# Presentation: 700455

##    The Great Observatories Origins Deep Survey: Preliminary Results and Lessons Learned

-    The Great Observatories Origins Deep Survey: Preliminary Results and Lessons Learned

- Mauro Giavalisco
- Space 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

## 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 *h*65-1 Mpc comoving transverse extent at *z* = 3
- Both fields at high galactic & ecliptic latitude, with low zodiacal & galactic
- foregrounds, *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 layout

- 5 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**

## ∆m ~ 0.7-0.8

**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=10**
**Diffuse source, 0.5” diameter**
**Add ~ 0.9 mag for stellar sources**

**5-Epoch stack**

## SIRTF Imaging

**GOODS **
**sensitivity**

**0.55**
**24.5**

**0.55**
**24.5**

**0.55**
**24.5**

**0.55**
**24.5**

**0.55**
**24.5**

**5-σ limiting flux μJy**
**5-σ limiting AB mag**

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

**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**

*  **B**435**            **V**606** ** **           **i**775**         **z**850*

***Z~4***

## LBG color selection

- B-dropouts, z~4

- V-dropouts, z~5

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

*Dickinson et al. 2003*

- Galaxies at z~6

## Observed redshift distribution

**B**

**V**

**i**

**Z=5.78**

**Z=5.83**

**Z=6.24?**

*Spectra from*
*Bunker et al. 2003;*
*Stanway et al. 2003;*
*Vanzella et al. 2004*
*and the GOODS Team*

## LBG spectroscopy3 < z < 6: examples

- Dawson, Stern, Spinrad, Madau et al.:
- 1 ok night with DEIMOS spectrograph, May 2003
- targeting 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

## ...some more examples...

## ...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 fraction
- Large 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, 3.6********m**
******rest****=5300A**

**ch2, 4.5********m**
******rest****=6600A**

## Did we find the sources 

**Stiavelli, Fall & Panagia 2004**

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

## Evolution of M* ?

*Possible evidence of evolution of*
*M**
*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 LF*
*of late type galaxies, even in the *
*local and intermediate redshift*
*universe**.*

*GOODS*

*Ground*
*[UnGRs]*

*Giavalisco et al. 2004, in prep.*

## Rest-frame m(1600) - B

*Rest-frame 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 

*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

*Implications for Galaxy Evolution*

*Dickinson, Papovich, Ferguson, & Budavari 2003*

## Implications for Galaxy Evolution

*Implications for Galaxy Evolution*

*Dickinson, Papovich, Ferguson, & Budavari 2003*

*GOODS; Papovich et al. 2003*

## Stellar mass & star formation

***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

## 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

- 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 redshifts***
***Testing key tenets of the theory***
***We found that galaxies grow hierarchically***
***Major improvements with full-dept ACS***
***Will add point at z~6***

*Ferguson et al. 2003*

## Proto Spirals or Proto Ellipticals?

- 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 spheroids
- The 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

**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 resolution
- enabled the first
- systematic kinematical
- studies of galaxies
- at z~2

*Erb et al. 2004*
*Steidel et al. 2004*

- 13 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 show**
**evidence of **
**coherent velocity**
**field/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 GOODSRavindranath 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 redshifts***
***SDSS-like quality measures***
***    ******at z~0.5***
***Huge improvements over  previous HST surveys (e.g. MDS)**** *

*Casertano et al. 2004*

*SDSS at*
*z~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:
- r0 from Limber inversion of (
- 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 range**
**5x10****10**** – 10****12**** M****O**
**1-σ scatter between mass and SFR**
**smaller that 100%**

*Giavalisco & Dickinson 2001*
*Porciani & Giavalisco 2002*
*Lee 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 sources
- Comparable to integrated
- Point-source Luminosity of
- Local galaxies.
- X-ray variability shows that
- Several are likely accreating
- Single BH.

## GOODS discovery of a significant population of hidden SMBH

- Meg Urry, Ezequiel Treister, Jeffrey van Duyne *(Yale University) & GOODS AGN team*

## HST ACS z-band counts

- Number

- z-band magnitude

***Treister et al. 2004***

***faint***

***bright***

- obscured AGN

- normal AGN

## Redshift distribution (GOODS-N)

- photz

***Treister et al. 2004***

- Number

- Redshift

## Redshift distribution (GOODS-S)

- photz

***Treister et al. 2004***

- Redshift

- Number

## 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)

- 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 Ia
- at 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 orbits**
**of deep imaging**
**for extragalactic**
**studies**

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

**Notes:**
Only HST can find these, but HST is a narrow field imager, 
fortunately we have friends who need deep and wide images with HST to
Study galaxy evolution and we have been able to hitch a ride on their program
Like the parasites we are and!

## 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.*

## Searching for SNe Ia with ACS

- 5 z-band epochs, spaced by 45 days, simultaneous v,i band, 120 tiles

- CDFS=08/02-02/03                             HDFN=11/02-05/03

**Notes:**
GOODs observes 2 fields every 45 days, 15 tiles in the z-band and we search for supernovae.
So far we have found 5 or 6 each time we do this and 1 or 2 look like high-redshift Ia’s.  We
Then target with our ToO program to get the measurements we need.

