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Notes for object NGC 1300

20 note(s) found in NED.

1. 2008MNRAS.386.2242H
Re:NGC 1300
NGC 1300 and NGC 2748 - NGC 1300 has spiral-like dust lanes down to the
centre, wrapping around the nucleus (Scarlata et al. 2004) and
connecting to the leading edge of a strong kpc-scale bar (Martini et al.
2003), which suggests gas inflow in both large and small scale. The
bulge of NGC 1300 is disc-like with Sersic index n= 1.3 (Laurikainen et
al. 2004), and identified as a pseudo-bulge by Kormendy & Fisher (2005).
The nuclei of N2748 are not well defined in HST observations due to
dust-lane obscuration (Scarlata et al. 2004). The masses of SMBHs in NGC
1300 (6.6^+6.3^_-3.2_ x 10^7^ M_sun_) and NGC 2748 (4.4^+3.5^_-3.6_ x
10^7^ M_sun_) are measured by nuclear gas kinematics (Atkinson et al.
2005). The authors neglected the effect of extinction by dust in the
analysis of the gaseous rotation curves. The extinction in the H band
which was used to measure the black hole masses yields an
underestimation in luminosity of ~20 per cent for NGC 1300 and ?58 per
cent for NGC 2748 in their central 50 pc regions. Furthermor e, the
extinction is probably uneven due to the complex dust structures.
Therefore, the M_bh_ in two galaxies is not well estimated. Their
results are much higher than the prediction of M_bh_-{sigma}* or M_bh_-L
relations ( 7 x 10^6^ or 2 x 10^7^ M_sun_ for NGC 1300; 6 x 10^6^ or 7 x
10^6^ M_sun_ for NGC 2748). In fact, the HST can only barely resolved
the sphere of influence of SMBHs with the mass predicted by the
M_bh_-{sigma}* or M_bh_-L relations ( rbh= 0.04 ~ 0.1 arcsec for NGC
1300; r_bh_ = 0.03 arcsec for NGC 2748).

2. 2008ApJS..174..337M
Re:NGC 1300
NGC 1300 (Fig. 5d).-Twelve H II regions form a small complete ring in H{alpha},
although there is no clear pattern in EWs.

3. 2005ApJS..160...76B
Re:NGC 1300
A low level of discordance and good S/N has produced a velocity field showing
rotation and a clear centrally peaked {sigma} _*_ field. Color maps suggest
possible obscuration from spiral structures (Hughes et al. 2003). See Figures 6
and 10b.

4. 2004A&A...415..941E
Re:NGC 1300
NGC 1300: Suggested as a possible double bar by Moiseev (2001), on the basis of
optical plates in Baumgart & Peterson (1986). Using ground-based and NICMOS
near-IR images, Perez-Ramirez et al. (2000) found a nuclear ring, but no
evidence for an inner bar.

5. 2003ApJS..146..353M
Re:NGC 1300
NGC 1300 (GD)
This very well known, strongly barred galaxy is one of the prototypes
of the grand-design nuclear dust spiral class. The dust lanes clearly
connect to the dust lanes along the leading edges of the bar studied
by Lindblad & Kristin (1996).

6. 2003AJ....126..742H
Re:NGC 1300
The morphological classification as determined by us is indicated in
parentheses next to the galaxy name, with our "chaotic circumnuclear
dust" (C) category now not including those galaxies with obvious dust
lanes (DL). Where the classification has already been made by Martini
et al. (2003), we indicate this with "-mp."
3.5. NGC 1300 (GD-mp)
Figure 2 (bottom).
Spectra: There is some continuum and a broad feature on NUC spectrum.
Generally, emission lines are faint.
Images: Color map shows spiral structure down to the resolution of

7. 2002MNRAS.337..808K
Re:NGC 1300
A1 NGC 1300
This barred galaxy is a prototype grand-design SBb spiral. It has a very
prominent and smooth bar and two spiral arms that start abruptly at the end
of the bar (Fig. 1a). In our B-I image, we can see two straight, offset
dust lanes rather parallel to the major axis of the bar. These dust lanes
are smooth when compared with the arms, which corresponds to a lack of
distinct emitting regions. It is also apparent from our colour map that,
near the ends of the bar, the bar dust lanes join the dust lanes along the
inner edge of the arms. SF is not obvious in the bar, nor in the nucleus.
The CNR is a site of considerable SF, concentrated in a small area. There
is a concentration of HII regions where the arms join the bar, and mainly
so on the western side. The western arm also contains several very luminous
HII regions, while the eastern arm shows some less luminous enhancements.
The H{alpha} profile shows a modest peak of luminosity at radii
corresponding to those of the CNR, and a gradual decrease in the region of
the bar. The radial profiles reflect and confirm the distribution of SF in
this galaxy.
The nuclear ring in NGC 1300 (Figs 1a and 2a) is rather small
angularly, and our H{alpha} image does not give much information. It is
clear, however, that the massive SF occurs in a number of discrete clumps
(see also Pogge 1989), which are not reproduced in the NIR colour index
images. Whereas the nuclear ring is incomplete in H{alpha}, it appears
complete in the NIR, although in Paper I we showed that the NIR ring is in
fact a pair of tightly wound spirals. The HST image (fig. 1 of Paper I)
shows structure in the nuclear ring, but no hotspots corresponding to the
H{alpha} emission peaks.

