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Notes for object 2MASX J05210136-2521450

17 note(s) found in NED.

1. 2008A&A...484..341R
Re:IRAS 05189-2524
Observations of this Seyfert 2 galaxy at micron show a completely unresolved
core with no deviations from the PSF larger then 1 {sigma}. An unresolved core
is also reported by Siebenmorgen et al. (2004) with 8.6, 10.4 and 11.9 micron
flux densities of 420, 420 and 570 mJy, respectively, and by Soifer et al.
(2000), who present a 12.5 micron image and 12.5 24.5 micron fluxes.

2. 2007ApJ...671.1388D
Re:IRAS 05189-2524
A2.2. IRAS 05189-2524 Figure 12 shows the H-band spectrum integrated across two
segments of the NACO slit, located on either side of the nucleus. It shows that
even away from the nucleus, the depth of the stellar absorption features is only
a few percent. We have therefore decomposed the data into the stellar and
nonstellar parts using both the stellar absorption features and the spectral
slope of the continuum. The latter method has been shown to work for
well-sampled data by Davies et al. (2004a). The rationale is that the hot dust
associated with the AGN will be much redder than the stellar continuum. An AGN
component is also expected to be unresolved for a galaxy at the distance (170
Mpc) of IRAS 05189-2524. The spectral slope was determined by fitting a linear
function to the spectrum at each spatial position along the slit. It is plotted
as a function of position in Figure 13, showing a single narrow peak. A Gaussian
fit to this yields a spatial resolution of 0.12" (100 pc) FWHM. The stellar
continuum, also shown in Figu re 13, has been determined by summing the four
most prominent absorption features: CO(4-1), Si i, CO(5-2), and CO(6-3). While a
Gaussian is not an optimal fit to this profile, it does yield an approximate
size scale, which we find to be 0.27" FWHM. Quadrature correction with the
spatial resolution yields an intrinsic size of 0.25" (200 pc). As a cross-check,
in the figure we have compared the sum of these two components to the full
continuum profile. The good match indicates that the decomposition appears to be
Remarkably, the 200 pc size of the nuclear stellar light is very similar to
that of the 8.44 GHz radio continuum map of Condon et al. (1991). With a beam
size of 0.50" * 0.25" , they resolved the nuclear component to have an intrinsic
size of 0.20" * 0.17". In contrast to radio sources that are powered by AGNs and
have brightness temperatures T_b_ >> 10^5^ K, the emission here is resolved and
has a low brightness temperature of ~4000 K. This implies a star-forming origin.
Using their scaling relations further suggests that the flux density corresponds
to a supernova rate of ~1 yr^-1^.

3. 2007ApJ...671.1388D
Re:IRAS 05189-2524
As described in {section} 3, we have estimated the stellar luminosity by
comparing the H-band spectrum to a template star to correct for dilution. We
used HR 8465, a K1.5 I star for which the equivalent width of CO(6-3) is 4.2 A,
within the 4-5 A range predicted by STARS in Figure 2. By extrapolating from the
spatial profiles along the slit, we have estimated the integrated equivalent
width within a 1.1" aperture, for which Scoville et al. (2000) gave an H-band
magnitude of 11.83. Using all four features above, we find for the template W =
14.4 A and for IRAS 05189-2524 W_CO(6-3) = 6.7 A A. This implies that in the
central 1.1", approximately 45% of the H-band continuum originates in stars.
Using the color conversion H-K = 0.15 from Figure 3 (see {section} 3), we find a
K-band magnitude for the stars of 12.55 mag and hence a K-band stellar
luminosity of 2 * 10^9^ L_sun_. Putting these results together, we derive a
ratio of supernova rate to K-band stellar luminosity of
{nu}_SN_(yr^-1^)/L_K_(10^10^ L_sun_) ~ 5. Applying corrections for extinction
and an AGN contribution would tend to decrease this ratio.
As a second diagnostic, we use W_Br{gamma}_ = 4-5 A. We estimate the dilution
of the K-band continuum via two methods. First, we measure W_Na I_ = 0.3 A,
indicating a stellar fraction of 0.10-0.15. A consistency check is provided by
the H-band dilution, which we extrapolate to the K band using blackbody
functions for the stars and dust assuming characteristic temperatures of 5000
and 1000 K, respectively. This method suggests that the K-band stellar fraction
is around ~0.14. Hence, correcting the directly measured equivalent width of the
narrow Br{gamma} for the nonstellar continuum yields W_Br{gamm}_ = 4-5 A.
Since IRAS 05189-2524 is close to face-on (Scoville et al. 2000), it is not
straightforward to make a reliable estimate of the dynamical mass. Nevertheless,
requiring v_SN_/L_K_ to be high while W_Br{gamma}_ is low already puts
significant constraints on the star formation history. Thus, although the star
formation has probably ended, the age is unlikely to be greater than 100 Myr and
could be as low as 50 Myr where {nu}_SN_/L_K_ peaks. For such ages the ratio
L_bol_/L_K_ is in the range 100-150. Hence, for the young stars within 0.55"
(450 pc) of the nucleus we find L_bol_ ~ (2-3) * 10^11^ L_sun_, about 20% of
L_bol_ for the galaxy.

