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Notes for object CGCG 173-014

16 note(s) found in NED.


1. 2006ApJS..164..307M
Re:3C 382
This galaxy has a very bright unresolved nucleus with marked diffraction spikes.
This galaxy lies on a field populated by unresolved sources.

2. 2003ApJS..146....1W
Re:3C 382
3C382.0.-This is one of three low-latitude sight lines in the sample
toward which H I associated with the Outer Arm is seen (e.g., Habing
1966; Kepner 1970; Hulsbosch & Wakker 1988; Haud 1992). 0 VI is seen at
corresponding velocities, extending to - 130 km s^-1^. The O VI
measurement for the thick disk includes this component. A separate
measurement is also given for the velocity range over which Outer Arm
H I is seen.
The feature at 1033.650 {angstrom} (500 km s^-1^ on the O VI velocity
scale) is intrinsic C III-the corresponding Ly{beta}, Ly{gamma}, and
Ly{delta} lines are also seen. The features at 1033.090 and 1035.020
{angstrom} (340 and 900 km s^-1^ on the O VI velocity scale) remain
unidentified. There are no intrinsic Lyman lines at these velocities.
Although there are no known galaxy groups in this low-latitude (high
extinction) direction, these features may be Ly{beta} at v = 2155 and
2715 km s^-1^. Unfortunately, the other Lyman lines are then in a part
of the spectrum that is too noisy to confirm this, and no Ly{alpha} data
are available.

3. 2002ApJS..139..411A
Re:3C 382
3C 382-The UV image of 3C 382 (Fig. 28a) is dominated by the strong
nucleus. The faint object 1.5" northwest of the nucleus is the ghost
described in section 2.

4. 2001MNRAS.325..636A
Re:3C 382
5.5 3C 382
3C 382 has a double-lobe structure, with a clear jet in the northern lobe
that ends in a hotspot. A hotspot in the southern lobe is also detected,
but a counterpart jet is not clear, although a trail of low fractional
polarization is detected (Black et al. 1992). The total 3.85 GHz size
between hotspots is 179 arcsec (Hardcastle et al. 1998).
Optically, the radiosource is identified with a disturbed elliptical
galaxy dominated by a very bright and unresolved nucleus (Matthews,
Morgan & Schmidt 1964; Martel et al. 1999), located in a moderately rich
environment (Longair & Seldner 1979). The optical spectra show a strong
continuum and prominent broad lines photoinized by a power-law type of
spectrum (Saunders et al. 1989; Tadhunter, Fosbury & Quinn 1989). The
stellar population of the host galaxy, as we show in our study, is barely
detected in the nuclear regions.
The Einstein satellite detected 3C 382 in X-rays at a flux level
f(0.5-3 keV) = 1.3 x 10^-13^ erg cm^-2^ s^-1^, or 2 x 10^44^ erg s^-1^
(Fabbiano et al. 1984). The source is resolved in ROSAT HRI observations
but its interpretation is debatable since the luminosity is too strong for
a galaxy environment which is only moderately rich (Prieto 2000).
3C 382 is a variable source at X-ray (Dower et al. 1980; Barr & Giommi
1992), radio (Strom, Willis & Willis 1978), optical and UV frequencies
(Puschell 1981; Tadhunter, Perez & Fosbury 1986)

5. 2001ApJ...552..508G
Re:3C 382
1833+32 (3C 382). - A 8.4 GHz VLBI image of this source was published
in Giovannini et al. (1994). We present here new observations with a
global array of 17 telescopes for 6 hr at 5 GHz. The new image is in good
agreement with the old one. Thanks to the better sensitivity and UV
coverage, we see a more extended jet with a peak brightness at its end
(Fig. 16). The possible change in the jet P.A. near the core is not
confirmed by the new data. A comparison of the 8.4 and 5 GHz images shows
some displacement between local peaks, possibly due to proper motion, but
the large epoch difference and the very different UV coverage
(and frequency) do not allow us to estimate it.

