VO activities at CfA

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

2. 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 Chandra Whipple g-ray Oak Ridge 1.2m CO MMT SIRTF Hubble VLA Sub-mm array Antartica sub-mm Magellan 6.5m

3. Data Center & Service Expertise at CfA • 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/) • ADS (in collaboration with Optical-IR) • Bibliography search engine(http://adswww.harvard.edu/)

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 workssee Tom McGlynn’s talk

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

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 (ChaSeRand 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 ishttp://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 Model Data • Operate on any data axis or combination (e.g. X, Y, time, spectrum) • Example: modelling spatial distribution of X-ray cluster (Sherpa) Adaptively smoothed residuals Residuals

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

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

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

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

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

16. The TDC maintains archives of spectroscopic data from SAO telescopes (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) • FAST: 5,400/88,166 spectra (Jan 94 – now) public. The rest awaits policy decision (processed)(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 M44 • 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

23. 5 degrees (~tens of pc) SIRTF Legacy Coverage of Perseus COMPLETE, Part 1A. 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 AV>2” FCRAO/SEQUOIA 13CO and 13CO Observations: gas temperature, density and velocity information ~40" resolution on all AV>1 Science: Combined Thermal Emission (SIRTF/HHT) data: dust spectral-energy distributions, giving emissivity, Tdust and Ndust Extinction/Thermal Emission inter-comparison: unprecedented constraints on dust properties and cloud distances, in addition to high-dynamic range Ndust map Spectral-line/Ndust 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 YSOoutflow census

24. Molecular Line Map 2MASS/NICER Extinction Map of Orion Johnstone et al. 2001 Johnstone et al. 2001 Nagahama et al. 1998 13CO (1-0) Survey Un(coordinated) Molecular-Probe Line, Extinction and Thermal Emission Observations Lombardi & Alves 2001

25. FCRAO N2H+ map with CS spectra superimposed. COMPLETE, Part 2 (Lee, Myers & Tafalla 2001). 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 N2H+ 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)

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’ grantCfA 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 connectionsee Jonathan McDowell’s talk this afternoon Chandra Data Model provides starting-point experience

29. CfA NVO Testbed and Prototype

30. CfA NVO Testbed and Prototype • Query i/f: translates user’s query into QML (Query Model Language) and dispatches grid search • Exploders resolve query into subqueries and dispatch them in grid • An SSE (Site Specific Translator) at each targeted archive receives and translates query into mission-specific LQM (Local Query Model) to generate request • Archival data are retrieved and via SSE pipeline and translated from LDM (Local Data Model format) to DMP (Data Model Protocol) compliant format • 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)