Pub Date : 2025-03-21DOI: 10.1088/1475-7516/2025/03/054
Sohan Kumar Jha
We consider Schwarzschild black hole (BH) embedded in a Dehnen-(1,4,0) type dark matter halo (DDM) with two additional parameters — core radius rs and core density ρs apart from mass M. We analyze the event horizon, photon orbits, and ISCO around DDM BHs and emphasize the impact of DDM parameters on them. Our study reveals that the presence of dark matter (DM) favourably impacts the radii of photon orbits, the innermost stable circular orbit (ISCO), and the event horizon. We find the expressions for specific energy and angular momentum for massive particles in time-like geodesics around DDM BH and investigate their dependence on DDM parameters. We display BH shadows for various values of core density and radius that reveal larger shadows cast by a Schwarzschild BH surrounded by DDM (SDDM) than a Schwarzschild BH in vacuum (SV). We then move on to study quasinormal modes (QNMs) with the help of the 6th order WKB method, the greybody factor using the semi-analytic bounds method, and the Hawking spectrum for scalar and electromagnetic perturbations. Core density and radius are found to have a significant impact on QNMs. Since QNMs for scalar and electromagnetic perturbations differ significantly, we can differentiate the two based on QNM observation. The greybody factor increases with core density and radius, whereas, the power emitted as Hawking radiation is adversely impacted by the presence of DM. We then study the weak gravitational lensing using the Gauss-Bonnet theorem and obtain the deflection angle with higher-order correction terms. Here, we see the deflection angle gets enhanced due to DM. Finally, we use bounds on the deviation from Schwarzschild, δ, reported by EHT for M87*, Keck, and VLTI observatories for SgrA* to gauge the viability of our model. Our model is found to be concordant with observations. This leads to the possibility of our galactic center being surrounded by DDM.
{"title":"Shadow, ISCO, quasinormal modes, Hawking spectrum, weak gravitational lensing, and parameter estimation of a Schwarzschild black hole surrounded by a Dehnen type dark matter halo","authors":"Sohan Kumar Jha","doi":"10.1088/1475-7516/2025/03/054","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/03/054","url":null,"abstract":"We consider Schwarzschild black hole (BH) embedded in a Dehnen-(1,4,0) type dark matter halo (DDM) with two additional parameters — core radius rs and core density ρs apart from mass M. We analyze the event horizon, photon orbits, and ISCO around DDM BHs and emphasize the impact of DDM parameters on them. Our study reveals that the presence of dark matter (DM) favourably impacts the radii of photon orbits, the innermost stable circular orbit (ISCO), and the event horizon. We find the expressions for specific energy and angular momentum for massive particles in time-like geodesics around DDM BH and investigate their dependence on DDM parameters. We display BH shadows for various values of core density and radius that reveal larger shadows cast by a Schwarzschild BH surrounded by DDM (SDDM) than a Schwarzschild BH in vacuum (SV). We then move on to study quasinormal modes (QNMs) with the help of the 6th order WKB method, the greybody factor using the semi-analytic bounds method, and the Hawking spectrum for scalar and electromagnetic perturbations. Core density and radius are found to have a significant impact on QNMs. Since QNMs for scalar and electromagnetic perturbations differ significantly, we can differentiate the two based on QNM observation. The greybody factor increases with core density and radius, whereas, the power emitted as Hawking radiation is adversely impacted by the presence of DM. We then study the weak gravitational lensing using the Gauss-Bonnet theorem and obtain the deflection angle with higher-order correction terms. Here, we see the deflection angle gets enhanced due to DM. Finally, we use bounds on the deviation from Schwarzschild, δ, reported by EHT for M87*, Keck, and VLTI observatories for SgrA* to gauge the viability of our model. Our model is found to be concordant with observations. This leads to the possibility of our galactic center being surrounded by DDM.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"34 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143675228","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 : 2025-03-21DOI: 10.1088/1475-7516/2025/03/050
Thomas C. Bachlechner, Kate Eckerle, Oliver Janssen and Matthew Kleban
Random axion theories with several hundred fields have enormous numbers of distinct meta-stable minima. A small fraction of these have vacuum energy compatible with current measurements of dark energy. The potential also contains regions suitable for inflation, and gives rise to a natural type of dark matter. First-order phase transitions from one minimum to the vicinity of another play the role of big bangs and produce many bubbles containing evolving Friedmann-Lemaître-Robertson-Walker universes. The great majority either collapse in a tiny fraction of a second, or expand exponentially forever as empty, structureless universes. However, restricting to those bubble universes that form non-linear structure at some time in their history we find cosmologies that look remarkably similar to ours. They undergo about 60 efolds of inflation, making them flat, homogeneous and isotropic, and endowing them with a nearly scale-invariant spectrum of primordial density perturbations with roughly the observed magnitude and tilt. They reheat after inflation to a period of radiation domination, followed by matter domination with roughly the observed abundance, followed by vacuum energy domination at roughly the observed density. These features are largely insensitive to the dimensionful and dimensionless parameters of the theory, which can be set to the grand unified scale and order one respectively. In our benchmark model we assume the number of high-scale contributions to the axion potential is not much larger than the amount of axions, and that there is a single field direction which is left massless by these contributions. The small value of dark energy ultimately comes from non-perturbative gravitational effects, giving ρDE ≈ Λ4 e-𝒪(1) × M_Pl/f, where f ≈ Λ ≈ 10-2MPl. Therefore, random axion landscapes can account for many of the apparently tuned features of our universe, including its current enormous size, age, and tiny energy densities compared to the scales of fundamental physics.
