Pith. sign in

REVIEW 5 minor 2 cited by

Science of the LISA mission: A Summary for the European Strategy for Particle Physics

T0 review · 0 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read LISA’s millihertz band is a direct window on TeV-scale early-universe physics.

desk verdict A competent, honest LISA summary for the ESPP; not new science but a useful and properly hedged framing document. read the letter →

arxiv 2507.05130 v1 pith:C3UPCLHP submitted 2025-07-07 gr-qc astro-ph.COhep-ph

Chiara Caprini , Anna Heffernan , Richard Brito , Gabriele Franciolini , Germano Nardini , Nicola Tamanini , Danièle Steer This is my paper
classification gr-qcastro-ph.COhep-ph MSC 83C3583F05 PACS 04.30.-w98.80.-k
keywords LISAgravitationalwavesstochasticwavebackgroundfirst-orderphasetransitionscosmicstringsstandardsirensHubbleconstantTeV-scaleearlyuniverse
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper argues that LISA, the space-based gravitational-wave observatory, will give particle physics a new observational channel: the millihertz frequencies it detects map, through cosmic redshift, to physical processes that operated at temperatures around and beyond the TeV scale in the early universe. The authors focus on four science objectives: testing the fundamental nature of gravity and black holes, measuring the universe’s expansion with standard sirens, detecting stochastic gravitational-wave backgrounds from first-order phase transitions, cosmic strings, and inflation, and searching for unforeseen sources. Their central quantitative claim is that a detection, or even a strong upper limit, on these backgrounds would constrain specific beyond-Standard-Model parameters, such as a singlet mass and a new gauge coupling, in a way complementary to particle colliders. A sympathetic reader should care because LISA would probe energies at the frontier of particle physics through a completely independent messenger.

What carries the argument

The load-bearing identity is the frequency–temperature relation $f \simeq 1.65 \times 10^{-4}\,\mathrm{Hz}\,(g_*/100)^{1/6}(f_*/H_*)(T_*/1\,\mathrm{TeV})$, which converts the temperature $T_*$ of a gravitational-wave source in the early universe into the frequency observed today; it is what turns a detector band into an energy scale. Around this sit two analysis mechanisms: for the stochastic-background objectives, an equal-arm detector approximation combined with a parameterized instrument-noise model, a bin-wise Bayes-factor identification test, and a piecewise power-law spectral reconstruction code (SGWBinner) that can recover a spectral break; for the standard-siren objectives, the distance-from-waveform measurement combined with redshifts from electromagnetic counterparts or galaxy catalogs in a global fit. The machinery’s job is to translate strain data into particle-physics parameters and cosmological distances.

What would settle it

Compare the on-orbit effective noise-plus-foreground curve with the nominal sensitivity used in the benchmark: if it lies more than 30% above the assumed curve at any frequency in the identification band, or if a simulated injection at $h^2\Omega_p = 10^{-10}$ and $f_p = 2\times10^{-4}$ Hz no longer yields a Bayes factor $\log\mathrm{BF}>50$ under 30% relative uncertainty, the central detectability claim fails.

Watch

Extended reading notes

Core claim

The paper’s core claim is that LISA is effectively a TeV-scale observatory in gravitational waves. The frequency a primordial source has today is tied, by the expansion of the universe, to the temperature at which it operated, so the LISA band of $10^{-4}$ to $0.1$ Hz reaches processes at temperatures around and above $1$ TeV. On that basis the authors report quantitative forecasts: standard sirens (sources whose luminosity distance is measured directly from the waveform) should constrain $H(z=2)$ to better than 10% and, combining extreme-mass-ratio inspirals as dark sirens with massive-black-hole binaries as bright sirens, $H_0$ to sub-percent precision; a detected first-order phase transition would pin down the singlet mass and Higgs–singlet coupling to about 10% and a new gauge coupling to about 1%; cosmic-string tensions could be probed down to $G\mu \sim 10^{-16}$; and scalar-induced backgrounds would bound the curvature power spectrum to $A_s \le 10^{-3.5}$ while testing whether asteroid-mass primordial black holes are all of the dark matter. These outcomes are stated to follow if the observatory meets its nominal sensitivity and the combined noise-plus-foreground system can be characterized to the 5–30% relative uncertainty used in the identification study.

Load-bearing premise

The forecasts stand on the assumption that the observatory meets its nominal noise curve and that instrument noise plus astrophysical foregrounds can be characterized to within the 5–30% relative uncertainty used in the identification study; if either falls short, the quoted thresholds, Bayes factors, and parameter errors change.

Editorial extensions

If this is right

  • If the observatory meets nominal sensitivity, LISA’s standard sirens should constrain the Hubble rate $H(z=2)$ to better than 10%, with a combined sub-percent measurement of $H_0$ from massive-black-hole binaries and extreme-mass-ratio inspirals.
  • A detected first-order phase-transition background would constrain the singlet mass and Higgs–singlet coupling to about 10% in a $Z_2$-singlet extension, and the new gauge coupling to about 1% in a scale-invariant $U(1)_{B-L}$ extension.
  • LISA would probe cosmic-string tensions down to $G\mu \sim 10^{-16}$, covering symmetry-breaking scales near $10^{11}$ GeV that are out of reach of ground-based detectors and pulsar timing.
  • A scalar-induced background or null result would improve the bound on the primordial curvature amplitude at LISA scales to $A_s \le 10^{-3.5}$, constraining inflationary dynamics and the asteroid-mass primordial-black-hole dark-matter window.
  • Ringdown and extreme-mass-ratio inspiral measurements would either confirm the Kerr description of black holes or reveal deviations such as scalar/vector radiation or horizonless compact objects.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Beyond the paper: the frequency–temperature mapping transfers directly to other bands, so a future detector with a different frequency window would probe a different early-universe temperature scale using the same reconstruction methods.
  • Beyond the paper: the combined sub-percent $H_0$ forecast depends on an extreme-mass-ratio inspiral rate that the paper itself quotes as uncertain between a few and several thousands per year, so the realized precision is one of the first things the mission would measure.
  • Beyond the paper: the 10% first-order-phase-transition parameter forecasts assume fixed peak amplitude and frequency and a known singlet quartic coupling, so folding LISA’s reconstructed spectral shape into a joint fit with collider observables over the full model space is a natural next step the paper does not itself take.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

0 major / 5 minor

Summary. This manuscript is a concise policy-facing summary, prepared for the European Strategy for Particle Physics, of the LISA mission's science objectives (SO1–SO8) as presented in the LISA Red Book. The paper emphasizes four objectives: SO5 (tests of fundamental gravity and black holes), SO6 (standard-siren cosmology), SO7 (stochastic gravitational-wave backgrounds and TeV-scale particle physics), and SO8 (bursts and unforeseen sources). Its central argument is that the millihertz band opened by LISA provides access to early-universe sources at temperatures around and beyond the TeV scale, giving the mission discovery potential complementary to the LHC and future colliders. The paper also summarizes quantitative forecasts imported from cited simulation studies, including a few-percent determination of H0 with EMRIs, a better-than-10% constraint on H(z=2) with MBHB bright sirens, detection of cosmic-string SGWBs down to Gμ ~ 1e-16, and reconstruction of first-order-phase-transition parameters at the 10% level (singlet mass and Higgs-singlet coupling) and the new gauge coupling to 1%. Section 2.3 contains two proof-of-concept analyses, extracted from the LISA Red Book, demonstrating that a cosmological SGWB could be identified and spectrally reconstructed in simulated LISA data under explicitly stated simplifying assumptions: an equal-arm detector, a parametrized noise model, and a hard prior on noise plus foregrounds with relative uncertainties of 5% and 30%.