8. 2002ApJS..143...73E
Re:NGC 1300
NGC 1300.---SBb (type example---see Fig. 3e): Strong bar, aligned with
bulge major axis. Arms commence at the ends of the bar and are roughly
perpendicular to the bar. Arms extend roughly 180deg before fading. Far
ends of the arms straighten out, rather than curving back into a
pseudoring. Arms rich with star-forming knots.

9. 2002A&A...391...83B
Re:NGC 1300
NGC 1300 (Fig. 6) has one of the most pronounced optical bars in
our sample. Total radio intensity is maximum in the nuclear region
and at the ends of the bar where the spiral arms start (both are
sites of strong star formation). No significant radio emission has
been detected in the bar. The polarized emission is weak. The
northern extensions visible in the maps at {lambda}22 and {lambda}6 cm
are not real and result from poor data coverage in the uv plane. The
{lambda}18 cm and {lambda}3 cm maps show less emission than those at
{lambda}22 cm and {lambda}6 cm because the signal-to-noise ratios are

10. 2000MNRAS.317..234P
Re:NGC 1300
3.1 NGC 1300
Our broad-band NIR images are remarkably smooth, and do not show any
structure in the CNR (Fig. 2a). The colour index images, however, show a
red ring-like structure, possibly outlining a single spiral arm that
departs from the nucleus towards the west side of the image and
continues to wrap around the nucleus until it closes in a ring. This
ring appears more continuous and broader in the northern part than in
the south where it looks patchy. The feature seen in our NIR colour
index map cannot be an artefact of combining two images with slightly
different spatial resolution, because such an artefact would show up as
a complete ring, whereas the observed red feature is not at constant
galactocentric radius. Pogge (1989a) saw an incomplete nuclear ring in
H{alpha} emission with a number of distinct 'hotspots'.
The HST H-band image resolves the nuclear ring into a series of
tightly wound spiral armlets, outlined in dust and stellar populations.
The ring region is of a relatively low amplitude compared with the
central bulge component, in contrast to nuclear rings in other objects,
e.g. NGC 3351, as can be observed in Fig. 1.
The location of the ring corresponds to a bump in all radial profiles
(i.e. surface brightness, colour, ellipticity and PA). The J-K colour of
the ring is redder by 0.1 mag than the background. No isophotal twists
are seen in the ellipticity and PA profiles or in the contour map of the
K-band image. Thus we confirm that there is no evidence for a nuclear
bar (Regan & Elmegreen 1997).

11. 1994CAG1..B...0000S
Re:NGC 1300
Hubble Atlas, p. 45
Oct 14/15, 1950
30 min
NGC 1300 is the prototype for the spiral
pattern where the arms spring from the ends of
the bar. Most galaxies of this spiral-arm subclass
(s) have grand design arms rather than a filamentary,
multiple-armed MAS pattern where the
arms generally begin tangent to an almost-complete
ring (which defines the (r) subclass). The
arms in NGC 1300 are tightly wound but not as
tightly as in NGC 3185 (Sa; panel 99) where they
nearly overlap after each arm unwinds by half a
revolution to form an almost-complete inner ring.
SBb(s) galaxies like NGC 1300 have several
distinctive features characteristic of the class. (1)
The bar is well formed and prominent. (2) In
most SBb(s) types two straight dust lanes exist
within the bar, each on the outside of the otherwise
smooth bar; the lanes are on symmetrically
opposite sides of the central amorphous center.
In every case, the dust lanes are on the sides of
the bar that lead the rotation, the direction of
the rotation being judged from the sense of the
spiral pattern. (3) Recent star formation is
generally most robust in the arms near the ends
of the bar. The increased star-formation rate
near these two points is clearly evident in the
arms and outer tips of the bar in NGC 1300,
shown by the many bright knots that are probably
small HII regions. None of the candidate HII
regions resolve at the 2" level. The redshift of
NGC 1300 is v_o = 1526 km/s.
These several characteristic features have
been reproduced in a series of theoretical studies
concerned with the hydrodynamic response of
the gas in the disk to the presence of the rotating
bar. Following pioneering work by Prendergast
(1962), detailed hydrodynamical models of the
velocity field and the presence of shocks in the
gas in the neighborhood of the bar have been
made. The early papers that predict the velocity
field in detail are by Huntley (1978), Huntley,
Sanders, and Roberts (1978), Roberts, Huntley,
and van Albada (1979), Peterson and Huntley
(1980), and Huntley (1980). A review up to
1983 is given by Prendergast (1983).
The comparison of the calculated models
with the observed features in NGC 1300 is
generally so close that it can be said that the
straight dust lanes in SBb(s) types and the
enhanced star-formation rate at the ends of the bar
are both understood. The features are related to
the shock properties of the gas at these points.
In viewing the SBb galaxies in this section
and in the SBc section later, it is useful to keep
in mind the three conclusions of Prendergast
(1) Weak bars give open spiral patterns
which extend throughout the gas;
stronger bars give spirals which emerge at
sharp angles to the bar. [added here: as in
NGC 1300]
(2) The gas response leads the bar,
by an angle which is greater the weaker the
(3) Strong bars favor the appearance
of strong shocks within the bar.
When they occur, they lie near the leading
edge, which is just where they should be if the
identification of shocks and dust lanes is

