scholarly journals Large scale distribution of gas, dust and stars deduced from observations from the UV to the IR

1991 ◽  
Vol 148 ◽  
pp. 69-70
Author(s):  
J. Koornneef
Keyword(s):  
Large Scale ◽  
Cross Correlation ◽  
Stellar Population ◽  
Dust Emission ◽  
Interstellar Extinction ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Stellar Associations

We introduce an as yet unpublished set of OAO-II observations of stellar associations in the Large Magellanic Cloud (LMC). Cross-correlation of the photometric characteristics of these fields with the infrared fluxes at these same positions obtained by the IRAS satellite provides information on the local stellar population, the amounts of interstellar extinction and thermal dust emission.

scholarly journals Discovery of an extended, halo-like stellar population around the Large Magellanic Cloud

2008 ◽  
Vol 4 (S256) ◽  
pp. 51-56 ◽  
Author(s):  
Steven R. Majewski ◽  
David L. Nidever ◽  
Ricardo R. Muñoz ◽  
Richard J. Patterson ◽  
William E. Kunkel ◽  
...  
Keyword(s):  
Large Scale ◽  
Stellar Population ◽  
Large Magellanic Cloud ◽  
Mean Value ◽  
Magellanic Cloud ◽  
Stellar Surface ◽  
Two Dimensional ◽  
Radial Limit ◽  
Dimensional Distribution ◽  
Red Giant

AbstractWe describe an ongoing, large-scale, photometric and spectroscopic survey of the Large Magellanic Cloud (LMC) periphery. This survey uses WashingtonM,T2+DDO51 photometry to identify distant LMC red giant branch (RGB) star candidates; multi-object spectroscopy is used to confirm the stellar surface gravities of these RGB stars and their association with the LMC (e.g., through radial velocities). The survey now encompasses hundreds of fields ranging from the LMC center with full azimuthal coverage around the LMC and out to 23° from the LMC center. We have confirmed the existence of RGB stars with (the unusual) Magellanic velocities out to the radial limit of this survey coverage. From data in a subsample of these fields, we show that this extended population of stars makes up a diffuse structure enveloping the LMC with a two-dimensional distribution resembling a classical halo with a shallow de Vaucouleurs profile and a broad metallicity spread around a typical mean value of [Fe/H] ~ −1.0.

Infrared Studies of the Young Stellar Population of 30 Doradus

1980 ◽  
Vol 4 (1) ◽  
pp. 90-92
Author(s):  
P. J. McGregor ◽  
A. R. Hyland
Keyword(s):  
Star Formation ◽  
Stellar Population ◽  
Cluster Formation ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Formation Processes ◽  
Excellent Opportunity ◽  
Infrared Studies ◽  
30 Doradus

The 30 Doradus region offers an excellent opportunity to study cluster formation processes and recent star formation in the Large Magellanic Cloud.

Wide Field Star Count Mapping of Large Scale Areas of Star Formation in the Large Magellanic Cloud

1994 ◽  
pp. 516-517
Author(s):  
E. Kontizas ◽  
S. E. Maravelias ◽  
A. Dapergolas ◽  
Y. Bellas-Velidis ◽  
M. Kontizas
Keyword(s):  
Star Formation ◽  
Large Scale ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Wide Field ◽  
Field Star ◽  
Star Count

scholarly journals A Photometric Survey of Field Stars in the Large Magellanic Cloud: Probing its Star-Formation History

1999 ◽  
Vol 190 ◽  
pp. 343-344 ◽  
Author(s):  
T. A. Smecker-Hane ◽  
J. S. Gallagher ◽  
Andrew Cole ◽  
P. B. Stetson ◽  
E. Tolstoy
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Stellar Population ◽  
Formation Rate ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Formation History ◽  
Wide Field ◽  
Formation History ◽  
Magnitude Diagram

The Large Magellanic Cloud (LMC) is unique among galaxies in the Local Group in that it is the most massive non-spiral, is relatively gas-rich, and is actively forming stars. Determining its star-formation rate (SFR) as a function of time will be a cornerstone in our understanding of galaxy evolution. The best method of deriving a galaxy's past SFR is to compare the densities of stars in a color-magnitude diagram (CMD), a Hess diagram, with model Hess diagrams. The LMC has a complex stellar population with ages ranging from 0 to ~ 14 Gyr and metallicities from −2 ≲ [Fe/H] ≲ −0.4, and deriving its SFR and simultaneously constraining model input parameters (distance, age-metallicity relation, reddening, and stellar models) requires well-populated CMDs that span the magnitude range 15 ≤ V ≤ 24. Although existing CMDs of field stars in the LMC show tantalizing evidence for a significant burst of star formation that occurred ~ 3 Gyr ago (for examples, see Westerlund et al. 1995; Vallenari et al. 1996; Elson, et al. 1997; Gallagher et al. 1999, and references therein), estimates of the enhancement in the SFR vary from factors of 3 to 50. This uncertainty is caused by the relatively large photometric errors that plague crowded ground-based images, and the small number statistics that plague CMDs created from single Wide Field Planetary Camera 2 (WFPC2) images.

scholarly journals SPITZEROBSERVATIONS OF DUST EMISSION FROM H II REGIONS IN THE LARGE MAGELLANIC CLOUD

2014 ◽  
Vol 784 (2) ◽  
pp. 147 ◽  
Author(s):  
Ian W. Stephens ◽  
Jessica Marie Evans ◽  
Rui Xue ◽  
You-Hua Chu ◽  
Robert A. Gruendl ◽  
...  
Keyword(s):  
Dust Emission ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
H Ii Regions

scholarly journals Kinematics of the LMC CH-stars

1991 ◽  
Vol 148 ◽  
pp. 77-80 ◽  
Author(s):  
F.D.A. Hartwick ◽  
A. P. Cowley
Keyword(s):  
Globular Cluster ◽  
Stellar Population ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

Velocities have been measured for 74 CH stars in the direction of the Large Magellanic Cloud (LMC). These have been used to study the kinematics of the oldest stellar population. Velocities of these objects appear to reflect two distinct subgroups - one associated with the old globular cluster population and a second with the LMC disk.

Interstellar extinction in the Large Magellanic Cloud

Nature ◽  
1980 ◽  
Vol 283 (5749) ◽  
pp. 725-729 ◽  
Author(s):  
K. Nandy ◽  
D. H. Morgan ◽  
A. J. Willis ◽  
R. Wilson ◽  
P. M. Gondhalekar ◽  
...  
Keyword(s):  
Interstellar Extinction ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud
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