Bohdan Bidenko, Léon V. E. Koopmans, P. Daniel Meerburg
The 21-cm brightness-temperature field of neutral hydrogen during the Epoch of Reionization and Cosmic Dawn is a rich source of cosmological and astrophysical information, primarily due to its significant non-Gaussian features. However, the complex, nonlinear nature of the underlying physical processes makes analytical modelling of this signal challenging. Consequently, studies often resort to semi-numerical simulations. Traditional analysis methods, which rely on a limited set of summary statistics, may not adequately capture the non-Gaussian content of the data, as the most informative statistics are not predetermined. This paper explores the application of machine learning (ML) to surpass the limitations of summary statistics by leveraging the inherent non-Gaussian characteristics of the 21-cm signal. We demonstrate that a well-trained neural network can independently reconstruct the hydrogen density, spin-temperature, and neutral-fraction fields with cross-coherence values exceeding 0.95 for $k$-modes below $0.5$ Mpc h$^{-1}$, based on a representative simulation at a redshift of $z approx 15$. To achieve this, the neural network utilises the non-Gaussian information in brightness temperature images over many scales. We discuss how these reconstructed fields, which vary in their sensitivity to model parameters, can be employed for parameter inference, offering more direct insights into underlying cosmological and astrophysical processes only using limited summary statistics of the brightness temperature field, such as its power spectrum.
{"title":"Inferring the density, spin-temperature and neutral-fraction fields of HI from its 21-cm brightness temperature field using machine learning","authors":"Bohdan Bidenko, Léon V. E. Koopmans, P. Daniel Meerburg","doi":"arxiv-2409.06769","DOIUrl":"https://doi.org/arxiv-2409.06769","url":null,"abstract":"The 21-cm brightness-temperature field of neutral hydrogen during the Epoch\u0000of Reionization and Cosmic Dawn is a rich source of cosmological and\u0000astrophysical information, primarily due to its significant non-Gaussian\u0000features. However, the complex, nonlinear nature of the underlying physical\u0000processes makes analytical modelling of this signal challenging. Consequently,\u0000studies often resort to semi-numerical simulations. Traditional analysis\u0000methods, which rely on a limited set of summary statistics, may not adequately\u0000capture the non-Gaussian content of the data, as the most informative\u0000statistics are not predetermined. This paper explores the application of\u0000machine learning (ML) to surpass the limitations of summary statistics by\u0000leveraging the inherent non-Gaussian characteristics of the 21-cm signal. We\u0000demonstrate that a well-trained neural network can independently reconstruct\u0000the hydrogen density, spin-temperature, and neutral-fraction fields with\u0000cross-coherence values exceeding 0.95 for $k$-modes below $0.5$ Mpc h$^{-1}$,\u0000based on a representative simulation at a redshift of $z approx 15$. To\u0000achieve this, the neural network utilises the non-Gaussian information in\u0000brightness temperature images over many scales. We discuss how these\u0000reconstructed fields, which vary in their sensitivity to model parameters, can\u0000be employed for parameter inference, offering more direct insights into\u0000underlying cosmological and astrophysical processes only using limited summary\u0000statistics of the brightness temperature field, such as its power spectrum.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"13 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192776","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The 408 MHz Haslam map is widely used as a low-frequency anchor for the intensity and morphology of Galactic synchrotron emission. Multi-frequency, multi-experiment fits show evidence of spatial variation and curvature in the synchrotron frequency spectrum, but there are also poorly-understood gain factors between experiments. We perform a Bayesian model comparison across a range of scenarios, using fits that include recent spectroscopic observations at $sim 1$~GHz by MeerKAT. A large uncorrected gain factor of about 60% in the Haslam data is strongly preferred, partly undermining its use as a reference template.
