Forward models of the galaxy density field enable simulation based inference as well as field level inference of galaxy clustering. However, these analysis techniques require forward models that are both computationally fast and robust to modeling uncertainties in the relation between galaxies and matter. Both requirements can be addressed with the Effective Field Theory of Large Scale Structure. Here, we focus on the physical and numerical convergence of the LEFTfield model. Based on the perturbative nature of the forward model, we derive an analytic understanding of the leading numerical errors, and we compare our estimates to high-resolution and N-body references. This allows us to derive a set of best-practice recommendations for the numerical accuracy parameters, which are completely specified by the desired order of the perturbative solution and the cut-off scale. We verify these recommendations by an extended set of parameter recovery tests from fully nonlinear mock data and find very consistent results. A single evaluation of the forward model takes seconds, making cosmological analyses of galaxy clustering data based on forward models computationally feasible.
星系密度场的前向模型可以进行基于模拟的推断以及星系聚类的场级推断。然而，这些分析技术要求前向模型既要计算速度快，又要对星系与物质之间关系的建模不确定性具有鲁棒性。大尺度结构有效场理论（Effective Field Theory of Large ScaleStructure）可以满足这两个要求。在这里，我们重点讨论了LEFT场模型的物理和数值收敛性。基于前向模型的微扰性质，我们对主要的数值误差有了分析性的理解，并将我们的估计与高分辨率和N体参考进行了比较。这样，我们就得出了一组数值精度参数的最佳实践建议，这些参数完全由所需的扰动解阶数和截止尺度所规定。我们通过对完全非线性模拟数据的参数恢复测试，验证了这些建议，并发现了非常一致的结果。对前导模型的一次评估只需要几秒钟，这使得基于前导模型的星系聚类数据宇宙学分析在计算上是可行的。
{"title":"Fast, Accurate and Perturbative Forward Modeling of Galaxy Clustering Part I: Galaxies in the Restframe","authors":"Julia Stadler, Fabian Schmidt, Martin Reinecke","doi":"arxiv-2409.10937","DOIUrl":"https://doi.org/arxiv-2409.10937","url":null,"abstract":"Forward models of the galaxy density field enable simulation based inference\u0000as well as field level inference of galaxy clustering. However, these analysis\u0000techniques require forward models that are both computationally fast and robust\u0000to modeling uncertainties in the relation between galaxies and matter. Both\u0000requirements can be addressed with the Effective Field Theory of Large Scale\u0000Structure. Here, we focus on the physical and numerical convergence of the\u0000LEFTfield model. Based on the perturbative nature of the forward model, we\u0000derive an analytic understanding of the leading numerical errors, and we\u0000compare our estimates to high-resolution and N-body references. This allows us\u0000to derive a set of best-practice recommendations for the numerical accuracy\u0000parameters, which are completely specified by the desired order of the\u0000perturbative solution and the cut-off scale. We verify these recommendations by\u0000an extended set of parameter recovery tests from fully nonlinear mock data and\u0000find very consistent results. A single evaluation of the forward model takes\u0000seconds, making cosmological analyses of galaxy clustering data based on\u0000forward models computationally feasible.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257635","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}
Yongda Zhu, Marcia J. Rieke, Zhiyuan Ji, Charlotte Simmonds, Fengwu Sun, Yang Sun, Stacey Alberts, Rachana Bhatawdekar, Andrew J. Bunker, Phillip A. Cargile, Stefano Carniani, Anna de Graaff, Kevin Hainline, Jakob M. Helton, Gareth C. Jones, Jianwei Lyu, George H. Rieke, Pierluigi Rinaldi, Brant Robertson, Jan Scholtz, Hannah Übler, Christina C. Williams, Christopher N. A. Willmer
For the first time, we systematically search for galaxies with extended emission line and potential outflows features using medium-band images in the GOODS-S field by comparing the morphology in medium-band images to adjacent continuum and UV bands. We look for galaxies that have a maximum extent 50% larger, an excess area 30% greater, or an axis ratio difference of more than 0.3 in the medium band compared to the reference bands. After visual inspection, we find 326 candidate galaxies at $1 < z < 6$, with a peak in the population near cosmic noon, benefiting from the good coverage of the medium-band filters. By examining their SEDs, we find that the candidate galaxies are at least 20% more bursty in their star-forming activity and have 60% more young stellar populations compared to a control sample selected based on the continuum band flux. Additionally, these candidates exhibit a significantly higher production rate of ionizing photons. We further find that candidates hosting known AGN produce extended emission that is more anisotropic compared to non-AGN candidates. A few of our candidates have been spectroscopically confirmed to have prominent outflow signatures through NIRSpec observations, showcasing the robustness of the photometric selection. Future spectroscopic follow-up will better help verify and characterize the kinematics and chemical properties of these systems.
