Pub Date : 2026-02-10DOI: 10.1088/1475-7516/2026/02/026
Jason Arakawa, Muhammad H. Zaheer, Volodymyr Takhistov, Marianna S. Safronova, Joshua Eby and Charles Cheung
Ultralight bosonic (ULB) fields with mass mϕ ≪ 1 eV often arise in theories beyond the Standard Model (SM). If such fields exist, violent astrophysical events that result in emission of gravitational wave, photon, or neutrino signals could also produce bursts of high-density relativistic ULB fields. Detection of such ULB fields in terrestrial or space-based laboratories correlated with other signals from transient astrophysical events opens a novel avenue for multimessenger astronomy. We show that quantum sensors are particularly well-suited to observe emitted scalar and pseudoscalar axion-like ULB fields coupled to SM. We demonstrate that multimessenger astronomy with ULB fields is possible even when accounting for matter screening effects.
{"title":"Multimessenger astronomy beyond the Standard Model: New window from quantum sensors","authors":"Jason Arakawa, Muhammad H. Zaheer, Volodymyr Takhistov, Marianna S. Safronova, Joshua Eby and Charles Cheung","doi":"10.1088/1475-7516/2026/02/026","DOIUrl":"https://doi.org/10.1088/1475-7516/2026/02/026","url":null,"abstract":"Ultralight bosonic (ULB) fields with mass mϕ ≪ 1 eV often arise in theories beyond the Standard Model (SM). If such fields exist, violent astrophysical events that result in emission of gravitational wave, photon, or neutrino signals could also produce bursts of high-density relativistic ULB fields. Detection of such ULB fields in terrestrial or space-based laboratories correlated with other signals from transient astrophysical events opens a novel avenue for multimessenger astronomy. We show that quantum sensors are particularly well-suited to observe emitted scalar and pseudoscalar axion-like ULB fields coupled to SM. We demonstrate that multimessenger astronomy with ULB fields is possible even when accounting for matter screening effects.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"45 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2026-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146145913","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}
Pub Date : 2026-02-10DOI: 10.1088/1475-7516/2026/02/027
Serena Gambino, Roberto Giambò and Orlando Luongo
We investigate relativistic Bondi accretion in the Simpson-Visser spacetime, which, via a single parameter ℓ, interpolates between the Schwarzschild, regular black hole, extremal and wormhole regimes. First, we analyse the neutral Simpson-Visser geometry, recovering Schwarzschild at ℓ=0, and then its charged extension of the Reissner-Nordström metric. In both these cases, we derive the conservation equations and analyse two representative fluid models: a barotropic perfect fluid and a constituent with an exponential density profile. By varying the parameters across regimes, we locate critical (sonic) points and integrate velocity, density, and pressure profiles. Although near-horizon inflow velocities are similar across the different solutions, we find that the critical radius, as well as the resulting accretion rates and luminosities, change significantly depending on the value of the parameter and the type of fluid. Remarkably, the barotropic and exponential cases exhibit different trends in the outer regions. Moreover, by extending the analysis to the charged SV spacetime, we find that the presence of a central charge Q produces additional, albeit modest, shifts in the sonic radius which, in combination with those induced by the regularisation parameter ℓ, could provide a double observational marker. In particular, while ℓ acts predominantly on the position of the critical point, in the barotropic fluid case, the electromagnetic contribution of Q slightly dampens the inflow velocity near the horizon.
