Date and Time of the Query: 2019-05-20 T18:13:42 PDT
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Notes for object Large Magellanic Cloud

9 note(s) found in NED.

1. 2005ApJ...622..217W
Because the major methods of distance determination (Cepheids and
TRGB) are calibrated to an LMC distance of 18.50 (50 kpc), it is here
fixed at that distance.

2. 2005ApJ...622..217W
Neither of these has K-band photometry, for reasons that are obvious
on reflection. They are in fact brighter than most of the galaxies in
the sample and so by rights should be included somehow. However,
since they are so close to the Milky Way, their K luminosities do not
affect any calculations separately from it, and their luminosities
are almost certainly much smaller than the uncertainty in the Milky
Way's. They are therefore ignored in the K-band calculations.

3. 1997AstL...23..656G
The LMC. Humphreys and Davidson (1979) (a summary of photoelectric data on the
brightest stars of spectral types O, B, and A). The color-magnitude diagram of
Massey and Armandroff (1995) yields approximately the same LF (Fig. 1b, dashed
line). The LF (for B magnitudes) that was constructed from the data of the
survey (Humphreys 1979a) used by Sandage and Tammann (1974) is shifted to
fainter magnitudes by 0.4^m^.

4. 1997AstL...23..644G
The LMC. van den Bergh (1992) (a recommendation); Karachentsev and Tikhonov
(1994) - the selection that is based on the data of Humphreys (1979a) and
Vaucouleurs (1978a, 1978b).

5. 1994CAG1..B...0000S
Hubble Atlas, p. 38
Nov 4/5, 1951
103aE + Red Plexiglas
240 min
The print of the LMC here is made from an
original H{alpha} plate taken by Henize with the
Mount Wilson 10-inch refractor. This telescope had
been set up by Henize in South Africa in a
cooperative arrangement between the Carnegie
Institution, the University of Michigan, and the
South African Science Research Council.
The LMC is a satellite of our own Galaxy at
a distance modulus of m - M = 18.5 (D = 50 kpc),
determined from Cepheids.
Weak spiral features exist (de Vaucouleurs
1955). The galaxy is also rotating with a peak
velocity for young disk objects of 40 km/s
(reviewed by Andrews and Evans 1972, and by
Freeman, Illingworth, and Oemler 1983 with
references to previous data). The smallness of the
rotational velocity is presumed to be the reason
that the spiral pattern is so poorly developed
(compare Kennicutt 1981).

6. 1982ESOU..C...0000L
Re:ESO 052400-6948.
=ESO 056- G115
the Large Magellanic Cloud
optical centre defined by the symmetry of the bar

7. 1976RC2...C...0000d
Re:[RC2] A0524-69
= Large Magellanic Cloud
Member of the Local Group.
Interacting pair with the Small Magellanic Cloud at 21 deg.
For REVIEWS and REFERENCES see the Notes for Small Magellanic Cloud = A0051-73

8. 1964RC1...C...0000d
Re:[RC1] A0524
Large Magellanic Cloud.
Local Group.
Interacting pair with Small Magellanic Cloud at 21 degrees.
Note correction to HA 88,2 coordinates.
Monograph and References to 1954:
Suppl. Austral. J. Sci., 17, No.3, 1954.
B(asymptotic) = 0.63 (Ap. J., 131, 574, 1960).
Reviews and Additional References to 1960:
Trans. I.A.U., XI A, 292, 1961.
Reviews and Additional References to 1962:
"Advances in Astron. and Astroph.", 1, , 1963.
Reviews and Additional References to 1963:
I.A.U. Symposium No.20 (Canberra).

9. 1961Hubbl.B...0000S
Irr I
Nov.4/5, 1951
103aE + red plexiglass
Enlarged 1.6X
This is the Large Magellanic Cloud. The plate was taken
by Dr. Karl Henize with the Mount Wilson 10-inch refractor
in the light of H{alpha}. Although the form of this galaxy
suggests the lack of rotational symmetry, it is known
from the 21-cm radiation of neutral hydrogen (Kerr, Hindman,
and Robinson, interpreted by Kerr and de Vaucouleurs
(Australian J. Phys., 8, 508, 1956)] that the LMC is rotating.
de Vaucouleurs believes that the LMC has a flattened equatorial
plane inclined at 65 degrees +/- 5 degrees to the line
of sight (A. J., 60, 126, 1955). He also believes that a
very faint spiral pattern can be traced over the face of the
cloud, but the degree of spiral structure is certainly of a
different order from that in galaxies classed as Sa, Sb, and
Sc. The idea that this and the Small Magellanic Cloud
may be highly flattened systems is interesting because it
suggests that irregular galaxies are not so disorganized as
first inspection of photographs indicates.
The LMC contains many HII regions, open star clusters,
globular star clusters, and Cepheid variable stars. It
and the Small Cloud are the most important singie galaxies
in the sky, because they are the systems where the
tie-in of the absolute magnitudes of Cepheids with normal
stars must be made. The distance modulus for both
clouds is about (m-M) = 19.2. They are 10 times closer
to us than M31.
A catalogue of the HII regions in the LMC is given by
Henize in Ap. J. Suppl. Sec.,II, no. 22, 315, 1956. A
summary discussion of the stellar content is given by Buscombe,
Gascoigne, and de Vaucouleurs in the Supplement
to the Australian Journal of Science, 17, no. 3, 1954.
The largest HII region in the LMC is 30 Doradus. It
is a complex region containing overlapping Stromgren
spheres. Henize gives the dimensions of the nebulosity
as 1849 sec by 1781 sec of arc. At a distance modulus of
(m-M) = 19.2, these angles correspond to 640 parsecs by
615 parsecs. These dimensions are of the same order (a
factor of 2 larger) as those of NGC 0604 but are much larger
than the Orion Nebula and other large H{alpha} complexes that
have so far been recognized in our own galaxy.

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