1. VO activities at CfA G. Fabbiano (Harvard-Smithsonian Center for Astrophysics) With contributions from: Aneta Siemiginowska, Margarita Karovska, Doug Mink, Alyssa Goodman and the entire CfA NVO Team Harvard College Observatory Smithsonian Astrophysical Observatory

2. Chandra Hubble MMT Sub-mm array VLA The Harvard-Smithsonian Center for Astrophysics A natural place for VO activities The largest single astrophysical center in the USA Radio through gamma-rays waveband expertise: ground-based and space Solar system through cosmology areas of research: observational and theory Antartica sub-mmMagellan 6.5m Whipple  -ray SIRTF Oak Ridge 1.2m CO

3. HEAD (The X-ray Group) –Legacy: UHURU, HEAO-1, Einstein, ROSAT –Chandra X-ray Center (CXC) Supports all phases of the Chandra mission Processing, archival, and distribution of data Chandra user support (http://cxc.harvard.edu/)http://cxc.harvard.edu/ –ADS (in collaboration with Optical-IR) Bibliography search engine (http://adswww.harvard.edu/)http://adswww.harvard.edu/ Data Center & Service Expertise at CfA

4. CfA and NASA Data Centers SAO is a partner in HEASARC with NASA-GSFC CXC and ADS are members of NASA ADEC (Astro. Data centers Executive Committee) ADEC scope is to further VO-like connections between NASA archives and data services –ADS – data links implemented with MAST (STScI), CXC, IRSA –Wider inter-archive operability is in the works see Tom McGlynn’s talk

5. Established –Chandra Data Archive (CDA) –OIR Data Archive (Harvard and SAO ground based telescopes): Telescope Data Center (TDC) Soon to come –Sub-mm –Radio –COMPLETE Data Archives at CfA

6. Chandra Data Archive Contains all Chandra telemetry and processed data products (proprietary and public) Current data product volume is 1.3 TB Mirror site in UK (Leicester) Access through CXC S&R interface (ChaSeR and WebChaSeR) and via HEASARC

7. The CXC/X-ray Community Data Approach leading to VO-ready archives Uniform pipeline processing of all data see poster by Evans et al –Aspect correction, filtering (e.g. hot pix removal), coadding frames, source properties Well-defined data product levels –Each level depends only on data in preceding level Adoption of standard data formats –HEASARC FITS conventions; event files Separate tracked calibration information –HEASARC CALDB, expanded for Chandra Chandra L3 processing will produce source-based archival information

8. X-ray multi-mission analysis software Moving towards a VO analysis tool-kit –FTOOLS (GSFC), CIAO (CXC) –Mix and match tool-boxes –FTOOLS operate on FITS files –CIAO uses Chandra Data Model I/O –FTOOLS and CIAO tools can be used in single analysis session Freely available on the Web On line manuals, tutorial and documentation CIAO web page is http://cxc.harvard.edu/ciao/ http://cxc.harvard.edu/ciao/

9. The Chandra Data Model (CDM) CDM was developed (see J. McDowell’s talk) –To handle different format & multi-mission data Different X-ray missions Non X-ray data –Data filtering and extraction From user-defined regions in any data hypercube axis –Data subspace Information on what was done to the data is carried by the data

10. CIAO +CDM Operate on any data axis or combination (e.g. X, Y, time, spectrum) –Example: modelling spatial distribution of X-ray cluster (Sherpa) Data Model Residuals Adaptively smoothed residuals

11. CIAO + CDM Multi-mission / multi wave- band analysis –Optical-X-ray spectrum –Red line is Sherpa fit

12. CIAO +CDM+DS9 Eta Car X-rays: Chandra Choose your wavelength band multi-color images

13. CIAO +CDM+DS9 Eta Car Radio: VLA Choose your wavelength band multi-color images

14. CIAO +CDM+DS9 Eta Car Optical: HST Choose your wavelength band multi-color images

15. CIAO +CDM+DS9 Eta Car Choose your wavelength band multi-color images Radio + Optical +X-rays

16. The TDC maintains archives of spectroscopic data from SAO telescopes (http://tdc-www.harvard.edu/)http://tdc-www.harvard.edu/ Uniform pipeline processing is performed before inclusion in TDC Public access and proprietary data policy is under discussion –Z-Machine: all 27,171 spectra (Aug 78 –Sep 93) on line and searchable by position, name, reduced file number (http://tdc-www.harvard.edu/zmach/minkd.html)http://tdc-www.harvard.edu/zmach/minkd.html –FAST: 5,400/88,166 spectra (Jan 94 – now) public. The rest awaits policy decision (processed) (http://tdc-www.harvard.edu/fast/tokarzs.html)http://tdc-www.harvard.edu/fast/tokarzs.html

17. –7,026 Z-Machine and 4,488 FAST spectra accessible through Updated Zwicky Catalog search page –MMT Blue Channel Spectrograph: 8,784 spectra (Oct 80 –Oct 94) archived but not released. –Echelle data (archived but not released): Oak Ridge: 120,559 spectra (from Jul 82) Whipple: 69,008 spectra (from Dec 88) MMT: 24,507 spectra (Ap 81 – Jan 98)

