Download - Arjen van der Wel -- MPIA, Heidelberg
Arjen van der Wel -- MPIA, Heidelberg
THE PATH FROM COMPACT Z = 2 GALAXYTO GIANT ELLIPTICAL
with the 3D-HST and CANDELS teams
Arjen van der Wel -- MPIA, Heidelberg
THE PATH FROM COMPACT Z = 2 GALAXYTO GIANT ELLIPTICAL
The size-mass relationfrom CANDELS & 3D-HST
with the 3D-HST and CANDELS teams
Arjen van der Wel -- MPIA, Heidelberg
THE PATH FROM COMPACT Z = 2 GALAXYTO GIANT ELLIPTICAL
with the 3D-HST and CANDELS teams
Why spend >800 orbitson blank pieces of sky?
5 kpc NGC 300 M871 kpc
gradual gas accretion/coolingstar formation
early, rapid dissipationmerging
Disks Spheroids
Global structure encodes formation/assembly history
ESO / La Silla ESA / Hubble
CANDELS• Multi-Cycle Legacy Program -- 902 orbits• PIs: Sandy Faber (UCSC) & Harry Ferguson (STScI)• NUV -- NIR imaging over 788 sq. arcmin. / 5 fields
3D-HST• Treasury Program -- 245 orbits• PI: Pieter van Dokkum (Yale)• optical/NIR grism spectroscopy of 4 CANDELS fields
Grogin et al. (2011); Koekemoer et al. (2011)Brammer et al. (2012)
CANDELS & 3D-HST
Arjen van der Wel -- MPIA
CANDELS• Multi-Cycle Legacy Program -- 902 orbits• PIs: Sandy Faber (UCSC) & Harry Ferguson (STScI)• NUV -- NIR imaging over 788 sq. arcmin. / 5 fields
3D-HST• Treasury Program -- 245 orbits• PI: Pieter van Dokkum (Yale)• optical/NIR grism spectroscopy of 4 CANDELS fields
Grogin et al. (2011); Koekemoer et al. (2011)Brammer et al. (2012)
For this talk• ~40,000 galaxies at 0 < z < 3• with redshifts, stellar masses, colors• robustly measured half-light radii
CANDELS & 3D-HST
Arjen van der Wel -- MPIA
CANDELS• Multi-Cycle Legacy Program -- 902 orbits• PIs: Sandy Faber (UCSC) & Harry Ferguson (STScI)• NUV -- NIR imaging over 788 sq. arcmin. / 5 fields
3D-HST• Treasury Program -- 245 orbits• PI: Pieter van Dokkum (Yale)• optical/NIR grism spectroscopy of 4 CANDELS fields
Grogin et al. (2011); Koekemoer et al. (2011)Brammer et al. (2012)
For this talk• ~40,000 galaxies at 0 < z < 3• with redshifts, stellar masses, colors• robustly measured half-light radii
CANDELS & 3D-HST
Arjen van der Wel -- MPIA
Photometry (+redshifts, masses, etc)Skelton et al. 2014, arXiv:1403.3689
Sizes (+ Sersic n, axis ratios, etc.)van der Wel et al. 2012, ApJS, 203, 14
Sersic index = 5.9 Residual = 11%Elliptical
Spiral Sersic index = 1.4 Residual = 21%
How are sizes measured?
Sersic profile:
GALFIT (Peng+10)
Sersic index = 5.9 Residual = 11%Elliptical
Spiral Sersic index = 1.4 Residual = 21%
How are sizes measured?
Sersic profile:
GALFIT (Peng+10)
Color-color separation into two types (e.g., Wuyts+07)
Arjen van der Wel -- MPIA
Color-color separation into two types (e.g., Wuyts+07)
Arjen van der Wel -- MPIA
Sersic n > 2.5
Sersic n < 2.5
Color-color separation into two types (e.g., Wuyts+07)
Arjen van der Wel -- MPIA
Evolution of the size-mass distribution
Arjen van der Wel -- MPIA
Evolution of the size-mass distribution
Arjen van der Wel -- MPIA
Evolution of the size-mass distribution
Arjen van der Wel -- MPIA
Evolution of the size-mass distribution
Arjen van der Wel -- MPIA
1.2 < z < 2 (Cimatti+08) 2 < z < 2.5 (van Dokkum+08)
Evolution of the size-mass distribution
Arjen van der Wel -- MPIA
Co-moving number density evolution
Muzzin+13
All Early Types
Co-moving number density evolution
Muzzin+13
All Early Types Compact Early Types
Co-moving number density evolution
Muzzin+13
All Early Types Compact Early Types
Co-moving number density evolution
Muzzin+13
All Early Types Compact Early Types
Increasing number density of early-type galaxiesfrom z ~ 3 to the present
Decreasing number density of small early-type galaxies from z ~ 1-1.5 to the present
also see Cassata+11, Newman+12, Szomoru+12, Cassata+13but cf. Carollo+13; Poggianti+13
Combined mass and size growth
Combined mass and size growth
Growth in mass by a factor 2-3:Number density matching (e.g., Lundgren+14)
Abundance matching (e.g., Moster+13)
Combined mass and size growth
Growth in mass by a factor 2-3:Number density matching (e.g., Lundgren+14)
Abundance matching (e.g., Moster+13)
Combined mass and size growth
Growth in mass by a factor 2-3:Number density matching (e.g., Lundgren+14)
Abundance matching (e.g., Moster+13)
van der Wel+11 (based on WFC3 Early Release Science data (PI: Windhorst)
Disk-like quiescent galaxies at z ~ 2
Yu-Yen Chang, van der Wel+13ab (CANDELS):majority of z~2 quiescent galaxies are oblate
with an intrinsic axis ratio of c/a ~ 0.3
Present-day descendants
proj
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d ax
is ra
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10,000 SDSS Early Types at z < 0.1
van der Wel+09
• CANDELS & 3D-HST have provided an enormous increase in sample size and dynamic range in the empirical description of the size-mass distribution (van der Wel+14).
• First constraints on the (non-)evolution of scatter and slope.
• Increasingly clear path from compact, disk-like quiescent galaxy to massive elliptical.
Summary
Arjen van der Wel -- MPIA