{"title":"The Axidental Universe","authors":"Thomas C. Bachlechner, Kate Eckerle, Oliver Janssen and Matthew Kleban","doi":"10.1088/1475-7516/2025/03/050","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/03/050","url":null,"abstract":"Random axion theories with several hundred fields have enormous numbers of distinct meta-stable minima. A small fraction of these have vacuum energy compatible with current measurements of dark energy. The potential also contains regions suitable for inflation, and gives rise to a natural type of dark matter. First-order phase transitions from one minimum to the vicinity of another play the role of big bangs and produce many bubbles containing evolving Friedmann-Lemaître-Robertson-Walker universes. The great majority either collapse in a tiny fraction of a second, or expand exponentially forever as empty, structureless universes. However, restricting to those bubble universes that form non-linear structure at some time in their history we find cosmologies that look remarkably similar to ours. They undergo about 60 efolds of inflation, making them flat, homogeneous and isotropic, and endowing them with a nearly scale-invariant spectrum of primordial density perturbations with roughly the observed magnitude and tilt. They reheat after inflation to a period of radiation domination, followed by matter domination with roughly the observed abundance, followed by vacuum energy domination at roughly the observed density. These features are largely insensitive to the dimensionful and dimensionless parameters of the theory, which can be set to the grand unified scale and order one respectively. In our benchmark model we assume the number of high-scale contributions to the axion potential is not much larger than the amount of axions, and that there is a single field direction which is left massless by these contributions. The small value of dark energy ultimately comes from non-perturbative gravitational effects, giving ρDE ≈ Λ4 e-𝒪(1) × M_Pl/f, where f ≈ Λ ≈ 10-2MPl. Therefore, random axion landscapes can account for many of the apparently tuned features of our universe, including its current enormous size, age, and tiny energy densities compared to the scales of fundamental physics.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"45 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143675235","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 : 2025-03-21DOI: 10.1088/1475-7516/2025/03/052
Garv Chauhan, Shunsaku Horiuchi, Patrick Huber and Ian M. Shoemaker
Sterile neutrinos can be produced through mixing with active neutrinos in the hot, dense core of a core-collapse supernova (SN). The standard bounds on the active-sterile mixing (sin2θ) from SN arise from SN1987A energy-loss, requiring Eloss < 1052 erg. In this work, we discuss a novel bound on sterile neutrino parameter space arising from the energy deposition through its decays inside the SN envelope. Using the observed underluminous SN IIP population, this energy deposition is constrained to be below ∼ 1050 erg. Focusing on sterile neutrino mixing only with tau neutrino, for heavy sterile masses ms in the range 100 – 500 MeV, we find stringent constraints on sin2θτ reaching two orders of magnitude lower than those from the SN1987A energy loss argument, thereby probing the mixing angles required for Type-I seesaw mechanism. Similar bounds will also be applicable to sterile mixing only with muons (sin2θμ).
