Understanding the shape of the galaxy two-point correlation function at z~1 in the COSMOS field
S. de la Torre, L. Guzzo, K. Kovac, C. Porciani, U. Abbas, B. Meneux, C. M. Carollo, T. Contini, J. -P. Kneib, O. Le Fevre, S. J. Lilly, V. Mainieri, A. Renzini… 展开作者
S. de la Torre, L. Guzzo, K. Kovac, C. Porciani, U. Abbas, B. Meneux, C. M. Carollo, T. Contini, J. -P. Kneib, O. Le Fevre, S. J. Lilly, V. Mainieri, A. Renzini, D. Sanders, M. Scodeggio, N. Scoville, G. Zamorani, S. Bardelli, M. Bolzonella, A. Bongiorno, K. Caputi, G. Coppa, O. Cucciati, L. de Ravel, P. Franzetti, B. Garilli, A. Iovino, P. Kampczyk, C. Knobel, A. M. Koekemoer, F. Lamareille, J. -F. Le Borgne, V. Le Brun, C. Maier, M. Mignoli, R. Pello, Y. Peng, E. Perez-Montero, E. Ricciardelli, J. Silverman, M. Tanaka, L. Tasca, L. Tresse, D. Vergani, N. Welikala, E. Zucca, D. Bottini, A. Cappi, P. Cassata, A. Cimatti, M. Fumana, O. Ilbert, A. Leauthaud, D. Maccagni, C. Marinoni, H. J. McCracken, P. Memeo, P. Nair, P. Oesch, L. Pozzetti, V. Presotto, R. Scaramella
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6 pages, 3 figures, accepted for publication in MNRAS
We investigate how the shape of the galaxy two-point correlation function as measured in the zCOSMOS survey depends on local environment, quantified in terms of the density contrast on scales of 5 Mpc/h. We show that the flat shape previously observed at redshifts between z=0.6 and z=1 can be explained by this volume being simply 10% over-abundant in high-density environments, with respect to a Universal density probability distribution function. When galaxies corresponding to the top 10% tail of the distribution are excluded, the measured w_p(r_p) steepens and becomes indistinguishable from LCDM predictions on all scales. This is the same effect recognised by Abbas & Sheth in the SDSS data at z~0 and explained as a natural consequence of halo-environment correlations in a hierarchical scenario. Galaxies living in high-density regions trace dark matter halos with typically higher masses, which are more correlated. If the density probability distribution function of the sample is particularly rich in high-density regions because of the variance introduced by its finite size, this produces a distorted two-point correlation function. We argue that this is the dominant effect responsible for the observed "peculiar" clustering in the COSMOS field.
Fast Radio Bursts (hereafter FRBs) can be used in cosmology by studying the Dispersion Measure (hereafter DM) as a function of redshift. The large scale structure of matter distribution is regarded as a major error budget for such application. Using optical galaxy and dispersion measure mocks built from N-body simulations, we have shown that the galaxy number density can be used as a tracer for large scale electron density and help improve the measurement of DM as a function of redshift. We have shown that, using the line-of-sight galaxy number counts within 1' around the given localized FRB s…
Intrinsic galaxy alignments yield an important contribution to the observed statistics of galaxy shapes. The general bias expansion for galaxy sizes and shapes in three dimensions has been recently described by Vlah, Chisari \& Schmidt using the general perturbative effective field theory (EFT) framework, in analogy to the clustering of galaxies. In this work, we present a formalism that uses the properties of spherical tensors to project galaxy shapes onto the observed sky in the flat-sky approximation and compute the two-point functions at next-to-leading order as well as the leading-order t…
One of the cornerstones of general relativity is the equivalence principle. However, the validity of the equivalence principle has only been established on solar system scales for standard matter fields; this result cannot be assumed to hold for the non-standard matter fields that dominate the gravitational dynamics on cosmological scales. Here we show how the equivalence principle may be tested on cosmological scales for non-standard matter fields using the odd multipoles of the galaxy cross-power spectrum and bispectrum. This test makes use of the imprint on the galaxy cross-power spectrum a…
The halo mass function (HMF) is a critical element in cosmological analyses of galaxy cluster catalogs. We quantify the impact of uncertainties in HMF parameters on cosmological constraints from cluster catalogs similar to those from Planck, those expected from the Euclid, Roman and Rubin surveys, and from a hypothetical larger future survey. We analyse simulated catalogs in each case, gradually loosening priors on HMF parameters to evaluate the degradation in cosmological constraints. While current uncertainties on HMF parameters do not substantially impact Planck-like surveys, we find that t…
The shape of relaxed galaxy clusters and the public release of a HST shape measurement code, pyRRG
我们研究了八个动态松弛的星系团的形状与哈勃太空望远镜和钱德拉X射线天文台观测。利用强、弱引力透镜、布里渊星系团的形状和X射线等照度线，研究了四种不同半径的星系团晕的椭圆率。我们发现，代理探测的内部区域的集群是强烈耦合的BCG形状与预测的形状由强引力透镜和X射线等照度线。相反，我们发现没有这样的形状之间的相关性预测的弱透镜和其他三个探针之间的任何耦合的内部和外部区域是弱的。我们还在本文中公开发布了HST弱透镜形状测量代码pyRRG，可直接从PyPi（https：//pypi.org/project/pyRRG/）获得。这段基于Rhodes et al.（2000）的python3.7代码采用了一个基于随机森林的自动化恒星-星系分类器，并输出了科学上有用的产品，例如适用于质量映射算法Lentool的弱透镜星表。
