We present the luminosity-halo mass relations of satellite (sLHMRs) galaxies in the SDSS redMaPPer cluster catalogue and the effects of the dense cluster environment on subhalo mass evolution. We use data from the Subaru Hyper Suprime-Cam survey Year-3 catalogue of galaxy shapes to measure the weak lensing signal around these satellites. This signal serves as a probe of the matter distribution around the satellites, thereby providing the masses of their associated subhalos. We bin our satellites based on physical observable quantities such as their luminosity or the host cluster's richness, combined with their cluster-centric radial separations. Our results indicate that although more luminous satellites tend to reside in more massive halos, the sLHMRs depend on the distance of the satellite from the cluster centre. Subhalos near the cluster centre (within $<0.3 h^{-1}Mpc$) are stripped of mass. Consequently, the ratio of subhalo mass to luminosity decreases near the cluster centre. For low luminosity galaxies ($L < 10^{10} h^{-2}L_{odot}$), the lack of evidence of increasing subhalo masses with luminosity shows the impact of tidal stripping. We also present stellar-to-subhalo mass relations (sSHMRs) for our satellite sample evolving at different cluster-centric separations. Inferred sSHMRs in the outer radial bin appear to match that observed for the field galaxies. We show that the sSHMRs from the mock-redMaPPer run on galaxy catalogues generated by the empirical UniverseMachine galaxy formation model are in good agreement with our observational results. Satellites, when binned based on the host cluster's richness, show very little dependence of the subhalo mass on the richness.
{"title":"Environmental dependence on galaxy-halo connections for satellites using HSC weak lensing","authors":"Amit Kumar, Surhud More","doi":"arxiv-2409.05795","DOIUrl":"https://doi.org/arxiv-2409.05795","url":null,"abstract":"We present the luminosity-halo mass relations of satellite (sLHMRs) galaxies\u0000in the SDSS redMaPPer cluster catalogue and the effects of the dense cluster\u0000environment on subhalo mass evolution. We use data from the Subaru Hyper\u0000Suprime-Cam survey Year-3 catalogue of galaxy shapes to measure the weak\u0000lensing signal around these satellites. This signal serves as a probe of the\u0000matter distribution around the satellites, thereby providing the masses of\u0000their associated subhalos. We bin our satellites based on physical observable\u0000quantities such as their luminosity or the host cluster's richness, combined\u0000with their cluster-centric radial separations. Our results indicate that\u0000although more luminous satellites tend to reside in more massive halos, the\u0000sLHMRs depend on the distance of the satellite from the cluster centre.\u0000Subhalos near the cluster centre (within $<0.3 h^{-1}Mpc$) are stripped of\u0000mass. Consequently, the ratio of subhalo mass to luminosity decreases near the\u0000cluster centre. For low luminosity galaxies ($L < 10^{10} h^{-2}L_{odot}$),\u0000the lack of evidence of increasing subhalo masses with luminosity shows the\u0000impact of tidal stripping. We also present stellar-to-subhalo mass relations\u0000(sSHMRs) for our satellite sample evolving at different cluster-centric\u0000separations. Inferred sSHMRs in the outer radial bin appear to match that\u0000observed for the field galaxies. We show that the sSHMRs from the\u0000mock-redMaPPer run on galaxy catalogues generated by the empirical\u0000UniverseMachine galaxy formation model are in good agreement with our\u0000observational results. Satellites, when binned based on the host cluster's\u0000richness, show very little dependence of the subhalo mass on the richness.","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":"142192566","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}
Pierre Ocvirk, Joseph S. W. Lewis, Luke Conaboy, Yohan Dubois, Matthieu Bethermin, Jenny G. Sorce, Dominique Aubert, Paul R. Shapiro, Taha Dawoodbhoy, Joohyun Lee, Romain Teyssier, Gustavo Yepes, Stefan Gottlöber, Ilian T. Iliev, Kyungjin Ahn, Hyunbae Park
We investigate the spatial offsets between dust and ultraviolet (UV) emission in high-redshift galaxies using the Cosmic Dawn III (CoDa III) simulation, a state-of-the-art fully coupled radiation-hydrodynamics cosmological simulation. Recent observations have revealed puzzling spatial disparities between ALMA dust continuum and UV emission as seen by HST and JWST in galaxies at z=5-7, compelling us to propose a physical interpretation of such offsets. Our simulation, which incorporates a dynamical dust model, naturally reproduces these offsets in massive, UV-bright galaxies (log$_{10}$(M$_{rm{DM}}$/M$_{odot}$)>11.5, M$_{rm{AB1500}}$<-20). We find that dust-UV offsets increase with halo mass and UV brightness, reaching up to $sim 2$ pkpc for the most massive systems, in good agreement with observational data from the ALPINE and REBELS surveys. Our analysis reveals that these offsets primarily result from severe dust extinction in galactic centers rather than a misalignment between dust and stellar mass distributions. The dust remains well-aligned with the bulk stellar component, and we predict the dust continuum should therefore align well with the stellar rest-frame NIR component, less affected by dust attenuation. This study provides crucial insights into the complex interplay between star formation, dust distribution, and observed galaxy morphologies during the epoch of reionization, highlighting the importance of dust in shaping the appearance of early galaxies at UV wavelengths.
