Paulo Montero-Camacho, Catalina Morales-Gutiérrez, Yao Zhang, Heyang Long, Yi Mao
The tumultuous effects of ultraviolet photons that source cosmic reionization, the subsequent compression and shock-heating of low-density regions, and the modulation of baryons in shallow potential wells induced by the passage of ionization fronts, collectively introduce perturbations to the evolution of the intergalactic medium in the post-reionization era. These enduring fluctuations persist deep into the post-reionization era, casting a challenge upon precision cosmology endeavors targeting tracers in this cosmic era. Simultaneously, these relics from reionization also present a unique opportunity to glean insights into the astrophysics that govern the epoch of reionization. In this work, we propose a first study of the cross-correlation of lya forest and 21 cm intensity mapping, accounting for the repercussions of inhomogeneous reionization in the post-reionization era. We investigate the ability of SKA $times$ DESI-like, SKA $times$ MUST-like, and PUMA $times$ MUST-like instrumental setups to achieve a high signal-to-noise ratio (SNR) in the redshift range $3.5 leq z leq 4$. Moreover, we assess how alterations in integration time, survey area, and reionization scenarios impact the SNR. Furthermore, we forecast the cross-correlation's potential to constrain cosmological parameters under varying assumptions: considering or disregarding reionization relics, marginalizing over reionization astrophysics, and assuming perfect knowledge of reionization. Notably, our findings underscore the remarkable capability of a futuristic PUMA $times$ MUST-like setup, with a modest 100-hour integration time over a 100 sq. deg. survey, to constrain the ionization efficiency error to $sigma_zeta = 3.42 $.
{"title":"Reionization relics in the cross-correlation between the Ly$α$ forest and 21 cm intensity mapping in the post-reionization era","authors":"Paulo Montero-Camacho, Catalina Morales-Gutiérrez, Yao Zhang, Heyang Long, Yi Mao","doi":"arxiv-2409.11613","DOIUrl":"https://doi.org/arxiv-2409.11613","url":null,"abstract":"The tumultuous effects of ultraviolet photons that source cosmic\u0000reionization, the subsequent compression and shock-heating of low-density\u0000regions, and the modulation of baryons in shallow potential wells induced by\u0000the passage of ionization fronts, collectively introduce perturbations to the\u0000evolution of the intergalactic medium in the post-reionization era. These\u0000enduring fluctuations persist deep into the post-reionization era, casting a\u0000challenge upon precision cosmology endeavors targeting tracers in this cosmic\u0000era. Simultaneously, these relics from reionization also present a unique\u0000opportunity to glean insights into the astrophysics that govern the epoch of\u0000reionization. In this work, we propose a first study of the cross-correlation\u0000of lya forest and 21 cm intensity mapping, accounting for the repercussions of\u0000inhomogeneous reionization in the post-reionization era. We investigate the\u0000ability of SKA $times$ DESI-like, SKA $times$ MUST-like, and PUMA $times$\u0000MUST-like instrumental setups to achieve a high signal-to-noise ratio (SNR) in\u0000the redshift range $3.5 leq z leq 4$. Moreover, we assess how alterations in\u0000integration time, survey area, and reionization scenarios impact the SNR.\u0000Furthermore, we forecast the cross-correlation's potential to constrain\u0000cosmological parameters under varying assumptions: considering or disregarding\u0000reionization relics, marginalizing over reionization astrophysics, and assuming\u0000perfect knowledge of reionization. Notably, our findings underscore the\u0000remarkable capability of a futuristic PUMA $times$ MUST-like setup, with a\u0000modest 100-hour integration time over a 100 sq. deg. survey, to constrain the\u0000ionization efficiency error to $sigma_zeta = 3.42 $.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"3 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257595","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Weilun Zheng, Kwan Chuen Chan, Haojie Xu, Le Zhang, Ruiyu Song
Accurately characterizing the true redshift (true-$z$) distribution of a photometric redshift (photo-$z$) sample is critical for cosmological analyses in imaging surveys. Clustering-based techniques, which include clustering-redshift (CZ) and self-calibration (SC) methods--depending on whether external spectroscopic data are used--offer powerful tools for this purpose. In this study, we explore the joint inference of the true-$z$ distribution by combining SC and CZ (denoted as SC+CZ). We derive simple multiplicative update rules to perform the joint inference. By incorporating appropriate error weighting and an additional weighting function, our method shows significant improvement over previous algorithms. We validate our approach using a DES Y3 mock catalog. The true-$z$ distribution estimated through the combined SC+CZ method is generally more accurate than using SC or CZ alone. To account for the different constraining powers of these methods, we assign distinct weights to the SC and CZ contributions. The optimal weights, which minimize the distribution error, depend on the relative constraining strength of the SC and CZ data. Specifically, for a spectroscopic redshift sample that represents 1% of the photo-$z$ sample, the optimal combination reduces the total error by 20% (40%) compared to using CZ (SC) alone, and it keeps the bias in mean redshift [$Delta bar{z} / (1 + z) $] at the level of 0.3%. Furthermore, when CZ data is only available in the low-$z$ range and the high-$z$ range relies solely on SC data, SC+CZ enables consistent estimation of the true-$z$ distribution across the entire redshift range. Our findings demonstrate that SC+CZ is an effective tool for constraining the true-$z$ distribution, paving the way for clustering-based methods to be applied at $zgtrsim 1$.
