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Notes for object 3C 111

10 note(s) found in NED.

1. 2007A&A...461.1209D
Re:3C 111
3C 111: Lewis et al. (2005) reported the possible detection of a broad
iron emission line in the spectra of the source using simultaneous
XMM-Newton and Rossi XTE data. Alternatively, the authors speculated
that the curvature of the X-ray spectrum could be either to a truncated
accretion disk or to a blob-like complex absorber. The analysis of the
BeppoSAX data presented here cannot distinguish between these scenarios,
and the X-ray spectrum of the source is well fit, adding a reflection
component to the power law-like continuum.

2. 2006ApJS..164..307M
Re:3C 111
This galaxy has a very bright nucleus with the host clearly visible. 3C 111 is
an elliptical elongated north to south.

3. 2005AJ....130.1418J
Re:3C 111
The innermost jet of this galaxy exhibits strong activity. At least
seven moving components (B1-B7; see Fig. 16) can be identified inside
1 mas of the core. These knots move ballistically at a typical
apparent speed of ~3c. There are two bright features near the core,
A1 and A2, that are stationary according to the {chi}^2^ test. The
most prominent feature of the jet is an extended, polarized blob
northeast of the core. The feature appears to be associated with a
major outburst observed at 90 GHz in 1996 January (Alef et al. 1998),
at 37 GHz in 1996 March, and at 22 GHz in 1996 August (Terasranta et
al. 2004). The first ejection around this time appears to have
occurred earlier than the derived epoch of ejection T_0_ (see
Table 5), since complex structure of the core region was detected
already in a 43 GHz VLBI map obtained in 1996 July (Alef et al.
1998). This implies slower motion of the disturbance near features A1
and A2, which agrees with the description of the structure by Alef et
al. (1998) as "a mix of dimming and flaring of stationary and moving
emission components." In our observations we identify the brightest
part of the outburst remnant as C1, which moves ballistically at a
higher apparent speed than that of the innermost components. Knots c1
and c2 detected behind C1 seem to belong to the same disturbance. At
the last three epochs the parameters of C1, c1, and c2 are obtained
after tapering the images by reducing the weighting of the data from
the longest baselines and are not used to compute the jet velocities.

4. 2003ApJ...589..126Z
Re:3C 111
3.3. 3C111 The RM image for this radio galaxy was published in Zavala &
Taylor (2002). No reliable RMs could be determined for the core
because of a weak-to-nonexistent polarization at 12 and 8 GHz. The jet
had an RM of -750 +- 61 rad m^-2^ at 3 mas east of the core, which
decreased to -200 +- 56 rad m^-2^ at 5 mas east of the core. A positive
spectral index coincides with the depolarized core of this radio galaxy
(Fig. 5). The E-vectors are well ordered along the jet.

5. 1999ApJS..122...81M
Re:3C 111
3C 111. - This has been detected as a faint, slightly resolved source
with ground-based imaging (Colina & Perez-Fournon 1990) with no
information about the morphology and structure of the host.
Unfortunately, our WFPC2 image is not significantly more informative. We
find that the optical counterpart to 3C 111 is a very small
elliptical-like galaxy strongly dominated by a bright, pointlike nucleus
with very faint underlying fuzz. As for 3C 98, the two radio hotspots
(Leahy et al. 1997) are located off the WFPC2 field.

6. 1998AJ....115.1295K
Re:3C 111
0415+379.--While 3C 111 appears clearly one-sided at 2 cm, higher resolution 7
mm observations indicate that the apparent double structure seen at the west end
of the 2 cm jet breaks up into a more complex multicomponent symmetric
configuration with no obvious component that can be identified as the core (Alef
et al. 1998). Our multiepoch 2 cm observations suggest motion toward the east.

7. 1998A&AS..131..451R
Re:3C 111
This is a classical double-lobed FRII radio-source with an extended jet
in PA ~-45^deg^ (Preuss et al. 1990). Components are seen moving out
from the core at superluminal velocities ~1mas/year. In Fig. 3 we
present the highest resolution map of this source available to this
date. The core is unresolved and there is a weak component in the same
PA as the mas scale jet at a distance of 0.5mas. The result from model
fitting Gaussian components to the UV data can be found in Table 6.
The Gaussian model fit clearly substantiates the general structure
presented in the hybrid map. With only one epoch we are unable to
determine whether the superluminal motion seen at lower frequencies
(Preuss et al. 1990) is present on {mu} as scales. Further observations
are needed to detect the possible proper motion of components in this

8. 1997MNRAS.291...20L
Re:3C 111
4.4 3C 111
3C 111 is a broad-line radio galaxy with strong X-ray emission (e.g. Nandra &
Pounds 1994). An optical image is given by Colina & Perez-Fournon (1990).
3C 111 has a prominent straight jet (N 1) reminiscent of those in higher-power
quasars. It has previously been mapped at high resolution by Linfield & Perley
(1984, hereafter LP84). The core of the source is very bright (around 1.2 Jy)
and variable (its flux increased by 100 mJy between the epochs of our B- and C-
configuration observations), and difficulties in correcting for this in
multi-epoch, two-pointing observation account for the high level of noise on
the total-intensity images. The core appears to be ~1 per cent polarized; this
is not simply an instrumental effect, as it is polarized in the same intensity
and position angle on maps made from the two different VLA pointings.
The large-scale structure is best seen in the low-resolution image of Leahy &
Williams (1984). The hotspots, core, and jet are embedded in a large-scale
halo, the brighter parts of which are visible in Fig. 10. The halo is sharply
bounded to the southeast and west, and the southern hotspot complex is sited at
the tip of the structure. The main part of the halo is also bounded by a sharp
brightness drop to the north-east, and the northern hotspot and its following
tail form a promontory in this border. Very faint emission continues around and
well ahead of the northern hotspot. A similar case of a hotspot with faint
emission ahead of it is found in another broad-lined object, 3C 390.3. It is
plausible that the structures of both are significantly distorted by
projection, which would also explain why their bridges are continuous across
the host galaxies.
The jet is longitudinally polarized (i.e. the B-field is perpendicular) in the
few places where polarization can be detected, mainly just as it enters the
bright tail behind the hotspot (i.e. before the knot N2, see Fig. 11). Faraday
rotation is low in this object, despite its low Galactic latitude (Leahy,
Pooley & Riley 1986), and so this unusual orientation can be confirmed on the
1.4-GHz map of LP84. The low-resolution map of Leahy et al. suggests a more
normal parallel-field orientation about halfway between core and hotspot. The
jet can be traced into the centre of the hotspot tail, but at knot N2 the
ridge-line splits (this is also visible on the LP84 maps). Until this point the
jet is narrower than the hotspot. It is not clear whether the splitting
represents a broadening of the jet to about the width of the hotspot or whether
one of the ridges represents the true jet.
There is no sign of a jet in the southern lobe. The southern hotspot complex is
a canonical double, i.e, it has a recessed compact primary (S1) and a more
diffuse secondary (S2) at the lobe tip (Fig. 13). Although S1 is only slightly
resolved in this tapered image, a `B'-configuration-only image (with about
twice the resolution) shows little extra compact structure.

9. 1995ApJ...447..121W
Re:3C 111
3C 111.-We find no features or complexity. The HEAO 1 upper limits for
the Fe K EW and N_HFe_ are consistent with Ginga (NP4).

10. 1991ApJ...381...85T
Re:3C 111
This source has a flat spectrum both in this analysis and in the EXOSAT
data, although earlier HEAO 1 data indicated a "canonical" spectrum. This
spectral change is significant at better than 99% cofidence (Fig. 3).

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