4. 2007A&A...461.1209D
Re:IRAS 05189-2524
IRAS 05189-2524: The BeppoSAX data set was previously analyzed by
Severgnini et al. (2001). The model reported here is similar to what was
previously presented. The photon index observed here is slightly steeper
({GAMMA}=2.8+/-0.3) with respect to what was presented before
({GAMMA}=2.4+/-0.1, Severgini et al. 2001). A different modelization of
the soft component present at E<=2.5 keV (a power law is used in the
present work while Severgini et al. (2001) used a thermal component) may
have caused this effect, leading here to an underestimation of the
importance of the soft component.

5. 2004MNRAS.353.1151S
Re:APMUKS(BJ) B051859.09-252441.7
F05189-2524. Has been studied as part of the H_2_0 maser emission survey
by Greenhill et al. (2002). In addition, F05189-252 has also been
studied extensively in CO. Rigopoulou et al. (1996) studied molecular
line CO (2-1) observations of ULIRGs and Mirabel et al. (1990) studied
CO(1-0) in emission in F05189-792.

6. 2003MNRAS.343..585F
Re:IRAS 05189-2524
05189-2524. This object appears to be a late-stage merger. It possesses
a single, compact, very red nucleus with a Sy2 spectrum (Veilleux et
al. 1995), bisected by a dust lane (Scoville et al. 2000). Young et
al. (1996) observed broad lines in polarized flux in this object,
suggesting the presence of an obscured AGN. Later observations (Dudley
1999) observed the 11.3 {microns} dust feature, suggesting that this
object also contains a buried starburst. The X-ray spectrum (Risaliti et
al. 2000) is well fitted by a two-component model, consisting of a power
law with {GAMMA] = 1.89^+0.35^_-0.34_, absorbed by a column density of
N_H_ = 4.7^+1.4^_1.1_ cm^-2^, and a thermal component with kT =
0.88^+0.89^_-0.35_ keV. Overall the power-law component can be
interpreted as arising from a Compton thin AGN, with the thermal
component either due to the AGN or to starburst activity. For our SED
fitting we compiled an additional N-band (10.6 {microns}) flux of 498 +-
100 mJy from Maiolino et al. (1995). From our results, we find that this
object contains both a starburst and an AGN, where the AGN provides a
significant fraction of the total IR luminosity.

7. 2002ApJS..143..315V
Re:IRAS F05189-2524
F05189-2524 (IVb). This compact galaxy has a faint curved tidal
feature to the northwest (refer to Surace et al. 1998 for a
high-resolution HST image of this object).

8. 2002A&A...386..379R
Re:IRAS 05189-2524
IRAS 05189-2524: the BeppoSAX observation of this source
was analyzed in detail by Severgnini et al. (2000). The
reflected component is not required from the fit
({DELTA}{chi}^2^ = 2 with one more free parameter). The
fit obtained with model B is in agreement with that of
Severgnini et al. (2000). The poor statistics
({chi}^2^_r_ = 1.2) is mainly due to an excess in the PDS
data around 20 keV. The statistics is however not good
enough to understand whether this excess is real or not.
We note that given the high noise in the PDS data,
Severgnini et al. (2000) chose not to use these data in
their analysis.

9. 2001MNRAS.327..459L
Re:IRAS 05189-2524
0518-2524: The higher resolution optical spectrum we used in determining
the line ratios in Table 2 (which will be discussed in greater detail in a
paper in preparation) also shows that 0518-2524 has a strong Balmer
absorption-line spectrum in the blue. This is probably also the reason why
many previous papers failed to detect the H{beta} emission present. There
is therefore clear evidence for a recent starburst episode in 0518-2524.
In addition, Clavel et al. (2000) show that there is relatively strong PAH
emission in the mid-infrared spectrum of this object, which is usually
taken as an indication of the 10-micron emission being due in significant
part to star formation. It is a moot point as to whether the large
far-infrared luminosity is due to any star formation or the obvious AGN
activity. The relatively low W_{lambda}5007_ and the failure to detect a
compact core at longer radio wavelengths when a prominent core exists at
shorter wavelengths may indicate the former however. It is also notable
that this galaxy has the coolest mid-far-infrared colours of any of the
HBLRs presented here, even though the inferred extinction to the core from
the X-ray data is small, which also suggests that there may be a
significant contribution to L_FIR_ from something other than the AGN.

10. 2000AJ....120..604S
Re:IRAS 05189-2524
IRAS 05189-2524.-The U' emission essentially mirrors that at all
other wavelengths (Surace et al. 1998; Surace & Sanders 1999). The
east-west and north-south tidal loops are easily seen. There are no
apparent knots, although there may be some undetected in the resolved,
extended nucleus.

