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Notes for object 3C 120

28 note(s) found in NED.

1. 2008ApJS..175..314D
Re:VSOP J0433+0521
J0433+0521.-The VSOP observations suggest that the core is <0.3 mas in size.
Only some of the extended structure to the west is imaged with VSOP.

2. 2008ApJ...673...96A
Re:3C 120
3C 120 is a Seyfert 1 galaxy. This source was observed by ASCA. The best fit to
ASCA and BAT data is an absorbed power-law model with absorption consistent with
the Galactic one, a photon index of 1.80^+0.04^_-0.04_ , and a blackbody
component with a temperature of 0.27^+0.026^_-0.025_ keV.

3. 2008A&A...488..897H
Re:3C 120
3C 120 (0430+052): This radio galaxy has been monitored in Metsahovi for over 20
years at 22 and 37 GHz and for 15 years at 90 GHz. It is a well-studied object
at all wavelengths and has been a target of many multiwavelength campaigns. Its
radio jet has been studied and modelled using VLBI observations by several
authors (e.g. Walker et al. 2001; Hardee et al. 2005; Gomez et al. 2001). Our
wavelet analyses reveal a timescale of 4.3 years at both 22 and 37 GHz. At 22
GHz the timescale has been present for 85% of the total observing period lasting
for 4.4 cycles. At 37 GHz it has been present for 84% of the time and persisted
for 4.6 cycles. In Paper I the DCF analyses showed a timescale of 4.2 years at
22 GHz which is very close to what we obtained here. Both frequencies also show
flare timescales of 1.4 years and in addition 0.5 years at 22 GHz and 0.3 years
at 37 GHz. These timescales are also seen in the DCF and SF analyses of Paper I.
At 90 GHz the timescale obtained is 2.7 years and it has been presen t for 73%
of the time and continued for 4 cycles. This timescale is also very close to the
DCF timescale of 2.9 years.
Visual inspection of the flux curve at 37 GHz shows that indeed many of the
larger flares have approximately 4.5 to 5 years between them but there are also
additional flares in between. The last big flare included in our analysis at 37
GHz peaked in the autumn of 2003. The next big flare was observed at the end of
2006 with an interval of 3 years between the flares. This indicates that the
source is not strictly periodic but has shown a characteristic timescale of 4.3

4. 2007A&A...461.1209D
Re:3C 120
3C 120: The BeppoSAX observation of 3C 120 was previously published by
Zdziarski & Grandi (2001). The baseline model adopted here is the same
adopted by these authors and consists of a primary power law plus a
reflection component and an emission FeK{alpha} line. Overall, the
spectral analysis performed here confirms the results previously
published. Slight differences are found in the determination of the
FeK{alpha} EW and E_c_, where Zdziarski & Grandi found higher values
(but consistent within the 90% confidence intervals) for both parameters
and for R (in this case Zdziarski & Grandi found a slighly lower value).
This is probably due to the fact that the LECS data are not considered
here so that no soft component is present in the best-fit model of this
work. This may have introduced a slightly higher normalization of the
primary continuum that resulted in the observed differences.

5. 2006AJ....131.1262H
Re:3C 120
0430+052 (3C 120): We find a limit of |m_c_| < 0.29% in the core at 15 GHz
in 2003 February. HW99 also found limits between 0.2% and 0.3% in the core
at 15 GHz throughout 1996. Both signs of circular polarization (with a
clear preference for positive circular polarization) were detected
intermittently in the historical integrated measurements (WdP83; K84) at
8.9 GHz and below.

