Journal of Cosmology and Astroparticle Physics最新文献

{"title":"Tidal effects on primordial black hole capture in neutron stars","authors":"Ian Holst, Yoann Génolini and Pasquale Dario Serpico","doi":"10.1088/1475-7516/2025/09/050","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/09/050","url":null,"abstract":"We revisit the problem of the capture of a primordial black hole (PBH) by a neutron star, accounting for the tidal perturbation from a nearby star or planet. For asteroid-mass PBHs, which could constitute all of the dark matter in the universe, a weakly bound post-capture orbit could be tidally disturbed to the point of preventing the PBH from settling in the neutron star and consuming it within a cosmologically short timescale. We show how this effect depends on environmental parameters and can weaken the proposed constraints based on observations of old neutron stars in high-density dark matter environments for PBH masses ≲ 1022g. We also provide approximate analytical formulae for the capture rates.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"29 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145077710","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Modified gravity constraints from the full shape modeling of clustering measurements from DESI 2024","authors":"M. Ishak, J. Pan, R. Calderon, K. Lodha, G. Valogiannis, A. Aviles, G. Niz, L. Yi, C. Zheng, C. Garcia-Quintero, A. de Mattia, L. Medina-Varela, J.L. Cervantes-Cota, U. Andrade, D. Huterer, H.E. Noriega, G. Zhao, A. Shafieloo, W. Fang, S. Ahlen, D. Bianchi, D. Brooks, E. Burtin, E. Chaussidon, T. Claybaugh, S. Cole, A. de la Macorra, A. Dey, K. Fanning, S. Ferraro, A. Font-Ribera, J.E. Forero-Romero, E. Gaztañaga, H. Gil-Marín, S.Gontcho A. Gontcho, G. Gutierrez, C. Hahn, K. Honscheid, C. Howlett, S. Juneau, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, A. Leauthaud, M.E. Levi, A. Meisner, R. Miquel, J. Moustakas, J.A. Newman, N. Palanque-Delabrouille, W.J. Percival, C. Poppett, F. Prada, I. Pérez-Ràfols, A.J. Ross, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, M. Vargas-Magaña, B.A. Weaver, R.H. Wechsler, C. Yèche, P. Zarrouk, R. Zhou and H. Zou","doi":"10.1088/1475-7516/2025/09/053","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/09/053","url":null,"abstract":"We present cosmological constraints on deviations from general relativity (GR) from the first-year of clustering observations from the Dark Energy Spectroscopic Instrument (DESI) in combination with other available datasets including the CMB data from Planck with CMB-lensing from Planck and ACT, BBN constraints on the physical baryon density, the galaxy weak lensing and clustering from DESY3 and supernova data from DESY5. We first consider the μ(a,k)–Σ(a,k) modified gravity (MG) parameterization (as well as η(a,k)) in a ΛCDM and a w0waCDM cosmological backgrounds. Using a functional form for time-only evolution gives μ0 = 0.11+0.44-0.54 from DESI(FS+BAO)+BBN and a wide prior on ns. Using DESI(FS+BAO)+CMB+DESY3+DESY5-SN, we obtain μ0 = 0.05 ± 0.22 and Σ0 = 0.008 ± 0.045 and similarly μ0 = 0.02+0.19-0.24 and η0 = 0.09+0.36-0.60, in an ΛCDM background. In w0waCDM we obtain μ0 = -0.24+0.32-0.28 and Σ0 = 0.006 ± 0.043, consistent with GR, and we still find a preference of the data for a dynamical dark energy with w0 > -1 and wa < 0. Using functional dependencies in both time and scale gives μ0 and Σ0 with a same level of precision as above but other scale MG parameters remain hard to constrain. We then move to binned parameterizations in a ΛCDM background starting with two bins in redshift and obtain, μ1 = 1.02 ± 0.13, μ2 = 1.04 ± 0.11, Σ1 = 1.021 ± 0.029 and Σ2 = 1.022+0.027-0.023, all consistent with the unity value of GR in the binning formalism. We then extend the analysis to combine two bins in redshift and two in scale giving 8 MG parameters that we find all consistent with GR. We note that we find here that the tension reported in previous studies about Σ0 being inconsistent with GR when using Planck PR3 data goes away when we use the recent LoLLiPoP+HiLLiPoP likelihoods. As noted in previous studies, this seems to indicate that the tension is indeed related to the CMB lensing anomaly in PR3 which is also resolved when using the recent likelihoods. We then constrain the class of Horndeski theory in the effective field theory of dark energy approach. We consider both EFT-basis and α-basis in the analysis. Assuming a power law parameterization for the EFT function Ω, which controls non-minimal coupling, we obtain Ω0 = 0.012+0.001-0.012 and s0 = 0.996+0.54-0.20 from the combination of DESI(FS+BAO)+DESY5SN+CMB in a ΛCDM background, which are consistent with GR. Similar results are obtained when using the α-basis and assuming no-braiding (αB = 0) giving cM < 1.14 at 95% CL in a ΛCDM background, also in agreement with GR. However, we see a mild yet consistent indication for cB > 0 when αB is allowed to vary which will require further study to determine whether this is due to systematics or new physics.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"73 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145077716","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Non-commutativity in Hayward spacetime","authors":"N. Heidari, A.A. Araújo Filho and Iarley P. Lobo","doi":"10.1088/1475-7516/2025/09/051","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/09/051","url":null,"abstract":"In this work, we propose a new black hole solution, namely, a Hayward-like metric incorporating corrections due to non-commutativity by taking into account ∂r ∧ ∂θ Moyal twist. We begin by deriving this solution using the non-commutative gauge theory framework. The general properties of the metric are then analyzed, including the event horizon structure and the Kretschmann scalar. Analogous to the standard Hayward solution, the modified black hole remains regular, provided that additional dependence on the angle θ. Next, we examine the thermodynamic properties, computing the Hawking temperature, entropy, and heat capacity. From the temperature profile, we verify that there is no physical