Journal of Cosmology and Astroparticle Physics最新文献

{"title":"Dark sector interactions in light of weak lensing data","authors":"M. Benetti, P.T.Z. Seidel, C. Pigozzo, I.P.R. Baranov, S. Carneiro and J.C. Fabris","doi":"10.1088/1475-7516/2025/06/046","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/06/046","url":null,"abstract":"The current observational tensions in the standard cosmological model have reinforced the research on dynamical dark energy, in particular on models with non-gravitational interaction between the dark components. Analyses of late-time observables like type Ia supernovas (SNe Ia) and large-scale structures (LSS) are not conclusive about the presence of energy flux between dark energy and dark matter, while the anisotropy spectrum of the cosmic microwave background (CMB) is fully consistent with no interaction at all. As background and visible matter tests are less sensitive to the suppression/enhancement in the dark matter power spectrum, which is a characteristic of interacting models, while the CMB spectrum is strongly affected by it, this could be the origin of those results. In order to confirm it and at the same time to rule out the role of possible systematics between early and late-time observations, the use of a low redshift observable sensitive to the gravitational potential generated by dark matter is crucial. In the present paper, we investigate the observational viability of a class of interacting dark energy models, namely with energy exchange between vacuum-type and dust components, in the light of the Dark Energy Survey (DES) observations of galaxy weak lensing, in the context of a spatially-flat Friedmann-Lemaître-Robertson-Walker spacetime. The best fit of our analysis is entirely consistent with null interaction, confirming the CMB based constraints.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"101 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-06-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144479142","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":"Do assumptions about the central density of subhaloes affect dark matter annihilation and lensing calculations?","authors":"Nicole E. Drakos, James E. Taylor and Andrew J. Benson","doi":"10.1088/1475-7516/2025/06/049","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/06/049","url":null,"abstract":"Subhalo models play a critical role in dark matter annihilation predictions and galaxy-galaxy lensing studies; however the internal structure of subhaloes remains highly uncertain. In particular, a growing body of evidence suggests that the central density of cuspy dark matter subhaloes is conserved in minor mergers, whereas empirical models of subhalo evolution — calibrated using limited-resolution simulations — often assume a drop in the central density. To assess the impact of these assumptions, we systematically explore how a wide range of initial mass profiles and tidal evolution prescriptions influence annihilation and lensing calculations, including the physically motivated Energy Truncation model, which explicitly preserves the central density of subhaloes. We find that annihilation calculations are very sensitive to the assumed inner density profile, and different models can produce more than an order of magnitude difference in the annihilation rate of individual subhaloes, and a factor of ∼5 in the total annihilation rate expected in the Milky Way. Since the innermost parts of haloes will always be difficult to resolve in simulations, we conclude that developing a theoretical understanding of subhalo evolution is crucial to be able to make accurate predictions of the dark matter annihilation signal. On the other hand, while the shear and convergence profiles used in galaxy-galaxy lensing are sensitive to the initial profile assumed (e.g., NFW versus Einasto), they are otherwise well-approximated by a simple stripping model in which the original profile is sharply truncated at a tidal radius.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"53 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-06-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144478956","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":"Simulation of thermal conduction by asymmetric dark matter in realistic stars and planets","authors":"Hannah Banks, Stephanie Beram, Rashaad Reid and Aaron C. Vincent","doi":"10.1088/1475-7516/2025/06/047","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/06/047","url":null,"abstract":"Dark matter captured in stars can act as an additional heat transport mechanism, modifying fusion rates and asteroseismoloigcal observables. Calculations of heat transport rates rely on approximate solutions to the Boltzmann equation, which have never been verified in realistic stars. Here, we simulate heat transport in the Sun, the Earth, and a brown dwarf model, using realistic radial temperature, density, composition and gravitational potential profiles. We show that the formalism developed in ref. [1] remains accurate across all celestial objects considered, across a wide range of kinematic regimes, for both spin-dependent and spin-independent interactions where scattering with multiple species becomes important. We further investigate evaporation rates of dark matter from the Sun, finding that previous calculations appear robust. Our Monte Carlo simulation software cosmion is publicly available: https://github.com/aaronvincent/cosmion.