{"title":"Dust-UV offsets in high-redshift galaxies in the Cosmic Dawn III simulation","authors":"Pierre Ocvirk, Joseph S. W. Lewis, Luke Conaboy, Yohan Dubois, Matthieu Bethermin, Jenny G. Sorce, Dominique Aubert, Paul R. Shapiro, Taha Dawoodbhoy, Joohyun Lee, Romain Teyssier, Gustavo Yepes, Stefan Gottlöber, Ilian T. Iliev, Kyungjin Ahn, Hyunbae Park","doi":"arxiv-2409.05946","DOIUrl":"https://doi.org/arxiv-2409.05946","url":null,"abstract":"We investigate the spatial offsets between dust and ultraviolet (UV) emission\u0000in high-redshift galaxies using the Cosmic Dawn III (CoDa III) simulation, a\u0000state-of-the-art fully coupled radiation-hydrodynamics cosmological simulation.\u0000Recent observations have revealed puzzling spatial disparities between ALMA\u0000dust continuum and UV emission as seen by HST and JWST in galaxies at z=5-7,\u0000compelling us to propose a physical interpretation of such offsets. Our\u0000simulation, which incorporates a dynamical dust model, naturally reproduces\u0000these offsets in massive, UV-bright galaxies\u0000(log$_{10}$(M$_{rm{DM}}$/M$_{odot}$)>11.5, M$_{rm{AB1500}}$<-20). We find\u0000that dust-UV offsets increase with halo mass and UV brightness, reaching up to\u0000$sim 2$ pkpc for the most massive systems, in good agreement with\u0000observational data from the ALPINE and REBELS surveys. Our analysis reveals\u0000that these offsets primarily result from severe dust extinction in galactic\u0000centers rather than a misalignment between dust and stellar mass distributions.\u0000The dust remains well-aligned with the bulk stellar component, and we predict\u0000the dust continuum should therefore align well with the stellar rest-frame NIR\u0000component, less affected by dust attenuation. This study provides crucial\u0000insights into the complex interplay between star formation, dust distribution,\u0000and observed galaxy morphologies during the epoch of reionization, highlighting\u0000the importance of dust in shaping the appearance of early galaxies at UV\u0000wavelengths.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"82 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192565","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}
M. Kosiba, N. Cerardi, M. Pierre, F. Lanusse, C. Garrel, N. Werner, M. Shalak
The number density of galaxy clusters across mass and redshift has been established as a powerful cosmological probe. Cosmological analyses with galaxy clusters traditionally employ scaling relations. However, many challenges arise from this approach as the scaling relations are highly scattered, may be ill-calibrated, depend on the cosmology, and contain many nuisance parameters with low physical significance. In this paper, we use a simulation-based inference method utilizing artificial neural networks to optimally extract cosmological information from a shallow X-ray survey of galaxy clusters, solely using count rates (CR), hardness ratios (HR), and redshifts. This procedure enables us to conduct likelihood-free inference of cosmological parameters $Omega_{mathrm{m}}$ and $sigma_8$. We analytically generate simulations of galaxy cluster distribution in a CR, HR space in multiple redshift bins based on totally random combinations of cosmological and scaling relation parameters. We train Convolutional Neural Networks (CNNs) to retrieve the cosmological parameters from these simulations. We then use neural density estimation (NDE) neural networks to predict the posterior probability distribution of $Omega_{mathrm{m}}$ and $sigma_8$ given an input galaxy cluster sample. The 1 $sigma$ errors of our density estimator on one of the target testing simulations are 1000 deg$^2$: 15.2% for $Omega_{mathrm{m}}$ and 10.0% for $sigma_8$; 10000 deg$^2$: 9.6% for $Omega_{mathrm{m}}$ and 5.6% for $sigma_8$. We also compare our results with Fisher analysis. We demonstrate, as a proof of concept, that it is possible to calculate cosmological predictions of $Omega_{mathrm{m}}$ and $sigma_8$ from a galaxy cluster population without explicitly computing cluster masses and even, the scaling relation coefficients, thus avoiding potential biases resulting from such a procedure. [abridged]
星系团在不同质量和红移下的数量密度已被确定为一个强大的宇宙学探测器。利用星系团进行宇宙学分析，传统上采用比例关系。然而，这种方法面临许多挑战，因为缩放关系高度分散，可能未经校准，依赖于宇宙学，而且包含许多物理意义不大的干扰参数。在本文中，我们利用人工神经网络，使用一种基于模拟的推理方法，从星系团的浅层 X 射线调查中，仅利用计数率（CR）、硬度比（HR）和红移，优化提取宇宙学信息。这一过程使我们能够对宇宙学参数$Omega_{mathrm{m}}$和$sigma_8$进行无似然推理。我们根据宇宙学参数和比例关系参数的完全随机组合，分析生成多个红移箱内CR、HR空间中星系团分布的模拟结果。然后，我们使用神经密度估计（NDE）神经网络来预测输入星系团样本的$Omega_{mathrm{m}}$和$sigma_8$的后验概率分布。我们的密度估算器在一个目标测试模拟中的1 $/sigma$误差是1000 deg$^2$：$Omega_{mathrm{m}}$为15.2%，$sigma_8$为10.0%；10000 deg$^2$：$Omega_{mathrm{m}}$为9.6%，$sigma_8$为5.6%。我们还将结果与费雪分析进行了比较。作为概念证明，我们证明了可以通过星系团来计算$Omega_{mathrm{m}}$和$sigma_8$的宇宙学预测值，而不需要明确计算星系团质量，甚至不需要计算缩放相关系数，从而避免了这种方法可能产生的偏差。[节略]
