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Dark Energy Survey Collaboration Meeting Madrid – May 2010

DES stars: DC5 results and planing for DC6. Dark Energy Survey Collaboration Meeting Madrid – May 2010. Milky-Way Working Group DES-Brazil. DC5 stellar sample. DES MWWG provided input stellar sample Trilegal code (Girardi et al): ‏ Thin and thick disks, bulge, halo

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Dark Energy Survey Collaboration Meeting Madrid – May 2010

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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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