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Notes for object NGC 1052

25 note(s) found in NED.

1. 2007MNRAS.377.1696M
Re:NGC 1052
NGC 1052. Kadler et al. (2004) have used VLBA to resolve the core into mas-scale
twin jets, with a total flux at 0.7, 3.6 and 6 cm of 670, 2390 and 2410 mJy,
respectively. There is a small gap between the jets, and it is not clear which
component, if any, can be associated directly with the nucleus.
In the single epoch measured by M05 in 2002, the UV flux was 7.7 * 10^-17^
erg cm^-2^ s^-1^ A^-1^ at 2500 A and 9.0 * 10^-17^ erg cm^-2^ s^-1^ A^-1^ at
3300 A. The short wavelength flux was at half the level of the 2300-A flux in a
1997 HST Faint Object Spectrograph (FOS) spectrum (Gabel et al. 2000), as
measured by Pogge et al. (2000; 15 * 10^-17^ erg cm^-2^ s^-1^ A^-1^), which I
will adopt as a high flux. Based on the variable fraction, the lower limit on
the AGN flux is then (15 - 7.7) * 10^-17^ erg cm^-2^ s^-1^ A^-1^).
Kadler et al. (2004) have used Chandra to measure an unabsorbed nuclear 0.2-8
keV flux of 300 * 10^-14^ erg cm^-2^ s^-1^. They find the X-rays are moderately
absorbed by a column density of -10^22^ cm^-1^. The photon index they derive,
{GAMMA} = 0.3, is extremely low, but they note that this could be the result of
pile up in the detector at low energies. I therefore adopt the photon index of
{GAMMA} = 1.4 obtained by Guainazzi et al. (2000) using BeppoSAX. For this
index, the 2-10 keV flux would be 240 * 10^-14^ erg cm^-2^ s^-1^.

2. 2007A&A...469..451T
Re:PKS B0238-084
B0238-084, also known as NGC 1052, is an elliptical galaxy and the nearest
object in the sample (z = 0.005). It was referred to as a GPS source in de Vries
et al. (1997). It has the most prominent variability in our sample: a factor of
3 at several frequencies with Var_{DELTA}S,MAX_ = 4.57 for the data bin centred
at 8.8 GHz. The overall shape of the spectrum (Fig. 2) is clearly not
gigahertz-peaked, and the semi-simultaneous spectra shown in Fig. 1a show that
the shape of the spectrum changes depending on the state of the activity. For
comparison, the semi-simultaneous spectra of a distant (z = 2.624) classical GPS
source B0742+103 are shown in Fig. 1b. This genuine GPS source is only
moderately variable, and the turnover frequency stays more or less the same,
regardless of the level of variability. With the first two spectra, both sources
could be classified as non-variable GPS sources, but longer monitoring reveals
the difference in their behaviour. Thus, Fig. 1 shows that one or two years of
monitoring at differen t frequencies may not be enough to show the long-term
changes in the spectrum. Concerning the long-term changes in the radio spectrum,
B0238-084 is the only source in this sample that resembles the high-variability
sources with spectra becoming inverted during the outbursts that were found to
be common among the quasar-type GPS sources identified in the literature (Paper

3. 2006A&A...460...45G
Re:NGC 1052
NGC 1052. The X-ray morphology clearly indicates the presence of an unresolved
nuclear source in the hard bands (Fig. 5), in agreement with the classification
by Satyapal et al. (2004). Evidence of the AGN nature of this object has already
been given with the detection of broad lines in spectropolarimetric measurements
by Barth et al. (1999). Guainazzi et al. (2000) confirm that its X-ray spectrum
may therefore resemble that of Seyfert galaxies with the analysis of its
BeppoSAX spectrum (0.1-100 keV), for which they derive a very good fit with a
two-component model, constituted by an absorbed (N_H_ = 2.0 x 10^23^ cm^-2^) and
rather flat ({GAMMA} ~ 1.4) power-law plus a "soft excess" below 2 keV. The
corresponding flux in the 2-10 keV is 4.0 x 10^-12^ erg cm^-2^ s^-1^. The
presence of various jet-related X-ray emitting regions from a short (2.3 ks)
Chandra observation, together with a bright compact core, unresolved knots in
the jet structure, and an extended emitting region inside the galaxy that is
well aligned with the radio synchrotron jet-emission, have been reported by
Kadler et al. (2004); they derive {GAMMA}~0.25 and kT ~ 0.5 keV for the fitting
of the core spectrum. The value they estimate for the luminosity is within the
factor of 3 of our estimation (see Table 5).

