Downsizing & Galaxy Formation 2 nd Mitchell Symposium - April 2006 P. McCarthy OCIW Gemini Deep Deep...
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![Page 1: Downsizing & Galaxy Formation 2 nd Mitchell Symposium - April 2006 P. McCarthy OCIW Gemini Deep Deep Survey Team.](https://reader035.fdocuments.us/reader035/viewer/2022062714/56649d445503460f94a2172f/html5/thumbnails/1.jpg)
Downsizing & Galaxy Formation
2nd Mitchell Symposium - April 2006
P. McCarthyOCIW
Gemini Deep Deep Survey
Team
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How are Galaxies Formed?
Monolithic Collapse ala ELS
Hierarchical Assembly
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The Hierarchical Merger Tree
-------------
-----------------
--------------- Z = 1
Z = 0
Z = 3
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Two Kinds of Galaxies
Kauffmann et al 2003
Light-Active
-------------------------------Massive-Passive
3 x 1010Msun
Blu
e
Red
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Star Formation History
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Mass Assembly History
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Gemini Deep Deep Survey
GMOS spectrographGemini
GMOSLRISLDSS1
30 hour exposures - 300+ redshifts
I (Vega) ~ 24.5 1 < z < 2
Abraham, Glazebrook, PMcC, et al.
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Stellar Mass Determinations
100,000 Model Spectral Energy Distributions
f(Age, SF history,abundance, reddening)
Observed Spectral Energy Distributions, Redshifts
Best-fit Template, range of templates
Best-fit M/L, range
Mstar, range
MK
+
2
X
=
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The Most Massive Galaxies
Glazebrook et al.
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Mass Downsizing
L. Cowie 1996
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Three Views of Downsizing
• Stellar Mass Density Evolution
• Star Formation Histories by Mass
• Early Assembly of Massive Galaxies
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Stellar Mass Density
Cosmic Stellar mass density has not evolved at the high-mass end since z ~ 2
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The Evolving Stellar Mass Density
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New, improved semi-analytic models
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Star Formation Histories by Mass
Massive Galaxies ceased star formation at z > 2, low mass galaxies continued active star formation to late epochs
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Star Formation HistoriesJu
neau
et a
l.
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Mass Downsizing
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Post Starburst Galaxies
Only 1 in
10,000 galaxies in LCRS
have similar EWs
50% Post-Star Burst
@ z ~ 1.5
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Early Assembly of Massive Galaxies
10% of today’s stellar mass was assembled into
massive galaxies at z > 3,
and 5% before z ~ 4.
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The Most Massive Galaxies
~ 20% z = 0
mass density
Glazebrook et al.
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Spectral Types at z > 1.3
Star Forming
Pure Passive
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Old Galaxies at 1.3 < z < 1.8
<z>=1.3
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Old Galaxies at 1.3 < z < 1.8
<z>=1.3
<z>=1.8
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Old Galaxies at 1.3 < z < 1.8
<z>=1.3
<z>=1.8
<z>=0.3
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Old Galaxies at 1.3 < z < 1.8
<z>=1.3
<z>=1.8
2GyrPegase Model
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Old Galaxies at 1.3 < z < 1.8Age Fitting of 20
individual Galaxies
1.3 < z < 2.0
<zf> ~ 2.5
[Fe/H] > 0
E(B-V) ~ 1
<zf> ~ 4
[Fe/H] = 0
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Star Forming Galaxies 1.3 < z < 2.0
ACS F814W
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Pure Passive Systems
ACS F814W
NICMOS F160W
75-80%
Spheroids
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Surface Brightness Profiles
Z = 1.32
Z = 1.84
0.3 < Re< 1
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Size Distribution
Little or no evolution in the size
distribution
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Kormendy Relation at 1.3 < z < 2
Rest Frame
V-Band
Kormendy Diagram
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Kormendy Relation at 1.3 < z < 2
Passive Evolution
~1 mag per unit redshift
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“Old” Galaxies at z ~ 6
~ 1/2 M* @ z ~ 10!
Eyles et al. 2005
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Mobasher et al. 2005
10 M*!
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Basics ``Up-SizingGiant Magellan Telescope
24m Aperture
18 x 18 VMOS
7 x 7 NIRMOS
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Conclusions
• Galaxy Formation Proceeds from high to low masses
• Some of today’s massive galaxies formed quite early
• Good prospects for JWST and ELTs
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Wider or Deeper Surveys?
IMACS on the 6.5m Baade Telescope
27 Diameter field of view
Wider
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350-500 slits per mask
R ~ 1000
Nod & Shuffle sky subtraction
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Spectral Evolution
Passive
Intermediate
Composite
Young
Spectral Classes
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Le
Bor
gne
et a
l.
M > 3 x 1010 Msun
Z = 0.1
Abs
orpt
ion
Em
issi
on
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Le
Bor
gne
et a
l.
M > 3 x 1010 Msun
Z = 1.2
Em
issi
onA
bsor
ptio
n
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Post-Starburst Galaxies
M > 3 x 1010 Msun
50% of massive galaxies are post-starburstSystems at z ~ 1 !
H
Str
ong
Fra
ctio
n
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Massive Post Starburst Galaxies
Intermediate Mass Galaxies had their star formation truncated at z ~ 1.5
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CIRSI + LCO Wide Field IR Camera
du Pont 2.5m telescope 4 1024 x 1024 arrays
cryogenic Offner relay 16 channel electronics Persson, Murphy, Birk
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Post-Starburst GalaxiesL
e B
orgn
e et
al.
50% Post-Star Burst
@ z ~ 1.5