Journal of Cosmology and Astroparticle Physics最新文献

{"title":"Investigating primordial black hole accretion through cosmic optical depth","authors":"Zi-Xuan Zhang, Junsong Cang, Yu Gao and Hong Li","doi":"10.1088/1475-7516/2025/07/027","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/07/027","url":null,"abstract":"Primordial black holes (PBH) accretion in the late Universe can lead to significant mass growth. A larger mass further accelerates the accretion radiation output for PBHs with initial masses greater than one solar mass, potentially leading to a stringent energy-dumping constraint derived from observations of the cosmic microwave background. The energy injected via PBH accretion is capable of ionizing and heating the intergalactic medium (IGM), ultimately affecting the optical depth of cosmic reionization and the 21-cm signal. This work investigates primordial black hole mass growth using the Bondi-Hoyle accretion model and accounts for additional ionization and heating induced by PBHs. We derive stringent PBH abundance limits using an upper limit on optical depth set by Planck 2018 CMB measurements. We find that accretion growth significantly strengthens late-time observational constraints for primordial black holes with initial masses ranging from several solar masses up to 104 solar masses. The PBH fraction of the Universe's unobserved mass content can be constrained to fPBH, ini ∼ 10-2 to 10-7 in this mass range, and when accounting for mass evolution our constraints can be strengthened by up to one order of magnitude. In addition, we show that PBH mass growth will lead to an observable impact on the predicted hydrogen 21-cm brightness temperature.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"31 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-07-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144593936","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 minimal axio-dilaton dark sector","authors":"Adam Smith, Maria Mylova, Philippe Brax, Carsten van de Bruck, C.P. Burgess and Anne-Christine Davis","doi":"10.1088/1475-7516/2025/07/023","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/07/023","url":null,"abstract":"In scalar-tensor theories it is the two-derivative sigma-model interactions that like to compete at low energies with the two-derivative interactions of General Relativity (GR) — at least once the dangerous zero-derivative terms of the scalar potential are suppressed (such as by a shift symmetry). But nontrivial two-derivative interactions require at least two scalars to exist and so never arise in the single-scalar models most commonly explored. Axio-dilaton models provide a well-motivated minimal class of models for which these self-interactions can be explored. We review this class of models and investigate whether these minimal two fields can suffice to describe both Dark Matter and Dark Energy. We find that they can — the axion is the Dark Matter and the dilaton is the Dark Energy — and that they robustly predict several new phenomena for the CMB and structure formation that can be sought in observations. These include specific types of Dark Energy evolution and small space- and time-dependent changes to particle masses post-recombination that alter the Integrated Sachs-Wolfe effect, cause small changes to structure growth and more.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"8 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-07-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144593932","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":"Addendum: Fitting the DESI BAO data with dark energy driven by the Cohen-Kaplan-Nelson bound","authors":"Patrick Adolf, Martin Hirsch, Sara Krieg, Heinrich Päs and Mustafa Tabet","doi":"10.1088/1475-7516/2025/07/a01","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/07/a01","url":null,"abstract":"Motivated by the recent Year-2 data release of the DESI collaboration, we update our results on time-varying dark energy models driven by the Cohen-Kaplan-Nelson bound. The previously found preference of time-dependent dark energy models compared to ΛCDM is further strengthend by the new data release. For our particular models, we find that this preference increases up to ≈ 2.6 σ depending on the used supernova dataset.