The Great Observatories Origins Deep Survey: Preliminary Results and Lessons Learned Mauro Giavalisco Space Telescope Science Institute and the GOODS team

The Great Observatories Origins Deep Survey:

Preliminary Results and Lessons Learned

Mauro GiavaliscoSpace Telescope Science Institute

and the GOODS team

STScI/ESO/ST-ECF/JPL/SSC/Gemini/Boston U./U. Ariz./U. Fla./U. Hawai/UCLA/UCSC/IAP/Saclay/Yale/AUI

GOODS: Great Observatories Origins Deep Survey

The GOODS Treasury/Legacy Mission

Aim: to establish deep reference fields with public data sets from X-ray through radio wavelengths for the study of galaxy and AGN evolution of the broadest accessible range of redshift and cosmic time.

GOODS unites the deepest survey data from NASA’s Great Observatories (HST, Chandra, SIRTF), ESA’s XMM-Newton, and the great ground-based observatories.

Primary science goals:• The star formation and mass assembly history of galaxies• The growth distribution of dark matter structures • Supernovae at high redshifts and the cosmic expansion• Census of energetic output from star formation and supermassive black holes• Measurements or limits on the discrete source component of the EBL

Raw data public upon acquisition; reduced data released as soon as possible


A Synopsis of GOODS

GOODS Space• HST Treasury (PI: M. Giavalisco)

– B, V, i, z (3, 2.5, 2.5, 5 orbits)– 400 orbits

– Δθ = 0.05 arcsec, or ~0.3 kpc at 0.5<z<5– 0.1 sq.degree– 45 days cadence for Type Ie Sne at z~1

• SIRTF Legacy (PI: M. Dickinson)– 3.6, 4.5, 5.8, 8, 24 μm– 576 hr– 0.1 sq.degree

• Chandra (archival):– 0.5 to 8 KeV– Δθ < 1 arcsec on axis

• XMM-Newton (archival)

GOODS Ground• ESO, institutional partner (PI C. Cesarsky),

CDF-S– Full spectroscopic coverage in CDF-S

– Ancillary optical and near-IR imaging

• Keck, access through GOODS’ CoIs– Deep spectroscopic coverage

• Subaru, access through GOODS’ CoI– Large-area BVRI imaging

• NOAO support to Legacy & Treasury– Very deep U-band imaging

• Gemini– Optical spectroscopy, HDF-N

– Near-IR spectroscopy, HDF-S

• ATCA, ultra deep (5-10 Jy) 3-20 cm imaging, of CDF-S

• VLA, ultra deep HDF-N (+Merlin, WSRT)

• JCMT + SCUBA sub-mm maps of HDF-N


The GOODS “space” fields

The GOODS HST fields: HDF-North & CDF-South~33x solid angle of combined HDF-N+S central fields~ 4x solid angle of combined HDF-N+S flanking fields~2.5x solid angle of WFPC2 Groth Strip~22 x 35 h65

-1 Mpc comoving transverse extent at z = 3

Both fields at high galactic & ecliptic latitude, with low zodiacal & galacticforegrounds, N(HI), stellar & radio contamination, etc.

KEY FEATURE: Simultaneous occurrence of :•Area………………………0.1 sq.deg•Sensitivity………………galaxies and AGN up to z~6-7•Angular resolution……0.5 kpc at 0.5<z<5•Wavelength coverage…0.4 to 24 m


We almost give you the Full Moon


GOODS/ACS field layout5 epochs/field, spaced by 45 days, simultaneous V,i,z bands

