This Resource Letter provides a guide to a selection of the literature on gravitational lensing and its applications. Journal articles, books, popular articles, and websites are cited for the ...following topics: foundations of gravitational lensing, foundations of cosmology, history of gravitational lensing, strong lensing, weak lensing, and microlensing.
We present the size-luminosity relation (SLR) for disk galaxies observed in eight clusters from the ESO Distant Cluster Survey (EDisCS). These clusters, at redshifts 0.4 < z < 0.8, were observed with ...the Hubble Space Telescope's Advanced Camera for Surveys. While we observe a change in the SLR with redshift, namely that there is an absence of low surface brightness galaxies at high redshift, we demonstrate that this could be a product of selection effects and thus is not a confirmation of evolution. We also compare the SLR for cluster and field galaxies in each redshift bin and see no significant effects of environment on the SLR.
Astron.Astrophys. 395 (2002) 385-398 We present mass reconstructions from weak lensing for the galaxy clusters
A1835 and A2204 over 34'x34' fields using data from the ESO/MPG Wide Field
Imager. Using ...a background galaxy population of 22<R<25.5 we detect the
gravitational shear of A1835 at 8.8 sigma significance, and obtain best-fit
mass profiles of sigma_v=1233^{+66}_{-70} km/s for a singular isothermal sphere
model and r_{200}=1550 h^{-1} kpc, c=2.96 for a `universal' CDM profile. Using
a color-selected background galaxy population of 22<R<25.8 we detect the
gravitational shear of A2204 at 7.2 sigma significance, and obtain best-fit
mass profiles of sigma_v=1035^{+65}_{-71} km/s for a SIS model and r_{200}=1310
h^{-1} km/s, c=6.3 for a `universal' CDM profile. The gravitational shear at
distances greater than 10' is significantly detected for both clusters. The
best fit weak lensing cluster masses agree well with both X-ray and dynamical
mass measurements, although the central concentration of A1835 is much lower in
the weak lensing mass profile than that measured by recent Chandra results. We
suggest that this lower concentration is most likely a combination of
contamination of the 'background' galaxy population with cluster dwarf galaxies
and the effect of a prolate or tri-axial cluster core with the major axis lying
near the plane of the sky. We also detect a number of additional structures at
moderate significance, some of which appear to be sub-haloes associated with
the clusters.
We analyse the restaframe (U$-$V) colouramagnitude relation for 2 clusters at redshift 0.7 and 0.8, drawn from the ESO Distant Cluster Survey. By comparing them with the population of red galaxies in ...the Coma cluster, we show that the high redshift clusters exhibit a deficit of passive faint red galaxies. Our results show that the redasequence population cannot be explained in terms of a monolithic and synchronous formation scenario. A large fraction of faint passive galaxies in clusters today has moved onto the red sequence relatively recently as a consequence of the fact that their star formation activity has come to an end at $z<0.8$. To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html
We present the weak lensing mass reconstructions of three clusters of
galaxies from data taken on the ESO Wide Field Imager. We detect a lensing
signal in all three clusters over a range of 1' < r < ...17' (~0.1 h^-1 Mpc < r <
2 h^-1 Mpc). We measure the best fitting SIS and NFW profiles for each cluster
and show that in two of the three clusters the NFW profile is preferred to the
SIS with marginal significance (~95%).
We present a mass profile for A1689 from 0.13 h^{-1} Mpc < r < 2 h^{-1} Mpc
from a weak lensing analysis of a 34'x34' R-band image from the ESO/MPG Wide
Field Imager. We detect the gravitational ...shearing of a 23<R<25.5 background
galaxy population even at the edge of the image with a 4-sigma significance,
and find a two-dimensional mass reconstruction has a 13.4-sigma significance
mass peak centered on the brightest cluster galaxy. This peak is well fit by
both a 1028+-35 km/s singular isothermal sphere and a r200 = 1.28 Mpc, c = 6
universal CDM profile, although the universal CDM profile provides a better fit
with 95.5% confidence. These mass measurements are lower than most of those
derived by other means and we discuss possible reasons for weak lensing
providing an underestimate of the true mass of the cluster. We find that the
correction factors needed to reconcile the weak lensing mass models with the
strong lensing Einstein radius would result is a much larger fraction of faint
stars and foreground and cluster dwarf galaxies in the 23<R<25.5 object catalog
than is seen in other fields.
