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Notes for object NGC 7582

27 note(s) found in NED.


1. 2009ApJ...702.1127R
Re:NGC 7582
NGC 7582 is a Sy2 galaxy that harbors a nuclear starburst surrounding the active
nucleus (Cid Fernandes et al. 2001; Sosa-Brito et al. 2001; Wold & Galliano
2006; Bianchi et al. 2007) and presents a nuclear outflow (Morris et al. 1985).
The fit with the clumpy models shown in Figure 7 does not reproduce the 18.2
{mu}m point, and the resulting probability distributions of the parameters are
very different compared with the rest of Sy2 galaxies discussed here (except for
NGC 1808). Low values of {sigma} are more probable (<29^deg^), as are
extremely small numbers of clouds (N_0_< 2). High values of q (>2.5) and low
values of the {tau}_V_ (<27) are preferred. The i probability distribution has a
Gaussian shape whose median value is i = 41^deg^ +/- ^19^_28_. The optical
obscuration produced by the torus results in an unrealistic value of A^LOS^_V_ <
6 mag. The reprocessing efficiency fraction of this galaxy is among the lowest
in the sample (~10%), a consequence of the low values of N_0_ and { sigma}. The
10 {mu}m silicate feature appears in emission in the fitted models, in
contradiction with TIMMI2 mid-IR observations (Siebenmorgen et al. 2004a) that
show a strong absorption band characterized by {tau}_10 {mu}m_ = 1.1. All these
results are probably due to stellar contamination of our mid-IR data (obtained
at the 4 m CTIO). The intense circumnuclear star formation present in this
galaxy makes it more difficult to isolate the torus emission from that of the
host galaxy. Consequently, as for the case of NGC 1808, we consider the model
fit of NGC 7582 unreliable.

2. 2008MNRAS.386.2242H
Re:NGC 7582
NGC 7582 - The influence radius of the SMBH is not well resolved,
2r_bh_/r_res_= 0.7 (Wold et al. 2006).

3. 2008A&A...484..341R
Re:NGC 7582
NGC 7582 is a classic Seyfert 2 galaxy which, during a period of five months in
1999 showed broad lines characteristic of a Seyfert 1 galaxy, which may indicate
the presence of a patchy torus. Aretxaga et al. (1999). 50% of the flux found in
extended emission with a peak offset from the center of the extended emission.
The extended emission is seen elongated along the South-North direction. The
12.9 micron image shows two weak sources to the North and to the South of the
main peak, also clearly seen in the 12.9 micron image of Acosta-Pulido et al.
(2003). The 11.9 micron image shows one slightly resolved peak surrounded by
extended emission. Flux at 11.9 micron is very similar to that of Siebenmorgen
et al. (2004), although the 11.9 micron image they present shows considerably
less extended emission. Similar extended emission can also be seen in the N1
(~8-95.5 micron) image of Acosta-Pulido et al. (2003).

4. 2007A&A...461.1209D
Re:NGC 7582
NGC 7582: Turner et al. (2000) presented the analysis of the BeppoSAX
observation of NGC 7582. They interpreted the X-ray spectrum in terms of
complex absorption due to two components: one covering the entire source
(N_H_ ~ 1.4 x 10^23^ cm^-2^) and the second covering ~60% of the high
energy source with N_H_ ~ 1.6 x 10^24^ cm^-2^. Here a slightly different
model is proposed. An absorption edge is detected at E ~ 7.9 +/- 0.3 keV
with {tau} = 0.3 +/- 0.2, i.e., not consistent with the origin from
neutral matter. The origin of the edge could be ascribed either to an
ionized reflection or an absorption component. Both hypotheses have been
tested, but none gave a significant improvement in the quality of the
fit.