12. 1985SGC...C...0000C
Re:NGC 1300
Plate 3749
Overexposed center, pretty bright bar, thin knotty arms.
Plate 5541
(r'): 2.8 x 2.0.

13. 1976RC2...C...0000d
Re:NGC 1300
Description and Classification:
P.A.S.P., 81, 51, 1969.
Vistas in Ast., Vol. 14, 241, 1972.
A.J., 78, 606, 1973.
J.R.A.S. Canada, 68, 117, 1974.
Sov. A.J., 10, 34, 1966.
A.J., 78, 606, 1973.
HII Regions:
"Atlas and Catalogue", Univ. of Washington, Seattle, 1966.
Ap. J., 155, 417, 1969.
Radio Observations:
Astr. Ap., 29, 249, 1973.

14. 1974UGCA..C...0000N
Re:UGCA 066
UGCA 066:
SB(rs)bc (RC1)

15. 1968MCG4..C...0000V
Re:MCG -03-09-018
Pair with MCG -03-09-017. {rho}=19.5 arcmin. Type of MCG -03-09-017: vB - E2,
Morg - gk?D2.

16. 1968MCG4..C...0000V
Re:MCG -03-09-018
Widely known, typical SB. {omega}=49 degrees, {mu}1=77 degrees, {mu}2=80
degrees, {phi}1=205 degrees, {phi}2=190 degrees, l1=1.6, l2=1.5.
Type: Sand - SBb, vB - SBb I, Morg - fB2-gB3, Vauc - SB(rs)bc. Photo:
Handbuch der Astrophysik 5; Lick 13; ScA 1956 Sept; PASP 70, 364; ST 18
No. 3; Rudaux and de Vaucouleurs, Astronomie, Paris, 1948; Gas Dynamics
of Cosmic Clouds; Lund A, No. 10; Sand (SBb(s)). Red shift: +1538,
emission of H{alpha} and [N II] (ApJ 135, 694); CI=0.53, Cp'=0.67.
Photometry of the nucleus, mass, density distribution: Gorbachev
(Sov AJ (Russian) 43, No. 1, 46, 1966).

17. 1964RC1...C...0000d
Re:NGC 1300
Very small, extremely bright nucleus
in a narrow bar: 2.3 arcmin x 0.5 arcmin
Pseudo (r): 2.7 arcmin x 2.0 arcmin.
2 main regular, partially resolved arms form loops:
3.9 arcmin x 3.5 arcmin
4.3 arcmin x 3.5 arcmin
P.A.S.P., 59, 309, 1947.
Handbuch der Ap., 5, 2, 843, 1933.
I.A.U. Symp., No. 5, 1958 = Lick Contr. II, 81, 1958.
Ap. J., 135, 697, 1962.

18. 1961Hubbl.B...0000S
Re:NGC 1300
Oct. 14/15, 1950
30 min
Enlarged 7.5X
NGC 1300 is the prototype of the pure SBb(s). The bar is
distinct and smooth in texture. Two straight dust lanes
emerging on opposite sides of the nucleus can be traced
to the ends of the bar, where they turn sharply and follow
the insides of the spiral arms. The arms form nearly
complete ellipses. The foci of each ellipse are the nucleus and
the end of the bar of the opposite arm. Each arm can be
traced through about 340 degrees.

19. 1956AJ.....61...97H
Re:NGC 1300
HMS Note No. 021
Slit on bar.

20. 1918PLicO..13....9C
Re:NGC 1300
An unusually interesting two-branched spiral of the {phi}-type, 6' x 3' in p.a.
95^deg^; the whorls start abruptly from the extremities of straight extensions
on each side of the nucleus. Figure in Publ Astr. Soc. of the Pacific, Oct.
1912. Nucleus moderately large and bright; a few faint, almost stellar
condensations. 16 s.n.

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