{"title":"The cosmological analysis of X-ray cluster surveys: VI. Inference based on analytically simulated observable diagrams","authors":"M. Kosiba, N. Cerardi, M. Pierre, F. Lanusse, C. Garrel, N. Werner, M. Shalak","doi":"arxiv-2409.06001","DOIUrl":"https://doi.org/arxiv-2409.06001","url":null,"abstract":"The number density of galaxy clusters across mass and redshift has been\u0000established as a powerful cosmological probe. Cosmological analyses with galaxy\u0000clusters traditionally employ scaling relations. However, many challenges arise\u0000from this approach as the scaling relations are highly scattered, may be\u0000ill-calibrated, depend on the cosmology, and contain many nuisance parameters\u0000with low physical significance. In this paper, we use a simulation-based\u0000inference method utilizing artificial neural networks to optimally extract\u0000cosmological information from a shallow X-ray survey of galaxy clusters, solely\u0000using count rates (CR), hardness ratios (HR), and redshifts. This procedure\u0000enables us to conduct likelihood-free inference of cosmological parameters\u0000$Omega_{mathrm{m}}$ and $sigma_8$. We analytically generate simulations of\u0000galaxy cluster distribution in a CR, HR space in multiple redshift bins based\u0000on totally random combinations of cosmological and scaling relation parameters.\u0000We train Convolutional Neural Networks (CNNs) to retrieve the cosmological\u0000parameters from these simulations. We then use neural density estimation (NDE)\u0000neural networks to predict the posterior probability distribution of\u0000$Omega_{mathrm{m}}$ and $sigma_8$ given an input galaxy cluster sample. The\u00001 $sigma$ errors of our density estimator on one of the target testing\u0000simulations are 1000 deg$^2$: 15.2% for $Omega_{mathrm{m}}$ and 10.0% for\u0000$sigma_8$; 10000 deg$^2$: 9.6% for $Omega_{mathrm{m}}$ and 5.6% for\u0000$sigma_8$. We also compare our results with Fisher analysis. We demonstrate,\u0000as a proof of concept, that it is possible to calculate cosmological\u0000predictions of $Omega_{mathrm{m}}$ and $sigma_8$ from a galaxy cluster\u0000population without explicitly computing cluster masses and even, the scaling\u0000relation coefficients, thus avoiding potential biases resulting from such a\u0000procedure. [abridged]","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":"142192564","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}
Rongpu Zhou, Julien Guy, Sergey E. Koposov, Edward F. Schlafly, David Schlegel, Jessica Aguilar, Steven Ahlen, Stephen Bailey, David Bianchi, David Brooks, Edmond Chaussidon, Todd Claybaugh, Kyle Dawson, Axel de la Macorra, Biprateep Dey, Daniel J. Eisenstein, Simone Ferraro, Andreu Font-Ribera, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Stephanie Juneau, Robert Kehoe, David Kirkby, Theodore Kisner, Anthony Kremin, Andrew Lambert, Martin Landriau, Laurent Le Guillou, Michael E. Levi, Ting S. Li, Marc Manera, Paul Martini, Aaron Meisner, Ramon Miquel, John Moustakas, Adam D. Myers, Jeffrey A. Newman, Gustavo Niz, Nathalie Palanque-Delabrouille, Will J. Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Graziano Rossi, Eusebio Sanchez, Andrew K. Saydjari, Michael Schubnell, David Sprayberry, Gregory Tarl, Benjamin A. Weaver, Pauline Zarrouk, Hu Zou
We present new Galactic reddening maps of the high Galactic latitude sky using DESI imaging and spectroscopy. We directly measure the reddening of 2.6 million stars by comparing the observed stellar colors in $g-r$ and $r-z$ from DESI imaging with the synthetic colors derived from DESI spectra from the first two years of the survey. The reddening in the two colors is on average consistent with the cite{fitzpatrick_correcting_1999} extinction curve with $R_mathrm{V}=3.1$. We find that our reddening maps differ significantly from the commonly used cite{schlegel_maps_1998} (SFD) reddening map (by up to 80 mmag in $E(B-V)$), and we attribute most of this difference to systematic errors in the SFD map. To validate the reddening map, we select a galaxy sample with extinction correction based on our reddening map, and this yields significantly better uniformity than the SFD extinction correction. Finally, we discuss the potential systematic errors in the DESI reddening measurements, including the photometric calibration errors that are the limiting factor on our accuracy. The $E(g-r)$ and $E(g-r)$ maps presented in this work, and for convenience their corresponding $E(B-V)$ maps with SFD calibration, are publicly available.