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"17 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-06-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144479143","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":"Inhomogeneous cosmology with space-varying dark energy and dark matter profiles","authors":"D. Comelli","doi":"10.1088/1475-7516/2025/06/048","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/06/048","url":null,"abstract":"We analyse an inhomogeneous cosmological model featuring a spherically symmetric bubble solution induced by a unified single perfect fluid, comprising spatially dependent Dark Energy (with w = -1) and Dark Matter (with w = 0) components. We impose an Hubble profile that matches the Planck value at early times (h0 = 67.4 ± 0.5 Km/s Mpc) and the local value (ℋ0 = 73.52 ± 1.62 Km/s Mpc). We explicitly derive perturbative solutions in two distinct regimes: one expanded around the center (for small r ℋ0 ≪ 1) and the other expanded around a homogeneous FRW universe. In both cases, we compute the cosmographic parameters, redshift profiles for the Hubbles expansion rates, and effective equations of state. Furthermore, we investigate the redshift drift behaviour extended to a Lemaître metric.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"148 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-06-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144479147","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":"Accelerating HI density predictions during the Epoch of Reionization using a GPR-based emulator on N-body simulations","authors":"Gaurav Pundir, Aseem Paranjape and Tirthankar Roy Choudhury","doi":"10.1088/1475-7516/2025/06/045","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/06/045","url":null,"abstract":"Building fast and accurate ways to model the distribution of neutral hydrogen during the Epoch of Reionization (EoR) is essential for interpreting upcoming 21 cm observations. A key component of semi-numerical models of reionization is the collapse fraction field fcoll(x), which represents the fraction of mass within dark matter halos at each location. Using high-dynamic range N-body simulations to obtain this is computationally prohibitive and semi-analytical approaches, while being fast, end up compromising on accuracy. In this work, we bridge the gap by developing a machine learning model that can generate fcoll maps by sampling from the full distribution of fcoll conditioned on the dark matter density contrast δ. The conditional distribution functions and the input density field to the model are taken from low-dynamic range N-body simulations that are more efficient to run. We evaluate the performance of our ML model by comparing its predictions to a high-dynamic range N-body simulation. Using these fcoll maps, we compute the HI and HII maps through a semi-numerical code for reionization. We are able to recover the large-scale HI density field power spectra (k ≲ 1 h Mpc-1) at the ≲ 10% level, while the HII density field is reproduced with errors well below 10% across all scales. Compared to existing semi-analytical prescriptions, our approach offers significantly improved accuracy in generating the collapse fraction field, providing a robust and efficient alternative for modeling reionization.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"59 1","pages":"045"},"PeriodicalIF":6.4,"publicationDate":"2025-06-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144335030","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":"Free streaming of warm wave dark matter in modified expansion histories","authors":"Andrew J. Long and Moira Venegas","doi":"10.1088/1475-7516/2025/06/043","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/06/043","url":null,"abstract":"In models of warm dark matter, there is an appreciable population of high momentum particles in the early universe, which free stream out of primordial over/under densities, thereby prohibiting the growth of structure on small length scales. The distance that a dark matter particle travels without obstruction, known as the free streaming length, depends on the particle's mass and momentum, but also on the cosmological expansion rate. In this way, measurements of the linear matter power spectrum serve to probe warm dark matter as well as the cosmological expansion history. In this work, we focus on ultra-light warm wave dark matter (WWDM) characterized by a typical comoving momentum q* and mass m. We first derive constraints on the WWDM parameter space (q*, m) using Lyman-α forest observations due to a combination of the free-streaming effect and the white-noise effect. We next assess how the free streaming of WWDM is affected by three modified expansion histories: early matter domination, early dark energy, and very early dark energy.