{"title":"A Systematic Search for Galaxies with Extended Emission Line and Potential Outflows in JADES Medium-Band Images","authors":"Yongda Zhu, Marcia J. Rieke, Zhiyuan Ji, Charlotte Simmonds, Fengwu Sun, Yang Sun, Stacey Alberts, Rachana Bhatawdekar, Andrew J. Bunker, Phillip A. Cargile, Stefano Carniani, Anna de Graaff, Kevin Hainline, Jakob M. Helton, Gareth C. Jones, Jianwei Lyu, George H. Rieke, Pierluigi Rinaldi, Brant Robertson, Jan Scholtz, Hannah Übler, Christina C. Williams, Christopher N. A. Willmer","doi":"arxiv-2409.11464","DOIUrl":"https://doi.org/arxiv-2409.11464","url":null,"abstract":"For the first time, we systematically search for galaxies with extended\u0000emission line and potential outflows features using medium-band images in the\u0000GOODS-S field by comparing the morphology in medium-band images to adjacent\u0000continuum and UV bands. We look for galaxies that have a maximum extent 50%\u0000larger, an excess area 30% greater, or an axis ratio difference of more than\u00000.3 in the medium band compared to the reference bands. After visual\u0000inspection, we find 326 candidate galaxies at $1 < z < 6$, with a peak in the\u0000population near cosmic noon, benefiting from the good coverage of the\u0000medium-band filters. By examining their SEDs, we find that the candidate\u0000galaxies are at least 20% more bursty in their star-forming activity and have\u000060% more young stellar populations compared to a control sample selected based\u0000on the continuum band flux. Additionally, these candidates exhibit a\u0000significantly higher production rate of ionizing photons. We further find that\u0000candidates hosting known AGN produce extended emission that is more anisotropic\u0000compared to non-AGN candidates. A few of our candidates have been\u0000spectroscopically confirmed to have prominent outflow signatures through\u0000NIRSpec observations, showcasing the robustness of the photometric selection.\u0000Future spectroscopic follow-up will better help verify and characterize the\u0000kinematics and chemical properties of these systems.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"52 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257632","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}
Andrey Prokopenko, Daniel Arndt, Damien Lebrun-Grandié, Bruno Turcksin, Nicholas Frontiere, J. D. Emberson, Michael Buehlmann
ArborX is a performance portable geometric search library developed as part of the Exascale Computing Project (ECP). In this paper, we explore a collaboration between ArborX and a cosmological simulation code HACC. Large cosmological simulations on exascale platforms encounter a bottleneck due to the in-situ analysis requirements of halo finding, a problem of identifying dense clusters of dark matter (halos). This problem is solved by using a density-based DBSCAN clustering algorithm. With each MPI rank handling hundreds of millions of particles, it is imperative for the DBSCAN implementation to be efficient. In addition, the requirement to support exascale supercomputers from different vendors necessitates performance portability of the algorithm. We describe how this challenge problem guided ArborX development, and enhanced the performance and the scope of the library. We explore the improvements in the basic algorithms for the underlying search index to improve the performance, and describe several implementations of DBSCAN in ArborX. Further, we report the history of the changes in ArborX and their effect on the time to solve a representative benchmark problem, as well as demonstrate the real world impact on production end-to-end cosmology simulations.