22. Digitizing the Harvard Plate Collection 400,000 glass photographic plates Northern and Southern emisphere 104 year coverage: 1885 – 1989 Trial scanning of 100 plates (8x10 in) this summer (2002) Uncompressed data volume ~80 TB M44

23. COMPLETE, Part 1 A. Goodman Observations:  Mid- and Far-IR SIRTF Legacy Observations: dust temperature and column density maps ~5 degrees mapped with ~15" resolution (at 70  m)  NICER/2MASS Extinction Mapping: dust column density maps, used as target list in HHT & FCRAO observations + reddening information ~5 degrees mapped with ~5' resolution  HHT Observations: dust column density maps, finds all "cold" source ~20" resolution on all A V >2”  FCRAO/SEQUOIA 13 CO and 13 CO Observations: gas temperature, density and velocity information ~40" resolution on all A V >1 Science:  Combined Thermal Emission (SIRTF/HHT) data: dust spectral-energy distributions, giving emissivity, T dust and N dust  Extinction/Thermal Emission inter-comparison: unprecedented constraints on dust properties and cloud distances, in addition to high-dynamic range N dust map  Spectral-line/N dust Comparisons Systematic censes of inflow, outflow & turbulent motions will be enabled—for regions with independent constraints on their density.  CO maps in conjunction with SIRTF point sources will comprise YSO outflow census 5 degrees (~tens of pc) SIRTF Legacy Coverage of Perseus

24. Un(coordinated) Molecular-Probe Line, Extinction and Thermal Emission Observations Molecular Line Map Nagahama et al. 1998 13 CO (1-0) Survey Lombardi & Alves 2001Johnstone et al. 2001

25. COMPLETE, Part 2 Observations, using target list generated from Part 1:  NICER/8-m/IR camera Observations: best density profiles for dust associated with "cores". ~10" resolution  SCUBA Observations: density and temperature profiles for dust associated with "cores" ~10" resolution  FCRAO+ IRAM N 2 H + Observations: gas temperature, density and velocity information for "cores” ~15" resolution Science:  Multiplicity/fragmentation studies  Detailed modeling of pressure structure on <0.3 pc scales  Searches for the "loss" of turbulent energy (coherence) FCRAO N 2 H + map with CS spectra superimposed. (Lee, Myers & Tafalla 2001).

26. CfA Participation in theVO Member of the `Large' NSF proposal team -SAO leads Data Model effort (J. McDowell) - SAO participates in metadata (A. Rots) and testbed (I. Evans, M. Noble) Awarded NSF `medium’ grant CfA team with AAVSO (Janet Mattei) and BU (Tania Szlateva) participation - CfA collaborators: RG (Alyssa Goodman), OIR (Bob Kirshner, Mike Kurtz), HEAD (Pepi Fabbiano, Arnold Rots, Jonathan McDowell, Ian Evans, Mike Noble, Janet DePonte Evans, Martin Elvis), SED (Phil Sadler) Membership in the NASA-NSF NVO SDT - Roger Brissenden, Pepi Fabbiano Membership in the AVO science working group

27. CfA Participation in theVO Design Data Model(DM) Participate in large NVO testbed (CDA) Build a CfA prototype to validate our VO development Federate CfA Archives (in order of readiness) - Chandra Data Archive (CDA) - OIR/MMT - TRACE (solar high res. X-ray images) - Radio (COMPLETE, CO galactic plane survey) Link Archive with ADS (implemented in CDA) Include AAVSO data in the federation Implement CfA DM and QM layers Build simple User Interface Build simple EPO Interface CfA prototype will be available to the VO

28. CfA NVO Focus: the VO Data Model Object Oriented model of the sky and of the archives, to support: - query language that translates astronomical queries into database queries - extraction mechanism allowing user-specified filters and format, while preserving coordinate information - preservation of calibration - generalized analysis tools, independent of data domain - strongly linked data analysis - archive connection see Jonathan McDowell’s talk this afternoon Chandra Data Model provides starting-point experience

29. CfA NVO Testbed and Prototype

30. 1.Query i/f: translates user’s query into QML (Query Model Language) and dispatches grid search 2.Exploders resolve query into subqueries and dispatch them in grid 3.An SSE (Site Specific Translator) at each targeted archive receives and translates query into mission-specific LQM (Local Query Model) to generate request 4.Archival data are retrieved and via SSE pipeline and translated from LDM (Local Data Model format) to DMP (Data Model Protocol) compliant format 5.GDFs (Generic Data Filters) process DMP data from subqueries and Data Fusers concatenate data for return to the DAL (Data Access Layer)

31. VO: Creating the Future of Astrophysics Data Analysis Territory covered by CfA VO prototype and testbed

32. How do we proceed? CfA multi-wavelength VO team gives input to DM and QM design Input is shared with entire VO community and vice-versa Design will be tested via prototypes/demos that will exercise key threads through the CfA testbed A successive approximation approach will be applied to get to the final working system (this method was used successfully to build the CXC Data System)