5. 2005ApJ...633..105D
Re:NGC 7582
4.5. NGC 7582 - NGC 7582 is the brightest narrow-line X-ray galaxy and is
perhaps prototypical of this class (Schachter et al. 1998). That it has an AGN
cannot be doubted, due to the rapid and large variations in hard (2-10 keV)
X-ray flux occurring while the soft (0.5-2 keV) X-ray flux remained constant
(Schachter et al. 1998; Xue et al. 1998), and the presence of an [O III]
ionization cone (Storchi-Bergmann & Bonatto 1991). Aretxaga et al. (1999) noted
the appearance and subsequent variations in a broad component to several
optical emission lines. We also have detected a broad bump in the K-band
spectrum, which most likely corresponds to broad (~4000 km s^-1^) Br{gamma}.
This is also apparent in the nuclear spectrum of Sosa-Brito et al. (2001), who
noted the complex morphologies of the emission lines. Aretxaga et al. (1999)
reached no consensus on whether this type 2 to type 1 transition was due to the
appearance of type IIn supernovae or to patchy obscuration in the torus around
the AGN. By examining the FUV flux, Storchi-Bergmann et al. (2001b) found
evidence for young stars in the nucleus (central 2") of NGC 7582, superposed on
the older bulge population. We also see relatively strong Na I absorption in
the spectrum of the central 100 pc. On the other hand, the equivalent width of
this absorption feature decreases steadily from a radius of +/-3" (300 pc) to a
minimum at the nucleus of ~1 A. This feature could imply a transition to a
rather young stellar population or, more likely, the presence of hot dust
grains-although whether the heating on such extended scales can be attributed
to the AGN is unclear.

6. 2003MNRAS.343..192R
Re:NGC 7582
3.8 NGC 7582 NGC 7582 is a nearby (z = 0.00540; distance = 20.9 Mpc)
(R'_1_)SB(s)ab galaxy in the Grus quartet with a Sy2 nucleus. Optical
broad-band images (e.g. Malkan, Goijian & Tam 1998) show a disturbed
morphology with an optically obscured nucleus, a red star-forming ring
(diameter 2 arcsec) and a dust lane crossing the nuclear region. In the
NIR, the galaxy appears smoother, and in the L-band the nucleus
dominates, albeit the ring remains visible (Prieto, Reunanen &
Kotilainen 2002). Optical spectropolarimetry does not reveal a hidden
BLR (Heisler, Lumnden & Bailer 1997), and even hard X-ray emission is
attenuated by large column density (Warwick et al. 1993), indicating
that an edge-on torus blocks even the scattered light from the
nucleus. However, the nuclear emission is variable, and the broad
hydrogen recombination line has been detected by Sosa-Brito et
al. (2001). The sharp-edged [0 III] outflow cone of NGC 7582 (PA =
250deg) was detected by Storchi-Bergmann & Bonatto (1991).
The H- and K-band spectra are shown in Fig. 8. The strongest nuclear
line is Br{gamma}, while the other lines detected are 1-0 S(1) and other
H_2_ lines, [Fe II] and an unidentified emission feature at 2.195
{microns}, which remains visible after subtracting the continuum.
Br{gamma} can be decomposed into broad (~3000 km s^-1^) and narrow (420
km s^-1^) components (Fig. 10). The broad component has an additional
blue wing and is therefore not perfectly fitted by a simple
two-component fit. Two coronal lines ([Si VI] and [Si VII]) are also
detected.
1-0 S(1) is the most extended line (Fig. 4) and is more extended
perpendicular to the cone (8 arcsec, 900 pc) than parallel to it (2.5
arcsec, 270 pc). 1-0 S(1) emission declines smoothly, but the effect of
the ring on the H_2_ emission is also notable, especially perpendicular
to the cone. The ring is more prominent in Br{gamma} and [Fe II], which
are detected parallel to the cone up to 4 arcsec (430 pc) in the NE, 2.5
arcsec in the SW and ~2 arcsec perpendicular to the cone. The emission
lines are narrow, comparable to or slightly larger than the instrumental
resolution. He I is also strong in the ring, in agreement with
relatively recent star formation.
The velocity field of NGC 7582 is shown in Fig. 5. Parallel to the cone
the velocity curves of various emission lines are relatively flat and
similar to each other. [Fe II] is systematically blueshifted with
respect to H_2_. The ratio of [Fe II]/narrow Br{gamma} = 3.1 is larger
than models predict for star-forming regions, but in agreement with
shocks or X-rays.
The ratio of 2-1 S(1)/1-0 S(1) = 0.20 + 0.06 in the nucleus in agreement
with thermal excitation of H_2_ (T_vib_ = 2900 +- 500 K). Assuming
T_vib_ = 2000 K, the density of H_2_ is 7.8 x 10^17^ cm^-2^,
corresponding to a gas mass of 220 M_{sun}_. The integrated mass of the
excited hydrogen is 320 M_{sun}_ parallel to the cone and 480 M_{sun}_
perpendicular to it across the galaxy. The nuclear H_2_ emission is too
weak to accurately determine the FWHM size of the nucleus.
The coronal lines [Si VI] 1.964 {microns} and [Si VII] 2.483 {microns}
are weak, and it is not possible to reliably measure the size of the
coronal emission region. However, the detection of coronal lines
supports the presence of AGN in NGC 7582, as does the detection of broad
Br{gamma}.

