The Milky Way’s bar structural properties from gravitational waves

Wilhelm, Martijn J. C.; Korol, Valeriya; Rossi, Elena M.; D’Onghia, Elena

doi:10.1093/mnras/staa3457

Cited by 18 publications

(18 citation statements)

References 64 publications

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“…Our results reinforce the potential of LISA in providing large statistical samples of several thousand detected binaries for studying the overall properties of the Galactic DWD population and for mapping the Milky Way shape (e.g. Adams et al 2012;Korol et al 2019;Korol & Safarzadeh 2021;Wilhelm et al 2021).…”

Section: Resultssupporting

confidence: 75%

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Observationally driven Galactic double white dwarf population for LISA

Korol,

Hallakoun,

Toonen

et al. 2021

Preprint

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Realistic models of the Galactic double white dwarf (DWD) population are crucial for testing and quantitatively defining the science objectives of the Laser Interferometer Space Antenna (LISA), a future European Space Agency's gravitational-wave observatory. In addition to numerous individually detectable DWDs, LISA will also detect an unresolved confusion foreground produced by the underlying Galactic population, which will affect the detectability of all LISA sources at frequencies below a few mHz. So far, the modelling of the DWD population for LISA has been based on binary population synthesis (BPS) techniques. The aim of this study is to construct an observationally driven population. To achieve this, we employ a model developed by Maoz, Hallakoun & Badenes (2018) for the statistical analysis of the local DWD population using two complementary large, multi-epoch, spectroscopic samples: the Sloan Digital Sky Survey (SDSS), and the Supernova Ia Progenitor surveY (SPY). We calculate the number of LISA-detectable DWDs and the Galactic confusion foreground, based on their assumptions and results. We find that the observationally driven estimates yield 1) 2 − 5 times more individually detectable DWDs than various BPS forecasts, and 2) a significantly different shape of the DWD confusion foreground. Both results have important implications for the LISA mission. A comparison between several variations to our underlying assumptions shows that our observationally driven model is robust, and that the uncertainty on the total number of LISA-detectable DWDs is in the order of 20 per cent.

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Section: Resultssupporting

confidence: 75%

“…Our study identified two main results: the observationally driven model yields 1) a factor 2 − 5 increase in the number of detectable DWDs compared to the BPS-based forecasts (e.g. Korol et al 2017;Lamberts et al 2019;Breivik et al 2020;Wilhelm et al 2021) and 2) a significantly different shape of the DWD confusion foreground (cf. Fig.…”

Section: Discussionmentioning

confidence: 82%

Observationally driven Galactic double white dwarf population for LISA

Korol,

Hallakoun,

Toonen

et al. 2021

Preprint

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“…The diversity of GW frequencies potentially included in Eq. ( 9) and the appropriate modeling of the gravitational shift could improve PTA and/or LISA observations [6,45] and the low frequency domain due to periodic sources (e.g., Galactic binary WDs identified by Gaia), further enhancing the mapping of the Milky Way substructures [46]. Moreover, the advantage of Eq.…”

Section: Concluding Remarks and Perspectivesmentioning

confidence: 99%

On the principle of Astrometric Gravitational Wave Antenna

Crosta¹,

Lattanzi²,

Poncin-Lafitte³

et al. 2022

Preprint

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The direct detection of gravitational waves by ground-based optical interferometers has opened a new window in astronomy. Nevertheless, as these detectors are a combination of two Michelson-Morley like baselines, their sensitivity for determining the incident direction of a gravitational wave is quite weak compared to current high-precision of space astrometry. We therefore present a novel concept for a gravitational wave antenna in space that uses close pairs of point-like sources as natural sensors to record and characterize the very tiny variations in angular separations induced by a passing gravitational wave, thus operating complementarily to linear arm detectors and enabling to gain informations on the gravitational wave incoming direction. Indeed, the proposed astrometric gravitational wave observable builds on methods of relativistic astrometry that can substantially enhance the strength of gravitational wave signals by exploiting to the fullest the telescope optical resolution and, at same time, provide a powerful tool for identifying the direction to the sources that originated the gravitational wave by monitoring close pairs of stars. Furthermore, the use of two local-line-of-sights in a differential formulation avoids issues related to high order modeling of the local (Solar System) background geometry and the need for accurate satellite ephemeris and attitude.

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“…However, out of millions, LISA will be able to extract ∼ O (10 4 ) DWDs, which makes them the most numerous type among LISA sources (e.g. Korol et al 2017;Lamberts et al 2019;Breivik et al 2020a;Li et al 2020;Wilhelm et al 2021;Thiele et al 2021). The rest of compact Galactic binaries will blend together to form a confusion-limited foreground that is expected to affect the LISA data at frequencies below a few mHz (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…Several studies investigated the use of the resolved binaries for constraining the properties of the Milky Way (Adams et al 2012;Korol et al 2019;Wilhelm et al 2021). Only a few have exploited the confusion foreground to address similar constraints (Benacquista & Holley-Bockelmann 2006;Breivik et al 2020b).…”

Section: Introductionmentioning

confidence: 99%

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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The Milky Way’s bar structural properties from gravitational waves

Cited by 18 publications

References 64 publications

Observationally driven Galactic double white dwarf population for LISA

Observationally driven Galactic double white dwarf population for LISA

On the principle of Astrometric Gravitational Wave Antenna

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

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