Multiprobe cosmology forecasts from halo-occupation-distribution-based forward modeling of galaxy and void statistics
Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Department of Physics, University of Arizona（亚利桑那大学物理系）；Aix-Marseille Université, CNRS/IN2P3, CPPM（艾克斯-马赛大学，法国国家科学研究中心/法国国家核子和粒子物理研究所，粒子与宇宙学中心）；Department of Astrophysical Sciences, Peyton Hall, Princeton University（普林斯顿大学天体物理学系）；Universitäts-Sternwarte München, Fakultät für Physik, Ludwig-Maximilians-Universität（慕尼黑大学天文台，慕尼黑大学物理学院）
Effects of simulated cosmological magnetic fields on the galaxy population
我们调查的原始磁种子场的强度变化的影响，在理想的磁流体动力学宇宙学模拟与移动网格代码AREPO进行的星系人口的全球性质。我们在计算中改变了种子场，使其值的范围仍然与当前宇宙学的上限相兼容。我们表明，以上的$\simeq 10^{-9}\,{\rm G}$的临界强度，从外地产生的额外的压力强烈影响的气体结构的演变，导致宇宙恒星形成历史的抑制，\rev{which is stronger for larger seed fields. This directly reflects into a lower total galaxy count above a fixed stellar mass threshold at all redshifts, and}一个较低的星系数密度在固定的恒星质量和质量较小的恒星组件在所有质量尺度上固定维里质量。除了现有的方法之外，这些签名可以用于导出对原始磁种子场强度的更严格的约束。
The galaxies form and evolve in the early epochs through the anisotropic merging process along the primary narrow filaments, in the direction of which their shapes become elongated and intrinsically aligned. The nonlinear evolution of the cosmic web broadens the primary filaments, by entangling them with multiple secondary filaments, which has an effect of reducing the anisotropy of the merging process and in consequence weakens the galaxy shape-shape correlations in the later epochs. Assuming that the degree of the nonlinearity and complexity of the cosmic web depends on the nature of dark ma…
We discover a linear relation between two sets of galaxy-lensing cross-correlations. This linear relation holds, as long as light follows the geodesic and the metric is Friedmann-Lemaître-Robertson-Walker (FLRW). Violation of the cosmological principle (and equivalently the FLRW metric) will break this linear relation. Therefore it provides a powerful test of the cosmological principle, based on direct observables and relied on no specific cosmological models. We demonstrate that stage IV galaxy surveys and CMB-S4 experiments will be able to test this linear relation stringently and therefore …
In the past several decades, multiple cosmological theories that are based on the contention that the Universe has a major axis have been proposed. Such theories can be based on the geometry of the Universe, or multiverse theories such as black hole cosmology. The contention of a cosmological-scale axis is supported by certain evidence such as the dipole axis formed by the CMB distribution. Here I study another form of cosmological-scale axis, based on the distribution of the spin direction of spiral galaxies. Data from four different telescopes is analyzed, showing nearly identical axis profi…
Star-forming galaxies with strong nebular and collisional emission lines are privileged target galaxies in forthcoming cosmological large galaxy redshift surveys. We use the COSMOS2015 photometric catalog to model galaxy spectral energy distributions and emission-line fluxes. We adopt an empirical but physically-motivated model that uses information from the best-fitting spectral energy distribution of stellar continuum to each galaxy. The emission-line flux model is calibrated and validated against direct flux measurements in subsets of galaxies that have 3D-HST or zCOSMOS-Bright spectra. We …
We identify a new cosmological signal, the Doppler-boosted Cosmic Infrared Background (DB-CIB), arising from the peculiar motion of the galaxies whose thermal dust emission source the cosmic infrared background (CIB). This new observable is an independent probe of the cosmic velocity field, highly analogous to the well-known kinematic Sunyaev-Zel'dovich (kSZ) effect. Interestingly, DB-CIB does not suffer from the 'kSZ optical depth degeneracy', making it immune from the complex astrophysics of galaxy formation. We forecast that the DB-CIB effect is detectable in the cross-correlation of CCAT-P…
In String Gas Cosmology, the simplest shape modulus fields are naturally stabilized by taking into account the presence of string winding and momentum modes. We determine the resulting effective potential for these fields and show that it obeys the de Sitter conjecture, one of the swampland criteria for effective field theories to be consistent with superstring theory.
Galaxy imaging surveys provide us with information on both the galaxy distribution and their shapes. In this paper, we systematically investigate the sensitivity of galaxy shapes to new physics in the initial conditions. For this purpose, we decompose the galaxy shape function into spin components, and compute the contributions to each spin component from both intrinsic alignment and weak lensing. We then consider the angular-dependent primordial non-Gaussianity, which is generated by a non-zero integer spin particle when active during inflation, and show that a galaxy imaging survey essential…