7. 2003ApJS..146..353M
Re:NGC 7582
NGC 7582 (HI/C)
There is a great deal of star formation in the central kiloparsec,
although the high inclination makes it difficult to determine whether
or not the star formation is connected to the dust lanes.

8. 2002ApJS..143...73E
Re:NGC 7582
NGC 7582.---(R)SBb?: Bright nuclear point source embedded in large
bulge. System is nearly edge-on. The inner bulge isophotes are
elliptical. At lower intensity, the bulge has a strong "X" feature. The
high inclination makes any spiral pattern impossible to detect.
However, there is obvious structure in the disk, with clumps of star
formation, and dust obscuration visible. No coherent dust lanes are
apparent. At low surface brightness levels, the X structure resembles a
peanut bulge, and the disk shows a pronounced integral-sign warp. There
are very LSB spiral features extending from the disk and wrapping
nearly entirely around the galaxy. These features are broad and
smooth, with no sign of internal structure.

9. 2002A&A...386..379R
Re:NGC 7582
NGC 7582: Turner et al. (2000) present a detailed analysis of the
same BeppoSAX data. The results are compatible, but these authors
prefer a different interpretation for the high energy emission in
excess of the simple powerlaw, which we fit with a strong cold
reflection component. Arguing that the required reflection component
is too high, they suggest that the intrinsic continuum (which is
completely covered by gas with N_H_ ~ 1.4 x 10^23^ cm-2, in
agreement with our results), is also absorbed by a second screen
with N_H_ ~ 1.6 x 10^24^ cm-2, and a covering factor of 60%.

10. 2001MNRAS.327..459L
Re:NGC 7582
NGC 7582: This galaxy showed brief evidence of broad H{alpha} in direct
flux (Aretxaga et al. 1999), probably due to a lowering of the obscuring
column density, since there is also evidence for considerable hard X-ray
variability in this galaxy (Schachter et al. 1998; Xue et al. 1998).
Turner et al. (2000) summarize the evidence for a 'patchy' torus in this
source, and the alternative possibility that the broad permitted line
arose in a supernova, as suggested by Aretxaga et al. Turner et al. find
that the best fit to their 2-100 keV BeppoSAX data requires an obscuring
column of 1.4 x 10^23^ cm^-2^ which completely covers the source, plus a
Compton-thick absorber with N_H_ ~ 1.6 x 10^24^ cm^-2^ which only covers
60 per cent of it. Because the Compton-thick component does not cover the
entire source, 'holes' in the thinner component could lead to unobscured
sight lines towards the BLR. The optical classification (Table 2) is a
reflection of fact that there is significant ongoing star formation in
this galaxy.

