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Notes for object ESO 383- G 035

18 note(s) found in NED.


1. 2007A&A...461.1209D
Re:MCG -06-30-015
MCG-6-30-15: The source is known to exibit a relativistically broadened
FeK{alpha} line (Tanaka et al. 1995). This data set was previously
analized by Guain azzi et al. (1999), who confirmed the existence of
such a spectral feature. The results presented here are in agrement with
previous findings. The larger uncertainities in the continuum shape
parameters reported in this work with respect of the Guainazzi et al.
(1999) results are most probably due to the exclusion of the LECS data.

2. 2006ApJ...638..642B
Re:MCG -06-30-015
MCG -06-30-015 - This Seyfert 1 galaxy (z = 0.0077) was detected by all
three instruments (Fig. 4). The spectrum is well represented (Chi^2^nu_ =
1.19) by a power law with GAMMA = 2.8^+0.4^_-0.3_ and weak evidence for
absorption of N_H_ = 5.9^+8.6^_-5.5_ x 10^22^ cm^-2^ (Chi^2^nu_ = 1.11).

3. 2006A&A...459...55B
Re:MCG -06-30-015
A.6 MCG -6-30-15
.
The E/S0 galaxy MCG -6-30-15 hosts an X-ray bright AGN of Seyfert 1.2 type
(NED). It has been the subject to intense spectroscopic studies in the X-ray
band (e.g. Iwasawa et al. 1996) and is the best candidate for harbouring a
relativistically broadened iron line (e.g. Tanaka et al. 1995).
.
A multiwavelength study has been performed by Reynolds et al. (1997). In the
optical, an extracted host galaxy spectrum with Balmer and Ca II absorption
features is subtracted to gain the absorption-line free AGN spectra. The
nuclear spectrum reveals a strong non-stellar continuum, broad Balmer lines,
and narrow permitted and forbidden lines. High-excitation forbidden lines
(e.g. [Fe X], [Fe XI] {lambda}7892 A, and [Fe XIV] {lambda}5303 A) are
clearly displayed. A significant amount of dust extinction is deduced from
optical line and continuum emission, lying in the range E_(B-V)_ =0.6-1 mag.
Due to the absence of cold (neutral) absorption in the X-ray spectra, Reynolds
et al. (1997) postulate that the dust resides in the so-called warm absorber,
i.e. ionised gas that absorbs X-rays produced in the accretion disk of the AGN.
.
VLA observations at both 3.6 and 20 cm show that MCG -6-30-15 is an unresolved
radio source (Nagar et al. 1999b). HST continuum images and colour maps from
Ferruit et al. (2000) show a dust lane south of the nucleus, running roughly
parallel to the photometric major axis of the galaxy (PA ~ 115^deg^;
i ~ 60^deg^). The southwest side of the galaxy is found to be systematically
redder than the northeast side, with the central regions redder than the outer
ones.
.
The VLT long-slit spectra of MCG -6-30-15 allow us to trace [O III] emission
out to a distance of +/- 12" from the optical nucleus, i.e. six times larger
than the [O III] extension seen in the HST image of Schmitt et al. (2003a).
We confirm the existence of high-excitation forbidden lines in the central
spectra as reported by Reynolds et al. (1997).