{"title":"Low-energy supernovae bounds on sterile neutrinos","authors":"Garv Chauhan, Shunsaku Horiuchi, Patrick Huber and Ian M. Shoemaker","doi":"10.1088/1475-7516/2025/03/052","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/03/052","url":null,"abstract":"Sterile neutrinos can be produced through mixing with active neutrinos in the hot, dense core of a core-collapse supernova (SN). The standard bounds on the active-sterile mixing (sin2θ) from SN arise from SN1987A energy-loss, requiring Eloss < 1052 erg. In this work, we discuss a novel bound on sterile neutrino parameter space arising from the energy deposition through its decays inside the SN envelope. Using the observed underluminous SN IIP population, this energy deposition is constrained to be below ∼ 1050 erg. Focusing on sterile neutrino mixing only with tau neutrino, for heavy sterile masses ms in the range 100 – 500 MeV, we find stringent constraints on sin2θτ reaching two orders of magnitude lower than those from the SN1987A energy loss argument, thereby probing the mixing angles required for Type-I seesaw mechanism. Similar bounds will also be applicable to sterile mixing only with muons (sin2θμ).","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"94 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143675231","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 : 2025-03-21DOI: 10.1088/1475-7516/2025/03/051
C. Erices, L. Guajardo and K. Lara
We study a class of solutions within the context of modified gravity theories, characterized by a non-trivial field that does not generate any back-reaction on the metric. These stealth configurations are effectively defined by the stealth conditions, which correspond to a vanishing stress-energy tensor. In this work, we introduce a novel approach to constructing this class of solutions. In contrast to the standard procedure, the starting point requires satisfying the stealth conditions for a given ansatz independently of the gravitational dynamics. This approach simultaneously determines the non-trivial field and the geometries capable of supporting it as a stealth configuration. Consequently, a gravity model can accommodate a stealth field only if its vacuum solution falls within the geometries permissible under stealth conditions. By applying this reverse procedure in the non-minimal Rϕ2 coupling, we recover all previously known stealth configurations and present new solutions. Although it seems intuitive to assume that this “gravitationally undetectable” scalar field leaves no physical traces, it remarkably reveals thermodynamic imprints, as its presence screens the black hole mass and modifies the entropy according to the first law.
{"title":"Reverse stealth construction and its thermodynamic imprints","authors":"C. Erices, L. Guajardo and K. Lara","doi":"10.1088/1475-7516/2025/03/051","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/03/051","url":null,"abstract":"We study a class of solutions within the context of modified gravity theories, characterized by a non-trivial field that does not generate any back-reaction on the metric. These stealth configurations are effectively defined by the stealth conditions, which correspond to a vanishing stress-energy tensor. In this work, we introduce a novel approach to constructing this class of solutions. In contrast to the standard procedure, the starting point requires satisfying the stealth conditions for a given ansatz independently of the gravitational dynamics. This approach simultaneously determines the non-trivial field and the geometries capable of supporting it as a stealth configuration. Consequently, a gravity model can accommodate a stealth field only if its vacuum solution falls within the geometries permissible under stealth conditions. By applying this reverse procedure in the non-minimal Rϕ2 coupling, we recover all previously known stealth configurations and present new solutions. Although it seems intuitive to assume that this “gravitationally undetectable” scalar field leaves no physical traces, it remarkably reveals thermodynamic imprints, as its presence screens the black hole mass and modifies the entropy according to the first law.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"27 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143675227","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 : 2025-03-21DOI: 10.1088/1475-7516/2025/03/047
Sourav Pal, Rickmoy Samanta and Supratik Pal
In the standard cosmological framework, neutrinos begin to free-stream after the weak interaction phase ends in the early universe, at a temperature of approximately T ∼ 1 MeV. However, the onset of neutrino free-streaming can be delayed if additional interactions occur in the early universe, leaving imprints on both the cosmic microwave background (CMB) angular power spectra and the large-scale structure (LSS) matter power spectra. We present a thorough analysis of early universe neutrino interactions with a fairly generalized parameterization of the interaction rates as a power law in neutrino temperature. In this (6+2) parameter scenario, we constrain the cosmological parameters along with the free-streaming redshift and the sum of the neutrino mass in presence of such interactions, with the help of full shape (FS) galaxy power spectra from BOSS Data Release 12. Our analysis reveals that a combined dataset of FS along with CMB and BAO offers improved constraints on the free-streaming redshift from present data, comparable to the forecast results from future CMB-S4 data. Additionally, we investigate the prospects of future galaxy surveys by forecasting on Euclid mission in combination with Planck and CMB-S4, and find significant improvement on both the free-streaming redshift and the sum of the neutrino mass than the existing constraints as well as than CMB-S4 alone.
