faint red galaxies evolved stars at high redshift nov 6, 2002 p. j. mccarthy stsci carnegie...
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Faint Red Galaxies
Evolved stars at High Redshift
Nov 6, 2002
P. J. McCarthy
STScI
Carnegie Observatories
Distant Galaxy Studies in the 20th Century
• Focused on faint blue galaxies
• Samples UV bright populations
• Traces heavy element production
• Global census of conversion of gas into stars
Evolution of UV luminosity density
Steidel et al 99
Lilly, Madau
Distant Galaxy Studies in the 20th Century
• Probes galaxy building via star formation• Insensitive to assembly of galaxies via mergers• Selects by light not mass• Near-IR offers a window on mass evolution
Build-up of stellar mass over cosmic time
Near-IR luminosity provides proxy for
stellar mass
Near IR-surveys are technically challenging
Optical and near-IR Detectors
Large formats: 2k x 4k
3 edge buttable
100 Mpixel FPAs common
Cheap - $ 0.01 per pixel
2k x 2k maximum Non-buttable
Expensive
$ 0.13 per pixel !
Challenges facing Deep near-IR Surveys
• Detectors small and Expensive
• Cryogenic Optics & baffles required
• Sky 3 orders of magnitude brighter
• Can’t observe when the moon is down!
Earliest IR Surveys – New Red population
Elston, Rieke & Rieke 1989 10 sq .arcminutes
Hu & Ridgeway 1992
100 sq. arcminutes
Some EROs are Sub-mm sources
Dey et al. 1999
Smail et al. 1999
Two Red populations?
Elston, Rieke & Rieke 1989 10 sq .arcminutes
Z ~ 1 early types
Hu & Ridgeway 1992
100 sq. arcminutes
Z > 1 Starbursts
Las Campanas IR Survey
McCarthy, Persson, Martini, Koviak (OCIW)
Chen (MIT), Marzke(SFSU), Carlberg, Abraham(UT)
Ellis (Caltech), Firth, McMahon, Lahav (IoA)
PHASE I: A Carnegie-Cambridge-Toronto Collaboration
PHASE II: A Diversified Conglomerate
• Galaxy Assembly in the 1 < z < 2 Epoch• Space density of massive galaxies• Stellar evolution in early type galaxies• Evolution of 3-D Clustering• Growth of massive galaxies and structure
GOALS
Why Select in the near-IR?
•Selects on basis of population with high
M/L
•Optical-IR color indices excellent for foreground rejection
•That where the light is!
V I H KZ = 1.5
Approach
• Multi-color optical & near-IR imaging survey
• Depths keyed to z = 2 elliptical: Ks ~ 21 !
• Photometric redshifts
• Six fields around the celestial sphere
• 1 square degree
Color-Mag Diagrams Color-Redshift Diagrams
Number Counts Color-Color Diagrams
Luminosity Functions Angular Clustering
Morphologies Spectroscopy
• Phase I: 1 square degree to H = 20.5 + VRI • Phase II: 1 square degree to K = 20.8 + BVRIz’JH • VRIH survey completed in spring 2001• 0.5 square degrees J & K in hand• ~10,000 K-selected objects• ~70,000 photometric redshifts• 250 spectroscopic redshifts
Reality Intrudes!
