A framework for measuring weak-lensing magnification using the Fundamental Plane
Abstract
ABSTRACT Galaxy–galaxy lensing is an essential tool for probing dark matter haloes and constraining cosmological parameters. While galaxy–galaxy lensing measurements usually rely on shear, weak-lensing magnification contains additional constraining information. Using the Fundamental Plane (FP) of elliptical galaxies to anchor the size distribution of a background population is one method that has been proposed for performing a magnification measurement. We present a formalism for using the FP residuals of elliptical galaxies to jointly estimate the foreground mass and background redshift errors for a stacked lens scenario. The FP residuals include information about weak-lensing magnification κ, and therefore foreground mass, since to first order, non-zero κ affects galaxy size but not other FP properties. We also present a modular, extensible code that implements the formalism using emulated galaxy catalogues of a photometric galaxy survey. We find that combining FP information with observed number counts of the source galaxies constrains mass and photo-z error parameters significantly better than an estimator that includes number counts only. In particular, the constraint on the mass is 17.0 per cent if FP residuals are included, as opposed to 27.7 per cent when only number counts are included. The effective size noise for a foreground lens of mass $$M_\mathrm{ H}=10^{14}\, \mathrm{M}_\odot$$, with a conservative selection function in size and surface brightness applied to the source population, is σκ, eff = 0.250. We discuss the improvements to our FP model necessary to make this formalism a practical companion to shear analyses in weak-lensing surveys.
- Authors:
-
[1];
- Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, Columbus, Ohio 43210, USA, Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, Ohio 43210, USA
- Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA
- Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, Columbus, Ohio 43210, USA, Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, Ohio 43210, USA, Department of Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, Ohio 43210, USA
- Publication Date:
- Research Org.:
- The Ohio State Univ., Columbus, OH (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC)
- OSTI Identifier:
- 1636227
- Alternate Identifier(s):
- OSTI ID: 1803551
- Grant/Contract Number:
- SC0019083
- Resource Type:
- Published Article
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Additional Journal Information:
- Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 496 Journal Issue: 3; Journal ID: ISSN 0035-8711
- Publisher:
- Oxford University Press
- Country of Publication:
- United Kingdom
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; Astronomy & Astrophysics; gravitational lensing: weak; methods: statistical; galaxies: fundamental parameters; large-scale structure of Universe
Citation Formats
Freudenburg, Jenna K. C., Huff, Eric M., and Hirata, Christopher M. A framework for measuring weak-lensing magnification using the Fundamental Plane. United Kingdom: N. p., 2020.
Web. doi:10.1093/mnras/staa1505.
Freudenburg, Jenna K. C., Huff, Eric M., & Hirata, Christopher M. A framework for measuring weak-lensing magnification using the Fundamental Plane. United Kingdom. https://doi.org/10.1093/mnras/staa1505
Freudenburg, Jenna K. C., Huff, Eric M., and Hirata, Christopher M. Thu .
"A framework for measuring weak-lensing magnification using the Fundamental Plane". United Kingdom. https://doi.org/10.1093/mnras/staa1505.
@article{osti_1636227,
title = {A framework for measuring weak-lensing magnification using the Fundamental Plane},
author = {Freudenburg, Jenna K. C. and Huff, Eric M. and Hirata, Christopher M.},
abstractNote = {ABSTRACT Galaxy–galaxy lensing is an essential tool for probing dark matter haloes and constraining cosmological parameters. While galaxy–galaxy lensing measurements usually rely on shear, weak-lensing magnification contains additional constraining information. Using the Fundamental Plane (FP) of elliptical galaxies to anchor the size distribution of a background population is one method that has been proposed for performing a magnification measurement. We present a formalism for using the FP residuals of elliptical galaxies to jointly estimate the foreground mass and background redshift errors for a stacked lens scenario. The FP residuals include information about weak-lensing magnification κ, and therefore foreground mass, since to first order, non-zero κ affects galaxy size but not other FP properties. We also present a modular, extensible code that implements the formalism using emulated galaxy catalogues of a photometric galaxy survey. We find that combining FP information with observed number counts of the source galaxies constrains mass and photo-z error parameters significantly better than an estimator that includes number counts only. In particular, the constraint on the mass is 17.0 per cent if FP residuals are included, as opposed to 27.7 per cent when only number counts are included. The effective size noise for a foreground lens of mass $M_\mathrm{ H}=10^{14}\, \mathrm{M}_\odot$, with a conservative selection function in size and surface brightness applied to the source population, is σκ, eff = 0.250. We discuss the improvements to our FP model necessary to make this formalism a practical companion to shear analyses in weak-lensing surveys.},
doi = {10.1093/mnras/staa1505},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 3,
volume = 496,
place = {United Kingdom},
year = {2020},
month = {6}
}
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