{"total":26,"items":[{"citing_arxiv_id":"2606.24992","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Synergies Between Pulsar Timing Array and Astrometry","primary_cat":"astro-ph.IM","submitted_at":"2026-06-23T15:33:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Joint SKA PTA and astrometry analysis improves gravitational wave background detection sensitivity by 10-50%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.13597","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Natural Supercooling and Reheating along Supersymmetric Flat Directions and Observable Gravitational Waves at the Einstein Telescope and the Cosmic Explorer","primary_cat":"hep-ph","submitted_at":"2026-06-11T17:15:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Radiative barriers in SUSY flat directions enable supercooled PTs yielding Ω_GW h² up to ~3e-10 for M_λ̃/v_X in 0.05-0.23, with the hidden sector also reproducing Ω_CDM h²=0.12 for m_q ~30-800 keV.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.28804","ref_index":76,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Whispers of Supergravity in Gravitational Wave Backgrounds: Determining the Gravitino Mass from Cosmic Thermal History","primary_cat":"astro-ph.CO","submitted_at":"2026-05-27T17:55:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Gravitino masses in the 100 TeV to 10^10 TeV range can be inferred from two frequency features in the stochastic gravitational wave spectrum produced by an early matter-dominated phase.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.24715","ref_index":66,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational Waves from Post-Inflationary Magnetism: Direct and Scalar-Induced Contributions","primary_cat":"astro-ph.CO","submitted_at":"2026-05-23T20:01:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"In a post-inflationary magnetogenesis scenario with time-dependent gauge couplings, magnetic anisotropic stress dominates peak GW amplitude while scalar-induced terms matter on larger scales, both showing f^3 infrared scaling for blue spectra and potentially reaching PTA frequencies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21477","ref_index":76,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Opening the Window of Ultra-Light PBHs by Exorcising the Poltergeist","primary_cat":"hep-ph","submitted_at":"2026-05-20T17:57:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Incorporating the general-relativity mass tail df_PBH/d ln M ∝ M^3.78 smooths PBH evaporation, suppresses the scalar-induced GW signal by orders of magnitude, and reopens the ultra-light PBH window for the hot Big Bang.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21474","ref_index":238,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational Waves from Black Hole Reheating: The Scalar-Induced Component","primary_cat":"hep-ph","submitted_at":"2026-05-20T17:55:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Accounting for the minimal mass spread of primordial black holes from gravitational collapse suppresses the Poltergeist GW background to the level of generic scalar-induced signals and reopens ultra-light PBH parameter space.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"(280). We model this enhancement by the log-normal profile of Eq. (24), characterized by an amplitudeA R, a width ∆, and a peak positionk f. In the narrow-width approximation (cf. Eq. (317)), the initial PBH energy fraction is exponentially sensitive to the smoothed density variance and can be written as βf ≃ σ0(M)√ 2π δc exp \u0014 − δ2 c 2σ2 0(M) \u0015 ,(238) whereδ c is the collapse threshold andσ 0(M) denotes the rms density contrast smoothed on the mass scaleM, as defined in Eq. (299). The threshold depends on the shape of the collapsing perturbation, and typically lies in the rangeδ c ≃0.40-0.67 [267, 268]. For definiteness, we fix δc ≃0.5 in the numerical analysis. In the plots, however, we do not rely on the asymptotic"},{"citing_arxiv_id":"2605.21050","ref_index":63,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on Kaniadakis Cosmology from Starobinsky Inflation and Primordial Tensor Perturbations","primary_cat":"gr-qc","submitted_at":"2026-05-20T11:34:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Kaniadakis entropic cosmology modifies early-universe dynamics and is constrained by its predictions for Starobinsky inflation and the primordial tensor spectrum using current CMB and gravitational-wave observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18286","ref_index":26,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Primary gravitational waves at high frequencies II: Emergence of the exponential cut-off in the power spectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-05-18T12:15:02+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"For infinitely differentiable