CDF-S: Aug ‘02 - Feb ‘03 HDF-N: Nov ’02 - May ’03

•Four more epochs in HDF-N by Aug 04•Five more epochs in both fields in ~ 1 year


ACS

B = 27.2

V = 27.5

i = 26.8

z = 26.7

WFPC2

B = 27.9

V = 28.2

I = 27.6

∆m ~ 0.7-0.8

AB mag; S/N=10Diffuse source, 0.5” diameterAdd ~ 0.9 mag for stellar sources


5-Epoch stack


SIRTF Imaging

3.6 , m

MIPS

IRAC

Numberof

Pixels

Fieldof

View

4.5 5.8 8.0

256x256 256x256 256x256 256x256

5’x5’ 5’x5’ 5’x5’ 5’x5’ 1’x1.2’

IRS

15

33x45

24

5’x5’

128x128

70

5’x5’

32x32

160

0.5’x5’

2x20

GOODS sensitivity

0.5524.5

0.5524.5

0.5524.5

0.5524.5

0.5524.5

5-σ limiting flux μJy5-σ limiting AB mag


GOODS-South [SST/IRAC & HST/ACS]

ACS F850LP

SST IRAC

3.6+5.8

3.6+4.5+5.8

4.5


Galaxies at High Redshift

•Theory predicts that dark matter structures form at z~20-30

•It does not clearly predict galaxies, because we do not fully understand star formation

•We need to push empirical studies of galaxy evolution to the highest redshifts

•We collected the deepest and largest quality samples of galaxies at z~4 through ~6

B435 V606 z850

Unattenuated Spectrum Spectrum

Attenuated by IGM

B435 V606 i775 z850

Z~4


LBG color selection

B-dropouts, z~4 V-dropouts, z~5


Galaxies at z~6 (~6.8% of the cosmic age)

S123 #5144: m(z) = 25.3

ACS/grism, Keck/LRIS & VLT/FORS2 observations confirm z=5.83

Dickinson et al. 2003


B435 V606 i775 z850

Galaxies at z~6


Observed redshift distribution

B

V

i

Z=5.78

Z=5.83

Z=6.24?

Spectra fromBunker et al. 2003;Stanway et al. 2003;Vanzella et al. 2004and the GOODS Team


LBG spectroscopy3 < z < 6: examples

Dawson, Stern, Spinrad, Madau et al.:

1 ok night with DEIMOS spectrograph, May 2003targeting B, V, and i-dropout selected LBG candidates

Good success for B- and V-dropouts considering sky conditions

No additional secure confirmations of i-dropouts

[OIII] [OIII]serendip.


…some more examples…

[OIII]


…more examples…


The history of the cosmic star formation activity:

We found that at z~6 the cosmic star formation activity was nearly as vigorous as it was at its peak, between z~2 and z~3.

•Dust obscuration not truly constrained•Escaping UV radiation only a small fractionLarge progress with SIRTF

•Selection effects•Estimated from detailed numerical simulations:•Found the input LF that minimizes for colors, sizes and n(m)

Giavalisco et al. 2003


Still uncertainty on measures

Bouwens et al. 2004

•LF still not well constrained •Clean z~6 color selection still missing•Cosmic variance still not understood

•Will use SST data to define z~6 sample•Will double exp time in GOODS


Area is key at very high redshift

Cosmic variance is empirically unknown,but obviously important

Very dangerous to base conclusions on small fields (eg. UDF), no matter how deep

Also, care needed to match samples with largely different sensitivity

IR-based selection needed (IRAC)

Down to z(AB)<27 and S/N>=5

GOODS~ 1 galaxies/arcmin2

UDF~ 1.5 galaxies/arcmin2


HUDF vs. GOODS

GOODS CDFS – 13 orbits HUDF – 400 orbits


Morphology of i-band dropouts

Candidates for galaxies at redshifts

greater than 6


Defining i-band dropouts

Selecting UDF samples with same criteria as the GOODS samples (eg. S/N(B,v)<~2) misses lots of galaxies, including a number of spectroscopically confirmed ones

Color selection using IR photometry is critical

Equally important: we need larger multi- surveys to constraint SF at z>6


rest-optical & -IR at z~6

• SST IRAC detections of z~6 galaxies=> stellar population & dust fitting possible

Dickinson et al in prep

ch1, 3.6mrest=5300A

ch2, 4.5mrest=6600A


Stiavelli, Fall & Panagia 2004

Did we find the sources Responsible for the Reionization at z~6?