{"title":"Bayesian evidence for uncorrected gain factors in Galactic synchrotron template maps","authors":"Michael J. Wilensky, Melis O. Irfan, Philip Bull","doi":"arxiv-2409.06770","DOIUrl":"https://doi.org/arxiv-2409.06770","url":null,"abstract":"The 408 MHz Haslam map is widely used as a low-frequency anchor for the\u0000intensity and morphology of Galactic synchrotron emission. Multi-frequency,\u0000multi-experiment fits show evidence of spatial variation and curvature in the\u0000synchrotron frequency spectrum, but there are also poorly-understood gain\u0000factors between experiments. We perform a Bayesian model comparison across a\u0000range of scenarios, using fits that include recent spectroscopic observations\u0000at $sim 1$~GHz by MeerKAT. A large uncorrected gain factor of about 60% in\u0000the Haslam data is strongly preferred, partly undermining its use as a\u0000reference template.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"75 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192775","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Victor C. Chan, Renée Hložek, Joel Meyers, Alexander van Engelen
The Small-Correlated-Against-Large Estimator (SCALE) for small-scale lensing of the cosmic microwave background (CMB) provides a novel method for measuring the amplitude of CMB lensing power without the need for reconstruction of the lensing field. In our previous study, we showed that the SCALE method can outperform existing reconstruction methods to detect the presence of lensing at small scales ($ell gg 3000$). Here we develop a procedure to include information from SCALE in cosmological parameter inference. We construct a precise neural network emulator to quickly map cosmological parameters to desired CMB observables such as temperature and lensing power spectra and SCALE cross spectra. We also outline a method to apply SCALE to full-sky maps of the CMB temperature field, and construct a likelihood for the application of SCALE in parameter estimation. SCALE supplements conventional observables such as the CMB power spectra and baryon acoustic oscillations in constraining parameters that are sensitive to the small-scale lensing amplitude such as the neutrino mass $m_nu$. We show that including estimates of the small-scale lensing amplitude from SCALE in such an analysis provides enough constraining information to measure the minimum neutrino mass at $4sigma$ significance in the scenario of minimal mass, and higher significance for higher mass. Finally, we show that SCALE will play a powerful role in constraining models of clustering that generate scale-dependent modulation to the distribution of matter and the lensing power spectrum, as predicted by models of warm or fuzzy dark matter.
{"title":"SCALE at Scale: Cosmological applications of small-scale CMB lensing","authors":"Victor C. Chan, Renée Hložek, Joel Meyers, Alexander van Engelen","doi":"arxiv-2409.05326","DOIUrl":"https://doi.org/arxiv-2409.05326","url":null,"abstract":"The Small-Correlated-Against-Large Estimator (SCALE) for small-scale lensing\u0000of the cosmic microwave background (CMB) provides a novel method for measuring\u0000the amplitude of CMB lensing power without the need for reconstruction of the\u0000lensing field. In our previous study, we showed that the SCALE method can\u0000outperform existing reconstruction methods to detect the presence of lensing at\u0000small scales ($ell gg 3000$). Here we develop a procedure to include\u0000information from SCALE in cosmological parameter inference. We construct a\u0000precise neural network emulator to quickly map cosmological parameters to\u0000desired CMB observables such as temperature and lensing power spectra and SCALE\u0000cross spectra. We also outline a method to apply SCALE to full-sky maps of the\u0000CMB temperature field, and construct a likelihood for the application of SCALE\u0000in parameter estimation. SCALE supplements conventional observables such as the\u0000CMB power spectra and baryon acoustic oscillations in constraining parameters\u0000that are sensitive to the small-scale lensing amplitude such as the neutrino\u0000mass $m_nu$. We show that including estimates of the small-scale lensing\u0000amplitude from SCALE in such an analysis provides enough constraining\u0000information to measure the minimum neutrino mass at $4sigma$ significance in\u0000the scenario of minimal mass, and higher significance for higher mass. Finally,\u0000we show that SCALE will play a powerful role in constraining models of\u0000clustering that generate scale-dependent modulation to the distribution of\u0000matter and the lensing power spectrum, as predicted by models of warm or fuzzy\u0000dark matter.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"24 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192571","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
J. Chaves-Montero, L. Cabayol-Garcia, M. Lokken, A. Font-Ribera, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, S. Cole, A. de la Macorra, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, R. Kehoe, D. Kirkby, A. Kremin, A. Lambert, M. Landriau, M. Manera, P. Martini, R. Miquel, A. Muñoz-Gutiérrez, G. Niz, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver
