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— a VO test case?

— 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

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— a VO test case?

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  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: • www.stsci.edu/science/goods/ • www.eso.org/science/goods/ 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 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 GOODS & IVO

  4. Science #1 • The mass assembly of galaxies • 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 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 GOODS & IVO

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

  9. GOODS sensitivity GOODS & IVO

  10. Major components • SIRTF Legacy • 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) GOODS & IVO

  11. Components cont. • Chandra • 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 GOODS & IVO

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

  13. SIRTF imaging GOODS & IVO

  14. Schematic layout of GOODS fields GOODS & IVO

  15. Chandra/SIRTF exposure maps GOODS & IVO

  16. ACS layouts GOODS & IVO

  17. 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 ISAAC JHKs imaging of CDF-S GOODS & IVO

  18. SIRTF observations GOODS & IVO

  19. Handbook PSF 100 hour exposure Optimistic PSF IRAC (3.6–8µm) simulations of HDF-N 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 0.5-0.8 magnitudes shallower than WFPC2 HDF observations GOODS & IVO

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

  22. ISAAC & FORS, BVRIJHKs GOODS & IVO

  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) 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) 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 10 + 13 nights 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 www.eso.org/science/goods/ 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 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 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 • … 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 • … 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 GOODS & IVO

  32. 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? …so, is GOODS a good VO test case? GOODS & IVO

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