scholarly journals Ultraviolet Imaging Telescope Observations of OB Stars in the N 11 Region of the Large Magellanic Cloud

1996 ◽  
Vol 472 (1) ◽  
pp. L29-L32 ◽  
Author(s):  
Joel Wm. Parker ◽  
Jesse K. Hill ◽  
Ralph C. Bohlin ◽  
Robert W. O'Connell ◽  
Susan G. Neff ◽  
...  
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Ob Stars ◽  
Imaging Telescope

A Nitrogen Rich OB Supergiant in the Large Magellanic Cloud

1975 ◽  
Vol 2 (6) ◽  
pp. 353-355 ◽  
Author(s):  
A.R. Hyland ◽  
M.S. Bessell
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Ob Stars ◽  
Striking Resemblance ◽  
Spectroscopic Investigations ◽  
Common Process

Recent spectroscopic investigations of OB stars by Walborn (1970,1971a) have revealed the existence of OB stars with anomalous nitrogen and carbon spectra. In particular, two groups of stars were identified — those with strong nitrogen features and accompanying weak carbon-oxygen blends (called ON stars), and those with weak nitrogen features and strong carbon features (called OC stars). These groups bear a striking resemblance to the WN, WC dichotomy exhibited by the Wolf Rayet stars and is suggestive that a common process may be responsible for both phenomena.

scholarly journals Discovery of a Stellar Association Surrounding the Massive Binary Sk–67°105 in the Large Magellanic Cloud

1999 ◽  
Vol 190 ◽  
pp. 235-236
Author(s):  
P. G. Ostrov ◽  
V. S. Niemela ◽  
N. I. Morrell
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Stellar Association ◽  
Ob Stars ◽  
Spectroscopic Binary ◽  
Short Period ◽  
H Ii Region ◽  
Compact Cluster

Sk–67°105, a luminous O4f type stars in the Large Magellanic Cloud, is the exiting star of the H II region N 50 (DEM 193). Niemela & Morrell (1986) found this hot star to be a massive short period double lined spectroscopic binary. Because luminous OB stars are usually found in young stellar groups, we have searched for such an aggregate in the vicinity of Sk–67°105.Here we report, as a result of our search, the discovery of a new OB association in the LMC. We also find that Sk–67°105 is the most luminous star of a small compact cluster inside this OB association.

A Deep Objective Prism Survey of Two Regions in the Large Magellanic Cloud for Ob and Supergiant Stars

1979 ◽  
Vol 47 ◽  
pp. 481-481
Author(s):  
A. G. Davis Philip ◽  
N. Sanduleak
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Ob Stars ◽  
Objective Prism

AbstractTwo regions in the Large Magellanic Cloud (centered atα = 5h 11m, δ= -66° 08’ (34B), α = 5h 27m, δ= -72° 15’ (47B) have been searched for OB and supergiant stars. A catalogue of 312 stars is presented in which objective prism spectral types, positions (1975), approximate B magnitues and cross identifications are given. About half the stars catalogued in each area are OB stars, the remainder are supergiants. The region at δ=-72° has two to three times as many F and G-type supergiants as the region at δ= -66°.

scholarly journals 21 Cm Hydrogen-Line Survey Of The Large Magellanic Cloud Ii. Distribution And Motions Of Neutral Hydrogen

1966 ◽  
Vol 19 (3) ◽  
pp. 343 ◽  
Keyword(s):  
Hydrogen Atom ◽  
Neutral Hydrogen ◽  
Hii Regions ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Radial Velocities ◽  
Hydrogen Line ◽  
Ob Stars ◽  
Mean Diameter ◽  
Line Survey

The 21 cm hydrogen-line data from a survey of the Large Magellanic Oloud with a 14',5 aerial beam have been simplified into distributions of intensities and radial velocities at profile peaks. Fifty-two large HI complexes of mean diameter 575 pc, density I hydrogen atom per cm3, and mass 4 X 106M o have been delineated. The study of the correlation between optically visible Population I components, such as HII regions and supergiant OB stars, and the neutral hydrogen has been greatly extended.