On large scales, measurements of the Lyman-$alpha$ forest offer insights into the expansion history of the Universe, while on small scales, these impose strict constraints on the growth history, the nature of dark matter, and the sum of neutrino masses. This work introduces ForestFlow, a cosmological emulator designed to bridge the gap between large- and small-scale Lyman-$alpha$ forest analyses. Using conditional normalizing flows, ForestFlow emulates the 2 Lyman-$alpha$ linear biases ($b_delta$ and $b_eta$) and 6 parameters describing small-scale deviations of the 3D flux power spectrum ($P_mathrm{3D}$) from linear theory. These 8 parameters are modeled as a function of cosmology $unicode{x2013}$ the small-scale amplitude and slope of the linear power spectrum $unicode{x2013}$ and the physics of the intergalactic medium. Thus, in combination with a Boltzmann solver, ForestFlow can predict $P_mathrm{3D}$ on arbitrarily large (linear) scales and the 1D flux power spectrum ($P_mathrm{1D}$) $unicode{x2013}$ the primary observable for small-scale analyses $unicode{x2013}$ without the need for interpolation or extrapolation. Consequently, ForestFlow enables for the first time multiscale analyses. Trained on a suite of 30 fixed-and-paired cosmological hydrodynamical simulations spanning redshifts from $z=2$ to $4.5$, ForestFlow achieves $3$ and $1.5%$ precision in describing $P_mathrm{3D}$ and $P_mathrm{1D}$ from linear scales to $k=5,mathrm{Mpc}^{-1}$ and $k_parallel=4,mathrm{Mpc}^{-1}$, respectively. Thanks to its parameterization, the precision of the emulator is also similar for both ionization histories and two extensions to the $Lambda$CDM model $unicode{x2013}$ massive neutrinos and curvature $unicode{x2013}$ not included in the training set. ForestFlow will be crucial for the cosmological analysis of Lyman-$alpha$ forest measurements from the DESI survey.
{"title":"ForestFlow: cosmological emulation of Lyman-$α$ forest clustering from linear to nonlinear scales","authors":"J. Chaves-Montero, L. Cabayol-Garcia, M. Lokken, A. Font-Ribera, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, S. Cole, A. de la Macorra, S. Ferraro, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, R. Kehoe, D. Kirkby, A. Kremin, A. Lambert, M. Landriau, M. Manera, P. Martini, R. Miquel, A. Muñoz-Gutiérrez, G. Niz, I. Pérez-Ràfols, G. Rossi, E. Sanchez, M. Schubnell, D. Sprayberry, G. Tarlé, B. A. Weaver","doi":"arxiv-2409.05682","DOIUrl":"https://doi.org/arxiv-2409.05682","url":null,"abstract":"On large scales, measurements of the Lyman-$alpha$ forest offer insights\u0000into the expansion history of the Universe, while on small scales, these impose\u0000strict constraints on the growth history, the nature of dark matter, and the\u0000sum of neutrino masses. This work introduces ForestFlow, a cosmological\u0000emulator designed to bridge the gap between large- and small-scale\u0000Lyman-$alpha$ forest analyses. Using conditional normalizing flows, ForestFlow\u0000emulates the 2 Lyman-$alpha$ linear biases ($b_delta$ and $b_eta$) and 6\u0000parameters describing small-scale deviations of the 3D flux power spectrum\u0000($P_mathrm{3D}$) from linear theory. These 8 parameters are modeled as a\u0000function of cosmology $unicode{x2013}$ the small-scale amplitude and slope of\u0000the linear power spectrum $unicode{x2013}$ and the physics of the\u0000intergalactic medium. Thus, in combination with a Boltzmann solver, ForestFlow\u0000can predict $P_mathrm{3D}$ on arbitrarily large (linear) scales and the 1D\u0000flux power spectrum ($P_mathrm{1D}$) $unicode{x2013}$ the primary observable\u0000for small-scale analyses $unicode{x2013}$ without the need for interpolation\u0000or extrapolation. Consequently, ForestFlow enables for the first time\u0000multiscale analyses. Trained on a suite of 30 fixed-and-paired cosmological\u0000hydrodynamical simulations spanning redshifts from $z=2$ to $4.5$, ForestFlow\u0000achieves $3$ and $1.5%$ precision in describing $P_mathrm{3D}$ and\u0000$P_mathrm{1D}$ from linear scales to $k=5,mathrm{Mpc}^{-1}$ and\u0000$k_parallel=4,mathrm{Mpc}^{-1}$, respectively. Thanks to its\u0000parameterization, the precision of the emulator is also similar for both\u0000ionization histories and two extensions to the $Lambda$CDM model\u0000$unicode{x2013}$ massive neutrinos and curvature $unicode{x2013}$ not\u0000included in the training set. ForestFlow will be crucial for the cosmological\u0000analysis of Lyman-$alpha$ forest measurements from the DESI survey.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"72 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192570","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Marked power spectra provide a computationally efficient way to extract non-Gaussian information from the matter density field using the usual analysis tools developed for the power spectrum without the need for explicit calculation of higher-order correlators. In this work, we explore the optimal form of the mark function used for re-weighting the density field, to maximally constrain cosmology. We show that adding to the mark function or multiplying it by a constant leads to no additional information gain, which significantly reduces our search space for optimal marks. We quantify the information gain of this optimal function and compare it against mark functions previously proposed in the literature. We find that we can gain around $sim2$ times smaller errors in $sigma_8$ and $sim4$ times smaller errors in $Omega_m$ compared to using the traditional power spectrum alone, an improvement of $sim60%$ compared to other proposed marks when applied to the same dataset.