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"34 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-07-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144593928","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":"Calibration requirements for epoch of reionization 21-cm signal observations. Part IV. Bias and variance with time and frequency correlated residual gains","authors":"Saikat Gayen, Jais Kumar, Prasun Dutta, Khandakar Md Asif Elahi, Samir Choudhuri and Nirupam Roy","doi":"10.1088/1475-7516/2025/07/024","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/07/024","url":null,"abstract":"Observation of multifrequency angular power spectrum of the redshifted 21-cm brightness temperature fluctuation from the neutral hydrogen holds the key to understand the structure formation and its evolution during the reionization and post-reionization era. A major challenge in observing the neutral hydrogen arises from presence of strong foreground signals in the frequency range of interest. Mitigating the direct effect of foregrounds are being addressed through various techniques in literature. An additional second order effect arises, in presence of foreground, with limited accuracy in time and frequency dependent gain calibrations. This manifests as the residual gain and bandpass error in the observed data, introduces bias and increases uncertainty in the estimates of multifrequency angular power spectrum. In this work, we present an analytic method to estimate the bias and excess uncertainty in the estimates of multifrequency angular power spectrum in presence of residual gain and bandpass errors. We use this framework to estimate the effect of these errors for detection of redshifted 21-cm emission from a redshift of ∼ 8 with the upcoming SKA1-Low. Due to the high baseline density at the required range of angular multipoles, the SKA1-Low is found to be a tuned instrument for the redshifted 21-cm signal detection. We find that, there are scenario with residual gain and bandpass errors where there can be significant bias in these estimates. Certain foreground mitigation strategies, is expected to reduce a part of the bias. The detailed study of different aspects of gain and bandpass errors and their relative effects are discussed. We find, with assumed models of gain and bandpass errors, signal detection is possible at this redshift with 128 hours of observations. However, to achieve this one needs to have better calibration accuracy than present day interferometers.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"1 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-07-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144593933","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":"Gravitational wave lensing: probing Fuzzy Dark Matter with LISA","authors":"Shashwat Singh, Guilherme Brando, Stefano Savastano and Miguel Zumalacárregui","doi":"10.1088/1475-7516/2025/07/025","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/07/025","url":null,"abstract":"Gravitational lensing is a universal phenomenon: it affects both gravitational waves (GWs) and electromagnetic signals travelling through the gravitational field of a massive object. In this work, we explore the prospects of observing lensed GW signals from the mergers of massive black holes, lensed by dark matter halos composed of Fuzzy Dark Matter (FDM), which form dense cores known as solitons. We focus on wave optics phenomena, where frequency-dependent signatures can be observed in the weak lensing regime (i.e. single-image). Our results show that lensing diffraction signatures differ for low-mass halos in FDM, and can reveal the presence of a solitonic core. Furthermore, we demonstrate that FDM and cold dark matter profiles can be distinguished in GW signals from binary massive black hole mergers, which will be observed by the Laser Interferometer Space Antenna (LISA) mission. However, the dense solitonic core does not substantially enhance the detectability of FDM halos at large source-lens offsets, relative to standard cold dark matter. Our analysis confirms FDM halos as a promising signature of dark matter on GW observations.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"109 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-07-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144593934","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":"The evolving role of astrophysical modelling in dark matter halo relaxation response","authors":"Premvijay Velmani and Aseem Paranjape","doi":"10.1088/1475-7516/2025/07/026","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/07/026","url":null,"abstract":"We study the change in the radial distribution of dark matter within haloes in response to baryonic astrophysical processes in galaxies at different epochs, investigating the role of astrophysical modeling in cosmological hydrodynamic simulations in producing the response. We find that the linear quasi-adiabatic relaxation with additional dependence on the halo-centric distance provides a good description not only at z = 0, but also at an earlier epoch (z = 1) in the IllustrisTNG simulation suite, with parameters being more universal across a much larger variety of haloes at z = 1 than at z = 0. Through systematic analysis of a large collection of simulations from the CAMELS project, we find that the baryonic