Evolution of M* ?

Possible evidence of evolution ofM*

Here absolute magnitudes are Rs band (~1700 Ang rest)at z=3 (not 10 pc!)

Slope alpha is assumed same as at z~3; real error most certainly larger, because of covariance.

Note that alpha~1.5-1.6 for UV LFof late type galaxies, even in the local and intermediate redshiftuniverse.

GOODSGround[UnGRs]

Giavalisco et al. 2004, in prep.


Rest

-fra

me m

(1600)

- B

UV-Optical Color-Magnitude Diagrams at z ~ 3 and z ~ 4

Rest-frame B-band

Papovich et al. 2003


Luminosity Density versus Color and Redshift

increase of ~33%

U- and B- dropouts have similar UV-Optical color-magnitude "trends”.

Rest-frame UV luminosity density roughly comparable at z ~ 3 and 4.

Increase of ~33% in the rest-frame B-band luminosity density from z ~ 4 to 3.

UV-Optical color reddens from z ~ 4 to 3, which implies an increase in the stellar-mass/light ratio.

Suggests that the stellar mass is increasing by > 33% growth in B-band luminosity density.

Papovich et al. 2003


Implications for Galaxy Evolution

Dickinson, Papovich, Ferguson, & Budavari 2003


Implications for Galaxy Evolution

Dickinson, Papovich, Ferguson, & Budavari 2003

GOODS; Papovich et al. 2003


Stellar mass & star formation

PAH + continuum (24 m)

UV

Far IR(GTO)

Optical+ near-IR+ nebular lines

Mass: Rest-frame near-IR (e.g., rest-frame K-band at z~3), provides best photometric measure of total stellar content Reduces range of M/L() for different stellar populations Minimizes effects of dust obscuration

Star formation: Use many independent indicators for to calibrate star formation (obscured & open) in “ordinary” starbursts (e.g. LBGs) at z > 2.• mid- to far-IR (SIRTF/MIPS); rest-frame UV (e.g, U-band); radio (VLA, ATCA); sub-mm (SCUBA, SEST); nebular lines (spectroscopy)

Stellar mass fitting

Measuring star formation


Testing the Hierarchical Cosmology

Hierarchical models predict a simple scaling relation of galaxy size with redshift:– Baryonic matter of mass-fraction md settles into disks with a fraction jd of the

halo angular momenta. The disk radii are

– The dark-matter halo radii grow as

)(10)(100

3/1

2 zH

V

zH

GMr virvir

vir

mjrr

d

dvird

C2

2/130

200,0,0 111)( zzHzH


Expectations

• Size evolution at fixed circular velocity:– R ~ H-1(z)

• Size evolution at fixed mass:– R ~ H-2/3(z)

• Log-normal size distribution proportional to the spin parameter

• Disk-like morphologies

ddp

2

2

2

lnexp

2

1

Fall & Efstathiou 1980; Mo, Mao & White 1998; Dalcanton, Spergel & Summers

1997; Bowens & Silk 2002


The Evolution of galaxy size

Standard ruler

R~H(z)-2/3

R~H(z)-1

First measures at these redshiftsTesting key tenets of the theory

We found that galaxies grow hierarchicallyMajor improvements with full-dept ACS

Will add point at z~6

Ferguson et al. 2003


Proto Spirals or Proto Ellipticals?

B dropouts z~4

disks

spheroids

C 5log r80/r20

spheroids

disks

Ferguson et al. 2003

The theory predicts that early galaxies are disks.At z~ 4 we found a mix of disks and spheroidsThe z~4 galaxies do not seem to be primeval.Next: the z~5 and z~6 galaxies


Morphology of Lyman Break Galaxies at z~4

Sersic profile fits and Sersic indices:

[Ravindranath et al. 2004]

Irregulars: (n < 0.5)

Disks: (0.5 > n > 1.0)


Morphology of Lyman Break Galaxies at z~4

Bulges (n > 3.0)

Central compact component / point sources? (n = 5.0)


LBGs at z~4-5: disks or spheroids?

