2011A&A...535A.115I


Query : 2011A&A...535A.115I

2011A&A...535A.115I - Astronomy and Astrophysics, volume 535A, 115-115 (2011/11-1)

The recent star-formation history of the Large and Small Magellanic Clouds.

INDU G. and SUBRAMANIAM A.

Abstract (from CDS):

Recent interactions between the Large and the Small Magellanic Clouds (LMC and SMC) and the Milky Way can be understood by studying their recent star formation history. This study aims to detect any directional or propagating star formation in the last 500Myr. We traced the age of the last star-formation event (LSFE) in the inner Large and Small Magellanic Cloud (L&SMC) using the photometric data in V and I passbands from the Optical Gravitational Lensing Experiment (OGLE-III) and the Magellanic Cloud Photometric Survey (MCPS). The LSFE is estimated from the main sequence turn-off point in the color-magnitude diagram (CMD) of a subregion. After correcting for extinction, the turn-off magnitude is converted to age, which represents the LSFE in a region. The spatial distribution of the age of the LSFE shows that the star-formation has shrunk to within the central regions in the last 100Myr in both the galaxies. The location as well as age of LSFE is found to correlate well with those of the star cluster in both the Clouds. The SMC map shows two separate concentrations of young star-formation, one near the center and the other near the wing. We detect peaks of star-formation at 0-10Myr and 90-100Myr in the LMC, and 0-10Myr and 50-60Myr in the SMC. The quenching of star-formation in the LMC is found to be asymmetric with respect to the optical center such that most of the young star forming regions are located to the north and east. On deprojecting the data onto the LMC plane, the recent star-formation appears to be stretched in the northeast direction and the HI gas is found to be distributed preferentially in the north. We found that the centroid is shifted to the north during the time interval 200-40Myr, whereas it is found to have shifted to the northeast in the last 40Myr. In the SMC, we detect a shift in the centroid of the population younger than 500Myr and as young as 40Myr in the direction of the LMC. We propose that the HI gas in the LMC has been pulled to the north of the LMC in the last 200Myr because of the gravitational attraction of our Galaxy at the time of perigalactic passage. The shifted HI gas was preferentially compressed in the north during the time interval 200-40Myr and in the northeast in the last 40Myr, owing to the motion of the LMC in the Galactic halo. The recent star-formation in the SMC is due to the combined gravitational effect of the LMC and the perigalactic passage.

Abstract Copyright:

Journal keyword(s): stars: formation - galaxies: kinematics and dynamics - galaxies: evolution - Magellanic Clouds - galaxies: star formation

Simbad objects: 9

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Number of rows : 9
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NAME Magellanic Stream HVC 00 32 -30.0           ~ 916 1
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10456 1
3 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6487 1
4 NAME LMC 1 Supergiant Shell sh 04 59 41 -65 44.7           ~ 36 0
5 NAME LMC 5 Supergiant Shell sh 05 22 42 -66 05.6           ~ 51 0
6 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16388 1
7 NAME LMC 4 Supergiant Shell sh 05 31 33 -66 40.5           ~ 173 0
8 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1896 1
9 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 13305 0

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2022.11.28-12:46:51

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