The future with ALMA / JWST

86 Pages·2016·10.25 MB·English

by  Fabian Walter

The future with ALMA / JWST
Fabian Walter (MPIA)
theoretical framework
big bang
hydrodyn. simulations of structure formation
recombination
z~1000
0.0003 Gyr
z=100 e
z~15-1000
.
‘dark ages’ g
z=10
0.0003-0.3 Gyr .
,

S
z=1 p
r
i
n
g
e
l

e
z~8-15 t
reionization a
0.3-1 Gyr l.
ti
m
e
galaxy
z<~8
build-up >1 Gyr galaxies grow through gas accretion...
...but this gas supply and early galaxy
growth is largely unconstrained
today’s
z~0 observationally
universe 14.3 Gyr
cosmic star formation
Volume density of star formation in galaxies as f(cosmic time)
B
o
u
w
e
epoch of galaxy n
?
s
assembly
e
First galaxies
epoch of t

a
present galaxy l
.

day 2
assembly
0
1
6
present
first
day
galaxies
what causes this evolution?
outline / summary
ALMA JWST
galaxy evolution
✓ gas, star formation improve on HST
0 < z < 6
epoch of [CII], [OIII]?, dust? ✓stellar ages, SFR,
reionization (z > 6) kinematics, sizes masses
resolved imaging ✓ <0.02” (<100pc) ✓ ~0.1” (~500pc)
multi-line
✓ ✓
diagnostics
needs significant NIR: ✓
high S/N
investments MIR: more difficult
outline / summary
ALMA JWST
galaxy evolution
✓ gas, star formation improve on HST
0 < z < 6
epoch of [CII], [OIII]?, dust? ✓stellar ages, SFR,
reionization (z > 6) kinematics, sizes masses
resolved imaging ✓ <0.02” (<100pc) ✓ ~0.1” (~500pc)
multi-line
✓ ✓
diagnostics
needs significant NIR: ✓
high S/N
investments MIR: more difficult
outline / summary
ALMA JWST
galaxy evolution
✓ gas, star formation improve on HST
0 < z < 6
epoch of [CII], [OIII]?, dust? ✓stellar ages, SFR,
reionization (z > 6) kinematics, sizes masses
resolved imaging ✓ <0.02” (<100pc) ✓ ~0.1” (~500pc)
multi-line
✓ ✓
diagnostics
needs significant NIR: ✓
high S/N
investments MIR: more difficult
outline / summary
ALMA JWST
galaxy evolution
✓ gas, star formation improve on HST
0 < z < 6
epoch of [CII], [OIII]?, dust? ✓stellar ages, SFR,
reionization (z > 6) kinematics, sizes masses
resolved imaging ✓ <0.02” (<100pc) ✓ ~0.1” (~500pc)
multi-line
✓ ✓
diagnostics
needs significant NIR: ✓
high S/N
investments MIR: more difficult
outline / summary
ALMA JWST
galaxy evolution
✓ gas, star formation improve on HST
0 < z < 6
epoch of [CII], [OIII]?, dust? ✓stellar ages, SFR,
reionization (z > 6) kinematics, sizes masses
resolved imaging ✓ <0.02” (<100pc) ✓ ~0.1” (~500pc)
multi-line
✓ ✓
diagnostics
needs significant NIR: ✓
high S/N
investments MIR: more difficult
outline / summary
ALMA JWST
galaxy evolution
✓ gas, star formation improve on HST
0 < z < 6
epoch of [CII], [OIII]?, dust? ✓stellar ages, SFR,
reionization (z > 6) kinematics, sizes masses
resolved imaging ✓ <0.02” (<100pc) ✓ ~0.1” (~500pc)
multi-line
✓ ✓
diagnostics
needs significant NIR: ✓
high S/N
investments MIR: more difficult
Galaxy Spectral Energy Distribution
example SED: M82
models from Galliano et al.
HI absorption
HII absorption