6. 2005AJ....130.1418J
Re:3C 120
Our observations continue to trace components d, h, l, o1, and o2
detected in Gomez et al. (2001), and we identify new components t, u,
u1, and v (Fig. 16). Components d and h move ballistically with the
same apparent speed found previously, while l has decelerated since
earlier epochs. Components o1 and o2 represent the front section of
the major disturbance designated in Figure 17 as the "o complex."
Component o1 brightens in total and polarized flux at ~3.4 mas,
similar to the behavior seen for h and l (Gomez et al. 2001). After
flaring, o1 and o2 diverge in their behavior: o1 accelerates and o2
decelerates (Fig. 16). Such a development is expected if o2 is a
trailing component that forms in the wake of the accelerating knot
o1, which represents the major disturbance in the flow (Gomez et al.
2001). The most prominent feature at later epochs is t , which
evolves in the same manner as l. The components have nearly equal
proper motions, 2.17 +/- 0.06 (l; Gomez et al. 2001) and 2.04 +/-
0.08 mas yr^-1^ (t), and similar trajectories (Fig. 18). They both
undergo a flare in total and polarized flux at a location between 2.5
and 3.5 mas from the core, and the EVPAs of both rotate during the
flare (Fig. 37). Gomez et al. (2000) explained these properties as
the results of an interaction between the jet and an interstellar
cloud. The behavior of component t is consistent with this, which
suggests that it interacts with the same cloud. However, there is a
significant shift (~0.6 mas) between the projected positions of the
peaks of the flares (see Fig. 37). Most likely, the shift is a
consequence of the slightly more southern trajectory of t (Fig. 18).
For a viewing angle of ~21^deg^ and an opening angle of ~4^deg^ (see
Table 11), the shift by 0.6 mas gives a lower limit to the size of
the cloud of 1 pc at a deprojected distance from the VLBI core of
-8 pc.

7. 2005AJ....129..630B
Re:UGC 03087
Previous studies of UGC 3087 have mainly concentrated on its nuclear
activity. It is a strong radio source (3C 120), and the optical
spectrum suggests a Seyfert 1 nucleus (Tadhunter et al. 1993). It has
a faint optical jet in the same apparent direction as the radio jet.
The optical jet is clearly visible in our images and distorts the
isophotal profiles in the inner region.

8. 2004MNRAS.350.1049G
Re:3C 120
9.8 3C 120 Lebofsky & Rieke (1980) reported a decline in the K flux of
3C 120 from levels of 64-71 mJy, that had been observed in 1970-1972 by
Penston et al. (1974), to ~24 mJy in 1978. This decline took at least
three years. In the present work the (not dereddened) K flux varied from
32 to 47 mJy. Only three galaxies in the present sample have shown such
large changes. However, the case for 3C 120 seems to be well
corroborated and is almost certainly real. The Penston et al and
Lebofsky & Rieke values are plotted with the present data in Fig. 5 as
crosses. The fluxes tend to lie quite close to the regression lines
shown except at L, where the Penston L values seem too bright. However,
the standard errors of his measurements were quite high.
Long-term B light curves of 3C 120 have been presented by Hagen-Thorn
et al. (1997) and Clements et al. (1995), in which a decline over the
years 1973 to 1978 is clearly seen.
A cross-correlation analysis between J and L shows that the longer
wavelength emission is delayed by about 160 d compared to the shorter.

9. 2003ApJ...589..126Z
Re:3C 120
3.5. 3C120 As for 3C 111, the RM maps for this radio galaxy were
presented in Zavala & Taylor (2002). The core RM was
2080 +- 100 rad m^-2^. This decreased to approximately
100 +- 60 rad m^-2^ after a projected distance of 1 pc, which is
similar to what is observed in quasars. The jet, where the percent
polarization is ~18%, was shown to have good agreement to a
{lambda}^2^ law. The spectral index in the jet is
{alpha}^12.1^_8.1_ = -0.5 or less (Fig. 7). Electric field vectors
are perpendicular to the jet axis. The E-vectors in the core are
coincident with RMs that may show a deviation from a {lambda}^2^ law
(Zavala & Taylor 2002, Fig. 4).