4. 2006A&A...459...55B
Re:MCG -06-30-015
MCG -6-30-15 is the only galaxy in our sample in which we were not able to
disentangle the broad and narrow Balmer emission lines. This is first due to
the classification as Sy1.2 whereas the other Seyfert-1 galaxies (apart from
Fairall 51) can be classified as either Sy1.5 or Sy1.9, i.e. a clear
separation of the narrow emission line superimposed on the broad one is
visible. Second, it is also due to the lower resolution of our VLT/FORS1
spectra while all other type 1s were observed with the higher spectral
resolution of the NTT/EMMI. Thus, we cannot determine the central emission
line fluxes relative to H{beta} . Moreover, it was difficult to disentangle
the [O III] {lambda}4363 A emission line from the broad H{gamma} and we
therefore do not measure the temperature. MCG -6-30-15 is also the only
Seyfert-1 galaxy for which we applied a stellar template subtraction. This
was necessary since strong Balmer and Ca II H&K absorption lines were seen
in the NLR spectra (Fig. 2), in agreement with the results of Bonatto et al.
(2000) who find an old bulge population dominating the stellar contribution,
with indications of previous bursts of star formation.
.
The continuum gets steadily redder towards the nucleus where it reaches the
highest reddening value of E_B-V_ ~ 0.3+/- 0.02 mag. This amount of dust
extinction is significantly lower than what has been determined by
Reynolds et al. (1997). They were also not able to disentangle the broad and
narrow emission lines in their low resolution spectra and use instead the
total Balmer decrement. They derive a range of E_B-V_ ~ 0.6-1 mag. The
difference may arise from either additional reddening of the BLR only
(as Reynolds et al. 1997 use the total Balmer decrement) or is due to the
fact that our reddening value is a value relative to the stellar template
and simply reflects the differences of dust extinction between the NLR and
the template. If the extinction is at least partially due to dust in the
ISM of the host galaxy as proposed by Ballantyne et al. (2003), both the
stellar template and the central continuum suffer the same extinction which
will then not reflect in the reddening determined by the fitting of the
stellar template to the continuum slope of the NLR spectra.
.
Since the broad Balmer lines are limited to the central 2-3", we are able to
measure the narrow line fluxes in the outer regions to a distance of +/- 4".
We find that the line ratios are typical of AGNs when inserting them in the
diagnostic diagrams. Given the broad emission lines, it is reasonable to
believe that the central values also lie in the AGN regime and that the NLR
extends out to at least 4" distance from the nucleus.
.
The BH mass we estimate (0.8-3 x 10^7^M_sun_) is roughly in agreement with
the various measurements of the BH mass presented by McHardy et al. (2005)
(3-6 x 10^6^ M_sun_), when taking the errors into account.
.
We used the reddening determined from the continuum slope variation relative
to the stellar template to correct the observed [O II]/[O III] ratio
throughout the whole NLR. The thus derived ionisation parameter may have a
greater uncertainty than when using the reddening within the NLR as measured
from the Balmer decrement. In those objects in which we measured the reddening
from both the continuum slope and the narrow H{alpha}/H{beta} value, we observe
differences in the reddening distributions; moreover, a smaller reddening of
the continuum is observed (Papers I and II). Thus, for MCG -6-30-15, the
absolute ionisation parameter values may be overestimated due to a correction
by reddening values that are too low, but we consider the deduced general
behaviour as reliable. In Paper I, we showed with NGC 1386 that the general
distribution of the ionisation parameter does not change significantly for
either reddening value for correction.

5. 2004MNRAS.350.1049G
Re:MCG -06-30-015
9.19 MCG-6-30-15 This well-known X-ray galaxy has shown only modest
variations in the IR and its flux variation gradients cannot be
determined very accurately. A delay of about 34 d between J and L is
indicated.

6. 2004A&A...428..373B
Re:MCG -06-30-015
4.5. MCG-06-30-15. The Seyfert 1 MCG-06-30-15 is a very elongated
lenticular galaxy. Photometric colour maps show a small dust lane south
of the nucleus and roughly parallel to the major axis of the galaxy. The
central region of the galaxy is much redder than the outer regions
(Ferruit et al. 2000).
The nuclear spectrum, although that of a Seyfert 1, still clearly shows
the effect of dust extinction: the continuum flux strongly decreases
towards the blue (see Fig. 7).
Along PA = 86deg, we have extracted spectra of two circumnuclear regions
located at 360 and 650 pc from the nucleus (extending from 200 to 510
pc and from 510 to 790 pc, respectively). The absence of any hint of
broad Balmer lines in these spectra shows that we have successfully
isolated the stellar component. Both regions have a similar stellar
content dominated by an old mildly metallic population, although the
contribution from intermediate age stars (~1 Gyr) increases further away
from the nucleus (Table 2). The synthetic and observed dereddened
spectra are shown in Fig. 8. A high internal reddening, E(B - V) = 0. 15
-0.2, is inferred. An even higher reddening (E(B - V) = 0.61 to 1.09)
within the very nucleus has been deduced based on a multi-wavelength
study by Reynolds et al. (1997).

