scholarly journals Hubble Space TelescopePhotometry and Keck Spectroscopy of the Rich Cluster MS 1054−03: Morphologies, Butcher‐Oemler Effect, and the Color‐Magnitude Relation atz= 0.83

2000 ◽  
Vol 541 (1) ◽  
pp. 95-111 ◽  
Author(s):  
Pieter G. van Dokkum ◽  
Marijn Franx ◽  
Daniel Fabricant ◽  
Garth D. Illingworth ◽  
Daniel D. Kelson
Keyword(s):  
Rich Cluster ◽  
The Rich

scholarly journals Spectroscopy of arcs in the rich cluster Abell 963

1991 ◽  
Vol 249 (1) ◽  
pp. 184-190 ◽  
Author(s):  
Richard Ellis ◽  
Jeremy Allington-Smith ◽  
Ian Smail
Keyword(s):  
Rich Cluster ◽  
The Rich

scholarly journals Spatially Resolved Spectroscopy of Starburst and Post-Starburst Galaxies in the Rich z ∼0.55 Cluster CL 0016+16

2010 ◽  
Vol 27 (3) ◽  
pp. 360-373 ◽  
Author(s):  
Michael B. Pracy ◽  
Warrick J. Couch ◽  
Harald Kuntschner
Keyword(s):  
Age Distribution ◽  
Starburst Galaxies ◽  
Small Sample ◽  
Spectral Signature ◽  
Rich Cluster ◽  
Spatially Resolved ◽  
Radial Profiles ◽  
Field Samples ◽  
The Rich ◽  
Spatially Resolved Spectroscopy

AbstractWe have used the Low Resolution Imaging Spectrograph on the W. M. Keck I telescope to obtain spatially resolved spectroscopy of a small sample of six ‘post-starburst’ and three ‘dusty-starburst’ galaxies in the rich cluster CL 0016+16 at z=0.55. We use this to measure radial profiles of the Hδ and [OII]λ3727 lines which are diagnostic probes of the mechanisms that give rise to the abrupt changes in star formation rates in these galaxies. In the post-starburst sample we are unable to detect any radial gradients in the Hδ line equivalent width — although one galaxy exhibits a gradient from one side of the galaxy to the other. The absence of Hδ gradients in these galaxies is consistent with their production via interaction with the intracluster medium; however, our limited spatial sampling prevents us from drawing robust conclusions. All members of the sample have early-type morphologies, typical of post-starburst galaxies in general, but lack the high incidence of tidal tails and disturbances seen in local field samples. This argues against a merger origin and adds weight to a scenario where truncation by the intra-cluster medium is at work. The post-starburst spectral signature is consistent over the radial extent probed with no evidence of [OII]λ3727 emission and strong Hδ absorption at all radii, i.e. the post-starburst classification is not an aperture effect. In contrast the ‘dusty-starburst’ sample shows a tendency for a central concentration of [OII]λ3727 emission. This is most straightforwardly interpreted as the consequence of a central starburst. However, other possibilities exist such as a non-uniform dust distribution (which is expected in such galaxies) and/or a non-uniform starburst age distribution. The members of the sample exhibit late-type and irregular morphologies.

scholarly journals The Mass‐to‐Light Ratio of Early‐Type Galaxies: Constraints from Gravitational Lensing in the Rich Cluster AC 114

1998 ◽  
Vol 499 (2) ◽  
pp. 600-607 ◽  
Author(s):  
Priyamvada Natarajan ◽  
Jean‐Paul Kneib ◽  
Ian Smail ◽  
Richard S. Ellis
Keyword(s):  
Gravitational Lensing ◽  
Early Type ◽  
Rich Cluster ◽  
The Rich

scholarly journals Measuring the Evolution of the M/L ratio from the Fundamental Plane in Cl 0024+16 at z=0.39

1996 ◽  
Vol 171 ◽  
pp. 233-240 ◽  
Author(s):  
Marijn Franx ◽  
Pieter G. van Dokkum
Keyword(s):  
Luminosity Function ◽  
Evolutionary Models ◽  
Early Type ◽  
Rich Cluster ◽  
Fundamental Plane ◽  
Evolution Of Galaxies ◽  
Cluster Environment ◽  
Dynamical Properties ◽  
The Rich

