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Notes for object IC 1459

22 note(s) found in NED.


1. 2009MNRAS.397.2148G
Re:IC 1459
Although Lauer et al. (2005) provide a V-magnitude for the nucleus of IC 1459,
the blue point source (Forbes, Franx & Illingworth 1995; Tomita et al. 2000;
Verdoes Kleijn et al. 2002) is a LINER associated with an AGN that has been
detected in X-rays (Fabbiano et al. 2003). We have excluded this object, due to
the order of magnitude uncertainty on its BH mass (Cappellari et al. 2002).

2. 2009ApJ...703.1034Y
Re:IC 1459
IC 1459. The X-ray emission is well fitted by a jet, while the contribution of
the ADAF is constrained by the radio data to be at a very low level. Given that
L_2-10 keV_ > L_X,crit_, the origin of X-ray emission is apparently inconsistent
with the prediction of YC05, but, as mentioned above, we should be wary about
the overinterpretation of individual sources, especially in this case where
L_X_/L_X,crit_ is only marginally greater than unity. The value of p is 1.9,
formally but not significantly smaller than 2. Fabbiano et al. (2003) also
fitted the X-ray spectrum with a jet model, but with a much larger p = 2.78. The
discrepancy in the value of p is because they do not consider the effect of
radiative cooling on the energy distribution of electrons. In other words, the
value of p adopted there is the spectral index of the steady distribution rather
than the injected distribution.

3. 2006A&A...460...45G
Re:IC 1459
IC 1459 (IC 5265). This galaxy presents an unresolved nuclear source on top of a
diffuse halo at high energies (Fig. 5), in agreement with the classification by
Satyapal et al. (2004). It hosts a Super-massive black hole (2 x 10^9^
M_sun_, Cappellari et al. 2002) but with rather moderate nuclear activity.
Fabbiano et al. (2003) find that it shows a rather weak (L(2-10 keV) =
8.0 x 10^40^ erg s^-1^ ) unabsorbed nuclear X-ray source with
{GAMMA} = 1.88 and a faint FeK{alpha} line at 6.4 keV. These characteristics
describe a normal AGN radiating at sub-Eddington luminosities, at $3 x 10$-7
below the Eddington limit. They suggest that ADAF solutions can explain the
X-ray spectrum, but these models failed to explain the high radio power of its
compact source (Drinkwater et al. 1997). Our fitting parameters are in a
remarkably good agreement with theirs ( {GAMMA }= 1.89, kT = 0.30 keV and
L(2-10 keV) = 3.6 x 10^40^ erg s^-1^).

4. 2006A&A...447...97B
Re:IC 1459
IC 1459: Fabbiano et al. (2003) detected an un-absorbed nuclear X-ray source
(~6500 total counts), with a power law slope {GAMMA} = 1.88.

5. 2005ApJ...635.1031B
Re:IC 1459
IC 1459.-This galaxy has among the lowest Galactic H I column in the sample and
very little reddening (1.19 x 10^20^ cm^-2^), although it has the usual
Galactic atomic absorption lines that can be seen on the stellar continuum
(Fig. 24). The airglow lines are strong during the daytime observing, so
although only 25% of the observing time was at night (only 2.5 ks), the
night-time data are better for the analysis of the O VI region, while the total
data set is better for analysis in the C III region. There is a broad emission
line coincident with the strong redshifted O VI line, which is relatively
uncontaminated by Galactic absorption features (also present in the LiF2b
channel). The weaker O VI line is not detected at a statistically significant
level, but as it is half the strength of the O VI {lambda}1032 line, this is
not inconsistent with a detection of the O VI {lambda}1032 line. The C III
{lambda}977 line is also detected with a flux that is poorly determined because
it is unclear where to mark the boundaries of the l ine. If we use the single
peak, blueward of line center, the line width is 0.8 A (line flux of 1.3 x
10^-14^ ergs cm^-2^ s^-1^) and a line center at 982.0 A (expected to be at
982.5 A). If we use the weaker red part of the line as well, the line center is
exactly that expected for the recession velocity, the line width becomes 2.1 A
(at a line flux of 2.1 x 10^-14^ ergs cm^-2^ s^-1^). Given the uncertainties
associated with each of the lines, it is difficult to compare the O VI and C
III lines. This galaxy has a strong radio source and is known to be a LINER.

