Date and Time of the Query: 2019-06-24 T08:26:59 PDT
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Notes for object NGC 6300

21 note(s) found in NED.

1. 2009ApJ...690.1322W
Re:NGC 6300
NGC 6300. In the analysis, the authors (see Table 1 for reference) model
the soft and hard spectrum separately. The additional parameter is the
ratio of the hard to soft power law flux.

2. 2009A&A...502..457G
Re:NGC 6300
A.1.8 NGC 6300 This is one of a sample of "changing-look" AGN whose spectra
exhibit transitions between Compton-thick and Compton-thin obscuration on
timescales of years (Matt et al. 2003). It was found to be reflection-dominated
in 1997, but has since been in a Compton-thin state (RXTE and BeppoSAX analysis;
Guainazzi 2002). Assuming a Compton-thin column of N_H_ = 2 x 10^23^ cm^-2^
(from the XMM-Newton analysis of Matsumoto et al. 2004) obscuring a PL with
{GAMMA} = 2.42 (Beckmann et al. 2006) and normalizing to JEM-X and ISGRI 2-100
keV fluxes of the later publication, the implied intrinsic log L_2-10_ = 42.76.
But, in addition to its changing-look nature, the source also exhibits large
flux variability (Awaki et al. 2006), and a much lower luminosity of log L_2-10_
= 41.8 was derived by Matsumoto et al. (2004) from their XMM-Newton analysis. We
use a mean log L_2-10_ = 42.3.

3. 2007AJ....134..648M
Re:NGC 6300
NGC 6300 (Figs. 7.63, 9.63, 20.63): This galaxy is heavily obscured, so only
faint diffuse emission can be appreciated in our image.

4. 2007A&A...461.1209D
Re:NGC 6300
NGC 6300: The source as observed by BeppoSAX is Compton-thin (Guainazzi
2002), and the primary emission is seen through an absorber with N_H_
=2.5 x 10^23^ cm^-2^. Nonetheless, the source was seen in a reflection
dominated state (Leighly et al. 1999).

5. 2004A&A...415..941E
Re:NGC 6300
NGC 6300: Both Mulchaey et al. (1997) and Laine et al. (2002) have suggested
that this galaxy is double-barred (though with disagreements about the size of
the inner bar). Inspection of the NIMCOS2 F160W image shows that the inner
isophotes are indeed elongated and twisted; however, these are distortions
caused by a strong dust lane (clearly visible in WFPC2 images).

6. 2003ApJS..146..353M
Re:NGC 6300
NGC 6300 (C)
This galaxy is difficult to classify as the nucleus falls in a corner
of the H image. There is a great deal of dust visible in the color
map, and the V image shows that this dust extends to the south, yet it
is dominated by a large cloud of dust rather than any filamentary
structure. A two-arm spiral is apparent at larger scales than shown in
these frames.

7. 2002ApJS..143...73E
Re:NGC 6300
NGC 6300.---SB(r)a: Slightly elliptical nucleus, and bulge. Strong bar
is skewed to bulge major axis by ~45deg. Bar intersects a ring/tight
arms. Bright ansae at the intersections. Ring/arms are patchy but
fairly well defined. Ring/ arms clearly have many knots, despite
obvious contamination by foreground stars. The optical types for
this galaxy are SB(rs)b (RC3), SBb(s)II pec (CAG), and SAB(r)bc (OSU
B). The substantially earlier type in the near-IR is due to the
enhanced prominence of the bulge in the H band compared to the

8. 2002A&A...389...68G
Re:NGC 6300
NGC 6300: the results of the kinematical values of
Ryder et al. (1996) and of Buta (1987b) are in perfect
agreement, so we adopt these values. Our two methods are
less reliable, since the HII regions are mainly lying in
a ring for both catalogs. Nevertheless, it is worth noting
that there is a reasonable agreement between our values and
the adopted ones and also with the rest of the values.