{"title":"Advances in ArborX to support exascale applications","authors":"Andrey Prokopenko, Daniel Arndt, Damien Lebrun-Grandié, Bruno Turcksin, Nicholas Frontiere, J. D. Emberson, Michael Buehlmann","doi":"arxiv-2409.10743","DOIUrl":"https://doi.org/arxiv-2409.10743","url":null,"abstract":"ArborX is a performance portable geometric search library developed as part\u0000of the Exascale Computing Project (ECP). In this paper, we explore a\u0000collaboration between ArborX and a cosmological simulation code HACC. Large\u0000cosmological simulations on exascale platforms encounter a bottleneck due to\u0000the in-situ analysis requirements of halo finding, a problem of identifying\u0000dense clusters of dark matter (halos). This problem is solved by using a\u0000density-based DBSCAN clustering algorithm. With each MPI rank handling hundreds\u0000of millions of particles, it is imperative for the DBSCAN implementation to be\u0000efficient. In addition, the requirement to support exascale supercomputers from\u0000different vendors necessitates performance portability of the algorithm. We\u0000describe how this challenge problem guided ArborX development, and enhanced the\u0000performance and the scope of the library. We explore the improvements in the\u0000basic algorithms for the underlying search index to improve the performance,\u0000and describe several implementations of DBSCAN in ArborX. Further, we report\u0000the history of the changes in ArborX and their effect on the time to solve a\u0000representative benchmark problem, as well as demonstrate the real world impact\u0000on production end-to-end cosmology simulations.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"315 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257642","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. Koussour, A. Altaibayeva, S. Bekov, F. Holmurodov, S. Muminov, J. Rayimbaev
This study explores the extension of teleparallel gravity within the framework of general relativity, introducing an algebraic function $f(T)$ dependent on the torsion scalar $T$. Motivated by the teleparallel formulation, we investigate cosmological implications, employing the simplest parametrization of the dark energy equation of state. Our chosen $f(T)$ function, $f(T)=alpha(-T)^n$, undergoes stringent constraints using recent observational data ($H(z)$, SNeIa, BAO, and CMB). The model aligns well with cosmic dynamics, exhibiting quintessence behavior. The evolution of the deceleration parameter, the behavior of dark energy components, and the $Om(z)$ diagnostic further reveal intriguing cosmological phenomena, emphasizing the model's compatibility with quintessence scenarios.
{"title":"Exploring cosmological evolution and constraints in $f(T)$ teleparallel gravity","authors":"M. Koussour, A. Altaibayeva, S. Bekov, F. Holmurodov, S. Muminov, J. Rayimbaev","doi":"arxiv-2409.10757","DOIUrl":"https://doi.org/arxiv-2409.10757","url":null,"abstract":"This study explores the extension of teleparallel gravity within the\u0000framework of general relativity, introducing an algebraic function $f(T)$\u0000dependent on the torsion scalar $T$. Motivated by the teleparallel formulation,\u0000we investigate cosmological implications, employing the simplest\u0000parametrization of the dark energy equation of state. Our chosen $f(T)$\u0000function, $f(T)=alpha(-T)^n$, undergoes stringent constraints using recent\u0000observational data ($H(z)$, SNeIa, BAO, and CMB). The model aligns well with\u0000cosmic dynamics, exhibiting quintessence behavior. The evolution of the\u0000deceleration parameter, the behavior of dark energy components, and the $Om(z)$\u0000diagnostic further reveal intriguing cosmological phenomena, emphasizing the\u0000model's compatibility with quintessence scenarios.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"20 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257636","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}
Ana Contreras-Santos, Fernando Buitrago, Alexander Knebe, Elena Rasia, Frazer R. Pearce, Weiguang Cui, Chris Power, Jordan Winstanley
The observation of a massive galaxy with an extremely low dark matter content (i.e. NGC 1277) has posed questions about how such objects form and evolve in a hierarchical universe. We here report on the finding of several massive, dark matter-deficient galaxies in a set of 324 galaxy clusters theoretically modelled by means of full-physics hydrodynamical simulations. We first focus on two example galaxies selected amongst the most massive and dark matter-deficient ones. By tracing the evolution of these galaxies, we find that their lack of dark matter is a result of multiple pericentre passages. While orbiting their host halo, tidal interactions gradually strip away dark matter while preserving the stellar component. A statistical analysis of all massive satellite galaxies in the simulated clusters shows that the stellar-to-total mass ratio today is strongly influenced by the number of orbits and the distance at pericentres. Galaxies with more orbits and closer pericentres are more dark matter-deficient. Additionally, we find that massive, dark matter-deficient galaxies at the present day are either the remnants of very massive galaxies at infall or former central galaxies of infalling groups. We conclude that such massive yet dark matter-deficient galaxies exist and are natural by-products of typical cluster galaxy evolution, with no specific requirement for an exotic formation scenario.