6. 2000MNRAS.317..120R
Re:3C 382
5.13 3C 382 (z=0.05787)
This is the only galaxy in this sample in which the optical luminosity
is dominated by a central point source, an AGN, which is saturated on
both our V and U images. The AGN is extremely blue but the colour
estimated for the host galaxy is within the range of the other radio
galaxies in this sample, and similar to a normal early-type spiral.
3C 382 (Fig. 20) is interacting with a companion (G2), a large barred
spiral 85.1 arcsec away at PA 677. Two long filaments connect the two
galaxies, forming a 'loop'. G2 is confused with a very bright foreground
star, but by subtracting the flux of the star we estimate V ~ 15.29 for
the underlying galaxy, with an early-type spiral colour of U - V ~ 1.14.
The pair orientation is close to the radio axis, and the radio map
(Black et al. 1992) shows the north-eastern radio jet to be enhanced in
brightness and deflected through ~ 25^deg^ at the position of G2.
The main body of the galaxy appears rather featureless, except for a
bright spot H1, with V = 17.13, 16.7 arcsec from the 3C 382 nucleus at
PA -844 and joined to it by a short filament. H1 is very blue
(U - V = 0.38) and corresponds to a bright spot in the H{alpha} image of
McCarthy et al. (1995). It might be a gas-rich starburst dwarf galaxy,
far less massive than G2, in the process of merging into 3C 382.

7. 2000A&A...362..871C
Re:3C 382
1833+32 (3C 382): This source is associated with the broad line radio
galaxy 3C382. The nuclear emission dominates the optical emission but
the underlying host galaxy is clearly seen in these images. See also
Martel et al. (1999).

8. 1999MNRAS.310...30C
Re:B2 1833+32
B2 1833+32 is an FR II radio galaxy (Laing, Riley & Longair 1983; Black
et al. 1992) with broad emission lines (Osterbrock, Koski & Phillips
1975; Tadhunter, Perez & Fosbury 1986; Kaastra, Kunieda & Awaki 1991).
Its higher than expected X-ray flux, as compared with the core radio
strength, may arise from emission in the central accretion disc around
the active nucleus, seen due to an advantageous viewing angle as
indicated by the broad emission lines.

9. 1999ApJS..122...81M
Re:3C 382
3C 382. - This elliptical galaxy is dominated by a very bright,
unresolved nucleus and the halo appears very smooth. At a distance of
85" (100 kpc) to the northeast of 3C 382 lies a beautiful galaxy with
three extended tails of material.

10. 1998MNRAS.296..721C
Re:3C 382
3.5 3C382
The broad-line intensities and profiles of 3C 382 are known to be variable
(Tadhunter, Perez & Fosbury 1986). In our spectrum the H{alpha} profile shows a
prominent blue shoulder, a feature which is absent in EH94's data. Consequently,
the profile shape is intermediate between those of Arp 102B and 3C 390.3 on the
one hand, and 3C 227 on the other. Although the profile is not clearly
double-peaked, it is possible that the prominent blue and red shoulders are
actually displaced components at 3800+/-200 and 3300+/-200 km s^-1^. The line
is extremely broad, with a FWZI of 26000+/-2000 km s^-1^ (even this is probably
an underestimate, given that the extreme red wing is affected by the atmospheric
H_2_O absorption band).
A84 concluded from a series of observations obtained between 1980 and 1982 that
the optical polarization is intrinsically variable. On the other hand, no
significant variations in P or {psi} were observed by Rudy et al. (1983) during
a partly overlapping period (1979-81; although their quoted uncertainties are
larger). Our measurements for the integrated continuum fall well within the
ranges of the variations in P and {psi} (0.7<=P<=1.5 per cent and
54^deg^<{psi}<62^deg^) reported by A84. In our spectra, there is a significant
decrease in P associated with the broad H{alpha} feature which roughly mirrors
the profile shape (including dips corresponding to the narrow H{alpha} and
[N II]{lambda}6583 lines where P->0). On the other hand, there is no significant
change in {psi}. This behaviour suggests that the continuum is strongly
depolarized by line emission which is itself weakly polarized, if at all. After
subtraction of the continuum, we measure a residual polarization of
P=0.15+/-0.04 per cent at {psi}=46.0^deg^+/-7.5^deg^. This could either be due
to dichroic absorption in the Galaxy or, perhaps more likely, it reflects the
error in the fit to the continuum Stokes spectra. Hence, in contrast to A84, we
find no evidence for inmnsic polarization of the broad H{alpha} line in
3C 382. In particular, we note that the pronounced variations in the Q and U
Stokes parameters reported by A84 to be associated with the broad H{alpha} line
are not present in our data.
The continuum polarization PA is closely aligned with the axis of the extended
double-lobed radio source (in PA~55^deg^; Antonucci 1985; Black et al. 1992). On
milliarc-second scales VLBI observations (Giovannini et al. 1994) reveal a jet
in PA~50^deg^ with a complex twisted structure.

