Weak Lensing

Wittman, David

doi:10.1007/3-540-45857-3_2

Cited by 14 publications

(8 citation statements)

References 124 publications

(147 reference statements)

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“…After correcting for PSF and CTE effects for objects in an individual science field, we can apply the standard weak lensing formalism (see e.g., Seitz & Schneider 1997;Bartelmann & Schneider 2001;Wittman 2002) to the field and determine an average mass profile from a stack of fields.…”

Section: Catalog Stackingmentioning

confidence: 99%

Cosmic Evolution of Virial and Stellar Mass in Massive Early-Type Galaxies

Lagattuta

Fassnacht

Auger

et al. 2010

ApJ

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We measure the average mass properties of a sample of 41 strong gravitational lenses at moderate redshift (z ∼ 0.4 -0.9), and present the lens redshift for 6 of these galaxies for the first time. Using the techniques of strong and weak gravitational lensing on archival data obtained from the Hubble Space Telescope, we determine that the average mass overdensity profile of the lenses can be fit with a powerlaw profile (∆Σ ∝ R −0.86±0.16 ) that is within 1-σ of an isothermal profile (∆Σ ∝ R −1 ) with velocity dispersion σ v = 260 ± 20 km s −1 . Additionally, we use a two-component de Vaucouleurs+NFW model to disentangle the total mass profile into separate luminous and dark matter components, and determine the relative fraction of each component. We measure the average rest frame V-band stellar mass-to-light ratio (Υ V = 4.0±0.6 h M ⊙ /L ⊙ ) and virial mass-to-light ratio (τ V = 300±90 h M ⊙ /L ⊙ ) for our sample, resulting in a virial-to-stellar mass ratio of M vir /M * = 75 ± 25. Relaxing the NFW assumption, we estimate that changing the inner slope of the dark matter profile by ∼20% yields a ∼30% change in stellar mass-to-light ratio. Finally, we compare our results to a previous study using low redshift lenses, to understand how galaxy mass profiles evolve over time. We investigate the evolution of M vir /M * (z) = α(1 + z) β , and find best fit parameters of α = 51 ± 36 and β = 0.9 ± 1.8, constraining the growth of virial to stellar mass ratio over the last ∼7 Gigayears. We note that, by using a sample of strong lenses, we are able to constrain the growth of M vir /M * (z) without making any assumptions about the IMF of the stellar population.

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Section: Catalog Stackingmentioning

confidence: 99%

Cosmic Evolution of Virial and Stellar Mass in Massive Early-Type Galaxies

Lagattuta

Fassnacht

Auger

et al. 2010

ApJ

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“…We additionally also chose not to weight each source galaxy by the critical surface mass density because all of our source galaxies are at a much higher redshift than Coma and therefore the weights are very nearly equal. In the case of no weights, the shear responsivity is R = 1 − σ 2 SN , where σ SN is the shape noise (the width of the intrinsic ellipticity distribution per ellipticity component) (Wittman 2002). Here we use a shape noise of σ SN = 0.37 which was used previously in Hirata et al (2004) for the same source galaxy magnitude range.…”

Section: Shear Measurementmentioning

confidence: 99%

The Mass of the Coma Cluster from Weak Lensing in the Sloan Digital Sky Survey

Kubo

Stebbins

Annis

et al. 2007

ApJ

138

130

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We present a weak lensing analysis of the Coma Cluster using the Sloan Digital Sky Survey (SDSS) Data Release Five. Complete imaging of a ∼ 200 square degree region is used to measure the tangential shear of this cluster. The shear is fit to an NFW model and we find a virial radius of r 200 = 1.99 +0.21 −0.22 h −1 Mpc which corresponds to a virial mass of M 200 = 1.88 +0.65 −0.56 × 10 15 h −1 M ⊙ . We additionally compare our weak lensing measurement to the virial mass derived using dynamical techniques, and find they are in agreement. This is the lowest redshift, largest angle weak lensing measurement of an individual cluster to date.

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“…Such ''cosmic shear'' is induced by the (differential) gravitational deflection of a light bundle, and happens regardless of the nature and state of the foreground mass. It is therefore a uniquely powerful probe of the dark matter distribution, directly and simply linked to theories of structure formation that may be ill-equipped to predict the distribution of light (for reviews, see Bartelmann & Schneider 2001;Wittman 2002;Refregier 2003). Furthermore, the main difficulties in this technique lie within the optics of a telescope that has been built on Earth and can be thoroughly tested.…”

Section: Introductionmentioning

confidence: 99%

“…Large, dedicated surveys with ground-based telescopes have recently measured the projected two-dimensional power spectrum of the large-scale mass distribution and drawn competitive constraints on cosmological parameters ( Brown et al 2003;Bacon et al 2003;Hamana et al 2003;Jarvis et al 2003;Van Waerbeke et al 2005;Hoekstra et al 2006). The addition of photometric redshift estimation for large numbers of galaxies has led to the first measurements of a changing lensing signal as a function of redshift (Bacon et al 2004;Wittman 2005;Semboloni et al 2006).…”

Section: Introductionmentioning

confidence: 99%

COSMOS: Three‐dimensional Weak Lensing and the Growth of Structure

Massey

Rhodes

Leauthaud

et al. 2007

ASTROPHYS J SUPPL S

247

221

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We present a three-dimensional cosmic shear analysis of the Hubble Space Telescope COSMOS survey, the largest ever optical imaging program performed in space. We have measured the shapes of galaxies for the telltale distortions caused by weak gravitational lensing and traced the growth of that signal as a function of redshift. Using both 2D and 3D analyses, we measure cosmological parameters m , the density of matter in the universe, and 8 , the normalization of the matter power spectrum. The introduction of redshift information tightens the constraints by a factor of 3 and also reduces the relative sampling (or ''cosmic'') variance compared to recent surveys that may be larger but are only two-dimensional. From the 3D analysis, we find that 8 ( m /0:3) 0:44 ¼ 0:866 þ0:085 À0:068 at 68% confidence limits, including both statistical and potential systematic sources of error in the total budget. Indeed, the absolute calibration of shear measurement methods is now the dominant source of uncertainty. Assuming instead a baseline cosmology to fix the geometry of the universe, we have measured the growth of structure on both linear and nonlinear physical scales. Our results thus demonstrate a proof of concept for tomographic analysis techniques that have been proposed for future weak-lensing surveys by a dedicated wide-field telescope in space. Subject headingg s: cosmology: observations -gravitational lensing -large-scale structure of universe

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Weak Lensing

Cited by 14 publications

References 124 publications

Cosmic Evolution of Virial and Stellar Mass in Massive Early-Type Galaxies

Cosmic Evolution of Virial and Stellar Mass in Massive Early-Type Galaxies

The Mass of the Coma Cluster from Weak Lensing in the Sloan Digital Sky Survey

COSMOS: Three‐dimensional Weak Lensing and the Growth of Structure

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