{"title":"Stellar reddening map from DESI imaging and spectroscopy","authors":"Rongpu Zhou, Julien Guy, Sergey E. Koposov, Edward F. Schlafly, David Schlegel, Jessica Aguilar, Steven Ahlen, Stephen Bailey, David Bianchi, David Brooks, Edmond Chaussidon, Todd Claybaugh, Kyle Dawson, Axel de la Macorra, Biprateep Dey, Daniel J. Eisenstein, Simone Ferraro, Andreu Font-Ribera, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Stephanie Juneau, Robert Kehoe, David Kirkby, Theodore Kisner, Anthony Kremin, Andrew Lambert, Martin Landriau, Laurent Le Guillou, Michael E. Levi, Ting S. Li, Marc Manera, Paul Martini, Aaron Meisner, Ramon Miquel, John Moustakas, Adam D. Myers, Jeffrey A. Newman, Gustavo Niz, Nathalie Palanque-Delabrouille, Will J. Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Graziano Rossi, Eusebio Sanchez, Andrew K. Saydjari, Michael Schubnell, David Sprayberry, Gregory Tarl, Benjamin A. Weaver, Pauline Zarrouk, Hu Zou","doi":"arxiv-2409.05140","DOIUrl":"https://doi.org/arxiv-2409.05140","url":null,"abstract":"We present new Galactic reddening maps of the high Galactic latitude sky\u0000using DESI imaging and spectroscopy. We directly measure the reddening of 2.6\u0000million stars by comparing the observed stellar colors in $g-r$ and $r-z$ from\u0000DESI imaging with the synthetic colors derived from DESI spectra from the first\u0000two years of the survey. The reddening in the two colors is on average\u0000consistent with the cite{fitzpatrick_correcting_1999} extinction curve with\u0000$R_mathrm{V}=3.1$. We find that our reddening maps differ significantly from\u0000the commonly used cite{schlegel_maps_1998} (SFD) reddening map (by up to 80\u0000mmag in $E(B-V)$), and we attribute most of this difference to systematic\u0000errors in the SFD map. To validate the reddening map, we select a galaxy sample\u0000with extinction correction based on our reddening map, and this yields\u0000significantly better uniformity than the SFD extinction correction. Finally, we\u0000discuss the potential systematic errors in the DESI reddening measurements,\u0000including the photometric calibration errors that are the limiting factor on\u0000our accuracy. The $E(g-r)$ and $E(g-r)$ maps presented in this work, and for\u0000convenience their corresponding $E(B-V)$ maps with SFD calibration, are\u0000publicly available.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"79 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192562","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}
Mohd Kamran, Martin Sahlén, Debanjan Sarkar, Suman Majumdar
The neutral hydrogen (HI) power spectrum, measured from intensity fluctuations in the 21-cm background, offers insights into the large-scale structures (LSS) of our Universe in the post-reionization era (redshift $z<6$). A significant amount of HI is expected to reside in low- and intermediate-density environments, but the power spectrum mainly captures information from high-density regions. To more fully extract the information contained in the HI field, we investigate the use of a marked power spectrum statistic. Here, the power spectrum is effectively re-weighted using a non-linear mark function which depends on the smoothed local density, such that low- or high-density regions are up- or down-weighted. This approach may also capture information on some higher-order statistical moments of the field. We model the HI distribution using semi-numerical simulations and for the first time study the marked HI power spectrum, across $1 leq z leq 5$. Our analysis indicates that there is considerable evolution of the HI field during the post-reionization era. Over a wide range of length scales (comoving wave numbers $0.05leq k leq 1.0$ Mpc$^{-1}$) we expectedly find that the HI evolves slowly at early times, but more rapidly at late times. This evolution is not well-captured by the power spectrum of the standard (unmarked) HI field. We also study how the evolution of the HI field depends on the chosen smoothing scale for the mark, and how this affects the marked power spectrum. We conclude that the information about the HI content at low and intermediate densities is important for a correct and consistent analysis of HI content and evolution based on the 21-cm background. The marked power spectrum can thus provide a less biased statistic for parameter constraints than the normal power spectrum.
中性氢（HI）的功率谱是通过 21 厘米背景的强度波动测量的，它提供了对我们宇宙在后电离时代（红移 $z<6$）的大尺度结构（LSS）的洞察。为了更充分地提取 HI 场中包含的信息，我们研究了标记功率谱统计量的使用。在这里，使用非线性标记函数对功率谱进行有效的重新加权，该函数取决于平滑后的局部密度，从而对低密度或高密度区域进行加权或减权。这种方法还可以捕捉场的一些高阶统计矩的信息。我们用半数值模拟的方法对HI分布进行了建模，并首次研究了HI的标记功率谱，跨度为1 leq z leq 5$。我们的分析表明，在后重离子时代，HI场有相当大的演化。在很宽的长度尺度范围内（移动波数为0.05±q k leq 1.0$ Mpc$^{-1}$），我们意外地发现，HI在早期的演化很缓慢，而在晚期则更迅速。我们还研究了HI场的演化如何依赖于所选择的标记平滑尺度，以及这如何影响标记功率谱。我们得出的结论是，低密度和中密度下的 HI 含量信息，对于基于 21 厘米背景对 HI 含量和演化进行正确一致的分析非常重要。因此，与正常功率谱相比，标记功率谱可以为参数约束提供更少偏差的统计量。
{"title":"The re-markable 21-cm power spectrum I: Probing the HI distribution in the post-reionization era using marked statistics","authors":"Mohd Kamran, Martin Sahlén, Debanjan Sarkar, Suman Majumdar","doi":"arxiv-2409.05187","DOIUrl":"https://doi.org/arxiv-2409.05187","url":null,"abstract":"The neutral hydrogen (HI) power spectrum, measured from intensity\u0000fluctuations in the 21-cm background, offers insights into the large-scale\u0000structures (LSS) of our Universe in the post-reionization era (redshift $z<6$).\u0000A significant amount of HI is expected to reside in low- and\u0000intermediate-density environments, but the power spectrum mainly captures\u0000information from high-density regions. To more fully extract the information\u0000contained in the HI field, we investigate the use of a marked power spectrum\u0000statistic. Here, the power spectrum is effectively re-weighted using a\u0000non-linear mark function which depends on the smoothed local density, such that\u0000low- or high-density regions are up- or down-weighted. This approach may also\u0000capture information on some higher-order statistical moments of the field. We\u0000model the HI distribution using semi-numerical simulations and for the first\u0000time study the marked HI power spectrum, across $1 leq z leq 5$. Our analysis\u0000indicates that there is considerable evolution of the HI field during the\u0000post-reionization era. Over a wide range of length scales (comoving wave\u0000numbers $0.05leq k leq 1.0$ Mpc$^{-1}$) we expectedly find that the HI\u0000evolves slowly at early times, but more rapidly at late times. This evolution\u0000is not well-captured by the power spectrum of the standard (unmarked) HI field.\u0000We also study how the evolution of the HI field depends on the chosen smoothing\u0000scale for the mark, and how this affects the marked power spectrum. We conclude\u0000that the information about the HI content at low and intermediate densities is\u0000important for a correct and consistent analysis of HI content and evolution\u0000based on the 21-cm background. The marked power spectrum can thus provide a\u0000less biased statistic for parameter constraints than the normal power spectrum.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"139 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192591","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}
