1. — a VO test case? The Great Observatories Origins Deep Survey
A deep, multi-wavelength public survey to study the formation and evolution of galaxies and AGN
Bob Fosbury on behalf of the GOODS teams
STScI/ESO/ST-ECF/JPL/SSC/Gemini/Boston U./U. Ariz./ U. Fla./UCLA/UCSC/IAP/Saclay/Yale/AUI
See:
10 June 2002
GOODS & IVO

2. What is GOODS?
An orchestration of limiting observations of the HDF-N and the CDF-S regions (~ 300 square arcmin in total) with the most powerful telescopes over the widest wavelength range
30 times larger solid angle than HDF-N + HDF-S
Based on large programmes with SIRTF, HST, Chandra, Newton, VLT etc.
Producing datasets and derived products for the public domain
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GOODS & IVO

3. Primary science goals The mass assembly history of galaxies
Tracking the formation of the Hubble sequence
Census of energetic output from star formation and supermassive black holes
Measurements or limits on the discrete source component of the extragalactic background light (EBL)
Discovery of high-z supernovæ to explore the cosmic expansion
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GOODS & IVO

4. Science #1 The mass assembly of galaxies Aims:
Goal: to measure distribution function of stellar mass and star formation rates -> assembly via quiescent star formation, starbursts & mergers
IRAC observes restframe near-IR at high redshift, providing the best photometric measure of total stellar content
Aims:
Reach ~1 mag fainter than L* at z ~ 3
Reach ~L* at z ~ 5
Provide correspondingly deep optical
to near-IR data for SEDs, phot-z’s, M/L
Extensive spectroscopy to measure z’s,
spectral properties, calibrate phot-z’s
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GOODS & IVO

5. Science #2 Supermassive black holes in AGN
contribute to ‘energy budget’ at high z
may (re)ionize the IGM
may be an integral component of galaxy formation and evolution
Connection to bulge mass & evolution
Fueling through interactions/mergers
Relation to starbursts/ULIRGs
Seeds of early galaxy formation ?
Census of high redshift AGN hampered by lack of knowledge of population of obscured ‘type 2’ objects, especially at high z
Obscured AGN detectable in hard X-rays (Chandra, XMM-Newton) and (sometimes) radio
Dust-absorbed radiation is re-emitted at mid- and far-IR wavelengths
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GOODS & IVO

6. Starburst/AGN discrimination
Using broad-waveband SED and orientation to identify ‘ordinary’ AGN (obscured & unobscured) at the ‘QSO epoch’ (z > 2)
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GOODS & IVO

7. Science #3 The Extragalactic Background Light
EBL provides an integral record of emission, absorption and re-radiation of photons over cosmic history
Backgrounds may consist of discrete, cosmologically distributed sources + a possible diffuse/isotropic component
Goals:
Faint source counts and P(D) at 3–24 mm
Provide best measure of discrete source component to EBL (lower limit)
Compare to other measures of total EBL (COBE/DIRBE, IRTS, g-ray limits)
GOODS
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GOODS & IVO

8. Science #4 High z supernova search
Hubble ACS observations designed (time sequence of z-band exposures) to find ~12 Type 1 supernovæ 1.2<z<1.8
Critical epoch for exploring the dynamics of the cosmic expansion
Hubble time allocated to follow 6 SNe
P70 FORS2 proposal for spectroscopy of 3 SNe in CDF-S
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GOODS & IVO

9. GOODS sensitivity
10 June 2002
GOODS & IVO

10. Major components SIRTF Legacy Hubble Treasury ESO Large Program
PI: M Dickinson STScI
647 hours IRAC + MIPS
Hubble Treasury
PI: M Giavalisco STScI
398 orbits ACS
(+ existing WFPC2, NICMOS and STIS)
ESO Large Program
PI: C Cesarsky ESO
Imaging: 396 hours ISAAC, 40 hours WFI
Spectroscopy: proposals for complete low-res spectroscopy of ~ 6000 sources in CDF-S to R~25
(> 30 nights MOS already allocated to other programs in CDF-S)
10 June 2002
GOODS & IVO

11. Components cont. Chandra XMM-Newton VLA, ATCA, Merlin, WSRT
1 Msec on CDF-S & HDF-N
HDF-N to go to 2 Msec in CXO Cycle 3, — 5 Msec goal
XMM-Newton
500 ksec CDF-S; 225 ksec HDF-N
VLA, ATCA, Merlin, WSRT
Radio continuum imaging
KPNO, CTIO, Subaru, Gemini, Keck, Palomar, MMT
Optical/NIR imaging and spectroscopy
JCMT
SCUBA imaging of HDF-N
GALEX
UV imaging
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GOODS & IVO

12. IRAC 3.6 – 8 µm
MIPS 24 µm
(contingent on performance relative to GTO program)
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GOODS & IVO

13. SIRTF imaging
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GOODS & IVO

14. Schematic layout of GOODS fields
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GOODS & IVO

15. Chandra/SIRTF exposure maps
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GOODS & IVO

16. ACS layouts
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GOODS & IVO

17. ISAAC JHKs imaging of CDF-S
The tiles numbered in cyan were completed in period 68.
The yellow tiles are from a program by Giallongo et al.
Blue is EIS WFI field
10 June 2002
GOODS & IVO