6. 2005ApJ...622..235T
Re:IC 1459
IC 1459. Chaotic dust absorption visible; galaxy crossed by a disk of ionized
gas; H I not detected, but CO (H2) is; heavy dust lane in 1" with more
chaotic and patchy dust farther out; central starlight core is bluer; ionized
gas disk; stellar shells; bright point source in center; powerful compact
radio-core source

7. 2004A&A...424...91E
Re:PKS J2257-3627
J2257-3627 was identified as a GPS source in this ATCA monitoring
program (Tingay et al. 2003a). As a low-redshift galaxy, high linear
resolution studies over a range of wavelengths have been possible, and,
as discussed in Tingay et al. (2003a), there is strong evidence for
merger activity in the galaxy which is quite likely to be related to the
GPS spectrum.

8. 2003AJ....126.2237D
Re:IC 1459
.
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) <
10^11^L_solar_].

9. 2002ApJ...574..740T
Re:IC 1459
IC 1459.
The mass estimate that we use (Cappellari et al. 2002), based on
stellar kinematics, is much larger than an earlier estimate by the
same group from gas kinematics, (2-6) x 10^8^ M_sun_ (Verdoes
Kleijn et al. 2000). The mass estimate from stellar kinematics is
much more reliable, since the gas rotation curve is asymmetric and
non-Keplerian. The dispersion also comes from Cappellari et al. (2002).

10. 2002A&A...386...97J
Re:PKS B2254-367
= IC 1459.

11. 2001A&A...374..421B
Re:IC 1459
4.2 IC 1459
The absolute magnitude and the intrinsic diameter of this galaxy (see
Table 1) are both characteristic of a giant elliptical. IC 1459 has a
massive counterrotating stellar core (M ~ 10^10^ M_sun_, according to
Franx & Illingworth 1988) and its outer stellar isophotes are twisted,
an indication that the stellar body is triaxial. This galaxy shows dust
absorption in the central 10" (Sparks et al. 1985) and faint pseudo-arms
in the outer part (r ~ 3.5' Malin 1985). The counterrotating core, which
hosts a compact radio source (Franx & Illingworth 1988), has a radius of
~2" (200 pc) and a projected spin velocity of 170 +/- 20 km s^-1^. On
dynamical grounds, the core can be described as a disk, rather than as an
ellipsoid. In contrast, the outer directly-rotating stellar body has a
slower rotation figure; it reaches ~45 +/- 8 km s^-1^ at r = 40" (4 kpc).
The galaxy is crossed by a disk of ionized gas, whose emission is evenly
detected up to r = 35" (3.5 kpc); the ionized gas rotates in the same
direction than the outer stellar body, but at a higher speed (350 km s^-1^)
(Franx & Illingworth 1988). Therefore counterrotation in this galaxy seems
confined to the inner core and affects only the stars. X-ray emission peaks
in the galaxy nucleus (Roberts et al. 1991), an indication of central
activity.
Walsh et al. (1990) report a negative detection of HI emission, the
upper limit on M_HI_ being ~10^7^ M_sun_. Our ^12^CO(J = 1 - 0) spectrum
also shows a negative detection for molecular gas emission. In contrast,
the integrated ^12^CO(J = 2 - 1) spectrum shows clearly a narrow emission
line of FWHM ~ 35 km s^-1^, centered at 1782 km s^-1^ (see Fig. 1). The
velocity centroid of CO is redshifted by ~100 km s^-1^ with respect to the
galaxy systemic velocity (v_sys_ = 1691 km s^-1^). This discrepancy of
velocity centroids and the narrowness of the ^12^CO(J = 2 - 1) line both
indicate that emission cannot come from a rotating molecular gas disk in
equilibrium that could be associated with the ionized disk or,
alternatively, with the counterrotating core. In the discarded scenario of
a molecular gas disk, the CO line should be 3-5 times wider than is
actually observed, considering the size of our beam. Instead, the CO
profile may come from a Giant Molecular Association (GMA). Furthermore,
the derived upper limit on the mass of molecular gas,
M_mol_ < 2 x 10^7^ M_sun_, is noticeably low. Additional support for the
interpretation outlined above comes from the high resolution deconvolved
V-band images of the dust distribution, obtained with the HST. The
morphology of the dust lane source in the inner 4" of the galaxy is very
irregular and indicates non equilibrium motions (Forbes et al. 1994).
Finally, the estimated 3 {sigma} upper limit on the (J = 2 - 1)/(J = 1 - 0)
ratio (>1.3) suggests that the CO emission might be partly optically thin.
Similar molecular gas components have been found in other early-type
galaxies, such as NGC 404 (Wiklind & Henkel 1990), classified as a gas
accreting elliptical with a minor axis dust lane (Bertola & Galletta 1978).
This GMA may be a residual of one of the galaxies involved in the passed
merger that is supposed to be at the origin of IC 1459
(Franx & Illingworth 1988).