对暗物质含量极低的大质量星系（即 NGC 1277）的观测提出了关于这类天体如何在层次宇宙中形成和演化的问题。我们在这里报告在一组通过全物理流体力学模拟进行理论模拟的 324 个星系团中发现的几个大质量暗物质缺乏星系。我们首先从质量最大、暗物质最缺乏的星系中挑选出两个星系作为研究对象。通过追踪这些星系的演化过程，我们发现它们的暗物质缺乏是由多个圆心通道造成的。在环绕宿主光环的过程中，潮汐相互作用逐渐剥离了暗物质，同时保留了恒星成分。对模拟星团中所有大质量卫星星系的统计分析显示，恒星质量与总质量之比在很大程度上受轨道数量和圆心距离的影响。轨道数量越多、中心距离越近的星系，暗物质缺失程度越高。此外，我们还发现，目前的大质量暗物质缺乏星系要么是正在衰变的超大质量星系的残余，要么是正在衰变的星系团的前中心星系。我们的结论是，这种大质量但暗物质缺乏的星系是存在的，而且是典型的星团星系演化的自然副产品，不需要特殊的形成过程。
{"title":"The Three Hundred: The existence of massive dark matter-deficient satellite galaxies in cosmological simulations","authors":"Ana Contreras-Santos, Fernando Buitrago, Alexander Knebe, Elena Rasia, Frazer R. Pearce, Weiguang Cui, Chris Power, Jordan Winstanley","doi":"arxiv-2409.10356","DOIUrl":"https://doi.org/arxiv-2409.10356","url":null,"abstract":"The observation of a massive galaxy with an extremely low dark matter content\u0000(i.e. NGC 1277) has posed questions about how such objects form and evolve in a\u0000hierarchical universe. We here report on the finding of several massive, dark\u0000matter-deficient galaxies in a set of 324 galaxy clusters theoretically\u0000modelled by means of full-physics hydrodynamical simulations. We first focus on\u0000two example galaxies selected amongst the most massive and dark\u0000matter-deficient ones. By tracing the evolution of these galaxies, we find that\u0000their lack of dark matter is a result of multiple pericentre passages. While\u0000orbiting their host halo, tidal interactions gradually strip away dark matter\u0000while preserving the stellar component. A statistical analysis of all massive\u0000satellite galaxies in the simulated clusters shows that the stellar-to-total\u0000mass ratio today is strongly influenced by the number of orbits and the\u0000distance at pericentres. Galaxies with more orbits and closer pericentres are\u0000more dark matter-deficient. Additionally, we find that massive, dark\u0000matter-deficient galaxies at the present day are either the remnants of very\u0000massive galaxies at infall or former central galaxies of infalling groups. We\u0000conclude that such massive yet dark matter-deficient galaxies exist and are\u0000natural by-products of typical cluster galaxy evolution, with no specific\u0000requirement for an exotic formation scenario.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"75 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257725","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 utilize the Sloan Digital Sky Survey (SDSS) extended Baryon Oscillation Spectroscopic Survey (eBOSS) and Baryon Oscillation Spectroscopic Survey (BOSS) catalogs with precise spectroscopic redshifts to estimate the kinematic redshift dipole caused by the proper motion of the Solar system. We find that the velocity extracted from the kinematic dipole is consistent with Cosmic Microwave Background inferred values. Although the small sky coverage and limited number density of the SDSS sources constrain us from obtaining precise and robust measurements, we leverage the redshift dipole method to estimate the kinematic dipole. The velocity measurements in this study are insensitive to intrinsic clustering, associated with the source count dipole. The kinematic dipole measured in this work and its consistency with CMB values do not guarantee isotropy at large scales. The anisotropy (excess dipole) measured with the NRAO VLA Sky Survey (NVSS) and the WISE Catalog (CatWISE) could be due to the intrinsic distribution of galaxies. The results in this work focus solely on the kinematic dipole term.
