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PI Total time #CoIs, team

Star cluster complexes. Young star clusters clustered themselves in regions. There interactions, mergers and disruptions may occur. Here we propose to measure the kinematics of these regions. PI Total time #CoIs, team. M. Mora 4.0n (ELT 42m)

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PI Total time #CoIs, team

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  1. Star cluster complexes. Young star clusters clustered themselves in regions. There interactions, mergers and disruptions may occur. Here we propose to measure the kinematics of these regions. • PI • Total time • #CoIs, team M. Mora 4.0n (ELT 42m) Experts in 3D spectroscopy, theoretician involved in star cluster disruption and interaction simulations, star cluster experts and PhD students .

  2. Star cluster complexes • -Important stage in the star clusters life. • -Stars may be released from their clusters becoming field stars. • -Some star clusters may be interacting and eventually will merge. • We aim to study : • -Kinematic of the clusters, stars and the surrounding media: Chaotic? Small group interactions? How much the media affects to the clusters? • Is the velocity field of the gas coupled/de-coupled with the clusters ? • -Important information about the process of cluster disruptions • -Input for simulations.

  3. Telescope Setup : Extrapolation of VLT VIMOS 0.67” fiber of 54”x54” Young star cluster region in NGC 45 0.01” pix scale (simulated from ACS ) IFU FOV with fibre size of 0.37” 30”x30” FOV Opportunity to observe star and cluster interactions!!!

  4. ELT Justification: Only instrument available to reach objects of V=24 with s/n=30 using 3D spectroscopy. (Extrapolating VIMOS efficiency) Legacy Value: Metallicity estimation of the clusters and the media. Ages and masses in combination with models can be also derived. Data Reduction: 3D data skills. Run MP Mode AO T. FOV Pixel  Notes A IFU R=1000 LTAO 40h 30” 10 510 nm 10h x 4 (IFU) Run Target R.A. Dec. ToT Mag Notes A NGC 45 0h -23˚ 40h V=24 S/N ~30

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