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Spectroscopy of Resolved Stellar Populations Beyond the Local Group

Spectroscopy of Resolved Stellar Populations Beyond the Local Group. Chris Evans (UKATC) Yanbin Yang, Mathieu Puech, Matt Lehnert (GEPI); Annette Ferguson, Mike Barker (Edinburgh); Jean-Gabriel Cuby (LAM); Simon Morris (Durham) AO4ELT – Paris – June 2009. Overview.

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Spectroscopy of Resolved Stellar Populations Beyond the Local Group

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  1. Spectroscopy of Resolved Stellar Populations Beyond the Local Group Chris Evans (UKATC) Yanbin Yang, Mathieu Puech, Matt Lehnert (GEPI); Annette Ferguson, Mike Barker (Edinburgh); Jean-Gabriel Cuby (LAM); Simon Morris (Durham) AO4ELT – Paris – June 2009

  2. Overview • Resolved stellar populations in the 8-10m and ELT eras • EAGLE Phase A study • Science simulations

  3. Resolved Stellar Populations in the Local Group MW Halo M31 Belokurov et al. (2006) Dwarf Sphs (e.g. Fornax) Richardson et al. (2008) Battaglia et al. (2006)

  4. Resolved Stellar Populations in the Local Group MW Halo M31 Belokurov et al. (2006) Dwarf Sphs (e.g. Fornax) Richardson et al. (2008) Battaglia et al. (2006) Bullock, Johnston et al.

  5. Moderate-resolution spectroscopy of the Ca Triplet @860nm Spectroscopy of Resolved Stellar Populations Abundances & kinematics Tolstoy et al (2001)

  6. Moderate-resolution spectroscopy of the Ca Triplet @860nm Spectroscopy of Resolved Stellar Populations Abundances & kinematics Tolstoy et al (2001) Richardson et al. (2008)

  7. Spectroscopy of Resolved Stellar Populations Abundances & kinematics KECK-DEIMOS in M31 Chapman et al. (2006) Richardson et al. (2008)

  8. The ELT era Resolved Stellar Populations in the Local Volume ELTs will unlock a huge range of new targets, including: • NGC 3109 & Sextans A (1.3 Mpc) • Spiral-dominated Sculptor Group (2-4 Mpc) • M83/NGC5128 grouping (4-5 Mpc) • NGC3379 (11 Mpc) • Virgo Cluster galaxies (16-17 Mpc)

  9. The (near) Local Volume 1.5 3 4.5 6 Mpc Image Credit: Richard Powell

  10. The (near) Local Volume E-ELT (if in Sth. America) 1.5 3 4.5 6 Mpc TMT (if in HI) Image Credit: Richard Powell

  11. EAGLE Phase A study • A multi-IFU, near-IR spectrometer for the E-ELT • French-UK consortium • PI: Jean-Gabriel Cuby (Marseille) • 2 year study (09/07-09/09) • Phase 1 review (07/08), Midterm review (02/09)

  12. EAGLE Science Science areas that drive the EAGLE requirements: • Physics & evolution of high-z galaxies • See talk by Mathieu Puech • Detection and characterisation of “first-light” galaxies • Galaxy assembly/evolution from stellar archaeology • Star-formation, stellar clusters and the IMF • Co-ordinated growth of black holes and galaxies/AGN

  13. EAGLE Baseline Design

  14. EAGLE Baseline Design

  15. EAGLE Baseline Design

  16. EAGLE AO Multi-Object Adaptive Optics (MOAO) See talk by Gerard Rousset • CANARY: 2010-2012: • Demonstrate MOAO in EAGLE config. • Improve real-time control techniques • Develop calibration techniques See talk by Tim Morris

  17. 7.3’ FoV Selected NGS Science Simulations: MOAO performances • MOAO PSFs from Francois Assemat et al. (ONERA) • Seeing: 0.65” and 0.8” • 84x84 DM; 2 x NGS configurations

  18. Science Simulations: MOAO performances • MOAO PSFs from Francois Assemat et al. (ONERA) • Seeing: 0.65” and 0.8” • 84x84 DM; 2 x NGS configurations 42m primary 10 hr integration (20x1800s) Δλ = 8400-8750Å @ R = 10,000 37.5 mas spaxels 1x1 arcsec IFU Total th’put = 0.19 Ulisse Munari’s spectral library RON = 5e/pix, dark = 0.01e/pix/s Puech et al. (2008)

  19. Science Simulations: MOAO performances I = 23.5 S/N = 24 • MOAO PSFs from Francois Assemat et al. (ONERA) • Seeing: 0.65” and 0.8” (@ zenith, eqv. 0.71” & 0.90” @30º) • 84x84 DM; 2 x NGS configurations 42m primary 10 hr integration (20x1800s) Δλ = 8400-8750Å @ R = 10,000 37.5 mas spaxels 1x1 arcsec IFU Total th’put = 0.19 Ulisse Munari’s spectral library RON = 5e/pix, dark = 0.01e/pix/s Puech et al. (2008)

  20. EAGLE CaT performance • Seeing = 0.8”, 84x84 DM • texp = 20x1800s • R = 10,000 NGS config 10 NGS config 1 cf. E-ELT ETC: LTAO/50mas/R=10,000/I=24.5/M2V S/N=14

  21. EAGLE CaT performance Want ~15-20% EE in 75 mas at 0.85µm 4 mags deeper than FLAMES LR08 observations • Seeing = 0.8”, 84x84 DM • texp = 20x1800s • R = 10,000 NGS config 10 NGS config 1 cf. E-ELT ETC: LTAO/50mas/R=10,000/I=24.5/M2V S/N=14

  22. HST GHOSTS Survey De Jong, Radburn-Smith et al., see: www.stsci.edu/~djrs/ghosts 27 target galaxies out to ~17 Mpc 1.9 Mpc 3.6 Mpc

  23. EAGLE Observations in the Sculptor Group ACS: F814W [~3x3 arcmin] ACS image

  24. 9 arcsec ACS image ACS image

  25. 9 arcsec ACS image Simulated EAGLE cube ACS image

  26. 9 arcsec ACS image I = 22.8 S/N=28

  27. 9 arcsec ACS image I = 23.1 S/N=23

  28. 9 arcsec ACS image I = 22.5 S/N=43 & 36

  29. Formation & evolution of galaxies in the Sculptor Group 10 hrs/pointing 15 hrs/pointing x20 pointings: > 1,000 stars in ~250 hrs Image Credits: David Radburn-Smith

  30. Summary • R=10,000 CaT spectroscopy, S/N > 10 at I ~24.5 in 10 hrs • Multiple stars per IFU –> much larger effective multiplex • Large patrol field enables efficient surveys • Sculptor is just one conceivable EAGLE “Large Programme”

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