{"title":"Exploring neutrino interactions in light of present and upcoming galaxy surveys","authors":"Sourav Pal, Rickmoy Samanta and Supratik Pal","doi":"10.1088/1475-7516/2025/03/047","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/03/047","url":null,"abstract":"In the standard cosmological framework, neutrinos begin to free-stream after the weak interaction phase ends in the early universe, at a temperature of approximately T ∼ 1 MeV. However, the onset of neutrino free-streaming can be delayed if additional interactions occur in the early universe, leaving imprints on both the cosmic microwave background (CMB) angular power spectra and the large-scale structure (LSS) matter power spectra. We present a thorough analysis of early universe neutrino interactions with a fairly generalized parameterization of the interaction rates as a power law in neutrino temperature. In this (6+2) parameter scenario, we constrain the cosmological parameters along with the free-streaming redshift and the sum of the neutrino mass in presence of such interactions, with the help of full shape (FS) galaxy power spectra from BOSS Data Release 12. Our analysis reveals that a combined dataset of FS along with CMB and BAO offers improved constraints on the free-streaming redshift from present data, comparable to the forecast results from future CMB-S4 data. Additionally, we investigate the prospects of future galaxy surveys by forecasting on Euclid mission in combination with Planck and CMB-S4, and find significant improvement on both the free-streaming redshift and the sum of the neutrino mass than the existing constraints as well as than CMB-S4 alone.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"33 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143675224","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 : 2025-03-21DOI: 10.1088/1475-7516/2025/03/048
Yuyang Zhou, Adrian Lee and Yuji Chinone
E to B mixing or "leakage" due to time-ordered data (TOD) filtering has become an important source of sensitivity loss that ground-based cosmic microwave background polarization experiments must address. However, it is a difficult problem for which very few viable solutions exist. In this paper, we expand upon satellite E-mode methods to cover E/B leakage specifically due to TOD filtering. We take a satellite E-mode map and TOD filter it through the ground-based experiment data analysis pipeline, from which we construct a map-space "leakage template" and subtract it from the ground-based experiment map. We evaluate the residual leakage by simulating the satellite E-mode maps with Planck-like and LiteBIRD-like noise levels, and simulate the ground-based experiment with Simons Observatory-like and CMB-S4-like noise levels. The effectiveness of the method is measured in the improvement of the Fisher uncertainty σ(r = 0). We find that our method can reduce σ(r = 0) by ∼ 15–75% depending on the noise levels considered.
{"title":"Map-based E/B separation of filtered timestreams using space-based E-mode observations","authors":"Yuyang Zhou, Adrian Lee and Yuji Chinone","doi":"10.1088/1475-7516/2025/03/048","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/03/048","url":null,"abstract":"E to B mixing or \"leakage\" due to time-ordered data (TOD) filtering has become an important source of sensitivity loss that ground-based cosmic microwave background polarization experiments must address. However, it is a difficult problem for which very few viable solutions exist. In this paper, we expand upon satellite E-mode methods to cover E/B leakage specifically due to TOD filtering. We take a satellite E-mode map and TOD filter it through the ground-based experiment data analysis pipeline, from which we construct a map-space \"leakage template\" and subtract it from the ground-based experiment map. We evaluate the residual leakage by simulating the satellite E-mode maps with Planck-like and LiteBIRD-like noise levels, and simulate the ground-based experiment with Simons Observatory-like and CMB-S4-like noise levels. The effectiveness of the method is measured in the improvement of the Fisher uncertainty σ(r = 0). We find that our method can reduce σ(r = 0) by ∼ 15–75% depending on the noise levels considered.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"24 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143675225","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 : 2025-03-21DOI: 10.1088/1475-7516/2025/03/049
Sara Rufrano Aliberti, Gaetano Lambiase and Tanmay Kumar Poddar
Dark matter (DM) within the solar system induces deviations in the geodetic drift of a gyroscope spin due to its gravitational interaction. Considering a constant DM density as a minimal scenario, we constrain DM overdensity within the Gravity Probe B (GP-B) orbit around the Earth and for Earth's and Neptune's orbits around the Sun. The presence of electrons in gravitating sources and test objects introduces an electrophilic scalar-mediated Yukawa potential, which can be probed from the measurement of geodetic drift as well as using terrestrial and space-based precision clocks. We derive projected DM overdensity (η) limits from Sagnac time measurements using onboard satellite clocks, highlighting their dependence on the source mass and orbital radius. The strongest sensitivity, η ∼ 4.45 × 103, is achieved at Neptune's orbit (∼ 30 AU), exceeding existing constraints. Correspondingly, the cosmic neutrino overdensity is ξ ∼ 5.34 × 1010, surpassing results from KATRIN and cosmic ray studies. The strongest sensitivity on the electrophilic scalar coupling, g ∼ 7.09 × 10-24, is achieved for a scalar mass mφ ≲ 1.32 × 10-18 eV. This result, obtained from the projected precision clock studies probing non-gravitational potentials, is competitive with the leading bounds from fifth-force searches. These precision measurements offer a robust framework for testing gravity at solar system scales and probing DM in scenarios inaccessible to direct detection experiments.
