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Date and Time of the Query: 2019-05-25 T07:08:14 PDT
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Notes for object 3C 299

11 note(s) found in NED.


1. 2008ApJS..175..423P
Re:3C 299
3C 299 (Figs. 38 and 39) has aligned emission-line and radio morphology. Both
the emission-line region and the radio source are asymmetric about the center of
the host galaxy.

2. 2004MNRAS.347..508G
Re:3C 299
3.1.3.7 Source 3C 299 (Fig. 27) The source is the least luminous in all
of the samples. The source shows a large change in rotation measure
between the lobes, but the difference is probably due to the small
number of pixels with rotation measure information in the north-eastern
lobe.

3. 2002AJ....124.1239H
Re:3C 299
3C 299: Due in part to the large lobe length asymmetry
of this source, the eastern lobe of this source was once
thought to be a separate compact steep-spectrum source, which
is why many maps show only the eastern component. Using the
core position from the L-band map of Leahy, Bridle, and Strom,
the L-band map of Liu, Pooley, & Riley (1992) was used for
FR measurements because the L-band map of Leahy et al. is
probably undersampled. The Q-values from these two maps
differ by 17%, probably due to differences in resolution.
The Q-value from the higher resolution map of Leahy et al.
is listed in Table 1.

4. 1999ApJ...526...27D
Re:3C 299
3C 299.-[O III], z = 0.367. This source has a very asymmetric radio
structure, with lobe-nucleus separations of 2.6" and 13", respectively
(Liu & Pooley 1991; van Breugel et al. 1992). Thus, 3C 299 is not a true
CSS source. These images show the closer lobe, in which prominent line
emission is detected. The filamentary or shell-like structures to the
northeast are due to line emission, whereas most of the underlying host
galaxy is continuum emission (I_cont_). Because of problems with precise
image alignment, however, some of the filamentary structure is still
present in the continuum image.

5. 1997ApJS..110..191d
Re:3C 299
3C 299 (galaxy, z = 0.367, m_F702W_ = 19.64).-The HST image shows complex
structure including a system of arcs or filaments to the northeast of the
multimodal structure around the galaxy nucleus. The radio source is
actually an asymmetric double with a separation of ~13" (Liu & Pooley
1991; van Breugel et al. 1992) and is larger than the cutoff for CSS
sources. The radio component overlaid on the HST image is the brighter
east lobe. The optical center is taken to be the brightest spot in the
lower right-hand corner. From maps presented in Liu & Pooley, we measured
a core-lobe distance of ~2.6" in P.A. of ~60^deg^, with large
uncertainties. Since the scale of our optical/radio map is only
4" x 4", there is some freedom in positioning the lobe relative to the
core by varying the position angle slightly. The radio core is not
visible in the radio map we used (1.7 GHz VLBI; Spencer et al. 1991), but
since the radio core is taken to coincide with the optical center we can
define both the radio and optical axes. We measured an alignment angle of
8^deg^. This value is not as accurate as in other sources; lobe
positional uncertainty gives rise to a 1 {sigma} error of ~10^deg^.

6. 1996ApJS..106..247C
Re:3C 299
3C 299 (z=0.367; Figs. 16 and 17).--[O III] {lambda}5007 and R images are
shown in Paper I. We obtained spectra both at Lick and Palomar at position
angle 70^deg^. The spectra show that the peak [O III] {lambda}5007 emission is
offset from the continuum peak. The velocity field is complex, but the
amplitude is not large.

7. 1995ApJS...99...27M
Re:3C 299
3C 299 (z = 0.367;Fig. 18).-This object has very high surface brightness
both in the continuum and in [O III]. The continuum is highly elongated
and is aligned with the radio source axis. The [O III] image shows strong
emission extended over ~10". The radio source is quite asymmetric
(Pearson, Perley, & Readhead 1985; van Breugel & McCarthy 1995).The
region of highest surface brightness [O III] emission is offset from the
nucleus toward the northeast, the direction of the closer lobe. In many
respects this object resembles the high-redshift (z > 1) radio galaxies,
and yet it is at a rather low redshift.

8. 1995A&AS..112..235A
Re:3C 299
3C299 (1419+41)
Liu and Pooley (1991) and van Breugel et al. (1992) find a central
component near to the northern component. This confirms that this source
is an asymmetric double radio galaxy with a total extent of about 35 kpc
across and should not really be classed as a CSS source. Liu and Pooley
(1991) also find strong depolarization at 20 cm in the northern component
and suggest that this is caused by line emitting gas to the north-east of
the core (McCarthy et al. 1991).

9. 1992MNRAS.257..545L
Re:3C 299
Two components are visible on the low-resolution maps of this source, the
south-western lobe (Y) and the brighter component X. Component X is noted
by Kiley & Pooley (1975) as being coincident with the probable
identification. They postulated that there might be a faint lobe north-
east of the source below the sensitivity of their observation. Such a
lobe is not visible in the current observations with high dynamic range.
Indeed, our high-resolution observations show a core (~ 1 mJy at 5 GHz,
marked A in Fig. 17a) lying on the source axis about 3 arcsec from
component X. We believe that the component A is coincident with the
identification and the brighter component X is the Nf lobe of this double
source. The source is thus highly asymmetrical with respect to the
position of the identification, like 3C254.
There are two galaxies between the brighter component X and the core A.
The position listed by Kiley & Pooley and marked as a cross on the maps
is the average position of the two galaxies. The radio core is within the
uncertainty of the position given by Kiley & Pooley.
The Nf component appears compact in the low-resolution observations and
shows little variation in spectral index across it, leading to a high
velocity, 0.2c.

10. 1992A&A...256...56v
Re:3C 299
3C 299 (Fig. 19): This source has a secondary component at 12" to the SW
which has 5% of the flux density of the main component. Both components
are clearly extended along the source major axis (Fig. 4). Observations
at 8.4 GHz (van Breugel et al. in preparation) show a faint, compact core
2" SW of the brightest component. Thus the source is a very asymmetric
double with the brightest lobe being the CSS component. At 15 GHz this
bright lobe is ~10-15%+/-2% polarized.

11. 1974ApJ...191...43K
Re:3C 299
Brightest member of faint cluster
on basis of 2 arcsec position agreement.
The present identification is same as
Wyndham, J.D. (1966) Ap. J., 144, 459.
and confirmed by
Veron, P. (1966) A.J., 144, 861.
Redshift by Spinrad and Smith (1973) of z = 0.367.


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