Significance. The paper is not a new research derivation but a summary document. Its value lies in distilling the LISA Red Book and the LISA Cosmology Working Group forecasts for a particle-physics audience, and in clearly attributing each quantitative claim to a specific reference. The manuscript is appropriately hedged in most places: it acknowledges population-model uncertainties for EMRI rates, model-dependence of cosmic-string forecasts, and the proof-of-concept nature of the SGWB identification and reconstruction exercises. If the quoted forecasts are realized, LISA would indeed open a new observational window on TeV-scale early-universe physics and provide precision tests of gravity and cosmology in a regime inaccessible to ground-based detectors. The paper's central claim — that LISA has discovery potential in complementarity with the LHC and future colliders — is defensible and supported by the cited literature. The main weaknesses are presentation issues: a few categorical statements of future capability that should be more strongly tied to the underlying models and assumptions, and minor wording inconsistencies in the SGWB proof-of-concept section.

minor comments (5)
  1. [Section 2.2, SO6 bright sirens bullet] The statement "LISA will be able to constrain H(z = 2) with an accuracy better than 10%" is presented as an unconditional mission capability, but the preceding sentence indicates that the number of MBHB bright sirens ranges from about 7 to 20 depending on the model. Please make this a forecast conditional on the fiducial assumptions of Ref. [75] (for example, "is forecast to" or "could") so that the level of model-dependence is transparent to the policy audience.
  2. [Section 2.3, paragraphs before Fig. 5] The text says cosmological SGWBs "must be searched for by minimising a priori assumptions on their spectrum, while remaining as agnostic as possible about the instrument noise," but the subsequent proof-of-concept imposes a hard prior on the noise and foregrounds and only varies the relative uncertainty ε. These two statements are in tension. Please clarify that the hard prior is a controlled test of the method's sensitivity to noise knowledge, not a claim of full agnosticism about the instrument noise.
  3. [Section 2.3, Fig. 5 and surrounding text] The identification and reconstruction exercise is an injection-recovery test of a single benchmark signal with h^2Ω_p = 1e-10 and f_p = 2e-4 Hz. Please state explicitly that the quoted Bayes factors (log BF > 50) and the reconstructed power-law segments in Fig. 5 are conditional on this injected benchmark and on the assumed noise/foreground uncertainties, and that they are not statements about the probability of detecting a cosmological SGWB in the real mission data.
  4. [Section 2.3, right panel of Fig. 5] The text says Ref. [1] reports the SNR and the marginalised 2σ errors on all model parameters, but the paper itself does not quote the reconstructed amplitude, spectral index, or break frequency with errors. Including one representative reconstructed parameter value with its 2σ error would help the reader assess the claimed reconstruction precision without needing to consult the Red Book.
  5. [Throughout] There are several typographical and minor language issues: "in an heliocentric orbit" (abstract) should be "in a heliocentric orbit"; the table heading and label read "T able 1" and should be "Table 1"; and the abbreviation "L VK" (e.g., Section 1.1 and Section 2.1) should be "LVK" without the space.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the paper is a mission-summary whose quantitative forecasts are explicitly sourced to external simulation studies and whose proof-of-concept SGWB exercises are disclosed injection-recovery demonstrations, not predictions derived from their own inputs.

full rationale

This paper is a policy-facing summary of the LISA science case, not an original derivation, and I find no step in which a claimed prediction is equivalent, by construction, to a fitted input or to a self-citation. The Section 2.3 identification and reconstruction demonstrations are explicitly labelled proof-of-concept analyses and are injection-recovery exercises: a benchmark FOPT SGWB with h2Omega_p set to 1e-10 and f_p to 2e-4 Hz is placed into simulated LISA data, and the pipeline then identifies and reconstructs that same signal. This is a pipeline-validation exercise, not a prediction about the universe, and the paper discloses the equal-arm detector assumption, the parametrized noise model, and the tested 5% and 30% relative uncertainties on noise plus foregrounds. The quantitative capability claims (H(z=2) to better than 10%, H0 at few percent from EMRIs, sub-percent from MBHBs and EMRIs combined, FOPT model parameters to about 10%, the new gauge coupling to 1%, and cosmic string tensions down to G mu about 1e-16) are all attributed to external simulation studies with stated population and completeness assumptions; they are conditional sensitivity forecasts, not outputs of the present paper. Equation (1) is the standard frequency-temperature redshift mapping and is not derived from LISA data. No uniqueness theorem, ansatz, or fitted parameter is smuggled in via self-citation. Although the authors are members of the LISA collaboration and cite their own Red Book and Cosmology Working Group papers, those citations are used as sources for externally published, assumption-disclosed forecasts, and the summary does not invoke a self-citation to forbid alternatives or to define a target quantity in terms of itself. The proof-of-concept limitation noted by the reader is a validation concern, not a circularity, because the paper explicitly conditions its demonstration on the stated simplifying assumptions and does not present the recovered signal as external evidence.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The central claims are not derived here but summarized from prior mission documents and simulation studies. The main external inputs are the LISA sensitivity/noise specifications, astrophysical foreground models, the injected benchmark SGWB template, and population models used for standard sirens. No new physical entities are introduced.

free parameters (4)
  • Injected SGWB benchmark peak amplitude h2Omega_p = 1e-10
    Chosen by hand for the proof-of-concept FOPT SGWB injection in Section 2.3; the reconstruction posteriors are conditional on this value.
  • Injected SGWB benchmark peak frequency f_p = 2e-4 Hz
    Chosen by hand in Section 2.3; signal detectability and spectral shape reconstruction depend on this value.
  • Assumed relative uncertainty on noise plus foregrounds, epsilon = 5% and 30%
    Two assumed values in Section 2.3 used in the identification study; the claimed Bayes factor log BF > 50 depends on this assumption.
  • Fiducial EMRI population rate = a few to several thousands per year
    Section 2.2 notes the EMRI rate is highly uncertain; the few-percent H0 forecast is based on a fiducial population and assumed galaxy catalogue completeness, not on measured rates.
assumptions (5)
  • domain assumption LISA sensitivity curve and noise requirements as defined in the LISA Red Book [1]
    All science capability statements, including Table 1 and Figure 2, assume the nominal 4.5-year mission with specified strain sensitivity and noise levels, without verifying on-orbit performance.
  • domain assumption Astrophysical foreground models for galactic binaries and sBHBs accurately represent unresolved backgrounds
    Section 2.3 uses fixed spectral shapes for the foreground amplitudes A_GB and A_sBHB; the conclusion that a cosmological SGWB can be identified or reconstructed depends on these models.
  • ad hoc to paper Equal-arm detector approximation for the T-channel
    The proof-of-concept analyses in Section 2.3 explicitly assume an equal-arm detector to exploit the signal-orthogonal T-channel; the real LISA constellation has unequal arms, and Ref. [99] studies that complication.
  • ad hoc to paper Benchmark FOPT spectral shape h2Omega_PT(f) = h2Omega_p (f/f_p)^3 [7/(4+3(f/f_p)^2)]^(7/2)
    Section 2.3 adopts this template from Ref. [90] as the injected signal. The reconstruction accuracy is only demonstrated for this family of spectra.
  • domain assumption Forecast population models for MBHB bright sirens and EMRI dark sirens
    Section 2.2 builds on population models from Refs. [75,76]. If merger rates, EMRI rates, or galaxy catalogue completeness differ, the quoted H(z), H0, and w0 constraints would change.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Science of the LISA mission: A Summary for the European Strategy for Particle Physics." pith.science (2026). https://pith.science/paper/C3UPCLHP

