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DES.Dark Energy Survey Collaboration Meeting Madrid, May 2010 MILKY-WAY Working Group | Planning for DC6

Summary of the DES Dark Energy Survey Collaboration Meeting in May 2010, discussions on Milky Way working group activities, adding globular clusters and tidal tails, simulating star clusters, and modeling other stellar populations.

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DES.Dark Energy Survey Collaboration Meeting Madrid, May 2010 MILKY-WAY Working Group | Planning for DC6

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  1. DES stars: DC5 results and planing for DC6 Dark Energy Survey Collaboration MeetingMadrid – May 2010 Milky-Way Working Group DES-Brazil

  2. DC5 stellar sample • DES MWWG provided input stellar sample • Trilegal code (Girardi et al):‏ • Thin and thick disks, bulge, halo • IMF, SFH, AMR • Padova evolutionary tracks • Proper motions

  3. Truth tables vs DC5-VAC • Analysis used Brazilian portal: star counts, colour-mag, colour-colour diagrams, photometric errors and residuals, astrometry. • Matching number of VAC stars to truth table requires class_star ≃ 0.50.

  4. Distribution of class_star All obj w/ r < 23 Ngal / Ntotal

  5. Phot. errors and residuals(all objects)‏ GSN/VAC: g errors vs true g GSN/VAC: g vs true g Brazilian Portal

  6. Colour-magnitude diagramsstars only GSN - Truth Table GSN - VAC Brazilian Portal

  7. Colour-colour diagramsstars only GSN – Truth table GSN – VAC Brazilian Portal

  8. Photometric residuals DC5: class_star > 0.50 r < 23 GSN: all objects Brazilian portal

  9. Mean residuals and sigma DC5 – class_star > 0.50

  10. Astrometry Brazilian portal GSN – all obj

  11. Proper motions  cos GSN: from Huan Lin DC5

  12. Validating PMs with UCAC close to Galactic pole Blue: Trilegal; Black: UCAC-3 from Julio Camargo

  13. Validating PMs with UCAC close to equatorial pole Blue: Trilegal; Black: UCAC-3 from Julio Camargo

  14. Planing for DC6Add globular clusters and tidal tails • AddClus • positions, masses, magnitudes, and colours • 3 isochrone sets: Padova, PEL, BaSTI • simulate both GC and tidal tails • GC: Hubble-Reynolds, modified Hubble, King profile • unresolved binaries, photometric errors • mass segregation and other dynamical effects.

  15. AddClus: adding positions Simulation of NGC 2298: m-M = 15.1, Z=5 10-4 ,  = 12.5 Gyrs N = 105 stars King profile: rc=2.5pc, rtidal=75pc fbin = 0.5

  16. Adding a tidal tail Tidal tail: from 30 to 1000pc N = 40% of GC stars PA = 45o;  = 20o

  17. CMDs

  18. Mass segregation MF slopes (): (m) ∝ m- inner: 1.3, 2.0, 1.6 mid: 2.0, 2.35, 2.35 outer:-0.2, 2.7, 2.8

  19. Detecting a GC tidal tail:matched filter • Technique to detect a low signals mixed to high background From Rockosi et al (2002)‏

  20. Validation:Pal 5 and field (SDSS)‏ Eduardo Balbinot

  21. Comparison to Rockosi et al 2002 Eduardo Balbinot Rockosi et al

  22. Modelling other Stellar Populations Extra remarks: GC tails and the Galaxy cover large solid angles, especially the latter.

  23. Outer LMC: a lot to improve • 1 sq deg • uniform SFH assumed • No depth effects yet

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