10. 2003AJ....126.2237D
Re:3C 120
4.5. Radio Galaxies
3C 120 (F04305+0514) is a powerful radio galaxy [L_{nu}_(4.8 GHz) =
10^25.4^ W Hz-1] with a large radio excess of u = -0.43. It has FR I
morphology on large scales with a total extent of greater than 760 kpc
(Walker et al. 1987). Superluminal motion has been detected in the
small-scale radio structure and an optical and radio jet is observed
on arcsecond scales. This object is highly variable at all wavelengths
(radio--X-ray) and may be a blazar. The optical nucleus has a Seyfert
1 spectrum and the host galaxy may be disturbed. The FIR luminosity is
moderate at {nu}L_{nu}_(60 micron) = 10^10.9^L_solar_.

11. 2002AJ....124..675C
Re:UGC 03087
Very extended radio source. 3C 120. Unusually warm FIR source:
alpha(25,60) = 0.80. Seyfert 1.

12. 2000A&AS..143..369G
Re:3C 120
0430+052: 3C 120 is a well studied radio source, displaying superluminal
motion (Zensus 1989). The spectrum of the optical counterpart is quasar
like (Tadhunter et al. 1993), and the galaxy has been often classified
as Seyfert 1, even if its spiral morphology has never been clearly

13. 1998ApJS..114..177Z
Re:3C 120
3C 120.--This is also a nearby radio galaxy whose optical image is rather large
(1' in extent), with extensive H II regions that are thought to be photoionized
by the nucleus (Baldwin, Phillips, & Terlevich 1981). 3C 120 has a large-scale
FR I morphology. Based on its emission-line properties, 3C 120 is classified as
a Seyfert galaxy, but its spiral nature has never been clearly established. It
has an unusual optical morphology in which neither elliptical nor spiral models
adequately represent the luminosity profile for this object (Smith 1988). The
nucleus is a strong and variable source of radiation at all wavelengths from
radio to X-ray (Maraschi et al. 1991). In many ways 3C 120 resembles a
low-luminosity quasar. Also, 3C 120 has a faint optical jet described by Hjorth
et al. (1995). The jet properties are apparently similar to that of
PKS 0521-26. The optical jet apparently coincides with the radio jet and emits
continuum radiation (B, V, I) with a radio-to-optical spectral index of 0.65.
In the FOC images we see a clear nuclear source, particularly in the F165W and
the F130M filters (in both cases the PSF contribution is 100%). The F320W and
F372M images are highly saturated. No extended structure is visible. The
optical image, which is a combination of the F555W, F685W and the F814W filters
(to get a higher S/N image), shows extended structure that resembles that of
spiral arms. The inner regions show extensions to the northwest and southeast.

14. 1998ApJS..114...73G
Re:3C 120
Section A3. 3C 120
This bright, flat-spectrum radio source has Seyfert 1 properties in the
optical regime. The source was first detected in X-rays by SAS-3 (Schnopper
et al. 1977) and has since been observed by all the major X-ray astronomy
satellites except Ginga. From our analysis of the data from the ASCA
observation performed in 1994 February, we find model A(i) to provide an
adequate description of the spectra, with some evidence for intrinsic
absorption (N_H, z_ ~ 5 x 10^20^ cm^-2^). However, we find some evidence for
a "hard tail" in this source, with significantly superior fits obtained if
0% of the continuum is attenuated by N_H, z_ ~ 5 x 10^23^ cm^-2^ [model
A(ii); Fig. 4] or by a flattening of the underlying continuum >~6 keV
(Section 6.4.2). We find no compelling evidence for ionized gas in 3C 120
[intense emission from ionized gas is implied by the best-fitting solution
assuming model C(ii), but at a level incompatible with strength of the
observed Fe K-shell line; see Fig. 12]. This confirms the finding of R97 who
also found a lack of evidence for O VII and O VIII absorption edges in their
analysis of these ASCA data. They find a best-fitting photon index consistent
with our value but a slightly larger absorbing column density intrinsic to
the source (N_H, z_ ~ 8 x 10^20^ cm^-2^) than we found for model A(i).
In all cases, the derived slope is {GAMMA} ~ 2.0 and is consistent with a
poorly constrained ROSAT PSPC spectrum ({GAMMA} ~ 1.5^+1.2^_-1.8_; Boller et
al. 1992) and slightly steeper than those derived from HEAO-1, Einstein, and
EXOSAT ({GAMMA} ~ 1.5-1.9, W95; T91; TP89). Spectral variability was apparent
in the Einstein observations (T91). Unfortunately, the ASCA data are unable
to constrain the Compton-reflection component seen in HEAO-1 observations
(W95), although such a component clearly offers an alternative explanation of
the hard tail. We also note that many of the fits to the 3C 120 data set
imply a local column density >N^gal^_H,0_ ({DELTA}N_H, 0_ ~ 5 x 10^20^ cm^-2^).
Furthermore, this data set seems particularly badly affected by a troughlike
deficit of counts at energies <0.6 keV compared to the extrapolated model. It
is unclear how these facts may be related to the well-known, but poorly
understood, calibration problems of the XRT/SIS at these energies (see also
Section 2.3).

