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

Karnesis, Nikolaos; Babak, Stanislav; Pieroni, Mauro; Cornish, Neil; Littenberg, Tyson

doi:10.48550/arxiv.2103.14598

Cited by 6 publications

(11 citation statements)

References 58 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…where k denotes one of the three noise-independent TDI channels A, E and T , and S n,k (f ) is the one-sided power spectral density of the channel k [62][63][64].…”

Section: B Faithfulness Comparisonsmentioning

confidence: 99%

EFPE: Efficient fully precessing eccentric gravitational waveforms for binaries with long inspirals

Klein¹

2021

Preprint

View full text Add to dashboard Cite

In this paper, we derive a set of equations of motions for binaries on eccentric orbits undergoing spin-induced precession that can efficiently be integrated on the radiation-reaction timescale. We find a family of solutions with a computation cost improved by a factor 10 -50 down to ∼ 10 ms per waveform evaluation compared to waveforms obtained by directly integrating the precession equations, that maintain a mismatch of the order 10 −4 -10 −6 for waveforms lasting a million orbital cycles and a thousand spin-induced precession cycles. We express it in terms of parameters that make the solution regular in the equal-mass limit, thus bypassing a problem of previous similar solutions. We point to ways in which the solution presented in this paper can be perturbed to take into account effects such as general quadrupole momenta and post-Newtonian corrections to the precession equations. This new waveform, with its improved efficiency and its accuracy, makes possible Bayesian parameter estimation using the full spin and eccentricity parameter volume for long lasting inspiralling signals such as stellar-origin black hole binaries observed by LISA.

show abstract

“…where k denotes one of the three noise-independent TDI channels A, E and T , and S n,k (f ) is the one-sided power spectral density of the channel k [62][63][64].…”

Section: B Faithfulness Comparisonsmentioning

confidence: 99%

EFPE: Efficient fully precessing eccentric gravitational waveforms for binaries with long inspirals

Klein¹

2021

Preprint

View full text Add to dashboard Cite

show abstract

“…In this section we will restrict our analysis to a single data stream, corresponding to the TDI X channel, and we will denote the data points as D k , where the index k runs over the reduced set of frequencies f k , and their weights 10 with n k . In this work we neglect the effects of astrophysical foregrounds of either galactic or extra-galactic origin [2,[25][26][27][28][29][30][31] which require more elaborate techniques [32]. For completeness, the SNR is computed as:…”

Section: Principal Component Analysismentioning

confidence: 99%

Detecting primordial features with LISA

Fumagalli,

Pieroni,

Renaux-Petel

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

Oscillations in the frequency profile of the stochastic gravitational wave background are a characteristic prediction of small-scale features during inflation. In this paper we present a first investigation of the detection prospects of such oscillations with the upcoming space-based gravitational wave observatory LISA. As a proof of principle, we show for a selection of feature signals that the oscillations can be reconstructed with LISA, employing a method based on principal component analysis. We then perform a Fisher forecast for the parameters describing the oscillatory signal. For a sharp feature we distinguish between the contributions to the stochastic gravitational wave background induced during inflation and in the post-inflationary period, which peak at different frequencies. We find that for the latter case the amplitude of the oscillation is expected to be measurable with < 10% accuracy if the corresponding peak satisfies h 2 Ω GW 10 −12 -10 −11 , while for inflationary-era gravitational waves a detection of the oscillations requires a higher peak amplitude of h 2 Ω GW , as the oscillations only appear on the UV tail of the spectrum. For a resonant feature the detection prospects with LISA are maximised if the frequency of the oscillation falls into the range ω log = 4 to 10. Our results confirm that oscillations in the frequency profile of the stochastic gravitational wave background are a worthwhile target for future detection efforts and offer a key for experimentally testing inflation at small scales.

show abstract

“…As such, when there are more than one binary per two frequency bins, there will be more parameters than data points, and resolution of an individual binary will be challenging. However, recent studies have made progress in characterizing the galactic foreground coming from an astrophysical population of binaries, as in Karnesis et al (2021).…”

Section: Amplitude Calculationmentioning

confidence: 99%

Spectral separation of the stochastic gravitational-wave background for LISA in the context of a modulated Galactic foreground

Boileau,

Lamberts,

Christensen

et al. 2021

Preprint

View full text Add to dashboard Cite

Within its observational band the Laser Interferometer Space Antenna, LISA, will simultaneously observe orbital modulated waveforms from Galactic white dwarf binaries, a binary black hole produced gravitational-wave background, and potentially a cosmologically created stochastic gravitational-wave background (SGWB). The overwhelming majority of stars end their lives as white dwarfs, making them very numerous in the Milky Way. We simulate Galactic white dwarf binary gravitational-wave emission based on distributions from various mock catalogs and determine a complex waveform from the Galactic foreground with 3.5 × 10 7 binaries. We describe the effects from the Galactic binary distribution population across mass, position within the Galaxy, core type, and orbital frequency distribution. We generate the modulated Galactic white dwarf signal detected by LISA due to its orbital motion, and present a data analysis strategy to address it. The Fisher Information and Markov Chain Monte Carlo methods give an estimation of the LISA noise and the parameters for the different signal classes. We estimate the detectable limits for the future LISA observation of the SGWB in the spectral domain with the 3 LISA channels 𝐴, 𝐸, and 𝑇. We simultaneously estimate the Galactic foreground, the astrophysical and cosmological backgrounds. Assuming the expected astrophysical background and a Galactic foreground, a cosmological background energy density of around Ω 𝐺𝑊 ,𝐶𝑜𝑠𝑚𝑜 ≈ 8 × 10 −13 could be detected by LISA. LISAwill either detect a cosmologically produced SGWB, or set a limit that will have important consequences.

show abstract

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

Cited by 6 publications

References 58 publications

EFPE: Efficient fully precessing eccentric gravitational waveforms for binaries with long inspirals

EFPE: Efficient fully precessing eccentric gravitational waveforms for binaries with long inspirals

Detecting primordial features with LISA

Spectral separation of the stochastic gravitational-wave background for LISA in the context of a modulated Galactic foreground

Contact Info

Product

Resources

About