12. 1997ApJ...481..710C
Re:IC 1459
A heavy dust lane is present in the innermost ~1.1", tilted at
~15^deg^ from the apparent major axis. The lane is asymmetric with
respect to the center, although it is present on both sides of it. More
chaotic patchy dust is present farther away from the nucleus, and other
filamentary absorption features show up at ~2" from the very center.
Inside the dust lane region, a sharp increase in ellipticity (whose
amplitude is larger in V than in I) is observed, together with ~20^deg^
twisting and a C_4_ large and positive in the I band. However, at the
same radii, the C_4_ values show a large scatter in the V band, as do the
other terms of the Fourier expansion. All these features are much reduced
in amplitude in the isophotal parameters derived from the dust-improved I
frame. We conclude that the major features are induced by the dust rather
than by real variations in the galactic structure or in the stellar
population and that there is little photometric evidence for the nuclear
stellar disk suggested by the analysis of the line-of-sight velocity
distribution (Franx & Illingworth 1988). The V - I color map traces the
dust distribution and suggests the presence of a spiral-like structure
reminiscent of that detected on larger scales on deep photographs (Malin
1985) and also from the ionized gas distribution (see, e.g., Forbes,
Sparks, & Macchetto 1990). The central point source (V ~ 18.4, M_V_ ~
-12.7) already detected by F95 stands out in the color map owing to its
V - I color (~1.0 mag), which is bluer than the surrounding stellar
population.

13. 1995AJ....109.1988F
Re:IC 1459
IC 1459: This galaxy is a giant elliptical in a loose group with
several spiral galaxies. It reveals a variety of indicators suggesting a
recent merger, such as a nuclear dust lane (Sparks et al. 1965), ionized
gas disk (Forbes et al. 1990) and shells (Forbes, et al. 1994). It also
contains the fastest known counter-rotating core (Franx & Illingworth
1988). Planetary camera imaging of the nuclear region has been presented
elsewhere by Forbes et al. (1994). We found a bright (V~18.3^m^) point
source at the galaxy nucleus; making it the only galaxy in our sample to
show such an obvious feature. Photometric evidence for a disk, associated
with the distinct core, was ambiguous (see, also Fig. 3). An irregular
dust distribution was seen near the nucleus, which may indicate ongoing
infall of material. The nucleus reveals a powerful compact radio core
(Sadler et al. 1989) which appears to be variable with time (Slee et al.
1994).

