Date and Time of the Query: 2019-03-21 T19:33:42 PDT
Help | Comment | NED Home

Notes for object NGC 6166

26 note(s) found in NED.

1. 2010A&A...516A...1L
Re:3C 338
3C 338 in Abell 2199. A2199 ( z = 0.0304) has a prototypical cooling core. A
Chandra observation of this cluster has detected a point-like source coinciding
with the center of the galaxy NGC 6166 (Di Matteo et al. 2001), which is a
multiple nuclei cD galaxy. This galaxy hosts the relatively powerful radio
source 3C 338, which emits a total power at 330 MHz of Log P ~ 25.64 W/Hz. This
radio source has been known for a few decades to have an unusual structure on
both large and small scales (Feretti et al. 1993; Giovannini et al. 1998). It is
classified as a FR I radio source and shows central optical [O III] line
emission (Fisher et al. 1995). On kiloparsec scales 3C 338 has two symmetric
extended radio lobes, characterized by a steep spectrum ({alpha} ~ -1.7) and
misaligned with the central emission. The two radio lobes are connected by a
bright filamentary structure. Polarimetric observations by Ge & Owen (1994)
revealed strong rotation measure gradients across most of the extended emission
and inferred the prese nce of cluster magnetic fields. Both the steep radio
spectrum and strong filamentary emission may be caused by interactions with the
dense intracluster medium (Gentile et al. 2007).
On parsec-scales, 3C 338 has a compact radio core with two short (~10
pc), symmetric jets. In VLBA maps at 5 GHz (Feretti et al. 1993), the
parsec-scale structure shows a central dominant feature (the core emission) with
flux density ~92 mJy/beam and two symmetric jets. The total flux density is 133
mJy. The eastern jet shows a couple of low-brightness regions in its center
suggesting it could be limb-brightened. The orientation of this structure
appears to be very constant in time despite the complex dynamic conditions
present in the 3C 338 central regions. Comparing maps obtained at different
epochs (Gentile et al. 2007), a change in the parsec-scale morphology is clearly
evident and is probably correlated with the arcsecond core flux density
variability. The structural changes suggest the presence of proper motion with
{beta} ~ 0.4 h^-1^ on both sides of the core (Gentile et al. 2007). These
properties suggest that the extended emission in 3C 338 is a relic structure
that is not related to the present nuclear activity (Giovannini et al. 1998).

2. 2008MNRAS.391.1009L
Re:NGC 6166
NGC 6166: this is a classic multiple nucleus cD galaxy in a rich cluster. The
surface brightness profile was published by Schombert (1986). Carter et al.
(1999) found the velocity dispersion of this galaxy to increase from 325 km
s^-1^ at the centre to 450 km s^-1^ at 35 arcsec along the MA. They also found
the galaxy to show modest MA rotation (45 km s^-1^ at 40 arcsec). The profiles
derived here do not extend out to the radii necessary to confirm the positive
velocity dispersion slope found by Carter et al. (1999). Rotation of the order
of 31 km s^-1^ is found in the centre of the galaxy, although this is not a very
clear rotation curve.

3. 2008ApJS..177..148F
Re:3C 338
4.2.10. 3C 338 (Abell 2199; NGC 6166); z = 0.030354 An FR I radio source in a
dense environment. Two companions are prominent on the NICMOS image. The
elliptical host galaxy is disturbed, with a dust lane crossing the nucleus,
faintly visible in the IR. First published by Jensen et al. (2001); see also
Ravindranath et al. (2001).

4. 2006ApJ...642...96E
Re:3C 338
Simple one-component models of either thermal emission or a power law provided
adequate fits to the data ({chi}^2^ = 1.66 and 4.47 for 3 dof, respectively).
The best-fitting parameters for the power-law model are {GAMMA} = 2.37+/-0.81
with a 1 keV normalization 5.2^+2.1^_-2.1_ x 10^-6^ photons cm^-2^ s^-1^
keV^-1^. A radial surface brightness profile showed a clear excess of counts
over extended emission at distances < 1"; from the core, and so we adopt as the
best-fitting model for the nuclear spectrum a single unabsorbed power law. We
compared the results of my Chandra spectral fitting to a previously published
Chandra analysis of 3C 338 (Di Matteo et al. 2001). These authors found an
unabsorbed 1 keV flux density of (7+/-2) x 10^-15^ ergs cm^-2^ s^-1^ keV^-1^,
which is consistent with the value of (10.6 +/-2.8) x 10^-15^ ergs cm^-2^ s^-1^
keV^-1^ that we measure (errors here are 1 {sigma} for one interesting

