Group items tagged

This paper describes how to use shear detected mass peaks to measure the evolution of the power spectrum, and thereby cosmological parameters, in a method complementary to cosmic-shear analysis. (A)

Results from a large blind analysis study of shear measurements of galaxies. This paper contains good summaries of various methods to correct shear measurements for PSF smearing. (A)

There is no publicly available package to fully perform a cosmic-shear analysis of a data set. However, some very useful tools can be found at Martin Kilbinger's webpage under his software section. (A)

Weak lensing can be used to measure statistically the distribution of mass in structures that are not dense enough to be detected individually in mass reconstructions. This weak-lensing signal is conventionally known as "cosmic shear," and its measurement is one of the primary methods that has been proposed for accurately measuring cosmological parameters such as the matter and energy content of the universe, the curvature of the universe, and the scale of matter density fluctuations. From 2000-2002, several competing groups produced the first measurements of cosmic shear from surveys each covering ~10 square degrees. A summary of these results can be found in this review article.

Weak lensing can be used to measure statistically the distribution of mass in structures that are not dense enough to be detected individually in mass reconstructions. This weak-lensing signal is conventionally known as "cosmic shear," and its measurement is one of the primary methods that has been proposed for accurately measuring cosmological parameters such as the matter and energy content of the universe, the curvature of the universe, and the scale of matter density fluctuations. From 2000-2002, several competing groups produced the first measurements of cosmic shear from surveys each covering ~10 square degrees. A summary of these results can be found in this review article.

This paper describes how to use shear detected mass peaks to measure the evolution of the power spectrum, and thereby cosmological parameters, in a method complementary to cosmic-shear analysis. (A)

This paper discusses the impact on cosmological-parameter measurement from cosmic-shear surveys owing to the intrinsic alignments of galaxy shapes (prior to their being lensed). (A)

This paper discusses the impact on cosmological-parameter measurement from cosmic-shear surveys owing to a variety of systematic errors. Of particular importance are the intrinsic alignments of galaxy shapes (prior to their being lensed) and the accuracy with which the lensed-galaxies redshifts can be estimated from their colors alone. (A)

Results from a public shear simulation challenge that was specifically targeted for participation outside the weak lensing astronomical community. Also includes a summary of the results from the previous shear measurement challenges. (A)

Software for measuring galaxy shapes in images, including the PSF correction. Comes with some documentation, but also has a steep learning curves if is to be used effectively. We strongly encourage testing the software on the GREAT/STEP simulations before using them on actual data. (A)

Software for measuring galaxy shapes in images, including the PSF correction. Comes with some documentation, but also has a steep learning curves if is to be used effectively. We strongly encourage testing the software on the GREAT/STEP simulations before using them on actual data. (A)

Software for measuring galaxy shapes in images, including the PSF correction. Comes with some documentation, but also has a steep learning curves if is to be used effectively. We strongly encourage testing the software on the GREAT/STEP simulations before using them on actual data. (A)

Software for measuring galaxy shapes in images, including the PSF correction. Comes with some documentation, but also has a steep learning curves if is to be used effectively. We strongly encourage testing the software on the GREAT/STEP simulations before using them on actual data. (A).

Software for measuring galaxy shapes in images, including the PSF correction. Comes with some documentation, but also has a steep learning curves if is to be used effectively. We strongly encourage testing the software on the GREAT/STEP simulations before using them on actual data. (A)

This paper presents results from a combination of 4 blank-field surveys to achieve a 100 square degree total area, and contains a good discussion on how errors in Point Spread Function correction and background galaxy selection can propagate through to the cosmic-shear measurement. (A)

This paper describes an attempt to detect clusters by mass in a blank-field survey, thereby avoiding selection bias when measuring the evolution of the mass function. (A)

This paper describes measurements of cosmic shear from a 2 square degree Hubble Space Telescope survey, combined with photometric redshifts of the lensed galaxies. The addition of the photometric redshifts allowed the authors to measure the evolution of the mass power-spectrum, which provides additional information about the cosmological model beyond what the integrated power-spectrum can provide.

This paper describes measurements of cosmic shear from a 2 square degree Hubble Space Telescope survey, combined with photometric redshifts of the lensed galaxies. The addition of photometric redshifts allowed the authors to produce a three dimensional reconstruction of the mass structures in the field. (A)

This paper presents results from a combination of 4 blank-field surveys to achieve a 100 square degree total area, and contains a good discussion on how errors in Point Spread Function correction and background galaxy selection can propagate through to the cosmic-shear measurement. (A)

Introduces and explains the process of inferring a cluster of galaxies' mass distribution, from weak shear data. (I, A)