Date and Time of the Query: 2019-06-19 T00:39:42 PDT
Help | Comment | NED Home

Notes for object IC 5063

23 note(s) found in NED.

1. 2009ApJ...702.1127R
Re:IC 5063
This Sy2 nucleus is hosted by a merger remnant classified as an elliptical
galaxy (Colina et al. 1991). An obscuring dust lane partially covers the eastern
side of the galaxy. A peculiarity of this source is its strong radio luminosity,
which is 2 orders of magnitude larger than the typical values for Seyfert
galaxies (Colina et al. 1991). From an N-band acquisition image of IC 5063
obtained with T-ReCS/Gemini-South, Young et al. (2007) tentatively found the
nucleus of this galaxy slightly resolved. However, from our T-ReCS Si2 and Qa
band imaging the nucleus appears unresolved, and consequently, we subtracted the
corresponding PSF at the 100% level to derive the nuclear fluxes. From the fit
with the clumpy models, we establish lower limits for three of the parameters
({sigma}>57^deg^, N_0_ > 11, and i > 65^deg^) and an upper limit for the index
of the radial density profile (q < 1.5). The only Gaussian-like distribution
resulting from the fit corresponds to {tau}_V_ (median value of 70+/-^ 31^_23_).
A^LOS^_V_ is calculated to be 780+/-^485^_345_ mag. The galaxy presents one of
the highest L^AGN^_bol_ of the sample (2.4 * 10^44^ erg s^-1^, see Table 9), and
also a high reprocessing efficiency (87%), consistent with the large values of
N_0_ and {sigma} we find. X-ray observations with the ASCA satellite allow us to
infer an intrinsic 2-10 keV luminosity of ~10^43^ erg s^-1^, that is within the
range expected for Seyfert 1 galaxies (Turner et al. 1997). The silicate feature
appears in absorption in the fitted models, in qualitative agreement with mid-IR
spectroscopic observations obtained with T-ReCS/Gemini-South (Young et al.
2007). However, the absorption band appears deeper in our models ({tau}^app^_10
{mu}m_ = 0.94) than in the mid-IR spectrum ({tau}_10 {mu}m_ = 0.33).

2. 2008A&A...483...79R
Re:IC 5063
IC 5063 is classed as a NLRG, having 5 x 10^23^ W Hz^-1^ at 1.4 GHz. The nuclear
component was resolved into a 4"-long linear triple structure at 8.6 GHz by
Morganti et al. (1998). Our 8.4 GHz image (Fig. 6a) with the larger beam of 6.4"
x 5.8" did not resolve the jet, as expected.
We used the upper limits on the H91{alpha} + H92{alpha} line emission to
constrain the properties of the nuclear emission-line regions. We assumed that
the line FWHM was the same as the velocity resolution of the data (from Tables 1
and 2). We modelled each source as a collection of uniform-density spherical H
II regions. The model solutions were constrained to produce an 8.3 GHz free-free
emission equal to 30% of the continuum flux density integrated over the central
region and an H92{alpha} line emission equal to the observed upper limit. The
derived value for the gas density varied between 100 cm^-3^ and 5 x 10^5^ cm^-3^
and the total effective diameter of the H II regions varied between 5 pc to 200
pc with the effective size decreasing with increasing density. The total flux of
ionizing photons required to maintain such nebulae on the limit of our
detectability ranged between 3 x 10^51^ s^-1^ and 2 x 10^54^ s^-1^depending on
density and size of the individual H II regions. This provides upper limits to
the number of O5 stars powering the ionization in the range 100 to 70 000, with
the higher values corresponding to those models whose combination of parameters
yield high free-free continuum emission from the ionized gas.
Parameters derived for typical allowed models are given in Table 3.

3. 2007AJ....134..648M
Re:IC 5063
IC 5063 (Figs. 7.38, 9.38, 20.38): This shows very bright, compact, but resolved
blobs within the nuclear region and some bright filaments along the
southeast-northwest direction. Those could be scattered light from the AGN.

4. 2006A&A...457..425C
Re:[Sdd95] 432a
P432a (IC 5063): N-type. This galaxy has been well studied, with more than 100
papers describing it. According to its spectral type, it is classified as Sy2
(Storchi-Bergman et al. 1990; Busko & Steiner 1992; Bonato et al. 1996).

5. 2006A&A...457..405C
Re:[Sdd95] 432a
P432a (S0 p): this object is a Seyfert 2 (Storchi-Bergmann et al. 1990; Busko &
Steiner 1992; Bonatto et al. 1996, among others). The color map points out small
blue knots within the nuclear region. Dopita et al. (2002) detected H_{alpha}
knots in this peculiar early-type galaxy. The b_4_ distribution indicates that
this lenticular shows a pure elliptical shape (b_4_ ~ 0). The mean values for
the ellipticity distributions are {epsilon}_b_ ~ 0.20, and {epsilon}_d_ ~ 0.26.
The PA distribution is very noisy; however, we considered {DELTA}PA_bd_ ~