18. SIRTF observations Component IRAC Deep IRAC Ultradeep MIPS
Nominal area
~300 arcmin2
~50 arcmin2
Exposure time per map position
23.6 h (47.2 h in overlap)
+46.5 h
(total 70.1/93.7 h)
10.4 h
Total time
409 h
99.3 h
139.2 h
Individual exposure time
200 s
30 s
Total dithers per map position
425
837
240
AOR information:
Map positions per AOR
2 x 2 1 2
Number of AORs 68 18 48
Total clock time per AOR
21653 s
19852 s
10442 s
Time per map position per AOR
5000 s
18600 s
4680 s
Dithers per map position 25 93 30
Repeats within each AOR
5 (6)
AOR repeats 17 9 4
Epochs per field / total
2 / 4
2 / 2
1 / 2
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GOODS & IVO

19. IRAC (3.6–8µm) simulations of HDF-N
Handbook PSF
100 hour exposure
Optimistic PSF
10 June 2002
GOODS & IVO

20. ACS observations (starting soon)
Four broad, non-overlapping filters:
F435W (B), F606W (V), F775W (i), & F850LP (z)
Exposures of 3, 2.5, 2.5, and 5 orbits, respectively
Five visits separated by about 45 days to search for high redshift supernovæ
Extended-source sensitivities only magnitudes shallower than WFPC2 HDF observations
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GOODS & IVO

21. Chandra: CDF-S and HDF-N
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GOODS & IVO

22. ISAAC & FORS, BVRIJHKs
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23. ISAAC number counts
Ks-band number counts from ~ 60 arcmin2 from ISAAC observations (red histogram)
Central 2 x 2 arcmin regions only (blue dotted histogram)
(Gilles Bergond 2002)
10 June 2002
GOODS & IVO

24. CDF-S: X, opt, NIR FORS-B,R, ISAAC-Ks, Chandra
Classification by opt. spect.
Type 2
QSO 2
Type 1
Galaxies
G.Hasinger, P.Rosati, J.Bergeron, V.Mainieri, G.Szokoly and the CDFS Team (2002)
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GOODS & IVO

25. CDF-S spectroscopy
Already have several hundred redshifts in CDF-S area (Cimatti, Rosati) — but mostly for specific types of object
GOODS proposes to do ‘complete’ low-res spectroscopy for ~ 6000 objects to RAB = 25
Using FORS2 for red sources (~ 560) and VIMOS for the remainder: needs nights
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GOODS & IVO

26. Data products
“All data and data products from GOODS Legacy program and its supporting observations will be made public and distributed as quickly as possible to enable community research.”
SIRTF data:
Raw and basic pipeline processed frames: available from SSC archive
Version 0.5 – best-effort reduced images (BCD-based or with limited reprocessing) 3 months after each campaign; mosaics if possible
Version 1.0 – full release of image data products and initial catalogs, 3 months after last campaign
Version 2.0 – final recalibrated data products and catalogs, 1 year after last campaign
Similar release schedule for Hubble and ESO data
ISAAC V0.5 was April 2002, V1.0 in July 2002 (thanks to EIS!)
See
10 June 2002
GOODS & IVO

27. GOODS and VO
What is the attraction of the GOODS project for the development of VO?
GOODS is not huge in data volume but it is extremely rich in complexity:
Multi-wavelength imaging with different PSFs
Resolution of confusion limits at long SIRTF ls
Complex mosaicing strategies
incorporation of geometric distortion corrections
Photometric quality control
catalogue production for different purposes
Multi-object spectroscopy
Number counts, P(D) for the EBL
Archiving of complex data products
i.e., it may make a useful prototype
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GOODS & IVO

28. Products from GOODS V0.5, V1 and V2 data products
Including photometric/astrometrically calibrated mosaics and catalogues
Catalogues extending beyond confusion limit (e.g., for MIPS)
Spectral catalogues and atlases
Colour composite images
Enhanced calibration files and models
Software developed as needed for the programme
Self-calibration; deconfusion; SED construction and analysis…
PR materials
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GOODS & IVO

29. Products to GOODS Tailored archive utilities …
e.g., for derived data products
housekeeping tools for complex datasets
cutout servers: multi-instrument image-based comparison tools …
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GOODS & IVO

30. What GOODS needs People
To pipeline process data, check quality, do photometric and astrometric calibration
To build and check catalogues
To develop dedicated s/w for special needs
To design and implement archive data structures and descriptions
To select sources and design MOS programmes …
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GOODS & IVO

31. What the science user needs
A scientific objective
An accessible, easy to navigate, archive
Clear, complete and trustworthy descriptions of the contents
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GOODS & IVO

32. …so, is GOODS a good VO test case?
The GOODS teams are obliged to structure and describe the data and the derived products
The archives will be tailored by collaboration between the teams and the archive providers
Which part of this process do we call the VO?
10 June 2002
GOODS & IVO