TY  - JOUR
A1  - Piatti, Andres E.
A1  - de Grijs, Richard
A1  - Ripepi, Vincenzo
A1  - Ivanov, Valentin D.
A1  - Cioni, Maria-Rosa L.
A1  - Marconi, Marcella
A1  - Rubele, Stefano
A1  - Bekki, Kenji
A1  - For, Bi-Qing
T1  - The VMC survey - XVI. Spatial variation of the cluster formation activity in the innermost regions of the Large Magellanic Cloud
JF  - Monthly notices of the Royal Astronomical Society
KW  - techniques: photometric
KW  - galaxies: individual: LMC
KW  - Magellanic Clouds
Y1  - 2015
U6  - https://doi.org/10.1093/mnras/stv2054
SN  - 0035-8711
SN  - 1365-2966
VL  - 454
IS  - 1
SP  - 839
EP  - 848
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Piatti, Andres E.
A1  - de Grijs, Richard
A1  - Rubele, Stefano
A1  - Cioni, Maria-Rosa L.
A1  - Ripepi, Vincenzo
A1  - Kerber, Leandro
T1  - The VMC survey - XV. The Small Magellanic Cloud-Bridge connection history as traced by their star cluster populations
JF  - Monthly notices of the Royal Astronomical Society
N2  - We present results based on YJK(s) photometry of star clusters located in the outermost, eastern region of the Small Magellanic Cloud (SMC). We analysed a total of 51 catalogued clusters whose colour-magnitude diagrams (CMDs), having been cleaned from field-star contamination, were used to assess the clusters' reality and estimate ages of the genuine systems. Based on CMD analysis, 15 catalogued clusters were found to be possible non-genuine aggregates. We investigated the properties of 80 per cent of the catalogued clusters in this part of the SMC by enlarging our sample with previously obtained cluster ages, adopting a homogeneous scale for all. Their spatial distribution suggests that the oldest clusters, log(t yr(-1)) >= 9.6, are in general located at greater distances to the galaxy's centre than their younger counterparts - 9.0 <= log(t yr(-1)) <= 9.4 - while two excesses of clusters are seen at log(t yr(-1)) similar to 9.2 and log(t yr(-1)) similar to 9.7. We found a trail of younger clusters which follow the wing/bridge components. This long spatial sequence does not only harbour very young clusters, log(t yr(-1)) similar to 7.3, but it also hosts some of intermediate ages, log(t yr(-1)) similar to 9.1. The derived cluster and field-star formation frequencies as a function of age are different. The most surprising feature is an observed excess of clusters with ages of log(t yr(-1)) <9.0, which could have been induced by interactions with the LMC.
KW  - techniques: photometric
KW  - galaxies: individual: SMC
KW  - Magellanic Clouds
Y1  - 2015
U6  - https://doi.org/10.1093/mnras/stv635
SN  - 0035-8711
SN  - 1365-2966
VL  - 450
IS  - 1
SP  - 552
EP  - 563
PB  - Oxford Univ. Press
CY  - Oxford
ER  -