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Round 1B - Data Sets
Round 1B is now compeleted The key files linked below. You can see the submissions here
Round 1B is a re-issue of the Round 1 challenges to provide new groups an
opportunity to develop their codes, while experienced groups work to improve their algorithms.
Though the sources are drawn from the same distributions as in Round 1, the codes used to generate the datasets are those of Round2. Round 1B will terminate
in December 2007. Submit your results here.
For further information about the challenges, see the
MLDC How-to produced
for round 2.
Challenge 1B.1 - Galactic White Dwarf Binaries
Challenge 1B.1.1 - Single Galactic Binaries
- a) 1 year of Gaussian stationary instrument noise + 1 exactly monochromatic WD with SNR ~10 ->20 over 1 year (for single IFO) at frequency 1.0+/-.1 mHz
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- b) 1 year of Gaussian stationary instrument noise + 1 exactly monochromatic WD with SNR ~10 -> 20 over 1 year (for single IFO) at frequency a 3.0+/-.1 mHz
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- c) 1 year of Gaussian stationary instrument noise + 1 exactly monochromatic WD with SNR ~10 -> 20 over 1 year (for single IFO) at frequency a 10+/-1 mHz
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Challenge 1B.1.2 - Verification Binaries 1 year of
Gaussian stationary instrument noise with 5 true verification
binaries (parameters chosen according to our current best guess)
+ 20 mock verification binaries in the frequency range 0.5 mHz -
12 mHz. All the signals will be monochromatic (no fdot). Since
these are verification binaries, the sky locations and orbital
frequencies are given (here). The
orientation parameters and distances will be considered unknown.
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Challenge 1B.1.3 - Resolvable Binaries
1 year of Gaussian stationary instrument noise with 20 resolvable binaries (parameters chosen from the BLT population synthesis code) with frequencies spread over the LISA band. All the signals will be monochromatic (no fdot).
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Challenge 1B.1.4 - Source Confusion
1 year of Gaussian stationary instrument noise with 40 < N < 60 WD binaries chosen with frequencies f in a narrow band ( 3.000 mHz < f < 3.015 mHz ) and with SNR > 5. Sources are drawn from the BLT population synthesis code. All the signals will be monochromatic (no fdot). The number of sources will not be given.
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Challenge 1B.1.5 - Strong Source Confusion
1 year of Gaussian stationary instrument noise with 30 < N < 50 WD binaries chosen with frequencies f in a very narrow band ( 2.9985 mHz < f < 3.0015 mHz ) and with SNR > 5. Sources are drawn from the BLT population synthesis code. All the signals will be monochromatic (no fdot). The number of sources will not be given.
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Challenge 1B.2 - MBH Binaries
Challenge 1B.2.1
1 year of Gaussian stationary instrument noise + 1 Schwarzschild SMBH binary with time to coalescence 6(+/-1) months and masses m1 1-5 million solar masses and m2 = m1/x, where 1 < x < 4 . The signals have SNR for one IFO in the range 450 < SNR < 500 . The waveform model for the inspiral is restricted to the 2PN approximation with no spin-orbit nor spin-spin modultations.
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Challenge 1B.2.2
1 year of Gaussian stationary instrument noise + 1 Schwarzschild SMBH binary with time to coalescence 400+/-40 days and masses m1 1-5 million solar masses and m2 = m1/x, where 1 < x < 4 . The signals have SNR for one IFO in the range 20 < SNR < 100 . The waveform model for the inspiral is restricted to the 2PN approximation with no spin-orbit nor spin-spin modultations.
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Challenge 1B.3 - EMRIs
Each of the 5 elements of Challenge 1B.3 includes precisely one EMRI source in a ~2-yr long (to be precise: 2^22 data points with cadence 15 seconds) data set. For each case, the EMRI parameters more reduced mass, spin of the central black hole, eccentricity and duration are drawn as follows: mu/M in U[9.5, 10.5], S/M2 in U[0.5, 0.7] time at plunge in U[2^21, 2^22] x 15 sec, and eccentricity at plunge in U[0.15, 0.25]. The mass of the central black hole varies.
Challenge 1B.3.1
Central mass M/10^7 in U[0.95, 1.05] solar masses. Est SNR in U[40,110].
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Challenge 1B.3.2
Central mass M/10^6 in U[4.75, 5.25] solar masses. Est SNR in U[70,110].
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Challenge 1B.3.3
Central mass M/10^6 in U[4.75, 5.25] solar masses. Est SNR in U[40,60].
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Challenge 1B.3.4
Central mass M/10^6 in U[0.95, 1.05] solar masses. Est SNR in U[70,110].
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Challenge 1B.3.5
Central mass M/10^6 in U[0.95, 1.05] solar masses. Est SNR in U[40,60].
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