5. 2005MNRAS.364.1253V
Re:NGC 6166
NGC 6166 is an elliptical and is located in a very busy field - it is the
dominant galaxy in the cluster Abell 2199. The presence of dust lanes is well
documented in the literature. We note that our SCANPI measurements are in good
agreement with those of Knapp et al. (1989). Using all available radio fluxes
from the literature we estimate that as little as 4 per cent or as much as 100
per cent of the 850-{mu}m flux from this elliptical may be due to synchrotron
contamination from a radio source associated with the galaxy (depending whether
a spectral index is assumed constant over the whole galaxy or whether it is
assumed to have a flatter core) - this is a preliminary analysis and discussion
of this and the other five ellipticals detected in the OS sample will be the
subject of a separate paper (Vlahakis et al. in preparation).

6. 2003A&A...403..889T
Re:3C 338
3C 338. A Chandra observation of the cluster A 2199 (December 1999) has
detected a point-like source coinciding with the center of the galaxy
NGC 6166 (Di Matteo et al. 200 1). The low count rate does not provide
a well constrained estimate of the parameters: for a power law model
we deduce {alpha}_x_ = 0.54^+0.56^_0.54_ and flux 1.8 X 10^-14^ erg
cm^-2^ s^-1^ (in the Rosat 0.54 energy band). However it has been found
that the value of the spectral slope rapidly increases with the hydrogen
column: for N_H,loc_ 2 x 10^21^ cn^-2^ , Di Matteo et al. obtain
{alpha}_x_ 1.9 and a flux {approx}2 times larger.

7. 2002ApJS..139..411A
Re:3C 338
3C 338. The UV emission of 3C 338 is dominated by two bright point
sources (see Fig. 26a). The brighter southern source coincides with
the nucleus of the galaxy. We also detect very faint emission from the
underlying galaxy star-light. The prominent optical dust feature
(Fig. 26h) can just be discerned in a smoothed version of the UV
image. The northern point source has a faint optical counterpart.

8. 2001ApJ...552..508G
Re:3C 338
1626+39 (3C 338). - We are monitoring this source because of its
two-sided structure and measured proper motion. Our last paper on this
source is Giovannini et al. (1998a).

9. 2001ApJ...550..503J
Re:NGC 6166
Abell 2199 (NGC 6166). - The central galaxy in A2199 has dust lanes
within 3" of the center. The dust lanes were masked prior to performing
the SBF analysis, but measurements in the innermost aperture are suspect.
The SBF analysis did not include the region between NGC 6166 and two
nearby companions, where the fit to the galaxy profile is not very good.
The fit to the power spectrum in the intermediate annulus was excellent,
but the outer two apertures disagree at a level (0.64 mag) that cannot be
corrected properly by adopting a value of P_g_ that scales with area. We
adopted the measurement in the intermediate aperture and a relatively
large range of permitted fluctuation magnitudes.

10. 2000ApJS..129...33D
Re:3C 338
3C 338 (NGC 6166), z = 0.0298. - This galaxy lies in the cluster
Abell 2199. The absorption map (Fig. 31) shows filamentary dust
structures. One arm of dust south of the nucleus has an S shape.
Northeast of the nucleus there is a second arm of dust. Some patches of
dust are also seen.
Figure 31 shows the central radio contours overlaid on the optical
image. Ge & Owen (1994) describe this unusually looking radio source in
detail. The optical component northeast of the radio core is related to
a weak radio component. 3C 338 was the first radio source in which a
two-sided jet was observed on parsec scales. South of the radio core a
part of the strange "ridge" first reported by Burns, Schwendeman, &
White (1983) is seen. There seems to be no morphological relation
between the dust arms and the radio source.

11. 2000A&AS..143..303D
Re:WN J1628+3932
This is the well studied galaxy NGC 6166 in the galaxy cluster
Abell 2199 (e.g. Zabludoff et al. 1993).

12. 2000A&A...362..871C
Re:NGC 6166
1626+39 (NGC 6166, 3C 338): Brightest galaxy of the cluster Abell 2199.
An unresolved nucleus is superposed on the flat core of the galaxy. An
arc-like dust feature extends from to nucleus to the West for ~ 3". Two
fainter elliptical companions are also present. (see Martel et al.