## CDFS

- 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**

**Notes:**
We inspected these fields for a year and found 42 weapons of mass destruction
About half were type Ia’s, median redshift 1, many significantly higher

## Color Selection: An example

- z

- v

- b

- i

- SN Ia

- SN II

- b

- v

- i

- z

**SN Ia UV deficit**

**Notes:**
Two vivid examples are seen here from our last search in May

## Color Discrimination

**Notes:**
This has been an effective technique...here is where some of the apparent
And later confirmed Sne Ia have appeared in the redshift/color space

## 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

**Notes:**
Our first target was Aphrodite (SN 2002fw).  New modes of HST are critical
To the measurements.

## Our Second Higher-z SN Ia, Thoth

- red, elliptical
- host

- z=1.3

**Notes:**
Our second was Thoth---you need to subtract image to actually see this one.

## Rich Field of 4 SNe Ia

- HDFN, 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

- ACS
- f850lp

- Nicmos
- F110W
- F160W

- discovery

- ~+10 days           ~+20 days

**Notes:**
One of the more distant ones, had to use NICMOS to follow...

## 16 SN Ia Light Curves

**ToO**

**ToO**

**ToO**

**ToO**

**ToO**

**ToO**

**ToO**

**ToO**

**Notes:**
Now that we have taken a break from searching, we have had a chance to beging reducing
The light curves and analyzing...here is all the photometry from 8 ToO, and another 8 serendipitious Ia’s

## The HST Advantage

**ToO**

- Highest 2
- Ground-based

- z=1.06

- z=1.20

- z=1.30

- z=1.30

- HST-ACS

**Notes:**
Now that we have taken a break from searching, we have had a chance to beging reducing
The light curves and analyzing...here is all the photometry from 8 ToO, and another 7 serendipitious Ia’s

## SN Ia Spectraat 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

**Notes:**
One of the biggest surprises of this campaign was the quality of our spectroscopy.  Usually
This is very hard from the ground because the relevant features shift
To the IR where the sky is bright and the highest spectroscopic id from the ground is z=1.2 achieved once in 5 years
By each team.  In our first year we obtained the 3 highest spectroscopic classifications.  Even though HST is much
Smaller than Keck, the slitless grism on ACS easily beats it for red point sources. 

So what about the cosmology?  Well unfortunately we have not finished the data analysis
So I can not yet show you the cosmological conclusions we can reach yet, but I can give you some idea of
Our success in extending the Hubble diagram...

## Matching Shapes and Colors

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

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

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

**Notes:**
Before doing cosmology, we can compare the light curve shapes and colors
of SNe Ia to look for signs of systematics differences.
They are remarkably similar and totally consistent.

## The New SN Ia Hubble Diagram

- The New SN Ia Hubble Diagram

- 97ff

- 6 of the 7 highest redshift SNe Ia

**Notes:**
As you can see we have approximately doubled the well-observed redshift range of the Hubble diagram.
6 of the 7 highest redshift known

## Is Cosmic Acceleration Real?

- ?

**Notes:**
The first question we have considered is, is cosmic acceleration real,
That is, are Sne Ia tracking cosmology or astrophysical effects.
click
The results look very encouraging, the data is highly consistent with a mixed dark energy dark matter cosmology
Inconsistent with simple, monotonic dust or evolution
I think a more complex model of dust or evolution can always be constructed to match the data,
For example, if gray dust were emitted at the exact same rate the Universe expands and dilutes it
Could mimic a lambda cosmology, but this is not a natural explanation

## A Cosmic Jerk: Deceleration gave way to Acceleration, 

**Notes:**
The next question we have looked at is evidence for past deceleration.
A continualy coasting model is a bad fit to low z, but constant acceleration is
We need both acceleration (neg q0) and a positive dq/dz, this is exact
But we can also consider the next term in a taylor expansion, jerk which must be positive

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

**Notes:**
Joint constraints on q0 and dq/dz shows 99% confidence intervals live in
A presently accelerating, past decelerating region,
The redshift of the transition between the two is 0.3-0.6 or 5 Gyr ago
We also looked at other parameterizations

## (If the Dark Energy is Lambda), Updated Constraintsfactor of 7 improvement!

- Riess et al 1998; High-z Team

- New

**Notes:**
I also had a chance to recalculate constraints in the omega_M,omega_l space
The new constraints are about 5 times more precise than the ones either team published in 1998
There is a lot more we can do with this data and more like it in the future to understand the nature of dark energy

## Probing Dark Energy 

**We have doubled our knowledge of w****0**** 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?

**Notes:**
By observing sne over a wide range in redshift we can ...

## Closing in on Dark Energy: The Future

- Rejection of lambda:
- i.e.,                or
- would be a tremendous
- Breakthrough!
- GOODS has been an effective technology demonstrator for SNAP/JDEM

-   CFHT L,
- ESSENCE,
- Sloan DSS,
- Carnegie

**There should be another**
**8-12 Type Ia at z>1 in ~1 yr**
**time frame**

**Notes:**
I am confident we will continue to make progress if we
Keep trying...

## 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