6. 2003ApJS..148..327S
Re:IC 5063
5.54. IC 5063 = PKS 2048-57
The ground-based [O III] image of this Seyfert 2 galaxy shows
emission extended over a region larger than ~30", along P.A. =
-65^deg^ (Morganti, Oosterloo, & Tsvetanov 1998; Morganti et al.
1999). The line emission is aligned with the radio emission and the
host galaxy major axis. This galaxy is also known to have polarized
broad emission lines (Inglis et al. 1993). Our [O III] image confirms
the ground-based results but shows only a much smaller portion of the
extended emission, owing to the field of view of the Linear Ramp
Filter (Fig. 13, bottom right). This emission can be represented by a
bicone centered at the nucleus, with opening angle of 60^deg^,
extending by 12" (2640 pc) along P.A. = -65^deg^ and ~3" (660 pc)
along the perpendicular direction. At distances larger than 3" north
of the nucleus the emission seems to split on the two sides of the
host galaxy major axis, giving it the appearance of an X-shaped NLR.

7. 2003ApJS..146..353M
Re:IC 5063
IC 5063 (C)
Although the circumnuclear dust structure is classified as chaotic,
the straight dust lanes crossing to the north of the nucleus suggest
that they could have a spiral morphology if viewed at a smaller
inclination. Host galaxy dust may be responsible for its Seyfert 2
classification as the peak nuclear brightnesses in V and H are not
coincident. There are also pronounced ionization cones extending to
the east and west of the nucleus.

8. 2003AJ....126.2237D
Re:IC 5063
4.2. Seyfert Galaxies
IC 5063 (F20482-5715) has properties in common with both Seyfert
galaxies and radio galaxies (Colina, Sparks, & Macchetto 1991). It is
an X-ray-bright Seyfert 2 galaxy, with intermediate radio excess (u =
1.16) and low radio power [L_{nu}_(4.8 GHz) = 10^23.5^ W Hz-1]. The
radio emission arises from a compact double-lobed source 1.3 kpc in
extent (Morganti et al. 1999b). The host galaxy is a nearby elliptical
with dust lanes, so it has probably undergone a recent merger. The
galaxy has a moderate FIR luminosity of {nu}L_{nu}_(60 micron) =

9. 2003AJ....126.2237D
Re:IC 5063
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..143...47D
Re:IRAS 20481-5715
IRAS 20481-5715 (IC 5063).---This is a well-known merger remnant with
a very bright Seyfert 2 nucleus (Kewley et al. 2001b; Colina, Sparks,
& Macchetto 1991). Our H{alpha} image of this galaxy confirms the
presence of dust lanes and bright H{alpha} knots (Heisler & Vader
1994; Turner et al. 1997) in this galaxy.

11. 1999A&AS..137..457M
Re:IC 5063
IC 5063 (PKS 2048-57): This is an early-type galaxy hosting a Seyfert 2
(Colina et al. 1991). Its radio luminosity is nearly 100 times larger
than typical values for nearby Seyferts. Our ATCA radio map (Fig. 14,
see also Morganti et al. 1998) resolves a linear radio structure
comprising three compact features aligned along PA_radio_ = 305^deg^.
The spectral index is steep: {alpha}_6_^20^ = -1.1 (Danziger et al.
1981). The optical line-emitting gas traces an X-shape (Morganti et al.
1998), and the radio emission coincides with the inner part of the line
emitting region. Recent H I observations with ATCA and VLBI reveal a
well defined H I disk aligned with a morphologically similar system of
dust lanes (Morganti et al. 1998; Oosterloo et al. 1998). PTI
observations measure a flux of 140 mJy at 13 cm and 10 mJy at 3 cm Slee
et al. (1994).

12. 1997ApJS..113...23T
Re:IC 5063
A22. IC 5063
IC 5063 has a radio power 2 orders of magnitude greater than that of typical
Seyfert galaxies; thus, it is classified as a Seyfert 2 galaxy and as a narrow
line radio galaxy (Ulvestad & Wilson 1984). This AGN has an elliptical host,
with dust lanes covering the nucleus and extending outwards (Colina, Sparks, &
Macchetto 1991).
A Ginga observation showed a power-law photon index {GAMMA}=1.5 with
N_H_=2x10^23^ cm^-2^. The intrinsic 2-20 keV X-ray luminosity was inferred to
be 10^43^ ergs s^-1^ within the range expected for Seyfert 1 galaxies (Koyama
et al. 1992). The ASCA data are best fitted by a double power-law model with
the hard component and absorption in good agreement with the Ginga result and a
slightly steeper unabsorbed continuum component. The ROSAT PSPC observation
shows a pointlike nuclear source adjacent to a faint extended source (which is
not close enough or bright enough to contaminate the ASCA spectrum

13. 1995AJ....110...87H
Re:IRAS 20481-5715
20481-5715 (IC 5063, PKS 20481) [Fig. 1(dd)]: H{alpha} imaging has
uncovered several bright knots in this galaxy. Digitally enhanced
broadband optical images taken under subarcsec seeing conditions (Heisler
& Vader 1989) have revealed a similar structure. The relative brightness
of these knots within 3" apertures are similar, thus we cannot rule out
the possibility that a bisecting dust lane is causing their appearance.
The fact that the dust lanes visible in optical continuum images are
orientated in the same direction as the nuclei, and not perpendicular
argues against this. The H{alpha} emission is strongly centrally
concentrated into multiple knots or nuclei in the center of the galaxy,
unlike the continuum emission. The radio source is much weaker than in
typical radio galaxies, but is unusually strong for Seyferts. The FIR-to-
radio spectral index is among the flattest for our sample. A 21 cm radio
continuum map reveals an extended source (8 kpc) coinciding with the
optical center of the galaxy, and a small mass of ionized and neutral
hydrogen which is characteristic of early-type galaxies (Danziger et at.