{"title":"Optimizing Redshift Distribution Inference through Joint Self-Calibration and Clustering-Redshift Synergy","authors":"Weilun Zheng, Kwan Chuen Chan, Haojie Xu, Le Zhang, Ruiyu Song","doi":"arxiv-2409.12009","DOIUrl":"https://doi.org/arxiv-2409.12009","url":null,"abstract":"Accurately characterizing the true redshift (true-$z$) distribution of a\u0000photometric redshift (photo-$z$) sample is critical for cosmological analyses\u0000in imaging surveys. Clustering-based techniques, which include\u0000clustering-redshift (CZ) and self-calibration (SC) methods--depending on\u0000whether external spectroscopic data are used--offer powerful tools for this\u0000purpose. In this study, we explore the joint inference of the true-$z$\u0000distribution by combining SC and CZ (denoted as SC+CZ). We derive simple\u0000multiplicative update rules to perform the joint inference. By incorporating\u0000appropriate error weighting and an additional weighting function, our method\u0000shows significant improvement over previous algorithms. We validate our\u0000approach using a DES Y3 mock catalog. The true-$z$ distribution estimated\u0000through the combined SC+CZ method is generally more accurate than using SC or\u0000CZ alone. To account for the different constraining powers of these methods, we\u0000assign distinct weights to the SC and CZ contributions. The optimal weights,\u0000which minimize the distribution error, depend on the relative constraining\u0000strength of the SC and CZ data. Specifically, for a spectroscopic redshift\u0000sample that represents 1% of the photo-$z$ sample, the optimal combination\u0000reduces the total error by 20% (40%) compared to using CZ (SC) alone, and it\u0000keeps the bias in mean redshift [$Delta bar{z} / (1 + z) $] at the level of\u00000.3%. Furthermore, when CZ data is only available in the low-$z$ range and the\u0000high-$z$ range relies solely on SC data, SC+CZ enables consistent estimation of\u0000the true-$z$ distribution across the entire redshift range. Our findings\u0000demonstrate that SC+CZ is an effective tool for constraining the true-$z$\u0000distribution, paving the way for clustering-based methods to be applied at\u0000$zgtrsim 1$.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"13 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257594","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}
A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
We present a weak lensing analysis of the galaxy cluster Abell 2390 at z = 0.23 using second moment shape measurements made in 411 short 60s exposures. The exposures are obtained in three broadband photometric filters (g, r, i) using WIYN-ODI. Shape measurement in individual exposures is done using a moment matching algorithm. Forced measurement is used when the moment matching algorithm fails to converge at low signal to noise ratio (SNR). The measurements made in individual images are combined using inverse error weight to obtain accurate shape of sources and hence recover shear. We use PhoSim simulations to validate shear measurements recovered by our pipeline. We find the mass of Abell 2390 is in agreement with previously published results. We also find the E-Mode maps show filamentary structures consistent with baryonic structures and recovers most clusters/groups of galaxies found using Optical and X-Ray data. Thus we demonstrate the feasibility of using Weak Lensing to map large scale structure of the universe. We also find the central portion of the cluster has a bimodal mass distribution and the relative orientation of the peaks are similar to X-Ray. We discuss earlier research on this galaxy cluster and show that a late stage merger accounts for all the observed data.