{"title":"Limits on dark matter, ultralight scalars, and cosmic neutrinos with gyroscope spin and precision clocks","authors":"Sara Rufrano Aliberti, Gaetano Lambiase and Tanmay Kumar Poddar","doi":"10.1088/1475-7516/2025/03/049","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/03/049","url":null,"abstract":"Dark matter (DM) within the solar system induces deviations in the geodetic drift of a gyroscope spin due to its gravitational interaction. Considering a constant DM density as a minimal scenario, we constrain DM overdensity within the Gravity Probe B (GP-B) orbit around the Earth and for Earth's and Neptune's orbits around the Sun. The presence of electrons in gravitating sources and test objects introduces an electrophilic scalar-mediated Yukawa potential, which can be probed from the measurement of geodetic drift as well as using terrestrial and space-based precision clocks. We derive projected DM overdensity (η) limits from Sagnac time measurements using onboard satellite clocks, highlighting their dependence on the source mass and orbital radius. The strongest sensitivity, η ∼ 4.45 × 103, is achieved at Neptune's orbit (∼ 30 AU), exceeding existing constraints. Correspondingly, the cosmic neutrino overdensity is ξ ∼ 5.34 × 1010, surpassing results from KATRIN and cosmic ray studies. The strongest sensitivity on the electrophilic scalar coupling, g ∼ 7.09 × 10-24, is achieved for a scalar mass mφ ≲ 1.32 × 10-18 eV. This result, obtained from the projected precision clock studies probing non-gravitational potentials, is competitive with the leading bounds from fifth-force searches. These precision measurements offer a robust framework for testing gravity at solar system scales and probing DM in scenarios inaccessible to direct detection experiments.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"56 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143675226","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 : 2025-03-21DOI: 10.1088/1475-7516/2025/03/045
Di Wu, Jing-Zhi Zhou, Yu-Ting Kuang, Zhi-Chao Li, Zhe Chang and Qing-Guo Huang
Observational constraints on small-scale primordial gravitational waves are considerably weaker than those on large scales. We focus on scenarios with significant primordial gravitational waves and curvature perturbations on small scales, studying the energy density spectrum of the second-order tensor-scalar induced gravitational wave (TSIGW). By leveraging current data from cosmic microwave background (CMB), baryon acoustic oscillations (BAO), and pulsar timing array (PTA), combined with the signal-to-noise ratio (SNR) analysis of Laser Interferometer Space Antenna (LISA), we can investigate how tensor-scalar induced gravitational waves affect observations on various scales, thus constraining the parameter space for primordial gravitational waves and curvature perturbations. The Bayes factor analysis suggests that tensor-scalar induced gravitational wave (TSIGW)+primordial gravitational wave (PGW) might be more likely to dominate current pulsar timing array (PTA) observations compared to supermassive black hole binary (SMBHB).
{"title":"Can tensor-scalar induced GWs dominate PTA observations?","authors":"Di Wu, Jing-Zhi Zhou, Yu-Ting Kuang, Zhi-Chao Li, Zhe Chang and Qing-Guo Huang","doi":"10.1088/1475-7516/2025/03/045","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/03/045","url":null,"abstract":"Observational constraints on small-scale primordial gravitational waves are considerably weaker than those on large scales. We focus on scenarios with significant primordial gravitational waves and curvature perturbations on small scales, studying the energy density spectrum of the second-order tensor-scalar induced gravitational wave (TSIGW). By leveraging current data from cosmic microwave background (CMB), baryon acoustic oscillations (BAO), and pulsar timing array (PTA), combined with the signal-to-noise ratio (SNR) analysis of Laser Interferometer Space Antenna (LISA), we can investigate how tensor-scalar induced gravitational waves affect observations on various scales, thus constraining the parameter space for primordial gravitational waves and curvature perturbations. The Bayes factor analysis suggests that tensor-scalar induced gravitational wave (TSIGW)+primordial gravitational wave (PGW) might be more likely to dominate current pulsar timing array (PTA) observations compared to supermassive black hole binary (SMBHB).","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"17 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143675203","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 : 2025-03-21DOI: 10.1088/1475-7516/2025/03/046
Sudip Jana and Yago Porto
We show that non-standard neutrino interactions (NSI) can notably modify the pattern of resonant flavor conversion of neutrinos within supernovae and significantly impact the neutronization burst signal in forthcoming experiments such as the Deep Underground Neutrino Experiment (DUNE). The presence of NSI can invert the energy levels of neutrino matter eigenstates and even induce a new resonance in the inner parts close to the proto-neutron star. We demonstrate how DUNE can use these new configurations of energy levels to have sensitivity to NSIs down to 𝒪(0.1). We also elucidate how the effect may result in a puzzling confusion of normal and inverted mass orderings by highlighting the emergence or vanishing of the neutronization peak, which distinguishes between the two mass orderings. Potential implications are analyzed thoroughly.