{"title":"An Independent Measure of the Kinematic Dipole from SDSS","authors":"Prabhakar TiwariGTIIT, Shantou, Dominik J. SchwarzBielefeld U., Gong-Bo ZhaoBeijing Observ., Ruth DurrerGeneva U., Dept. Theor. Phys., Martin KunzU. Geneva, Hamsa PadmanabhanU. Geneva","doi":"arxiv-2409.09946","DOIUrl":"https://doi.org/arxiv-2409.09946","url":null,"abstract":"We utilize the Sloan Digital Sky Survey (SDSS) extended Baryon Oscillation\u0000Spectroscopic Survey (eBOSS) and Baryon Oscillation Spectroscopic Survey (BOSS)\u0000catalogs with precise spectroscopic redshifts to estimate the kinematic\u0000redshift dipole caused by the proper motion of the Solar system. We find that\u0000the velocity extracted from the kinematic dipole is consistent with Cosmic\u0000Microwave Background inferred values. Although the small sky coverage and\u0000limited number density of the SDSS sources constrain us from obtaining precise\u0000and robust measurements, we leverage the redshift dipole method to estimate the\u0000kinematic dipole. The velocity measurements in this study are insensitive to\u0000intrinsic clustering, associated with the source count dipole. The kinematic\u0000dipole measured in this work and its consistency with CMB values do not\u0000guarantee isotropy at large scales. The anisotropy (excess dipole) measured\u0000with the NRAO VLA Sky Survey (NVSS) and the WISE Catalog (CatWISE) could be due\u0000to the intrinsic distribution of galaxies. The results in this work focus\u0000solely on the kinematic dipole term.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"17 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257641","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}
Measurements of the redshift drift -- the real time variation of the redshift of distance sources -- are expected in the next couple of decades using next generation facilities such as the ANDES spectrograph at the ELT and the SKAO survey. The unprecedented precision of such observations will demand precise theoretical and numerical modeling of the effect in the standard $Lambda$CDM cosmology. In this work, we use the Gadget4 $N$-body code to simulate the redshift drift and its fluctuations in $Lambda$CDM cosmologies, deriving the corresponding power spectra from a simulation with $1024^3$ particles in a $1textrm{Gpc},h^{-1}$ box. Our results provide an estimate for the distribution and amplitude of the fluctuations and the spectra, which match previous work in the literature using Einstein-Boltzmann solvers to within an order of magnitude. Our work provides a methodology for performing statistical analysis of the redshift drift effect and deriving its fluctuation power spectra from future large scale surveys.
{"title":"Redshift Drift fluctuations from N-body simulations","authors":"Pedro Bessa, Valerio Marra, Tiago Castro","doi":"arxiv-2409.09977","DOIUrl":"https://doi.org/arxiv-2409.09977","url":null,"abstract":"Measurements of the redshift drift -- the real time variation of the redshift\u0000of distance sources -- are expected in the next couple of decades using next\u0000generation facilities such as the ANDES spectrograph at the ELT and the SKAO\u0000survey. The unprecedented precision of such observations will demand precise\u0000theoretical and numerical modeling of the effect in the standard $Lambda$CDM\u0000cosmology. In this work, we use the Gadget4 $N$-body code to simulate the\u0000redshift drift and its fluctuations in $Lambda$CDM cosmologies, deriving the\u0000corresponding power spectra from a simulation with $1024^3$ particles in a\u0000$1textrm{Gpc},h^{-1}$ box. Our results provide an estimate for the\u0000distribution and amplitude of the fluctuations and the spectra, which match\u0000previous work in the literature using Einstein-Boltzmann solvers to within an\u0000order of magnitude. Our work provides a methodology for performing statistical\u0000analysis of the redshift drift effect and deriving its fluctuation power\u0000spectra from future large scale surveys.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"18 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257639","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}
Shawn Knabel, Tommaso Treu, Michele Cappellari, Anowar J. Shajib, Chih-Fan Chen, Vardha N. Bennert
We obtain spatially resolved kinematics with the Keck Cosmic Web Imager (KCWI) integral-field spectrograph for a sample of 14 massive (11 < log10 M* < 12) lensing early-type galaxies (ETGs) at redshifts z=0.15-0.35 from the Sloan Lens ACS (SLACS) survey. We integrate within the galaxy effective radius and examine the rotational and dispersion velocities, showing that 11/14 are quantitatively classified as slow rotators in comparison with local galaxy surveys. Of key interest is the ability of this data to enable the precision required for cosmological inference with lensing time delays on scales of 1-2% uncertainty. The dataset is unprecedented for galaxy-scale lens galaxies, in terms of signal-to-noise ratio, sampling, and calibration. We test sources of systematic error and identify primary contributions from choice of stellar template library and wavelength range of the spectral fit. Systematics are quantified at the spatial bin level, resulting in systematic error at 3% and positive spatial covariance of 2%. We examine the effects of integration of the kinematic maps within circular apertures of different sizes and compare with SDSS single-aperture velocity dispersions. The most recent velocity dispersion estimates from SDSS spectra are found to be biased by a factor of 5.3% with respect to KCWI data, and to underestimate uncertainties. We examine correlations between scaling relations and show the correlations to agree with previous SLACS analysis with no statistically significant disagreement. A follow-up paper will present Jeans modeling and discuss the context of these observations within broader studies of galaxy evolution and cosmology.