The existence of the Fundamental Plane of early-type galaxies implies that the M/L ratios of early-types are well behaved. It provides therefore an important tool to measure the evolution of the M/L ratio with redshift. These measurements, in combination with measurements of the evolution of the luminosity function, can be used to constrain the mass evolution of galaxies.We present the Fundamental Plane relation measured for galaxies in the rich cluster CL 0024+16 at z=0.391. The galaxies satisfy a tight Fundamental Plane, with relatively low scatter (15 %). The M/L is 31 ± 12 % lower than the M/L measured in Coma, which is consistent with simple evolutionary models. Hence, galaxies with very similar dynamical properties existed at a z=0.4.More, and deeper data are needed to measure the evolution of the slope and the scatter of the Fundamental Plane to higher accuracy. Furthermore, data on the richest nearby clusters would be valuable to test the hypothesis that the Fundamental Plane is independent of cluster environment.

scholarly journals Formation Of Giant Luminous Arcs And Arclets Using An Optical Gravitational Lens Experiment

1996 ◽  
Vol 173 ◽  
pp. 417-418
Author(s):  
J. Surdej ◽  
S. Refsdal ◽  
A. Pospieszalska-Surdej
Keyword(s):  
Light Source ◽  
Gravitational Lens ◽  
Light Deflection ◽  
Rich Cluster ◽  
Optical Lens ◽  
Multiple Images ◽  
Galaxy Disk ◽  
The Rich ◽  
The Right ◽  
Compact Light Source

It is well known that simple optical lenses simulating light deflection due to a foreground object may easily reproduce all types of image configurations observed among known multiply imaged QSOs and AGN (cf. simulations in Refsdal and Surdej 1992, 1994, Surdej et al. 1993). Such an optical lens experiment can also be used to simulate the formation of multiple giant luminous arcs and arclets seen near massive foreground galaxy clusters. The optical setup used to make this experiment is shown in Fig. 1 (a similar setup was presented during the Melbourne conference). A compact light source is located on the right side (not very clearly seen), then comes to the left a ‘spiral galaxy disk’ optical lens (manufactured by the authors) and a cardboard perforated by multiple pinholes. In the absence of light deflection (i.e. by simply removing the optical lens), direct (non distorted) images of the background galaxies are seen by an observer, like those projected on the distant white screen (see Fig. 2a). When the optical lens is inserted between the light source and the multiple pinholes screen (cf. Fig. 1), images of the background galaxies get distorted (arclets) and/or transformed into multiple images, including giant luminous arcs (see Figs. 2bc for examples). We showed during the conference that by covering the pinholes with various transparent colored filters and translating the multiple pinholes screen, it was possible to reproduce, in a very inexpensive way, distorted images of background galaxies like the very impressive strong lensing artifacts seen behind the rich cluster Abell 1689 (cf. the color videotape of simulations by Tony Tyson).

The dynamics of the rich cluster A2634

1991 ◽  
Author(s):  
George Rhee ◽  
Jason Pinkney ◽  
Jack Burns ◽  
J. M. Hill ◽  
W. Oegerle ◽  
...  
Keyword(s):  
Rich Cluster ◽  
The Rich

Dynamical Friction in the Rich Cluster A2029

1988 ◽  
pp. 115-119
Author(s):  
R. G. Bower ◽  
R. S. Ellis ◽  
G. F. Efstathiou
Keyword(s):  
Dynamical Friction ◽  
Rich Cluster ◽  
The Rich

Hubble Space Telescope Observations of Gravitationally Lensed Features in the Rich Cluster AC 114

1995 ◽  
Vol 440 ◽  
pp. 501 ◽  
Author(s):  
Ian Smail ◽  
Warrick J. Couch ◽  
Richard S. Ellis ◽  
Ray M. Sharples
Keyword(s):  
Hubble Space Telescope ◽  
Rich Cluster ◽  
Space Telescope ◽  
The Rich
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