{"title":"Weak Lensing analysis of Abell 2390 using short exposures","authors":"A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski","doi":"arxiv-2409.12119","DOIUrl":"https://doi.org/arxiv-2409.12119","url":null,"abstract":"We present a weak lensing analysis of the galaxy cluster Abell 2390 at z =\u00000.23 using second moment shape measurements made in 411 short 60s exposures.\u0000The exposures are obtained in three broadband photometric filters (g, r, i)\u0000using WIYN-ODI. Shape measurement in individual exposures is done using a\u0000moment matching algorithm. Forced measurement is used when the moment matching\u0000algorithm fails to converge at low signal to noise ratio (SNR). The\u0000measurements made in individual images are combined using inverse error weight\u0000to obtain accurate shape of sources and hence recover shear. We use PhoSim\u0000simulations to validate shear measurements recovered by our pipeline. We find\u0000the mass of Abell 2390 is in agreement with previously published results. We\u0000also find the E-Mode maps show filamentary structures consistent with baryonic\u0000structures and recovers most clusters/groups of galaxies found using Optical\u0000and X-Ray data. Thus we demonstrate the feasibility of using Weak Lensing to\u0000map large scale structure of the universe. We also find the central portion of\u0000the cluster has a bimodal mass distribution and the relative orientation of the\u0000peaks are similar to X-Ray. We discuss earlier research on this galaxy cluster\u0000and show that a late stage merger accounts for all the observed data.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"21 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257593","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}
We confirm for the first time the existence of distinctive halo bias associated with the quadrupolar type of statistical anisotropy (SA) of the linear matter density field using cosmological $N$-body simulations. We find that the coefficient of the SA-induced bias for cluster-sized halos takes negative values and exhibits a decreasing trend with increasing halo mass. This results in the quadrupole halo power spectra in a statistically anisotropic universe being less amplified compared to the monopole spectra. The anisotropic feature in halo bias that we found presents a promising new tool for testing the hypothesis of a statistically anisotropic universe, with significant implications for the precise verification of anisotropic inflation scenarios and vector dark matter and dark energy models.
{"title":"First confirmation of anisotropic bias from statistically anisotropic matter distributions","authors":"Shogo Masaki, Maresuke Shiraishi, Takahiro Nishimichi, Teppei Okumura, Shuichiro Yokoyama","doi":"arxiv-2409.12004","DOIUrl":"https://doi.org/arxiv-2409.12004","url":null,"abstract":"We confirm for the first time the existence of distinctive halo bias\u0000associated with the quadrupolar type of statistical anisotropy (SA) of the\u0000linear matter density field using cosmological $N$-body simulations. We find\u0000that the coefficient of the SA-induced bias for cluster-sized halos takes\u0000negative values and exhibits a decreasing trend with increasing halo mass. This\u0000results in the quadrupole halo power spectra in a statistically anisotropic\u0000universe being less amplified compared to the monopole spectra. The anisotropic\u0000feature in halo bias that we found presents a promising new tool for testing\u0000the hypothesis of a statistically anisotropic universe, with significant\u0000implications for the precise verification of anisotropic inflation scenarios\u0000and vector dark matter and dark energy models.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"2 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257724","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}
Sophia R. Flury, Anne E. Jaskot, Alberto Saldana-Lopez, M. S. Oey, John Chisholm, Ricardo Amorín, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, Henry C. Ferguson, Mauro Giavalisco, Matthew Hayes, Timothy Heckman, Alaina Henry, Zhiyuan Ji, Lena Komarova, Floriane Leclercq, Alexandra Le Reste, Stephan McCandliss, Rui Marques-Chaves, Göran Östlin, Laura Pentericci, Swara Ravindranath, Michael Rutkowski, Claudia Scarlata, Daniel Schaerer, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Bingjie Wang, Gábor Worseck, Xinfeng Xu
One of the fundamental questions of cosmology is the origin and mechanism(s) responsible for the reionization of the Universe beyond $zsim6$. To address this question, many studies over the past decade have focused on local ($zsim0.3$) galaxies which leak ionizing radiation (Lyman continuum or LyC). However, line-of-sight effects and data quality have prohibited deeper insight into the nature of LyC escape. To circumvent these limitations, we analyze stacks of a consolidated sample of {it HST}/COS observations of the LyC in 89 galaxies at $zsim0.3$. From fitting of the continuum, we obtain information about the underlying stellar populations and neutral ISM geometry. We find that most LyC non-detections are not leaking appreciable LyC ($f_{esc}^{rm LyC}<1$%) but also that exceptional cases point to spatial variations in the LyC escape fraction $f_{esc}^{rm LyC}$. Stellar populations younger than 3 Myr lead to an increase in ionizing feedback, which in turn increases the isotropy of LyC escape. Moreover, mechanical feedback from supernovae in 8-10 Myr stellar populations is important for anisotropic gas distributions needed for LyC escape. While mechanical feedback is necessary for any LyC escape, high $f_{esc}^{rm LyC}$ ($>5$%) also requires a confluence of young stars and ionizing feedback. A two-stage burst of star formation could facilitate this optimal LyC escape scenario.
