On the effectiveness of null TDI channels as instrument noise monitors in LISA

Muratore, M.; Hartwig, Olaf; Vetrugno, D.; Vitale, S.; Weber, William J.

doi:10.48550/arxiv.2207.02138

Cited by 2 publications

(4 citation statements)

References 27 publications

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“…and are therefore slightly more complex. We remark that while the equal arm models derived here are accurate enough to describe the GW-sensitive channels X,Y,Z, as well as for the quasi-orthogonal channels A and E, it was demonstrated that this assumption is insufficient for accurately describing the behaviour of the null-channel T, in particular at low frequencies [32,33].…”

Section: Analytical Formulationsmentioning

confidence: 78%

Time-delay interferometry noise transfer functions for LISA

Quang Nam,

Martino,

Lemière

et al. 2023

Phys. Rev. D

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The Laser Interferometry Space Antenna (LISA) mission is the future space-based gravitationalwave (GW) observatory of the European Space Agency. It is formed by 3 spacecraft exchanging laser beams in order to form multiple interferometers. The data streams to be used in order to extract the large number and variety of GW sources are time-delay interferometry (TDI) data. One important processing step to produce these data is the TDI on-ground processing, which recombines multiple interferometric on-board measurements to remove certain noise sources from the data, such as laser frequency noise or spacecraft jitter noise. The LISA noise budget is therefore expressed at the TDI level in order to account for the different TDI transfer functions applied for each noise source and thus estimate their real weight on mission performance. In this study, we present an update model for the beams, measurements and TDI, with several approximations to derive the noise transfer functions. The laser locking and noise correlation are taken into account to see their impact in the transfer functions. A methodology for such a derivation has been established in details, as well as verification procedures against simulated data. It results in a set of transfer functions, which are now used by the LISA project, in particular in its performance model. Using these transfer functions, realistic noise curves for various instrumental configurations are provided to data analysis algorithms and used for instrument design.

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Section: Analytical Formulationsmentioning

confidence: 78%

Time-delay interferometry noise transfer functions for LISA

Quang Nam,

Martino,

Lemière

et al. 2023

Phys. Rev. D

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“…We use Equation (17) to compute the q × q covariance Σe n (f ) of the q lowest-variance aPCI variables. We assume that all singlelink noises are uncorrelated and have the same PSD, set by Equation (11). Hence, their covariance Σy (f ) is diagonal.…”

Section: Orthogonalizationmentioning

confidence: 99%

“…In this section we write down the analytical expressions for the acceleration and OMS noises PSDs form1ing the secondary noises in Equation (11). The acceleration noise PSD is…”

Section: Appendix A: Secondary Noises Modelmentioning

confidence: 99%

“…[2] and references therein), including studying its interplay with anti-aliasing filters, [6] measurements units, [7] clock jitters, [8] clock synchronization, [9] new noise-cancelling combinations [4] and the construction of null channels. [10,11] A new approach to the laser frequency noise problem has gained interest in the last 2 years, which formulates how the noise enters phase measurements with a design matrix, and interprets TDI as the solution to a linear algebra problem. Romano and Woan [12] took a first step in that direction (further explored in ref.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Fully Data‐Driven Time‐Delay Interferometry with Time‐Varying Delays

et al. 2023

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Raw space‐based gravitational‐wave data like laser interferometer space antenna's (LISA) phase measurements are dominated by laser frequency noise. The standard technique to make this data usable for gravitational‐wave detection is time‐delay interferometry (TDI), which cancels laser noise terms by forming suitable combinations of delayed measurements. To do so, TDI relies on inter‐spacecraft distances and on how laser noise enters the interferometric data. The basic concepts of an alternative approach which does not rely on independent knowledge of temporal correlations in the dominant noise recently introduced. Instead, this automated principal component interferometry (aPCI) approach only assumes that one can produce some linear combinations of the temporally nearby regularly spaced phase measurements, which cancel the laser noise. Then the data is let to reveal those combinations, thus providing a set of laser‐noise‐free data channels. The authors' previous approach relies on the simplifying additional assumption that the filters which lead to the laser‐noise‐free data streams are time‐independent. In LISA, however, these filters will vary as the constellation armlengths evolve. Here, a generalization of the basic aPCI concept compatible with data dominated by a still unmodeled but slowly varying dominant noise covariance is discussed. Despite its independence on any model, aPCI successfully mitigates laser frequency noise below the other noises' level, and its sensitivity to gravitational waves is the same as the state‐of‐the‐art second‐generation TDI, up to a 2% error.

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On the effectiveness of null TDI channels as instrument noise monitors in LISA

Cited by 2 publications

References 27 publications

Time-delay interferometry noise transfer functions for LISA

Time-delay interferometry noise transfer functions for LISA

Fully Data‐Driven Time‐Delay Interferometry with Time‐Varying Delays

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