Local Group cosmology with ngcfht

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1 Local Group cosmology with ngcfht Nicolas Martin (Strasbourg Observatory & MPIA, Heidelberg)

2 Cosmology on galaxy scales the new frontier observed halo kpc Large scale cosmology is now largely understood Λ Cold Dark Matter universe How do baryons condense at the center of dark matter halos? hierarchical build-up (stars, globular clusters, gas ) Cooper et al. (2009)

3 Cosmology on galaxy scales the new frontier observed halo kpc Large scale cosmology is now largely understood Λ Cold Dark Matter universe How do baryons condense at the center of dark matter halos? hierarchical build-up (stars, globular clusters, gas ) Cooper et al. (2009)

4 Cosmology on galaxy scales the new frontier observed halo kpc Large scale cosmology is now largely understood Λ Cold Dark Matter universe How do baryons condense at the center of dark matter halos? hierarchical build-up (stars, globular clusters, gas ) Cooper et al. (2009)

5 Where the Local Group comes into play SDSS ( ) Pan-STARRS ( ) 800 kpc MW plane PAndAS ( )

6 PAndAS The Pan-Andromeda Archaeological Survey ( ) Building on pilot M31 CFHT surveys (Ibata, Martin et al. 2007, McConnachie et al. 2008) CFHT large program 220 hours over 3 years 3.6m telescope on Mauna Kea MegaCam/MegaPrime 1 deg 2 field of view 2 bands (g & i) All ~400 deg 2 now observed

7 PAndAS The Pan-Andromeda Archaeological Survey ( ) Building on pilot M31 CFHT surveys (Ibata, Martin et al. 2007, McConnachie et al. 2008) CFHT large program 220 hours over 3 years 3.6m telescope on Mauna Kea MegaCam/MegaPrime 1 deg 2 field of view 2 bands (g & i) All ~400 deg 2 now observed

8 PAndAS data Observing 3 mag. below the tip of RGB seeing ~20 min integration in g & i S/N=10 depths g 25.5 i million sources ~10 million stars in M31 RGB selection box Galactic halo Galactic disk

9 PAndAS 150 kpc McConnachie et al. (2009), Ibata et al. (2013), Martin et al. (2013) 50 kpc

10 PAndAS 150 kpc McConnachie et al. (2009), Ibata et al. (2013), Martin et al. (2013) kpc 50 kpc Cooper et al. (2010)

11 Different causes produce different halos µ (mag/arcsec 2 ) [Fe/H] Johnston et al. (2008) Highest luminosity accretion events

12 Different causes produce different halos µ (mag/arcsec 2 ) [Fe/H] Johnston et al. (2008) Highest luminosity accretion events Lowest luminosity accretion events

13 Different causes produce different halos Johnston et al. (2008) µ (mag/arcsec 2 ) [Fe/H] [α/fe] vr (km/s) σ (km/s) Highest luminosity accretion events Lowest luminosity accretion events

14 150 kpc 50 kpc

15 150 kpc 50 kpc ~250 ngcfht fields

16 A complete survey of M31 s surroundings?

17 A complete survey of M31 s surroundings?

18 A complete survey of M31 s surroundings?

19 What could ngcfht do in 1h? Martin et al. (2007) DEIMOS Medium resolution 1h exposure Calcium triplet velocities Å

20 Interesting targets DEIMOS 1n observing 2-3 km/s Dwarf galaxies 1s 100s of stars σvr 3 10 km/s 5 15 km/s Metallicities Stacked [α/fe]

21 Needs Medium resolution imperative Table 10: Signal-to-Noise Ratios and Velocity Accuracies for M31/M33 Surveys g R = R = R = R = (S/N, v) (S/N, v) (S/N, v) (S/N, v) 22.5 (19, 10) (12, 7) (10, 6) (8.5, 5) 23.0 (12, 17) (8, 11) (7, 9) (5, 8) 23.5 (8, 25) (5, 17) (4, 15) (3.5, 11) 24.0 (5.5, 36) (3, 29) (2.8, 21) (2.1, 19) 24.5 (3, 67) (2, 43) (1.8, 33) (1.3, 31)

22 Needs Medium resolution imperative Large field of view (>deg 2 ) Chapman et al. (2007)

23 Needs Medium resolution imperative Large field of view (>deg 2 ) Heavy multiplexing Martin et al. (2013)

24 M31 µ (mag/arcsec2) [Fe/H] [α/fe] vr (km/s) σ (km/s)

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