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Date and Time of the Query: 2018-12-17 T03:39:26 PST
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Notes for object NGC 0300

14 note(s) found in NED.


1. 2007ApJS..173..538T
Re:NGC 0300
NGC 300 (Fig. 16.1).-GALEX imaging of this SA(s)d galaxy reveals a bright inner
disk filled with SF complexes, in addition to an outer disk occupied by low
surface brightness, wispy arcs of clumpy XUV emission. Radial surface brightness
profiles in FUV and NUV from the GALEX Atlas (Gil de Paz et al. 2007a) indicate
a downward break in the slope of the profile at the D_25_ radius. NGC 300 is
known to have a large H I envelope (D_H I_ ~ 61'; Puche et al. 1990) with a warp
beginning at radii of 10'. The outer parts of this H I distribution are only
very sparsely populated with UV clumps. Some of the XUV disk clusters associated
with NGC 300 can be recognized on the DSS2-red plate, using the UV imagery as a
prior. Bland-Hawthorn et al. (2005) recently reported a disklike component of
the resolved stellar population out to 10 radial scale lengths (24', or
2.2r_25_) in this galaxy. A causal relation between the outer disk star
formation evident from our GALEX data and the extended disk of Bland-Hawthorn
remains speculative, however. A member of the Sculptor group, NGC 300 is
frequently described as a twin of M33. It dominates a "loose quartet"
(Karachentsev et al. 2003) of Sculptor galaxies including NGC 55, ESO 410-05,
and ESO 294-10 (later two are not listed in the NOG catalog; Giuricin et al.
2000).

2. 2004ApJ...608...42S
Re:NGC 0300
NGC 300. Eighteen Cepheids were discovered by Graham (1984) based on
photographic data; CCD BVRI photometry was obtained for 16 of these by
Freedman et al. (1992) and used to calculate the distance reported in
column (2) of Table 3. Recently, Pietrzynski et al. (2002) recovered and
refined the magnitudes and periods for all of Graham's variable stars,
using BV ground-based CCD data. This study revealed that three of the
Cepheids used by Freedman et al. (1992) were blended. These were
excluded for the purpose of this paper; the distances listed in
columns (3) and (4) of Table 3 were calculated from the remaining 13
Cepheids using the periods and V-band magnitudes from Pietrzynski
et al. (2002) and the I-band magnitudes from Freedman et al. (1992).

3. 1999ApJ...519...89C
Re:NGC 0300
NGC 300.-This is a normal spiral galaxy similar to M33 in
appearance, located in the Sculptor group. We did not find any compact
X-ray sources within 2' of the nucleus of NGC 300.

4. 1999A&AS..136...35S
Re:NGC 0300
NGC 300 -- Fifteen positions were observed by D'Odorico et al. (1983) in
this Sculptor group galaxy often considered as a twin of M 33. Two
regions showed He II {lambda}4686 one also C IV {lambda}5808. Several
investigations were undertaken subsequently to search for individual WR
stars or small clusters. The latest work (Breysacher et al. 1997, cf.
references therein) detected 12 WR stars increasing the total to 34
known WR stars.

5. 1997AstL...23..656G
Re:NGC 0300
NGC 300. We estimated the magnitude V(5) for stars with U-B<0.1 using the
color-magnitude diagram of Friedman (1984). The estimate of V(5) is unreliable.

6. 1997AstL...23..644G
Re:NGC 0300
NGC 300. Freedman et al. (1992) (Cepheids); Humphreys and Graham (1986) (R 13,
R10, R14); Friedman (1984) (we selected the brightest blue stars using the
color-magnitude diagram alone).