13. 1999MNRAS.310...30C
Re:B2 1626+39
B2 1626+39 lies in a cluster (A2 199), with a prototypical cooling flow.
Owen & Eilek (1998) conclude that the radio source is relatively young
and has been disrupted by the surrounding gas. The ROSAT HRI data set
for this source consists of two OBIs roughly 7 months apart. Only in the
second observation does the source appear extended, with two adjacent
peaks. We have taken this to be due to errors in the aspect correction
or processing effects and therefore have used only the first OBI in our

14. 1999MNRAS.309..969H
Re:3C 338
3.35 3C 338
This radio galaxy, located in the cluster A2199, shows a complex and
asymmetrical X-ray structure (Owen & Eilek 1998), and is also unusual in
the radio. Radial profiling is clearly not particularly appropriate, but
a simple application to the inner regions of the source gives the
decomposition tabulated here, which represents our best estimate of the
core contribution.

15. 1999ApJS..122...81M
Re:3C 338
3C 338 (NGC 6166). - NGC 6166 is a beautiful elliptical located in a
very rich group of galaxies. Two of its nearest neighbors are prominent
ellipticals at a comparable distances of 12" (7 kpc) to the east and
northeast of the nucleus, well within the halo of NGC 6166. A thin,
filamentary strand of dust is seen to meander across the core in a
general northeast to southwest direction. It is roughly S-shaped and is
much more prominent to the east of the nucleus. To the west, it
separates into two very faint but distinct filaments. The dust filament
intersects the central unresolved nucleus roughly at its halfway point.

16. 1998A&AS..128..153M
Re:GB2 1626+396
NGC6166; UGC10409. WSRT 1.4 and 5GHz maps in
Jaffe & Perola (1974A&A....31..223J). Physical parameters in
Condon & Broderick (1988AJ.....87.1064C)

17. 1997A&AS..126..335M
Re:B2 1626+39
1626+39 Using the 2.7 GHz polarization position angle in Parma & Weiler (1981),
we obtain a rotation measure of 116 rad m^-2^ (n=1, see Sect. 4.1).

18. 1995ApJ...438..539F
Re:NGC 6166
This is a dominant multiple-nucleus cD galaxy in Abell 2199. One of the
Mathews et al. (1964) cD prototypes, NGC 6166 is a strong radio source
(3C 338) and shows central optical [O III] line emission in our data.
Schombert (1987) classifies NGC 6166 as a low central surface brightness
cD galaxy. Based on Einstein and EX0SAT X-ray observations, Edge et al.
(1992) found that there is a gas inflow of 204 M_sun_ yr^-1^ in Abell
2199. Bertola et al. (1986) studied the stellar population and concluded
that a ~4% contribution of young early- to mid-O stars was needed to
model their IUE and optical spectra. McNamara & O'Connell (1992) found
color profiles indicative of dust lanes or dust features in NGC 6166.
Rood-Sastry cluster type: cD (Struble & Rood 1987).

19. 1986A&AS...64..135P
Re:B2 1626+39
Brightest member of Abell 2199. The peculiar radio morphology was
discussed by Burns et al. (1983). See also Jaffe and Perola (1974).

20. 1985ApJS...57..643D
Re:VV 364
Double-nucleus (about 10 arcsec apart) elliptical.