15. 1998ApJ...501...82P
Re:3C 120
Continuum and emission-line variability was first reported in this source by
Oke, Readhead, & Sargent (1980) and French & Miller (1980), who placed an upper
limit on the size of the H{beta}-emitting region of ~0.2 pc ~ 240 light
days. Our light curve is not particularly well sampled; however, we do find a
statistically significant lag, but with a large formal uncertainty
({tau}_cent_=43.8_-20.3_^+27.7^ days).

16. 1998AJ....116.2682C
Re:IRAS 04305+0514
UGC 03087, Mrk 1506, 3C 120. Seyfert 1. Flat radio spectrum, radio
variable. Multifrequency VLA and VLBI maps in Walker, Benson, & Unwin
(1987) and Walker, Walker, & Benson 1988).

17. 1998AJ....115.1295K
Re:3C 120
0430+052.--This is a well-known superluminal source (3C 120) with a long, thin
jet with small oscillations. Observations at 18 cm trace the jet out to 200 mas
(Benson et al. 1988).

18. 1997MNRAS.286..513R
Re:3C 120
7.2.1 3C 120
As previously mentioned, the broad-line radio galaxy 3C 120 possesses an
extremely broad ({sigma}=1.5_-0.4_^+0.6^ keV) and strong (W_Fe_=960_270_^+520^
eV) spectral feature with a centroid energy E=6.43_-0.24_^+0.23^ keV. This is
not consistent with being iron fluorescence emission from the immediate
vicinity of a Schwarzschild black hole. More investigation is required to
determine the origin of such features.

19. 1995ApJS..100...37G
Re:3C 120
3C 120 is a superluminal source (Zensus 1989), and the optical
continuum is highly variable (Wlerick, Westerlund, & Garnier 1979; French
& Miller 1980; Oke, Readhead, & Sargent 1980). It is an OVV-type blazar
(Webb et al. 1988; Burbidge & Hewitt 1992). This source was observed on
14 occasions with EXOSAT between 1983 August and 1986 February. Signal
significances of the two spectra are less than 4 {sigma}, and those of
the remaining 12 spectra are above 4 {sigma}(Table 2). Results of
simultaneous/quasi-simultaneous observations of this blazar in the
optical, ultraviolet, and X-ray bands have been described by Maraschi et
Best-fit parameters of the LE and ME spectra with the power-law plus
absorption model are listed in Table 3. Results of our analysis are
consistent with the results of Turner & Pounds (1989) and Maraschi et al.
(1991). It may be noted from Table 3 that the spectral slope ({GAMMA} ~
1.6-1.94) is correlated with the LE flux and anticorrelated with the ME
flux. This result suggests a pivoting of the spectrum around 2 keV.
Derived values of N_H_ from the power-law fits suggest that no intrinsic
absorption is present in this source. Variability in the LE and ME bands
with timescales shorter than a day is not found. Using the simultaneous
observations of optical, ultraviolet, and X-ray bands (Maraschi et al.
1991) and nonsimultaneous observations between radio and IR bands, we
have constructed the multifrequency spectrum of this blazar (Fig. 3d),
which shows the spectral discontinuity between UV and X-ray region, and
two parabolic components can represent the multifrequency spectrum.

