CFHTLenS: the relation between galaxy dark matter haloes and baryons from weak gravitational lensing

By M. Velander, E. V. Uitert, H. Hoekstra, Jean Coupon, T. Erben, Catherine Heymans, H. Hildebrandt, Thomas D. Kitching, Y. Mellier, L. Miller and 9 more. 2013

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We present a study of the relation between dark matter halo mass and the baryonic content of their host galaxies, quantified through galaxy luminosit y and stellar mass. Our investigation uses 154deg 2 of Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS) lensing and photometric data, obtained from the CFHT Legacy Survey. To interpret the weak lensing signal around our galaxies we employ a galaxy-galaxy lensing halo model which allows us to constrain the halo mass and the satellite fraction . Our analysis is limited to lenses at redshifts between 0.2 and 0.4, split into a red and a blue sa mple. We express the relationship between dark matter halo mass and baryonic observable as a power law with pivot points of 10 11 h −2

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b775834ab6eb095cc6b0257271caeab2da65d124

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Citations in the corpus

Lensing is Low: Cosmology, Galaxy Formation, or New Physics? (2016, background): “Following Velander et al. (2014), we do not reject pointings that did not pass the requirements for cosmic shear.”
Constraining the Galaxy's dark halo with RAVE stars (2014, methodology): “Studies of weak lensing (Velander et al. 2014) and thermal X-ray emission (Das et al. 2011) have been used to map dark matter on large scales, while the kinematics of stars and gas provide the most powerful probe on small scales.”
Constraining the galaxy–halo connection over the last 13.3 Gyr: star formation histories, galaxy mergers and structural properties (2017, methodology): “We also include the stacked weak-lensing analysis from Velander et al. (2014) based on the CFHTLens survey, empty blue triangles.”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, methodology): “While some studies (Velander et al. 2014; Hudson et al. 2015) adopted the “tidally stripped” subhalo lensing model proposed in Mandelbaum et al. (2005), other studies (e.g., Leauthaud et al. 2012b; Coupon et al. 2015) ignored the lensing from subhalos, either based on the result of Yoo et al.…”
Gravitational lensing analysis of the Kilo-Degree Survey (2015, background): “…(Albrecht et al. 2006; Peacock et al. 2006), as well as to study the distribution of dark matter around galaxies with more accuracy than has been possible thus far from the ground (e.g. Mandelbaum et al. 2006; van Uitert et al. 2011; Velander et al. 2014) or space (e.g. Leauthaud et al. 2012).”
The Intrinsic Alignment of Galaxies and its Impact on Weak Gravitational Lensing in an Era of Precision Cosmology (2014, background): “…(2006); Zentner et al. (2008); Mead et al. (2010); Semboloni et al. (2011, 2013); Yang et al. (2013); Zentner et al. (2013); Eifler et al. (2014); Velander et al. (2014)), which causes changes in small scale (e.g., single halo) clustering relative to a dark matter only model and thus the matter…”
Galaxy Alignments: Observations and Impact on Cosmology (2015, background): “This is often referred to as galaxy-galaxy lensing, especially on scales where the lensing is dominated by the haloes of the foreground galaxies (e.g. Mandelbaum et al. 2006b; van Uitert et al. 2011; Velander et al. 2014).”
Intrinsic alignments of SDSS-III BOSS LOWZ sample galaxies (2014, background): “…the 1-halo satellite term and the halo-halo terms, which are important at larger rp values for galaxies in this mass range (see, e.g., figure 3 of Velander et al. 2014, which shows the contributions of these terms for a lower mass sample; all contributions tend to shift to the right for higher…”
H0LiCOW - IV. Lens mass model of HE 0435-1223 and blind measurement of its time-delay distance for cosmology (2016, methodology): “We use Lephare (Ilbert et al. 2006) to measure stellar masses for the best-fitting redshift using the spectral energy distribution (SED) templates employed by CFHTLenS (Velander et al. 2014), which assume a Chabrier (2003) initial mass function.”