21. 1977A&AS...28....1V
Re:VV 364
Plate 3 Radio Nests of Spherical Galaxies
=MCG +07-34-060 = NGC 6166; 12.79m, the brightest member of the cluster
Abell 2199 is a well known radio galaxy 3C 338, its radio luminosity
being comparable to that of Virgo A.
VV 364a gives its position in the cluster, b, c and d frames, (scale
1mm=5.7"), obtained by Minkowski (1961) and the Burbidges (1962), using
decreasing exposures to show the structure of VV 364. Most interacting
galaxies, especially nests, should be studied in a similar way. VV 364
is a "mininest" composed of three galaxies. Minkowski (1961) studied
this object photometrically and spectroscopically and states: "The
bright nuclear region typical for galaxies of types E and S0 is absent.
Traces of structure or dust in the central mass on the southern side.
It has a semistellar nucleus that emits moderately strong [O II] lines
and therefore is bluish. Otherwise the spectra and absorption are
normal". Minkowski holds the remote object to be the fourth member of
the group and gives the following data, corrected for absorption and
for solar motion. Data reduced to H=50 km s^-1^ Mpc^-1^.
Component Aperture B_0_ (B-V)_0_ V_0_km s^-1^ M_B_
All 1' 13.24 +0.85 - -
All 2.5' 12.79 +0.83 +9082 -22.9
A 13.1 +9480 -22.6
B 14.5 +7960 -21.2
C 16.0 +10050 -19.7
D 17.5 - -18.2
The main members are supergiants with completely overlapping
atmospheres, especially if taken up to the surface brightness of 27.5mg
per 1" square, not to 25m as here. From the virial theorem, the mass of
the system is 3x10^13^m_sun_ and m:L=7.5.
The nest VV 364 must be younger than the other galaxies in a cluster.
The central supermassive object has undergone fragmentation. Strong
radio emission is a complimentary indication of the younger age.
We stress that E like galaxies, which seem somewhat irregular as a
consequence of their tight multiplicity, and surrounded by an unusually
large halo, were discovered by us (Vorontsov and Rrasnogorskaya 1961)
while compiling the MCG. They were completely described there and it
was shown that mamny of them (not all!) are the brightest, central
objects of clusters. There exist isolated objects of this type.
This discovery was falsely and repeatly ascribed to the Mathews,
Morgan and Schmidt (1964). Although we did remonstrate (Vorontsov
1965), the unjust wrong statement lives on.
In MCG it was stated that MCG +02-07-017, +02-27-004, +02-29-020,
+02-58-021, +02-59-035, +01-39-009, +05-38-005, +03-41-078 and 6
others belong to the same type. We showed that, even by the eye
estimate, with H_0_=75 km s ^-1^ Mpc^-1^ NGC 7469 has a diameter of
60 000 pc. NGC 1275 possibly is also a very young tight nest of
spheroidal peculiar giants. At the 1973 IAU Symposium it was said that
the nest NGC 6166 could have been formed in the cluster by captures! We
showed in MCG that such nests (cD) also exist as isolated entities,
consequently the capture theory is as unvalid here as it is in the case
of numerous isolated nests!

22. 1976RC2...C...0000d
Re:NGC 6166
= 3C 338
I Zw 153 at 1 arcmin south-following.
Brightest in Abell 2199.
Classification and Dimensions:
Ap. J., 140, 35, 1964.
Ap. J., 173, 485, 1972.
Ap. J., 140, 44, 1964.
Ap. J., 142, 1364, 1965.
IAU Symp. No.44, 349, 1972.
Cont. Asiago, No. 300, 79, 1973.
Photometry (UBVR):
A.J., 75, 695, 1970.
Ap. J., 173, 485, 1972.
Ap. J., 178, 1, 1972.
Ap. J., 178, 25, 1972.
Ap. J., 183, 731, 1973.
Bull. A.A.S., 5, 447, 1973.
Spectrum (velocities of many cluster members):
Ap. J., 188, 221, 1974.
Radio Observations:
Ap. J., 140, 44, 1964.
Ap. J., 142, 106, 1965.
Ap. J., 144, 216, 1966.
Ap. J., 148, 367, 1967.
Ap. J. (Letters), 191, L11, 1974.
Obser., 87, 124, 1967.
A.J., 73, 1, 1968.
Astr. Ap., 31, 223, 1974.
Astr. Ap., 34, 341, 1974.
X-rays (from Cluster):
Ap. J. (Letters), 185, L13, 1973.
Ap. J. (Letters), 193, L57, 1974.

23. 1973UGC...C...0000N
Re:UGC 10409
E pec (de Vaucouleurs)
Companion superimposed north-following center
A large number of small galaxies near

24. 1964RC1...C...0000d
Re:NGC 6166
[Not = Holm 751a,b,c,d,e which are companion galaxies. The objects
NGC 6166A,B,C,D are condensations within NGC 6166 itself.]
Description and Photograph:
P.A.S.P., 70, 143, 1958.
A.J., 66, 558, 1961.
Ap. J., 136, 1134, 1962.
Color, Magnitude, Systemic Velocity
A.J., 66, 558, 1961.
Radio Emission:
P.A.S.P., 70, 143, 1958.
Caltech Radio Obs., 5, 1960.

25. 1964ApJ...140...35M
Re:3C 338
No. 40.-Three secondary components in same envelope. Outstandingly brightest
member of cluster A2199, richness 2. 200-inch plate and redshift by Minkowski

26. 1961AJ.....66..562V
Re:NGC 6166
6166 Multiple E. Brightest member of a cluster.

Back to NED Home