Ravindranath et al. 2004

Theory predicts that when they form undisturbed, galaxies are disks.

Data show that a significant number of z~4-5 LBGs are disks; spheroids are present, too.


LBGs’ morphology

There appears to be a correlation between UV luminosity and size of LBGs at z~4 and z~3


Rotation curves at z~2

GOODS large area and angular resolutionenabled the first systematic kinematical studies of galaxies at z~2

Erb et al. 2004Steidel et al. 200413 GOODS-N galaxies

morphologically selected


“Rotation curves” at z~2

What is the relationship between morphology and kinematics?

HDF-BX1397

Seeing is crucial!!Imagine what JWST will do

Only 3 out of 13 galaxies showevidence of coherent velocityfield/shear

Erb et al. 2004

Steidel et al. 2004


Galaxy kinematics at z~2

Erb et al. 2004; Steidel et al. 2004

Compact galaxies appear to have larger kinematics

Ravindranath et al. 2003

–Sersic indices n<2–Rest-frame MB <-19.5–Photometric redshifts


Disk galaxy evolution from GOODSRavindranath et al. 2003

Tendency for smaller sizes at z~1 (30% smaller)

Number-densities are

relatively constant to z~1


Using Sne to Measure the Evolution of SF

Dahlem et al. 2004, in press

Core Collapse Type Ia


GOODS weak lensing program:mapping dark matter in space

and time

• Galaxy-galaxy shear– GOODS is measuring

• Shear vs. redshift

• Shear on angular scales < 2 arcmin – Measure dark-matter halo profiles

– Evolution of M/L with redshift

– Test the “galaxy-in-peak” paradigm

– Shear is dominated by non-linear fluctuations• Insensitive to CDM large-scale power spectrum (shape and

normalization): complementary to WMAP

• Sensitive to cosmic energy contents through angular-diameter distance and growth-rate of perturbations


Weak Lensing: Mapping the Growth of Dark Matter

•Galaxy-galaxy shear around bright galaxies•Direct measure of dark matter•HST-unique science at these and larger redshiftsSDSS-like quality measures at z~0.5Huge improvements over previous HST surveys (e.g. MDS)

Casertano et al. 2004

SDSS atz~0.1

Lenses:19<z<22;Sources:24<z<26.5


Clustering at z~3

•Measured at z~ 3 from a very large sample of U-band dropouts (2300 galaxies)

•Selected from KPNO (U) and Subaru + Supreme (BR) large-area (25x25 arcmin), deep images (Capak et al. 2003, part of GOODS)

•Sample goes down to R<26

•Spatial correlation length is smaller than that of brighter samples at the same redshifts

Lee et al. 2004, in preparation


Clustering at High Redshift

Notes: 1. r0 from Limber inversion of

(2. GOODS redshift distribution

function from numerical simulations

Adelberger et al. (1998, 2002)Giavalisco et al. (1998)Giavalisco & Dickinson (2001)

New measure consistent with presence of clustering segregation

GOODS


Halos and Galaxies at z~3-5

Good agreement with theory

Implied halo mass in the range5x1010 – 1012 MO

1-σ scatter between mass and SFRsmaller that 100%

Giavalisco & Dickinson 2001Porciani & Giavalisco 2002Lee et al. 2004, in prep.


When did Super-Massive Black Holes Form?

Chandra and Hubble working together:

we found 7 sources detected by Chandra but not detected by HST. Among them, most likely there are:

The most distant active galaxies (super-massive black holes) ever observed, at z>7 ?

SIRTF will determine whether this interpretation is correct or not


The Most Distant Black Holes (z>7)?