{"title":"The Low-Redshift Lyman Continuum Survey: The Roles of Stellar Feedback and ISM Geometry in LyC Escape","authors":"Sophia R. Flury, Anne E. Jaskot, Alberto Saldana-Lopez, M. S. Oey, John Chisholm, Ricardo Amorín, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, Henry C. Ferguson, Mauro Giavalisco, Matthew Hayes, Timothy Heckman, Alaina Henry, Zhiyuan Ji, Lena Komarova, Floriane Leclercq, Alexandra Le Reste, Stephan McCandliss, Rui Marques-Chaves, Göran Östlin, Laura Pentericci, Swara Ravindranath, Michael Rutkowski, Claudia Scarlata, Daniel Schaerer, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Bingjie Wang, Gábor Worseck, Xinfeng Xu","doi":"arxiv-2409.12118","DOIUrl":"https://doi.org/arxiv-2409.12118","url":null,"abstract":"One of the fundamental questions of cosmology is the origin and mechanism(s)\u0000responsible for the reionization of the Universe beyond $zsim6$. To address\u0000this question, many studies over the past decade have focused on local\u0000($zsim0.3$) galaxies which leak ionizing radiation (Lyman continuum or LyC).\u0000However, line-of-sight effects and data quality have prohibited deeper insight\u0000into the nature of LyC escape. To circumvent these limitations, we analyze\u0000stacks of a consolidated sample of {it HST}/COS observations of the LyC in 89\u0000galaxies at $zsim0.3$. From fitting of the continuum, we obtain information\u0000about the underlying stellar populations and neutral ISM geometry. We find that\u0000most LyC non-detections are not leaking appreciable LyC ($f_{esc}^{rm\u0000LyC}<1$%) but also that exceptional cases point to spatial variations in the\u0000LyC escape fraction $f_{esc}^{rm LyC}$. Stellar populations younger than 3 Myr\u0000lead to an increase in ionizing feedback, which in turn increases the isotropy\u0000of LyC escape. Moreover, mechanical feedback from supernovae in 8-10 Myr\u0000stellar populations is important for anisotropic gas distributions needed for\u0000LyC escape. While mechanical feedback is necessary for any LyC escape, high\u0000$f_{esc}^{rm LyC}$ ($>5$%) also requires a confluence of young stars and\u0000ionizing feedback. A two-stage burst of star formation could facilitate this\u0000optimal LyC escape scenario.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"10 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257644","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 reduced speed of light approximation has been employed to speed up radiative transfer simulations of reionization by a factor of $gtrsim 5-10$. However, it has been shown to cause significant errors in the HI-ionizing background near reionization's end in simulations of representative cosmological volumes. This can bias inferences on the galaxy ionizing emissivity required to match observables, such as the Ly$alpha$ forest. In this work, we show that using a reduced speed of light is, to a good approximation, equivalent to re-scaling the global ionizing emissivity in a redshift-dependent way. We derive this re-scaling and show that it can be used to ``correct'' the emissivity in reduced speed of light simulations. This approach of re-scaling the emissivity after the simulation has been run is useful in contexts where the emissivity is a free parameter. We test our method by running full speed of light simulations using these re-scaled emissivities and comparing them with their reduced speed of light counterparts. We find that for reduced speeds of light $tilde{c} geq 0.2$, the 21 cm power spectrum at $0.1 leq k /[h{rm Mpc}^{-1}] leq 0.2$ and key Ly$alpha$ forest observables agree to within $20%$ throughout reionization, and often better than $10%$. Position-dependent time-delay effects cause inaccuracies in reionization's morphology on large scales that produce errors up to a factor of $2$ for $tilde{c} leq 0.1$. Our method enables a factor of $5$ speedup of radiative transfer simulations of reionization in situations where the emissivity can be treated as a free parameter.