{"title":"Hitting the mark: Optimising Marked Power Spectra for Cosmology","authors":"Jessica A. Cowell, David Alonso, Jia Liu","doi":"arxiv-2409.05695","DOIUrl":"https://doi.org/arxiv-2409.05695","url":null,"abstract":"Marked power spectra provide a computationally efficient way to extract\u0000non-Gaussian information from the matter density field using the usual analysis\u0000tools developed for the power spectrum without the need for explicit\u0000calculation of higher-order correlators. In this work, we explore the optimal\u0000form of the mark function used for re-weighting the density field, to maximally\u0000constrain cosmology. We show that adding to the mark function or multiplying it\u0000by a constant leads to no additional information gain, which significantly\u0000reduces our search space for optimal marks. We quantify the information gain of\u0000this optimal function and compare it against mark functions previously proposed\u0000in the literature. We find that we can gain around $sim2$ times smaller errors\u0000in $sigma_8$ and $sim4$ times smaller errors in $Omega_m$ compared to using\u0000the traditional power spectrum alone, an improvement of $sim60%$ compared to\u0000other proposed marks when applied to the same dataset.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"75 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192569","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Xiaoyun Shao, Carlos A. P. Bengaly, Rodrigo S. Gonçalves, Gabriela C. Carvalho, Jailson Alcaniz
In this paper, we obtain new measurements of the angular homogeneity scale ($theta_H$) from the BOSS DR12 and eBOSS DR16 catalogs of Luminous Red Galaxies of the Sloan Digital Sky Survey. Considering the flat $Lambda$CDM model, we use the $theta_H(z)$ data to constrain the matter density parameter ($Omega_{m0}$) and the Hubble constant ($H_{0}$). We find $H_0 = 65.7 pm 7.0$ km s$^{-1}$ Mpc$^{-1}$ and $Omega_{m0}>0.293$. By combining the $theta_H$ measurements with current Baryon Acoustic Oscillations (BAO) and Type Ia Supernova (SN) data, we obtain $H_{0}= 69.9^{+4.9}_{-4.5}$ km s$^{-1}$ Mpc$^{-1}$ and $Omega_{m0} = 0.294^{+0.013}_{-0.015}$ ($theta_H$ + BAO) and $H_{0}=70.7^{+5.2}_{-4.1}$ km s$^{-1}$ Mpc$^{-1}$ and $Omega_{m0}=0.299 pm 0.022$ ($theta_H$ + SN). We show that $theta_H$ measurements help break the BAO and SN degeneracies concerning $H_0$, as they do not depend on the sound horizon scale at the drag epoch or the SN absolute magnitude value obtained from the distance ladder method. Hence, despite those constraints being loose compared to other probes, $theta_H$ data may provide an independent cosmological probe of $H_0$ in light of the Hubble tension. For completeness, we also forecast the constraining power of future $theta_H$ data via Monte Carlo simulations. Considering a relative error of the order of 1$%$, we obtain competitive constraints on $Omega_{m0}$ and $H_0$ ($approx 5%$ error) from the joint analysis with current SN and BAO measurements.
