Deep Multi-Color Imaging in Deep Multi-Color Imaging in 47 Tuc: Some Early Results47 Tuc: Some Early Results

Deep Multi-Color Imaging in Deep Multi-Color Imaging in 47 Tuc: Some Early Results47 Tuc: Some Early Results

2MASS ALL SKY IMAGE

DiskBulge

Magellanic Clouds47 Tuc

Halo

H. Richer (UBC)H. Richer (UBC)

Hubble’s 25th Anniversary!!Hubble’s 25th Anniversary!!Hubble’s 25th Anniversary!!Hubble’s 25th Anniversary!!Cycle 1

Deep Multi-Color Imaging in Deep Multi-Color Imaging in 47 Tuc: Some Early Results47 Tuc: Some Early Results

Deep Multi-Color Imaging in Deep Multi-Color Imaging in 47 Tuc: Some Early Results47 Tuc: Some Early Results

2MASS ALL SKY IMAGE

DiskBulge

Magellanic Clouds47 Tuc

Halo

H. Richer (UBC)H. Richer (UBC)

Collaborators Collaborators Collaborators Collaborators

R. Goldsbury, H. Richer, K. Woodley - UBCR. Goldsbury, H. Richer, K. Woodley - UBC J. Anderson, J. Kalirai - STScIJ. Anderson, J. Kalirai - STScI B. Hansen, D. Reitzel, M. Rich - UCLAB. Hansen, D. Reitzel, M. Rich - UCLA A. Dotter - UVicA. Dotter - UVic G. Fahlman, P. Stetson - HIA/NRCG. Fahlman, P. Stetson - HIA/NRC J. Hurley - SwinburneJ. Hurley - Swinburne I. King - UWI. King - UW M. Shara - AMNHM. Shara - AMNH

WD Cooling Model and N6397WD Cooling Model and N6397WD Cooling Model and N6397WD Cooling Model and N6397

Model from Bergeron (2008)Model from Bergeron (2008)

Note:Excellent fit throughmost cooling region

At bright end real WDstoo red or too bright- radii too large or minorcolour transformationproblems?

At faint end real stars turn blue (CIA) faster thanmodels

See poster by Rich et al.

Model Fit to DataModel Fit to Data Model Fit to DataModel Fit to Data Age = 12.21 +/-0.35 Gyr Includes opacity from red wing L (Kowalski 2006) Systematic errors from different

models not included

Hansen et al 2007

Comparison N6397 and M4Luminosity Functions

Galactic Disk is Younger than HaloGalactic Disk is Younger than Halo Galactic Disk is Younger than HaloGalactic Disk is Younger than Halo

Dots = disk

Line = M4 (halo)

M4 LF fainter WDs

M4 older than disk

Disk age 7.5±1.0 Gyr

47 Tuc - an Important Template47 Tuc - an Important Template

47 Tuc - an Important Template47 Tuc - an Important Template

Brown et al. 2009

Disk/Bulge Template Template RGBs Nearby Galaxies

Harris 2010

GO 11677 on 47 Tuc (Cycle 17)GO 11677 on 47 Tuc (Cycle 17)GO 11677 on 47 Tuc (Cycle 17)GO 11677 on 47 Tuc (Cycle 17)Orbits 121

Field 6’ west of centre

ACS F606W F814WArchival F475W F775W F850L

WFC3UVIS: F390W F606WIR: F160W F110W

ScienceAge, binary, variables, planets, H-burninglimit, brown dwarfs,motion & MF SMC

ACS ImagesACS Images ACS ImagesACS Images

Full Field

Center

Edge

ACS CMD WD Cooling SimulationsACS CMD WD Cooling Simulations

ACS CMD WD Cooling SimulationsACS CMD WD Cooling Simulations

WFC3 Images 47 Tuc WFC3 Images 47 Tuc WFC3 Images 47 Tuc WFC3 Images 47 Tuc

F110W F160W

47 Tuc Near IR CMD47 Tuc Near IR CMD 47 Tuc Near IR CMD47 Tuc Near IR CMD

TO

Kink (CIA)

Width (real)

SMC

TO

Kink

Width - RealSMC

47 Tuc Near IR CMD - Ages47 Tuc Near IR CMD - Ages 47 Tuc Near IR CMD - Ages47 Tuc Near IR CMD - AgesAge 2 waysTurnoff11 Gyrsmag or color (Kink-TO)11-12 Gyrs

Models by A. Dotter

47 Tuc Near IR CMD47 Tuc Near IR CMD 47 Tuc Near IR CMD47 Tuc Near IR CMDWidth Lower MS - real, easy to quantify as MS vertical· Models indicate lightelement variations (mainly O)· He can’t explain at fixed [Fe/H]

Cosmology and WDCosmology and WD Cooling Ages Cooling Ages Cosmology and WDCosmology and WD Cooling Ages Cooling Ages

WMAP Model z vs age z and Cosmic Star Formation

Disk 47 Tuc-->

N6397/M4

SFR (M

yr-1 Mpc-3)

1

0.1

0.01 2 4 6Z

Z

T (Gyr)

Disk

N6397/M4

6 8 10 12 14

2

3

4

5

1

0

47 Tuc -->

Spergel et al. 2003 Thompson et al. 2006

Photometric Errors on thePhotometric Errors on theLower Main SequenceLower Main Sequence

Photometric Errors on thePhotometric Errors on theLower Main SequenceLower Main Sequence