{"title":"Accurate simulations of reionization using the reduced speed of light approximation","authors":"Christopher Cain","doi":"arxiv-2409.11467","DOIUrl":"https://doi.org/arxiv-2409.11467","url":null,"abstract":"The reduced speed of light approximation has been employed to speed up\u0000radiative transfer simulations of reionization by a factor of $gtrsim 5-10$.\u0000However, it has been shown to cause significant errors in the HI-ionizing\u0000background near reionization's end in simulations of representative\u0000cosmological volumes. This can bias inferences on the galaxy ionizing\u0000emissivity required to match observables, such as the Ly$alpha$ forest. In\u0000this work, we show that using a reduced speed of light is, to a good\u0000approximation, equivalent to re-scaling the global ionizing emissivity in a\u0000redshift-dependent way. We derive this re-scaling and show that it can be used\u0000to ``correct'' the emissivity in reduced speed of light simulations. This\u0000approach of re-scaling the emissivity after the simulation has been run is\u0000useful in contexts where the emissivity is a free parameter. We test our method\u0000by running full speed of light simulations using these re-scaled emissivities\u0000and comparing them with their reduced speed of light counterparts. We find that\u0000for reduced speeds of light $tilde{c} geq 0.2$, the 21 cm power spectrum at\u0000$0.1 leq k /[h{rm Mpc}^{-1}] leq 0.2$ and key Ly$alpha$ forest observables\u0000agree to within $20%$ throughout reionization, and often better than $10%$.\u0000Position-dependent time-delay effects cause inaccuracies in reionization's\u0000morphology on large scales that produce errors up to a factor of $2$ for\u0000$tilde{c} leq 0.1$. Our method enables a factor of $5$ speedup of radiative\u0000transfer simulations of reionization in situations where the emissivity can be\u0000treated as a free parameter.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"37 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257637","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}
Emma Ayçoberry, Pranjal R. S., Karim Benabed, Yohan Dubois, Elisabeth Krause, Tim Eifler
Statistical properties of LSS serve as powerful tools to constrain the cosmological properties of our Universe. Tracing the gas pressure, the tSZ effect is a biased probe of mass distribution and can be used to test the physics of feedback or cosmological models. Therefore, it is crucial to develop robust modeling of hot gas pressure for applications to tSZ surveys. Since gas collapses into bound structures, it is expected that most of the tSZ signal is within halos produced by cosmic accretion shocks. Hence, simple empirical halo models can be used to predict the tSZ power spectra. In this study, we employed the HMx halo model to compare the tSZ power spectra with those of several hydrodynamical simulations: the Horizon suite and the Magneticum simulation. We examined various contributions to the tSZ power spectrum across different redshifts, including the one- and two-halo term decomposition, the amount of bound gas, the importance of different masses and the electron pressure profiles. Our comparison of the tSZ power spectrum reveals discrepancies that increase with redshift. We find a 20% to 50% difference between the measured and predicted tSZ angular power spectrum over the multipole range $ell=10^3-10^4$. Our analysis reveals that these differences are driven by the excess of power in the predicted two-halo term at low k and in the one-halo term at high k. At higher redshifts (z~3), simulations indicate that more power comes from outside the virial radius than from inside suggesting a limitation in the applicability of the halo model. We observe differences in the pressure profiles, despite the fair level of agreement on the tSZ power spectrum at low redshift with the default calibration of the halo model. In conclusion, our study suggests that the properties of the halo model need to be carefully controlled against real or mock data to be proven useful for cosmological purposes.