@misc{pith2026250705130,
  author       = {Pith},
  title        = {Pith review of: Science of the LISA mission: A Summary for the European Strategy for Particle Physics},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/C3UPCLHP}},
  note         = {Machine review of arXiv:2507.05130}
}
abstract

The LISA mission is an international collaboration between ESA, its member states, and NASA, for the detection of gravitational waves from space. It was adopted in January 2024 and is scheduled for launch in the mid-2030's. It will be a constellation of three identical spacecraft forming a near-equilateral triangle in an heliocentric orbit, transferring laser beams over $2.5 \cdot 10^6$ km long arms. Laser interferometry is used to track separations between test masses, thus measuring spacetime strain variations as a function of time. LISA Science Objectives tackle many open questions in astrophysics, fundamental physics and cosmology, including ESA's Cosmic Vision questions "What are the fundamental laws of the universe?" and "How did the universe originate and of what is it made?". In this contribution, based on the LISA Red Book, we present a summary of the LISA Science Objectives relevant for the European Strategy for Particle Physics.

Figures

Figures reproduced from arXiv: 2507.05130 by the authors.

Figure 1
Figure 1. Taken from [1]. LISA targets the milliHz band of gravitational waves, lying between the nanoHz regime probed by Pulsar Timing Arrays and the decaHz regime accessible to ground-based detectors. Several types of sources produce gravitational waves in this band, which also corresponds to the TeV energy scale in the early universe: LISA can thus access gravitational wave signals linked to beyond Standard Model processes… view at source ↗
Figure 2
Figure 2. Taken from [1]. Illustration of the primary LISA source classes in the GW frequency-amplitude plane. Included are merging massive black hole binaries; an extreme mass ratio inspiral at moderate redshift; stellar mass black hole binaries at low redshift, including potential multiband sources; galactic binaries, including verification binaries in the Milky Way. Solid teal, solid blue and dashed black lines denote sens… view at source ↗
Figure 3
Figure 3. Taken from [1]. Examples of SGWBs in the LISA band, together with the instrument sensitivity in the A-channel (black, dashed) and the effective Power Law Sensitivity [82] (grey, dashed). The SGWBs are: in red, the SGWB associated to the formation of pri￾mordial black holes in a mass range for which they could constitute the totality of the dark matter [83]; in orange, the SGWB from cosmic strings with tension provid… view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: Taken from Ref. [89]. Left panel: a FOPT in the context of the Z2-singlet extension of the SM can lead to a SGWB with peak amplitude and frequency detectable by LISA (given in the top legend). The LISA posterior on the SGWB parameters can in turn be translated into pos…
Figure 5
Figure 5. Figure 5: Taken from [1]. Left panel: the identification of a cosmological SGWB. The presence of the injected FOPT SGWB (green line) can be identified in the simulated LISA data imposing a hard prior on the instrument noise, for two tested values of the relative uncertainty on t…

Discussion (0). Sign in to comment.

Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. HydroGrav: Precise hydrodynamics and gravitational waves for cosmological phase transitions

    hep-ph 2026-06 unverdicted novelty 5.0 of 10

    HydroGrav code computes self-similar fluid profiles and GW spectra using exact EOS from effective potentials for EWPT models, identifying parameter regions in a Z2 SM extension where simplified EOS differ in amplitude...

  2. LISA and the LISA Science Team

    astro-ph.IM 2026-01 unverdicted novelty 1.0 of 10

    A review of LISA mission status, science objectives, waveform-modeling needs, and the LISA Science Team's working groups as of December 2025.

Reference graph

Works this paper leans on

138 extracted references · 3 canonical work pages · cited by 2 Pith papers

  1. [1]

    LISA collaboration, LISA Definition Study Report , 2402.07571

    arXiv

  2. [2]

    BR-247 of ESA Brochures, ESA (2005)

    Cosmic Vision: Space Science for Europe 2015–2025 , vol. BR-247 of ESA Brochures, ESA (2005)

    2005

  3. [3]

    LIGO Scientific, Virgocollaboration, Observation of Gravitational Waves from a Binary Black Hole Merger , Phys. Rev. Lett. 116 (2016) 061102 [ 1602.03837]

    arXiv 2016

  4. [4]

    LIGO Scientific, KAGRA, VIRGOcollaboration, Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences , Astrophys. J. Lett. 915 (2021) L5 [ 2106.15163]

    arXiv 2021

  5. [6]

    LIGO Scientific, Virgocollaboration, Tests of general relativity with binary black holes from the second LIGO-Virgo gravitational-wave transient catalog , Phys. Rev. D 103 (2021) 122002 [2010.14529]

    arXiv 2021

  6. [7]

    Search for gravitational wave signals , Astron

    EPTA, InPTA:collaboration, The second data release from the European Pulsar Timing Array - III. Search for gravitational wave signals , Astron. Astrophys. 678 (2023) A50 [ 2306.16214]

    arXiv 2023

  7. [8]

    NANOGrav collaboration, The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background, Astrophys. J. Lett. 951 (2023) L8 [ 2306.16213]

    arXiv 2023

  8. [9]

    Reardon et al., Search for an Isotropic Gravitational-wave Background with the Parkes Pulsar Timing Array , Astrophys

    D.J. Reardon et al., Search for an Isotropic Gravitational-wave Background with the Parkes Pulsar Timing Array , Astrophys. J. Lett. 951 (2023) L6 [ 2306.16215]

    arXiv 2023

Show all 138 references
  1. [10]

    Xu et al., Searching for the Nano-Hertz Stochastic Gravitational Wave Background with the Chinese Pulsar Timing Array Data Release I , Res

    H. Xu et al., Searching for the Nano-Hertz Stochastic Gravitational Wave Background with the Chinese Pulsar Timing Array Data Release I , Res. Astron. Astrophys. 23 (2023) 075024 [2306.16216]

    2023 arXiv

  2. [11]

    International Pulsar Timing Arraycollaboration, Comparing Recent Pulsar Timing Array Results on the Nanohertz Stochastic Gravitational-wave Background , Astrophys. J. 966 (2024) 105 [ 2309.00693]

    2024 arXiv

  3. [12]

    Tinto et al., Time-delay interferometry, Living Rev Relativ 24 (2021) 1 [ gr-qc/0409034]

    M. Tinto et al., Time-delay interferometry, Living Rev Relativ 24 (2021) 1 [ gr-qc/0409034]

    2021 arXiv

  4. [13]

    Vallisneri, Synthetic LISA: Simulating time delay interferometry in a model LISA , Phys

    M. Vallisneri, Synthetic LISA: Simulating time delay interferometry in a model LISA , Phys. Rev. D 71 (2005) 022001 [ gr-qc/0407102]

    2005 arXiv

  5. [14]

    Bayle et al., A unified model for the LISA measurements and instrument simulations , Phys