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"38 1","pages":"043"},"PeriodicalIF":6.4,"publicationDate":"2025-06-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144335028","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":"Constraints on dark matter annihilation in the Large Magellanic Cloud from multiple low-frequency radio observations","authors":"Zhanfang Chen, Feng Huang and Taotao Fang","doi":"10.1088/1475-7516/2025/06/044","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/06/044","url":null,"abstract":"Low-frequency radio emission from the Large Magellanic Cloud (LMC) is assumed to be dominated by nonthermal synchrotron radiation from energy loss of energetic e+/e- in magnetic field. Two different kinds of sources of e+/e-, dark matter (DM) annihilation and cosmic rays (CR) related to massive stars, are taken into account in this paper. We fit the multiple low-frequency radio observations, from 19.7 MHz to 1.4 GHz, with a double power-law model Snth = SDM(ν/ν★)-αDM+SCR(ν/ν★)-αCR. ν★ is set to be 1.4 GHz. For gaugino annihilation, the flux from dark matter annihilation exhibits a ν-0.75 power-law dependence on frequency. We fix αDM and treat SCR, SDM, and αCR as free parameters when fitting the low frequency radio data. Depending on whether thermal emission is included or not, our best-fit values for SDM(ν★) range from 98.4 Jy to 114.8 Jy. Furthermore, we derive upper limits on the particle properties of dark matter associated with gaugino annihilation across various radio frequencies. Future low-frequency and high-resolution radio surveys are expected to serve as promising and powerful tools for constraining the properties of dark matter.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"1 1","pages":"044"},"PeriodicalIF":6.4,"publicationDate":"2025-06-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144334928","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":"High-significance detection of correlation between the unresolved gamma-ray background and the large-scale cosmic structure","authors":"B. Thakore, M. Negro, M. Regis, S. Camera, D. Gruen, N. Fornengo, A. Roodman, A. Porredon, T. Schutt, A. Cuoco, A. Alarcon, A. Amon, K. Bechtol, M.R. Becker, G.M. Bernstein, A. Campos, A. Carnero Rosell, M. Carrasco Kind, R. Cawthon, C. Chang, R. Chen, A. Choi, J. Cordero, C. Davis, J. DeRose, H.T. Diehl, S. Dodelson, C. Doux, A. Drlica-Wagner, K. Eckert, J. Elvin-Poole, S. Everett, A. Ferté, M. Gatti, G. Giannini, R.A. Gruendl, I. Harrison, W.G. Hartley, E.M. Huff, M. Jarvis, N. Kuropatkin, P.-F. Leget, N. MacCrann, J. McCullough, J. Myles, A. Navarro-Alsina, S. Pandey, J. Prat, M. Raveri, R.P. Rollins, A.J. Ross, E.S. Rykoff, C. Sánchez, L.F. Secco, I. Sevilla-Noarbe, E. Sheldon, T. Shin, M.A. Troxel, I. Tutusaus, B. Yanny, B. Yin, Y. Zhang, M. Aguena, D. Brooks, J. Carretero, L.N. da Costa, T.M. Davis, J. De Vicente, S. Desai, P. Doel, B. Flaugher, J. Frieman, J. García-Bellido, E. Gaztanaga, G. Gutierrez, S.R. Hinton, D.L. Hollowood, K. Honscheid, D.J. James, K. Kuehn, O...","doi":"10.1088/1475-7516/2025/06/037","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/06/037","url":null,"abstract":"Our understanding of the γ-ray sky has improved dramatically in the past decade, however, the unresolved γ-ray background (UGRB) still has a potential wealth of information about the faintest γ-ray sources pervading the Universe. Statistical cross-correlations with tracers of cosmic structure can indirectly identify the populations that most characterize the γ-ray background. In this study, we analyze the angular correlation between the γ-ray background and the matter distribution in the Universe as traced by gravitational lensing, leveraging more than a decade of observations from the Fermi-Large Area Telescope (LAT) and 3 years of data from the Dark Energy Survey (DES). We detect a correlation at signal-to-noise ratio of 8.9. Most of the statistical significance comes from large scales, demonstrating, for the first time, that a substantial portion of the UGRB aligns with the mass clustering of the Universe as traced by weak lensing. Blazars provide a plausible explanation for this signal, especially if those contributing to the correlation reside in halos of large mass (∼ 1014M⊙) and account for approximately 30–40% of the UGRB above 10 GeV. Additionally, we observe a preference for a curved γ-ray energy spectrum, with a log-parabolic shape being favored over a power-law. We also discuss the possibility of modifications to the blazar model and the inclusion of additional γ-ray sources, such as star-forming galaxies, misalinged active galactic nuclei, or particle dark matter.