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MLDC – Round 2

MLDC – Round 2

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MLDC – Round 2

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  1. MLDC – Round 2 John Baker(NASA/GSFC) For the MLDC Task Force- K. A. Arnaud, S. Babak, J. B., M. J. Benacquista, N. J. Cornish, C. Cutler, L. S. Finn, S. L. Larson, E. Porter,B. S. Sathyaprakash, M. Vallisneri, A. Vecchio, J-Y. Vinet LIST MLDC F2F -Potsdam December 16, 2006

  2. MLDC Round 2 overview • Objective: Global LISA-data analysis • LISA will see many types of sources, overlapping in time and/or freq. • Round 1 has: • Established standards, codes, tools and experience for measuring several source classes independently • Provided a demonstration of readiness for data analysis on a source-by-source basis. • Round 2 will: • Utilize standards, codes, tools and experience from Round 1. • Establish experience in integrated global analysis, including full-scale galactic model. • Demonstrate readiness for integrated global analysis.

  3. Round 2 Overview • Challenge 2.1 - Galactic Foreground • The galaxy: a synthesized population of galactic binaries • ~ 30 Million sources • Challenge 2.2 – “The Whole Enchilada” • Synthesized population of galactic binaries • Verification binaries • Between 4 to 6 signals from MBHBs • 5 EMRI signals • LISA Model • 2 years data • Otherwise identical to Round 1

  4. MLDC Round 2 Challenge • Round 2 Resources • Data sets released on • AstroGravS website: http://astrogravs.nasa.gov/docs/mldc • Each challenge includes • A training data set with an answer key • A blind challenge data set • Updated MLDC Challenge 2 specification document • Helpful Codes Available • Available at sourceforgehttp://svn.sourceforge.net/viewvc/lisatools/ • Source/Simulator codes largely unmodified from Round 1 • Pipeline for regenerating Round 2-like data sets will be available • New FastGalaxy code for Galaxy realization (executable only) • The code to be used for evaluation/analysis will be available ~April-May

  5. Round 2 Sources • Galactic Binaries  Galaxy • Galaxy Model • Base galaxy model from Gijs Nelemans (Nelemans, Yungelsen, Zwart, 2001) • Partly randomized • Orientation • Phase • Small frequency perturbations • Plus 20 Verification binaries (2.2) • 5 real (Nelemans), 15 invented • Same as Round :. Approximate parameters provided • Each binary • Same as Round 1: Non-chirping (df/dt=0)

  6. Round 2 Sources • SMBH Binaries • Model (same as Round 1) • Non-spinning • Restricted 2PN waveforms • Tapered near merger. • Challenge 2.2 signals will include • A very loud (SNR ~ 2000) signal • in-spiral “in band” (min 1 week above 0.1 mHz) • coalescing T=3+/- 1 month after the beginning of data • A moderate-to-low SNR (~ 20) signal • Coalescence 1-2 months after end of data (T=25—26 mo.) • Challenge 2.2 signals may also include (choose 2—4 ) • A signal with SNR ~ 1000, T=6—24 mo. • A signal with SNR ~ 200, T=6—24 mo. • A signal with SNR ~ 100, T=18—21 mo. • A low signal with SNR ~ 10, T=27—28 mo.

  7. Round 2 Sources • EMRIs • 1.3 (Full-year challenge: Ends concurrently with Round 2) • Barack-Cutler “Kludge”-waveform (code provided) • 5 Examples with 30 < SNR < 100 • Parameters • SMBH mass : 0.95 < M / (106 MSun) < 1.05 • SMBH spin: 0.5 < a/m < 0.7 • Captured mass: 9.5 < M / MSun < 10.5 • Eccentricity: 0.15 < e < 0.25 • Duration: 1 < d < 2 years • 2.2 • Same as parameters as 1.3, but: • 2 with masses near 10^6 solar mass • 2 with masses near 5x10^6 solar mass • 1 with mass near 10^7 solar mass

  8. MLDC Round 2 Draft Data

  9. Results evaluation and reporting • Assessment plan • Stronger validation objective than Round 1: • More formal process evaluation process. • Analysis plan/code predetermined • Returned results should meet protocol • To be based on Round 1 experience. • New issues: • Global assessment • Source-by-source assessment for partial fits (e.g. SMBH only) • Galactic Binary focus zones: • Four narrow frequency bands near 0.3, 1, 3, and 6 mHz • Assessment codes: • Available before challenge end • Groups can self-check: correct conventions, formats, etc • Reporting • Presentation at Amaldi meeting in July • Peer-review publication submitted shortly thereafter.

  10. Future Challenge Rounds • Planned through 2008 • Evolving challenge content plan: • http://www.tapir.caltech.edu/dokuwiki/listwg1b:challenges3 • New sources classes • Bursts • Stochastic backgrounds • Increased source model realism • MBHB with NR-inspired merger-ringdowns, and spins • Chirping galactic binaries • Broader class of EMRIs • Increased noise realism • Data gaps • Non-gaussianity • Non-stationarity

  11. Summary • MLDC Round 2 objective: Global data analysis • Sources: Galaxy of binaries, 4-6 SMBHs, 5 EMRIs • Timeline: • Jan 8: Data Sets released • Jan: Challenge 2 document • April-May: Assessment code complete/released • June 15: Results returned • July: Presentation at Amaldi meeting • ~August: results submitted for publication. • Future Challenge rounds to follow • You are invited to participate: • For more information…http://astrogravs.nasa.gov:http://www.tapir.caltech.edu/dokuwiki/listwg1b:home