{"title":"Testing the thermal Sunyaev-Zel'dovich power spectrum of a halo model using hydrodynamical simulations","authors":"Emma Ayçoberry, Pranjal R. S., Karim Benabed, Yohan Dubois, Elisabeth Krause, Tim Eifler","doi":"arxiv-2409.11472","DOIUrl":"https://doi.org/arxiv-2409.11472","url":null,"abstract":"Statistical properties of LSS serve as powerful tools to constrain the\u0000cosmological properties of our Universe. Tracing the gas pressure, the tSZ\u0000effect is a biased probe of mass distribution and can be used to test the\u0000physics of feedback or cosmological models. Therefore, it is crucial to develop\u0000robust modeling of hot gas pressure for applications to tSZ surveys. Since gas\u0000collapses into bound structures, it is expected that most of the tSZ signal is\u0000within halos produced by cosmic accretion shocks. Hence, simple empirical halo\u0000models can be used to predict the tSZ power spectra. In this study, we employed\u0000the HMx halo model to compare the tSZ power spectra with those of several\u0000hydrodynamical simulations: the Horizon suite and the Magneticum simulation. We\u0000examined various contributions to the tSZ power spectrum across different\u0000redshifts, including the one- and two-halo term decomposition, the amount of\u0000bound gas, the importance of different masses and the electron pressure\u0000profiles. Our comparison of the tSZ power spectrum reveals discrepancies that\u0000increase with redshift. We find a 20% to 50% difference between the measured\u0000and predicted tSZ angular power spectrum over the multipole range\u0000$ell=10^3-10^4$. Our analysis reveals that these differences are driven by the\u0000excess of power in the predicted two-halo term at low k and in the one-halo\u0000term at high k. At higher redshifts (z~3), simulations indicate that more power\u0000comes from outside the virial radius than from inside suggesting a limitation\u0000in the applicability of the halo model. We observe differences in the pressure\u0000profiles, despite the fair level of agreement on the tSZ power spectrum at low\u0000redshift with the default calibration of the halo model. In conclusion, our\u0000study suggests that the properties of the halo model need to be carefully\u0000controlled against real or mock data to be proven useful for cosmological\u0000purposes.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"214 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257638","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 reports of cosmological parity violation in the 4PCF raises the question of how such violations could be systematically generated. Here we present a constructive procedure to generate arbitrary violations of vectorial and tensorial types on any scale, which is computationally efficient in the squeezed limit. We directly compute their numerical transfer function, and find strong conservation in the linear regime. This procedure spans all squeezed parity violating observables at the 4PCF, following the quadratic estimator classification.
{"title":"Systematic analysis of Parity-Violating modes","authors":"Hong-Ming Zhu, Ue-Li Pen","doi":"arxiv-2409.11400","DOIUrl":"https://doi.org/arxiv-2409.11400","url":null,"abstract":"Recent reports of cosmological parity violation in the 4PCF raises the\u0000question of how such violations could be systematically generated. Here we\u0000present a constructive procedure to generate arbitrary violations of vectorial\u0000and tensorial types on any scale, which is computationally efficient in the\u0000squeezed limit. We directly compute their numerical transfer function, and find\u0000strong conservation in the linear regime. This procedure spans all squeezed\u0000parity violating observables at the 4PCF, following the quadratic estimator\u0000classification.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"17 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257633","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}
Tibor Dome, Simon May, Alex Laguë, David J. E. Marsh, Sarah Johnston, Sownak Bose, Alex Tocher, Anastasia Fialkov
We study the implications of relaxing the requirement for ultralight axions to account for all dark matter in the Universe by examining mixed dark matter (MDM) cosmologies with axion fractions $f leq 0.3$ within the fuzzy dark matter (FDM) window $10^{-25}$ eV $lesssim m lesssim 10^{-23}$ eV. Our simulations, using a new MDM gravity solver implemented in AxiREPO, capture wave dynamics across various scales with high accuracy down to redshifts $zapprox 1$. We identify halos with Rockstar using the CDM component and find good agreement of inferred halo mass functions (HMFs) and concentration-mass relations with theoretical models across redshifts $z=1-10$. This justifies our halo finder approach a posteriori as well as the assumptions underlying the MDM halo model AxionHMcode. Using the inferred axion halo mass - cold halo mass relation $M_{text{a}}(M_{text{c}})$ and calibrating a generalised smoothing parameter $alpha$ to our MDM simulations, we present a new version of AxionHMcode. The code exhibits excellent agreement with simulations on scales $k< 20 h$ cMpc$^{-1}$ at redshifts $z=1-3.5$ for $fleq 0.1$ around the fiducial axion mass $m = 10^{-24.5}$ eV $ = 3.16times 10^{-25}$ eV, with maximum deviations remaining below 10%. For axion fractions $fleq 0.3$, the model maintains accuracy with deviations under 20% at redshifts $zapprox 1$ and scales $k< 10 h$ cMpc$^{-1}$, though deviations can reach up to 30% for higher redshifts when $f=0.3$. Reducing the run-time for a single evaluation of AxionHMcode to below $1$ minute, these results highlight the potential of AxionHMcode to provide a robust framework for parameter sampling across MDM cosmologies in Bayesian constraint and forecast analyses.