14. 1995A&A...297..643W
Re:IC 5063
IC 5063, This galaxy is usually classified as S0 but the luminosity
profile follows the r^1/4^ law (Colina et al. 1991). It has strong and
extended high excitation optical line emission, a Seyfert 2 type nucleus,
an extensive dust component and a double radio source. IC 5063 is a
merger remnant candidate. We detect 3.0 x 10^8^ M_sun_ of H_2_ in this

15. 1994CAG1..B...0000S
Re:IC 5063
S0_3_(3) pec/Sa
Aug 16/17, 1979
103aO + GG385
45 min
The only arms visible in IC 5063 are the
dust lanes silhouetted against the bulge and
against the disk in the lower right-hand side of
the print. The high visibility of the dust is due to
the high inclination of the disk to the line of sight.

16. 1994AJ....107...35H
Re:IRAS 20481-5715
20481-5715 (IC 5063, PKS 20481). Numerous dust lanes are clearly
visible in the northeast section of this well studied peculiar galaxy
(e.g., Caldwell & Phillips 1981, Danziger et al. 1981). It has been
previously classified as both an elliptical and an S0 galaxy. A contour
plot of the original CCD image displays smooth, elliptical isophotes
[Fig. 15(v)], while a masked image clearly delineates the dust lane
structure, and reveals a peanut-shaped nucleus, which has been proposed
to be the result of multiple nuclei (Heisler et at 1989a). Our H{alpha}
imaging has indeed revealed that there are three nuclei (Heisler et at
1989b), which is discussed in more detail in Paper III of this series.
The radio source is weaker than for typical radio galaxies, but unusually
strong for Seyfert galaxies. A 21 cm radio continuum map reveals an
extended source (~8 kpc) coinciding with the optical center of the
galaxy, and a small mass of ionized and neutral hydrogen which is
characteristic of early type galaxies (Danziger et at 1981). This galaxy
has a very red near-infrared nuclear source (K-L = 2.1) and a high
polarization (17%), which requires a contribution from a nonthermal
synchrotron source (Hough et at 1987). The presence of an active nucleus
is supported by a very high excitation emission-line spectrum
(Bergeron et al. 1983).

17. 1994A&AS..108...61F
Re:IRAS 20481-5715
IRAS 2048-572 (PKS 2048-57). This object has a Seyfert-like spectrum
extending by at least 4" on either side of the nucleus, including
relatively strong [O I]. There is a large velocity gradient, the emission
lines 3" east and west of the nucleus being shifted by 230km/s red- and
bluewards respectively, relative to the nucleus.

18. 1992ApJS...80..137J
Re:MRC 2048-572
Pair of unrelated sources, the east a point source.
The west source has a weak projection
linked to it extended at right angles to the separation. Mapped
by Danziger et al. (1981).
Galaxy 12.0 m, IC 5063, S0 with a dust-lane and in
a cluster, at 20 48 12.78 -57 15 31.8, 19 arcsec south-east from the east
peak and 76 arcsec from the centroid of the double, see Mills et al.
(1961) and Danziger et al. (1981). z = 0.0113, Whiteoak (1972). The
radio morphology is unusual for a radio galaxy double and the ID is
associated with the east source only, with the west source unrelated. Blank
optical field for the west source.

19. 1988A&AS...75..273D
Re:IC 5063
IC 5063 is a narrow line active galaxy surrounded by a very large
ionized nebulosity, which we have already analysed in detail (Bergeron
et al., 1983 , and references therein). Its UV continuum has also been
discussed by BD86, who showed this galaxy to be an obscured Seyfert 1
object, similar to those discussed above.

20. 1985SGC...C...0000C
Re:IC 5063
Plate 892
Strong dust lane. Background group: brightest is cE0 3.1 south-preceding-
preceding. IC 5064, SB?(s)0/a, 11.0 south-following.
Plate 1577
Bright bulge, strong dark lane. Several companions nearby. Overexposed
center with dark lane. Faint companion superposed 0.85 north-preceding.
Group 3' south-preceding.

21. 1982ESOU..C...0000L
Re:ESO 204812-5715.5
=ESO 187- G 23
absorption lane
brightest in group

22. 1976RC2...C...0000d
Re:IC 5063
= PKS 2048-57
Coordinates and Photograph:
A.J., 79, 453, 1974.
Australian J. Phys., 25, 233, 1972.

23. 1964RC1...C...0000d
Re:IC 5063
Small, bright nucleus.
Radio Source (?), possible identification:
Australian J. Phys., 14, 497, 1961.

Back to NED Home