CIRSI + LCO Wide Field IR Camera
du Pont 2.5m telescope 4 1024 x 1024 arrays
cryogenic Offner relay 16 channel electronics
4 1024x1024 detectors – 90% gaps
4 pointings – 16 1024 x 1024 images
4 pointings – 16 1024 x 1024 images
4 pointings – 16 1024 x 1024 images
13’ x 13’ mosaic – 3 hour exposure
100,000
1024 x 1024
Frames - 30 seconds each
Red Galaxies are Abundant
V,I,K
80”
Photometric Redshifts• 8 color photometery BVRIz’JHKs
• 6 Galaxy templates
• 1 AGN, 128 stellar templates
Best fit template and redshift
Likelihood function
See Connolly et al 1995,1997
Photometric Redshifts from LCIR
Chen et al 2002
Photometric Redshifts from LCIR
Recent update
GMOS redshifts
Basic Phenomenology:
Sky density, Space Density, Luminosity & Color Evolution
IR to Optical Color Selection
I-K > 4
Rejects z < 1
Foreground & late types at all redshifts
IR to Optical Color Selection
I-K > 4
Rejects z < 1
Foreground & late types at all redshifts
Color-Magnitude Diagram
Stars
0.0 < z < 1.0
1.0 < z < 1.5
1.5 < z < 2.0
700 sq. arcmin
Classical Star Counts
Classical Star Counts
Number-Magnitude Relations
I-K > 4.0
I-K > 4.5
I-K > 5.0
Number-Magnitude Relations
I-K > 4.0
I-K > 4.5
I-K > 5.0
Gardner et al K-band LF
UV & Optical Color DiagnosticsV I H KZ = 1.5
Optical to IR color sensitive to old
population I-K
Rest-frame UV slope sensitive to
recent star formation
V-I
Color-Color Diagrams
• Stars form distinct sequence
K < 17.5
Color-Color Diagrams
• Stars form distinct sequence
K < 18.5
Color-Color Diagrams
• Stars form distinct sequence
• Z > 1 galaxies appear at K ~ 19
K < 19.5
Color-Color Diagrams
• Stars form distinct sequence
• Z > 1 galaxies appear at K ~ 19
• Z > 1.5 galaxies at K ~ 20
K < 20.8
Color-Color Diagrams
• Stars form distinct sequence
• Z > 1 galaxies appear at K ~ 19
• Z > 1.5 galaxies at K ~ 20
• Reddest galaxies follow minimal evolution track
K < 20.8
Color-Redshift Diagrams
Evolving Luminosity Functions• LFs derived from photo-
z’s with modified likelihood approach
• LF at intermediate z agrees well with CNOC2
• Very little apparent evolution in L* to z ~ 1.2
Chen,Marzke et al. 2002
R-band Luminosity Density
Rest-Frame R-band Luminosity density
little or no evolution to z ~ 1.2
Clustering:
A proxy for merging
Tags populations at high and low redshift
Angular vs. 3-D Clustering
Clustering of Red Galaxies
Angular Clustering
Clustering amplitude of red galaxies is 20 x that
of the full field
Angular Clustering
= 12”
I – K > 4
= 1”
All K < 20.5
Angular Clustering
Clustering amplitude higher for redder colors and brighter magnitudes.
= 30”
K ~ 18 & I-K > 5
n(z) required for r_0
Inversion of to r0
All I-K K > 19 <z> 0.7
I-K > 4 19 < K < 20 <z> 1.0
I-K > 4 18 < K < 19 <z> 1.0
’’ I-K > 5 18 < K < 20 <z> 1.2
Generalized Limber equation:
n(z) for I-K selected subsamples
Inversion of to r0
All I-K K > 19 <z> 0.7 5 h-1Mpc
I-K > 4 19 < K < 20 <z> 1.0 9
I-K > 4 18 < K < 19 <z> 1.0 9
’’ I-K > 5 18 < K < 20 <z> 1.2 10
Generalized Limber equation:
Evolution and Color Dependence
Red color selection or E morphological
selection
Blue color selection or late
type morphological
selection
LCRS CNOC2 CFRS CFGRS LBG
Evolution and Color Dependence
Kauffmann et al 99
Early types
Star forming galaxies
LCRS CNOC2 CFRS CFGRS LBG
Morphology:
What type of Galaxy are we talking about after all?