20. 1995ApJ...447..121W
Re:3C 120
3C 120.-We present the first evidence for spectral flattening in this
Seyfert 1 galaxy. 3C 120 was not observed by Ginga.

21. 1994A&A...289..673T
Re:3C 120
0430+052 (3C 120)
In 3C 120 radio-optical connections have been found earlier (Usher 1972;
Balonek 1982). During the ten years of our radio monitoring this source
has had two strong radio flares which can be easily distinguished from
the flux curves at 22,37 and 90 GHz. There are also some smaller-scale
events visible. When numerically analysing the data it turned out that
there is a clear correlation between all the frequencies, radio and
optical, with significantly long time lags. The time lags between the
optical events and different radio events increase towards lower
frequencies, being 500-650 days for optical to 90 GHz, 700-850 for
optical to 37 GHz, and 85o-900 days for optical to 22 GHz. The time lags
between the different radio frequencies are in accordance, e.g. about 250
days between 90 and 37 GHz. Visual inspection indicates that the
correlation results from the similar shapes of the optical and radio

22. 1993MNRAS.263.1023M
Re:3C 120
0430+05 (3C120). This Seyfert galaxy has been exhaustively studied at a
variety of resolutions (see Walker, Benson & Unwin 1987). It has
structure on scales from 100 kpc to 1 Pc, including a prominent one-sided

23. 1993MNRAS.263..999T
Re:PKS 0430+05
0430+05 (3C 120). Broad-line radio galaxy, extensively studied. Quasar-
like spectrum: broad Balmer and Fe II lines/blends, strong [O III]
{lambda}{lambda}5007,4959 lines, blue continuum.

24. 1991ApJ...381...85T
Re:3C 120
This object was observed 4 times by the Einstein SSS+MPC combination.
Initial analysis of the MPC data suggested a variable slope in the hard
X-ray regime (Halpern 1982). EXOSAT observations, however, showed a
steady spectrum over six observations. Analysis of the SSS+MPC data once again
brings up evidence for spectral variability in this source (Fig. 3).
One of the SSS+MPC observations showed a significant line feature at ~0.92
keV (Table 4). Soft X-ray line emission was first suggested in an early
analysis of the SSS data (Holt et al. 1980).