    J.-B. Bayle et al., A unified model for the LISA measurements and instrument simulations , Phys. Rev. D 107 (2023) 083019 [ 2212.05351]

    2023 arXiv

  6. [15]

    Mitryk et al., Verification of time-delay interferometry techniques using the University of Florida LISA interferometry simulator , Class

    S.J. Mitryk et al., Verification of time-delay interferometry techniques using the University of Florida LISA interferometry simulator , Class. Quant. Grav. 27 (2010) 084012

    2010

  7. [16]

    Mitryk et al., Hardware-based demonstration of time-delay interferometry and TDI-ranging with spacecraft motion effects, Phys

    S.J. Mitryk et al., Hardware-based demonstration of time-delay interferometry and TDI-ranging with spacecraft motion effects, Phys. Rev. D 86 (2012) 122006 [ 1205.1934]. 11

    2012 arXiv

  8. [17]

    Gr¨ uning et al.,Status of the eLISA on table (LOT) electro-optical simulator for space based, long arms interferometers , Experimental Astronomy 39 (2015) 281 [ 1309.1059]

    P. Gr¨ uning et al.,Status of the eLISA on table (LOT) electro-optical simulator for space based, long arms interferometers , Experimental Astronomy 39 (2015) 281 [ 1309.1059]

    2015 arXiv

  9. [18]

    de Vine et al., Experimental Demonstration of Time-Delay Interferometry for the Laser Interferometer Space Antenna, Phys

    G. de Vine et al., Experimental Demonstration of Time-Delay Interferometry for the Laser Interferometer Space Antenna, Phys. Rev. Lett. 104 (2010) 211103 [ 1005.2176]

    2010 arXiv

  10. [19]

    Littenberg and N.J

    T.B. Littenberg and N.J. Cornish, Prototype global analysis of LISA data with multiple source types, Phys. Rev. D 107 (2023) 063004 [ 2301.03673]

    2023 arXiv

  11. [20]

    Rosati and T.B

    R. Rosati and T.B. Littenberg, Prototype Stochastic Gravitational Wave Background Recovery in the LISA Global Fit Residual , 2410.17180

    arXiv

  12. [21]

    M.L. Katz, N. Karnesis, N. Korsakova, J.R. Gair and N. Stergioulas, Efficient GPU-accelerated multisource global fit pipeline for LISA data analysis , Phys. Rev. D 111 (2025) 024060 [2405.04690]

    2025 arXiv

  13. [22]

    S. Deng, S. Babak, M. Le Jeune, S. Marsat, E. Plagnol and A. Sartirana, Modular global-fit pipeline for LISA data analysis , 2501.10277

    arXiv

  14. [23]

    Arun et al., New horizons for fundamental physics with LISA , Living Rev Relativ 25 (2022) 4 [ 2205.01597]

    K.G. Arun et al., New horizons for fundamental physics with LISA , Living Rev Relativ 25 (2022) 4 [ 2205.01597]

    2022 arXiv

  15. [24]

    Auclair et al., Cosmology with the Laser Interferometer Space Antenna , Living Reviews in Relativity 26 (2023) 5 [ 2204.05434]

    P. Auclair et al., Cosmology with the Laser Interferometer Space Antenna , Living Reviews in Relativity 26 (2023) 5 [ 2204.05434]

    2023 arXiv

  16. [25]

    Amaro-Seoane et al., Astrophysics with the Laser Interferometer Space Antenna , Living Rev Relativ 26 (2023) 2 [ 2203.06016]

    P. Amaro-Seoane et al., Astrophysics with the Laser Interferometer Space Antenna , Living Rev Relativ 26 (2023) 2 [ 2203.06016]

    2023 arXiv

  17. [26]

    Amaro Seoane et al., The effect of mission duration on LISA science objectives , General Rel

    P. Amaro Seoane et al., The effect of mission duration on LISA science objectives , General Rel. and Grav. 54 (2022) 3 [ 2107.09665]

    2022 arXiv

  18. [27]

    Littenberg et al., Gravitational wave survey of galactic ultra compact binaries , BAAS 51 (2019) 34

    T. Littenberg et al., Gravitational wave survey of galactic ultra compact binaries , BAAS 51 (2019) 34

    2019

  19. [28]

    Caldwell et al., Astro2020 Science White Paper: Cosmology with a Space-Based Gravitational Wave Observatory , BAAS 51 (2019) 67 [ 1903.04657]

    R. Caldwell et al., Astro2020 Science White Paper: Cosmology with a Space-Based Gravitational Wave Observatory , BAAS 51 (2019) 67 [ 1903.04657]

    2019 arXiv

  20. [29]

    Colpi et al., The Gravitational View of Massive Black Hole Mergers , BAAS 51 (2019) 432

    M. Colpi et al., The Gravitational View of Massive Black Hole Mergers , BAAS 51 (2019) 432

    2019

  21. [30]

    Cutler et al., What can we learn from multi-band observations of black hole binaries? , BAAS 51 (2019) 109 [ 1903.04069]

    C. Cutler et al., What can we learn from multi-band observations of black hole binaries? , BAAS 51 (2019) 109 [ 1903.04069]

    2019 arXiv

  22. [31]

    Baker et al., Multimessenger science opportunities with mHz gravitational waves , BAAS 51 (2019) 123 [ 1903.04417]

    J. Baker et al., Multimessenger science opportunities with mHz gravitational waves , BAAS 51 (2019) 123 [ 1903.04417]

    2019 arXiv

  23. [32]

    Natarajan et al., Disentangling nature from nurture: tracing the origin of seed black holes , BAAS 51 (2019) 73 [ 1904.09326]

    P. Natarajan et al., Disentangling nature from nurture: tracing the origin of seed black holes , BAAS 51 (2019) 73 [ 1904.09326]

    2019 arXiv

  24. [33]

    Berry et al., The unique potential of extreme mass-ratio inspirals for gravitational-wave astronomy, BAAS 51 (2019) 42 [ 1903.03686]

    C. Berry et al., The unique potential of extreme mass-ratio inspirals for gravitational-wave astronomy, BAAS 51 (2019) 42 [ 1903.03686]

    2019 arXiv

  25. [34]

    Cornish et al., The Discovery Potential of Space-Based Gravitational Wave Astronomy , BAAS 51 (2019) 76 [ 1904.01438]

    N. Cornish et al., The Discovery Potential of Space-Based Gravitational Wave Astronomy , BAAS 51 (2019) 76 [ 1904.01438]

    2019 arXiv

  26. [35]

    McWilliams et al., The state of gravitational-wave astrophysics in 2020 , BAAS 51 (2019) 455

    S. McWilliams et al., The state of gravitational-wave astrophysics in 2020 , BAAS 51 (2019) 455

    2019

  27. [36]

    Berti et al., Tests of General Relativity and Fundamental Physics with Space-based Gravitational Wave Detectors , BAAS 51 (2019) 32 [ 1903.02781]

    E. Berti et al., Tests of General Relativity and Fundamental Physics with Space-based Gravitational Wave Detectors , BAAS 51 (2019) 32 [ 1903.02781]

    2019 arXiv

  28. [37]

    Bellovary et al., Where are the Intermediate Mass Black Holes? , BAAS 51 (2019) 175 [1903.08144]

    J. Bellovary et al., Where are the Intermediate Mass Black Holes? , BAAS 51 (2019) 175 [1903.08144]. 12

    2019 arXiv

  29. [38]