Yan-Hong Yao, Jian-Qi Liu, Zhi-Qi Huang, Jun-Chao Wang, Yan Su
In this paper, we introduced the Unified Three-Form Dark Sector (UTFDS) model, a unified dark sector model that combines dark energy and dark matter through a three-form field. In this framework, the potential of the three-form field acts as dark matter, while the kinetic term represents dark energy. The interaction between dark matter and dark energy is driven by the energy exchange between these two terms. Given the dynamical equations of UTFDS, we provide an autonomous system of evolution equations for UTFDS and perform a stability analysis of its fixed points. The result aligns with our expectations for a unified dark sector. Furthermore, we discover that the dual Lagrangian of the UTFDS Lagrangian is equivalent to a Dirac-Born-Infeld (DBI) Lagrangian. By fixing the parameter $kappa X_0$ to 250, 500, 750, we refer to the resulting models as the $overline{rm UTFDS}$ model with $kappa X_0$=250, 500, 750, respectively. We then place constraints on these three $overline{rm UTFDS}$ models and the $Lambda$CDM model in light of the Planck 2018 Cosmic Microwave Background (CMB) anisotropies, Redshift Space Distortions (RSD) observations, Baryon Acoustic Oscillation (BAO) measurements, and the $S_8$ prior chosen according to the KiDS1000 Weak gravitational Lensing (WL) measuement. We find that the $overline{rm UTFDS}$ model with $kappa X_0$=500 is the only one among the four models where both $sigma_8$ and $S_8$ tensions, between CMB and RSD+BAO+WL datasets, are below 2.0$sigma$. Furthermore, the tensions are relieved without exacerbating the $H_0$ tension. Although both the CMB and RSD+BAO+WL datasets provide definite/positive evidence favoring $Lambda$CDM over the $overline{rm UTFDS}$ model with $kappa X_0$=500, the evidence is not strong enough to rule out further study of this model.
{"title":"A new unified dark sector model and its implications on the $σ_8$ and $S_8$ tensions","authors":"Yan-Hong Yao, Jian-Qi Liu, Zhi-Qi Huang, Jun-Chao Wang, Yan Su","doi":"arxiv-2409.04678","DOIUrl":"https://doi.org/arxiv-2409.04678","url":null,"abstract":"In this paper, we introduced the Unified Three-Form Dark Sector (UTFDS)\u0000model, a unified dark sector model that combines dark energy and dark matter\u0000through a three-form field. In this framework, the potential of the three-form\u0000field acts as dark matter, while the kinetic term represents dark energy. The\u0000interaction between dark matter and dark energy is driven by the energy\u0000exchange between these two terms. Given the dynamical equations of UTFDS, we\u0000provide an autonomous system of evolution equations for UTFDS and perform a\u0000stability analysis of its fixed points. The result aligns with our expectations\u0000for a unified dark sector. Furthermore, we discover that the dual Lagrangian of\u0000the UTFDS Lagrangian is equivalent to a Dirac-Born-Infeld (DBI) Lagrangian. By\u0000fixing the parameter $kappa X_0$ to 250, 500, 750, we refer to the resulting\u0000models as the $overline{rm UTFDS}$ model with $kappa X_0$=250, 500, 750,\u0000respectively. We then place constraints on these three $overline{rm UTFDS}$\u0000models and the $Lambda$CDM model in light of the Planck 2018 Cosmic Microwave\u0000Background (CMB) anisotropies, Redshift Space Distortions (RSD) observations,\u0000Baryon Acoustic Oscillation (BAO) measurements, and the $S_8$ prior chosen\u0000according to the KiDS1000 Weak gravitational Lensing (WL) measuement. We find\u0000that the $overline{rm UTFDS}$ model with $kappa X_0$=500 is the only one\u0000among the four models where both $sigma_8$ and $S_8$ tensions, between CMB and\u0000RSD+BAO+WL datasets, are below 2.0$sigma$. Furthermore, the tensions are\u0000relieved without exacerbating the $H_0$ tension. Although both the CMB and\u0000RSD+BAO+WL datasets provide definite/positive evidence favoring $Lambda$CDM\u0000over the $overline{rm UTFDS}$ model with $kappa X_0$=500, the evidence is\u0000not strong enough to rule out further study of this model.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"72 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192596","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}
Oliver NewtonAstrophysics Research Institute, LJMU, Liverpool, UKCenter for Theoretical Physics, Polish Academy of Sciences, Warsaw, Poland, Jonathan J. DaviesAstrophysics Research Institute, LJMU, Liverpool, UKUniversity College London, UK, Joel PfefferSwinburne University, Australia, Robert A. CrainAstrophysics Research Institute, LJMU, Liverpool, UK, J. M. Diederik KruijssenTechnical University of Munich, GermanyCosmic Origins Of Life Research DAO, Germany, Andrew PontzenUniversity College London, UK, Nate BastianDonostia International Physics Center, Guipuzkoa, SpainBasque Foundation for Science, Bilbao, Spain
Globular clusters (GCs) are sensitive tracers of galaxy assembly histories but interpreting the information they encode is challenging because mergers are thought to promote both the formation and disruption of GCs. We use simulations with controlled merger histories to examine the influence of merger mass ratio on the GC population of a present-day $L^ast$ galaxy, using the genetic modification technique to adjust the initial conditions of a galaxy that experiences major mergers at $z = 1.7$ and $z = 0.77$ (ORGANIC case), so the later merger has twice its original mass ratio (ENHANCED case), or is prevented from occurring (SUPPRESSED case). We evolve the three realizations with E-MOSAICS, which couples sub-grid star cluster formation and evolution models to the EAGLE galaxy formation model. Relative to the ORGANIC case, the mass of surviving GCs is elevated (reduced) in the ENHANCED (SUPPRESSED) case, indicating that major mergers promote a net boost to the GC population. The boost is clearly quantified by the GC specific mass, $S_{rm M}$, because it is sensitive to the number of the most massive GCs, whose long characteristic disruption timescales enable them to survive their hostile natal environments. In contrast, the specific frequency, $T_{rm N}$, is insensitive to assembly history because it primarily traces low-mass GCs that tend to be disrupted soon after their formation. The promotion of GC formation and disruption by major mergers imprints a lasting and potentially observable signature: an elevated mass fraction of field stars in the galaxy's stellar halo that were born in star clusters.
