{"total":11,"items":[{"citing_arxiv_id":"2605.18097","ref_index":59,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Effects of formation channels and gravitational lensing on stochastic gravitational wave background","primary_cat":"gr-qc","submitted_at":"2026-05-18T09:11:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Using HBI on GWTC-4 data the authors compute lensed SGWBs for ABHs and PBHs and conclude that LIGO and ET can distinguish the two formation channels in specific frequency ranges, with ET offering broader coverage.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15197","ref_index":148,"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":"arXiv:astro-ph/9605054. [145] J. Chluba et al., Bull. Am. Astron. Soc.51, 184 (2019), arXiv:1903.04218 [astro-ph.CO]. [146] J. Chluba, A. L. Erickcek, and I. Ben-Dayan, Astrophys. J.758, 76 (2012), arXiv:1203.2681 [astro-ph.CO]. [147] I. Musco, V. De Luca, G. Franciolini, and A. Riotto, Phys. Rev. D103, 063538 (2021), arXiv:2011.03014 [astro-ph.CO]. [148] D. S. Salopek and J. R. Bond, Phys. Rev. D42, 3936 (1990). [149] N. Deruelle and D. Langlois, Phys. Rev. D52, 2007 (1995), arXiv:gr-qc/9411040. [150] N. Afshordi and R. H. Brandenberger, Phys. Rev. D63, 123505 (2001), arXiv:gr-qc/0011075. [151] D. H. Lyth, K. A. Malik, and M. Sasaki, JCAP05, 004 (2005), arXiv:astro-ph/0411220. [152] M. Shibata and M."},{"citing_arxiv_id":"2605.11956","ref_index":35,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing the small-scale primordial power spectrum via relic neutrinos and acoustic reheating","primary_cat":"hep-ph","submitted_at":"2026-05-12T11:08:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Dissipation of small-scale primordial perturbations after neutrino decoupling cools relic neutrinos and reduces their abundance, enabling PTOLEMY to constrain the primordial curvature power spectrum to O(0.1) on scales k ≲ 3×10^5 Mpc^{-1}.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"5407 [astro- ph.CO]. [31] A. Naruko, A. Ota, and M. Yamaguchi, JCAP05, 049 (2015), arXiv:1503.03722 [astro-ph.CO]. [32] K. Inomata, M. Kawasaki, and Y. Tada, Phys. Rev. D 94, 043527 (2016), arXiv:1605.04646 [astro-ph.CO]. [33] A. Ota and M. Yamaguchi, JCAP06, 022 (2018), arXiv:1705.05196 [astro-ph.CO]. [34] J. C. Matheret al., Astrophys. J.420, 439 (1994). [35] D. J. Fixsen, E. S. Cheng, J. M. Gales, J. C. Mather, R. A. Shafer, and E. L. Wright, Astrophys. J.473, 576 (1996), arXiv:astro-ph/9605054. [36] D. J. Fixsen, Astrophys. J.707, 916 (2009), arXiv:0911.1955 [astro-ph.CO]. [37] M. G. Bettiet al.(PTOLEMY), JCAP07, 047 (2019), arXiv:1902.05508 [astro-ph.CO]. [38] J. Chluba and D. Grin, Mon. Not. Roy. Astron."},{"citing_arxiv_id":"2605.11083","ref_index":56,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"FLAMINGO: The thermal history of the Universe from tSZ effect cross-correlations and its dependencies on cosmology and baryon physics","primary_cat":"astro-ph.CO","submitted_at":"2026-05-11T18:00:10+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"tSZ cross-correlations with large-scale structure tracers prefer low S8 and strong baryonic feedback, yielding S8 = 0.72 and low group baryon fraction in FLAMINGO simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07616","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing the Inert Doublet Dark Matter with Stellar-Mass Black Hole Mini-Spikes","primary_cat":"hep-ph","submitted_at":"2026-05-08T11:43:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Fermi LAT data on mini-spikes around stellar-mass black holes rules out substantial regions of Inert Doublet Model dark matter parameter space, especially at multi-TeV masses.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"reinforcing the synergistic interplay between astrophysics and particle physics in the ongoing effort to unravel the nature of dark matter. Acknowledgments The work of RS is supported by ANRF CRG/2023/008234. References [1] V.C. Rubin and W.K. Ford, Jr.,Rotation of the Andromeda Nebula from a Spectroscopic Survey of Emission Regions,Astrophys. J.159(1970) 379. [2] D.J. Fixsen, E.S. Cheng, J.M. Gales, J.C. Mather, R.A. Shafer and E.L. Wright,The Cosmic Microwave Background spectrum from the full COBE FIRAS data set,Astrophys. J.473(1996) 576 [astro-ph/9605054]. [3]Planckcollaboration,Planck 2018 results. VI. Cosmological parameters,Astron. Astrophys.641 (2020) A6 [1807.06209]. [4] J.R. Primack,Dark matter and structure formation, inMidrasha Mathematicae in Jerusalem:"},{"citing_arxiv_id":"2604.27926","ref_index":8,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Thermal Spectra Without Detailed Balance","primary_cat":"hep-ph","submitted_at":"2026-04-30T14:29:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Thermal spectra can be produced by certain classes of emission kernels without probe thermalization, as when the differential cross section depends on angle but not on the Mandelstam variable s, providing a kernel-based criterion to distinguish genuine equilibrium from kernel artifacts.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Lett. B754, 235-248 (2016), arXiv:1509.07324 [nucl-ex]. [6] Chun Shen, \"Electromagnetic Radiation from QCD Mat- ter: Theory Overview,\" Nucl. Phys. A956, 184-191 (2016), arXiv:1601.02563 [nucl-th]. [7] John C. Matheret al., \"Measurement of the Cosmic Mi- crowave Background spectrum by the COBE FIRAS in- strument,\" Astrophys. J.420, 439-444 (1994). [8] D. J. Fixsen, E. S. Cheng, J. M. Gales, John C. Mather, R. A. Shafer, and E. L. Wright, \"The Cos- mic Microwave Background spectrum from the full COBE FIRAS data set,\" Astrophys. J.473, 576 (1996), arXiv:astro-ph/9605054. [9] D. J. Fixsen, \"The Temperature of the Cosmic Mi- crowave Background,\" Astrophys. J.707, 916-920 (2009), arXiv:0911.1955 [astro-ph."