    Echeverria, Gravitational Wave Measurements of the Mass and Angular Momentum of a Black Hole , Phys

    F. Echeverria, Gravitational Wave Measurements of the Mass and Angular Momentum of a Black Hole , Phys. Rev. D 40 (1989) 3194

    1989

  30. [39]

    Berti, V

    E. Berti, V. Cardoso and C.M. Will, On gravitational-wave spectroscopy of massive black holes with the space interferometer LISA , Phys. Rev. D 73 (2006) 064030 [ gr-qc/0512160]

    2006 arXiv

  31. [40]

    Cardoso, S

    V. Cardoso, S. Hopper, C.F.B. Macedo, C. Palenzuela and P. Pani, Gravitational-wave signatures of exotic compact objects and of quantum corrections at the horizon scale , Phys. Rev. D 94 (2016) 084031 [ 1608.08637]

    2016 arXiv

  32. [41]

    Berti, K

    E. Berti, K. Yagi, H. Yang and N. Yunes, Extreme Gravity Tests with Gravitational Waves from Compact Binary Coalescences: (II) Ringdown , Gen. Rel. Grav. 50 (2018) 49 [ 1801.03587]

    2018 arXiv

  33. [42]

    Dreyer, B.J

    O. Dreyer, B.J. Kelly, B. Krishnan, L.S. Finn, D. Garrison and R. Lopez-Aleman, Black hole spectroscopy: Testing general relativity through gravitational wave observations , Class. Quant. Grav. 21 (2004) 787 [ gr-qc/0309007]

    2004 arXiv

  34. [43]

    Babak et al., Science with the space-based interferometer LISA

    S. Babak et al., Science with the space-based interferometer LISA. V. Extreme mass-ratio inspirals, Phys. Rev. D 95 (2017) 103012 [ 1703.09722]

    2017 arXiv

  35. [44]

    Doneva, F.M

    D.D. Doneva, F.M. Ramazano˘ glu, H.O. Silva, T.P. Sotiriou and S.S. Yazadjiev, Spontaneous scalarization, Rev. Mod. Phys. 96 (2024) 015004 [ 2211.01766]

    2024 arXiv

  36. [45]

    Eichhorn, P.G.S

    A. Eichhorn, P.G.S. Fernandes, A. Held and H.O. Silva, Breaking black-hole uniqueness at supermassive scales, 2312.11430

    arXiv

  37. [46]

    Arvanitaki, M

    A. Arvanitaki, M. Baryakhtar and X. Huang, Discovering the QCD Axion with Black Holes and Gravitational Waves, Phys. Rev. D 91 (2015) 084011 [ 1411.2263]

    2015 arXiv

  38. [47]

    Herdeiro and E

    C.A.R. Herdeiro and E. Radu, Kerr black holes with scalar hair , Phys. Rev. Lett. 112 (2014) 221101 [1403.2757]

    2014 arXiv

  39. [48]

    Vaglio, C

    M. Vaglio, C. Pacilio, A. Maselli and P. Pani, Multipolar structure of rotating boson stars , Phys. Rev. D 105 (2022) 124020 [ 2203.07442]

    2022 arXiv

  40. [49]

    Bianchi et al., Distinguishing Fuzzballs from Black Holes through Their Multipolar Structure, Phys

    M. Bianchi et al., Distinguishing Fuzzballs from Black Holes through Their Multipolar Structure, Phys. Rev. Lett. 125 (2020) 221601 [ 2007.01743]

    2020 arXiv

  41. [50]

    Tinto and M.E

    M. Tinto and M.E. da Silva Alves, LISA Sensitivities to Gravitational Waves from Relativistic Metric Theories of Gravity , Phys. Rev. D 82 (2010) 122003 [ 1010.1302]

    2010 arXiv

  42. [51]

    Maselli et al., Detecting fundamental fields with LISA observations of gravitational waves from extreme mass-ratio inspirals , Nat

    A. Maselli et al., Detecting fundamental fields with LISA observations of gravitational waves from extreme mass-ratio inspirals , Nat. Astron. 6 (2022) 464 [ 2106.11325]

    2022 arXiv

  43. [52]

    Barsanti, A

    S. Barsanti, A. Maselli, T.P. Sotiriou and L. Gualtieri, Detecting Massive Scalar Fields with Extreme Mass-Ratio Inspirals, Phys. Rev. Lett. 131 (2023) 051401 [ 2212.03888]

    2023 arXiv

  44. [53]

    Moore, D

    C.J. Moore, D. Gerosa and A. Klein, Are stellar-mass black-hole binaries too quiet for LISA? , Mon. Not. Roy. Astron. Soc. 488 (2019) L94 [ 1905.11998]

    2019

  45. [54]

    Toubiana et al., Detectable Environmental Effects in GW190521-like Black-Hole Binaries with LISA , Phys

    A. Toubiana et al., Detectable Environmental Effects in GW190521-like Black-Hole Binaries with LISA , Phys. Rev. Lett. 126 (2021) 101105 [ 2010.06056]

    2021 arXiv

  46. [55]

    K. Eda, Y. Itoh, S. Kuroyanagi and J. Silk, New Probe of Dark-Matter Properties: Gravitational Waves from an Intermediate-Mass Black Hole Embedded in a Dark-Matter Minispike, Phys. Rev. Lett. 110 (2013) 221101 [ 1301.5971]

    2013 arXiv

  47. [56]

    Duque, C.F.B

    F. Duque, C.F.B. Macedo, R. Vicente and V. Cardoso, Extreme-Mass-Ratio Inspirals in Ultralight Dark Matter , Phys. Rev. Lett. 133 (2024) 121404 [ 2312.06767]

    2024 arXiv

  48. [57]

    Barausse, N

    E. Barausse, N. Yunes and K. Chamberlain, Theory-Agnostic Constraints on Black-Hole Dipole Radiation with Multiband Gravitational-Wave Astrophysics , Phys. Rev. Lett. 116 (2016) 241104 [1603.04075]. 13

    2016 arXiv

  49. [58]

    Carson and K

    Z. Carson and K. Yagi, Multi-band gravitational wave tests of general relativity , Class. Quant. Grav. 37 (2020) 02LT01 [1905.13155]

    2020 arXiv

  50. [59]

    Chamberlain and N

    K. Chamberlain and N. Yunes, Theoretical Physics Implications of Gravitational Wave Observation with Future Detectors , Phys. Rev. D 96 (2017) 084039 [ 1704.08268]

    2017 arXiv

  51. [60]

    de Rham and S

    C. de Rham and S. Melville, Gravitational Rainbows: LIGO and Dark Energy at its Cutoff , Phys. Rev. Lett. 121 (2018) 221101 [ 1806.09417]

    2018 arXiv

  52. [61]

    LIGO Scientific, Virgo, Fermi GBM, INTEGRAL, IceCube, AstroSat Cadmium Zinc Telluride Imager Team, IPN, Insight-Hxmt, ANTARES, Swift, AGILE Team, 1M2H Team, Dark Energy Camera GW-EM, DES, DLT40, GRA WITA, Fermi-LAT, ATCA, ASKAP, Las Cumbres Observatory Group, OzGrav, DWF (Deep...