4. 2005A&A...435..839T
4.2 Previously identified inverted-spectrum sources
B0238-084: this source, also known as NGC 1052, is a bright elliptical
Seyfert II-galaxy in the Cetus I cluster at a redshift of 0.0049. It is
known to have variability and an inverted radio spectrum (Condon et al.
1998). The source has been studied in detail by Vermeulen et al.
(2003). They suggest that both synchrotron self-absorption and
free-free absorption are present in the jets which are aligned close to
the plane of the sky.
de Vries et al. (1997) mentioned this source to be a GPS source but our
plot (Fig. 3) with new data shows a flat quiescent and a convex flaring

5. 2004ApJ...607..810M
Re:NGC 1052
NGC 1052. In addition to the two radial velocity -confirmed objects,
a visual inspection of the 75 kpc field surrounding NGC 1052 (Fig. 2)
reveals two other highly likely companions that presently do not have
confirming radial velocity data. They are [KKS2000] 04, a fine low
surface brightness dwarf spheroidal, to the southeast, and
2MASXi J0241351-081024 to the northeast. However, the grand-design
spiral galaxy NGC 1042 is only 15' away, suggesting that the elliptical
galaxy, NGC 1052, is by no means isolated but may share the potential
with at least two other sizeable galaxies, the other being NGC 1035.
This mixed-morphology triplet has already been cataloged and is known
as KTS 018.
We also suggest that [VC94] 023858-0820.4 (which has a radial velocity,
but at its published position has no obvious identification) should be
identified with 2MASXi J0241351-081024.

6. 2004A&A...424...91E
Re:PKS J0241-0815
J0241-0815 (0238-084, NGC1052) is a low redshift galaxy, considered in
detail by Kameno et al. (2001) and Vermeulen et al. (2003). A spectrum
compiled from an extensive list of sources is given by Tornikoski et
al. (2000), revealing variability by a factor of ~2 over a wide range of
frequencies. This variable nature is confirmed by the fact that the
source has the second highest variability index in Table 1. The low
frequency points lie above the nominal fit to the spectrum, and are
qualitatively consistent with the notion that this source has previously
been active, with the GPS spectrum reflecting a new stage of activity
(e.g., Tingay et al. 2003a).

7. 2004A&A...416...41X
Re:NGC 1052
NGC 1052. This giant elliptical galaxy which is classified as a
low-ionization nuclear emission-line region (LINER) galaxy (Ho et al.
1997) hosts a double-sided radio jet with a size of a few
milliarcseconds (Kameno et al. 2002). HST observations have revealed
dust absorption features in the center of this galaxy (van Dokkum et al.
1995). In the MIR maps of Fig. A.2 it is clearly seen that the 15 micron
emission is concentrated in a very compact region close to the center
and is dominated by the central source which, in this case, is an active
nucleus in agreement with the findings of Knapp et al. (1992). This is
also seen in the 6.7 and 15 micron radial profiles (Fig. 5) as well as
in the MIR flux ratio profiles (Fig. 6) where a steep turnover is
present at a distance close to the nucleus.

8. 2003ApJS..146..249B
Re:NGC 1052
5.2. NGC 1052
NGC 1052 is the only elliptical galaxy detected in H_2_O, and the
maser in this source is clearly unlike those in disk galaxies (but,
see also the discussion for TXS 2226-184). The broad maser in NGC 1052
seemed to drift redward between 1994 March and 1995 December, and
subsequently showed complex structure, with an apparent bifurcation of
the broad peak evident in the 1997 November spectrum. Several of the
spectra, especially those in 1994 November and 1998 February, are
adversely affected by baseline structure. Nevertheless, the maser
profile clearly changed during the monitoring period.
VLBI spectral line observations in 1995 November (Claussen et al.
1998) show that the maser in NGC 1052 arises primarily from two clumps
of gas having distinct but overlapping velocities. The two clumps
align parallel to the long known nuclear radio jet. The maser gas may
be entrained along the jet or perhaps a disk lies in front of one side
of the jet, in which case the masers may originate in gas amplifying
the background continuum emission of the jet (in NGC 4258 the maser
disk projects perpendicular to the radio continuum jet). It is not
clear whether the broad line emission represents gas being accelerated
by the jet or whether it is unrelated to the gas dynamics. It is
possible that the profile changes result simply from gas at different
line-of-sight velocities being lit up with maser emission at different
The GBT spectrum shows that in 2002 April, after a lengthy gap from
the previous spectrum, the maser had dimmed and possibly broadened.
That the emission lacks narrow lines is counter to the typical maser
profile, and the reason for the smooth, broad profile remains unknown.