{"title":"Cosmological constraints from angular homogeneity scale measurements","authors":"Xiaoyun Shao, Carlos A. P. Bengaly, Rodrigo S. Gonçalves, Gabriela C. Carvalho, Jailson Alcaniz","doi":"arxiv-2409.06009","DOIUrl":"https://doi.org/arxiv-2409.06009","url":null,"abstract":"In this paper, we obtain new measurements of the angular homogeneity scale\u0000($theta_H$) from the BOSS DR12 and eBOSS DR16 catalogs of Luminous Red\u0000Galaxies of the Sloan Digital Sky Survey. Considering the flat $Lambda$CDM\u0000model, we use the $theta_H(z)$ data to constrain the matter density parameter\u0000($Omega_{m0}$) and the Hubble constant ($H_{0}$). We find $H_0 = 65.7 pm 7.0$\u0000km s$^{-1}$ Mpc$^{-1}$ and $Omega_{m0}>0.293$. By combining the $theta_H$\u0000measurements with current Baryon Acoustic Oscillations (BAO) and Type Ia\u0000Supernova (SN) data, we obtain $H_{0}= 69.9^{+4.9}_{-4.5}$ km s$^{-1}$\u0000Mpc$^{-1}$ and $Omega_{m0} = 0.294^{+0.013}_{-0.015}$ ($theta_H$ + BAO) and\u0000$H_{0}=70.7^{+5.2}_{-4.1}$ km s$^{-1}$ Mpc$^{-1}$ and $Omega_{m0}=0.299 pm\u00000.022$ ($theta_H$ + SN). We show that $theta_H$ measurements help break the\u0000BAO and SN degeneracies concerning $H_0$, as they do not depend on the sound\u0000horizon scale at the drag epoch or the SN absolute magnitude value obtained\u0000from the distance ladder method. Hence, despite those constraints being loose\u0000compared to other probes, $theta_H$ data may provide an independent\u0000cosmological probe of $H_0$ in light of the Hubble tension. For completeness,\u0000we also forecast the constraining power of future $theta_H$ data via Monte\u0000Carlo simulations. Considering a relative error of the order of 1$%$, we\u0000obtain competitive constraints on $Omega_{m0}$ and $H_0$ ($approx 5%$ error)\u0000from the joint analysis with current SN and BAO measurements.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"14 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192563","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Daniele Sorini, Sownak Bose, Romeel Davé, Daniel Anglés Alcázar
The radial distribution of gas within galactic haloes is connected to the star formation rate and the nature of baryon-driven feedback processes. Using six variants of the hydrodynamic simulation Simba, we study the impact of different stellar/AGN feedback prescriptions on the gas density profiles of haloes in the total mass range $10^{11} , mathrm{M}_{odot} < M_{mathrm{200c}} < 10^{14} , mathrm{M}_{odot}$ and redshift interval $0
{"title":"The impact of feedback on the evolution of gas density profiles from galaxies to clusters: a universal fitting formula from the Simba suite of simulations","authors":"Daniele Sorini, Sownak Bose, Romeel Davé, Daniel Anglés Alcázar","doi":"arxiv-2409.05815","DOIUrl":"https://doi.org/arxiv-2409.05815","url":null,"abstract":"The radial distribution of gas within galactic haloes is connected to the\u0000star formation rate and the nature of baryon-driven feedback processes. Using\u0000six variants of the hydrodynamic simulation Simba, we study the impact of\u0000different stellar/AGN feedback prescriptions on the gas density profiles of\u0000haloes in the total mass range $10^{11} , mathrm{M}_{odot} <\u0000M_{mathrm{200c}} < 10^{14} , mathrm{M}_{odot}$ and redshift interval\u0000$0<z<4$. We find that the radial profiles are well represented by a power law\u0000and that, for a fixed total halo mass, the slope and amplitude of such power\u0000law are generally weakly dependent on redshift. Once AGN-driven jets are\u0000activated in the simulation, the gas density profile of haloes with $M_{rm\u0000200c} gtrsim 10^{13} , rm M_{odot}$ declines more gently with radial\u0000distance. We argue that this distinctive feature could be exploited with\u0000current observations to discriminate amongst the predictions of the different\u0000feedback models. We introduce a universal fitting formula for the slope and\u0000amplitude of the gas density profile as a function of total halo mass and\u0000redshift. The best-fit functions are suitable for all feedback variants\u0000considered, and their predictions are in excellent agreement with the numerical\u0000results. We provide the values of all fit parameters, making our fitting\u0000formula a versatile tool to mimic the effect of Simba feedback models onto\u0000N-body simulations and semi-analytical models of galaxy formation. Our results\u0000can also aid observational estimates of the gas mass within haloes that assume\u0000a specific slope for the underlying gas density profile.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"12 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192594","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Primordial black holes (PBHs) would induce non-Gaussianity in the cosmic microwave background (CMB) by sourcing recombination perturbations spatially modulated by relative velocities between PBHs and the baryons they accrete. The leading non-Gaussian signatures are non-vanishing connected 4-point correlation functions, or trispectra. Earlier, we computed the CMB temperature trispectrum, and forecasted Planck to be more sensitive to it than to changes in the CMB temperature power spectrum for light enough PBHs. Excitingly, accreting PBHs would also induce non-Gaussianity in CMB polarization, and source both E and B modes, which we compute in this paper. We first calculate linear-response perturbations to the tensor-valued photon distribution