11. 2001ApJS..136...61S
Re:NGC 7582
5.31. NGC 7582
NGC 7582 presents a fascinating puzzle. It is a classical Seyfert 2
galaxy, with a well-defined [O III] cone (Morris et al. 1985;
Storchi-Bergmann & Bonatto 1991) and normally narrow emission lines
(e.g., Cid Fernandes, Storchi-Bergmann, & Schmitt 1998). Its lack of broad
lines in spectropolarimetric observations coupled with a high
60 micron/25 micron flux ratio led Heisler, Lumsden, & Bailey (1997) to
infer that the nucleus itself is totally obscured, even to scattered light,
by an edge-on thick torus surrounding it. This is also consistent with the
results of Ginga observations of NGC 7582 (Warwick et al. 1993). That
stars contribute to the nuclear luminosity of NGC 7582 has been
demonstrated by the work of Oliva et al. (1995). They find, through
observations of strong CO bandhead absorption lines and an inferred large
near-IR light-to-mass ratio that young supergiants are present and dominate
the H- and K-band nuclear luminosity (but see also Schmitt,
Storchi-Bergmann, & Cid Fernandes 1999, who find, based on spectral
synthesis fitting to optical spectra, that only 6% of the optical light is
due to young stars). There is also a kiloparsec-scale disk of H II regions
surrounding the nucleus (Morris et al. 1985).
Recently, Aretxaga et al. (1999) report on the detection of hitherto
unseen broad lines in the optical spectra, effectively for a few months
turning this classical Seyfert 2 galaxy into a Seyfert 1 galaxy. These
authors debate the pros and cons of three models to explain the sudden
appearance of the broad lines: the capture of a star by a nuclear black
hole, a reddening change in the surrounding obscuring torus, and the
radiative onset of a Type IIn supernova. The first two of these models
deal directly with the active nucleus and its obscuring surroundings,
while the last model invokes pure stellar processes. Aretxaga et al.
(1999) raise serious concerns with the first two models, and favor the
SN theory. Evidence in favor of a nuclear-based explanation comes from
the BeppoSAX observations of Turner et al. (2000). They observed NGC 7582
in 1998 November and found a previously unseen hard X-ray component.
Correlated variability across the X-ray spectrum led Turner et al. (2000)
to the conclusion that a single component dominates the 2-100 keV band.
Further, these variations do not seem to be at all correlated with those
in the optical reported on by Aretxaga et al. (1999).
NGC 7582 was observed twice in the K band, once before and once just
after the optical anomaly. The second set of observations were done after
the anomaly was brought to our attention (R. Terlevich 1998, private
communication). A more detailed analysis of our observations will be
presented in a subsequent paper, but here we note simply that our second
observations show a broadening of the Br{gamma} line, along with a
reddening of the continuum in the seeing weighted aperture. Our observed
Br{gamma} equivalent width for the 1994 July ESO 2.2 m observations agrees
well with that obtained by Oliva et al. (1995), who also observed NGC 7582
during its "quiescence."

12. 2001ApJS..133..269L
Re:NGC 7582
5.13. NGC 7582
NGC 7582 is a group member and contains a bar. As mentioned above,
medium-energy emission from NGC 7582 varies (Xue et al. 1998), so we have
treated the two ASCA observations separately and combined each with the
single PSPC data set for the joint fits. In both cases, the best-fitting
model includes a scattered power law, thermal emission, and a narrow line
near 6.3 keV. We attribute the spectral variation to a change in absorbing
column density. The intrinsic AGN is strong in NGC 7582, nearly 10^-2^
photons keV^-1^ cm^-2^ s^-1^ at 1 keV. The intrinsic AGN thus contributes
to the soft X-ray flux, so the thermal emission accounts for 0.16 and 0.28
of the total in the two observations.
The X-ray emission is extended, on scales of 3.1 and 5.1 kpc in the HRI
and PSPC, respectively. The extended fraction is greater in the HRI
observation (0.56), from 1995 May, than in the PSPC observation (0.38),
taken in 1993 May. We also observe complex structure in this nearby galaxy,
and differences between the hard and soft PSPC images.
The optical spectrum of NGC 7582 has varied in recent years, exhibiting
broad lines as of 1998 July. Aretxaga et al. (1999) discuss several
possible causes for this transformation to an optical spectrum
characteristic of a Seyfert 1 and favor the appearance of a Type IIn
supernova in the starburst. These and other X-ray observations
(Turner et al. 2000) suggest, however, that the column density that
obscures the nucleus varies. Although a simple increase in extinction with
the local reddening law is not consistent with the optical continuum
variations, the contribution of the starburst component may not be
adequately distinguished in the present optical spectra
(Aretxaga et al. 1999). The nearby companion, RX J231829.9-422041
(discussed in section 3.2), is much fainter than NGC 7582, especially at
harder energies. The spectrum of RX J231829.9-422041 is soft. We fitted
the PSPC spectrum of this source alone with a single power law,
{GAMMA} = 2.1_-0.48_^+0.44^, and Galactic absorption.