effective potentials describing the post-inflation transition, the regularized power spectrum of primary gravitational waves exhibits exponential suppression at small scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15197","ref_index":259,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Primordial Black Hole from Tensor-induced Density Fluctuation: First-order Phase Transitions and Domain Walls","primary_cat":"astro-ph.CO","submitted_at":"2026-05-14T17:59:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Tensor perturbations from first-order phase transitions and domain wall annihilation induce curvature fluctuations at second order that form primordial black holes, allowing asteroid-mass PBHs to comprise all dark matter for specific parameter ranges with associated gravitational wave peaks in LISA,","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Janssen et al., PoSAASKA14, 037 (2015), arXiv:1501.00127 [astro-ph.IM]. [256] A. Weltman et al., Publ. Astron. Soc. Austral.37, e002 (2020), arXiv:1810.02680 [astro-ph.CO]. [257] C. L. Carilli and S. Rawlings, New Astron. Rev.48, 979 (2004), arXiv:astro-ph/0409274. [258] M. A. McLaughlin, Class. Quant. Grav.30, 224008 (2013), arXiv:1310.0758 [astro-ph.IM]. [259] Z. Arzoumanian et al. (NANOGRAV), Astrophys. J.859, 47 (2018), arXiv:1801.02617 [astro-ph.HE]. [260] K. Aggarwal et al., Astrophys. J.880, 2 (2019), arXiv:1812.11585 [astro-ph.GA]. [261] A. Brazier et al., (2019), arXiv:1908.05356 [astro-ph.IM]. [262] Z. Arzoumanian et al. (NANOGrav), Astrophys. J. Lett.905, L34 (2020), arXiv:2009.04496 [astro-ph."},{"citing_arxiv_id":"2605.04487","ref_index":62,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational wave emission from nonspherical collapse in an early matter-dominated era using N-body simulations","primary_cat":"astro-ph.CO","submitted_at":"2026-05-06T04:31:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Full numerical N-body treatment is required for reliable gravitational wave predictions from nonspherical collapse in early matter-dominated eras, with resulting spectra mappable to detector sensitivities via horizon mass and reheating temperature.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Trh ≳4MeV to be consistent with the thermal history of the Universe, e.g., the BBN (Big- Bang Nucleosynthesis) and the CMB (Cosmic Microwave Background) [55-60] (see also a review article [1]). The comparison with detector sensitivities is shown in Fig. 13. The four panels cor- respond, respectively, to the frequency bands probed by pulsar timing arrays (NANOGrav [61], EPTA [62], IPTA [63], PPTA [64], and SKA [65]) 8 , space-based interferometers (Big Bang Observatory-BBO [69], LISA [70], DECIGO [71], TAIJI [72], TIANQIN [73] andµ-Ares [74]), ground-based interferometers LVK [75, 76], LIGO A + [77], Einstein Telescope [78], and Cosmic Explorer [79]), and high-frequency resonant-cavity searches [80, 81] (we take the sensitivity band from Ref."},{"citing_arxiv_id":"2605.01318","ref_index":26,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gravitational waves from CP domain wall collapse and electron EDM in a complex singlet model with dimension-five Yukawa interactions","primary_cat":"hep-ph","submitted_at":"2026-05-02T08:28:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"In a complex singlet model with dimension-five Yukawa couplings, current electron EDM bounds already restrict part of the parameter space where gravitational waves from CP domain wall collapse would be detectable.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the CPV structure of the extended model, we construct basis-invariant CP-odd quantities that characterize both explicit CPV and SCPV. We then derive the CPDW configurations associated with SCPV and study the interplay between GW signals from DW annihilation and the electron EDM. In particular, we investigate whether the parameter region accessible to pulsar timing arrays, such as SKA [25] and space-based detectors like THEIA [26], can be probed by current or future EDM experiments. Our analysis shows that the current electron EDM bound already excludes the param- eter region in which the imaginary part of the singlet scalar VEV is below approximately O(10) TeV, near the maximal Higgs mixing allowed by current experiments. In contrast, the parameter region relevant for GW detection by SKA and THEIA corresponds to larger"},{"citing_arxiv_id":"2604.25726","ref_index":112,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Imprint of domain wall annihilation on induced gravitational waves","primary_cat":"hep-ph","submitted_at":"2026-04-28T14:53:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Domain wall annihilation imprints a two-peaked spectrum on induced gravitational waves via an early matter-dominated phase and entropy dilution.