E/S0
Template
Match
Giavalisco
et al
Cycle 11
Treasury
Program
10/5/02 public release
91 objects
Giavalisco
et al
Cycle 11
Treasury
Program
10/5/02 public release
Sab/Sbc
Template
Match
Giavalisco
et al
Cycle 11
Treasury
Program
10/5/02 public release
54 objects
E/S0
Template
Match
Giavalisco
et al
Cycle 11
Treasury
Program
10/5/02 public release
Sab/Sbc
Template
Match
Morphologies of Red Galaxies4.0 < I – K < 4.5 <z> = 1.0
Template type 1 (E/S0)
85% Compact 10% Disks 5% Diffuse
Template type 2 (Sab/Sbc)
60% Compact 35% Disks 5% Diffuse
Template type 1 (E/S0)
60% Compact 25% Disks 15% Diffuse
Template type 2 (Sab/Sbc)
40% Compact 30% Disks 30% Diffuse
4.5 < I – K < 5.0 <z> = 1.2
See Stiavelli
& Treu 1999
NICMOS results
Spectroscopy:
Real redshifts and Spectral Diagnostics
Goals:• First Complete sample 1<z<2
– use photo-z’s to weed out low-z galaxies (BVRIzJHK)
• Determine luminosity and mass functions– Can we see the assembly of mass? – Massive galaxies at z=2 would severely trouble CDM– Mass(z) more robust than SFR(z)
• Relate to galaxy morphology (ACS)– Identify Ell/Sp/Irr over 1<z<2– Track low-z behavior to high-z
• E.g. can we see mass assembly of giant Ellipticals?• Can we track the dynamical evolution of spiral disks
• Track SFH over 1<z<2: – Age of galaxies, metallicities of population
Conventional Slit Spectroscopy
• Sky subtraction is primary limitation– Slit irregularities– Flat-field errors– Residual Fringing– Geometric distortions– Low slit density on sky
• Beam switching ?– Variable sky spectrum– Read noise penalty– High read-out overhead
• The solution: ‘nod & shuffle’Glazebrook &
Bland-Hawthorn 99
Sky cancellation: ‘nod and shuffle’Storage of ‘sky’ image next to object image via ‘charge shuffling’Zero extra noise introduced, rapid switching (60s)
A
B
AB
Typically A=60s/15 cy: 1800s exposure10 subtraction
GMOS N&S Sky residualsSUMMED along long slit (1.8 arcmin)
Raw Sky/20
Subtracted sky
(i.e. ~10 level is enough for 200,000 sec pointed obs.)
Cycle:A=60sB=60s
+ 25s o/head
Gemini + GMOS
GMOS spectrographGemini
GMOSLRISLDSS1
Tel.+instr. efficiency
GMOS represents the best possible option for a red sensitive MOS. Ideal system for nod & shuffle
GDDS Spectra77 objects 40,000 secs
[OII] Redshifts from GDDS
23.7 < I(AB) < 24.2
Absorption Line Spectra
I = 24.0
Z = 1.67
I = 23.7
Z = 1.56
I = 24.2
Z = 1.39
Rest Wavelength
High Redshift Elliptical Galaxies?
FeIIMgII
53W091 at z=1.393VI=2.2 IK=2.94
Model: 4 Gyr old stellar populationat z=1.4, age of Universe = 4.5Gyr
z(form) ≈10
Obj # 398 from GDDS SA22VI=1.7 IK=2.7
Wavelength / Angstroms
f
Rest-frame UV absorption line redshifts!
Color-z of GDDS galaxies
At least halfway across the desert!!
Again just the easy ones…
Conclusions
• Counts: little density evolution to z ~ 1.2• LFs: R-band Luminosity density declines by < x
2 to z ~ 1.5• UV colors: wide range of star formation levels• Clustering: Strong clustering consistent with
local E population• Morphologies: Predominantly early types• Spectroscopy: Intermediate age populations
The Progenitors of Early Type Galaxies
Conclusions
Population of massive field early types largely unevolved since z ~ 1.5
The Future
Bridging the gap between the faint red galaxies at z ~ 1.5
and the LBGs at z > 2
Gemini Deep Deep Survey
GDDS Team: Karl Glazebrook (JHU), Bob Abraham (Toronto), Pat McCarthy (OCIW), Rick Murowinski (DAO), Ray Carlberg (Toronto), Ron Marzke (SDSU), Sandra Savaglio (JHU), H-W Chen (OCIW) David Crampton (DAO), Isobel Hook (Oxford), Inger Jørgensen & Kathy Roth (Gemini)