7. 2004A&A...428..373B
Re:MCG -06-30-015
4.5 MCG-06-30-15 The Seyfert 1 MCG-06-30-15 is a very elongated lenticular
galaxy. Photometric colour maps show a small dust lane south of the nucleus
and roughly parallel to the major axis of the galaxy. The central region of
the galaxy is much redder than the outer regions (Ferruit et al. 2000).
The nuclear spectrum, although that of a Seyfert 1, still clearly shows
the effect of dust extinction: the continuum flux strongly decreases
towards the blue (see Fig. 7).
Along PA = 86deg, we have extracted spectra of two circumnuclear regions
located at 360 and 650 pc from the nucleus (extending from 200 to 510 pc
and from 510 to 790 pc, respectively). The absence of any hint of broad
Balmer lines in these spectra shows that we have successfully isolated
the stellar component. Both regions have a similar stellar content
dominated by an old mildly metallic population, although the
contribution from intermediate age stars (~1 Gyr) increases further away
from the nucleus (Table 2). The synthetic and observed dereddened
spectra are shown in Fig. 8. A high internal reddening, E(B-V)=0.15-0.2,
is inferred. An even higher reddening ( E(B-V)=0.61 to 1.09) within the
very nucleus has been deduced based on a multi-wavelength study by
Reynolds et al. (1997).

8. 2003ApJS..148..327S
Re:MCG -06-30-015
5.40. MCG -6-30-15
The middle right panel of Figure 11 presents the [O III] image of
this Seyfert 1 galaxy. The emission is extended by 1.5" x 3.9" (230 x
590 pc), with the major axis of the [O III] emission at P.A. =
-65^deg^. This direction is at 10^deg^ from the host galaxy major
axis. The radio emission of this galaxy is unresolved (Nagar et al.
1999), and a detailed description of the NLR emission is given by
Ferruit et al. (2000).

9. 2001ApJ...550..261W
Re:MCG -06-30-015
3.3.9. MCG -6-30-15
The 2-10 keV flux varies by 40% between the five ASCA pointings
(Fig. 8i). Changes in the broad-line profile are well documented for this
galaxy (e.g., Iwasawa et al. 1996, 1999). Here this change is reflected as
a change in the effective line energy. We are insensitive to changes in the
line on short timescales, but on the longest timescales we find behavior
similar to NGC 4151 in that the line core flux remains fairly constant
while the EW decreases with increasing source flux (Fig. 9c, lower panel).
However, unlike NGC 4151, which has a constant line energy, MCG -6-30-15
has a variable line energy, which suggests that processes are occurring on
small spatial scales. The lack of reverberation signatures on long
timescales is consistent with the results of Reynolds (2000) and Lee et al.
(1998), based primarily on RXTE data.

10. 2000ApJS..128..139F
Re:ESO 383- G 035
5.8. ESO 383-G35 (MCG -6-30-15) - Seyfert 1.2
ESO 383-G35 is an E/S0 galaxy hosting a Seyfert 1.2 nucleus, which
has been studied primarily (and extensively) in X-rays (e.g.,
Iwasawa et al. 1996). The continuum images and color maps of this galaxy
are shown in Figure 16. The photometric major axis P.A. and the isophote
ellipticity of the galaxy, as measured beyond 3" (510 pc) from the
nucleus, are ~ 115^deg^ and ~ 0.45-0.50 (i.e., an inclination angle of
~ 60^deg^), respectively. There is a dust lane south of the nucleus,
running roughly parallel to the photometric major axis of the galaxy.
The southwest side of the galaxy is systematically redder than its
northeast side (see Fig. 16, bottom right-hand panel), suggesting that
it is the near side of the galaxy. The large scale color map (see
Fig. 16, bottom left-hand panel) shows that the central regions of the
galaxy are redder (lower log [F547M/F791W] ratio) than the outer
regions.
The [O III] and [N II] + H{alpha} images of ESO 383-G35 are shown
in Figure 17. The [O III] image reveals a nuclear extension aligned
parallel to the photometric major axis of the galaxy, which presumably
represents gas coplanar with the stellar disk. The two white pixels on
the nucleus (Fig. 17, left-hand panel) are artifacts. In the
[N II] + H{alpha} image, the nuclear disk is largely hidden by the
diffraction pattern of the bright, pointlike Seyfert 1.2 nucleus.

11. 1999ApJS..120..209N
Re:MCG -06-30-015
MCG -6-30-15 (type 1.2; Fig. 12) - The source is unresolved at both
3.6 and 20cm. There is another source (76 mJy at 20cm) at
{alpha}=13^h^33^m^06.07^s^, {delta} = -34^deg^04'49.0" (B1950.0). The
position listed in Table 1 is that of the peak at 3.6cm. The 20cm
source position is offset by ~1.4" to the southeast and is at
{alpha}=13^h^33^m^01.93^s^, {delta} = -34^deg^02'26.6" (B1950.0), but
it is consistent with the 3.6cm position, given the weakness of the
source. The 20cm flux measured here is more than twice the value of 1.7
+/- 0.7 mJy published in Paper VI.