11. 2000AJ....119..991S
Re:IRAS 05189-2524
This galaxy shows a single unresolved nucleus in all three bands.
In the PSF-subtracted images used in Figure 3, low-level emission is
seen to at least 3" radius. The nuclear source is extremely red (see
Fig. 3). (The sharper extensions east-west and to the north in the
2.2 micron image of Figs. 3 and 4 are probably due to incomplete PSF
removal.) At optical wavelengths (Surace et al. 1998; Surace & Sanders
2000), this galaxy has a nucleus that appears to be bisected by a dust
lane; the longer wavelength NICMOS data clearly penetrates this dust.
The optical images also exhibit a "plateau" of extended blue star
formation surrounding the nucleus, which may correspond to the extended
light seen in the NICMOS data, as well as several extended tidal loops.

12. 2000A&A...357...13R
Re:IRAS 05189-2524
IRAS 05189-2524: This source was observed by ASCA for ~ 40000 seconds.
The spectrum is well fitted by a two-component model, consisting of a
powerlaw with photon index {GAMMA} = 1.89^+0.35^_-0.34_ absorbed by a
column density of N_H_ = 4.7^+1.4^_-1.1_ cm^-2^, and a thermal component
with kT = 0.88^+0.89^_-0.35_keV. The iron line is not detected. From the
non-detection we estimate an upper limit to the equivalent width of
235 eV. The measured 2-10 keV flux is 5.3 x 10^-12^ erg cm^-2^ s^-1^. In
summary, the E > 2 keV spectrum is typical of a Compton-thin type 2 AGN,
while at lower energies an extra thermal component is present, that can
be either associated to the AGN itself or due to starburst activity.

13. 1999ApJ...522..139V
Re:IRAS 05189-2524
This object is one of six ULIGs from the Bright Galaxy Survey (BGS)
sample of Sanders et al. (1988) included in the present study. This is
the warmest object of this set (f_25_/f_60_ = 0.25). The optical
spectrum of this object is that of a Seyfert 2 galaxy (Veilleux et al.
1995). The K-band spectrum of this object clearly shows the presence of
broad ({DELTA}V_FWHM_ ~2600 km s^-1^) emission at Pa{alpha}. This
spectrum also illustrates very well the difficulty in detecting the
broad component to Br{gamma}. This explains the negative results of
Goldader et al. (1995) on this object. The J-band spectrum confirms the
presence of broad emission in the recombination lines. Both Pa{beta}
and He I 1.0832 micron present broad profiles. Note, however, that the
broad-line parameters derived from the J-band spectrum are considered
less accurate than those derived from Pa{alpha} because both Pa{beta}
and He I 1.0832 micron are weaker than Pa{alpha} and the intensities and
profiles of both lines are affected by strong atmospheric absorption
features. Based on the broad Pa{alpha} flux listed in Table 3 and the
assumption that a BLR with one-third the intensity of the observed
H{alpha} emission would have been detected in the optical spectrum of
VKS, a lower limit to the color excess in the BLR of
E(B-V)_bl_) > 2.8 mag is derived.

14. 1998ApJ...492..116S
Re:IRAS 05189-2524
IRAS 05189-2524.--Optically classified as a Seyfert 2 galaxy (Veilleux et al.
1995). The HST images clearly show that the plateau of emission seen in
ground-based images to the southeast of the nucleus is resolved into at least
two loops ~15 kpc in total length at right angles to each other; additionally,
there appear to be looplike or shell-like structures at slightly fainter
levels. Although not visible here, careful analysis of the PC and adjoining WF
frames reveals the two "hornlike" tidal features to the north seen in the
ground-based image (see Fig. 1), and this analysis indicates that they are
actually the high surface brightness base of a complete loop. There is no
obvious connecting feature in the HST images that would connect the inner disk
structure to the counter tidal tail previously identified by Sanders et al.
(1988b) that extends to the south from the western edge of the disk.

15. 1995AJ....110...87H
Re:IRAS 05189-2524
05189-2524 [Fig. 1(l)]: Narrow-band H{alpha} imaging shows that this
FIR-luminous galaxy has centrally concentrated, featureless region of
H{alpha} emission. It is a moderately strong radio source, with spatially
unresolved emission at 6 and 20 cm (paper I).

16. 1994AJ....107...35H
Re:IRAS 05189-2524
05189-2524. An off-center nucleus is visible in deep exposure CCD
frames of this amorphous galaxy [Fig. 15(j)]. The outer part of this
galaxy appears distorted, with ridges. A masked image uncovers a very low
surface brightness tail which forms an arc surrounding the galaxy. This
galaxy is one of the ultraluminous FIR galaxies discussed in detail by
Sanders et al. (1988a,b), and has been detected in the radio at 6 and 20
cm with fluxes of 12.7 and 28.3 mJy, respectively.

17. 1988ApJ...325...74S
Re:IRAS 05189-2524
This is the only object which appears "principally stellar" on the POSS.
A deep exposure on the Palomar 1.5m telescope was required to reveal
the 30" disk shown in Figure 1. In addition, two crossed tails are
revealed, leading us to identify this object as an advanced merger of
two spiral disks. The slightly curved tails extend from the midpoint of
the disk's western edge. At a redshift of 0.040 the larger northern
tail is ~40 kpc in length.

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