我们通过研究在模糊暗物质（FDM）窗口$10^{-25}$ eV $lesssim m lesssim 10^{-23}$ eV范围内轴子分数为$f leq 0.3$的混合暗物质（MDM）宇宙学，研究了放宽对超轻轴子的要求以解释宇宙中所有暗物质的影响。我们的模拟使用了在AxiREPO中实现的一种新的MDM引力求解器，能够高精度地捕捉到各种尺度的波动力学，直至红移$z（约1$）。我们用 "摇滚之星"（Rockstar）利用CDM部分识别光环，发现推断出的光环质量函数（HMF）和浓度-质量关系与理论模型在红移$z=1-10$之间非常吻合。这证明了我们的后验光晕发现方法以及MDM光晕模型AxionHMcode的假设是正确的。利用推断出的轴晕质量-冷晕质量相关性$M_{text{a}}(M_{text{c}})$，并校准一个通用的平滑参数$alpha$到我们的MDM模拟，我们提出了一个新版本的AxionHMcode。在红移$z=1-3.5$、轴子质量$m = 10^{-24.5}$ eV $ = 3.16乘以10^{-25}$eV的条件下，该代码在尺度$k< 20 h$ cMpc$^{-1}$ 和$fleq 0.1$周围的模拟结果显示出极好的一致性，最大偏差保持在10%以下。对于轴子分数$fleq 0.3$，该模型在红移$zapprox 1$和尺度$k< 10 h$ cMpc$^{-1}$时保持了低于20%的精确度，尽管当$f=0.3$时，在更高的红移下偏差可能达到30%。这些结果使AxionHMcode的单次评估运行时间缩短到1分钟以下，突出了AxionHMcode在贝叶斯约束和预测分析中为跨MDM宇宙学的参数采样提供稳健框架的潜力。
{"title":"Improved Halo Model Calibrations for Mixed Dark Matter Models of Ultralight Axions","authors":"Tibor Dome, Simon May, Alex Laguë, David J. E. Marsh, Sarah Johnston, Sownak Bose, Alex Tocher, Anastasia Fialkov","doi":"arxiv-2409.11469","DOIUrl":"https://doi.org/arxiv-2409.11469","url":null,"abstract":"We study the implications of relaxing the requirement for ultralight axions\u0000to account for all dark matter in the Universe by examining mixed dark matter\u0000(MDM) cosmologies with axion fractions $f leq 0.3$ within the fuzzy dark\u0000matter (FDM) window $10^{-25}$ eV $lesssim m lesssim 10^{-23}$ eV. Our\u0000simulations, using a new MDM gravity solver implemented in AxiREPO, capture\u0000wave dynamics across various scales with high accuracy down to redshifts\u0000$zapprox 1$. We identify halos with Rockstar using the CDM component and find\u0000good agreement of inferred halo mass functions (HMFs) and concentration-mass\u0000relations with theoretical models across redshifts $z=1-10$. This justifies our\u0000halo finder approach a posteriori as well as the assumptions underlying the MDM\u0000halo model AxionHMcode. Using the inferred axion halo mass - cold halo mass\u0000relation $M_{text{a}}(M_{text{c}})$ and calibrating a generalised smoothing\u0000parameter $alpha$ to our MDM simulations, we present a new version of\u0000AxionHMcode. The code exhibits excellent agreement with simulations on scales\u0000$k< 20 h$ cMpc$^{-1}$ at redshifts $z=1-3.5$ for $fleq 0.1$ around the\u0000fiducial axion mass $m = 10^{-24.5}$ eV $ = 3.16times 10^{-25}$ eV, with\u0000maximum deviations remaining below 10%. For axion fractions $fleq 0.3$, the\u0000model maintains accuracy with deviations under 20% at redshifts $zapprox 1$\u0000and scales $k< 10 h$ cMpc$^{-1}$, though deviations can reach up to 30% for\u0000higher redshifts when $f=0.3$. Reducing the run-time for a single evaluation of\u0000AxionHMcode to below $1$ minute, these results highlight the potential of\u0000AxionHMcode to provide a robust framework for parameter sampling across MDM\u0000cosmologies in Bayesian constraint and forecast analyses.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"20 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257631","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}
Dennis Neumann, Robert Reischke, Steffen Hagstotz, Hendrik Hildebrandt