25. 1988A&AS...75..273D
Re:3C 120
3C 120 is a thoroughly studied Seyfert type 1 object, observed to be
variable at all wavelengths. It was identified to an X-ray source by
Forman et al. (1978), and has also been observed in the UV by Wu et
al. (1980, 1983). At radio wavelengths, 3C 120 has several remarkable
properties, among which a bent jet existing from milliarcsecond scales
up to almost one arcminute (Walker et al., 1987, and references
therein) and coinciding at arcsecond scales with an optical jet.
However, except for this jet, no obvious relationship has been found
between the radio morphology and the optical stellar and gaseous
structures, as underlined for example by Balick et al. (1982). This
galaxy is poor in HI (Bieging and Biermann, 1983). Optical spectra of
3C 120 were obtained by Sargent (1967) and by Phillips and Osterbrock
(1975), who reported strong HeI and HeII emission lines, as well as
FeII multiplets. Baldwin et al. (1980, hereafter B80) have analysed
the physical and kinematical properties of the complex extended
ionized nebulosity surrounding this galaxy.
The nuclear redshift of 3C 120 is z = 0.0331 +/- 0.0002,
corresponding to a galactocentriG velocity of 9770 km s' and to a
distance of 196 Mpc.
We have detected ionized gas in the nucleus of 3C 120, in zone SE1
along PA = 311^deg^ and in four regions labeled Neb1-Neb4, observed
along PA = 297^deg^ with the spectrograph slit off-centered from the
nucleus by 5" to the north (see Tab. XVIa and Fig. 14). The latter
direction is parallel to that of the inner radio jet (Walker et al.,
1987) and to the galaxy optical major axis (B80). The total extent of
the detected ionized gas is about 23" (22 kpc) along PA = 311^deg^
and 29" (27.5 kpc) along PA = 297^deg^.
We shall not discuss the already extensively studied nuclear
spectrum of 3C 120, but we give the intensities of the main emission
lines (Tab. XVIa), after a deblend of the broad and narrow components
of the Balmer lines, which has not been previously reported. The FWHMs
found for H{alpha} and H{beta} are 4500 and 2100 km s^-1^
respectively. Relative intensities agree within 50% with measurements
by Phillips and Osterbrock (1975) and B80, except for the weak lines
and for the HeI 5876 and HeII 4686 lines.
Regions Neb3 and Neb4 intersect regions 1 and 2 of B80
respectively, but they are not identical. The relative line
intensities in these two regions agree with those of B80 within a
factor of 2. The excitation level is 3 to 5 times smaller than in the
nucleus. Since lines of low and high excitation ([OI] and [NeV]) are
present in the nebulosity (especially in Neb 2), photoionization by a
power-law UV continuum is also required for off-nuclear regions.
As the [OIII] 4363 line is blended with the broad and narrow
components of H{gamma}, the uncertainty on its intensity is large, and
we have not tried derive T_e_ or the other physical parameters in the
nucleus, for which the reddening estimate is also a problem. In region
Neb 2, we find T_c_ = 14500 K after a reddening correction of
E(B-V) = 0.4.
The kinematics of 3C 120 have been thoroughly analysed by B80, who
mapped the entire ionized nebulosity with a grid of high spectral
resolution (1 A) long slit spectra. They found that the ionized gas
has a highly disordered velocity field; however some general pattern
is apparent, with a line of nodes along PA = 72^deg^, velocities being
higher than that of the nucleus north of this line and smaller south.
Our observations along PA = 311^deg^ intersect their grid of
observations, while those along PA = 297^deg^ (see Tab. XVIb) coincide
with the {DELTA}Y = + 4 slit position of B80. Our data agree with the
general trends of the velocity field of B80; however, individual
values can differ by as much as 100 km s^-1^. Such discrepancies can
be due to the frequent double peaked or asymmetric shape of the
[OIII] 5007 line, which lead to uncertain line positioning.