9. 2003AJ....126.2237D
Re:NGC 1052
4.4. Ellipticals with Radio Cores
Several radio-excess galaxies belong to the sample of elliptical
galaxies with radio cores studied by Slee et al. (1994) and mentioned
in section 3.1: NGC 612 (F01317-3644), NGC 1052 (F02386-0828),
NGC 2110 (F05497-0728, discussed above), NGC 2911 (F09311+1022),
IC 5063 (F20482-5715, discussed above), NGC 7213 (F22061-4724), and
IC 1459 (F22544-3643). The radio cores in elliptical galaxies were
typically found by these authors to be extremely compact (unresolved
on scales of a few parsecs) and to have a large range of radio powers
[L_{nu}_(4.8 GHz) = 10^21^-10^26^ W Hz-1]. Their high-frequency
spectral indices are typically inverted or flat (<{alpha}>~0.3,
S_{nu}_ is proportional to {nu}^{alpha}^), as a result of absorption
consistent with SSA or FFA. These objects have a range of radio power
and radio excess, but low FIR luminosities [{nu}L_{nu}_(60 micron) <

10. 2002ApJS..139....1T
Re:NGC 1052
NGC 1052 (L1.9) .-ASCA results are presented in Guainazzi &
Antonelli (1999) and Weaver et al. (1999). Detection of hard X-rays up
to ~200 keV with Beppo SAX is reported in Guainazzi et al. (2000).
A heavily absorbed continuum, which indicates the presence of an
obscured AGN, is clearly seen in the ASCA spectrum. Systematic
undulations in the residuals were seen in the fits using a partially
covered power-law model or a RS plus absorbed power-law model. The
best-fit model we obtained is a RS plus partially absorbed power-law
model. The resulting photon index of 1.67^+0.57^_-0.40_ is similar to
those found in luminous AUNs and in other objects presented in this
paper. Since the photon index depends on the assumed spectral model
(see tables in this paper and Weaver et al. 1999), the very flat
spectral slope obtained by Guainazzi & Antonelli (1999) and Guainazzi
et al. (2000) ({GAMMA}~ 1.4) should be taken with caution. The thermal
plasma component in the best-fit model plausibly can be attributed to a
hot gaseous halo associated with the elliptical host of NGC 1052.

11. 2002A&A...386...97J
Re:PKS B0238-084
NGC 1052 LINER-type elliptical with inverted radio spectrum.

12. 2001AJ....122..653R
Re:NGC 1052
NGC 1052: The faint structure in the residual image is most likely
associated with the gas and dust complex seen in optical images.
Pogge et al. (2000) argue that the morphology of the optical emission is
reminiscent of ionization cones found in Seyfert galaxies.

13. 2000ApJS..131...95F
Re:VSOP J0241-0815
J0241-0815 (NGC 1052). - Our image agrees well with that reported by
Kellermann et al. (1999).

14. 2000ApJ...530..688A
Re:NGC 1052
NGC 1052.-This galaxy is the prototypical LINER. NGC 1052 is now
known to show broad Balmer lines in polarized light (Barth et al. 1999),
which makes it another AGN-dominated LINER. The properties of this LINER
together with the infrared spectroscopy were discussed in detail in
Alonso-Herrero et al. (1997).

15. 1998AJ....116.2682C
Re:IRAS 02386-0828
NGC 1052. Elliptical galaxy, Seyfert 2. Optical position from Argyle &
Eldridge (1990). Inverted radio spectrum, radio variable. VLA
D-configuration 4.86 GHz map in Condon, Anderson, & Broderick (1995);
flux density S = 2480 mJy at 4.85 GHz.

16. 1998AJ....115.1295K
Re:TXS 0238-084
0238-084.--This bright elliptical galaxy, NGC 1052, has two jets, each
containing multiple components moving away from the AGN in opposite directions.
The central core is not visible in our 2 cm image. Diamond et al. (1998) report
two H_2_O maser complexes located in the inner part of the western jet.

17. 1998A&AS..128...75P
Re:NGC 1052
4.3.3. NGC 1052
This galaxy is a well known E2 elliptical with gaseous disk (Davies et al.
1986). A detailed description of that object has been done by Plana &
Boulesteix (1996). It has also been discovered a double gaseous component in
that object.