12. 1999A&AS..137..457M
Re:MCG -06-30-015
MCG-6-30-15: This is an unresolved and barely detected object. Ulvestad
& Wilson (1984b) reported a flux density of 1 mJy at 6 cm and 1.7 at
20 cm, giving a spectral index of {alpha}_6_^20^ = -0.44. The flux
density from our observations give an inverted spectral index at high
frequencies {alpha}_6_^3^ = 0.24. The upper limit to the flux with the
PTI is S < 4 mJy at 13 cm (R94).

13. 1998ApJS..114...73G
Re:MCG -06-30-015
Section 7.3. MCG -6-30-15
Two data sets of MCG -6-30-15 are contained within our sample from
observations carried out in 1993 July, separated by ~3 weeks, with the
observed count rate ~52% higher for MCG -6-30-15(1) (Table 2). As shown in
Sections 5.3-5.6, there is clear evidence for ionized gas in this source,
with models B(i)-C(ii) providing acceptable fits. In all cases, a "1 keV
deficit" was also evident, which can be modeled by an additional absorption
edge (Section 6.2). The best-fitting continuum for MCG -6-30-15(1) has
{GAMMA} ~ 2.1, while that for MCG -6-30-15(2) is slightly flatter
({DELTA}{GAMMA} ~ 0.1). Both observations are consistent with D_f_ = 0.
As shown in Figure 16, there is clear evidence for an increase in N_H, z_
(by ~1-6 x 10^21^ cm^-2^) over the 3 weeks between the observations. However,
the ionization parameter remains constant, or perhaps even increases (but
with {DELTA}U_X_ <~ 50%), between the two observations despite a decrease in
the luminosity derived for the ionizing continuum from L_X_ ~ 4.5 x 10^43^
ergs s^-1^ to ~3.0 x 10^43^ ergs s^-1^ [for model C(ii), after correcting for
absorption]. Such behavior has been reported previously for these data sets
by Fabian et al. (1994) and, as in the case with NGC 4151, is difficult to
reconcile with that expected in the simplest picture whereby a uniform shell
of gas reacts to changes in the intensity of the photoionizing continuum.
Again appealing to only Keplerian motion to move inhomogeneities through the
cylinder of sight between the two observations (i.e., setting tabs <~ 3
weeks) and again setting the variability tvar ~ 10^3^ s, from equation (2)
one obtains the rather weak constraint r_ld_ <~ 5 x 10^2^(f_bolX_/f_Edd_)
lt-days. Again we note that these limits are based upon only the Keplerian
motion, which may not be the major component of the dynamics of the ionized
gas.
.
However, there is evidence in a subsequent ASCA observation that while the
depth of the O VII edge appears to be constant on long timescales in this
source, the depth of the O VIII edge varies on a timescale ~10^4^ s (Otani et
al. 1996). Such behavior has been recently confirmed in BeppoSAX LECS
observations (Orr et al. 1997). Setting t_abs_ ~ 10^4^ s in equation (2), one
obtains r_ld_ <~ 4(f_bolX_/f_Edd_) lt-hr. However, since the photoionization
and recombination timescales for these ions are similar, such behavior is
incompatible with the observed O VII and O VIII edges being produced in the
same region of ionized gas. Otani et al. suggested the most natural solution
was a two-zone model in which the gas giving rise predominately to the O VII
edge is stable, while that responsible for the O VIII edge undergoes rapid
variations. Such an hypothesis is of course supported by our observations of
a (relatively small) "1 keV deficit" in the data/model residual of all the
models considered in Section 5. In Section 6.2, we showed that this can be
modeled by an additional absorption edge ({tau}_ONe_ ~ 0.14) at an energy
close to that of O VIII (see Section 8.8).
.
Both observations of MCG -6-30-15 are consistent with the presence of
emission from the ionized material, with L_e_ <~ 10^42^ ergs s^-1^ in the
0.1-10 keV band (after correcting for absorption). However, the
signal-to-noise ratio of these data sets is too low to determine
unambiguously whether the intensity of this emission responded to the
decrease in the ionizing continuum.