remnant mass when T(Θ,l) → 0, indicating a complete evaporation process. Quantum radiation is analyzed by considering both bosonic and fermionic particle modes, with an estimation of the particle creation density provided for each case. The effective potential is evaluated perturbatively to accomplish the analysis of quasinormal modes and the time-domain response for scalar perturbations. The study of null geodesics is explored to enable the characterization of the photon sphere and black hole shadows. Furthermore, the Gaussian curvature is determined to assess the stability of critical orbits, followed by an analysis of gravitational lensing using the Gauss-Bonnet theorem. Finally, the constraints (bounds) on the parameters Θ (non-commutativity) and l (“Hayward parameter”) are derived based on solar system tests, including the perihelion precession of Mercury, light deflection, and the Shapiro time delay effect.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"1 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145077711","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Testing the growth of cosmic structures during the Dark Ages","authors":"Elena Vanetti, Eleonora Vanzan, Nicola Bellomo and Alvise Raccanelli","doi":"10.1088/1475-7516/2025/09/054","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/09/054","url":null,"abstract":"Hydrogen 21-cm Line Intensity Mapping offers the unique opportunity to access the Dark Ages and trace the formation and evolution of the large scale structure of the Universe prior to star and galaxy formation. In this work we investigate the potential of future Earth- and Moon-based 21-cm surveys to constrain the growth of structures during the currently unexplored redshift range 30 < z < 200. On the one hand we show how foreground contamination could limit the capabilities of future instruments in achieving precision below the 10% level. On the other hand, observations from the far side of the Moon have the potential to reach percent or even sub-percent precision in terms of reconstructing the growth of cosmic structures, if foregrounds are robustly accounted for. Such exquisite precision will provide tight constraints on models that induce deviations from ΛCDM, not only during the Dark Ages, but also during recombination or that manifest mostly in the low-redshift Universe, like Early Dark Energy and nDGP models, respectively. Thus, because of their insensitivity to non-linearities or astrophysical processes, line intensity mapping surveys will provide a formidable consistency check to potential claims of discoveries of new physics that affect the growth of structures.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"80 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145077713","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Dip and non-linearity in the curvature perturbation from inflation with a transient non-slow-roll stage","authors":"Tomohiro Fujita, Ryodai Kawaguchi, Misao Sasaki and Yuichiro Tada","doi":"10.1088/1475-7516/2025/09/046","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/09/046","url":null,"abstract":"We consider models of inflation that contain a transient non-slow-roll stage and investigate the conditions under which a dip appears in the power spectrum of the curvature perturbation. Using the δN formalism, we derive a general relation between the comoving curvature perturbation ℛ and the scalar field perturbation δπ and its velocity perturbation δπ. Compared with the result obtained in linear perturbation theory, it turns out that properly taking account of the δπ contribution is essential to reproduce the dip in the power spectrum. Namely, the curvature perturbation is proportional to a specific linear combination of δφ and δπ at the linear order. We also investigate the non-linearity at the dip scale and find that models with a bump or an upward step exhibit much larger non-linearity than ultra-slow-roll and Starobinsky's linear potential models. Finally, we demonstrate the importance of non-linearity by computing the probability density functions (PDFs) for the models mentioned above and show that highly asymmetric PDFs are realised for models with a bump or a step.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"80 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145077838","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Quantifying bias due to non-Gaussian foregrounds in an optimal reconstruction of CMB lensing and temperature power spectra","authors":"M. Doohan, M. Millea, S. Raghunathan, F. Ge, L. Knox, K. Prabhu, C.L. Reichardt and W.L.K. Wu","doi":"10.1088/1475-7516/2025/09/048","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/09/048","url":null,"abstract":"We estimate the magnitude of the bias due to non-Gaussian extragalactic foregrounds on the optimal reconstruction of the cosmic microwave background (CMB) lensing potential and temperature power spectra. The reconstruction is performed using a Bayesian inference method known as the marginal unbiased score expansion (MUSE). We apply MUSE to a minimum variance combination of multifrequency maps drawn from the Agora publicly available simulations of the lensed CMB and correlated extragalactic foreground emission. Taking noise levels appropriate to the SPT-3G D1 release, we find non-Gaussian foregrounds may bias the MUSE reconstruction of the lensing potential amplitude at the level of (0.7 ± 0.3)σ when using modes up to ℓmax = 3500. We do not detect a statistically significant bias, finding a value of (-0.4 ± 0.3)σ, when restricted to lower angular multipoles, ℓmax = 3000. This work is a first step toward understanding the impact of extragalactic foregrounds on optimal reconstructions of CMB temperature and lensing potential power spectra.