Tomography-based observational measurements of the halo mass function via the submillimeter magnification bias

被引：8

作者：

Cueli, M. M. ^{[1
,2
]}

Bonavera, L. ^{[1
,2
]}

Gonzalez-Nuevo, J. ^{[1
,2
]}

Crespo, D. ^{[1
,2
]}

Casas, J. M. ^{[1
,2
]}

Lapi, A. ^{[3
,4
,5
,6
]}

机构：

[1] Univ Oviedo, Dept Fis, C Federico Garcia Lorca 18, Oviedo 33007, Spain

[2] Inst Univ Ciencias & Tecnol Espaciales Asturias, ICTEA, C Independencia 13, Oviedo 33004, Spain

[3] SISSA, Via Bonomea 265, I-34136 Trieste, Italy

[4] IFPU Inst Fundamental Phys Universe, Via Beirut 2, I-34014 Trieste, Italy

[5] IRA INAF, Via Gobetti 101, I-40129 Bologna, Italy

[6] INFN, Sez Trieste, Via Valerio 2, I-34127 Trieste, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2022年 / 662卷

基金：

欧盟地平线“2020”;

关键词：

galaxies: halos; submillimeter: galaxies; gravitational lensing: weak; ASSEMBLY GAMA; STOCHASTIC-THEORY; GALAXY; MODEL; EVOLUTION; HERSCHEL; NONUNIVERSALITY; COSMOLOGY; ABUNDANCE; CLUSTERS;

D O I：

10.1051/0004-6361/202142949

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Aims. The main goal of this paper is to derive observational constraints on the halo mass fuction (HMF) by performing a tomographic analysis of the magnification bias signal on a sample of background submillimeter galaxies. The results can then be compared with those from a non-tomographic study. Methods. We measure the cross-correlation function between a sample of foreground GAMA galaxies with spectroscopic redshifts in the range 0.1 < z < 0.8 (and divided up into four bins) and a sample of background submillimeter galaxies from H-ATLAS with photometric redshifts in the range 1.2 < z < 4.0. We model the weak lensing signal within the halo model formalism and carry out a Markov chain Monte Carlo algorithm to obtain the posterior distribution of all HMF parameters, which we assume to follow the Sheth and Tormen (ST) three-parameter and two-parameter fits. Results. While the observational constraints on the HMF from the non-tomographic analysis are not stringent, there is a remarkable improvement in terms of uncertainty reduction when tomography is adopted. Moreover, with respect to the traditional ST triple of values from numerical simulations, the results from the three-parameter fit predict a higher number density of halos at masses below similar to 10(12) M-circle dot h(-1) at 95% credibility. The two-parameter fit yields even more restricting results, with a larger number density of halos below similar to 10(13) M-circle dot h(-1) and a lower one above similar to 10(14) M-circle dot h(-1), this time at more than 3 sigma credibility. Our results are therefore in disagreement with the standard N-body values for the ST fit at 2 sigma and 3 sigma, respectively.

引用

页数：18

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