HST imaging of the Large Magellanic Cloud: The field-star population near 30 Doradus

1994 ◽  
Vol 106 ◽  
pp. 632 ◽  
Author(s):  
Rebecca A. W. Elson ◽  
Duncan A. Forbes ◽  
Gerard F. Gilmore
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Field Star ◽  
30 Doradus

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.

scholarly journals The VLT–FLAMES Tarantula Survey

2009 ◽  
Vol 5 (S266) ◽  
pp. 35-40 ◽  
Author(s):  
C. J. Evans ◽  
N. Bastian ◽  
Y. Beletsky ◽  
I. Brott ◽  
M. Cantiello ◽  
...  
Keyword(s):  
Quantitative Analysis ◽  
Massive Stars ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Cluster Evolution ◽  
30 Doradus

AbstractThe Tarantula Survey is an ambitious ESO Large Programme that has obtained multi-epoch spectroscopy of over 1000 massive stars in the 30 Doradus region in the Large Magellanic Cloud. Here, we introduce the scientific motivations of the survey and give an overview of the observational sample. Ultimately, quantitative analysis of every star, paying particular attention to the effects of rotational mixing and binarity, will be used to address fundamental questions in both stellar and cluster evolution.

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 The Near Infrared Properties of Selected WN Stars in the Large Magellanic Cloud

1982 ◽  
Vol 99 ◽  
pp. 231-235
Author(s):  
N. Panagia ◽  
E.G. Tanzi ◽  
M. Tarenghi
Keyword(s):  
Near Infrared ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Infrared Photometry ◽  
Central Object ◽  
30 Doradus

We report here on preliminary infrared photometry of six WN stars in the Large Magellanic Cloud. Besides R136, the central object of the 30 Doradus Nebula, the sample includes three stars (R139, R140, R145) located near the center of the region (within ∼ 1 arcmin) and two more stars (R144, R147) at a distance of ∼ 5 arcmin from R136.

scholarly journals Studies of the large Magellanic Cloud using optical interstellar emission lines

1991 ◽  
Vol 148 ◽  
pp. 421-427
Author(s):  
J. Meaburn
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Emission Lines ◽  
Optical Observations ◽  
Sn 1987A ◽  
30 Doradus

Optical observations have been made of the halo of 30 Doradus, in the vicinity of SN 1987A and of giant shells in the LMC.

scholarly journals FROM GAS TO STARS IN ENERGETIC ENVIRONMENTS: DENSE GAS CLUMPS IN THE 30 DORADUS REGION WITHIN THE LARGE MAGELLANIC CLOUD

2014 ◽  
Vol 793 (1) ◽  
pp. 37 ◽  
Author(s):  
Crystal N. Anderson ◽  
David S. Meier ◽  
Jürgen Ott ◽  
Annie Hughes ◽  
Tony Wong ◽  
...  
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Dense Gas ◽  
30 Doradus

scholarly journals Superassociations in distant galaxies

1964 ◽  
Vol 20 ◽  
pp. 122-126 ◽  
Author(s):  
V. A. Ambartsumian
Keyword(s):  
Special Class ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Photographic Images ◽  
Large Complex ◽  
Distant Galaxies ◽  
Absolute Brightness ◽  
30 Doradus

It is well known that the Large Magellanic Cloud contains in addition to a considerable number of ordinary O-associations a certain number of large objects which, however, are similar in nature to the associations. These objects were named “constellations” by Shapley. But the large complex 30 Doradus surpasses notably all of these objects both in diameter and in absolute brightness. The latter is of the order of −15m0 while its diameter is of the order of 600 pc. If we take the average absolute brightness of associations in our Galaxy as equal to −10m0 then it turns out that 30 Doradus is 100 times more luminous than the ordinary associations. The photographic images of more distant galaxies reveal that sometimes complexes occur in them of the same order of luminosity and dimensions as 30 Doradus. Therefore it seems to us useful to regard these complexes as a special class of objects and call them superassociations.

CO J = 7 → 6 Emission in the Large Magellanic Cloud

2005 ◽  
Vol 13 ◽  
pp. 860-863
Author(s):  
Sungeun Kim ◽  
Wilfred Walsh ◽  
Kecheng Xiao ◽  
Adair P. Lane ◽  
Antony A. Stark
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Magellanic Clouds ◽  
The Antarctic ◽  
30 Doradus

AbstractWe present the first detection of 12CO (J = 7 → 6) emission in the Magellanic Clouds toward the 30 Doradus region using the Antarctic Sub-millimeter Telescope and Remote Observatory (AST/RO).

scholarly journals Radiative and mechanical feedback into the molecular gas in the Large Magellanic Cloud

2019 ◽  
Vol 628 ◽  
pp. A113 ◽  
Author(s):  
M.-Y. Lee ◽  
S. C. Madden ◽  
F. Le Petit ◽  
A. Gusdorf ◽  
P. Lesaffre ◽  
...  
Keyword(s):  
Far Infrared ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Continuum Emission ◽  
Molecular Gas ◽  
Stellar Content ◽  
Low Velocity ◽  
Line Energy ◽  
Star Forming ◽  
30 Doradus

With an aim of probing the physical conditions and excitation mechanisms of warm molecular gas in individual star-forming regions, we performed Herschel SPIRE Fourier Transform Spectrometer (FTS) observations of 30 Doradus in the Large Magellanic Cloud. In our FTS observations, important far-infrared (FIR) cooling lines in the interstellar medium, including CO J = 4–3 to J = 13–12, [C I] 370 μm, and [N II] 205 μm, were clearly detected. In combination with ground-based CO J = 1–0 and J = 3–2 data, we then constructed CO spectral line energy distributions (SLEDs) on ~10 pc scales over a ~60 pc × 60 pc area and found that the shape of the observed CO SLEDs considerably changes across 30 Doradus. For example, the peak transition Jp varies from J = 6–5 to J = 10–9, while the slope characterized by the high-to-intermediate J ratio α ranges from ~0.4 to ~1.8. To examine the source(s) of these variations in CO transitions, we analyzed the CO observations, along with [C II] 158 μm, [C I] 370 μm, [O I] 145 μm, H2 0–0 S(3), and FIR luminosity data, using state-of-the-art models of photodissociation regions and shocks. Our detailed modeling showed that the observed CO emission likely originates from highly compressed (thermal pressure P∕kB ~ 107–109 K cm−3) clumps on ~0.7–2 pc scales, which could be produced by either ultraviolet (UV) photons (UV radiation field GUV ~ 103–105 Mathis fields) or low-velocity C-type shocks (pre-shock medium density npre ~ 104–106 cm−3 and shock velocity vs ~ 5–10 km s−1). Considering the stellar content in 30 Doradus, however, we tentatively excluded the stellar origin of CO excitation and concluded that low-velocity shocks driven by kiloparsec-scale processes (e.g., interaction between the Milky Way and the Magellanic Clouds) are likely the dominant source of heating for CO. The shocked CO-bright medium was then found to be warm (temperature T ~ 100–500 K) and surrounded by a UV-regulated low-pressure component (P∕kB ~ a few (104 –105) K cm−3) that is bright in [C II] 158 μm, [C I] 370 μm, [O I] 145 μm, and FIR dust continuum emission.

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