum et al.
1988), where that in the northeast is brighter and more closely coincident with
the location of the radio core. The F702W image shows that the other nucleus is
composed of two blobs. Baum et al.'s emission-line image (in H{alpha}+[N II] is
S-shaped and appears to pass through those two blobs. Perhaps 3C 321 could have
a large disk? Also, Baum et al.'s 20 cm VLA map shows a jet emanating from the
core to the northwest that points toward the arc of the line-emitting gas. The
UV (F320W) image strongly resembles the structure of the optical image, with
the main difference being that the optically brighter nucleus is fainter in the
UV. Since Baum et al.'s emission-line gas is also brighter in the UV brighter
nuclei and structurally resembles that of a double-blobbed nucleus, it is
likely that the hot stars seen in the UV photoionize that gas. A further
difference is that the northern blob of the southeastern nucleus seems to
consist of two blobs (there is a weak indication of this in the F702W image).
Another unusual aspect of 3C 321 is that the narrow-line spectra of the nuclei
have identical line strengths and surface brightnesses (McCarthy, Spinrad, &
van Breugel 1995). McCarthy et al. consider a number of possible explanations
for the identical line spectra but conclude that photoionization by the
nucleus, that coincides with the radio core, is the most likely mechanism.
However, we performed PSF fits all the nuclei (while masking the others) and
did not detect any nuclear UV emission that is in excess to that expected for
normal elliptical galaxies.

10. 1995ApJS...99...27M
Re:3C 321
3C 321 (z = 0.09; Fig. 2) -This object has a large complex of extended
line emission. Spinrad et al. (1985a) list 3C 321 as having a double
nucleus. In our H{alpha} and continuum images the secondary peak is not
well resolved. An image with a larger field is given in Baum et al.
(1988). The continuum image presented here was taken with a narrow-line-
free filter. This image shows that the H{alpha} emission in both the
nucleus and the knot to the east is spatially offset from the continuum.
The most unusual aspect of this object is that the narrow-line spectra of
the nucleus and the knot have identical line strengths and surface
brightnesses (van Breugel, McCarthy, & Spinrad 1995). Van Breugel et al.
consider a number of possible explanations for the identical line
spectra, but conclude that photoionization by the nucleus (as defined by
the radio core) is the most likely mechanism. A low-resolution radio map
is given in Leahy & Williams (1984).

11. 1994ApJS...91..491G
Re:3C 321
1529+242 (3C 321) - This galaxy has steep-spectrum radio emission on
arcsecond as well as arcminute scales (Baum etal. 1988).

12. 1994AJ....107...35H
Re:IRAS 15295+2414
15295+2414 (3C 321). The double nuclei of this well-studied galaxy
(e.g., Filippenko 1987) have optical spectra characteristic of Seyfert
type 2 galaxies. The nuclei are separated by 3.1 arcsec, corresponding to
a linear projected separation of ~6 kpc [Fig. 15(q)]. The brighter
nucleus n1 is a flat-spectrum compact radio source with a one-sided jet
containing a steep spectrum radio knot near the second nucleus (Kuhr et
al. 1981). A low surface brightness tail extends to the south of the
galaxy, and the object to the north is a foreground star. 3C 321 is the
most distant galaxy among the previously identified 60PKs.

13. 1974ApJ...191...43K
Re:3C 321
Probable new identification with starlike image on 200-inch
red image-tube plates within about 5 arcsec optical uncertainty
at unpublished radio position by Adgie and Gent.
We assume that badly discrepant (33 arcsec) position by
Wyndham, J.D. (1965) A.J., 70, 384.
is in error.
Candidate not seen on 48-inch IIIa-J,
suggesting it is either red or variable.

14. 1965AJ.....70..384W
Re:3C 321
A faint red object, m_pg_~21, 16" S 16" E of the radio position, is the only
object visible within the search area.

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