{"title":"The formation and disruption of globular cluster populations in simulations of present-day $L^ast$ galaxies with controlled assembly histories","authors":"Oliver NewtonAstrophysics Research Institute, LJMU, Liverpool, UKCenter for Theoretical Physics, Polish Academy of Sciences, Warsaw, Poland, Jonathan J. DaviesAstrophysics Research Institute, LJMU, Liverpool, UKUniversity College London, UK, Joel PfefferSwinburne University, Australia, Robert A. CrainAstrophysics Research Institute, LJMU, Liverpool, UK, J. M. Diederik KruijssenTechnical University of Munich, GermanyCosmic Origins Of Life Research DAO, Germany, Andrew PontzenUniversity College London, UK, Nate BastianDonostia International Physics Center, Guipuzkoa, SpainBasque Foundation for Science, Bilbao, Spain","doi":"arxiv-2409.04516","DOIUrl":"https://doi.org/arxiv-2409.04516","url":null,"abstract":"Globular clusters (GCs) are sensitive tracers of galaxy assembly histories\u0000but interpreting the information they encode is challenging because mergers are\u0000thought to promote both the formation and disruption of GCs. We use simulations\u0000with controlled merger histories to examine the influence of merger mass ratio\u0000on the GC population of a present-day $L^ast$ galaxy, using the genetic\u0000modification technique to adjust the initial conditions of a galaxy that\u0000experiences major mergers at $z = 1.7$ and $z = 0.77$ (ORGANIC case), so the\u0000later merger has twice its original mass ratio (ENHANCED case), or is prevented\u0000from occurring (SUPPRESSED case). We evolve the three realizations with\u0000E-MOSAICS, which couples sub-grid star cluster formation and evolution models\u0000to the EAGLE galaxy formation model. Relative to the ORGANIC case, the mass of\u0000surviving GCs is elevated (reduced) in the ENHANCED (SUPPRESSED) case,\u0000indicating that major mergers promote a net boost to the GC population. The\u0000boost is clearly quantified by the GC specific mass, $S_{rm M}$, because it is\u0000sensitive to the number of the most massive GCs, whose long characteristic\u0000disruption timescales enable them to survive their hostile natal environments.\u0000In contrast, the specific frequency, $T_{rm N}$, is insensitive to assembly\u0000history because it primarily traces low-mass GCs that tend to be disrupted soon\u0000after their formation. The promotion of GC formation and disruption by major\u0000mergers imprints a lasting and potentially observable signature: an elevated\u0000mass fraction of field stars in the galaxy's stellar halo that were born in\u0000star clusters.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"26 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192603","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}
M. Amenouche, M. Smith, P. Rosnet, M. Rigault, M. Aubert, C. Barjou-Delayre, U. Burgaz, B. Carreres, G. Dimitriadis, F. Feinstein, L. Galbany, M. Ginolin, A. Goobar, L. Harvey, Y. -L. Kim, K. Maguire, T. E. Müller-Bravo, J. Nordin, P. Nugent, B. Racine, D. Rosselli, N. Regnault, J. Sollerman, J. H. Terwel, A. Townsend, S. L. Groom, S. R. Kulkarni, M. Kasliwal, R. R. Laher, J. Purdum
Type Ia supernovae (SNe Ia) constitute an historical probe to derive cosmological parameters through the fit of the Hubble-Lema^itre diagram, i.e. SN Ia distance modulus versus their redshift. In the era of precision cosmology, realistic simulation of SNe Ia for any survey entering in an Hubble-Lema^itre diagram is a key tool to address observational systematics, like Malmquist bias. As the distance modulus of SNe Ia is derived from the fit of their light-curves, a robust simulation framework is required. In this paper, we present the performances of the simulation framework skysurvey to reproduce the the Zwicky Transient Facility (ZTF) SN Ia DR2 covering the first phase of ZTF running from April 2018 up to December 2020. The ZTF SN Ia DR2 sample correspond to almost 3000 classified SNe Ia of cosmological quality. First, a targeted simulation of the ZTF SN Ia DR2 was carried on to check the validity of the framework after some fine tuning of the observing conditions and instrument performance. Then, a realistic simulation has been run using observing ZTF logs and ZTF SN Ia DR2 selection criteria on simulated light-curves to demonstrate the ability of the simulation framework to match the ZTF SN Ia DR2 sample. Furthermore a redshift dependency of SALT2 light-curve parameters (stretch and colour) was conducted to deduce a volume limited sample, i.e. an unbiased SNe Ia sample, characterized with $z_{lim} leq 0.06$. This volume limited sample of about 1000 SNe Ia is unique to carry on new analysis on standardization procedure with a precision never reached (those analysis are presented in companion papers).
