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on the LISA computational infrastructure


The Gravitational Lens (from Penn State)

Matters of Gravity

→ LIGO Newsletter (access through

LISA conferences:

4th LISA Symposium

5th LISA Symposium

6th LISA Symposium



Scoping out LISA data analysis (AEI-MPI, March 2004)

list of conferences (from ESA website)

LISA literature:

Shane's Penn State LISA discussion group

partial TDI bibliography

a bibliography on LISA data analysis for binaries and the LISA response

LISA software:

The LISA Simulator

The LISA Calculator

LSC MatApps

LISA policy:

ESA LISA Data Analysis Study

Aug 21, 2008

home (/lisa)
2008-08-21, 16:13 [edit] Michele's wikiblog

Back to conferences


Conference website

Selected plenary lectures

Stan Whitcomb: ground-based GW

Steve McMillan: gravitational dynamics of large stellar systems

Laurent Freidel: non-string quantum gravity

Bernd Bruegmann: numerical relativity -- the two body problem

Daniel Eisenstein: observing dark energy

Peter Schneider: cosmological probes by gravitational lensing

Francis Everitt: GPB

Daniel Shaddock: LISA

Robert Myers: quark soup al dente

Selected parallel sessions

GRG relativistic astrophysics

Amaldi GW part 1

Amaldi GW part 2

Amaldi LISA

Jul 16, 2007

amaldi2007 (/lisa)
2007-07-16, 15:25 [edit]

A partial TDI bibliography

Check the chronological order of apparition (not publication). Which are in the Rosetta stone?


M. Tinto and J. W. Armstrong, "Cancellation of Laser Noise in an Unequal-Arm Interferometer Detector of Gravitational Radiation", Phys. Rev. D 59, 102003 (1999). PRD

J. W. Armstrong, F. B. Estabrook, and M. Tinto, "Time-Delay Interferometry for Space-Based Gravitational Wave Searches", Astrophys. J. 527, 814 (1999). ApJ


F. B. Estabrook, M. Tinto, and J. W. Armstrong, "Time-Delay Analysis of LISA Gravitational Wave Data: Elimination of Spacecraft Motion Effects", Phys. Rev. D. 62, 042002 (2000). PRD


M. Tinto, J. W. Armstrong, and F. B. Estabrook, "Discriminating a Gravitational Wave Background from Instrumental Noise in the LISA Detector", Phys Rev. D. 63, 021101(R) (2001). PRD

J. W. Armstrong, F. B. Estabrook, and M. Tinto, "Sensitivities of Alternate LISA Configurations", Class. Quantum Grav. 18, 4059 (2001). CQG


M. Tinto, F. B. Estabrook, and J. W. Armstrong, "Time-Delay Interferometry for LISA", Phys. Rev. D 65, 082003 (2002). PRD

S. V. Dhurandhar, K. Rajesh Nayak, and J.-Y. Vinet, "Algebraic Approach to Time-Delay Data Analysis for LISA", Phys. Rev. D. 65, 102002 (2002). PRD

T. A. Prince, M. Tinto, S. L. Larson, and J. W. Armstrong, "The LISA Optimum Sensitivity", Phys. Rev. D 66, 122002 (2002). PRD


J. W. Armstrong, F. B. Estabrook, and M. Tinto, "Time Delay Interferometry", Class. Quantum Grav. 20, S283 (2003). CQG

N. J. Cornish and R. W. Hellings, "The Effects of Orbital Motion on LISA Time Delay Interferometry", Class. Quantum Grav. 20, 4851 (2003). CQG

Show that modified-TDI Michelson-type observables cancel noise in rotating configurations; verify that first-generation Sagnac-type observables don't; propose 12-link Sagnac-type observables that do (including zeta); point out problem with modified-TDI Michelson-type in flexing configurations.

M. Tinto, D. Shaddock, J. Sylvestre, and J. W. Armstrong, "Implementation of Time Delay Interferometry for LISA", Phys Rev. D. 67, 122003 (2003). PRD

D. A. Shaddock, M. Tinto, F. B. Estabrook, and J. W. Armstrong, "Data Combinations Accounting for LISA Spacecraft Motion", Phys. Rev. D 68, 061303(R) (2003). PRD

Discuss laser-noise cancellation problems with first-generation TDI in rotating and flexing configurations; define second-generation TDI Michelson-type and quasi-second-generation TDI Sagnac-type observables.