{"title":"Bondi accretion disc luminosity around neutral and charged Simpson-Visser spacetimes","authors":"Serena Gambino, Roberto Giambò and Orlando Luongo","doi":"10.1088/1475-7516/2026/02/027","DOIUrl":"https://doi.org/10.1088/1475-7516/2026/02/027","url":null,"abstract":"We investigate relativistic Bondi accretion in the Simpson-Visser spacetime, which, via a single parameter ℓ, interpolates between the Schwarzschild, regular black hole, extremal and wormhole regimes. First, we analyse the neutral Simpson-Visser geometry, recovering Schwarzschild at ℓ=0, and then its charged extension of the Reissner-Nordström metric. In both these cases, we derive the conservation equations and analyse two representative fluid models: a barotropic perfect fluid and a constituent with an exponential density profile. By varying the parameters across regimes, we locate critical (sonic) points and integrate velocity, density, and pressure profiles. Although near-horizon inflow velocities are similar across the different solutions, we find that the critical radius, as well as the resulting accretion rates and luminosities, change significantly depending on the value of the parameter and the type of fluid. Remarkably, the barotropic and exponential cases exhibit different trends in the outer regions. Moreover, by extending the analysis to the charged SV spacetime, we find that the presence of a central charge Q produces additional, albeit modest, shifts in the sonic radius which, in combination with those induced by the regularisation parameter ℓ, could provide a double observational marker. In particular, while ℓ acts predominantly on the position of the critical point, in the barotropic fluid case, the electromagnetic contribution of Q slightly dampens the inflow velocity near the horizon.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"35 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2026-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146146056","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}
Pub Date : 2026-02-10DOI: 10.1088/1475-7516/2026/02/030
Rutvik Ashish Mahajan, Raghunath Ghara, Nishant Deo and Arnab Mishra
We present an improved matched filter method for detecting large ionized regions in 21 cm observations of the Epoch of Reionization. In addition to detection, the method constrains the properties of these regions, offering insights into the underlying source populations. Extending a previously developed Bayesian framework, we replace the spherical filter with an eight-parameter spheroidal filter, enabling a more flexible characterization of ionized bubbles. This enhancement significantly improves both detectability and recovery of bubble orientations. For a representative reionization scenario with a mean ionization fraction of 0.4 at z = 7, we find that a 10σ detection of the largest ionized region can be achieved with ∼ 1 h of observation using the SKA-low AA4 and AA★ layouts. Our method can help identify regions in the observed field that host large ionized bubbles, making them prime targets for deeper follow-up observations.
{"title":"Enhancing the detectability of ionized regions during the Epoch of Reionization","authors":"Rutvik Ashish Mahajan, Raghunath Ghara, Nishant Deo and Arnab Mishra","doi":"10.1088/1475-7516/2026/02/030","DOIUrl":"https://doi.org/10.1088/1475-7516/2026/02/030","url":null,"abstract":"We present an improved matched filter method for detecting large ionized regions in 21 cm observations of the Epoch of Reionization. In addition to detection, the method constrains the properties of these regions, offering insights into the underlying source populations. Extending a previously developed Bayesian framework, we replace the spherical filter with an eight-parameter spheroidal filter, enabling a more flexible characterization of ionized bubbles. This enhancement significantly improves both detectability and recovery of bubble orientations. For a representative reionization scenario with a mean ionization fraction of 0.4 at z = 7, we find that a 10σ detection of the largest ionized region can be achieved with ∼ 1 h of observation using the SKA-low AA4 and AA★ layouts. Our method can help identify regions in the observed field that host large ionized bubbles, making them prime targets for deeper follow-up observations.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"314 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2026-02-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146146057","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}
Pub Date : 2026-02-09DOI: 10.1088/1475-7516/2026/02/025
V.T. Voronchev
The present paper completes a series of our works on non-thermal nuclear processes in big bang nucleosynthesis (BBN) started in JCAP 05 (2008) 010 (Part I) and 05 (2009) 001 (Part II). The processes are triggered by non-Maxwellian particles naturally born in the main BBN reactions. Half of these reactions generate fast particles k+ (= n,p,t,3He,α). The other half, being radiative capture processes, produce slow nuclei k- (= d,t,3He,7Li,7Be) which can undergo (k-,n) reactions with neutrons having large cross sections. The particle production rate Rk, thermalization time τk, and effective number density nk are determined. It is shown that at the early stage of BBN the number density of slow deuterons (respectively, 3He) can exceed the number densities of Maxwellian 7Li and 7Be (respectively, 7Be) ions. To clarify the overall non-Maxwellian effect on BBN, both types of the non-Maxwellian particles are taken into account in the reaction network. Particular attention is paid to two-step sequential processes like p(n,γ)d-(n,γ)t, d(p,γ)3He-(n,p)t, t(α,γ)7Li-(n,γ)8Li, 3He(α,γ)7Be-(n,p)7Li, d(t,α)n+(A,n)a1a2, and d(3He,α)p+(A,p)a1a2 with (A,a1,a2) = (7Li,t,α) and (7Be,3He,α). It is obtained that the non-Maxwellian particles can selectively affect the element abundances, e.g., improve the prediction on 7Li/H by ∼ 1.5% and at the same time leave unchanged the 4He abundance. The main conclusion however is that these particles are unable to significantly change the standard picture of BBN in general, and provide a pathway toward a solution of the cosmological lithium problem in particular.