13. 2000MNRAS.314..573T
Re:NGC 7582
NGC 7582: This source has a diffuse radio structure consistent with the
lower resolution observations of Ulvestad & Wilson (1984b).

14. 2000ApJ...544..747S
Re:NGC 7582
This galaxy is well known from the emission lines (diagnostic diagrams)
to present a composite Seyfert 2 + Starburst spectrum. The HOBL are easily
seen (Fig. 16c). The near-UV W values, CR, and spectral distribution are
well represented by a bulge template plus 1% mass contribution of a 50 Myr
stellar population. Again, we attribute the poor fit of the Ca II K line
mostly to the lower metallicity of the young templates as compared to the
nuclear region of the galaxy. There is contamination of the
Ca II H + H{epsilon} absorption by Ne III {lambda}3968 + H{epsilon}
emission.

15. 1999AJ....117.2676R
Re:NGC 7582
The dust morphology of NGC 7582 (Fig. 2v) is quite complex in this
galaxy but is dominated by a dense ring of extinction. This elliptical
ring of extinction with a minor axis of ~2" and a major axis of ~3"
surrounds the nucleus. The ring is broken to the southeast by a chain of
blue clumps. The closest of these clumps is ~0.5" from the nucleus, and
the chain extends out to 4" from the nucleus. Two other blue clumps can
be seen ~3" east and ~4" north of the nucleus. A broad dust lane enters
the image from the southeast and connects to the extinction ring north
of the chain of blue clumps. As in Markarian 1066 the NICMOS image alone
implies that there may be a nuclear bar, but the color map shows that
this may be just a combination of extinction and star formation
perturbing the 1.6 micron isophotes.

16. 1999A&AS..137..457M
Re:NGC 7582
NGC 7582: Ulvestad & Wilson (1984b) detected a weak core surrounded by
an extended emission. They measure 69 mJy at 6 cm and 166 mJy at 20 cm,
giving a spectral index of -0.73. We find (Fig. 15) that the spectral
index remains steep out to 3 cm with {alpha}_6_^3^ = -0.72. For
comparison, the NLR is a good example of an edge-brightened, wide angle
bi-cone with a cone axis projected along PA_e.l._ = 55^deg^. In
addition, the host galaxy has a prominent bar along PA_bar_ = 155^deg^.
An upper limit to the flux density of S < 6 mJy has been set by the PTI
observations (S95, R94).

17. 1998MNRAS.297..579C
Re:NGC 7582
NGC 7582. Morris et al. (1985) found circumnuclear H{alpha} emission in this
Seyfert 2 galaxy, suggesting a ring of rotating HII regions in the galaxy
plane. The Ws of this galaxy show a dilution, changing from S7 at the nucleus to
S3-S4 in the outer regions (Fig. 29). The continuum ratios are similar to S3 at
the nucleus and north-east (r<0), but decrease to values similar to S5-S6
towards r>0. The continuum ratios to the south-west are bluer than what we would
expect from the W results. The dilution measured in this object is probably due
to its inner star-forming ring.

18. 1997ApJS..113...23T
Re:NGC 7582
A25. NGC 7582
Four distinct X-ray sources were detected by the Einstein Observatory Imaging
Proportional Counter (IPC) in the 2A 2315-428 field. The strongest IPC source
was the Sersic 159-03 cluster, with significant flux from the heavily absorbed
galaxy NGC 7582. An EXOSAT observation found N_H_~2x10^23^ cm^-2^ assuming a
{GAMMA}=1.7 power-law continuum (Turner & Pounds 1989). NGC 7582 shows an
asymmetric, doubly peaked CO profile in the central region, which may be
associated with an ionized gas disk in the nucleus (Charles & Phillips 1982).
Models featuring attenuation by a partial-covering absorber or two
independently absorbed continuum components are significantly preferred over
the simple absorbed power law. The ROSAT PSPC observation shows the nuclear
source to be pointlike. Large factors of variability are evident in the
recorded 2-10 keV flux (Polletta et al. 1996), although these are difficult to
interpret because of the large number of bright X-ray sources in the immediate
proximity of NGC 7582.