9. 2002A&A...386..379R
Re:NGC 6300
NGC 6300: in Fig. A.1 we plot the residuals of the best fit
of NGC 6300, obtained with model C, but without the Gaussian
component that fits the iron K line. The asymmetry of the
line is apparent: a clear "red wing'' extends down to ~4 keV,
while a broad blue wing is absent. We fitted this excess with
a relativistic line model. We used the DISKLINE model in XSPEC,
leaving all the parameters free. The best fit is obtained with
a strongly relativistic profile: the best fit inner radius of
the emitting region is 6.5 Shwarzchild radii; the inclination
is ~30^deg^. The improvement of the fit, with respect to the
simple Gaussian fit, is {DELTA}{chi}^2^ = 27. We also tried a
diskline modelem for a rotating disk, but the fit is worse,
since this model can well reproduce the broad red wing, but not
the narrow peak at E=6.1 keV. We note that a possible warning on
this result could come from the high N_H_ of this source
(N_H_ ~ 2 x 10^23^ cm-2). This implies that the continuum at the
low energy peak of the line is partially absorbed. This could
introduce systematic errors, making the reality of the red wing
of the line less certain than it appears in our fit.
Another possible scenario is the one proposed by Guainazzi
(2001): a good fit of the MECS spectrum can be obtained accepting
very high values of the ratio Rbetween the reflected and intrinsic
component (R~4). In this way the flat profile of the cold reflection
spectrum can reproduce the excess between 4 and 6 keV which has been
interpreted above as a relativistic wing of the iron line. Such high
values of R are possible, as suggested by Guainazzi (2001), if the
intrinsic flux is variable, since the observed reflection component
is produced by radiation emitted at a different time with respect to
the observed primary emission.

10. 2000ApJ...544..747S
Re:NGC 6300
The near-UV W values, CR, and spectral distribution are best reproduced
by a mixture of a bulge template plus 10% mass contribution of a 1 Gyr
stellar population. The model is compared with the data in Fig. 17c, where
the HOBL are at the limit of detection.

11. 1999AJ....117.2676R
Re:NGC 6300
The overall morphology of the extinction in NGC 6300 (Fig. 2t)
shows no organization except that the extinction is much stronger to the
south of the nucleus than to the north with the peak emission being just
south of the nucleus.

12. 1999A&AS..137..457M
Re:NGC 6300
NGC 6300: The radio morphology (Fig. 13) of this object is slightly

13. 1998MNRAS.297..579C
Re:NGC 6300
NGC 6300. Storchi-Bergmann & Pastoriza (1989) observed the nuclear stellar
population of this galaxy to be old, with a small contribution from
intermediate-age stars. The Ws do not show a clear gradient (Fig. 26), with Ca K
varying between S2 and S3 templates, while the G band and Mg vary between S4 and
S5. The continuum ratios decrease from values much larger than those of an S1
template at the nucleus to values typical of an S6 template at 10 arcsec and
farther out, bluer than the values predicted from the Ws in this region.

14. 1997ApJS..110..299M
Re:NGC 6300
A large-scale bar is clearly visible in both the ellipse fits and the K_S_
image. A second bar on small scales (<~4") may also be present.

15. 1996ApJS..105..353C
Re:NGC 6300
NGC 6300 (Fig. 3, bottom).--H II regions concentrate along and just outside the
inner pseudoring (see also Ryder & Dopita 1993). They extend into the diffuse
outer disk region and do not concentrate at the bar ends. Instead, they
concentrate nearly perpendicular to the bar. There is one bright H II region in
the northeast side of the bar located near a dust lane. The region inside of
the ring is mostly devoid of H II regions, except for intense nuclear emission.