18. 1997ApJS..112..391H
Re:NGC 1052
NGC 1052.--This historically important object inspired much of the early
discussion on the relative contribution of shocks and photoionization to the
excitation of LINERs (Fosbury et al. 1978; Keel & Miller 1983; Rose & Tripicco
1984). We confirm the presence of broad H{alpha} emission (f_blend_~32%; FWHM
~1950 km s^-1^) suspected in Paper I. The evident asymmetry of the narrow lines
and the substantial rotational broadening (FWHM~480 km s^-1^), conspire to make
the fitting rather tricky. Nevertheless, a reasonably good fit can be achieved
using the model derived from the [S II] lines (Fig. 4e), and all three fitting
methods give consistent results for the broad H{alpha} flux. The detection of
broad H{alpha} furnishes strong evidence that the nucleus of NGC 1052 should
indeed be regarded as active.

19. 1995A&A...297..643W
Re:NGC 1052
NGC 1052. This is a moderately luminous galaxy of type E4 with apparent
normal stellar kinematics (Schechter & Gunn 1979). However, the central
region is spectroscopically unusual with bright and broad line emission
(Davies & Illingworth 1986). NGC 1052 is the brightest member of a small
group which together with the NGC 1069 group makes up the Cetus I
cluster. HI gas has been observed with the VLA (van Gorkom et al. 1986)
and is found to be situated in a rotating disk whose projected major axis
is close to that of the optical galaxy. The radius of the HI structure is
~3 times that of the optical extent of NGC 1052. The HI gas appears to
have a flat rotation curve with a velocity of 200 km s^-1^. The rotation
axis of the HI gas is closely aligned with that of the ionized gas in the
center, but is shifted 63^deg^ with respect to that of the old stellar
population. We observed NGC 1052 with both the 30-m (Fig. 1) and the 15-m
SEST (Fig. 2a) telescopes, without detecting any CO emission. This is in
contrast to the results of Wang et al. (1992b) who report a relatively
strong CO(J = 1-0) signal obtained with the Nobeyama 45-m telescope. The
peak strength of their profile is 150 mK (T_mb_), which is much higher
than our rms noise of 6.5 mK. We have no explanation for this
discrepancy. Our three sigma upper limit corresponds to an H_2_ mass of
<= 3 x 10^7^ M_sun_.

20. 1994CAG1..B...0000S
Re:NGC 1052
NGC 1052 Group
Nov 6/7, 1980
12 min
NGC 1052 is the eponymous member and
the brightest galaxy in the NGC 1052 group,
which includes NGC 991, 1022, 1033, 1035,
1042, 1047, 1048, 1051, and NGC 1052 here.
Many of these are late-type galaxies shown in this
atlas. There are also many dE dwarf candidates
in the group. The mean redshift from the
available data for group members is = 1500 km/s.

21. 1994A&AS..105..481M
Re:NGC 1052
NGC 1052: The e_4_ coefficient oscillates about zero (see BDM88). As
shown above in Fig. 3, there is a significant photometric evidence for a
disk, hence the adopted diE type.

22. 1976RC2...C...0000d
Re:NGC 1052
Brightest galaxy in NGC 1052 Group.
"Active" radio galaxy.
Description and Precise Position:
Ap. J. (Letters), 151, L75, 1968.
Photometry: (10 microns)
Ap. J. (Letters), 159, L165, 1970
Ap. J. (Letters), 176, L95, 1972.
C.R. Acad. Sc. Paris, B, 268, 1214, 1969.
Astr. Ap., 19, 405, 1972.
IAU Symp. No.44, 54, 1972.
Ap. J. (Letters), 179, L93, 1973.
Radio Observations:
Astrophys. Lett., 2, 187, 1968.
Astrophys. Lett., 6, 49, 1970.
Ap. J. (Letters), 151, L35, 1968.
Ap. J., 157, 481, 1969.
Ap. J., 170, 207, 1971.
Ap. J., 189, 399, 1974.
A.J., 75, 523, 1970.
A.J., 79, 1232, 1974.
Sov. A.J., 13, 881, 1970.
IAU Symp. No.44, 222, 1972.

23. 1964RC1...C...0000d
Re:NGC 1052
Brightest in NGC 1052 Group.
Diffuse, very bright center, smooth.
P.A.S.P., 48, 17, 1936.
Ap. J., 129, 583, 1959.

24. 1963MCG3..C...0000V
Re:MCG -01-07-034
At 0.6 arcmin southwest there is a pretty diffuse companion 18
mag of intensity 4. Type: Sand - E3, vB - E2, Morg - kE4. Redshift:
+1466, G5, {lambda} 3727 of intensity 5 (Lick B 19, 33); Cl = 0.80.

25. 1956AJ.....61...97H
Re:NGC 1052
HMS Note No. 015
Spectrum previously described (Mayall, N.U. 1936, P.A.S.P., 48, 14)
in connection with performance of the spectrograph.

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