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"+a \u0010 D1/3 f fp \u0011b/c\u0013c ,(36) wherea,bandcare real and positive parameters. Here the low-frequency slope4 a= 3can be fixed by causality, while numerical simulations suggestb≃c≃1[96]. InFig. 3, wefirstpresentthepower-lawintegratedsen- sitivity curves [106] of the future GW detectors ET [107], LISA [108], DECIGO [109],µAres [110], SKA [111], and THEIA [112] which are evaluated following Eq. (36) by calculating the signal-to-noise ratio (SNR) [113, 114] ϱ= \" ndettobs Z fmax fmin d f \u0012Ωsignal (f) Ωnoise (f) \u00132#1/2 , wheren det = 1for auto-correlated detectors andndet = 2 for cross-correlated detectors,t obs denotes the observa- tional time, andΩ noise represents the noise spectrum expressed in terms of the GW energy density spec-"},{"citing_arxiv_id":"2604.23384","ref_index":37,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Forecasting graviton-mass constraints from the full covariance of PTA-astrometry ORF estimators","primary_cat":"gr-qc","submitted_at":"2026-04-25T17:24:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A full-covariance formalism for PTA-astrometry ORF estimators forecasts graviton-mass upper limits of 4.41e-24 eV/c2 for current-like setups and 0.48e-24 eV/c2 for SKA/Theia-like future setups, with astrometry adding significant power in the latter case.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"A covariance matrix for this problem includes the finite- source, finite-pixel realization of cosmic variance, the different noise structures of the two channels, and signal-noise coupling [23, 24, 36]. A covariance-level treatment of the joint correlation curves is therefore required for likelihood-based graviton-mass inference. With next-generation facilities such as the Square Kilometre Array (SKA) [37], Gaia Near Infra- Red (Gaia-NIR) [38], and Theia [39], these cross-channel correlations will need to be included in forecasts and data analyses. We develop a full-covariance framework for joint inference with PTA and astrometric correlation-curve estimators. Building on the PTA covariance treatment of Refs. [23, 24], we derive analytic covariance formulae for the joint ORF estimators, including the PTA"},{"citing_arxiv_id":"2604.22731","ref_index":34,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Precision Analysis for $\\boldsymbol{H_0}$ Using Upcoming Multi-band Gravitational Wave Observations","primary_cat":"astro-ph.CO","submitted_at":"2026-04-24T17:28:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Multi-band GW observations of PBHs can reduce H0 uncertainty to ≲2 km/s/Mpc (conservative) or O(0.1) km/s/Mpc (optimistic) via Fisher forecasts on M_PBH and f_PBH.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"The horizontal dashed line denotes the BBN upper bound on the GW amplitude arising from constraints on extra relativistic degrees of freedom. whereuandvare dimensionless momentum ratios, andT(u, v) is the kernel encoding the transfer of scalar perturbations into tensor modes during horizon re-entry. Assuming a sharply peaked dirac-δtype primordial spectrum [34] 2, PR(k) =A R δ \u0012 ln k k∗ \u0013 ,(2.20) wherek ∗ denotes the characteristic comoving wavenumber at which the primordial curva- ture perturbation spectrum is peaked corresponding to the scale responsible for PBH for- mation and the generation of induced gravitational waves. This simplifies the dimensionless present-day energy density of induced GWs generated during the radiation-dominated era"},{"citing_arxiv_id":"2604.20975","ref_index":58,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing Supermassive Black Hole Mergers with Pulsar Timing Arrays","primary_cat":"astro-ph.HE","submitted_at":"2026-04-22T18:06:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Pulsar timing arrays can probe supermassive black hole binaries that merged prior to observations via the pulsar term, with SKA potentially detecting a few such zombie binaries at SNR > 3.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Kilometer Array (SKA) observatory [56]. For the IPTA DR3-like sensitivity, we consider 130 pulsars present in the previously published collaboration datasets, fixing their observing time to 10 years, with an observing ca- dence of 5 days. For the SKA configuration, we use 124 pulsars of our IPTA-like dataset with declination angle below 45 ◦ [57] and added randomly 6 pulsars from [58]. For pulsars whose distances to Earth could not be esti- mated, we randomly assign them a distance from 0.5 to 2.5 kiloparsecs using uniform weighting. In Figure 3, we show the detection efficiency for zom- bie binaries, evaluated for each PTA configuration. We find that the EPTA DR2new-like dataset can only probe massive systems withM c,r ≈10 9M⊙ at redshift below"},{"citing_arxiv_id":"2604.20792","ref_index":26,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Irreducible