Ia 型超新星（SNe Ia）是通过拟合哈勃-勒马（Hubble-Lema/^itre）图（即 Ia 型超新星距离模数与其红移的关系）来推导宇宙学参数的一个历史性探测器。在精确宇宙学时代，对进入哈勃-勒马^itre图的任何巡天观测的SNe Ia进行现实模拟，是解决观测系统性问题（如Malmquist偏差）的关键工具。由于SNe Ia的距离模量是通过拟合其光曲线得到的，因此需要一个强大的模拟框架。在本文中，我们介绍了模拟框架skysurvey的性能，以重建兹威基瞬变设施（ZTF）SN Ia DR2，涵盖ZTF从2018年4月到2020年12月的第一阶段。首先，对ZTF SN Ia DR2进行了有针对性的模拟，以检查在对观测条件和仪器性能进行微调之后框架的有效性。然后，在模拟光曲线上使用观测ZTF日志和ZTF SN Ia DR2选择标准进行了实际模拟，以证明模拟框架匹配ZTF SN Ia DR2样本的能力。此外，还对SALT2光曲线参数（拉伸和颜色）的红移依赖性进行了研究，以推导出一个体积有限的样本，即一个无偏的SNe Ia样本，其特征为$z_{lim}leq 0.06$。这个由大约1000个SNe Ia组成的体积受限样本是独一无二的，可以在标准化程序上进行新的分析，其精确度从未达到过（这些分析将在相关论文中介绍）。
{"title":"ZTF SN Ia DR2: Simulations and volume limited sample","authors":"M. Amenouche, M. Smith, P. Rosnet, M. Rigault, M. Aubert, C. Barjou-Delayre, U. Burgaz, B. Carreres, G. Dimitriadis, F. Feinstein, L. Galbany, M. Ginolin, A. Goobar, L. Harvey, Y. -L. Kim, K. Maguire, T. E. Müller-Bravo, J. Nordin, P. Nugent, B. Racine, D. Rosselli, N. Regnault, J. Sollerman, J. H. Terwel, A. Townsend, S. L. Groom, S. R. Kulkarni, M. Kasliwal, R. R. Laher, J. Purdum","doi":"arxiv-2409.04650","DOIUrl":"https://doi.org/arxiv-2409.04650","url":null,"abstract":"Type Ia supernovae (SNe Ia) constitute an historical probe to derive\u0000cosmological parameters through the fit of the Hubble-Lema^itre diagram, i.e.\u0000SN Ia distance modulus versus their redshift. In the era of precision\u0000cosmology, realistic simulation of SNe Ia for any survey entering in an\u0000Hubble-Lema^itre diagram is a key tool to address observational systematics,\u0000like Malmquist bias. As the distance modulus of SNe Ia is derived from the fit\u0000of their light-curves, a robust simulation framework is required. In this\u0000paper, we present the performances of the simulation framework skysurvey to\u0000reproduce the the Zwicky Transient Facility (ZTF) SN Ia DR2 covering the first\u0000phase of ZTF running from April 2018 up to December 2020. The ZTF SN Ia DR2\u0000sample correspond to almost 3000 classified SNe Ia of cosmological quality.\u0000First, a targeted simulation of the ZTF SN Ia DR2 was carried on to check the\u0000validity of the framework after some fine tuning of the observing conditions\u0000and instrument performance. Then, a realistic simulation has been run using\u0000observing ZTF logs and ZTF SN Ia DR2 selection criteria on simulated\u0000light-curves to demonstrate the ability of the simulation framework to match\u0000the ZTF SN Ia DR2 sample. Furthermore a redshift dependency of SALT2\u0000light-curve parameters (stretch and colour) was conducted to deduce a volume\u0000limited sample, i.e. an unbiased SNe Ia sample, characterized with $z_{lim}\u0000leq 0.06$. This volume limited sample of about 1000 SNe Ia is unique to carry\u0000on new analysis on standardization procedure with a precision never reached\u0000(those analysis are presented in companion papers).","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192573","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}
Tiger Yu-Yang Hsiao, Michael W. Topping, Dan Coe, John Chisholm, Danielle A. Berg, Abdurro'uf, Javier Álvarez-Márquez, Roberto Maiolino, Pratika Dayal, Lukas J. Furtak
Investigating the metal enrichment in the early universe helps us constrain theories about the first stars and study the ages of galaxies. The lensed galaxy MACS0647$-$JD at $z=10.17$ is the brightest galaxy known at $z > 10$. Previous work analyzing JWST NIRSpec and MIRI data yielded a direct metallicity $rm{12+log(O/H)}=7.79pm0.09$ ($sim$ 0.13 $Z_odot$) and electron density $rm{log}(n_e / rm{cm^{-3}}) = 2.9 pm 0.5$, the most distant such measurements to date. Here we estimate the direct C/O abundance for the first time at $z > 10$, finding a sub-solar ${rm log(C/O)}=-0.44^{+0.06}_{-0.07}$. This is higher than other $z>6$ galaxies with direct C/O measurements, likely due to higher metallicity. It is also slightly higher than galaxies in the local universe with similar metallicity. This may suggest a very efficient and rapid burst of star formation, a low effective oxygen abundance yield, or the presence of unusual stellar populations including supermassive stars. Alternatively, the strong CIII]${rm {lambda}{lambda}}$1907,1909 emission ($14pm 3,{r{A}}$ rest-frame EW) may originate from just one of the two component star clusters JDB ($r sim 20$ pc). Future NIRSpec IFU spectroscopic observations of MACS0647$-$JD will be promising for disentangling C/O in the two components to constrain the chemistry of individual star clusters just 460 Myr after the Big Bang.
