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Title: Using galaxy pairs to investigate the three-point correlation function in the squeezed limit

Abstract

We investigate the three-point correlation function (3PCF) in the squeezed limit by considering galaxy pairs as discrete objects and cross-correlating them with the galaxy field. We develop an efficient algorithm using fast Fourier transforms to compute such cross-correlations and their associated pair-galaxy bias bp, g and the squeezed 3PCF coefficient Qeff. We implement our method using N-body cosmological simulations and a fiducial halo occupation distribution (HOD) and present the results in both the real space and redshift space. In real space, we observe a peak in b p, g and Q eff at pair separation of ~2 Mpc, attributed to the fact that galaxy pairs at 2 Mpc separation trace the most massive dark matter haloes. We also see strong anisotropy in the b p, g and Qeff signals that track the large-scale filamentary structure. In redshift space, both the 2 Mpc peak and the anisotropy are significantly smeared out along the line of sight due to finger-of-God effect. In both the real space and redshift space, the squeezed 3PCF shows a factor of 2 variation, contradicting the hierarchical ansatz, but offering rich information on the galaxy-halo connection. Thus, we explore the possibility of using the squeezed 3PCF to constrainmore » the HOD. When we compare two simple HOD models that are closely matched in their projected two-point correlation function (2PCF), we do not yet see a strong variation in the 3PCF that is clearly disentangled from variations in the projected 2PCF. Nevertheless, we propose that more complicated HOD models, e.g. those incorporating assembly bias, can break degeneracies in the 2PCF and show a distinguishable squeezed 3PCF signal.« less

Authors:
ORCiD logo [1];  [1];  [1]
  1. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
Publication Date:
Research Org.:
Harvard Univ., Cambridge, MA (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1540614
Grant/Contract Number:  
SC0013718
Resource Type:
Accepted Manuscript
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Volume: 472; Journal Issue: 1; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Astronomy & Astrophysics

Citation Formats

Yuan, Sihan, Eisenstein, Daniel J., and Garrison, Lehman H. Using galaxy pairs to investigate the three-point correlation function in the squeezed limit. United States: N. p., 2017. Web. doi:10.1093/mnras/stx2032.
Yuan, Sihan, Eisenstein, Daniel J., & Garrison, Lehman H. Using galaxy pairs to investigate the three-point correlation function in the squeezed limit. United States. doi:10.1093/mnras/stx2032.
Yuan, Sihan, Eisenstein, Daniel J., and Garrison, Lehman H. Fri . "Using galaxy pairs to investigate the three-point correlation function in the squeezed limit". United States. doi:10.1093/mnras/stx2032. https://www.osti.gov/servlets/purl/1540614.
@article{osti_1540614,
title = {Using galaxy pairs to investigate the three-point correlation function in the squeezed limit},
author = {Yuan, Sihan and Eisenstein, Daniel J. and Garrison, Lehman H.},
abstractNote = {We investigate the three-point correlation function (3PCF) in the squeezed limit by considering galaxy pairs as discrete objects and cross-correlating them with the galaxy field. We develop an efficient algorithm using fast Fourier transforms to compute such cross-correlations and their associated pair-galaxy bias bp, g and the squeezed 3PCF coefficient Qeff. We implement our method using N-body cosmological simulations and a fiducial halo occupation distribution (HOD) and present the results in both the real space and redshift space. In real space, we observe a peak in bp, g and Qeff at pair separation of ~2 Mpc, attributed to the fact that galaxy pairs at 2 Mpc separation trace the most massive dark matter haloes. We also see strong anisotropy in the bp, g and Qeff signals that track the large-scale filamentary structure. In redshift space, both the 2 Mpc peak and the anisotropy are significantly smeared out along the line of sight due to finger-of-God effect. In both the real space and redshift space, the squeezed 3PCF shows a factor of 2 variation, contradicting the hierarchical ansatz, but offering rich information on the galaxy-halo connection. Thus, we explore the possibility of using the squeezed 3PCF to constrain the HOD. When we compare two simple HOD models that are closely matched in their projected two-point correlation function (2PCF), we do not yet see a strong variation in the 3PCF that is clearly disentangled from variations in the projected 2PCF. Nevertheless, we propose that more complicated HOD models, e.g. those incorporating assembly bias, can break degeneracies in the 2PCF and show a distinguishable squeezed 3PCF signal.},
doi = {10.1093/mnras/stx2032},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 1,
volume = 472,
place = {United States},
year = {2017},
month = {8}
}

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