Characterization of the stochastic signal originating from compact binary populations as measured by LISA

Karnesis, Nikolaos; Babak, S.; Pieroni, Mauro; Cornish, N.; Littenberg, T. B.

doi:10.1103/physrevd.104.043019

Cited by 81 publications

(68 citation statements)

References 75 publications

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“…A Gaussian realization of both the signal and noise components is then generated for each of these segments and the spectrum at each frequency is then estimated to be the average over these 𝑁 𝑐 realizations. On the other hand, in this work, and consistently with the procedure employed in Karnesis et al (2021), we perform some operations on the dataset provided by the procedure of section 3.1, which accounts for the complete mission duration (meaning that in the frequency domain the frequency resolution is ∼1/𝑇 obs ), to transform it into a dataset with the same statistical properties of the ones of Caprini et al (2019); Pieroni & Barausse (2020); Flauger et al (2021). For this purpose, averaging over segments is equivalent to averaging over neighboring frequencies, i.e.…”

Section: Data Pre-processingsupporting

confidence: 70%

“…Based on a fiducial binary population synthesis model, we first began by simulating catalogues of sources using different parameters describing the total stellar mass and the shape of the Galaxy. For each of them, we estimated the residual foreground signal after subtracting the 'loudest' sources, based on SNR criteria following the methodology presented in Karnesis et al (2021).…”

Section: Discussionmentioning

confidence: 99%

“…Usually, the analysis is being performed in short frequency segments (since the signal of interest is well localized in frequency), and the main result is then derived by the combination and post-processing of the analysis of the individual segments. Instead, we have chosen to work with an alternative method of estimating the foreground GW signal described in Karnesis et al (2021), which is based on SNR criteria. While this methodology follows simplified assumptions about data analysis with LISA, it can be proven to be producing optimistic estimates of the extracted sources and confusion signal.…”

Section: Estimation Of Foreground Signalmentioning

confidence: 99%

“…In this work we have assumed the nominal mission duration which is T obs = 4 years, and we have adopted an SNR threshold of 𝜌 thres = 5, which is used to classify the DWD binaries as detectable or not. We have also adopted the nominal 'sciRD' sensitivity levels, which are explained in detail in LISA Science Study Team (2018) and in Babak et al (2021). The data are simulated and analyzed directly in the noise orthogonal A and E Time Delay Interferometry (TDI) variables (Tinto & Dhurandhar 2005;Prince et al 2002).…”

Section: Estimation Of Foreground Signalmentioning

confidence: 99%

“…The form of the high-frequency 'knee' structure depends on assumptions about the detectability of these sources with LISA. For example, it heavily depends on the observation duration, and on the signal-to-noise (SNR) threshold criteria to classify the DWD sources as resolvable (Karnesis et al 2021). Variations of intrinsic properties of the DWD population such as the chirp mass distribution can influence the detectability of binaries at few mHz, and, hence, the shape of the knee as well.…”

Section: Introductionmentioning

confidence: 99%

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Gravitational Waves from Double White Dwarfs as probes of the Milky Way

Georgousi¹,

Karnesis²,

Korol³

et al. 2022

Preprint

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Future gravitational wave detectors, such as the Laser Interferometer Space Antenna (LISA), will be able to resolve a significant number of the ultra compact stellar-mass binaries in our own Galaxy and its neighborhood. These will be mostly double white dwarf (DWD) binaries, and their underlying population characteristics can be directly correlated to the different properties of the Galaxy. In particular, with LISA we will be able to resolve ∼ O (10 4 ) binaries, while the rest will generate a confusion foreground signal. Both categories can be used to address a number of astrophysical questions. Analogously to how the total electromagnetic radiation emitted by a galaxy can be related to the underlying total stellar mass, in this work we propose a framework to infer the same quantity by investigating the spectral shape and amplitude of the confusion foreground signal. For a fixed DWD evolution model, we retrieve percentage-level relative errors on the total stellar mass, which improves for increasing values of the mass. At the same time, we find that variations in the Miky Way shape, at a fixed mass and at scale heights smaller than 500 pc, are not distinguishable based on the shape of stochastic signal alone. Finally, we utilize the catalogue of resolvable sources to probe the characteristics of the underlying population of DWD binaries. We show that the DWD frequency, coalescence time and chirp mass (up to < 0.7 M ) distributions can be reconstructed from LISA data with no bias.

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Section: Data Pre-processingsupporting

confidence: 70%

Section: Discussionmentioning

confidence: 99%

Section: Estimation Of Foreground Signalmentioning

confidence: 99%

Section: Estimation Of Foreground Signalmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Gravitational Waves from Double White Dwarfs as probes of the Milky Way

Georgousi¹,

Karnesis²,

Korol³

et al. 2022

Preprint

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The effect of mission duration on LISA science objectives

et al. 2021

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The science objectives of the LISA mission have been defined under the implicit assumption of a 4-years continuous data stream. Based on the performance of LISA Pathfinder, it is now expected that LISA will have a duty cycle of $$\approx 0.75$$ ≈ 0.75 , which would reduce the effective span of usable data to 3 years. This paper reports the results of a study by the LISA Science Group, which was charged with assessing the additional science return of increasing the mission lifetime. We explore various observational scenarios to assess the impact of mission duration on the main science objectives of the mission. We find that the science investigations most affected by mission duration concern the search for seed black holes at cosmic dawn, as well as the study of stellar-origin black holes and of their formation channels via multi-band and multi-messenger observations. We conclude that an extension to 6 years of mission operations is recommended.

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