Off-nuclear X-ray sources

Hornschemeier et al. 2004

X-ray luminosity of sourcesComparable to integrated Point-source Luminosity of Local galaxies.

X-ray variability shows that Several are likely accreatingSingle BH.


GOODS discovery of a significant population of hidden SMBH

Meg Urry, Ezequiel Treister, Jeffrey van Duyne (Yale University) &

GOODS AGN team


Num

ber

z-band magnitude

HST ACS z-band counts

Treister et al. 2004

faint bright

obscured AGNnormal AGN

GOODS: Great Observatories Origins Deep Survey photz

Treister et al. 2004

Redshift distribution (GOODS-N)

Num

ber

Redshift

GOODS: Great Observatories Origins Deep Survey photz

Treister et al. 2004Redshift

Redshift distribution (GOODS-S)

Num

ber


Optical/X-ray picture so far:

• GOODS HST data suggest population of high-z obscured AGN

• Consistent with AGN unification – constant ratio of obscured:unobscured

• Implies missed X-ray sources, incomplete spectral identifications, missed optical sources

• Will be visible in infrared! Are visible with Spitzer IRAC!


First look at Spitzer IRAC data for GOODS (at 8 m)

Observed N(>S)

Predicted N(>S)

for obscured AGN


First look at Spitzer IRAC data for GOODS (at 3.6 m)

Observed N(>S)

Predicted N(>S)

for obscured AGN

observed counts

predicted counts


The GOODS ACS Treasury Program and

The Hubble Higher-z Supernova Search Team

“A Higher-z Supernova Search Piggybacking on the ACS Survey” 134 orbits ToO

for 6-8 SNe Iaat 1.2<z<1.8

Riess (STScI)Strolger (STScI)Tonry (UH)Filippenko (UCB)Kirshner, (CfA)Challis, (CfA)Casertano, (STScI)Dickinson (STScI)Giavalisco (STScI)Ferguson (STScI)

399 orbitsof deep imagingfor extragalacticstudies

~18% of HST in year 11,more searching this year


Finding High-z Sne

• GOODS found 6 of the 7 highest redshift (z>1) supernovae currently known

Search completed: 43 SNe identified~25 Type Ia candidates at z>1

–10 follow-ups by ToO program–12 spectroscopic confirmations so far–3 highest-z spectral confirmations (z>1.3)

Four Additional Epochs of HDFN in 2004: –Riess et al. and Perlmutter et al.

Eight Additional Epochs of HDFN and CDFS in 2004

•Riess et al. High-z SN “Artemis” fromCDF-S ACS observations


Searching for SNe Ia with ACSSearching for SNe Ia with ACS

5 z-band epochs, spaced by 45 days, simultaneous v,i band, 120 tilesCDFS=08/02-02/03 HDFN=11/02-05/03


2003ak(1.57)

2002fz(0.839)

2003aj(1.4)

2002ga(0.988)

2002kb(0.474)

2002fv(~1.0)

2002lg(0.61)

2002fw(1.3)

2002hs(0.388)

2002hp(1.3)

2002hq(0.74)

2002kd(0.735)

2002fx(~1.8)

2003al(0.91)2002ke

(0.578)

2002kc(0.214)

2002hr(0.526)

2002fy(0.88)

2002ht(?)