prescriptions for both AGN and stellar feedbacks have a strong influence on the relaxation response of the dark matter halo. In particular, only the parameters controlling the overall feedback energy flux have an effect on the relaxation response, while the wind speed and burstiness have negligible effect on the relaxation at a fixed amount of energy flux. However, the exact role of these parameters on the relaxation depends on the redshift. We also study the role of a variety of baryonic astrophysical processes through the EAGLE physics variation simulations. While these depict a similar picture regarding the importance of feedback effects, they also reveal that the gas equation of state has one of the strongest influences on the relaxation response, consistent with the expectation from self-similar analyses.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"37 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-07-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144593935","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":"DESI 2024 VII: cosmological constraints from the full-shape modeling of clustering measurements","authors":"A.G. Adame, J. Aguilar, S. Ahlen, S. Alam, D.M. Alexander, C. Allende Prieto, M. Alvarez, O. Alves, A. Anand, U. Andrade, E. Armengaud, S. Avila, A. Aviles, H. Awan, B. Bahr-Kalus, S. Bailey, C. Baltay, A. Bault, J. Behera, S. BenZvi, F. Beutler, D. Bianchi, C. Blake, R. Blum, M. Bonici, S. Brieden, A. Brodzeller, D. Brooks, E. Buckley-Geer, E. Burtin, R. Calderon, R. Canning, A. Carnero Rosell, R. Cereskaite, J.L. Cervantes-Cota, S. Chabanier, E. Chaussidon, J. Chaves-Montero, D. Chebat, S. Chen, X. Chen, T. Claybaugh, S. Cole, A. Cuceu, T.M. Davis, K. Dawson, A. de la Macorra, A. de Mattia, N. Deiosso, A. Dey, B. Dey, Z. Ding, P. Doel, J. Edelstein, S. Eftekharzadeh, D.J. Eisenstein, W. Elbers, A. Elliott, P. Fagrelius, K. Fanning, S. Ferraro, J. Ereza, N. Findlay, B. Flaugher, A. Font-Ribera, D. Forero-Sánchez, J.E. Forero-Romero, C.S. Frenk, C. Garcia-Quintero, L.H. Garrison, E. Gaztañaga, H. Gil-Marín, S.Gontcho A. Gontcho, A.X. Gonzalez-Morales, V. Gonzalez-Perez, C. Go..","doi":"10.1088/1475-7516/2025/07/028","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/07/028","url":null,"abstract":"We present cosmological results from the measurement of clustering of galaxy, quasar and Lyman-α forest tracers from the first year of observations with the Dark Energy Spectroscopic Instrument (DESI Data Release 1). We adopt the full-shape (FS) modeling of the power spectrum, including the effects of redshift-space distortions, in an analysis which has been thoroughly validated in a series of supporting papers as summarised in [1]. We combine the full-shape information with DESI's DR1 constraints from the baryon acoustic oscillations (BAO) of these tracers. In the flat ΛCDM cosmological model, DESI (FS+BAO), combined with a baryon density prior from Big Bang Nucleosynthesis and a weak prior on the scalar spectral index, determines matter density to Ωm = 0.2962 ± 0.0095, and the amplitude of mass fluctuations to σ8 = 0.842 ± 0.034. The addition of the cosmic microwave background (CMB) data tightens these constraints to Ωm = 0.3056 ± 0.0049 and σ8 = 0.8121 ± 0.0053, while further addition of the joint clustering and lensing analysis from the Dark Energy Survey Year-3 (DESY3) data further improves these measurements, and leads to a 0.4% determination of the Hubble constant, H0 = (68.40 ± 0.27) km s-1 Mpc-1. In models with a time-varying dark energy equation of state parametrised by w0 and wa, combinations of DESI (FS+BAO) with CMB and type Ia supernovae continue to show the preference, previously found in the DESI DR1 BAO analysis, for w0 > -1 and wa < 0 with similar levels of significance. DESI data, in combination with the CMB, improve the upper limits on the sum of the neutrino masses relative to the case when only the DR1 BAO was available, giving ∑mν < 0.071 eV at 95% confidence. We finally constrain deviations from general relativity represented by two modified gravity parameters. DESI (FS+BAO) data alone measure the parameter that controls the clustering of massive particles, μ0 = 0.11+0.45-0.54, in agreement with the zero value predicted by general relativity. The combination of DESI with the CMB and the clustering and lensing analysis from DESY3 constrains both modified-gravity parameters, giving μ0 = 0.04 ± 0.22 and Σ0 = 0.044 ± 0.047, again in agreement with general relativity.