7. 1994CAG1..B...0000S
Re:NGC 0300
South Polar Group
Sc(s)II.8
CD-2044-Bedke/Gregory
Nov 2/3, 1981
103aO
90 min
NGC 300 is a member of the South Polar
Group (de Vaucouleurs 1959a), which also
contains the well-resolved galaxies NGC 55,
NGC 147, NGC 253, and NGC 7793, The distance
modulus of NGC 300 is small, at m - M = 26.5
(D = 2.9 Mpc), determined from Cepheids
(Graham 1984). Because the distance is so small,
resolution into individual brightest stars in many
well-defined associations is exceptionally easy,
beginning at about B = 18 (estimated).
The brightest stars are contained in the
associations. Yet, only slightly fainter stars that
are also young are spread throughout the interarm
region.
The spiral-arm pattern is massive in the
sense of Reynolds (1927a,b). At least two major
arms exist on each side of the minor axis. Three
arm crossings of the major axis can be traced on
each side of the image.

8. 1985SGC...C...0000C
Re:NGC 0300
Plate 846
Well resolved, several stars superposed. Several background galaxies near.
Plate 1681r
Extremely small bright nucleus, well resolved, many knots. Similar to M33.

9. 1982ESOU..C...0000L
Re:ESO 005232-3757.2
=ESO 295- G 20
strong HII regions

10. 1976RC2...C...0000d
Re:NGC 0300
In the Sculptor Group.
Photograph:
Zeit. fur Ap., 64, 212, 1966.
Photometry:
Atlas Gal. Australis, 1968.
Dynamics, Mass Determination and M/L Ratio:
Astr. Ap., 16, 165, 1972.
HI 21cm:
Ap. J., 142, 616, 1965.
Ap. J., 150, 9, 1967.
Australian J. Phys., 20, 131, 1967.
HII Regions:
Zeit. fur. Ap., 64, 212, 1966.
H{alpha} Interferometry in the Disk:
Astr. Ap., 12, 379, 1971.
Radio Observations:
M.N.R.A.S., 152, 439, 1971.

11. 1964RC1...C...0000d
Re:NGC 0300
In the Sculptor Group with NGC 0045, NGC 0055, NGC 0247,
and NGC 7793 (Ap. J., 130, 718, 1959).
Extremely small, bright nucleus or star.
Well resolved,
Dark lanes.
Emission-line object.
Mt. Wilson velocity for "brighter of two emission patches
2.8 arcmin [south-preceding] nucleus." = +200 km/sec.
Photograph:
Occ. Notes R.A.S., 3, No.18, 1956.
Photometry:
Ap. J., 136, 107, 1962.
HII Regions:
Obsevatory, 79, 54, 1959.
Zeit. fur Ap., 50, 168, 1960.
HI Emission:
Epstein, Harvard Thesis, 1962.
Radio Emission:
Austral. J. Phys., 8, 368, 1955.
Handbuch der Phys., 53, 253, 1959.

12. 1961AJ.....66..541B
Re:NGC 0300
3. NGC 55 Group
De Vaucouleurs (1959) has argued that NGC 45, 55, 247, 253, 300, and 7793 form a
physical group about 8X 10^5^ pc in diameter. The group is only about 2.5 X
10^6^ pc distant and the galaxies are all spirals. The argument for their
forming a physical group is based on their distribution among the other bright
galaxies in the southern hemisphere. From the radial velocities, de Vaucouleurs
showed that the virial theorem would not be satisfied unless the average masses
of the galaxies were in excess of 10^12^ M_sun_, with a mass-to-light ratio
greater than 500. Thus if the galaxies form a physical group, it must be
expanding, unless there is a large concentration of intergalactic matter.

13. 1959ApJ...130..718D
Re:NGC 0300
NGC 300
The velocity +200 +/- 40 km/sec measured by Humason on a low-dispersion
spectrogram refers to the brighter of two emission patches 2'8 south-preceding
the nucleus. This region is very close to the minor axis of the system, which is
tilted about 45^deg^ to the line of sight, and the rotational component in the
observed velocity must be very small.

14. 1957HPh....53..275d
Re:NGC 0300
SA(s)d
(Plate 33)
A very small, round nucleus, similar to a globular cluster,
lies in the middle of the central region, from which emerge
several, highly resolved and branching arms of low surface
brightness.
Compare with NGC 7793 (Plate 20), and NGC 0045 (Plate 34).


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