Gravitational Wave Background as a Particle Detector","primary_cat":"hep-ph","submitted_at":"2026-04-22T17:17:40+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"support","context_text":"(AEDGE), EPJ Quant. Technol.7, 6 (2020), 1908.00802. [22] A. Sesana et al., Exper. Astron.51, 1333 (2021), 1908.11391. [23] J. Garcia-Bellido, H. Murayama, and G. White, JCAP 12, 023 (2021), 2104.04778. [24] C. L. Carilli and S. Rawlings, New Astron. Rev.48, 979 (2004), astro-ph/0409274. [25] G. Janssen et al., PoSAASKA14, 037 (2015), 1501.00127. [26] A. Weltman et al., Publ. Astron. Soc. Austral.37, e002 (2020), 1810.02680. [27] L. Lentati et al. (EPTA), Mon. Not. Roy. Astron. Soc. 453, 2576 (2015), 1504.03692. [28] S. Babak et al. (EPTA), Mon. Not. Roy. Astron. Soc. 455, 1665 (2016), 1509.02165. [29] Z. Arzoumanian et al. (NANOGRAV), Astrophys. J. 859, 47 (2018), 1801.02617. [30] K. Aggarwal et al."},{"citing_arxiv_id":"2604.17478","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A Unified Bogoliubov Approach to Primordial Gravitational Waves: From Inflation to Reheating","primary_cat":"hep-ph","submitted_at":"2026-04-19T15:09:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"An improved Bogoliubov numerical method computes the full primordial GW spectrum from inflation to reheating and shows that inflaton anharmonicity imprints distinctive features at high frequencies.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"spanning an extraordinarily broad range of frequencies-see Ref. [1] for a comprehensive review. The broad GW spectrum, together with many relevant experimental probes, is schematically illustrated in Fig. 1, where the spectrum extends from ultra-low frequen- cies accessible indirectly via cosmic microwave background (CMB) observations including Planck [2] and future missions like LiteBIRD [3], through the nano-Hz regime targeted by pulsar timing arrays (PTAs) including NANOGrav [4] and SKA [5], up to the Hz band relevant for space-based interferometers such as LISA [6], BBO [7-9], and DECIGO [10]. At even higher frequencies, above MHz or GHz, there has been growing interest in novel detection ideas [11-21] aimed at probing this regime-see Refs."},{"citing_arxiv_id":"2601.02458","ref_index":135,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmic Collider Gravitational Waves sourced by Right-handed Neutrino production from Bubbles: Testing Seesaw, Leptogenesis and Dark Matter","primary_cat":"astro-ph.CO","submitted_at":"2026-01-05T18:57:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Bubble collisions in a seesaw model produce right-handed neutrinos that source novel gravitational waves detectable by LISA, ET, and LVK while allowing the lightest RHN to explain dark matter or enable leptogenesis.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"126],DECIGO,U-DECIGO[127, 128],AEDGE[116, 129], andµ-ARES[130] are designed to detect gravitational waves from space, offering different advantages over ground-based counterparts. •Recasts of star surveys:Surveys such asGAIA/THEIA[131] utilize astrometric data from stars to indirectly infer the presence of gravitational waves. •Pulsar timing arrays (PTA):PTA experiments likeSKA[132-134],EPTA[135, 136], andNANOGRA V[137-139] use precise timing measurements of such pulsars to measure gravitational wave signatures. 19 F. Numerical Results We plot the Signal-to-Noise ratio for different detectors in theT ∗ vsβ/Hplane considering both bubble collision and particle production mechanisms as sources in Fig-3. We have checked numerically for largeαthe SNR values remain more or less constant and hence"},{"citing_arxiv_id":"2512.03959","ref_index":29,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Primary gravitational waves at high frequencies I: Origin of suppression in the power spectrum","primary_cat":"astro-ph.CO","submitted_at":"2025-12-03T16:52:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Adiabatic regularization combined with smoothed transitions suppresses the high-frequency oscillations in the power spectrum of primary gravitational waves about a zero mean.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.07956","ref_index":86,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Detecting Parity-Violating Gravitational Wave Backgrounds with Pulsar Polarization Arrays","primary_cat":"gr-qc","submitted_at":"2025-11-11T08:11:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Cross-correlating pulsar timing and polarimetry isolates the circular polarization of isotropic stochastic GW backgrounds and shares the Hellings-Downs angular pattern.