19. 1997A&A...319...52V
Re:NGC 7582
NGC 7582 has a "transition" nuclear emission spectrum (Ward et al., 1980;
Storchi-Bergmann et al., 1995) which has been shown to be a composite spectrum
by Veron et al. (1981a)
In addition, Kennicutt et al. (1989) have shown that many nuclear HII regions
also contained a weak Liner or Seyfert cloud. Using optical spectrophotometry
to compare the physical properties of HII regions located in galactic nuclei
and in the disks, they have discovered that, in the diagram
{lambda}5007/H{beta} vs. {lambda}6584/H{alpha}, the distributions of these two
categories of objects are significantly different: while the disk HII regions
define a narrow sequence, half of the nuclear regions have a larger value of
{lambda}6584/H{alpha} for a given {lambda}5007/H{beta}. High dispersion spectra
of a few of these objects show that, indeed, the line profiles are different,
the [OIII] lines having a broad component which is absent or very weak in
H{beta}.

20. 1996ApJS..103...81C
Re:NGC 7582
NGC 7582.--Pks 2316-423. Seyfert 2.

21. 1994CAG1..B...0000S
Re:NGC 7582
Grus Group
Triplet
SBab(rs)
CD-576-S
Oct 8/9, 1978
103aO + GG385
40 min
NGC 7582 is the brightest member of a close triplet of large
spirals. The triplet is a part of a larger loose group having several
condensations, called the IC 1459 Grus Group (Sandage 1975b). The two
other members of the triplet are NGC 7590 (Sc) at 9.4' separation and
NGC 7599 (Sc) at 12.2' separation. Both are in the RSA but are not
shown in this atlas.
The redshifts are v_o(7582) = 1475 km/s, v_o(7590) = 1487 km/s,
and v_o(7599) = 1670 km/s. At a mean redshift distance of 31 Mpc (H =
50), the projected linear separations from NGC 7582 are 85 kpc and 110
kpc, for NGC 7590 and NGC 7599, respectively.
The spiral pattern in NGC 7582 of two faint outer arms with a
different pitch angle from that of a complex inner spiral pattern, has
the form of the NGC 210 look seen more edge on.

22. 1985SGC...C...0000C
Re:NGC 7582
Plate 839
Overexposed.
Plate 2533
Overexposed center, smooth arms. Superposed on cluster.

23. 1982ESOU..C...0000L
Re:ESO 231538-4238.6
=ESO 291- G 16
in cluster

24. 1976RC2...C...0000d
Re:NGC 7582
= PKS 2315-426
In a group with NGC 7590 and NGC 7599 at 9.5 arcmin and 13 arcmin
Photograph:
M.N.R.A.S., 131, 351, 1966.
J.R.A.S. Canada, 68, 117, 1974.
Photometry:
Atlas Gal. Australis, 1968.
Photometry (I.R. 1-3.5 microns):
M.N.R.A.S., 162, 35P, 1973.
M.N.R.A.S., 164, 155, 1973.
Radio Observations:
Australian J. Phys., 19, 883, 1966.
Proc. A.S. Austr., 2, 159, 1972.

25. 1964RC1...C...0000d
Re:NGC 7582
Very small, bright nucleus in a bright complex lens and bar: 2.7 arcmin x
0.7 arcmin with dark lanes. 2 faint, smooth regular arms form a pseudo (R):
4.4 arcmin x 1.75 arcmin.
See also
M.N.R.A.S., 81, 602, 1921.
Non-interacting pair with NGC 7590 at 9.5 arcmin.
Non-interacting pair with NGC 7599 at 13 arcmin.
In a group with NGC 7590 and NGC 7599.
Photograph:
P.N.A.S., 26, 33, 1940.

26. 1957HPh....53..275d
Re:NGC 7582
(R')SB(s)a
(Plate 50)
Broad-side view.
Details of the bar and the lens, seen from "across"
are in Plate 53. Note the pattern of dark material.

27. 1957HPh....53..275d
Re:NGC 7582
(R')SB(s)a
(Plate 53)
Detailed view of the bar and lens.
Also illustrated in Plate 50.


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