{"title":"Spatially Resolved Kinematics of SLACS Lens Galaxies. I: Data and Kinematic Classification","authors":"Shawn Knabel, Tommaso Treu, Michele Cappellari, Anowar J. Shajib, Chih-Fan Chen, Vardha N. Bennert","doi":"arxiv-2409.10631","DOIUrl":"https://doi.org/arxiv-2409.10631","url":null,"abstract":"We obtain spatially resolved kinematics with the Keck Cosmic Web Imager\u0000(KCWI) integral-field spectrograph for a sample of 14 massive (11 < log10 M* <\u000012) lensing early-type galaxies (ETGs) at redshifts z=0.15-0.35 from the Sloan\u0000Lens ACS (SLACS) survey. We integrate within the galaxy effective radius and\u0000examine the rotational and dispersion velocities, showing that 11/14 are\u0000quantitatively classified as slow rotators in comparison with local galaxy\u0000surveys. Of key interest is the ability of this data to enable the precision\u0000required for cosmological inference with lensing time delays on scales of 1-2%\u0000uncertainty. The dataset is unprecedented for galaxy-scale lens galaxies, in\u0000terms of signal-to-noise ratio, sampling, and calibration. We test sources of\u0000systematic error and identify primary contributions from choice of stellar\u0000template library and wavelength range of the spectral fit. Systematics are\u0000quantified at the spatial bin level, resulting in systematic error at 3% and\u0000positive spatial covariance of 2%. We examine the effects of integration of the\u0000kinematic maps within circular apertures of different sizes and compare with\u0000SDSS single-aperture velocity dispersions. The most recent velocity dispersion\u0000estimates from SDSS spectra are found to be biased by a factor of 5.3% with\u0000respect to KCWI data, and to underestimate uncertainties. We examine\u0000correlations between scaling relations and show the correlations to agree with\u0000previous SLACS analysis with no statistically significant disagreement. A\u0000follow-up paper will present Jeans modeling and discuss the context of these\u0000observations within broader studies of galaxy evolution and cosmology.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257674","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}
N. Raffuzzi, M. Lembo, S. Giardiello, M. Gerbino, M. Lattanzi, P. Natoli, L. Pagano
V-mode polarization of the cosmic microwave background is expected to be vanishingly small in the $Lambda$CDM model and, hence, usually ignored. Nonetheless, several astrophysical effects, as well as beyond standard model physics could produce it at a detectable level. A realistic half-wave plate - an optical element commonly used in CMB experiments to modulate the polarized signal - can provide sensitivity to V modes without significantly spoiling that to linear polarization. We assess this sensitivity for some new-generation CMB experiments, such as the LiteBIRD satellite, the ground-based Simons Observatory and a CMB-S4-like experiment. We forecast the efficiency of these experiments to constrain the phenomenology of certain classes of BSM models inducing mixing of linear polarization states and generation of V modes in the CMB. We find that new-generation experiments can improve current limits by 1-to-3 orders of magnitude, depending on the data combination. The inclusion of V-mode information dramatically boosts the sensitivity to these BSM models.