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"172 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145077708","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A new census of the Universe's entropy","authors":"Stefano Profumo, Liam Colombo-Murphy, Gabriela Huckabee, Maya Diaz Svensson, Stuti Garg, Ishan Kollipara and Alison Weber","doi":"10.1088/1475-7516/2025/09/049","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/09/049","url":null,"abstract":"The question of what is the total entropy of the universe, how it compares to the maximal entropy of de Sitter space, and how it is distributed across the universe's components, bears considerable importance for a number of reasons. Here, we first update the computation of the entropy associated with various sectors of the observed universe, including in the diffuse cosmic and late-time gamma-ray and neutrino backgrounds, in baryonic matter both in diffuse components, in stars and stellar remnants, and in cosmic rays; we then update, crucially, the estimate of entropy in stellar-mass and super-massive black holes, whose abundance and mass function has come into increasingly sharp definition with recent observations and with the rapidly growing statistics of black-hole-black-hole mergers observed with gravitational wave detectors. We also provide a new, corrected estimate of the potential entropy associated with a stochastic gravitational wave background, with dark sector radiations, and with several dark matter models. Finally, we utilize the similarly recently updated constraints on the abundance of hypothetical primordial black holes — black holes, that is, of non-stellar origin — to assess the maximal amount of entropy they could store. We find that if supermassive primordial black holes exist, they can dominate the entropy budget of the universe consistently with current constraints on their abundance and mass function, to a level potentially not distant from the posited entropy associated with the cosmic event horizon of de Sitter spacetime. The same conclusion holds for certain dark sector models featuring a large number of dark degrees of freedom.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"155 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145077709","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Time-dependent, spherically symmetric background in Kaluza-Klein compactified Horndeski theory and the speed of gravity waves","authors":"S. Mironov, M. Sharov and V. Volkova","doi":"10.1088/1475-7516/2025/09/047","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/09/047","url":null,"abstract":"We revisit the models recently derived from a Kaluza-Klein compactification of higher dimensional Horndeski theory, where the resulting electromagnetic sector features non-trivial couplings to the Horndeski scalar. In particular, this class of theories admits the electromagnetic waves propagating at non-unit speed, which in turn allows to relax the constraints on Horndeski theories following from the multi-messenger speed test. In this work, we prove that both the gravitational wave and its electromagnetic counterpart propagate at the same, though non-unit, speed above an arbitrarily time-dependent, spherically symmetric background within the theories in question. Hence, we support the statement that several subclasses of Horndeski theories are not necessarily ruled out after the GW170817 event provided the photon-Galileon couplings are allowed. We also formulate a set of stability conditions for an arbitrary solution within the discussed theoretical setting.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"132 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145077847","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Peaks sphericity of non-Gaussian random fields","authors":"Cristiano Germani, Mohammad Ali Gorji, Michiru Uwabo-Niibo and Masahide Yamaguchi","doi":"10.1088/1475-7516/2025/09/052","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/09/052","url":null,"abstract":"We formulate the statistics of peaks of non-Gaussian random fields and implement it to study the sphericity of peaks. For non-Gaussianity of the local type, we present a general formalism valid regardless of how large the deviation from Gaussian statistics is. For general types of non-Gaussianity, we provide a framework that applies to any system with a given power spectrum and the corresponding bispectrum in the regime in which contributions from higher-order correlators can be neglected. We present an explicit expression for the most probable values of the sphericity parameters, including the effect of non-Gaussianity on the shape. We show that the effects of small perturbative non-Gaussianity on the sphericity parameters are negligible, as they are even smaller than the subleading Gaussian corrections. In contrast, we find that large non-Gaussianity can significantly distort the peak configurations, making them much less spherical.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"6 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145077712","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Primordial Black Hole formation from power spectrum with finite-width","authors":"Shi Pi, Misao Sasaki, Volodymyr Takhistov and Jianing Wang","doi":"10.1088/1475-7516/2025/09/045","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/09/045","url":null,"abstract":"Primordial Black Holes (PBHs) can form from gravitational collapse of large overdensities in the early Universe, giving rise to rich phenomena in astrophysics and cosmology. We develop a novel, general, and systematic method based on theory of density contrast peaks to calculate the abundance of PBHs for a broad power spectrum of curvature perturbations with Gaussian statistics. We introduce a window function to account for the relevant perturbation scales associated with PBHs of different masses, along with a filter function that removes unphysical contributions from super-horizon-scale overdensities. While some uncertainties remain due to the limited understanding of the nonlinear collapse process, our approach substantially reduces the discrepancy previously observed between peaks theory and the Press-Schechter formalism.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"93 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-09-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145072490","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}