11. 1997A&AS..126..335M
Re:3C 382
1833+32 (3C 382) A bright jet is visible in the northern lobe in the map by
Black et al. (1992). Using the 2.7 GHz polarization position angle in Parma &
Weiler (1981), we obtain a rotation measure of 64 rad m^-2^ (n=1, see Sect.
4.1).

12. 1995ApJS...99...27M
Re:3C 382
3C 382 (z = 0.06; Fig. 1).-This is one of the classic broad-lined radio
galaxies (Osterbrock, Koski, & Phillips 1986). The continuum has the
shape of a normal gE galaxy with some distortions in the outermost
isophotes. A continuum image is also given in Hutchings, Johnson, & Pike
(1988). The H{alpha} image shows diffuse emission surrounding the nucleus
and a high surface brightness patch of emission lying to the west. The
inner region of the H{alpha} image is saturated, and thus we cannot
determine the structure of the innermost regions. Long-slit spectra,
however, confirm that there is diffuse emission surrounding the nucleus.
Ultraviolet spectra of the nucleus and ground-based blue spectra of the
extended emission are given by Tadhunter, Perez, & Fosbury (1986). The
radio source is a large (184") double in position angle 50^deg^
(Tadhunter et al. 1986).

13. 1995ApJ...447..121W
Re:3C 382
3C 382.-No features or complexity are seen. The upper limits derived for
the Fe K line EW and N_HFe_ are consistent with Ginga (NP94).

14. 1994ApJS...90....1E
Re:3C 382
3C 382
This is also a well-studied BLRG. A spectrum obtained in 1974 by
Osterbrock et al. (1976) exhibits a remarkable difference from our own
spectrum shown in Figure 1: the 1974 spectrum shows the blue H{alpha}
shoulder to be stronger than the red one, while in our own spectrum the
red shoulder is the strongest. This behavior is very similar to the
behavior displayed by 3C 390.3 (see above).

15. 1991ApJ...381...85T
Re:3C 382
This source has a "canonical" spectrum with no evidence for a soft excess. An
IPC+MPC observation, however, claims a cool blackbody component of temperature
240 eV. A sample spectrum analyzed using the EXOSAT data base gives good
agreement on spectral index, but a somewhat lower absorbing column of
2.8^+0.2^_-0.1_ x 10^20^ cm^-2^. Fitting the ME data alone however, gives good
agreement on slope and column, suggesting that there is an unresolved soft
excess in the low-energy EXOSAT data.

16. 1986A&AS...64..135P
Re:B2 1833+32
The source is more extended than 2 arcmin and has a rather high total
radio power ( > 1.0 E 25 W/Hz). Its structure is clearly quite different
from all the other sources in this sample, and it is rather typical of
a high-luminosity radio source.


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