},{"citing_arxiv_id":"2512.02526","ref_index":96,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Updates on dipolar anisotropy in local measurements of the Hubble constant from Cosmicflows-4","primary_cat":"astro-ph.CO","submitted_at":"2025-12-02T08:42:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Local Hubble constant anisotropy in Cosmicflows-4 data is primarily attributed to peculiar velocities and survey structure rather than cosmic-scale isotropy violation, with limited implications for the Hubble tension.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2211.04492","ref_index":75,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Hubble Tension and Early Dark Energy","primary_cat":"astro-ph.CO","submitted_at":"2022-11-08T19:00:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The Hubble tension between local and early-universe expansion-rate measurements may be resolved by early dark energy that speeds up expansion before recombination while satisfying existing constraints.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"baryon density (today), where h≡ H0/(100 km sec−1 Mpc−1) is a dimensionless Hubble constant. This ωb is determined by the higher-peak structure in the CMB power spectrum far more precisely than Ωb orH0 separately. Planck's ΛCDM value is ωb = 0.0224±0.0001. At last scattering R∼ 0.5 and it is smaller at higher redshifts. And ωγ = 2.47× 10−5 is the physical photon energy density (75). The expansion rate at last scattering is Hls = 100 km sec−1 Mpc−1ω1/2 r (1 +zls)2 √ 1 +ωm ωr 1 1 +zls , 3. where ωm = Ωmh2 is the physical nonrelativistic-matter density today-this, again, is fixed fairly precisely by the higher-peak structure in the CMB; Planck's ΛCDM value is 16 Kamionkowski and Riess ωm = 0.142± 0.001. In the standard cosmological model, the early-Universe energy density"},{"citing_arxiv_id":"2005.01515","ref_index":260,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Dark Photon","primary_cat":"hep-ph","submitted_at":"2020-05-04T14:31:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The paper surveys theoretical motivations, experimental searches, and bounds on the dark photon as a kinetically mixed gauge boson from a dark sector, covering both massive and massless cases along with related milli-charged fermion constraints.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"medium at the epoch of He++ re-ionization in the presence of inhomogeneities [229, 230, 231], - cold Galactic Center gas clouds heating rates [259]; - cosmic microwave background spectral distortions (µ and y-type) [231]; - energy deposition during the dark ages [232], - the number of relativistic species ∆Neff during big-bang nucleosynthesis and recombina- tion [90] and - the diffuse X-ray background [260] yield a series of limits on the upper value ofε for different values ofMA′. These limits are depicted together by the curve labelled \"Dark Matter\" in Fig. 3.7. In addition, there are limits from: • Dark matter direct detection experiments: These experiments are part of the on-going search for dark matter through its direct detection. Data from XENON10/XENON100 ([242] based on"},{"citing_arxiv_id":"1907.08010","ref_index":77,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological searches for the neutrino mass scale and mass ordering","primary_cat":"astro-ph.CO","submitted_at":"2019-07-18T12:03:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Thesis summarizing an upper limit of 0.12 eV on the neutrino mass sum, bias calibration via CMB lensing cross-correlations, and tighter limits plus stronger normal-ordering preference in non-phantom dynamical dark energy models.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"ApJ another paper correctly interpreted their observation as being the first detection of the CMB [76]. Observations of the CMB continued over the coming years, culminating with the first precise measurement of its black-body spectrum from the Far Infrared Absolute Spectrophotometer (FIRAS)instrumenton board theCosmicBackgroundExplorer(COBE) satellite [77]. In 1992, COBE was also the first experiment to detect anisotropies in the CMB [78]. 1 Meanwhile, evidence for the existence of dark components in our Universe kept growing. 1A number of other CMB experiments were launched during those and subsequent years, but it is fair to say that two stand out particularly among the others: the Wilkinson Microwave Anisotropy Probe (WMAP),"},{"citing_arxiv_id":"1906.09299","ref_index":43,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Noncanonical Approaches To Inflation","primary_cat":"gr-qc","submitted_at":"2019-06-21T19:25:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"A review thesis covering Mukhanov parametrization, general scalar-tensor theories, and new slow-roll techniques for canonical and noncanonical inflation observables.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"see, it plays a crucial role in the understanding of the inflationary epoch because it contains information about the primordial density perturbations and also about the degree of homogeneity and isotropy present during the recombination epoch. 1.1.5 The Cosmic Microwave Background The energy spectrum of the CMB, as measured today, is precisely that of a black body [43] with a mean temperature ofT0 = 2.726± 0.001 K [44]. It was first detected in 1965 by Arno Penzias and Robert Wilson using their antenna from Bell Laboratories [45]. Once they ruled out any known source 5Heavier elements need higher densities to form. Carbon and other elements synthesized from it, are the result of thermonuclear reactions in stars once after they have burned"}],"limit":50,"offset":0}