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"691 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-07-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144593959","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":"Dark dwarfs: dark matter-powered sub-stellar objects awaiting discovery at the galactic center","authors":"Djuna Croon, Jeremy Sakstein, Juri Smirnov and Jack Streeter","doi":"10.1088/1475-7516/2025/07/019","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/07/019","url":null,"abstract":"We investigate the effects of dark matter annihilation on objects with masses close to the sub-stellar limit, finding that the minimum mass for stable hydrogen burning is larger than the ∼ 0.075M⊙ value predicted in the Standard Model. Below this limit, cooling brown dwarfs evolve into stable dark matter-powered objects that we name dark dwarfs. The timescale of this transition depends on the ambient dark matter density ρDM and circular velocity vDM but is independent of the dark matter mass. We predict a population of dark dwarfs close to the galactic center, where the dark matter density is expected to be ρDM ≳ 103 GeV/cm3. At larger galactic radii the dark matter density is too low for these objects to have yet formed within the age of the universe. Dark dwarfs retain their initial lithium-7 in mass ranges where brown/red dwarfs would destroy it, providing a method for detecting them.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"41 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-07-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144568527","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":"Improving cosmic birefringence constraints via delensing","authors":"Anto Idicherian Lonappan","doi":"10.1088/1475-7516/2025/07/009","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/07/009","url":null,"abstract":"We present a study on using delensing to enhance cosmic birefringence measurements based on full-sky, map-based simulations. In our analysis, we neglect foreground contamination and instrumental systematics to isolate the intrinsic impact of delensing on both isotropic and anisotropic birefringence. For the isotropic case, assuming a constant rotation angle of β = 0.35°, delensing reduces the lensing-induced variance in the EB power spectrum, yielding an improvement in sensitivity of approximately 10% at 6μK-arcmin noise for ℓ < 200 and 25–40% at lower noise levels for ℓ < 1000. For the anisotropic case, using simulations at 1 μK-arcmin noise, we reconstruct the birefringence angle for a scale-invariant spectrum and mitigate lensing bias by delensing, achieving a 50% reduction in the leading N(0) bias and a 30% improvement in the constraints on the amplitude ACB. Our results demonstrate that delensing is an effective tool for enhancing the detectability of subtle parity-violating signals in the CMB with forthcoming experiments such as the Simons Observatory, CMB-S4, and LiteBIRD.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"29 1","pages":"009"},"PeriodicalIF":6.4,"publicationDate":"2025-07-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144565975","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":"Pz Cats: photometric redshift catalogs based on DES Y3 BAO sample","authors":"Paula S. Ferreira and Ribamar R.R. Reis","doi":"10.1088/1475-7516/2025/07/008","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/07/008","url":null,"abstract":"Over the years, photometric redshift estimation (photo-z) has advanced through various methods. This study evaluates four distinct photo-z estimators — ANNz2, BPZ, ENF, and DNF — using the Dark Energy Survey Y3 BAO Sample. Unlike most studies, we explore selecting optimal galaxies based on their redshift Probability Distribution Function (PDF) by either reducing noise or identifying those approximating a Gaussian distribution. We cross-matched 25,760 galaxies drawn from four spectroscopic surveys with the photo-z sample to comprehend redshift bias and its 68th percentile σ68. The lowest σ for all estimators was found in the range 0.79 < zp < 0.85. Among the estimators, DNF exhibited the greatest bias, while ENF, ANNz2, and BPZ showed decreased precision outside 0.7 to 0.9 redshift range. To select galaxies with minimal bias, ANNz2 emerged as the most reliable algorithm across all criteria. PDFs selection significantly improves colour representation over the spectroscopic sample, underscoring the role of magnitude space in selection. While ANNz2 achieved superior precision, ENF poorly selected Gaussian PDFs, leaving few galaxies for LSS evaluation. Despite smooth PDFs, catastrophic redshift errors were present. Though DNF had the poorest precision, it offered enough galaxies for cosmological use. Subsampling galaxies with secondary peaks less than 30% of the main peak height, termed Small Peaks, showed ANNz2 excelled. The catalogs produced have been published as Pz Cats within the ZENODO repository.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"11 1","pages":"008"},"PeriodicalIF":6.4,"publicationDate":"2025-07-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144565974","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}