F. B. Estabrook, J. W. Armstrong, M. Tinto, and W. Folkner, "SyZyGy: A Straight Interferometer for Gravity Wave Detection", Phys. Rev. D 68, 062001 (2003). PRD

J. Sylvestre and M. Tinto, "Noise characterization for LISA", Phys. Rev. D 68, 102002 (2003). PRD

K. Rajesh Nayak, S. V. Dhurandhar, A. Pai, and J.-Y. Vinet, "Optimizing the directional sensitivity of LISA", Phys. Rev. D 68, 122001 (2003) PRD


D. A. Shaddock, "Operating LISA as a Sagnac interferometer," Phys. Rev. D 69, 022001 (2004). PRD

Discuss problem of Sagnac-type observables in rotating configurations; propose 12-link alpha-type observables that do.

M. Tinto, F. B. Estabrook, and J. W. Armstrong, "Time delay interferometry with moving spacecraft arrays," Phys. Rev. D 69, 082001 (2004). PRD

Extend second-generation TDI to all other six-oriented-arm observables, and to zeta.

A. Królak, M. Tinto, and M. Vallisneri, "Optimal filtering of the LISA data", Phys. Rev. D 70, 022003 (2004). PRD

M. Tinto and S. L. Larson, "LISA time-delay interferometry zero-signal solution: Geometrical properties", Phys. Rev. D 70, 062002 (2004). PRD

D. A. Shaddock, B. Ware, R. E. Spero, and M. Vallisneri, "Post-processed time-delay interferometry for LISA", Phys. Rev. D 70, 081101(R) (2004) PRD


D. Summers and D. Hoyland, "Results from the LISA phase measurement system project," Class. Quantum Grav. 22 S249 (2005). CQG

M. Vallisneri, "Synthetic LISA: Simulating Time Delay Interferometry in a Model LISA", Phys. Rev. D 71, 022001 (2005). PRD

M. Tinto, M. Vallisneri, and J. W. Armstrong, ‘TDIR: Time-Delay Interferometric Ranging for space-borne gravitational-wave detectors’, Phys. Rev. D 71, 041101(R) (2005). PRD

M. Vallisneri, ‘Geometric Time Delay Interferometry’, Phys. Rev. D 72, 042003 (2005). PRD

B. Chauvineau, T. Regimbau, J.-Y. Vinet, and S. Pireaux, "Relativistic analysis of the LISA long range optical links", Phys. Rev. D 72, 122003 (2005). PRD

M. Tinto and S. V. Dhurandhar, "Time-Delay Interferometry", Living Rev. Relativity 8, 4 (2005). Living Reviews

Mar 29, 2007

tdibib (/lisa)
2007-03-29, 19:45 [edit]

A bibliography on LISA data analysis for binaries and on the LISA response

Back to LISA and GWs


T. A. Moore and R. W. Hellings, "Angular resolution of space-based gravitational wave detectors", Phys. Rev. D, 65, 062001 (2002). PRD

Explores the angular resolution of space-based detectors of gravitational waves. In the long-wavelength approximation (similar to Cutler's, but for a single interferometric combination), using a "least-squares" approach that is essentially the Fisher formalism.


N. J. Cornish and S. L. Larson, "LISA data analysis: Doppler demodulation", Class. Quantum Grav. 20, S163 (2003). CQG

Discusses the detection of simple monochromatic sources as peaks in power after Doppler demodulation (but no amplitude demodulation), which is obtained in the frequency domain by a simple approximate mapping between Fourier coefficients (this mapping depends on source frequency, though). Shows effect of demodulating with the wrong sky position, and of overlapping-source interference. Cutler LISA response is assumed.

R. W. Hellings, "LISA data analysis: the detection and initial guess problems for monochromatic binaries", Class. Quantum Grav. 20, 1019 (2003). CQG

Discusses providing initial monochromatic-signal parameters as input to "least-squares" (essentially, maximum likelihood, a la Moore and Hellings) parameter-estimation procedure, by way of peak finding after Doppler demodulation, which is achieved in the time domain.

N. J. Cornish and L. J. Rubbo, "LISA response function", Phys. Rev. D 67, 022001 (2003). PRD

Derives the LISA response by integrating the GW strain along the photon trajectories, using a hybrid time-frequency approach that emphasizes the transfer function. Obtains also static (stationary LISA s/c) and long-wavelength limits of the expression. Describes the Keplerian orbits used in the LISA Simulator and in pseudo-LISA.

