%0 Generic %1 meschin2013spatially %A Meschin, I. %A Gallart, C. %A Aparicio, A. %A Hidalgo, S. L. %A Monelli, M. %A Stetson, P. B. %A Carrera, R. %D 2013 %K lmc sfh %T Spatially resolved LMC star formation history: I. Outside in evolution of the outer LMC disk %U http://arxiv.org/abs/1312.2584 %X We study the evolution of three fields in the outer LMC disk Rgc=3.5-6.2 Kpc. Their star formation history indicates a stellar populations gradient such that younger stellar populations are more centrally concentrated. We identify two main star forming epochs, separated by a period of lower activity between ~7 and ~4 Gyr ago. Their relative importance varies from a similar amount of stars formed in the two epochs in the innermost field, to only 40% of the stars formed in the more recent epoch in the outermost field. The young star forming epoch continues to the present time in the innermost field, but lasted only till ~0.8 and 1.3 Gyr ago at Rgc=5.5 degrees and 7.1 degrees, respectively. This gradient is correlated with the measured HI column density and implies an outside-in quenching of the star formation, possibly related to a variation of the size of the HI disk. This could either result from gas depletion due to star formation or ram-pressure stripping, or from to the compression of the gas disk as ram-pressure from the Milky Way halo acted on the LMC interstellar medium. The latter two situations may have occurred when the LMC first approached the Milky Way.

@misc{meschin2013spatially, abstract = {We study the evolution of three fields in the outer LMC disk Rgc=3.5-6.2 Kpc. Their star formation history indicates a stellar populations gradient such that younger stellar populations are more centrally concentrated. We identify two main star forming epochs, separated by a period of lower activity between ~7 and ~4 Gyr ago. Their relative importance varies from a similar amount of stars formed in the two epochs in the innermost field, to only 40% of the stars formed in the more recent epoch in the outermost field. The young star forming epoch continues to the present time in the innermost field, but lasted only till ~0.8 and 1.3 Gyr ago at Rgc=5.5 degrees and 7.1 degrees, respectively. This gradient is correlated with the measured HI column density and implies an outside-in quenching of the star formation, possibly related to a variation of the size of the HI disk. This could either result from gas depletion due to star formation or ram-pressure stripping, or from to the compression of the gas disk as ram-pressure from the Milky Way halo acted on the LMC interstellar medium. The latter two situations may have occurred when the LMC first approached the Milky Way.}, added-at = {2013-12-13T08:19:47.000+0100}, author = {Meschin, I. and Gallart, C. and Aparicio, A. and Hidalgo, S. L. and Monelli, M. and Stetson, P. B. and Carrera, R.}, biburl = {https://www.bibsonomy.org/bibtex/214074ae2b46209ff392a70da2ae0c718/miki}, description = {[1312.2584] Spatially resolved LMC star formation history: I. Outside in evolution of the outer LMC disk}, interhash = {4e8352139d19af5e48b2883425a549e7}, intrahash = {14074ae2b46209ff392a70da2ae0c718}, keywords = {lmc sfh}, note = {cite arxiv:1312.2584Comment: 15 pages, 13 figures, 4 tables. MNRAS, in press}, timestamp = {2013-12-13T08:19:47.000+0100}, title = {Spatially resolved LMC star formation history: I. Outside in evolution of the outer LMC disk}, url = {http://arxiv.org/abs/1312.2584}, year = 2013 }