MOCAM: A 4k x 4k CCD Mosaic for the Canada-France-Hawaii Telescope Prime Focus

Cuillandre, J. C.; Melliers, Y.; Murowinski, Richard; Crampton, D.; Arsenault, Robin

doi:10.1007/978-94-011-0383-1_27

Cited by 2 publications

(1 citation statement)

References 6 publications

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“…Cuillandre et al, 1995;Metzger et al, 1995;Cuillandre et al, 1996;Luppino et al, 1998). However, like any new technology it brings with it a wealth of calibration issues which were of low significance with smaller detectors (e.g.…”

Section: Calibrating Wide Field Imaging Datamentioning

confidence: 99%

Galaxy Evolution in Groups and Clusters

Lobo¹,

Roos²,

Biviano³

2003

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source• a link is made to the metadata record in Durham E-Theses• the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. AbstractIn this thesis, we investigate the extent to which galaxy evolution is driven by processes common to the group and cluster environments. A bimodality of galaxy properties such as star formation, strongly dependent upon the local overdensity of galaxies, suggests that the passive, early type galaxies common to groups and clusters originate in transformation processes, which are nurtured by the environment. This can only be important to global galaxy evolution if transformations are common in groups, which contain ^ 50% of the local galaxy population.We present deep Magellan spectroscopy and HST ACS imaging of our group and field samples at 0.3 < ^ < 0.55, selected from the CN0C2 survey by Carlberg et al. (2001b).We find that these groups contain significantly more passive galaxies than the field, with excesses of SO, elliptical and passive spiral galaxy types. The morphological composition is closely matched to that of irregular and X-ray-faint clusters at a similar epoch. In contrast with a low-redshift group sample selected from 2dFGRS (Eke et al., 2004), we find that the fraction of passive galaxies, fp, is strongly evolving in the group environment, with parallel evolution in the field population. Simple models confirm that galaxy transformations are required to match the evolution of both group and field populations. Qualitatively similar evolution and dependence on environment is found in physically-motivated simulations.However, these do not quantitatively match the environmental nor luminosity dependence in the evolution of fp. We also present a complementary method using photometric redshifts to identify infalling groups in the outskirts of clusters with Wide Field Imaging (WFI) technology.Finally,, we identify the key developments which will help to unravel the history of galaxy evolution in coming years.

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Section: Calibrating Wide Field Imaging Datamentioning

confidence: 99%

Galaxy Evolution in Groups and Clusters

Lobo¹,

Roos²,

Biviano³

2003

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CCD Mosaic Development for Large Optical Telescopes

Metzger

Miyazaki

1995

Symp. - Int. Astron. Union

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We outline the recent developments in CCD imager technology aimed at producing the very large format (8192 × 8192 pixels and larger) detector mosaics required for existing 4-m class and new 8 to 10-m class telescopes. The key technology areas include buttable array design and buttable element packaging, and optimization schemes for QE and readout time. As an example, we highlight the University of Hawaii effort to develop an 8192 × 8192 15 μm pixel CCD mosaic.

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MOCAM: A 4k x 4k CCD Mosaic for the Canada-France-Hawaii Telescope Prime Focus

Cited by 2 publications

References 6 publications

Galaxy Evolution in Groups and Clusters

Galaxy Evolution in Groups and Clusters

CCD Mosaic Development for Large Optical Telescopes

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