1. Space motion and Stellar content of GCs with GeMS Giuliana Fiorentino University of Bologna PI: A. McConnachie, CoI: P.B. Stetson, P. Turri, D. Anderson(NRC, Canada), G. Bono (University of Rome, Tor Vergata), J.P. Veran (NRC, Canada) Date 26-06-2013, Florence GeMS4ELT

2. MAD, a successful experiment Date 09-07-2012, Leiden 2 arcmin ≤ R=13.5 mag this limits the sky coverage Pixel scale=0.028”/pixel

3. MAD in Nature: the case of Terzan 5 Date 09-07-2012, Leiden

4. d~ 6 Kpc Date 09-07-2012, Leiden Ter 5 host two different populations (confirmed by spectroscopic follow-up): 1)one old (12Gyr) and metal-poor trace the early stage of the bulge formation 2)one young (6Gyr) and metal-rich could contain important information about the metal-enrichment and the dynamical evolution. Terzan 5: a pristine fragment of the galactic bulge [Fe/H]=-0.2 [Fe/H]=+0.3 Ferraro et al. (2009, Nature)

5. Deep and accurate CMDs are a feasible but not trivial target We need to update software program that can account for a strong PSF variation when NGS do not allow a uniform correction. Normal packages do prefer to work with uniform correction even with low Strehl ratio. (updating for DAOPHOT, Stetson et al 1994, STARFINDER, Diolaiti et al. 2000). Increase the sky coverage (e.g. laser guide stars, other ideas?). Stability of the correction: reproducibility of the images to increase the S/N ratio. Conclusions from MAD

6. Overtaking MAD: GSAOI/GeMS ★ GeMS pixel scale is 0.02”/pix --> comparable to MAD, 0.028”/pix. ★ GeMS FOV=83” --> comparable to MAD, camera=60”, FOV corrected 2x2’ ★ GeMS (NGS, R≤15.5mag) has a larger SKY coverage than MAD (NGS, R≤13.5mag) Date 26-06-2013, Florence GeMS4ELT NGC1851 d~12Kpc E(B-V)~0.02 ~

7. The Project: Globular Clusters ★ PROPER MOTIONS ★ STELLAR POPULATIONS ★ GeMS characterization and comparison with MAD@VLT Date 26-06-2013, Florence GeMS4ELT

8. Date 26-06-2013, Florence Proper Motions ★ Foreground cleaning using Proper Motions of field and cluster stars. ★ Systemic Proper motions: measurements of the tangential velocity (~10 km/sec for distances ≤10 Kpc) PM~0.0002”/year over 5-10 years PM=1-2 mas ~ the accuracy on each star -> σ PM /√N thousand of stars per GGC. possibility to trace GGCs in space and in time (using cluster ages) providing a link to their birthplace, thus constraints on the formation scenario of the Galaxy. ★ Internal Proper Motions: measure of the radial velocity dispersion profile and/or detection of high velocity stars very close to the center (as in our Galactic Center). with high accuracy (σ PM ~1-2 mas) we could obtain constraints on the occurrence of IMBH (M~10 4 Mo) in the center of Globular Clusters. HST (1st epoch) -- GeMS (2nd epoch?)

9. 1) “ad hoc” for NIR-filters 2)Based on a different physics: in low mass star (≤0.4Mo), due to collision- induced absorption of hydrogen molecules J-K (mag) K (mag) NIR CMD of NGC3201 as provided by the combination of MAD (red dots) and SOFI (black dots). The blue and purple points highlight the Main Sequence Turn Off (MSTO) and the Main Sequence Knee (MSK) locations. NGC3201 MAD+SOFI data GeMS4ELT Date 26-06-2013, Florence NGC3201 as seen by MAD Stellar Populations and ages classical MSTO new MSK NGC3201 d~5Kpc E(B-V)~0.25-0.30 Independent of Reddening, differential-Reddening and Distance σ(MSK)~σ(MSTO)/2 Bono et al. 2010, ApJL

