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Title: Measuring the scale dependence of intrinsic alignments using multiple shear estimates

Abstract

We present a new method for measuring the scale dependence of the intrinsic alignment (IA) contamination to the galaxy–galaxy lensing signal, which takes advantage of multiple shear estimation methods applied to the same source galaxy sample. By exploiting the resulting correlation of both shape noise and cosmic variance, our method can provide an increase in the signal-to-noise of the measured IA signal as compared to methods which rely on the difference of the lensing signal from multiple photometric redshift bins. For a galaxy–galaxy lensing measurement which uses LSST sources and DESI lenses, the signal-to-noise on the IA signal from our method is predicted to improve by a factor of ~2 relative to the method of Blazek et al. (2012), for pairs of shear estimates which yield substantially different measured IA amplitudes and highly correlated shape noise terms. We show that statistical error necessarily dominates the measurement of IAs using our method. We also consider a physically motivated extension of the Blazek et al. (2012) method which assumes that all nearby galaxy pairs, rather than only excess pairs, are subject to IA. In this case, the signal-to-noise of the method of Blazek et al. (2012) is improved.

Authors:
 [1];  [2]
  1. Carnegie Mellon Univ., Pittsburgh, PA (United States)
  2. Carnegie Mellon Univ., Pittsburgh, PA (United States); et al.
Publication Date:
Research Org.:
Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC); Univ. of California, Oakland, CA (United States); Stanford Univ., CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
Contributing Org.:
The LSST Dark Energy Science Collaboration
OSTI Identifier:
1543962
Grant/Contract Number:  
AC02-05CH11231; AC02-76SF00515
Resource Type:
Journal Article: Accepted Manuscript
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Volume: 479; 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

Leonard, C. Danielle, and Mandelbaum, Rachel. Measuring the scale dependence of intrinsic alignments using multiple shear estimates. United States: N. p., 2018. Web. doi:10.1093/mnras/sty1444.
Leonard, C. Danielle, & Mandelbaum, Rachel. Measuring the scale dependence of intrinsic alignments using multiple shear estimates. United States. doi:10.1093/mnras/sty1444.
Leonard, C. Danielle, and Mandelbaum, Rachel. Sat . "Measuring the scale dependence of intrinsic alignments using multiple shear estimates". United States. doi:10.1093/mnras/sty1444. https://www.osti.gov/servlets/purl/1543962.
@article{osti_1543962,
title = {Measuring the scale dependence of intrinsic alignments using multiple shear estimates},
author = {Leonard, C. Danielle and Mandelbaum, Rachel},
abstractNote = {We present a new method for measuring the scale dependence of the intrinsic alignment (IA) contamination to the galaxy–galaxy lensing signal, which takes advantage of multiple shear estimation methods applied to the same source galaxy sample. By exploiting the resulting correlation of both shape noise and cosmic variance, our method can provide an increase in the signal-to-noise of the measured IA signal as compared to methods which rely on the difference of the lensing signal from multiple photometric redshift bins. For a galaxy–galaxy lensing measurement which uses LSST sources and DESI lenses, the signal-to-noise on the IA signal from our method is predicted to improve by a factor of ~2 relative to the method of Blazek et al. (2012), for pairs of shear estimates which yield substantially different measured IA amplitudes and highly correlated shape noise terms. We show that statistical error necessarily dominates the measurement of IAs using our method. We also consider a physically motivated extension of the Blazek et al. (2012) method which assumes that all nearby galaxy pairs, rather than only excess pairs, are subject to IA. In this case, the signal-to-noise of the method of Blazek et al. (2012) is improved.},
doi = {10.1093/mnras/sty1444},
journal = {Monthly Notices of the Royal Astronomical Society},
issn = {0035-8711},
number = 1,
volume = 479,
place = {United States},
year = {2018},
month = {6}
}

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