Goal: Deep 100,000 sec MOS exposures on Las Campanas IR Survey fields to get redshifts of a complete K<22.4 I<25 sample covering 1<z<2
GDDS history• Sep 2001: start of GDDS evil planning• Jan 2002: team approached Gemini observatory with nod
& shuffle proposal• Feb 2002, obtained Gemini go-ahead.• Feb-May 2002. Implementation of N&S at DAO (~$10K
cost)• May 2002: first N&S engineering observations on 8m• July 2002: N&S commissioned on sky• Aug 2002: First 4 nights of GDDS Science Verification
for N&S success!!• Sep-Dec 2002: Band I queue time, 50 hrs
GDDS mask84 objects 2 tiers with150 l/mm grating
GDDS Nod&Shuffle Mask
GDDS Nod&Shuffle Mask
Photometric Redshifts from LCIR
I=23.8
Example object: raw object+skyOH forest
I=23.8 z=1.07
Example object: N&S subtracted[OII] 3727at 7700Å
GDDS: Oct 2002 snapshot• GDDS SV Aug 2002 + Band I Queue time
(Sep/Oct 2002) Up to 100 ksec on first field (SA22)First 40 ksec now reduced and very preliminary redshifts
• TO COME 2002-2003 (total time awarded 50 hrs in Band I):Complete 3 GDDS fields, secure 100 z>1 redshifts
GDDS: ultra-super-preliminary results
These are just the‘easy’ ones so far!~ 40 ksec
Working on CCF
Data on this field is still coming in.
Full 100,000 secswill pound on z=1.5old red galaxies
High Redshift Elliptical Galaxies?
FeIIMgII
53W091 at z=1.393VI=2.2 IK=2.94
Model: 4 Gyr old stellar populationat z=1.4, age of Universe = 4.5Gyr
z(form) ≈10
Obj # 398 from GDDS SA22VI=1.7 IK=2.7
Wavelength / Angstroms
f
Rest-frame UV absorption line redshifts!
Photometric Redshifts from LCIR
Colors of GDDS galaxies
GDDS
HDF LBGs (Papovich et al. 2001)
z=1.4 E/S0 template
z=1.4 Sbc template
Color-z of GDDS galaxies
At least halfway across the desert!!
Again just the easy ones…
GDDS: summary• GDDS hits complete sample at z>1
– Photo-z selection z>1 ~works
• Gets spectra via ‘nod & shuffle’ sky cancellation– Successfully commissioned July-Aug 2002, have data
on first (half) field
• Are we seeing a dearth of high mass galaxies at z>1 ? Possible epoch of mass assembly?
• TO COME 2002-2003:Complete 3 GDDS fields, secure 100 redshifts Apply for HST/ACS imaging for morphologies
Mass function vs Morphology vs z.
GDDS: seeking old
galaxies at z>1
z=1.4, IK=2.7
Obscured Charge
Storage Area
Obscured Charge Storage Area
First Exposure
Active slit area
“A” position
“B” position
Now nod telescope and shuffle charge
Nod & shuffle the other way
“A” position
“B” position
Repeat N times and then readout
Difference of two positions
Finally shift and add both
LBL High Resistivity CCDs
LBL High Resistivity CCDs
No fringing, but high CR rates
LBL High Resistivity CCDs
Straight average - 2 hours Nod & Shuffle
LBL High Resistivity CCDs
+/- 200 DN rejection
Las Campanas IR Survey
• Goal: Empirical understanding of early galaxy evolution
• Target: 1 square degree to K = 21
• Pilot survey in 2000/2001: VRIH to H=20.5
• Six fields around the equator (2 in south!)
• 1 square degree in BVRIz’H
• 0.5 square degrees in J & K to K = 20.8
• 200+ redshifts with LDSS2
• ~ 50 redshifts with GMOS & LRIS
Another example
Las Campanas IR Survey
McCarthy, Persson, Martini, Koviak (OCIW)
Chen (MIT), Marzke(SFSU), Carlberg, Abraham(UT)
Ellis (Caltech)
ConclusionsWe have identified a population having:
The colors and luminosities expected of evolved stellar systems
The space density & LF of early-type galaxies
Clustering scale lengths similar to present day massive galaxies
Morphologies that are primarily compact consistent with spheroid dominated systems
Spectral features indicative of turn-off ages > 1 Gyr
These are the progenitors of Elliptical Galaxies