Search for neutron star binaries in the Local Group galaxies using LISA

Seto, Naoki

doi:10.1093/mnras/stz2439

Cited by 18 publications

(12 citation statements)

References 39 publications

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“…The detection of GW170817 and the selection of LISA as ESA's third L-class mission in January 2017 has led to recent interest in LISA DNSs sources. Seto (2019) estimated the frequency distribution of DNSs in local group galaxies by extrapolating the comoving volumetric DNS merger rate inferred from GW170817. Kyutoku et al (2019) demonstrated that LISA-informed observations can enhance the efficiency of radio pulsar searches with the Square Kilometre Array (SKA).…”

Section: Introductionmentioning

confidence: 99%

Detecting double neutron stars with LISA

Lau

Mandel

Vigna-Gómez

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We estimate the properties of the double neutron star (DNS) population that will be observable by the planned space-based interferometer LISA. By following the gravitational radiation driven evolution of DNSs generated from rapid population synthesis of massive binary stars, we estimate that around 35 DNSs will accumulate a signalto-noise ratio above 8 over a four-year LISA mission. The observed population mainly comprises Galactic DNSs (94 per cent), but detections in the LMC (5 per cent) and SMC (1 per cent) may also be expected. The median orbital frequency of detected DNSs is expected to be 0.8 mHz, and many of them will be eccentric (median eccentricity of 0.11). LISA is expected to localise these DNSs to a typical angular resolution of 2 • . We expect the best-constrained DNSs to have eccentricities known to a few parts in a thousand, chirp masses measured to better than 1 per cent fractional uncertainty, and sky localisation at the level of a few arcminutes. The orbital properties will provide insights into DNS progenitors and formation channels. The localisations may allow neutron star natal kick magnitudes to be constrained through the Galactic distribution of DNSs, and make it possible to follow up the sources with radio pulsar searches. LISA is also expected to resolve ∼ 10 4 Galactic double white dwarfs, many of which may have binary parameters that resemble DNSs; we discuss how the combined measurement of binary eccentricity, chirp mass, and sky location may aid the identification of a DNS.

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Section: Introductionmentioning

confidence: 99%

Detecting double neutron stars with LISA

Lau

Mandel

Vigna-Gómez

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Black hole and neutron star binaries are stronger GW emitters compared to DWDs, but a minimum mass of 10 9 M is required for a host (Artale et al 2019). This implies that they should be expected only in the most massive satellites like the Magellanic Clouds (Andrews et al 2019;Lau et al 2020;Seto 2019). Extending our model to these binaries can improve the predicted number counts and the distance horizon for applicability of the method, although it may not improve the accuracy because double black hole and neutron star binaries are more sensitive to the metallicity assumtion than DWDs (e.g.…”

Section: Discussionmentioning

confidence: 99%

Weighing Milky Way Satellites with LISA

Korol,

Belokurov,

Moore

et al. 2020

Preprint

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White dwarf stars are a well-established tool for studying Galactic stellar populations. Two white dwarfs in a tight binary system offer us an additional messenger -gravitational waves -for exploring the Milky Way and its immediate surroundings. Gravitational waves produced by double white dwarf (DWD) binaries can be detected by the future Laser Interferometer Space Antenna (LISA). Numerous and widespread DWDs have the potential to probe shapes, masses and formation histories of the stellar populations in the Galactic neighbourhood. In this work we outline a method for estimating the total stellar mass of Milky Way satellite galaxies based on the number of DWDs detected by LISA. To constrain the mass we perform a Bayesian inference using binary population synthesis models and considering the number of detected DWDs associated with the satellite and the measured distance to the satellite as the only inputs. Using a fiducial binary population synthesis model we find that for large satellites the stellar masses can be recovered to within 1) a factor two if the star formation history is known and 2) an order of magnitude when marginalising over different star formation history models. For smaller satellites we can place upper limits on their stellar mass. Gravitational wave observations can provide mass measurements for large satellites that are comparable, and in some cases more precise, than standard electromagnetic observations.

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“…Although black hole and neutron star binaries are stronger GW emitters in the LISA band compared to DWDs, their rates are expected to be at least three orders of magnitude lower in the Milky Way and only a few sources are predicted to be detectable in nearby massive satellites (e.g. Andrews et al 2019;Lau et al 2020;Sesana et al 2020;Seto 2019).…”

Section: Introductionmentioning

confidence: 99%

Populations of double white dwarfs in Milky Way satellites and their detectability with LISA

Korol

Toonen

Klein

et al. 2020

A&A

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Context. Milky Way dwarf satellites are unique objects that encode the early structure formation and therefore represent a window into the high redshift Universe. So far, their study has been conducted using electromagnetic waves only. The future Laser Interferometer Space Antenna (LISA) has the potential to reveal Milky Way satellites through gravitational waves emitted by double white dwarf (DWD) binaries. Aims. We investigate gravitational wave signals that will be detectable by LISA as a possible tool for the identification and characterisation of the Milky Way satellites. Methods. We used the binary population synthesis technique to model the population of DWDs in dwarf satellites and we assessed the impact on the number of LISA detections when making changes to the total stellar mass, distance, star formation history, and metallicity of satellites. We calibrated predictions for the known Milky Way satellites on their observed properties. Results. We find that DWDs emitting at frequencies ≳3 mHz can be detected in Milky Way satellites at large galactocentric distances. The number of these high frequency DWDs per satellite primarily depends on its mass, distance, age, and star formation history, and only mildly depends on the other assumptions regarding their evolution such as metallicity. We find that dwarf galaxies with M⋆ > 106 M⊙ can host detectable LISA sources; the number of detections scales linearly with the satellite’s mass. We forecast that out of the known satellites, Sagittarius, Fornax, Sculptor, and the Magellanic Clouds can be detected with LISA. Conclusions. As an all-sky survey that does not suffer from contamination and dust extinction, LISA will provide observations of the Milky Way and dwarf satellites galaxies, which will be valuable for Galactic archaeology and near-field cosmology.

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Search for neutron star binaries in the Local Group galaxies using LISA

Cited by 18 publications

References 39 publications

Detecting double neutron stars with LISA

Detecting double neutron stars with LISA

Weighing Milky Way Satellites with LISA

Populations of double white dwarfs in Milky Way satellites and their detectability with LISA

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