Spectroscopic Classification of 42 Large Magellanic Cloud OB Stars: Selection of Probes for the Hot Gaseous Halo of the Large Magellanic Cloud

2001 ◽  
Vol 113 (787) ◽  
pp. 1130-1139 ◽  
Author(s):  
Elizabeth G. Jaxon ◽  
Martín A. Guerrero ◽  
J. Chris Howk ◽  
Nolan R. Walborn ◽  
You‐Hua Chu ◽  
...  
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Ob Stars ◽  
Gaseous Halo ◽  
Selection Of

scholarly journals Glazar-2: A Wide-Field Camera Aboard the MIR Space Station

1994 ◽  
Vol 161 ◽  
pp. 55-56
Author(s):  
H.M. Tovmassian ◽  
Y.M. Khodjayants ◽  
M.N. Krmoyan ◽  
R.V. Isadjanian ◽  
O.N. Gasparian ◽  
...  
Keyword(s):  
Space Station ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Wide Field ◽  
Late Type ◽  
Uv Imaging ◽  
Imaging Telescope ◽  
Stellar Associations

In 1987 the UV imaging telescope Glazar (Tovmassian et al. 1988) was launched to the Mir Space Station. Its sensitivity was lower than was expected. For this reason the UV survey of the sky was not done and only observations of OB stellar associations were made. The fields of about 15 stellar associations and of the Large Magellanic Cloud were observed. Only images of O, B or early A type stars were obtained on the Glazar photographs at 1640 å. The observations allowed the detection of an average ∼ 15 % new, unknown OB type stars in each of the observed fields, the discovery of hot unknown components of some late type stars and a detailed study of the distribution of stars in space. Some new, unknown OB stellar associations were discovered and more correct distances of stellar associations were determined. The distribution of the absorbing matter was also studied. New, B-type stellar associations, named B were discovered.

scholarly journals Study of OB-Stars in the Large Magellanic Cloud by UBV Photometry

1973 ◽  
Vol 164 (1) ◽  
pp. 43P-48P
Author(s):  
K. Nandy ◽  
R. J. Dodd ◽  
R. D. Wolstencroft
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Ob Stars ◽  
Ubv Photometry

Distance to SN 1987A and the LMC

1999 ◽  
Vol 190 ◽  
pp. 549-554
Author(s):  
Nino Panagia
Keyword(s):  
Angular Size ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Light Curves ◽  
Distance Modulus ◽  
Absolute Size ◽  
Sn 1987A

Using the new reductions of the IUE light curves by Sonneborn et al. (1997) and an extensive set of HST images of SN 1987A we have repeated and improved Panagia et al. (1991) analysis to obtain a better determination of the distance to the supernova. In this way we have derived an absolute size of the ringRabs= (6.23 ± 0.08) x 1017cm and an angular sizeR″ = 808 ± 17 mas, which give a distance to the supernovad(SN1987A) = 51.4 ± 1.2 kpc and a distance modulusm–M(SN1987A) = 18.55 ± 0.05. Allowing for a displacement of SN 1987A position relative to the LMC center, the distance to the barycenter of the Large Magellanic Cloud is also estimated to bed(LMC) = 52.0±1.3 kpc, which corresponds to a distance modulus ofm–M(LMC) = 18.58±0.05.

Novae in the Magellanic Clouds

1979 ◽  
Vol 46 ◽  
pp. 96-101
Author(s):  
J.A. Graham
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
University Of Michigan ◽  
The Past ◽  
Spectroscopic Information ◽  
Objective Prism ◽  
The University ◽  
Small Cloud ◽  
Low Dispersion

During the past several years, a systematic search for novae in the Magellanic Clouds has been carried out at Cerro Tololo Inter-American Observatory. The Curtis Schmidt telescope, on loan to CTIO from the University of Michigan is used to obtain plates every two weeks during the observing season. An objective prism is used on the telescope. This provides additional low-dispersion spectroscopic information when a nova is discovered. The plates cover an area of 5°x5°. One plate is sufficient to cover the Small Magellanic Cloud and four are taken of the Large Magellanic Cloud with an overlap so that the central bar is included on each plate. The methods used in the search have been described by Graham and Araya (1971). In the CTIO survey, 8 novae have been discovered in the Large Cloud but none in the Small Cloud. The survey was not carried out in 1974 or 1976. During 1974, one nova was discovered in the Small Cloud by MacConnell and Sanduleak (1974).

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