    2017 arXiv

  53. [62]

    Baker, E

    T. Baker, E. Barausse, A. Chen, C. de Rham, M. Pieroni and G. Tasinato, Testing gravitational wave propagation with multiband detections , JCAP 03 (2023) 044 [ 2209.14398]

    2023 arXiv

  54. [63]

    Perkins, N

    S.E. Perkins, N. Yunes and E. Berti, Probing Fundamental Physics with Gravitational Waves: The Next Generation , Phys. Rev. D 103 (2021) 044024 [ 2010.09010]

    2021 arXiv

  55. [65]

    Schutz, Determining the Hubble constant from gravitational wave observations , Nature 323 (1986) 310

    B.F. Schutz, Determining the Hubble constant from gravitational wave observations , Nature 323 (1986) 310

    1986

  56. [66]

    LIGO Scientific, Virgo, 1M2H, Dark Energy Camera GW-E, DES, DLT40, Las Cumbres Observatory, VINROUGE, MASTERcollaboration, A gravitational-wave standard siren measurement of the Hubble constant , Nature 551 (2017) 85 [ 1710.05835]

    2017 arXiv

  57. [67]

    LIGO Scientific, Virgocollaboration, A Standard Siren Measurement of the Hubble Constant from GW170817 without the Electromagnetic Counterpart , Astrophys. J. Lett. 871 (2019) L13 [ 1807.05667]

    2019 arXiv

  58. [68]

    DES, LIGO Scientific, Virgocollaboration, First Measurement of the Hubble Constant from a Dark Standard Siren using the Dark Energy Survey Galaxies and the LIGO/Virgo Binary–Black-hole Merger GW170814 , Astrophys. J. Lett. 876 (2019) L7 [ 1901.01540]

    2019 arXiv

  59. [69]

    LIGO Scientific, Virgo, KAGRAcollaboration, Constraints on the Cosmic Expansion History from GWTC–3 , Astrophys. J. 949 (2023) 76 [ 2111.03604]

    2023 arXiv

  60. [70]

    LIGO Scientific, Virgo, VIRGOcollaboration, A Gravitational-wave Measurement of the Hubble Constant Following the Second Observing Run of Advanced LIGO and Virgo , Astrophys. J. 909 (2021) 218 [ 1908.06060]

    2021 arXiv

  61. [71]

    Gray et al., Joint cosmological and gravitational-wave population inference using dark sirens and galaxy catalogues , JCAP 12 (2023) 023 [ 2308.02281]

    R. Gray et al., Joint cosmological and gravitational-wave population inference using dark sirens and galaxy catalogues , JCAP 12 (2023) 023 [ 2308.02281]

    2023 arXiv

  62. [72]

    Mastrogiovanni, D

    S. Mastrogiovanni, D. Laghi, R. Gray, G.C. Santoro, A. Ghosh, C. Karathanasis et al., Joint population and cosmological properties inference with gravitational waves standard sirens and galaxy surveys , Phys. Rev. D 108 (2023) 042002 [ 2305.10488]. 14

    2023 arXiv

  63. [73]

    Tamanini et al., Science with the space-based interferometer eLISA

    N. Tamanini et al., Science with the space-based interferometer eLISA. III: probing the expansion of the universe using gravitational wave standard sirens , JCAP 2016 (2016) 002 [1601.07112]

    2016 arXiv

  64. [74]

    Lops et al., Galaxy fields of LISA massive black hole mergers in a simulated Universe , MNRAS 519 (2023) 5962 [ 2207.10683]

    G. Lops et al., Galaxy fields of LISA massive black hole mergers in a simulated Universe , MNRAS 519 (2023) 5962 [ 2207.10683]

    2023 arXiv

  65. [75]

    Mangiagli et al., Massive black hole binaries in LISA: Multimessenger prospects and electromagnetic counterparts, Phys

    A. Mangiagli et al., Massive black hole binaries in LISA: Multimessenger prospects and electromagnetic counterparts, Phys. Rev. D 106 (2022) 103017 [ 2207.10678]

    2022 arXiv

  66. [76]

    Laghi et al., Gravitational-wave cosmology with extreme mass-ratio inspirals , MNRAS 508 (2021) 4512 [ 2102.01708]

    D. Laghi et al., Gravitational-wave cosmology with extreme mass-ratio inspirals , MNRAS 508 (2021) 4512 [ 2102.01708]

    2021 arXiv

  67. [77]

    Speri et al., Testing the quasar Hubble diagram with LISA standard sirens , Phys

    L. Speri et al., Testing the quasar Hubble diagram with LISA standard sirens , Phys. Rev. D 103 (2021) 083526 [ 2010.09049]

    2021 arXiv

  68. [78]

    Caprini et al., Constraining early and interacting dark energy with gravitational wave standard sirens: the potential of the eLISA mission , JCAP 2016 (2016) 006 [ 1607.08755]

    C. Caprini et al., Constraining early and interacting dark energy with gravitational wave standard sirens: the potential of the eLISA mission , JCAP 2016 (2016) 006 [ 1607.08755]

    2016 arXiv

  69. [79]

    Belgacem et al., Testing modified gravity at cosmological distances with LISA standard sirens, JCAP 2019 (2019) 024 [ 1906.01593]

    E. Belgacem et al., Testing modified gravity at cosmological distances with LISA standard sirens, JCAP 2019 (2019) 024 [ 1906.01593]

    2019 arXiv

  70. [80]

    C. Liu, D. Laghi and N. Tamanini, Probing modified gravitational-wave propagation with extreme mass-ratio inspirals, Phys. Rev. D 109 (2024) 063521 [ 2310.12813]

    2024 arXiv

  71. [81]

    Tamanini, Late time cosmology with LISA: probing the cosmic expansion with massive black hole binary mergers as standard sirens , J

    N. Tamanini, Late time cosmology with LISA: probing the cosmic expansion with massive black hole binary mergers as standard sirens , J. Phys. Conf. Ser. 840 (2017) 012029 [ 1612.02634]

    2017 arXiv

  72. [82]

    Thrane et al., Sensitivity curves for searches for gravitational-wave backgrounds , Phys

    E. Thrane et al., Sensitivity curves for searches for gravitational-wave backgrounds , Phys. Rev. D 88 (2013) 124032 [ 1310.5300]

    2013 arXiv

  73. [83]

    Bartolo et al., Testing primordial black holes as dark matter with LISA , Phys

    N. Bartolo et al., Testing primordial black holes as dark matter with LISA , Phys. Rev. D 99 (2019) 103521 [ 1810.12224]

    2019 arXiv

  74. [84]

    Antoniadis et al., The second data release from the European Pulsar Timing Array: V

    J. Antoniadis et al., The second data release from the European Pulsar Timing Array: V. Implications for massive black holes, dark matter and the early Universe , arXiv e-prints (2023) arXiv:2306.16227 [2306.16227]

    2023 arXiv

  75. [85]

    Babak et al., Stochastic gravitational wave background from stellar origin binary black holes in LISA , JCAP 2023 (2023) 034 [ 2304.06368]

    S. Babak et al., Stochastic gravitational wave background from stellar origin binary black holes in LISA , JCAP 2023 (2023) 034 [ 2304.06368]

    2023 arXiv

  76. [86]

    The LIGO Sci. Coll. et al., The population of merging compact binaries inferred using gravitational waves through GWTC-3 , Phys. Rev. X 13 (2021) 011048 [ 2111.03634]

    2021 arXiv

  77. [87]

    Karnesis et al., Characterization of the stochastic signal originating from compact binary populations as measured by LISA , Phys