{"title":"Non-thermal processes in standard big bang nucleosynthesis. Part III. Reactions with slow nuclei and the overall effect","authors":"V.T. Voronchev","doi":"10.1088/1475-7516/2026/02/025","DOIUrl":"https://doi.org/10.1088/1475-7516/2026/02/025","url":null,"abstract":"The present paper completes a series of our works on non-thermal nuclear processes in big bang nucleosynthesis (BBN) started in JCAP 05 (2008) 010 (Part I) and 05 (2009) 001 (Part II). The processes are triggered by non-Maxwellian particles naturally born in the main BBN reactions. Half of these reactions generate fast particles k+ (= n,p,t,3He,α). The other half, being radiative capture processes, produce slow nuclei k- (= d,t,3He,7Li,7Be) which can undergo (k-,n) reactions with neutrons having large cross sections. The particle production rate Rk, thermalization time τk, and effective number density nk are determined. It is shown that at the early stage of BBN the number density of slow deuterons (respectively, 3He) can exceed the number densities of Maxwellian 7Li and 7Be (respectively, 7Be) ions. To clarify the overall non-Maxwellian effect on BBN, both types of the non-Maxwellian particles are taken into account in the reaction network. Particular attention is paid to two-step sequential processes like p(n,γ)d-(n,γ)t, d(p,γ)3He-(n,p)t, t(α,γ)7Li-(n,γ)8Li, 3He(α,γ)7Be-(n,p)7Li, d(t,α)n+(A,n)a1a2, and d(3He,α)p+(A,p)a1a2 with (A,a1,a2) = (7Li,t,α) and (7Be,3He,α). It is obtained that the non-Maxwellian particles can selectively affect the element abundances, e.g., improve the prediction on 7Li/H by ∼ 1.5% and at the same time leave unchanged the 4He abundance. The main conclusion however is that these particles are unable to significantly change the standard picture of BBN in general, and provide a pathway toward a solution of the cosmological lithium problem in particular.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"59 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2026-02-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146138358","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}
Pub Date : 2026-02-06DOI: 10.1088/1475-7516/2026/02/021
Francesco Rescigno and Alberto Salvio
Theories with radiative symmetry breaking (RSB) lead to first-order phase transitions and the production of gravitational waves as well as primordial black holes if the supercooling period lasted long enough. Here we explain how to efficiently reheat the universe after such period in the above-mentioned class of theories. Two cases are possible, depending on whether the RSB scale is much larger than the electroweak (EW) symmetry breaking scale or not. When it is, the dominant reheating mechanism can be the decays of the field responsible for RSB in the Standard Model (SM) sector. We point out that in a similar way dark matter (DM) can be produced and we analyze in some detail the case of a sterile-neutrino, finding that the full DM abundance is reproduced when this particle is at the 102 MeV scale in a well-motivated SM completion. When the RSB scale is not much larger than the EW symmetry breaking scale, we find that efficient reheating always occurs when the energy density of the false vacuum is first entirely transferred to a dark photon and then to SM fermions via dark-photon decays.