16. 1996ApJS..105...93E
Re:NGC 6300
4.13. NGC 6300
NGC 6300 was first classified as a Seyfert 2 galaxy on the basis of the nuclear
emission-line profiles from optical spectrophotometry obtained by Phillips et
al. (1983). Additional optical spectra were obtained by Bonatto, Bica, & Alloin
(1989), who conclude that shock heating may play a role in the ionization
balance of the nucleus. Storchi-Bergmann & Pastoriza (1989) obtained further
optical spectrophotometry, and on the basis of comparison with photoionization
models, they concluded that the nuclear N/O ratio must be enhanced by a factor
of ~3 above the solar value. An H{alpha} image of the object is presented by
Ryder & Dopita (1993). Our continuum-subtracted H{alpha} image (Fig. 1) reveals
a wealth of compact H II regions and diffuse H{alpha} emission, both in the
ring structure and extending out to over 2' from the nucleus. There is some
evidence for weak H{alpha} emission interior to the ring, although this is
mostly diffuse. This is a low galactic latitude object and suffers from having
numerous faint foreground stars in the field. As discussed in section 3, a
small fraction of these may be misclassified as emission-line sources.

17. 1994CAG1..B...0000S
Re:NGC 6300
SBb(s)II pec
May 11/12, 1980
103aO + GG385
45 min
NGC 6300 is in low galactic latitude (b = -14^deg^),
and may have Galactic dust silhouetted
against its face.
The original plate from which the print here
is made was obtained in poor seeing, clearly seen
from the size of the stellar images.
The bar is ill defined but evidently is
straight. The arms spring from opposite sides of
outer regions, far from the nucleus and, evidently,
from the ends of a bar.
Dust is evident, but, again, some of what is
seen may be of superposed Galactic origin. The
arms are branched, one after about half a revolution
from its origin on the bar. The other arm
branches twice, once after about 15^deg^ of unwind
and again after about a one-quarter additional
turn. Outer, low-surface-brightness fragmented
multiple arms are extensions of the bright inner

18. 1993ApJS...88..415R
Re:NGC 6300
Yet another galaxy that suffers from being at low Galactic latitude,
NGC 6300 suffers particularly badly due to having two moderately bright
foreground stars right next to the nucleus. Fortunately, most of the
star-forming action seems to be taking place further out in a ring some
2.5' in diameter. Continuum subtraction indicates almost no star
formation activity inside of this ring. A number of short arms merge to
form the ring with a ragged outer edge, but a remarkably sharp inner
Comparison of NGC 6300 with other spirals in our atlas which exhibit
both a strong stellar bar and an inner ring (e.g., NGC 1187, NGC 1398,
NGC 5643, NGC 6744) tentatively suggests a sequence whereby the greater
the number of H II regions contained in the ring, the fewer that go into
delineating the bar itself. Such a trend is not evident in the old
stellar distribution. Work by Combes (1988) and by Kenney & Lord (1991)
leads us to suspect that this may be associated with the torque induced
by the bisymmetric bar potential: a strong torque could inhibit star
formation in the bar region, while causing gas to accumulate at the ring
encircling the bar, leading to enhanced star formation there instead.
Buta (1987) has carried out an extensive surface photometry and kinematic
analysis of NGC 6300, but was unable to definitively identify the ring
with any orbital resonance. High-resolution H II observations (now
possible with the advent of the Australia Telescope radio synthesis
array) ought to help resolve this issue.

19. 1985SGC...C...0000C
Re:NGC 6300
Plate 1619
(r): 2.0 x 1.2.
Plate 1659
Overexposed center, bright bar with dust; patchy knotty (r): 1.9 x 1.1.
Very faint arms.
Plate 2523
Overexposed center, knotty (r): 2.0 x 1.1, faint arms.

20. 1982ESOU..C...0000L
Re:ESO 171218-6245.9
=ESO 101- G 25
stars superimposed

21. 1964RC1...C...0000d
Re:NGC 6300
Faint nucleus. There are several stars superimposed. Dark lane on a bar.
(r): 2.0 arcmin x 1.1 arcmin.
See also HB, 914, 8, 1940.
Occ. Notes R.A.S., 3, No.18, 1956.

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