function sourced by a general spatially-varying ionization history, and apply our results to accreting PBHs. We then compute linear-order perturbations to the temperature and polarization 2-point functions sourced by inhomogeneities in recombination due to accreting PBHs; we find them to be negligible relative to their counterparts sourced by homogeneous perturbations to the ionization history. Lastly, we compute all CMB trispectra including temperature, E- and B-mode polarization at linear order in the PBH abundance. We forecast that including polarization data in a 4-point-function analysis would only increase Planck's sensitivity to accreting PBHs by a factor ~2 relative to using temperature alone. As a consequence, we find that a search for PBHs using all temperature and polarization trispectra with Planck data would mostly not be competitive with current bounds from temperature and polarization power spectra. In contrast, we forecast that a CMB Stage-4 experiment would gain significant sensitivity to accreting PBHs through a 4-point-function search, in particular through the contributions of parity-odd trispectra including one B-mode field.
{"title":"CMB polarization non-Gaussianity from accreting primordial black holes","authors":"Trey W. JensenNYU, Yacine Ali-HaïmoudNYU","doi":"arxiv-2409.06028","DOIUrl":"https://doi.org/arxiv-2409.06028","url":null,"abstract":"Primordial black holes (PBHs) would induce non-Gaussianity in the cosmic\u0000microwave background (CMB) by sourcing recombination perturbations spatially\u0000modulated by relative velocities between PBHs and the baryons they accrete. The\u0000leading non-Gaussian signatures are non-vanishing connected 4-point correlation\u0000functions, or trispectra. Earlier, we computed the CMB temperature trispectrum,\u0000and forecasted Planck to be more sensitive to it than to changes in the CMB\u0000temperature power spectrum for light enough PBHs. Excitingly, accreting PBHs\u0000would also induce non-Gaussianity in CMB polarization, and source both E and B\u0000modes, which we compute in this paper. We first calculate linear-response\u0000perturbations to the tensor-valued photon distribution function sourced by a\u0000general spatially-varying ionization history, and apply our results to\u0000accreting PBHs. We then compute linear-order perturbations to the temperature\u0000and polarization 2-point functions sourced by inhomogeneities in recombination\u0000due to accreting PBHs; we find them to be negligible relative to their\u0000counterparts sourced by homogeneous perturbations to the ionization history.\u0000Lastly, we compute all CMB trispectra including temperature, E- and B-mode\u0000polarization at linear order in the PBH abundance. We forecast that including\u0000polarization data in a 4-point-function analysis would only increase Planck's\u0000sensitivity to accreting PBHs by a factor ~2 relative to using temperature\u0000alone. As a consequence, we find that a search for PBHs using all temperature\u0000and polarization trispectra with Planck data would mostly not be competitive\u0000with current bounds from temperature and polarization power spectra. In\u0000contrast, we forecast that a CMB Stage-4 experiment would gain significant\u0000sensitivity to accreting PBHs through a 4-point-function search, in particular\u0000through the contributions of parity-odd trispectra including one B-mode field.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"15 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192568","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Recent large-scale structure (LSS) surveys have revealed a persistent tension in the value of $S_8$ compared to predictions from the standard cosmological model. This tension may suggest the need for new physics beyond the standard model, but an accurate characterisation of baryonic effects is essential to avoid biases. Although some studies indicate that baryonic effects are too small to resolve this tension, others propose that more aggressive feedback mechanisms could reconcile differences between cosmic microwave background (CMB) measurements and low-redshift LSS observations. In this paper, we investigate the role of baryonic effects in alleviating the $S_8$ tension. We extend the SP(k) model (Salcido et al. 2023), which was trained on hundreds of cosmological hydrodynamical simulations to map the suppression of the matter power spectrum to the baryon fraction in groups and clusters, to predict the required baryon fraction for a given $P(k)$ suppression. We then compare predictions from recent cosmic shear (weak lensing) analyses with the latest baryon budget measurements from X-ray and weak gravitational lensing studies. Our findings show that studies marginalising over baryonic effects while fixing cosmological parameters to a Planck-like cosmology predict strong $P(k)$ suppression and baryon fractions that are much lower than existing low-redshift baryon budget estimates of galaxy groups and clusters. Conversely, most studies that marginalise over both cosmological parameters and baryonic effects imply baryon fractions that are consistent with observations but lower values of $S_8$ than inferred from the CMB. Unless the observed baryon fractions are biased high by a factor of several, these results suggest that a mechanism beyond baryonic physics alone is required to modify or slow down the growth of structure in the universe in order to resolve the $S_8$ tension.
