Harvard College Observatory Smithsonian Astrophysical Observatory VO activities
Harvard College Observatory Smithsonian Astrophysical Observatory VO activities at Cf. A G. Fabbiano (Harvard-Smithsonian Center for Astrophysics) With contributions from: Aneta Siemiginowska, Margarita Karovska, Doug Mink, Alyssa Goodman and the entire Cf. A NVO Team
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. 2 m CO SIRTF Hubble MMT VLA Sub-mm array Antartica sub-mm Magellan 6. 5 m
Data Center & Service Expertise at Cf. A • 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/)
Cf. A 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 (STSc. I), CXC, IRSA – Wider inter-archive operability is in the works see Tom Mc. Glynn’s talk
Data Archives at Cf. A • 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
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 (Cha. Se. R and Web. Cha. Se. R) and via HEASARC
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 L 3 processing will produce source-based archival information
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/
The Chandra Data Model (CDM) • CDM was developed (see J. Mc. Dowell’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
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 Residuals Model Adaptively smoothed residuals
CIAO + CDM • Multi-mission / multi waveband analysis – Optical-X-ray spectrum – Red line is Sherpa fit
CIAO +CDM+DS 9 • Choose your wavelength band multi-color images Eta Car X-rays: Chandra
CIAO +CDM+DS 9 • Choose your wavelength band multi-color images Eta Car Radio: VLA
CIAO +CDM+DS 9 • Choose your wavelength band multi-color images Eta Car Optical: HST
CIAO +CDM+DS 9 • Choose your wavelength band multi-color images Eta Car Radio + Optical +X-rays
• 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)
– 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)
Digitizing the Harvard Plate Collection M 44 • 400, 000 glass photographic plates • Northern and Southern emisphere • 104 year coverage: 1885 – 1989 • Trial scanning of 100 plates (8 x 10 in) this summer (2002) • Uncompressed data volume ~80 TB
5 degrees (~tens of pc) COMPLETE, Part 1 A. Goodman Observations: SIRTF Legacy Coverage of Perseus Mid- and Far-IR SIRTF Legacy Observations: dust temperature and column density maps ~5 degrees mapped with ~15" resolution (at 70 m) NICER/2 MASS 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 13 CO and 13 CO 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 YSO outflow census
Nagahama et al. 1998 13 CO (1 -0) Survey Un(coordinated) Molecular-Probe Line, Extinction and Thermal Emission Observations Molecular Line Map 2 MASS/NICER Extinction Map of Orion Johnstone et al. 2001 Lombardi & Alves 2001 Johnstone et al. 2001
(Lee, Myers & Tafalla 2001). COMPLETE, Part 2 FCRAO N 2 H+ map with CS spectra superimposed. 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)
Cf. A Participation in the. VO • Member of the `Large' NSF proposal team -SAO leads Data Model effort (J. Mc. Dowell) - SAO participates in metadata (A. Rots) and testbed (I. Evans, M. Noble) • Awarded NSF `medium’ grant Cf. A team with AAVSO (Janet Mattei) and BU (Tania Szlateva) participation - Cf. A collaborators: RG (Alyssa Goodman), OIR (Bob Kirshner, Mike Kurtz), HEAD (Pepi Fabbiano, Arnold Rots, Jonathan Mc. Dowell, Ian Evans, Mike Noble, Janet De. Ponte Evans, Martin Elvis), SED (Phil Sadler) • Membership in the NASA-NSF NVO SDT - Roger Brissenden, Pepi Fabbiano • Membership in the AVO science working group
Cf. A Participation in the. VO • Design Data Model(DM) • Participate in large NVO testbed (CDA) • Build a Cf. A prototype to validate our VO development • Federate Cf. A 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 Cf. A DM and QM layers • Build simple User Interface • Build simple EPO Interface • Cf. A prototype will be available to the VO
Cf. A 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 Mc. Dowell’s talk this afternoon • Chandra Data Model provides starting-point experience
Cf. A NVO Testbed and Prototype
Cf. A NVO Testbed and Prototype 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)
VO: Creating the Future of Astrophysics Data Analysis Territory covered by Cf. A VO prototype and testbed
How do we proceed? Cf. A 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 Cf. A 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)
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