Deep Multi-Color Imaging in 47 Tuc: Some Early Results 2MASS ALL SKY IMAGE Disk Bulge Magellanic Clouds 47 Tuc Halo H. Richer (UBC)

Hubble’s 25th Anniversary!! Cycle 1

Deep Multi-Color Imaging in 47 Tuc: Some Early Results 2MASS ALL SKY IMAGE Disk Bulge Magellanic Clouds 47 Tuc Halo H. Richer (UBC)

CollaboratorsCollaborators l R. Goldsbury, H. Richer, K. Woodley - UBC l J. Anderson, J. Kalirai - STScI l B. Hansen, D. Reitzel, M. Rich - UCLA l A. Dotter - UVic l G. Fahlman, P. Stetson - HIA/NRC l J. Hurley - Swinburne l I. King - UW l M. Shara - AMNH

WD Cooling Model and N6397 Model from Bergeron (2008) Note: Excellent fit through most cooling region At bright end real WDs too red or too bright - radii too large or minor colour transformation problems? At faint end real stars turn blue (CIA) faster than models See poster by Rich et al.

Model Fit to Data Model Fit to Data l Age = /-0.35 Gyr l Includes opacity from red wing L  (Kowalski 2006) l Systematic errors from different models not included Hansen et al 2007 Comparison N6397 and M4 Luminosity Functions

Galactic Disk is Younger than Halo Galactic Disk is Younger than Halo lDots = disk lLine = M4 (halo) lM4 LF fainter WDs lM4 older than disk lDisk age 7.5±1.0 Gyr

47 Tuc - an Important Template 47 Tuc - an Important Template Brown et al Disk/Bulge TemplateTemplate RGBs Nearby Galaxies Harris 2010

GO on 47 Tuc (Cycle 17) Orbits 121 Field 6’ west of centre ACS F606W F814W Archival F475W F775W F850L WFC3 UVIS: F390W F606W IR: F160W F110W Science Age, binary, variables, planets, H-burning limit, brown dwarfs, motion & MF SMC

ACS Images ACS Images Full Field Center Edge

ACS CMD WD Cooling Simulations ACS CMD WD Cooling Simulations

WFC3 Images 47 Tuc F110W F160W

47 Tuc Near IR CMD 47 Tuc Near IR CMD TO Kink (CIA) Width (real) SMC TO Kink Width - Real SMC

47 Tuc Near IR CMD - Ages 47 Tuc Near IR CMD - Ages Age 2 ways Turnoff 11 Gyrs  mag or  color (Kink-TO) Gyrs Models by A. Dotter

47 Tuc Near IR CMD 47 Tuc Near IR CMD Width Lower MS - real, easy to quantify as MS vertical · Models indicate light element variations (mainly O) ·  He can’t explain at fixed [Fe/H]

Cosmology and WD Cooling Ages Cosmology and WD Cooling Ages WMAP Model z vs age z and Cosmic Star Formation Disk 47 Tuc--> N6397/M4 SFR (M  yr -1 Mpc -3 ) Z Z T (Gyr) Disk N6397/M Tuc --> Spergel et al Thompson et al. 2006

Photometric Errors on the Lower Main Sequence