14. 1994CAG1..B...0000S
Re:IC 1459
Grus Group
E4
CD-572-S
Oct 8/9, 1978
103aD + GG495
30 min
IC 1459 is the brightest galaxy in the Grus Group, which is a
loose group of wide extent (Sandage 1975b). IC 1459 is the brightest
member and is isolated, having only a few spirals nearby. The two
centers of concentration of the group are IC 1459 and NGC 7496 (SBc;
panels 303, S10), NGC 7531 (Sbc; panel 175), NGC 7582 (SBab; panel
122), NGC 7590 (ScII), and NGC 7599 (ScII). The brightest galaxy in
this second concentration is NGC 7582. The mean redshift of the group
is = 1580 km/s.
The nearest Dreyer galaxy to IC 1459 is IC 5265 (Sb? on edge),
6.5' distant, which is a projected linear separation of 60 kpc.

15. 1994AJ....108.2128C
Re:PGC 070090
PGC 070090 = IC 1459. Type = .E.3+.. , S_T_ = V.

16. 1994A&AS..105..341G
Re:IC 1459
This galaxy is an archetypical merger candidate in view of the presence
of a fast, counter-rotating stellar core (Franx & Illingworth 1988).
Furthermore, spiral-like structure has been found in both the outer
regions using a deep photograph (Malin 1985) and the distribution of
extended ionized gas (Goudfrooij et al. 1990). The B-V image (cf. also
Sparks et al. 1985; Goudfrooij et al. 1990) shows an asymmetric
distribution in the inner ~15" which is most probably due to dust
absorption, and a general similarity to the H{alpha}+[NII] image. A
small, low surface-brightness galaxy is found at 35" northwest of the
galaxy nucleus. Strongest IRAS source at 60 and 100 micron of the
sample. Compact, powerful nuclear radio source. X-ray emission.

17. 1994A&AS..104..179G
Re:IC 1459
The S3 profiles are different in the B, V, and I passbands. Asymmetric
colour index image (cf. Goudfrooij et al 1990). These features are most
probably due to dust absorption. Otherwise regular elliptical from the
surface photometry, but with a counter-rotating core (Franx & Illingworth
1988). Strongest IRAS source at 60 & 100 microns of the sample.
Relatively powerful nuclear radio source. X-ray emission.

18. 1993A&A...280..409B
Re:IC 1459
IC 1459: The emission is roughly aligned with the stellar major axis.
Goudfrooij et al. (1990) suggest that the ionized gas disk shows weak
spiral structure. Our continuum image shows no conspicuous features,
though Goudfrooij et a]. report a central red feature in their B-V colour
map which appears to be due to dust absorption, and Sparks et a]. (1985)
also identify IC 1459 as a dusty elliptical. The galaxy is an X-ray
source (Canizares et a]. 1987). Franx & Illingworth (1988) have shown
that IC 1459 has a counter-rotating stellar core confined to the inner 10
arcsec. Since the radial extension of this kinematically decoupled sub-
structure matches the size of the elongated emitting region, the origin
of the gaseous disk and the counter-rotating stellar core could be
related to a merger the galaxy underwent in the past. However, although a
sharp change in the slope of the Mg_2_ line strength gradient has been
observed in the nuclei of other ellipticals with kinematically decoupled
cores (Bender & Surma 1992), Carollo et a]. (1993) saw no evidence of
such a change in the inner 10 arcsec of IC 1459.

19. 1985SGC...C...0000C
Re:IC 1459
= IC 5265
Plate 756
1st in group.

20. 1982ESOU..C...0000L
Re:ESO 225423-3643.8
=ESO 406- G 30
in cluster

21. 1976RC2...C...0000d
Re:IC 1459
= IC 5265
Pair with IC 5264 south-preceding.
Magnitude and colors reduced using dimensions on POSS:
(4.5: arcmin x 3.4: arcmin).

22. 1964RC1...C...0000d
Re:IC 1459
= IC 5265
Photograph and Photometry:
M.N.R.A.S., 112, 606, 1952.


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