English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Weak gravitational lensing is a valuable probe of galaxy formation and cosmology. Here we quantify the effects of using photometric redshifts (photo‐ z ) in galaxy–galaxy lensing, for both sources and lenses, both for the immediate goal of using galaxies with photo‐ z  as lenses in the Sloan Digital Sky Survey (SDSS) and as a demonstration of methodology for large, upcoming weak lensing surveys that will by necessity be dominated by lens samples with photo‐ z . We calculate the bias in the lensing mass calibration as well as consequences for absolute magnitude (i.e.  k ‐corrections) and stellar mass estimates for a large sample of SDSS Data Release 8 (DR8) galaxies. The redshifts are obtained with the template‐based photo‐ z  code  zebra  on the SDSS DR8  ugriz  photometry. We assemble and characterize the calibration samples (∼9000 spectroscopic redshifts from four surveys) to obtain photometric redshift errors and lensing biases corresponding to our full SDSS DR8 lens and source catalogues. Our tests of the calibration sample also highlight the impact of observing conditions in the imaging survey when the spectroscopic calibration covers a small fraction of its footprint; atypical imaging conditions in calibration fields can lead to incorrect conclusions regarding the photo‐ z  of the full survey.  For the SDSS DR8 catalogue, we find σ Δ z /(1+ z ) = 0.096 and 0.113 for the lens and source catalogues, with flux limits of  r = 21 and 21.8, respectively. The photo‐ z  bias and scatter is a function of photo‐ z  and template types, which we exploit to apply photo‐ z  quality cuts. By using photo‐ z  rather than spectroscopy for lenses, dim blue galaxies and  L  *  galaxies up to  z ∼ 0.4 can be used as lenses, thus expanding into unexplored areas of parameter space. We also explore the systematic uncertainty in the lensing signal calibration when using source photo‐ z , and both lens and source photo‐ z ; given the size of existing training samples, we can constrain the lensing signal calibration (and therefore the normalization of the surface mass density) to within 2 and 4 per cent, respectively.

Photometric redshift requirements for lens galaxies in galaxy–galaxy lensing analyses