1. Looking forward to new telescopes and back to the dark ages
Jeremy Mould
NOAO

2. Outline The star formation history of the Universe “First light”
NGST
ALMA
GSMT
“First light”
after recombination and
before reionization
Source counts with GSMT

3. The star formation history
Three very complementary views:
Ha to redshift 10 with NGST
encumbered by dust
the FIR calorimeter and CO with ALMA
the fossil record with GSMT
count the low mass stars and infer the rest
encumbered by the IMF

4. Redshifted emission linesZ
[OII]
[OIII] Ha
Lya .5
5590A
1.0m 1
1.3m 2
1.5m 3
2.0m
4860A 5
2.23m 9
1.2m

5. SFH in local group galaxies
Just count the stars at the base of the red giant branch => SFR(t)

6. Stellar populations with ELTs
Basic assumption: IMF is robust
verified by HST studies of local dwarfs
maybe inapplicable to Pop.III
In all Local Group galaxies, full Star Formation History is on display
CMDs show number of stars formed each Gyr in the Hertsprung gap
just count the stars as they cross !

7. First light scenarios We have no real idea what first light was like
So, compare with things we do know
Globular clusters 10 pc = 1.5 mas
Starbursts 100 pc = 15 mas
Dwarf galaxies 1 kpc = 0.15 arcsec
assuming DA = 0.3 Hubble radius at 3 < z < 10
noting l/d = 10 mas at 1.5m for d = 30m GSMT

8. First light in the Universe
Assembly of galaxies
A diffraction limited GSMT will complement ALMA and NGST in resolution
First light in the Universe
What reionized the Universe ?
the first QSOs, formation and growth
supernovae in the first globular clusters

9. SNe in the 1st globular clusters
106 Mo star cluster => 104 SNe in 108 yrs
SN 1987A models yield 1051 ergs (only 1048 in photons)
100 such star clusters yield enough energy to ionize 4 x 1010 Mo hydrogen
t = 108 yrs in matter dominated Universe is
z = 20

10. Sensitivity GSMT 1m NGST 10m ALMA 1mm Young Globulars 108 Lo
J = 31 at z = 3
109 Lo
e.g. N5253
Starbursts
Dusty ?
1010 Lo
2mJy at z = 3
4mJy at z = 10
Dwarfs
SBF
P(D)

11. Source Counts Deeper counts will constrain 1 galaxy/arcsec =
107 gal deg-2
Deeper counts will constrain
[cosmology]
SFH / evolution
assembly

12. AGN counts Evolution of QSO luminosity and density Sloan survey coming
2dF survey
=>

13. Counts of star forming galaxies
Counts of absorbers
Clearly a constraint on reionization
Counts of star forming galaxies
SIRTF will be an interesting preview, but very confusion limited

14. CIB
DIRBE/
IRAS
data

15. IRAS / MIPS galaxy counts

16. ISO counts

17. MIPS simulation

18. White dwarf counts and dark matter
Early IMF rich in intermediate mass stars
dark halo with 10-3 Mo/pc3 in white dwarfs
carbon rich ISM
White dwarfs with MJ = 15, J = 30
r -3 density law
104 WDs deg-2 /mag

19. ALMA/GSMT synergies In galaxy formation science, GSMT offers
Resolution
Redshifts
Inventory of the parts for galaxy assembly
which parts ?
stars
giant HII regions
warm ISM