CDFS

2003dz(0.48)

2003er(0.63)

2003be(0.64)

2003dx(0.46)

2003bb(0.89)

2003bc(0.51)

2003ew(0.66)2003eu

(0.76)

2003ba(0.47)

2002kh(0.71)2003et

(0.83)

2003en(0.54)

2003es(0.968)

2003en(0.54)2003dy

(1.37)

2003ea(0.89)

Vilas(0.86)

2003eb(0.92)

2003bd(0.67)

2003eq(0.85)

2002kl(0.39)

2003az(1.27)

2002ki(1.14)

HDFN


zv

b

i

SN Ia

SN II

Color Selection: An example

b v i z

SN Ia UV deficit


Color Discrimination


Our first higher-z SN Ia, Aphrodite

Aphrodite (z=1.3)

ACS grism spectrum

NICMOS F110W

ACS F850lp

viz

Highest z spectrum of a SN


Our Second Higher-z SN Ia, Thoth

red, ellipticalhost

Epoch 3Epoch 2 3-2Images

Subtractions

discovery

z=1.3


Rich Field of 4 SNe IaHDFN, tile n4z_26/29

Villas (z=0.94)

Borg (z=1.34)

Anguta (z=0.67)

McEnroe (z=0.90) grism

grism


Gilgamesh z=1.6

ACSf850lp

NicmosF110W

F160W

discovery ~+10 days ~+20 days


16 SN Ia Light CurvesToO

ToO

ToO

ToOToO

ToO

ToO

ToO


The HST Advantage

ToO

Highest 2Ground-based

z=1.06

z=1.20

z=1.30

z=1.30

HST-ACS


SN Ia Spectraat High-z ACS

ACS ACS

ACS ACS ACS

indicates Ca II @ 3750 A

See Riess et al 2003, astro-ph 0308185,and Blakeslee et al 2003, ApJ

#1#2#3


Matching Shapes and Colors

Light Curves Shapes at z>1 match those at z<0.1

B-V and U-B colors atz>1 match those at z<0.1

U-B: Most chemically sensitivez<0.1: <U-B>=-0.45+/-0.02z>0.6: <U-B>=-0.47+/-0.02


The New SN Ia Hubble Diagram

97ff6 of the 7 highest redshift SNe Ia


Is Cosmic Acceleration Real?

?


A Cosmic Jerk: Deceleration gave way

to Acceleration,


Expansion Kinematics(How Long Has This Been Going On?)

z~0.3-0.6,~5 GYR ago

present acceleration

past

dec

eler

atio

n


(If the Dark Energy is Lambda), Updated

Constraints

factor of 7 improvement!

Riess et al 1998; High-z Team

New


Probing Dark Energy

•We have doubled our knowledge of w0 and w’ in 1 year with HST •Einstein’s model now looks better than ever, a way to go…

Two fundamental properties/clues of dark energy: its strength, w0, AND is it dynamic or static, i.e. is w’=0?

Einstein’s

w0 w0

W’


Closing in on Dark Energy: The Future

W

’

W

’

Rejection of lambda: i.e., or would be a tremendousBreakthrough!

GOODS has been an effective technology demonstrator for SNAP/JDEM

CFHT L,ESSENCE,Sloan DSS,Carnegie

There should be another8-12 Type Ia at z>1 in ~1 yrtime frame


Summary

• GOODS exploring fundamental issues of cosmic origins• Large-scale star formation in place at less than ~7% of the cosmic time:• Cosmic star formation (as traced by UV light) varies mildly at 3<z<6

– Universe is ~ as prolific a star former at z~6 as it is at z~3, after triplicating age

• Direct evidence of growth of stellar mass from z~4 to z~1 (big progress expected from SIRTF)

• Galaxy sizes evolve hyerarchically; all visible galaxies small at z>2• Massive galaxies in place at z~1; some galaxies are massive at z~2-3• Spatial clustering of star-forming galaxies depends on UV luminosity:

decreases for fainter galaxies– Total mass and star-formation activity correlate: more massive halos host more

star formation; scaling consistent with CDM spectrum– Implies relatively large total masses: 5x1010 – 1012 MO

• Evolution of galaxy size at low, high z consistent with hierarchical growth• Evidence of supermassive BH (AGN) already at z>7• Constraints to the evolution of LF of QSO at z>3

Documents

The Great Observatories Origins Deep Survey: Preliminary Results and Lessons Learned Mauro Giavalisco Space Telescope Science Institute and the GOODS team