{"title":"Non-standard interactions of supernova neutrinos and mass ordering ambiguity at DUNE","authors":"Sudip Jana and Yago Porto","doi":"10.1088/1475-7516/2025/03/046","DOIUrl":"https://doi.org/10.1088/1475-7516/2025/03/046","url":null,"abstract":"We show that non-standard neutrino interactions (NSI) can notably modify the pattern of resonant flavor conversion of neutrinos within supernovae and significantly impact the neutronization burst signal in forthcoming experiments such as the Deep Underground Neutrino Experiment (DUNE). The presence of NSI can invert the energy levels of neutrino matter eigenstates and even induce a new resonance in the inner parts close to the proto-neutron star. We demonstrate how DUNE can use these new configurations of energy levels to have sensitivity to NSIs down to 𝒪(0.1). We also elucidate how the effect may result in a puzzling confusion of normal and inverted mass orderings by highlighting the emergence or vanishing of the neutronization peak, which distinguishes between the two mass orderings. Potential implications are analyzed thoroughly.","PeriodicalId":15445,"journal":{"name":"Journal of Cosmology and Astroparticle Physics","volume":"70 1","pages":""},"PeriodicalIF":6.4,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143675223","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 : 2025-03-21DOI: 10.1088/1475-7516/2025/03/055
John McDonald
The Standard Model (SM) Higgs potential is likely to be metastable, in which case Higgs Inflation requires an extension of the SM to sufficiently stabilise the Higgs potential. Here we consider stabilisation by adding nQ ≤ 3 Vector-Like Quarks (VLQs) of mass mQ. We consider isosinglet T vector quarks transforming under the SM gauge group as (3, 1, 2/3) and B vector quarks transforming as (3, 1, -1/3). Requiring stability of the finite temperature effective potential after instant reheating, and assuming that the t-quark mass mt equals the mean value of its experimental range, we find that the upper bounds on mQ for T quarks are 5.8 TeV (for nQ = 2) and 55 TeV (for nQ = 3). The corresponding absolute stability upper bounds are 4.4 TeV and 29 TeV. For nQ = 1 there is stability only for mt at its -2-σ value, in which case mQ ≤ 1.6 TeV for one T quark. The upper bounds are generally smaller for B vector quarks, with finite temperature stability for mQ less than 2.8 TeV (for nQ = 2), 18 TeV (for nQ = 3) and 1.0 TeV (for nQ = 1). The upper bounds on mQ are sensitive to the t-quark mass, becoming smaller as mt increases. The inflation predictions depend upon the conformal frame in which the model is renormalised. For renormalisation in the Einstein frame (Prescription I) the predictions are almost indistinguishable from the classical values: ns = 0.966 and r = 3.3 × 10-3. In this case the stability upper bounds on mQ apply. Renormalisation in the Jordan frame (Prescription II) predicts larger values of ns and r, with ns generally in the range 0.980 to 0.990 and r of the order of 0.01. The predicted range of ns is consistent with the CMB range obtained in Hubble tension solutions which modify the sound horizon at decoupling, whilst the predicted values of r will be easily observable by forthcoming CMB experiments. The observational upper bound on r generally imposes a stronger constraint on mQ in Prescription II than the requirement of stability, with the T quark upper bound equal to 2.4 TeV for nQ = 2 and 13 TeV for nQ = 3, assuming mt equals its mean value. nQ = 1 is generally ruled out by the large value of r. The mQ upper bounds rapidly decrease with decreasing r. We conclude that VLQ-stabilised Higgs Inflation with Prescription II renormalisation favours 1-10 TeV vector-like quarks that will be accessible to future colliders, and predicts a tensor-to-scalar ratio that will be observable in forthcoming CMB experiments and values of ns that favour an early-time solution to the Hubble tension.
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