Nucl.Phys.Proc.Suppl.173:28-31,2007 We present X-ray and weak lensing observations of the merging cluster system
1E0657-556. Due to the recently collision of a merging subcluster with the main
...cluster, the X-ray plasma has been displaced from the cluster galaxies in both
components. The weak lensing data shows that the lensing surface potential is
in spatial agreement with the galaxies (~10% of the observed baryons) and not
with the X-ray plasma (~90% of the observed baryons). We argue that this shows
that regardless of the form of the gravitational force law at these large
distances and low accelerations, these observations require that the majority
of the mass of the system be some form of unseen matter.
We present mass reconstructions from weak lensing for the galaxy clusters A1835 and A2204 over 34'x34' fields using data from the ESO/MPG Wide Field Imager. Using a background galaxy population of ...22<R<25.5 we detect the gravitational shear of A1835 at 8.8 sigma significance, and obtain best-fit mass profiles of sigma_v=1233^{+66}_{-70} km/s for a singular isothermal sphere model and r_{200}=1550 h^{-1} kpc, c=2.96 for a `universal' CDM profile. Using a color-selected background galaxy population of 22<R<25.8 we detect the gravitational shear of A2204 at 7.2 sigma significance, and obtain best-fit mass profiles of sigma_v=1035^{+65}_{-71} km/s for a SIS model and r_{200}=1310 h^{-1} km/s, c=6.3 for a `universal' CDM profile. The gravitational shear at distances greater than 10' is significantly detected for both clusters. The best fit weak lensing cluster masses agree well with both X-ray and dynamical mass measurements, although the central concentration of A1835 is much lower in the weak lensing mass profile than that measured by recent Chandra results. We suggest that this lower concentration is most likely a combination of contamination of the 'background' galaxy population with cluster dwarf galaxies and the effect of a prolate or tri-axial cluster core with the major axis lying near the plane of the sky. We also detect a number of additional structures at moderate significance, some of which appear to be sub-haloes associated with the clusters.
We analyse the structures of all the clusters in the DAFT/FADA survey for which XMM-Newton and/or a sufficient number of galaxy redshifts in the cluster range is available, with the aim of detecting ...substructures and evidence for merging events. These properties are discussed in the framework of standard cold dark matter cosmology.XMM-Newton data were available for 32 clusters, for which we derive the X-ray luminosity and a global X-ray temperature for 25 of them. For 23 clusters we were able to fit the X-ray emissivity with a beta-model and subtract it to detect substructures in the X-ray gas. A dynamical analysis based on the SG method was applied to the clusters having at least 15 spectroscopic galaxy redshifts in the cluster range: 18 X-ray clusters and 11 clusters with no X-ray data. Only major substructures will be detected. Ten substructures were detected both in X-rays and by the SG method. Most of the substructures detected both in X-rays and with the SG method are probably at their first cluster pericentre approach and are relatively recent infalls. We also find hints of a decreasing X-ray gas density profile core radius with redshift. The percentage of mass included in substructures was found to be roughly constant with redshift with values of 5-15%, in agreement both with the general CDM framework and with the results of numerical simulations. Galaxies in substructures show the same general behaviour as regular cluster galaxies; however, in substructures, there is a deficiency of both late type and old stellar population galaxies. Late type galaxies with recent bursts of star formation seem to be missing in the substructures close to the bottom of the host cluster potential well. However, our sample would need to be increased to allow a more robust analysis.
We present a mass profile for A1689 from 0.13 h^{-1} Mpc < r < 2 h^{-1} Mpc from a weak lensing analysis of a 34'x34' R-band image from the ESO/MPG Wide Field Imager. We detect the gravitational ...shearing of a 23<R<25.5 background galaxy population even at the edge of the image with a 4-sigma significance, and find a two-dimensional mass reconstruction has a 13.4-sigma significance mass peak centered on the brightest cluster galaxy. This peak is well fit by both a 1028+-35 km/s singular isothermal sphere and a r200 = 1.28 Mpc, c = 6 universal CDM profile, although the universal CDM profile provides a better fit with 95.5% confidence. These mass measurements are lower than most of those derived by other means and we discuss possible reasons for weak lensing providing an underestimate of the true mass of the cluster. We find that the correction factors needed to reconcile the weak lensing mass models with the strong lensing Einstein radius would result is a much larger fraction of faint stars and foreground and cluster dwarf galaxies in the 23<R<25.5 object catalog than is seen in other fields.
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