    N. Karnesis et al., Characterization of the stochastic signal originating from compact binary populations as measured by LISA , Phys. Rev. D 104 (2021) 043019 [ 2103.14598]

    2021 arXiv

  78. [88]

    Caprini et al., Science with the space-based interferometer eLISA

    C. Caprini et al., Science with the space-based interferometer eLISA. II: gravitational waves from cosmological phase transitions, JCAP 2016 (2016) 001 [ 1512.06239]

    2016 arXiv

  79. [89]

    LISA Cosmology Working Groupcollaboration, Gravitational waves from first-order phase transitions in LISA: reconstruction pipeline and physics interpretation , JCAP 10 (2024) 020 [2403.03723]

    2024 arXiv

  80. [90]

    Caprini et al., Detecting gravitational waves from cosmological phase transitions with LISA: an update, JCAP 03 (2020) 024 [ 1910.13125]

    C. Caprini et al., Detecting gravitational waves from cosmological phase transitions with LISA: an update, JCAP 03 (2020) 024 [ 1910.13125]

    2020 arXiv

  81. [91]

    Bartolo et al., Science with the space-based interferometer LISA

    N. Bartolo et al., Science with the space-based interferometer LISA. IV: probing inflation with gravitational waves, JCAP 2016 (2016) 026 [ 1610.06481]

    2016 arXiv

  82. [92]

    Auclair et al., Probing the gravitational wave background from cosmic strings with LISA , JCAP 2020 (2020) 034 [ 1909.00819]

    P. Auclair et al., Probing the gravitational wave background from cosmic strings with LISA , JCAP 2020 (2020) 034 [ 1909.00819]. 15

    2020 arXiv

  83. [93]

    LISA Cosmology Working Groupcollaboration, Gravitational waves from cosmic strings in LISA: reconstruction pipeline and physics interpretation , 2405.03740

    arXiv

  84. [94]

    LISA Cosmology Working Groupcollaboration, Gravitational waves from inflation in LISA: reconstruction pipeline and physics interpretation , JCAP 11 (2024) 032 [ 2407.04356]

    2024 arXiv

  85. [95]

    LISA Cosmology Working Groupcollaboration, Reconstructing Primordial Curvature Perturbations via Scalar-Induced Gravitational Waves with LISA , 2501.11320

    arXiv

  86. [96]

    Muratore et al., Time delay interferometry combinations as instrument noise monitors for LISA, Phys

    M. Muratore et al., Time delay interferometry combinations as instrument noise monitors for LISA, Phys. Rev. D 105 (2022) 023009 [ 2108.02738]

    2022 arXiv

  87. [97]

    Muratore et al., On the effectiveness of null TDI channels as instrument noise monitors in LISA, arXiv e-prints (2022) arXiv:2207.02138 [ 2207.02138]

    M. Muratore et al., On the effectiveness of null TDI channels as instrument noise monitors in LISA, arXiv e-prints (2022) arXiv:2207.02138 [ 2207.02138]

    2022 arXiv

  88. [98]

    Muratore, J

    M. Muratore, J. Gair and L. Speri, Impact of the noise knowledge uncertainty for the science exploitation of cosmological and astrophysical stochastic gravitational wave background with LISA, Phys. Rev. D 109 (2024) 042001 [ 2308.01056]

    2024 arXiv

  89. [99]

    Hartwig, M

    O. Hartwig, M. Lilley, M. Muratore and M. Pieroni, Stochastic gravitational wave background reconstruction for a nonequilateral and unequal-noise LISA constellation , Phys. Rev. D 107 (2023) 123531 [ 2303.15929]

    2023 arXiv

  90. [100]

    Alvey, U

    J. Alvey, U. Bhardwaj, V. Domcke, M. Pieroni and C. Weniger, Leveraging Time-Dependent Instrumental Noise for LISA SGWB Analysis , 2408.00832

    arXiv

  91. [101]

    Pozzoli, R

    F. Pozzoli, R. Buscicchio, C.J. Moore, F. Haardt and A. Sesana, Weakly parametric approach to stochastic background inference in LISA , Phys. Rev. D 109 (2024) 083029 [ 2311.12111]

    2024 arXiv

  92. [102]

    Schwaller, Gravitational Waves from a Dark Phase Transition , Phys

    P. Schwaller, Gravitational Waves from a Dark Phase Transition , Phys. Rev. Lett. 115 (2015) 181101 [1504.07263]

    2015 arXiv

  93. [103]

    Fairbairn, E

    M. Fairbairn, E. Hardy and A. Wickens, Hearing without seeing: gravitational waves from hot and cold hidden sectors , JHEP 07 (2019) 044 [ 1901.11038]

    2019 arXiv

  94. [104]

    Jaeckel, V.V

    J. Jaeckel, V.V. Khoze and M. Spannowsky, Hearing the signal of dark sectors with gravitational wave detectors , Phys. Rev. D 94 (2016) 103519 [ 1602.03901]

    2016 arXiv

  95. [105]

    M. Aoki, H. Goto and J. Kubo, Gravitational Waves from Hidden QCD Phase Transition , Phys. Rev. D 96 (2017) 075045 [ 1709.07572]

    2017 arXiv

  96. [106]

    Breitbach, J

    M. Breitbach, J. Kopp, E. Madge, T. Opferkuch and P. Schwaller, Dark, Cold, and Noisy: Constraining Secluded Hidden Sectors with Gravitational Waves , JCAP 07 (2019) 007 [1811.11175]

    2019 arXiv

  97. [107]

    Helmboldt, J

    A.J. Helmboldt, J. Kubo and S. van der Woude, Observational prospects for gravitational waves from hidden or dark chiral phase transitions , Phys. Rev. D 100 (2019) 055025 [ 1904.07891]

    2019 arXiv

  98. [108]

    Croon, V

    D. Croon, V. Sanz and G. White, Model Discrimination in Gravitational Wave spectra from Dark Phase Transitions, JHEP 08 (2018) 203 [ 1806.02332]

    2018 arXiv

  99. [109]

    Bringmann, T.E

    T. Bringmann, T.E. Gonzalo, F. Kahlhoefer, J. Matuszak and C. Tasillo, Hunting WIMPs with LISA: correlating dark matter and gravitational wave signals , JCAP 05 (2024) 065 [2311.06346]

    2024 arXiv

  100. [110]

    Kierkla, A

    M. Kierkla, A. Karam and B. Swiezewska, Conformal model for gravitational waves and dark matter: a status update , JHEP 03 (2023) 007 [ 2210.07075]

    2023 arXiv

  101. [111]

    Baldes and C

    I. Baldes and C. Garcia-Cely, Strong gravitational radiation from a simple dark matter model , JHEP 05 (2019) 190 [ 1809.01198]

    2019 arXiv

  102. [112]

    Kibble, Evolution of a system of cosmic strings , Nucl

    T.W.B. Kibble, Evolution of a system of cosmic strings , Nucl. Phys. B 252 (1985) 227. 16

    1985

  103. [113]

    Damour et al., Gravitational wave bursts from cusps and kinks on cosmic strings , Phys

    T. Damour et al., Gravitational wave bursts from cusps and kinks on cosmic strings , Phys. Rev. D 64 (2001) 064008 [ gr-qc/0104026]

    2001 arXiv

  104. [114]

    Abbott et al., Constraints on Cosmic Strings Using Data from the Third Advanced LIGO-Virgo Observing Run , Phys