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"14 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144329224","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":"Fréchet vectors as sensitive tools for blind tests of CMB anomalies","authors":"Ricardo G. Rodrigues, Thiago S. Pereira and Miguel Quartin","doi":"10.1088/1475-7516/2025/06/039","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/06/039","url":null,"abstract":"Cosmological data collected on a sphere, such as CMB anisotropies, are typically represented by the spherical harmonic coefficients, denoted as aℓm. The angular power spectrum, or Cℓ, serves as the fundamental estimator of the variance in this data. Alternatively, spherical data and their variance can also be characterized using Multipole Vectors (MVs) and the Fréchet variance. The vectors that minimize this variance, known as Fréchet Vectors (FVs), define the center of mass of points on a compact space, and are excellent indicators of statistical correlations between different multipoles. We demonstrate this using both simulations and real data. Through simulations, we show that FVs enable a blind detection and reconstruction of the location associated with a mock Cold Spot anomaly introduced in an otherwise isotropic sky. Applying these tools to the 2018 Planck maps, we implement several improvements on previous null tests of Gaussianity and statistical isotropy, down to arc-minute scales. Planck's MVs appear consistent with these hypotheses at scales 2 ≤ ℓ ≤ 1500 when the common mask is applied, whereas the same test using the FVs rejects them with significances between 5.3 and 8.2σ. The inclusion of anisotropic noise simulations render the FVs marginally consistent (≥ 2σ) with the null hypotheses at the same scales, but still rejects them at 3.5-3.7σ when we consider scales above ℓ=1500, where the signal-to-noise is small. Limitations of the noise and/or foregrounds modeling may account for these deviations from the null hypothesis.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"46 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144329226","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":"Higgs-portal vector dark matter at a low reheating temperature","authors":"Sarif Khan, Jongkuk Kim and Hyun Min Lee","doi":"10.1088/1475-7516/2025/06/040","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/06/040","url":null,"abstract":"We study vector dark matter (DM) production with Higgs-portal type interactions in the scenarios with a low reheating temperature which can be realized by a prolonged decay of the inflaton after inflation. We take the reheating temperature to be large enough to match the observations in Standard Cosmology such as Big Bang Nucleosynthesis but small enough below the DM mass for the DM production. We analyze the impact of the model parameters including the extra gauge coupling and the reheating temperature on the DM relic density, collider bounds and DM direct and indirect detection experiments. Our results reveal a strong correlation between the DM mass (MWD) and the reheating temperature (TR) with ratio of around TR/MWD ∼ 0.1 to obtain correct DM density for detectable interaction strength. The decay processes are generally subdominant for the DM production but they can be important when kinematically allowed and the DM mass is close to half of the Higgses mass. The DM production with DM masses below 100 GeV is driven primarily by the scatterings of the SM fermions and Higgses decay whereas the case with higher DM masses is achieved mainly due to the Higgses scatterings. The enhanced coupling for the strong freeze-in in our framework enables potential detection prospects in direct and indirect detections and collider experiments. The parameter space of the model has already been explored partly by the current direct detection experiments and it can be explored further by future experiments such as Darwin. On the other hand, the indirect detection experiments in the current and near future are not sensitive enough to test our model.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"24 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144329227","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}