the effect of crowding on the gsmt stellar populations science case knut olsen, bob blum (noao),...
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The Effect of Crowding on the GSMT Stellar Populations
Science Case
Knut Olsen, Bob Blum (NOAO), François Rigaut (Gemini)
GSMT SWG Presentation
Hilo 2002
MotivationStudying galaxy formation through the star and chemical enrichment histories of galaxies requires precise photometry
What sources contribute to random photometric error?•Photon statistics•Errors in PSF fitting•Crowding•The pitfalls of photometry with AO systems
Modeling crowding effects
V I
Crowding introduces photometric error through luminosity fluctuations within a single resolution element of the telescope due to the unresolved stellar sources in that element.
To calculate the effects of crowding on magnitudes and colors, we need only consider the Poisson statistics of the luminosity functions (e.g. Tonry & Schneider 1988)
Issues:•characterizing resolution•luminosity range over which fluctuations are important
For magnitudes:
For colors:
Simulations
Overview:
•3 simulations of LMC globular cluster NGC 1835, at seeing-limited, HST, and GSMT resolution
•3 simulations of the center of M32, at resolution ofGemini+Hokupa’a, 8-m NGST, and GSMT
•GSMT simulations of the Arches cluster and the bulge of M33
Artificial stellar populations and artificial star tests
The Center of M32
Davidge et al. (2000)
~0.”12 FWHM H&K
Gemini N + Hokupa’a
Krist (1999) 8-m NGST PSF
0.”032 J, 0.”057 K FWHM 0.”035 pixels
30” 20” 20”
M32 Population: 10% 1 Gyr ([Fe/H]=0), 45% 5 Gyr ([Fe/H]=0), 45% 10 Gyr ([Fe/H]=-0.3); cent = 10.1 mag arcsec-2
F. Rigaut GSMT PSF
0.”009 J, 0.”015 K FWHM 0.”005 pixels
Gemini+Hokupa’a•Photometry with DAOPHOT/ALLSTAR
•Calibrated with Davidge et al. (2000) photometry
•14500 artificial stars added, PSF rederived and photometry repeated
•CMD and errors shown for 7.”4 < r < 13.”1 annulus centered on M32
•Crowding limit H,K~16.5
Crowding model
DAOPHOT
NGST•Artificial population
•Photometry with DAOPHOT/ALLSTAR
•Zero points adjusted to fit input magnitudes
•CMD and errors shown for 7.”4 < r < 13.”1 annulus centered on M32
•Crowding limit J~20.5,K~19.5
DAOPHOT
0.”07 J, 0.”057 K
0.”035 J, 0.”057 K
GSMT•Artificial population
•Photometry with DAOPHOT/ALLSTAR
•Zero points adjusted to fit input magnitudes
•CMD and errors shown for 7.”4 < r < 13.”1 annulus centered on M32
•Crowding limit J~23.5, K~22
DAOPHOT
0.”005 J, 0.”005 K
0.”009J, 0.”015 K
Beyond M32
Girardi et al. (2000) tracks
0.1,1,2,5,8,10,14 Gyr
[Fe/H]=-1.0, 0.0
K=19, V=22 mag arcsec-2
30-m + J,K100-m + J,K100-m + V,I
Crowding error also measures completeness
Conclusions
•Crowding is likely the limiting factor for the stellar populations science
•Analytical predictions are adequate for evaluating effects of crowding, but full understanding of photometry requires simulations
•Realistic GSMT simulations need, at the very least, to include the effect of stars placed at sub-pixel positions
•GSMT provides giant leap for stellar populations mainly through its resolution; how large does the Strehl need to be?