{"title":"Implications of feedback solutions to the $S_8$ tension for the baryon fractions of galaxy groups and clusters","authors":"Jaime Salcido, Ian G. McCarthy","doi":"arxiv-2409.05716","DOIUrl":"https://doi.org/arxiv-2409.05716","url":null,"abstract":"Recent large-scale structure (LSS) surveys have revealed a persistent tension\u0000in the value of $S_8$ compared to predictions from the standard cosmological\u0000model. This tension may suggest the need for new physics beyond the standard\u0000model, but an accurate characterisation of baryonic effects is essential to\u0000avoid biases. Although some studies indicate that baryonic effects are too\u0000small to resolve this tension, others propose that more aggressive feedback\u0000mechanisms could reconcile differences between cosmic microwave background\u0000(CMB) measurements and low-redshift LSS observations. In this paper, we\u0000investigate the role of baryonic effects in alleviating the $S_8$ tension. We\u0000extend the SP(k) model (Salcido et al. 2023), which was trained on hundreds of\u0000cosmological hydrodynamical simulations to map the suppression of the matter\u0000power spectrum to the baryon fraction in groups and clusters, to predict the\u0000required baryon fraction for a given $P(k)$ suppression. We then compare\u0000predictions from recent cosmic shear (weak lensing) analyses with the latest\u0000baryon budget measurements from X-ray and weak gravitational lensing studies.\u0000Our findings show that studies marginalising over baryonic effects while fixing\u0000cosmological parameters to a Planck-like cosmology predict strong $P(k)$\u0000suppression and baryon fractions that are much lower than existing low-redshift\u0000baryon budget estimates of galaxy groups and clusters. Conversely, most studies\u0000that marginalise over both cosmological parameters and baryonic effects imply\u0000baryon fractions that are consistent with observations but lower values of\u0000$S_8$ than inferred from the CMB. Unless the observed baryon fractions are\u0000biased high by a factor of several, these results suggest that a mechanism\u0000beyond baryonic physics alone is required to modify or slow down the growth of\u0000structure in the universe in order to resolve the $S_8$ tension.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"7 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192572","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
I. García-Bernete, D. Rigopoulou, F. R. Donnan, A. Alonso-Herrero, M. Pereira-Santella, T. Shimizu, R. Davies, P. F. Roche, S. García-Burillo, A. Labiano, L. Hermosa Muñoz, L. Zhang, A. Audibert, E. Bellocchi, A. Bunker, F. Combes, D. Delaney, D. Esparza-Arredondo, P. Gandhi, O. González-Martín, S. F. Hönig, M. Imanishi, E. K. S. Hicks, L. Fuller, M. Leist, N. A. Levenson, E. Lopez-Rodriguez, C. Packham, C. Ramos Almeida, C. Ricci, M. Stalevski, M. Villar Martín, M. J. Ward
We analyze JWST MIRI/MRS observations of the infrared PAH bands in the nuclear and circumnuclear regions of local AGN from the GATOS Survey. In this work, we examine the PAH properties in the circumnuclear regions of AGN and AGN-outflows, and compare them to those in star-forming regions and the innermost regions of AGN. This study employs 4.9-28.1 micron sub-arcsecond angular resolution data to investigate the properties of PAH in three nearby sources (DL~30-40 Mpc). Our findings align with previous JWST studies, showing that the central regions of AGN show a larger fraction of neutral PAH molecules (i.e. elevated 11.3/6.2 and 11.3/7.7 PAH ratios) compared to star-forming galaxies. We find that the AGN might affect not only the PAH population in the innermost region but also in the extended regions up to ~kpc scales. By comparing our observations to PAH diagnostic diagrams, we find that, in general, regions located in the projected direction of the AGN-outflow occupy similar positions