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SUMMARY:Spatio- temporal formation history and kinematics of star clusters
  in the Magellanic Clouds: Propagation of cluster formation and the LMC ba
 r
DTSTART;VALUE=DATE-TIME:20230322T145900Z
DTEND;VALUE=DATE-TIME:20230322T150100Z
DTSTAMP;VALUE=DATE-TIME:20240704T115745Z
UID:indico-contribution-276@meetings.aip.de
DESCRIPTION:Speakers: Dhanush Sathiavals Reselammal (Senior Research fello
 w\, IIA)\nThe Large Magellanic cloud(LMC) and Small Magellanic cloud(SMC) 
 are the nearest interacting dwarf galaxies in the local group.  And Magell
 anic clouds(MCs) have had interactions with each other as well as with the
  Milky Way. These interactions have triggered star formation in both galax
 ies\, resulting in the formation of star clusters. Thus a comprehensive an
 alysis of cluster population in MCs could indicate the structural evolutio
 n due to galaxy mergers. Our aim is to understand the age dating\, spatio-
 temporal map of cluster formation episodes\, and trace the cluster kinemat
 ics as a function of age.\nIn this study\, we used the GAIA DR3 data to ch
 aracterise the cluster population in the MCs. The clusters in the MCs is o
 btained mostly from general catalogue given by Bica et al. (2020)\, and se
 veral other recent literature. We classified the clusters as isolated and 
 merged based on projected sky coordinates. Around 2000 clusters were analy
 zed in our study based on a certain selection criteria. We used Gaia async
 hronous query to bulk handle the cluster data from Gaia archive\, after ap
 plying proper motion-parallax cut offs and faintness magnitude limit. We d
 eveloped a statistical algorithm to remove filed stars from the cluster re
 gion. We used single to multiple comparison field regions and retrieved th
 e most probable cluster members.  Using Padova-Parsec stellar evolutionary
  models\, we performed an iterative least square method to estimate the ag
 e and reddening of clusters that had sufficient members and a satisfactory
  fit of the isochrone. The spatio-temporal map of age and reddening was ob
 tained for clusters in both clouds. We traced the cluster formation episod
 es at ~ 1.6 Gyr\, 630 Myr\, 310 Myr\, and 80 Myr. The directional propagat
 ion of cluster formation is noted from the South to North of LMC over the 
 time scale of 2.8 Gyr to 10 Myr.  We are able to estimate the formation ti
 me of the LMC’s off-centered bar.  Using the proper motion data of the m
 embers we also study the proper motion of the clusters with respect to the
  field population in both the Clouds.\n\nhttps://meetings.aip.de/event/20/
 contributions/276/
LOCATION:Haus H\, Telegrafenberg
URL:https://meetings.aip.de/event/20/contributions/276/
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