scholarly journals Star formation history and X-ray binary populations: the case of the Large Magellanic Cloud

2016 ◽  
Vol 459 (1) ◽  
pp. 528-553 ◽  
Author(s):  
V. Antoniou ◽  
A. Zezas
Keyword(s):  
Star Formation ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Formation History ◽  
X Ray ◽  
Formation History

The Star-Formation History in the Vicinity of NGC 1866 in the Large Magellanic Cloud

1997 ◽  
Vol 109 ◽  
pp. 292 ◽  
Author(s):  
B. W. Stappers ◽  
J. R. Mould ◽  
K. M. Sebo ◽  
J. A. Holtzman ◽  
J. S., III Gallagher ◽  
...  
Keyword(s):  
Star Formation ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Formation History ◽  
Formation History

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 Constraints on the star formation history of the Large Magellanic Cloud

2005 ◽  
Vol 431 (1) ◽  
pp. 73-85 ◽  
Author(s):  
S. C. Javiel ◽  
B. X. Santiago ◽  
L. O. Kerber
Keyword(s):  
Star Formation ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Formation History ◽  
Formation History ◽  
History Of

scholarly journals The star formation history of the Large Magellanic Cloud star cluster NGC 1751★

2011 ◽  
Vol 414 (3) ◽  
pp. 2204-2214 ◽  
Author(s):  
Stefano Rubele ◽  
Léo Girardi ◽  
Vera Kozhurina-Platais ◽  
Paul Goudfrooij ◽  
Leandro Kerber
Keyword(s):  
Star Formation ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Cluster ◽  
Star Formation History ◽  
Formation History ◽  
History Of

scholarly journals Observations and Implications of the Star Formation History of the Large Magellanic Cloud

1999 ◽  
Vol 118 (5) ◽  
pp. 2262-2279 ◽  
Author(s):  
Jon A. Holtzman ◽  
John S. Gallagher III ◽  
Andrew A. Cole ◽  
Jeremy R. Mould ◽  
Carl J. Grillmair ◽  
...  
Keyword(s):  
Star Formation ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Formation History ◽  
Formation History ◽  
History Of

scholarly journals The Formation of Constellation III in the Large Magellanic Cloud

2008 ◽  
Vol 25 (3) ◽  
pp. 116-120 ◽  
Author(s):  
Jason Harris ◽  
Dennis Zaritsky
Keyword(s):  
Star Formation ◽  
Large Scale ◽  
Wave Model ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Formation History ◽  
Formation Model ◽  
Physical Conditions ◽  
Formation History ◽  
History Of

AbstractWe present a detailed reconstruction of the star-formation history of the Constellation III region in the Large Magellanic Cloud, to constrain the formation mechanism of this enigmatic feature. Star formation in Constellation III seems to have taken place during two distinct epochs: there is the 8–15 Myr epoch that had previously been recognized, but we also see strong evidence for a separate ‘burst’ of star formation 25–30 Myr ago. The ‘super-supernova' or GRB blast wave model for the formation of Constellation III is difficult to reconcile with such an extended, two-epoch star formation history, because the shock wave should have induced star formation throughout the structure simultaneously, and any unconsumed gas would quickly be dissipated, leaving nothing from which to form a subsequent burst of activity. We propose a ‘truly stochastic’ self-propagating star formation model, distinct from the canonical model in which star formation proceeds in a radially directed wave from the center of Constellation III to its perimeter. As others have noted, and we now confirm, the bulk age gradients demanded by such a model are simply not present in Constellation III. In our scenario, the prestellar gas is somehow pushed into these large-scale arc structures, without simultaneously triggering immediate and violent star formation throughout the structure. Rather, star formation proceeds in the arc according to the local physical conditions of the gas. Self-propagating star formation is certainly possible, but in a truly stochastic manner, without a directed, large scale pattern.

scholarly journals THE STAR FORMATION HISTORY OF THE LARGE MAGELLANIC CLOUD

2009 ◽  
Vol 138 (5) ◽  
pp. 1243-1260 ◽  
Author(s):  
Jason Harris ◽  
Dennis Zaritsky
Keyword(s):  
Star Formation ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Formation History ◽  
Formation History ◽  
History Of

scholarly journals High-mass X-ray binaries and recent star formation history of the Small Magellanic Cloud

2007 ◽  
Vol 33 (7) ◽  
pp. 437-454 ◽  
Author(s):  
P. E. Shtykovskiy ◽  
M. R. Gilfanov
Keyword(s):  
Star Formation ◽  
Magellanic Cloud ◽  
Star Formation History ◽  
High Mass ◽  
Small Magellanic Cloud ◽  
X Ray ◽  
Formation History ◽  
History Of ◽  
X Ray Binaries

scholarly journals The star formation history of the Large Magellanic Cloud star clusters NGC 1846 and NGC 1783★

2013 ◽  
Vol 430 (4) ◽  
pp. 2774-2788 ◽  
Author(s):  
Stefano Rubele ◽  
Léo Girardi ◽  
Vera Kozhurina-Platais ◽  
Leandro Kerber ◽  
Paul Goudfrooij ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Clusters ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Formation History ◽  
Formation History ◽  
History Of
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