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Date and Time of the Query: 2019-05-22 T22:51:09 PDT
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Notes for object 3C 105

7 note(s) found in NED.


1. 2008ApJ...678..102A
Re:SWIFT J0407.6+0336
XRT observed this source field for 7 ks on 2006 July 11. The only detected
object, at R.A. (J2000.0) = 04^h^07^m^16.2^s^, decl. (J2000.0) =
+03^deg^42^'24.3", is coincident with the Seyfert 2 galaxy 3C 105.0 and 4.7'
distant from the BAT position. This is the first time that 3C 105.0 has been
detected in X-rays.

2. 2008ApJ...673...96A
Re:3C 105
3C 105.0 is a Seyfert 2 galaxy. The BAT and XRT data can be fit by an absorbed
power-law model with a photon index of 1.65+/-0.13 and a hydrogen column density
of 29.4^+5.7^_-4.8_ X 10^22^ atoms cm^-2^. Given its absorption and its
luminosity (4.45 x 10^44^ ergs s^-1^), 3C 105.0 is a highly absorbed highly
luminous QSO.

3. 2006ApJS..164..307M
Re:3C 105
Highly flattened elliptical, faintly disturbed. A faint unresolved source is
visible 4" to the west-southwest off the nucleus.

4. 1999AJ....118.1963C
Re:3C 105
3C 105 is the only object in our sample that shows no evidence of
polarization, with p < 0.8% (3 {sigma}). The galaxy is exceptionally
red, with strong stellar absorption lines (Tadhunter et al. 1993). The
Keck spectra are shown in Figure 10; the bottom panel is the spectrum
with a galactic template (corrected for reddening) subtracted. There is
no reliable indication of broad lines. 3C 105 has a typical FR II radio
morphology, with a weak core and prominent hot spots, and it is similar
to 3C 357.

5. 1997MNRAS.291...20L
Re:3C 105
4.3 3C 105
A low-resolution 6-cm map is given in Baum et al. (1988). The maps presented
here show the same features but in greater detail. The `hammerhead' structure
at the end of the northern lobe (Fig. 7) could be interpreted in terms of the
recent escape of the lobe from a sharply bounded halo around the host galaxy.
If so, the halo would have to extend out to 270 kpc (more, allowing for
projection). This is not entirely implausible since 3C 105 is the most isolated
of all the radio galaxies studied by Prestage & Peacock (1988). The hotspot N1
is the only compact structure in the lobe, and can be seen in the
highest-resolution contour map (Fig. 8) to be extended approximately
north-south.
The southern hotspot complex (Fig. 9) dominates the source, to the extent that,
in the 1.4- and 5-GHz VLA snapshot images by Neff, Roberts & Hutchings (1995),
only this region and its bright tail were detected, causing them to
mis-identify it with the core. (Their maps at 0.35-arcsec resolution show the
main features seen in our higher-sensitivity map.) A linear feature, S1, points
into an extended peak S2 which merges with the compact component S3. A ridge of
emission connects S3 with the bright resolved component S4. There is also
complex structure in the fainter emission to the west, including at least two
more features which qualify as distinct. The obvious interpretation is to view
S1 and perhaps S2 as jet emission, S3 as a jet termination hotspot and S4 as a
recent disconnection event as discussed by Cox, Gull & Scheuer (1991). The
curved overall shape of the complex lends some credibility to this
interpretation. In our image S3 is just merged with S2 at the half-power level,
and the combined overall size is actually slightly larger than S4, so
apparently this interpretation involves the jet entering the secondary rather
than the primary hotspot. However the beam-shaped structure of S3 suggests that
it is poorly resolved, so that at higher resolution the half-power contour
probably would not include S2; thus S3 is probably the true primary. The main
problem with this model is that following S1 away from the hotspot complex, it
continues to curve and appears to end by pointing into the presumed backflow
structure in the lobe rather than into the core. Conceivably, the jet is
superposed on a relatively collimated backflow. The wealth of other knots and
structure in the complex is in any case suggestive of a rapidly evolving,
transient system.
Both the hotspot complexes in 3C 105 are remarkably compact, given the overall
size of the source.
The host galaxy is a typical NLRG with only nuclear emission lines (Baum et al.
1988; Smith & Heckman 1989; Tadhunter et al. 1993).

6. 1993MNRAS.263..999T
Re:PKS 0404+03
0404+03 (3C 105). Strong [O III] {lambda}{lambda}5007,4959 lines are
detected, as well as weak H{beta}; Curiously, [O II] {lambda}3727 is not
detected. This may indicate an unusually high ionization state or a large
reddening. The continuum colours appear typical of early-type galaxies,
although there are no clear detections of stellar continuum features.

7. 1974ApJ...191...43K
Re:3C 105
Empty to limit of all available shallow plates.
Possible smudge at radio position on a poor 200-inch image-tube plate.
Needs confirmation.


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