{"title":"Reheating after the supercooled phase transitions with radiative symmetry breaking","authors":"Francesco Rescigno and Alberto Salvio","doi":"10.1088/1475-7516/2026/02/021","DOIUrl":"https://doi.org/10.1088/1475-7516/2026/02/021","url":null,"abstract":"Theories with radiative symmetry breaking (RSB) lead to first-order phase transitions and the production of gravitational waves as well as primordial black holes if the supercooling period lasted long enough. Here we explain how to efficiently reheat the universe after such period in the above-mentioned class of theories. Two cases are possible, depending on whether the RSB scale is much larger than the electroweak (EW) symmetry breaking scale or not. When it is, the dominant reheating mechanism can be the decays of the field responsible for RSB in the Standard Model (SM) sector. We point out that in a similar way dark matter (DM) can be produced and we analyze in some detail the case of a sterile-neutrino, finding that the full DM abundance is reproduced when this particle is at the 102 MeV scale in a well-motivated SM completion. When the RSB scale is not much larger than the EW symmetry breaking scale, we find that efficient reheating always occurs when the energy density of the false vacuum is first entirely transferred to a dark photon and then to SM fermions via dark-photon decays.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"83 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2026-02-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146135505","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}
Pub Date : 2026-02-06DOI: 10.1088/1475-7516/2026/02/020
Federico Cima and Francesco D'Eramo
Observations of the hydrogen hyperfine transition through the 21 cm line near the end of the cosmic dark ages provide unique opportunities to probe new physics. In this work, we investigate the potential of the sky-averaged 21 cm signal to constrain metastable particles produced in the early universe that decay at later times, thereby modifying the thermal and ionization history of the intergalactic medium. The study begins by extending previous analyses of decaying dark matter (DM), incorporating back-reaction effects and tightening photon decay constraints down to DM masses as low as 20.4 eV. The focus then shifts to non-minimal dark sectors with multiple interacting components. The analysis covers two key scenarios: a hybrid setup comprising a stable cold DM component alongside a metastable sub-component, and a two-component dark sector of nearly degenerate states with a metastable heavier partner. A general parameterization based on effective mass spectra and fractional densities allows for a model-independent study. The final part presents two explicit realizations: an axion-like particle coupled to photons, and pseudo-Dirac DM interacting via vector portals or electromagnetic dipoles. These scenarios illustrate how 21 cm cosmology can set leading bounds and probe otherwise inaccessible regions of parameter space.
{"title":"Probing non-minimal dark sectors via the 21 cm line at cosmic dawn","authors":"Federico Cima and Francesco D'Eramo","doi":"10.1088/1475-7516/2026/02/020","DOIUrl":"https://doi.org/10.1088/1475-7516/2026/02/020","url":null,"abstract":"Observations of the hydrogen hyperfine transition through the 21 cm line near the end of the cosmic dark ages provide unique opportunities to probe new physics. In this work, we investigate the potential of the sky-averaged 21 cm signal to constrain metastable particles produced in the early universe that decay at later times, thereby modifying the thermal and ionization history of the intergalactic medium. The study begins by extending previous analyses of decaying dark matter (DM), incorporating back-reaction effects and tightening photon decay constraints down to DM masses as low as 20.4 eV. The focus then shifts to non-minimal dark sectors with multiple interacting components. The analysis covers two key scenarios: a hybrid setup comprising a stable cold DM component alongside a metastable sub-component, and a two-component dark sector of nearly degenerate states with a metastable heavier partner. A general parameterization based on effective mass spectra and fractional densities allows for a model-independent study. The final part presents two explicit realizations: an axion-like particle coupled to photons, and pseudo-Dirac DM interacting via vector portals or electromagnetic dipoles. These scenarios illustrate how 21 cm cosmology can set leading bounds and probe otherwise inaccessible regions of parameter space.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"30 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2026-02-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146135501","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}
Pub Date : 2026-02-06DOI: 10.1088/1475-7516/2026/02/022
Zhiyao Lu, Lian-Tao Wang and Huangyu Xiao
We use the precision measurements of the arrival time differences of the same fast radio burst (FRB) source along multiple sightlines to measure the primordial power spectrum and Non-Gaussianities. The anticipated experiment requires a sightline separation of 100 AU, achieved by sending three or more radio telescopes to the outer solar system. The Shapiro time delays, measured relatively between different telescopes, are sensitive to the gradient field of the gravitational potential between different sightlines. Since the arrival time difference is independent of when the transient signal is emitted from the source, every measurement of the detected FRB source can be correlated. With enough FRB sources discovered, we can map the gravitational potential across the sky. We further calculate the two-point and three-point correlation function of the arrival time difference between telescopes for different FRB sources in the sky. If 104 FRBs were to be detected, our results suggest that this technique can test the inflationary scale-invariant power spectrum down to ∼ 103 Mpc-1 and primordial Non-Gaussianities at a level of fNL ∼ 1.