10. The First Targets Date 26-06-2013, Florence GeMS4ELT ID D(Kpc)[Fe/H] E(B-V) σv(km/s) CC AGE(Gyr) ABS_PMs(mas/year) NGC1851 12.1 -1.18 0.02 10.4±0.5 N 10.0 1.28±0.68 2.39±0.65 NGC5904(M5) 7.5 -1.29 0.03 5.5±0.4 N 10.6 5.20±1.70 14.20±1.30 NGC6652 10.0 -0.81 0.09 n.d. N 12.9 n.d. NGC6681(M70) 9.0 -1.62 0.07 5.2±0.5 Y 12.8 n.d. NGC6723 8.7 -1.10 0.05 n.d. Y 13.1 n.d. NGC7078(M15) 10.4 -2.37 0.10 13.5±0.9 Y 12.9 2.40±1.00 8.30±1.00 Large Metallicity range d≤12Kpc Low reddening Velocity Dispersion σv ≤ 13 km/s core collapse Systemic Proper motions≤15mas/year with errors ≤ 1mas/year They all have exquisite HST (WFPC2-ACS) photometry

11. (a) GeMS/GSAOI Ks image of NGC1851 (one of the four arrays) showing the high quality data obtained during the Science Verification; (b) Magnification of the region highlighted in red; (c) Same region as seen by HST/ACS in F814W filter (Sarajedini et al. 2007). The GSAOI Ks data has a very similar FWHM to the HST optical data and is very uniform across the entire field. GeMS ACS@HST GeMS4ELT Date 26-06-2013, Florence FIRST GSAOI/GeMS results NGC1851 effective pixel scale = 0.03”/pixel DL(V)=0.05” V-band DL(K)=0.07” K-band

12. GeMS4ELT Date 26-06-2013, Florence VERY PRELIMINARY CMD VERY PRELIMINARY: DAOPHOT/ALLSTAR/ALLFRAME for 1 chip (P. Turri, PhD Thesis) ISOCHRONES from Dotter et al. 2007 WEBsite Z=0.001 age=10Gyrs

13. GeMS4ELT Date 26-06-2013, Florence ACS@HST + GeMS VERY PRELIMINARY: DAOPHOT/ALLSTAR/ALLFRAME for 1 chip (P. Turri, PhD Thesis) 83” 202” 83” V~25 mag ISOCHRONES from Dotter et al. 2007 WEBsite Z=0.001 age=10Gyrs chip 1 chip 2 chip 3 chip 4

14. GeMS4ELT Date 26-06-2013, Florence ACS@HST + GeMS VERY PRELIMINARY: DAOPHOT/ALLSTAR/ALLFRAME for 1 chip (P. Turri, PhD Thesis) Ks~22 mag ISOCHRONES from Dotter et al. 2007 WEBsite Z=0.001 age=10Gyrs

15. GeMS4ELT Date 26-06-2013, Florence Luminosity Functions Texp=1920s S/N~7 K~ 22.5 mag Texp= 2720s S/N~10 J~ 22.5 mag VERY PRELIMINARY: DAOPHOT/ALLSTAR/ALLFRAME for 1 chip (P. Turri, PhD Thesis)

16. GeMS4ELT Date 26-06-2013, Florence FWHM maps J-band DL(J)~0.05”Ks-band DL(Ks)~0.07” 14 12 14 12 seeing~0.7-0.8”seeing~1.0”

17. GeMS4ELT Date 26-06-2013, Florence SR maps J-band ~10% K-band ~27% 40 35 30 25 20 15 10 5 0 12 14 12 14 12 seeing~0.7-0.8”seeing~1.0”

18. GeMS4ELT Date 26-06-2013, Florence GeMS has obtaining very interesting performances!! If the photometric (Ks~22.5 mag with S/N~7) and astrometric (≤1 mas/year) accuracies are exactly what we guess: in the near future you will read a lot about GeMS!! Conclusion s

19. Looking for the near and next future.... THANKS! Metropolitan Museum of art, NY city Date 26-06-2013, Florence