{"title":"Unveiling V Modes: Enhancing CMB Sensitivity to BSM Physics with a Non-Ideal Half-Wave Plate","authors":"N. Raffuzzi, M. Lembo, S. Giardiello, M. Gerbino, M. Lattanzi, P. Natoli, L. Pagano","doi":"arxiv-2409.10424","DOIUrl":"https://doi.org/arxiv-2409.10424","url":null,"abstract":"V-mode polarization of the cosmic microwave background is expected to be\u0000vanishingly small in the $Lambda$CDM model and, hence, usually ignored.\u0000Nonetheless, several astrophysical effects, as well as beyond standard model\u0000physics could produce it at a detectable level. A realistic half-wave plate -\u0000an optical element commonly used in CMB experiments to modulate the polarized\u0000signal - can provide sensitivity to V modes without significantly spoiling that\u0000to linear polarization. We assess this sensitivity for some new-generation CMB\u0000experiments, such as the LiteBIRD satellite, the ground-based Simons\u0000Observatory and a CMB-S4-like experiment. We forecast the efficiency of these\u0000experiments to constrain the phenomenology of certain classes of BSM models\u0000inducing mixing of linear polarization states and generation of V modes in the\u0000CMB. We find that new-generation experiments can improve current limits by\u00001-to-3 orders of magnitude, depending on the data combination. The inclusion of\u0000V-mode information dramatically boosts the sensitivity to these BSM models.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"52 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257640","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}
Sebastián E. Nuza, Matthias Hoeft, Ana Contreras-Santos, Alexander Knebe, Gustavo Yepes
Galaxy cluster mergers are believed to generate large-scale shock waves that are ideal sites for electron acceleration. We compute radio emission light curves for galaxy group and cluster mergers simulated in a cosmological context to study the dependence of radio luminosity on cluster mass, redshift, and impact parameter. We used model galaxy clusters from The Three Hundred project to identify cluster mergers characterised by the two main merging structures and follow their evolution throughout the simulated cosmic history. We found that the median non-thermal radio relic luminosity light curve produced in galaxy cluster mergers can be described by a skewed Gaussian function abruptly rising after core-passage of the secondary cluster that peaks after $sim0.1-0.8,$Gyr as a function of $M_{200,1}$, the mass of the primary, displaying a mass-dependent luminosity output increase of $lesssim10$ to about $gtrsim10-50$ times relative to the radio emission measured at core-passage for galaxy groups and clusters, respectively. In general, most merger orbits are fairly radial with a median opening angle of $sim20^{circ}$ before the collision. We also found that, independent of the cluster mass, less radial mergers tend to last longer, although the trend is weak. Finally, we found that the peak radio luminosity shows a significant correlation with mass, $P_{1.4}propto M_{200,1}^{2.05}$, demonstrating that this relation holds all the way up from galaxy group scales to the most massive galaxy clusters. We conclude that cluster mass is the primary driver for radio `gischt' median luminosity, although there are significant variations for a given cluster mass. Our simulations suggest that the shock-driven, non-thermal radio emission observed on cluster outskirts are the result of massive galaxy cluster mergers at $zlesssim1$, peaking at $zsim0-0.5$.
{"title":"The Three Hundred project: Radio luminosity evolution from merger-induced shock fronts in simulated galaxy clusters","authors":"Sebastián E. Nuza, Matthias Hoeft, Ana Contreras-Santos, Alexander Knebe, Gustavo Yepes","doi":"arxiv-2409.09422","DOIUrl":"https://doi.org/arxiv-2409.09422","url":null,"abstract":"Galaxy cluster mergers are believed to generate large-scale shock waves that\u0000are ideal sites for electron acceleration. We compute radio emission light\u0000curves for galaxy group and cluster mergers simulated in a cosmological context\u0000to study the dependence of radio luminosity on cluster mass, redshift, and\u0000impact parameter. We used model galaxy clusters from The Three Hundred project\u0000to identify cluster mergers characterised by the two main merging structures\u0000and follow their evolution throughout the simulated cosmic history. We found\u0000that the median non-thermal radio relic luminosity light curve produced in\u0000galaxy cluster mergers can be described by a skewed Gaussian function abruptly\u0000rising after core-passage of the secondary cluster that peaks after\u0000$sim0.1-0.8,$Gyr as a function of $M_{200,1}$, the mass of the primary,\u0000displaying a mass-dependent luminosity output increase of $lesssim10$ to about\u0000$gtrsim10-50$ times relative to the radio emission measured at core-passage\u0000for galaxy groups and clusters, respectively. In general, most merger orbits\u0000are fairly radial with a median opening angle of $sim20^{circ}$ before the\u0000collision. We also found that, independent of the cluster mass, less radial\u0000mergers tend to last longer, although the trend is weak. Finally, we found that\u0000the peak radio luminosity shows a significant correlation with mass,\u0000$P_{1.4}propto M_{200,1}^{2.05}$, demonstrating that this relation holds all\u0000the way up from galaxy group scales to the most massive galaxy clusters. We\u0000conclude that cluster mass is the primary driver for radio `gischt' median\u0000luminosity, although there are significant variations for a given cluster mass.\u0000Our simulations suggest that the shock-driven, non-thermal radio emission\u0000observed on cluster outskirts are the result of massive galaxy cluster mergers\u0000at $zlesssim1$, peaking at $zsim0-0.5$.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"102 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257672","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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