{"title":"Probing primordial power spectrum and non-Gaussianities with fast radio bursts","authors":"Zhiyao Lu, Lian-Tao Wang and Huangyu Xiao","doi":"10.1088/1475-7516/2026/02/022","DOIUrl":"https://doi.org/10.1088/1475-7516/2026/02/022","url":null,"abstract":"We use the precision measurements of the arrival time differences of the same fast radio burst (FRB) source along multiple sightlines to measure the primordial power spectrum and Non-Gaussianities. The anticipated experiment requires a sightline separation of 100 AU, achieved by sending three or more radio telescopes to the outer solar system. The Shapiro time delays, measured relatively between different telescopes, are sensitive to the gradient field of the gravitational potential between different sightlines. Since the arrival time difference is independent of when the transient signal is emitted from the source, every measurement of the detected FRB source can be correlated. With enough FRB sources discovered, we can map the gravitational potential across the sky. We further calculate the two-point and three-point correlation function of the arrival time difference between telescopes for different FRB sources in the sky. If 104 FRBs were to be detected, our results suggest that this technique can test the inflationary scale-invariant power spectrum down to ∼ 103 Mpc-1 and primordial Non-Gaussianities at a level of fNL ∼ 1.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"107 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2026-02-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146135511","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}
Pub Date : 2026-02-06DOI: 10.1088/1475-7516/2026/02/018
Katsuki Aoki, Tomohiro Fujita, Ryodai Kawaguchi and Kazuki Yanagihara
When a (non-)Abelian gauge field acquires an isotropic background configuration during inflation, strong gravitational waves (GWs) with parity-violating polarization, known as chiral GWs, can be produced in addition to the intrinsic unpolarized GWs. However, previous studies have analyzed individual models, leaving the generality of this phenomenon unclear. To perform a model-independent analysis, we construct an effective field theory (EFT) of chiral GWs by extending the EFT of inflation and incorporating gauge fields. The resulting action unifies inflationary models with a SU(2) gauge field, such as chromo-natural inflation and gauge-flation, and ones with a triplet of U(1) gauge fields, systematically encompassing all possible GW production mechanisms consistent with the symmetry breaking induced by the gauge field background. We find that chiral GWs are generically and inevitably produced, provided that the effective energy density of the background gauge field is positive and the gauge kinetic function is not fine-tuned to a specific time dependence. This EFT offers a useful foundation for future phenomenological studies as well as for deepening our theoretical understanding of chiral GWs.