14. 1998ApJS..114...73G
Re:MCG -06-30-015
Section A11. MCG -6-30-15
This Seyfert 1.0 galaxy was first detected in X-rays by HEAO 1 A-2 (Marshall
et al. 1979). Absorption due to ionized gas first suggested by Ginga
observations, with N_H, z_ ~ 10^23^ cm^-2^ (Nandra et al. 1990). In our
analysis of the data from two ASCA observations separated by ~3 weeks in 1993
July, we confirm the presence of ionized gas. However, while none of the
models presented in Section 5 provide a fit that formally satisfies our
criteria for MCG -6-30-15(1), this is primarily due to the presence of a
deficit at ~1 keV (Fig. 6). An acceptable solution is obtained for
MCG -6-30-15(2) for model C(i), but again some evidence for a relatively
small deficit at ~1 keV (Fig. 10).
.
However, as further discussed in Section 7.3 there is a significant increase
in column density (from N_H, z_ ~ 6 x 10^21^ cm^-2^ to ~9 x 10^21^ cm^-2^),
along with a slight increase in ionization parameter (from U_X_ ~ 0.11 to
.15) despite a factor ~2 decrease in the intensity of the illuminating
continuum between the two observations (see, e.g., Fig. 16). This, the
presence of the ~1 keV deficit, and a decrease in the depth of the O VIII
edge on a timescale ~10^4^ s (but not in the depth of the O VII edge)
observed in an ASCA observation performed in 1994 July (Otani et al. 1996)
are impossible to reconcile with that expected from a uniform shell of gas
reacting to changes in the intensity of the photoionizing continuum.
.
A single-zone photoionization model has also been applied to these data by
Fabian et al. (1994) and Reynolds et al. (1995), assuming an ionizing
continuum consisting of a single power law of {GAMMA} = 2. Using Figure 1b to
convert from their quoted values of {xi}, we obtain results in good agreement
with those found here [N_H, z_ ~ 6 x 10^21^ cm^-2^, U_X_ ~ 0.09, and
N_H, z_ ~ 13 x 10^21^ cm^-2^, U_X_ ~ 0.11 for the MCG -6-30-15(1,2) data
sets, respectively]. Photoionization models for the extended (4 day) ASCA
observation carried out in 1994 July have been presented by Otani et al.
(1996) and R97. The source exhibited a factor ~4 variability in the observed
flux during this observation [covering the two flux states represented by
MCG -6-30-15(1,2)] leading Otani et al. to divide the observation into two
parts. They found N_H, z_ ~ 5 x 10^21^ cm^-2^, U_X_ ~ 0.04 for the first 300
ks of the observation, but N_H, z_ ~ 10 x 10^21^ cm^-2^, U_X_ ~ 0.18 for the
last 60 ks. For reference, R97 analyzed the time-averaged spectrum and
obtained U^R97^_X_ ~ 0.05 and N_H, z_ ~ 6 x 10^21^ cm^-2^). The physical
implications of these results have been further explored by Reynolds & Fabian
(1995).
.
Curiously (but see Reynolds & Fabian 1995), MCG -6-30-15 appears to be
heavily reddened in the optical/UV; thus, little is known regarding the
presence of UV absorption features.

15. 1997MNRAS.286..513R
Re:MCG -06-30-015
7.1.9 MCG-6-30-15
This object has been discussed in the introduction and Sections 5.2 and 6.2.1.

16. 1995AJ....110...87H
Re:IRAS 13329-3402
13329-3402 (MCG -06-30-015, ESO 383-G035) [Fig. 1(t)]: The H{alpha}
image shows that this galaxy has a centrally concentrated featureless
region of emission. It is a weak, unresolved radio source at 6 and 20 cm
with a size <80 pc (Ulvestad and Wilson 1984).

17. 1994AJ....107...35H
Re:IRAS 13329-3402
13329-3402 (MCG-6-30-15. ESO 383-G35). This galaxy resembles a very
elongated lenticular galaxy, with smooth, regular isophotes and a bright,
circular nucleus. The bright source south of the nucleus, within the
galaxy, is a foreground star. The detailed study by Pineda et al. (1980)
shows that it has a typical Seyfert 1 spectrum. It is an unresolved radio
source at 6 and 20 cm with a size < 80 pc (Ulvestad & Wilson 1984). There
are no features apparent on the deep exposure CCD images, but digitally
enhanced images reveal elongated, almost straight features on either side
of the nucleus. These features may be indicative of a nearby edge-on
disk, although no spiral structure is evident.

18. 1982ESOU..C...0000L
Re:ESO 133302-3402.4
=ESO 383- G 35
type 1 Seyfert
*X-ray source
*in cluster


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