N. J. Cornish and S. L. Larson, "LISA data analysis: Source identification and subtraction", Phys. Rev. D 67, 103001 (2003). PRD

Lays out gCLEAN, a method to identify and remove overlapping sources in a LISA data stream. The method is template-based, and templates for monochromatic signals are computed in the Fourier domain by a "total modulation" sum over AM and FM sidebands. Also studies the Doppler (Owen-Sathyaprakash) metric induced by the FM modulations, and uses it to place templates in banks. The gCLEAN method is generalized from CLEAN, used in optical astronomy. Basically, one looks for the strongest match w.r.t. the template bank, and subtracts a small fraction of it, repeating until no strong match is apparent anymore; then one reconstructs sources by pooling partial subtracted sources of nearby parameters. The method is easily confused by close overlapping binaries at low frequencies.

N. J. Cornish, "Rapid LISA Astronomy", gr-qc/0312042 (2003).


A. Krolak, M. Tinto, and M. Vallisneri, "Optimal filtering of the LISA data", Phys. Rev. D 70, 022003 (2004). PRD

Writes the LISA TDI responses (first and second gen.) to moderately chirping signals as analytic expressions, exact in the case of rigid LISA orbits. The expression lend themselves to write an F statistic that is automatically maximized over the initial signal phase, signal polarization, and (essentially) hp/hc ratio. Shows a simple test of this F statistic.

M. Tinto and S. L. Larson, "LISA time-delay interferometry zero-signal solution: Geometrical properties", Phys. Rev. D 70, 062002 (2004). PRD

Generalizing work by Gursel and Tinto for ground-based interferometer networks, derives a "zero-signal solution" TDI combination that has null response for sources at specific sky directions. Shows response patterns strongly peaked (at least in the high-frequency limit) at the "target" frequency. Shows that in the long-wavelength limit the ZSS limits to the null "zeta" variable. Does not deal with noise.

L. J. Rubbo, N. J. Cornish, and O. Poujade, "Forward modeling of space-borne gravitational wave detectors", Phys. Rev. D 69, 082003 (2004). PRD

Essentially, describes the mathematics behind the LISA Simulator, including eˆ2-accurate LISA orbits and plane wave conventions; introduces a highly-accurate "rigid adiabatic approximation" whereby the detector rotates rigidly, and its motion is neglected within the timescale needed to assemble the TDI combinations. Also reconciles its phase response with the Doppler frequency response of Seto (2004).


N. J. Cornish and E. K. Porter, "Detecting galactic binaries with LISA", Class. Quantum Grav. 22, S927 (2005). CQG

Lays out a template-bank based matched-filtering formalism for linearly chirping binaries, using an F statistic that removes the four extrinsic parameters (amplitude, inclination, initial phase, polarization angle). Shows a scaling for the size of the template bank, taking into account the F statistic by way of a projected metric; a steepening in the scaling, corresponding to the fdot parameter becoming meaningful, is evident above 1.5 mHz. In the long-wavelength approximation (from Rubbo, Cornish, Poujade).

J. A. Edlund, M. Tinto, A. Krolak, and Gijs Nelemans, "White-dwarf--white-dwarf galactic background in the LISA data", Phys. Rev. D 71, 122003 (2005). PRD

Describes a simulation of the LISA GWDB, where the "KTV" expressions for the TDI observables are rendered as truncated sums in the frequency domain. Handles infinite vs. finite Fourier transforms by assuming windowed data, and using the corresponding frequency-domain kernel. Generalizes the long-wavelength approximation to a series expansion in the parameter x = omega L (with omega the angular frequency of the source). Analyzes the simulated background as a cyclostationary process.

Jul 19, 2006

lisabinary (/lisa)
2006-07-19, 03:54 [edit]

LISA computational infrastructure

- Scheduling, DAGs: Condor, Pegasus (for the Grid)

- Standards: Safety in software (esp. space)

- Data formats: XSIL, XDF, more graphic formats, scientific data management (including data formats), comparison between XML and binary formats, BFD for XSIL (generate XSIL from arbitrary binary data)

- The fastest Python XML parser: pyRXP (see also what David Mertz has to say)

- LISA measurement system: Scott Pollack

Jan 17, 2006

infrastructure (/lisa)
2006-01-17, 13:55 [edit]

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© M. Vallisneri 2012 — last modified on 2010/01/29

Tantum in modicis, quantum in maximis