{"title":"Effective field theory of chiral gravitational waves","authors":"Katsuki Aoki, Tomohiro Fujita, Ryodai Kawaguchi and Kazuki Yanagihara","doi":"10.1088/1475-7516/2026/02/018","DOIUrl":"https://doi.org/10.1088/1475-7516/2026/02/018","url":null,"abstract":"When a (non-)Abelian gauge field acquires an isotropic background configuration during inflation, strong gravitational waves (GWs) with parity-violating polarization, known as chiral GWs, can be produced in addition to the intrinsic unpolarized GWs. However, previous studies have analyzed individual models, leaving the generality of this phenomenon unclear. To perform a model-independent analysis, we construct an effective field theory (EFT) of chiral GWs by extending the EFT of inflation and incorporating gauge fields. The resulting action unifies inflationary models with a SU(2) gauge field, such as chromo-natural inflation and gauge-flation, and ones with a triplet of U(1) gauge fields, systematically encompassing all possible GW production mechanisms consistent with the symmetry breaking induced by the gauge field background. We find that chiral GWs are generically and inevitably produced, provided that the effective energy density of the background gauge field is positive and the gauge kinetic function is not fine-tuned to a specific time dependence. This EFT offers a useful foundation for future phenomenological studies as well as for deepening our theoretical understanding of chiral GWs.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"72 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2026-02-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146135538","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}
Pub Date : 2026-02-06DOI: 10.1088/1475-7516/2026/02/024
Odelia V. Hartl, Evan Vienneau, Evan Batteas, Addy J. Evans, Nassim Bozorgnia and Louis E. Strigari
We examine velocity-dependent dark matter annihilation in subhalos using a sample of six Milky Way-like galaxies from the Aurgia simulation suite. We quantify the enhancement in the annihilation rate in subhalos when including the contribution from particles in the smooth component of the halo that overlap with the subhalos. The enhancement in the annihilation rate scales with the smooth component of the host halo dark matter density, and is evident for subhalos over the resolvable mass range. Maximal enhancement factors are ∼ 48 for p-wave models, and ∼ 37,000 for d-wave models. For p and d-wave annihilation models, ∼ 13 and ∼ 6 subhalos, respectively, across all six host halos have emission from dark matter annihilation in their direction that is above the foreground emission from the smooth dark matter component, and would therefore be resolvable as sources. Such subhalos with the most significant enhancement factors tend to be on the lower end of the mass range and located closer to the center of the host galaxy. We provide a prescription to calculate the enhancement for subhalos as a function of distance from the Galactic center, and use this to examine the impact on dark matter limits from a couple of example dwarf spheroidals. We show that, including the enhancement factors, limits from individual dwarf spheroidals are at a cross section scale that may approach those derived from the Galactic center.
{"title":"Enhancements in velocity-dependent dark matter annihilation in Galactic subhalos","authors":"Odelia V. Hartl, Evan Vienneau, Evan Batteas, Addy J. Evans, Nassim Bozorgnia and Louis E. Strigari","doi":"10.1088/1475-7516/2026/02/024","DOIUrl":"https://doi.org/10.1088/1475-7516/2026/02/024","url":null,"abstract":"We examine velocity-dependent dark matter annihilation in subhalos using a sample of six Milky Way-like galaxies from the Aurgia simulation suite. We quantify the enhancement in the annihilation rate in subhalos when including the contribution from particles in the smooth component of the halo that overlap with the subhalos. The enhancement in the annihilation rate scales with the smooth component of the host halo dark matter density, and is evident for subhalos over the resolvable mass range. Maximal enhancement factors are ∼ 48 for p-wave models, and ∼ 37,000 for d-wave models. For p and d-wave annihilation models, ∼ 13 and ∼ 6 subhalos, respectively, across all six host halos have emission from dark matter annihilation in their direction that is above the foreground emission from the smooth dark matter component, and would therefore be resolvable as sources. Such subhalos with the most significant enhancement factors tend to be on the lower end of the mass range and located closer to the center of the host galaxy. We provide a prescription to calculate the enhancement for subhalos as a function of distance from the Galactic center, and use this to examine the impact on dark matter limits from a couple of example dwarf spheroidals. We show that, including the enhancement factors, limits from individual dwarf spheroidals are at a cross section scale that may approach those derived from the Galactic center.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"224 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2026-02-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146135507","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}
Pub Date : 2026-02-06DOI: 10.1088/1475-7516/2026/02/019
Yo Toda and Osamu Seto
Primarily motivated by the Hubble tension, we analyze the varying electron mass model and axionlike early dark energy model (EDE) using baryon acoustic oscillation data from DESI DR2 data and including the recent results from ACT DR6. Our analysis indicates that me/me0 = 1.0078 ± 0.0047 in the varying me model, me/me0 = 1.0034 ± 0.0050 and α/α0 = 1.0039 ± 0.0016 in the varying me+α model, and the energy fraction of EDE is constrained as fEDE < 0.014. Since those cosmological models fit with different spectral index ns, we show the posterior of those models on the (ns-r) plane and point out that, for example, Starobinsky inflation works for varying electron mass model while the standard supersymmetric hybrid inflation is preferred in the EDE model.
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