{"title":"First direct carbon abundance measured at $z>10$ in the lensed galaxy MACS0647$-$JD","authors":"Tiger Yu-Yang Hsiao, Michael W. Topping, Dan Coe, John Chisholm, Danielle A. Berg, Abdurro'uf, Javier Álvarez-Márquez, Roberto Maiolino, Pratika Dayal, Lukas J. Furtak","doi":"arxiv-2409.04625","DOIUrl":"https://doi.org/arxiv-2409.04625","url":null,"abstract":"Investigating the metal enrichment in the early universe helps us constrain\u0000theories about the first stars and study the ages of galaxies. The lensed\u0000galaxy MACS0647$-$JD at $z=10.17$ is the brightest galaxy known at $z > 10$.\u0000Previous work analyzing JWST NIRSpec and MIRI data yielded a direct metallicity\u0000$rm{12+log(O/H)}=7.79pm0.09$ ($sim$ 0.13 $Z_odot$) and electron density\u0000$rm{log}(n_e / rm{cm^{-3}}) = 2.9 pm 0.5$, the most distant such\u0000measurements to date. Here we estimate the direct C/O abundance for the first\u0000time at $z > 10$, finding a sub-solar ${rm log(C/O)}=-0.44^{+0.06}_{-0.07}$.\u0000This is higher than other $z>6$ galaxies with direct C/O measurements, likely\u0000due to higher metallicity. It is also slightly higher than galaxies in the\u0000local universe with similar metallicity. This may suggest a very efficient and\u0000rapid burst of star formation, a low effective oxygen abundance yield, or the\u0000presence of unusual stellar populations including supermassive stars.\u0000Alternatively, the strong CIII]${rm {lambda}{lambda}}$1907,1909 emission\u0000($14pm 3,{r{A}}$ rest-frame EW) may originate from just one of the two\u0000component star clusters JDB ($r sim 20$ pc). Future NIRSpec IFU spectroscopic\u0000observations of MACS0647$-$JD will be promising for disentangling C/O in the\u0000two components to constrain the chemistry of individual star clusters just 460\u0000Myr after the Big Bang.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"24 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192598","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 wealth of high-quality observational data from the epoch of reionization that will become available in the next decade motivates further development of modeling techniques for their interpretation. Among the key challenges in modeling reionization are (1) its multi-scale nature, (2) the computational demands of solving the radiative transfer (RT) equation, and (3) the large size of reionization's parameter space. In this paper, we present and validate a new RT code designed to confront these challenges. FlexRT (Flexible Radiative Transfer) combines adaptive ray tracing with a highly flexible treatment of the intergalactic ionizing opacity. This gives the user control over how the intergalactic medium (IGM) is modeled, and provides a way to reduce the computational cost of a FlexRT simulation by orders of magnitude while still accounting for small-scale IGM physics. Alternatively, the user may increase the angular and spatial resolution of the algorithm to run a more traditional reionization simulation. FlexRT has already been used in several contexts, including simulations of the Lyman-$alpha$ forest of high-$z$ quasars, the redshifted 21cm signal from reionization, as well as in higher resolution reionization simulations in smaller volumes. In this work, we motivate and describe the code, and validate it against a set of standard test problems from the Cosmological Radiative Transfer Comparison Project. We find that FlexRT is in broad agreement with a number of existing RT codes in all of these tests. Lastly, we compare FlexRT to an existing adaptive ray tracing code to validate FlexRT in a cosmological reionization simulation.
{"title":"FlexRT -- A fast and flexible cosmological radiative transfer code for reionization studies I: Code validation","authors":"Christopher Cain, Anson D'Aloisio","doi":"arxiv-2409.04521","DOIUrl":"https://doi.org/arxiv-2409.04521","url":null,"abstract":"The wealth of high-quality observational data from the epoch of reionization\u0000that will become available in the next decade motivates further development of\u0000modeling techniques for their interpretation. Among the key challenges in\u0000modeling reionization are (1) its multi-scale nature, (2) the computational\u0000demands of solving the radiative transfer (RT) equation, and (3) the large size\u0000of reionization's parameter space. In this paper, we present and validate a new\u0000RT code designed to confront these challenges. FlexRT (Flexible Radiative\u0000Transfer) combines adaptive ray tracing with a highly flexible treatment of the\u0000intergalactic ionizing opacity. This gives the user control over how the\u0000intergalactic medium (IGM) is modeled, and provides a way to reduce the\u0000computational cost of a FlexRT simulation by orders of magnitude while still\u0000accounting for small-scale IGM physics. Alternatively, the user may increase\u0000the angular and spatial resolution of the algorithm to run a more traditional\u0000reionization simulation. FlexRT has already been used in several contexts,\u0000including simulations of the Lyman-$alpha$ forest of high-$z$ quasars, the\u0000redshifted 21cm signal from reionization, as well as in higher resolution\u0000reionization simulations in smaller volumes. In this work, we motivate and\u0000describe the code, and validate it against a set of standard test problems from\u0000the Cosmological Radiative Transfer Comparison Project. We find that FlexRT is\u0000in broad agreement with a number of existing RT codes in all of these tests.\u0000Lastly, we compare FlexRT to an existing adaptive ray tracing code to validate\u0000FlexRT in a cosmological reionization simulation.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"75 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192595","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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