We explore the potential for improving constraints on gravity by leveraging correlations in the dispersion measure derived from Fast Radio Bursts (FRBs) in combination with cosmic shear. Specifically, we focus on Horndeski gravity, inferring the kinetic braiding and Planck mass run rate from a stage-4 cosmic shear mock survey alongside a survey comprising $10^4$ FRBs. For the inference pipeline, we utilise hi_class to predict the linear matter power spectrum in modified gravity scenarios, while non-linear corrections are modelled with HMcode, including feedback mechanisms. Our findings indicate that FRBs can disentangle degeneracies between baryonic feedback and cosmological parameters, as well as the mass of massive neutrinos. Since these parameters are also degenerate with modified gravity parameters, the inclusion of FRBs can enhance constraints on Horndeski parameters by up to $40$ percent, despite being a less significant measurement. Additionally, we apply our model to current FRB data and use the uncertainty in the $mathrm{DM}-z$ relation to impose limits on gravity. However, due to the limited sample size of current data, constraints are predominantly influenced by theoretical priors. Despite this, our study demonstrates that FRBs will significantly augment the limited set of cosmological probes available, playing a critical role in providing alternative tests of feedback, cosmology, and gravity. All codes used in this work are made publically available.
{"title":"Fast radio bursts as a probe of gravity on cosmological scales","authors":"Dennis Neumann, Robert Reischke, Steffen Hagstotz, Hendrik Hildebrandt","doi":"arxiv-2409.11163","DOIUrl":"https://doi.org/arxiv-2409.11163","url":null,"abstract":"We explore the potential for improving constraints on gravity by leveraging\u0000correlations in the dispersion measure derived from Fast Radio Bursts (FRBs) in\u0000combination with cosmic shear. Specifically, we focus on Horndeski gravity,\u0000inferring the kinetic braiding and Planck mass run rate from a stage-4 cosmic\u0000shear mock survey alongside a survey comprising $10^4$ FRBs. For the inference\u0000pipeline, we utilise hi_class to predict the linear matter power spectrum in\u0000modified gravity scenarios, while non-linear corrections are modelled with\u0000HMcode, including feedback mechanisms. Our findings indicate that FRBs can\u0000disentangle degeneracies between baryonic feedback and cosmological parameters,\u0000as well as the mass of massive neutrinos. Since these parameters are also\u0000degenerate with modified gravity parameters, the inclusion of FRBs can enhance\u0000constraints on Horndeski parameters by up to $40$ percent, despite being a less\u0000significant measurement. Additionally, we apply our model to current FRB data\u0000and use the uncertainty in the $mathrm{DM}-z$ relation to impose limits on\u0000gravity. However, due to the limited sample size of current data, constraints\u0000are predominantly influenced by theoretical priors. Despite this, our study\u0000demonstrates that FRBs will significantly augment the limited set of\u0000cosmological probes available, playing a critical role in providing alternative\u0000tests of feedback, cosmology, and gravity. All codes used in this work are made\u0000publically available.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"28 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257634","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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