The WIYN 3.5m will soon have a new optical imager. The One Degree Imager (ODI) will take advantage of WIYN's wide field of view as well as its excellent delivered image quality. ODI will be capable of providing actively corrected images over the entire field of view using orthogonal transfer array (OTA) CCDs. The array of ODI detectors will consist of 64 OTA CCDs, each of which will have 64 selectable cells or sub-arrays. The pixel scale will be 0.1". The initial filter set will include the Sloan u, g, r, i, and z broad-band filters as well as an Halpha narrow-band filter. Additional details about the instrument are located on the WIYN Observatory pages about ODI. The Yale/WIYN Survey web pages have additional information regarding the survey.
Yale University has committed 90 nights of its share of WIYN 3.5-m observing time and is considering adding 60 additional nights for a total of 150 nights to undertake a survey program using ODI. The survey will be made during the first three years of science operations of ODI. An important aspect of the Yale/WIYN Survey is the opportunity for members of the community to be actively involved in the project. This opportunity for community involvement is due in part to the use of TSIP funding for the instrument. The data from the survey will also be publicly available.
The plan for the Yale/WIYN survey is to cover 30 - 100 square degrees with 1-2 hours of exposure time per filter in at least three filters (most probably g, i, z) for each field. The core elements of the survey will be set primarily by the PIs at Yale. The current intention is to use the best seeing conditions for the i band imaging, with g and z bands taking up the medium seeing time. Plans for the poor seeing time are still in development. Possible extensions to the survey, currently being considered, may include greater area, depth, filter coverage, or unusual cadence for the observations of each sub-field that would benefit from being embedded into the observing strategy of the survey (which is likely to include an observing queue), without being considered part of the survey proper. There may also be add-on proposals for additional time that can take advantage of the survey without necessarily being directly involved in the initial survey. Community participation could involve work with an existing science group at Yale, creation of a new science group, development of extensions or add-ons to the survey, or contribution to technical elements of survey design.
Some of the science groups already defined at Yale are:
High-z galaxy morphology
Gravitational lensing by galaxies and clusters of galaxies
Faint galaxy photometry
Galactic proper motion
Virgo Cluster Halpha survey
Many aspects of the survey have not yet been defined, including field choice, filter coverage, depth in each filter, and cadence of observation. There is an opportunity now for the community at large to have direct effect on the entire survey and to be active participants. A workshop will be held on October 2nd and 3rd in New Haven to develop the survey and all members of the astronomical community are invited to attend. Limited financial assistance for U.S. based researchers might be available to support participation in the workshop, through application to the Director of Kitt Peak National Observatory, Buell Jannuzi (email@example.com). For more information regarding the Yale/WIYN Survey and the October meeting, please contact Tom Matheson (NOAO) and/or Charles Bailyn (Yale University).
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