    R. Abbott et al., Constraints on Cosmic Strings Using Data from the Third Advanced LIGO-Virgo Observing Run , Phys. Rev. Lett. 126 (2021) 241102 [ 2101.12248]

    2021

  105. [115]

    Guth, The Inflationary Universe: A Possible Solution to the Horizon and Flatness Problems, Phys

    A.H. Guth, The Inflationary Universe: A Possible Solution to the Horizon and Flatness Problems, Phys. Rev. D 23 (1981) 347

    1981

  106. [116]

    Starobinsky, A New Type of Isotropic Cosmological Models Without Singularity , Phys

    A.A. Starobinsky, A New Type of Isotropic Cosmological Models Without Singularity , Phys. Lett. B 91 (1980) 99

    1980

  107. [117]

    Linde, A New Inflationary Universe Scenario: A Possible Solution of the Horizon, Flatness, Homogeneity, Isotropy and Primordial Monopole Problems , Phys

    A.D. Linde, A New Inflationary Universe Scenario: A Possible Solution of the Horizon, Flatness, Homogeneity, Isotropy and Primordial Monopole Problems , Phys. Lett. B 108 (1982) 389

    1982

  108. [118]

    Albrecht and P.J

    A. Albrecht and P.J. Steinhardt, Cosmology for Grand Unified Theories with Radiatively Induced Symmetry Breaking, Phys. Rev. Lett. 48 (1982) 1220

    1982

  109. [119]

    Lasky et al., Gravitational-Wave Cosmology across 29 Decades in Frequency , Phys

    P.D. Lasky et al., Gravitational-Wave Cosmology across 29 Decades in Frequency , Phys. Rev. X 6 (2016) 011035 [ 1511.05994]

    2016 arXiv

  110. [120]

    BICEP, Keckcollaboration, Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season , Phys. Rev. Lett. 127 (2021) 151301 [ 2110.00483]

    2021

  111. [121]

    Starobinsky, Spectrum of relict gravitational radiation and the early state of the universe , JETP Lett

    A.A. Starobinsky, Spectrum of relict gravitational radiation and the early state of the universe , JETP Lett. 30 (1979) 682

    1979

  112. [122]

    Tomita, Evolution of Irregularities in a Chaotic Early Universe , Prog

    K. Tomita, Evolution of Irregularities in a Chaotic Early Universe , Prog. Theor. Phys. 54 (1975) 730

    1975

  113. [123]

    Matarrese, O

    S. Matarrese, O. Pantano and D. Saez, A General relativistic approach to the nonlinear evolution of collisionless matter , Phys. Rev. D 47 (1993) 1311

    1993

  114. [124]

    Matarrese, O

    S. Matarrese, O. Pantano and D. Saez, General relativistic dynamics of irrotational dust: Cosmological implications, Phys. Rev. Lett. 72 (1994) 320 [ astro-ph/9310036]

    1994 arXiv

  115. [125]

    Acquaviva, N

    V. Acquaviva, N. Bartolo, S. Matarrese and A. Riotto, Second order cosmological perturbations from inflation, Nucl. Phys. B 667 (2003) 119 [ astro-ph/0209156]

    2003 arXiv

  116. [126]

    Ananda, C

    K.N. Ananda, C. Clarkson and D. Wands, The Cosmological gravitational wave background from primordial density perturbations , Phys. Rev. D 75 (2007) 123518 [ gr-qc/0612013]

    2007 arXiv

  117. [127]

    Barnaby and M

    N. Barnaby and M. Peloso, Large Nongaussianity in Axion Inflation , Phys. Rev. Lett. 106 (2011) 181301 [ 1011.1500]

    2011 arXiv

  118. [128]

    Sorbo, Parity violation in the Cosmic Microwave Background from a pseudoscalar inflaton , JCAP 06 (2011) 003 [ 1101.1525]

    L. Sorbo, Parity violation in the Cosmic Microwave Background from a pseudoscalar inflaton , JCAP 06 (2011) 003 [ 1101.1525]

    2011 arXiv

  119. [129]

    Endlich, A

    S. Endlich, A. Nicolis and J. Wang, Solid Inflation , JCAP 10 (2013) 011 [ 1210.0569]

    2013 arXiv

  120. [130]

    Ricciardone and G

    A. Ricciardone and G. Tasinato, Primordial gravitational waves in supersolid inflation , Phys. Rev. D 96 (2017) 023508 [ 1611.04516]

    2017 arXiv

  121. [131]

    Bartolo, D

    N. Bartolo, D. Cannone, A. Ricciardone and G. Tasinato, Distinctive signatures of space-time diffeomorphism breaking in EFT of inflation , JCAP 03 (2016) 044 [ 1511.07414]

    2016 arXiv

  122. [132]

    Fumagalli, G.A

    J. Fumagalli, G.A. Palma, S. Renaux-Petel, S. Sypsas, L.T. Witkowski and C. Zenteno, Primordial gravitational waves from excited states , JHEP 03 (2022) 196 [ 2111.14664]

    2022 arXiv

  123. [133]

    Bartolo, V

    N. Bartolo, V. De Luca, G. Franciolini, A. Lewis, M. Peloso and A. Riotto, Primordial Black Hole Dark Matter: LISA Serendipity , Phys. Rev. Lett. 122 (2019) 211301 [ 1810.12218]. 17

    2019 arXiv

  124. [134]

    B. Carr, K. Kohri, Y. Sendouda and J. Yokoyama, Constraints on primordial black holes , Rept. Prog. Phys. 84 (2021) 116902 [ 2002.12778]

    2021 arXiv

  125. [135]

    LISA Cosmology Working Groupcollaboration, Primordial black holes and their gravitational-wave signatures, Living Rev. Rel. 28 (2025) 1 [ 2310.19857]

    2025 arXiv

  126. [136]

    Karnesis et al., Assessing the detectability of a stochastic gravitational wave background with LISA, using an excess of power approach , Class

    N. Karnesis et al., Assessing the detectability of a stochastic gravitational wave background with LISA, using an excess of power approach , Class. Quant. Grav. 37 (2020) 215017 [1906.09027]

    2020 arXiv

  127. [137]

    Caprini et al., Reconstructing the spectral shape of a stochastic gravitational wave background with LISA , JCAP 2019 (2019) 017 [ 1906.09244]

    C. Caprini et al., Reconstructing the spectral shape of a stochastic gravitational wave background with LISA , JCAP 2019 (2019) 017 [ 1906.09244]

    2019 arXiv

  128. [138]

    Flauger et al., Improved reconstruction of a stochastic gravitational wave background with LISA, JCAP 2021 (2021) 059 [ 2009.11845]

    R. Flauger et al., Improved reconstruction of a stochastic gravitational wave background with LISA, JCAP 2021 (2021) 059 [ 2009.11845]

    2021 arXiv

  129. [139]

    Damour et al., Gravitational Wave Bursts from Cosmic Strings , Phys

    T. Damour et al., Gravitational Wave Bursts from Cosmic Strings , Phys. Rev. Lett. 85 (2000) 3761 [gr-qc/0004075]

    2000 arXiv

  130. [140]

    Auclair, S

    P. Auclair, S. Babak, H.Q. Leclere and D.A. Steer, Cosmic string bursts in lisa , Phys. Rev. D 108 (2023) 043519 [ 2305.11653]. 18

    2023 arXiv

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.