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.18958","ref_index":50,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Sensitivity forecasts for gravitational-wave detectors to dark matter decaying into gravitons","primary_cat":"hep-ph","submitted_at":"2025-10-21T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Model-independent forecasts for the stochastic gravitational-wave background from ultralight dark matter decaying into gravitons and the sensitivity of current and future detectors to this signal.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.10456","ref_index":53,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational Wave Signature and the Nature of Neutrino Masses: Majorana, Dirac, or Pseudo-Dirac?","primary_cat":"hep-ph","submitted_at":"2025-09-12T17:59:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"In the minimal B-L gauge extension, Majorana neutrinos at high breaking scale produce flat GW spectra from cosmic strings, Dirac at low scale produce peaked spectra from first-order phase transitions, and pseudo-Dirac produce kink features from domain wall annihilation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.16820","ref_index":134,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Isotropy, anisotropies and non-Gaussianity in the scalar-induced gravitational-wave background: diagrammatic approach for primordial non-Gaussianity up to arbitrary order","primary_cat":"astro-ph.CO","submitted_at":"2025-05-22T15:55:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Extends diagrammatic approach for scalar-induced gravitational waves to arbitrary-order local PNG, deriving semi-analytic spectra for energy density, anisotropies, bispectrum and trispectrum up to quartic terms.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"with the production of SIGWs and are considered potential candidates for cold dark matter. The model parameters inferred from the anisotropies in the future detected SIGW back- ground can impose constraints on the PBH formation, particularly within the mass ranges corresponding to the frequency bands of the sensitivity regimes of space-borne interferometers [122-133, 177] and pulsar timing array (PTA) programs [134-143]. Given that the presence of PNG has a substantial impact on the PBH formation, this work provides a brief discussion on the relationship between PBH formation and the SIGW anisotropies through a simplified example. Through this example, we demonstrate that the angular power spectrum of SIGWs is closely related to the PBH mass fraction at the formation epoch."},{"citing_arxiv_id":"2410.23348","ref_index":89,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Observable CMB B-modes from Cosmological Phase Transitions","primary_cat":"astro-ph.CO","submitted_at":"2024-10-30T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Phase transitions in dark sectors can generate CMB B-modes with amplitudes competitive with inflation but peaking at smaller angular scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2002.04615","ref_index":121,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"New Sensitivity Curves for Gravitational-Wave Signals from Cosmological Phase Transitions","primary_cat":"hep-ph","submitted_at":"2020-02-11T19:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Defines peak-integrated sensitivity curves (PISCs) that fold in the expected spectral shape of gravitational waves from cosmological phase transitions and supplies semianalytical fits plus public data for major detectors.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"timing residuals. We shall assume a future IPTA data set based on N = 20, T = 2 weeks, and σt = 100 ns, which goes beyond the timing precision achieved in the first IPTA data release [118]. As for SKA, we are even more optimistic, assuming an ambitious PTA with N = 50, T = 1 week, and σt = 30 ns. These values are inspired by the assumptions made in Refs. [121, 208]. We thus obtain the following timing noise spectra for IPTA and SKA, DIPTA noise (f)≃ 2.4× 10−8 Hz−3 , D SKA noise (f)≃ 1.1× 10−9 Hz−3 . (A.50) In Fig. 12, we plot the noise spectra of all present and future interferometer experiments that we consider this paper. The timing noise of PTA experiments, which has dimension Hz −3 instead of Hz−1 and which is frequency-independent in the idealized case, is not shown."},{"citing_arxiv_id":"1908.11391","ref_index":141,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Unveiling the Gravitational Universe at \\mu-Hz Frequencies","primary_cat":"astro-ph.IM","submitted_at":"2019-08-29T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Proposal for a μ-Hz space-based gravitational wave interferometer to observe massive black hole binaries in early inspiral and low-frequency galactic binaries.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"structure; pierce through the cosmic microwave background (CMB) to probe the physics of the early Universe [14, 23, 34, 66, 152, 157, 246]. At even lower frequencies, pulsar timing arrays (PTAs, [265]) and the square kilometre array (SKA, [89]) will probe the 10 −9