on the PAH diagnostic diagrams as those of the innermost regions of AGN. Star-forming regions that are not affected by the AGN in these galaxies share the same part of the diagram as Star-forming galaxies. We examine the potential of the PAH-H2 diagram to disentangle AGN versus star-forming activity. Our results suggest that in Sy-like AGN, illumination and feedback from the AGN might affect the PAH population at nuclear and kpc scales, in particular, the ionization state of the PAH grains. However, PAH sizes are rather similar. The carriers of the ionized PAH bands (6.2 and 7.7 micron) are less resilience than those of neutral PAH bands (11.3 micron), which might be particularly important for strongly AGN-host coupled systems. Therefore, caution must be applied when using PAH bands as star-formation rate indicators in these systems even at kpc scales, with the ionized ones being more affected by the AGN.
{"title":"The Galaxy Activity, Torus, and Outflow Survey (GATOS). V: Unveiling PAH survival and resilience in the circumnuclear regions of AGN with JWST","authors":"I. García-Bernete, D. Rigopoulou, F. R. Donnan, A. Alonso-Herrero, M. Pereira-Santella, T. Shimizu, R. Davies, P. F. Roche, S. García-Burillo, A. Labiano, L. Hermosa Muñoz, L. Zhang, A. Audibert, E. Bellocchi, A. Bunker, F. Combes, D. Delaney, D. Esparza-Arredondo, P. Gandhi, O. González-Martín, S. F. Hönig, M. Imanishi, E. K. S. Hicks, L. Fuller, M. Leist, N. A. Levenson, E. Lopez-Rodriguez, C. Packham, C. Ramos Almeida, C. Ricci, M. Stalevski, M. Villar Martín, M. J. Ward","doi":"arxiv-2409.05686","DOIUrl":"https://doi.org/arxiv-2409.05686","url":null,"abstract":"We analyze JWST MIRI/MRS observations of the infrared PAH bands in the\u0000nuclear and circumnuclear regions of local AGN from the GATOS Survey. In this\u0000work, we examine the PAH properties in the circumnuclear regions of AGN and\u0000AGN-outflows, and compare them to those in star-forming regions and the\u0000innermost regions of AGN. This study employs 4.9-28.1 micron sub-arcsecond\u0000angular resolution data to investigate the properties of PAH in three nearby\u0000sources (DL~30-40 Mpc). Our findings align with previous JWST studies, showing\u0000that the central regions of AGN show a larger fraction of neutral PAH molecules\u0000(i.e. elevated 11.3/6.2 and 11.3/7.7 PAH ratios) compared to star-forming\u0000galaxies. We find that the AGN might affect not only the PAH population in the\u0000innermost region but also in the extended regions up to ~kpc scales. By\u0000comparing our observations to PAH diagnostic diagrams, we find that, in\u0000general, regions located in the projected direction of the AGN-outflow occupy\u0000similar positions on the PAH diagnostic diagrams as those of the innermost\u0000regions of AGN. Star-forming regions that are not affected by the AGN in these\u0000galaxies share the same part of the diagram as Star-forming galaxies. We\u0000examine the potential of the PAH-H2 diagram to disentangle AGN versus\u0000star-forming activity. Our results suggest that in Sy-like AGN, illumination\u0000and feedback from the AGN might affect the PAH population at nuclear and kpc\u0000scales, in particular, the ionization state of the PAH grains. However, PAH\u0000sizes are rather similar. The carriers of the ionized PAH bands (6.2 and 7.7\u0000micron) are less resilience than those of neutral PAH bands (11.3 micron),\u0000which might be particularly important for strongly AGN-host coupled systems.\u0000Therefore, caution must be applied when using PAH bands as star-formation rate\u0000indicators in these systems even at kpc scales, with the ionized ones being\u0000more affected by the AGN.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"139 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192599","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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