26. 1976RC2...C...0000d
Re:[RC2] A0430+05
= 3C 120
= 4C 05.20
= II Zw 014
= BW Tau
Type 1 Seyfert nucleus.
Previously known as the variable star BW Tau.
Precise Position:
A.J., 78, 521, 1973.
Dimensions: (Unresolved Nucleus)
A.J., 73, S175, 1968.
A.J., 73, 927, 1968.
Ap. J., 152, 1101, 1968.
CGPG Fig. 5, 1971.
Photometry: (UBV) and Variability Studies:
Ap. J., 152, 1101, 1968.
Ap. J., 158, 535, 1969.
Ap. J., 178, 25, 1972.
Ap. J., 180, 687, 1973.
Ap. J. (Letters), 150, L177, 1967.
Ap. J. (Letters), 172, L25, 1972.
Ap. J. (Letters), 178, L51, 1972.
A.J., 73, 885, 1968.
Astrophys. Lett., 2, 77, 1968.
Nature, 225, 365, 1970.
Ap. Space Sc., 10, 402, 1971.
M.N.R.A.S., 152, 79, 1971
M.N.R.A.S., 169, 357, 1974.
Info. Bull. Var. Stars, No. 703, 1972.
Sov. A.J., 16, 763, 1973.
Tokyo Ast. Bull., 2nd ser., No. 228, 1974.
P.A.S.P., 86, 870, 1974.
Photometry: (I.R. 1.6-21 microns)
A.J., 73, 868, 1968.
Ap. J. (Letters), 159, L165, 1970.
Ap. J. (Letters), 176, L95, 1972.
M.N.R.A.S., 169, 357, 1974.
P.A.S.P., 79, 369, 1967.
Ap. J. (Letters), 148, L57, 1967.
Ap. J. (Letters), 149, L51, 1967.
Ap. J., 152, 1101, 1968.
Ap. J., 176, 75, 1973.
A.J., 73, 847, 1968.
Ap. J., 192, 581, 1974.
A.J., 73, 855, 1968.
Ap. J. (Letters), 150, L173, 1967.
Ap. J., 164, 1, 1971.
Ap. J., 176, 75, 1972.
Ap. J., 191, 309, 1974.
Bull. A.A.S., 4, 208, 1972.
"Nuclei of Galaxies", 151, 1971.
IAU Symp., No. 44, 144, 1972.
Astr. Ap., 27, 433, 1973.
Ap. J. (Letters), 148, L53, 1967.
Astrofizika, 7, 417, 1971.
Radio Observations:
Ap. J., 144, 216, 1966.
Ap. J., 146, 294, 1966.
Ap. J., 148, 367, 1967.
Ap. J., 152, 639, 1968.
Ap. J., 154, 423, 1968.
Ap. J., 161, 1, 1970
Ap. J., 161 793, 1970.
Ap. J., 193, 55, 1974
Ap. J., 193, 303, 1974.
Ap. J. (Letters), 151, L27, 1968.
Ap. J. (Letters), 152, L169, 1968.
Ap. J. (Letters), 154, L49, 1968.
Ap. J. (Letters), 175, L55, 1972.
Ap. J. (Letters), 178, L51, 1972.
Ap. J. (Letters), 183, L47, 1973.
Ap. J. (Letters), 183, L51, 1973.
A.J., 73, 1, 1968.
A.J., 73, 293, 1968.
A.J., 73, 873, 1968.
A.J., 73, 874, 1968.
A.J., 74, 824, 1969.
A.J., 76, 537, 1971.
A.J., 77, 342, 1972.
A.J., 77, 810, 1972.
A.J., 77, 819, 1972.
A.J., 78, 163, 1973
A.J., 78, 536, 1973.
A.J., 79, 1232, 1974.
Astrophys. Lett., 7, 225, 1970.
Astrophys. Lett., 8, 153, 1971.
Sov. A.J., 13, 21, 1969.
Bull. A.A.S., 4, 207, 314, 1972.
Mem. R.A.S., 77, Part 3, 1972.
IAU Symp. No.44, p.232, 1972.
Astr. Ap., 25, 303, 1973.
Tokyo Ast. Bull., 2nd Ser., No. 228, 1974.
Radio Observations: (VLBI)
Ap. J., 153, 705, 1968.
Ap. J., 159, 337, 1970.
Ap. J., 169, 1, 1971.
Ap. J., 170, 207, 1971.
Ap. J., 172, 299, 1972.
Ap. J. (Letters), 153, L209, 1968.
Ap. J. (Letters), 173, L147, 1972.
Gamma-Rays: (Possible detection)
Sov. A.J., 15, 879, 1972.

27. 1973UGC...C...0000N
Re:UGC 03087
II Zw 14
"3C 120, blue elliptical compact and extended halo... Identical with
PKS 0430+05. Noted as a variable star (BW Tau) by Hanley and Shapley" (CGPG)
Seyfert spectrum
Not in CGCG

28. 1971CGPG..C...0000Z
Re:CGPG 0430.5+0515
II Zw 014
Blue elliptical compact and extended halo,
Identical with PKS 0430 + 05.
Noted as a variable star (BW Tau) by Hanley and Shapley (1940).
Spectrum: Broad emission.
= +9,970 km/sec.
m(pg) = 14.5

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