1. WIYN Observing Program Overview The WIYN 3.5m telescope began science operations at Kitt Peak on 15 July 1995. The current median WIYN delivered image quality is 0.8" FWHM at R. WIYN delivers images (in the R band) 0.7" or smaller 25% of the time and 0.6" or smaller 10% of the time. This state-of-the-art alt-az telescope has a wide-field CCD imager and wide-field multi-object fiber spectrograph (MOS/Hydra) mounted at its two Nasmyth foci. The imager can be replaced by an optical fiber array (DensePak) for integral field spectroscopy. NOAO is allocated 40% of WIYN telescope time by the WIYN (Wisconsin-Indiana-Yale-NOAO) Consortium; roughly 9 - 12 nights per month. Approved WIYN programs will be scheduled in two modes: classical mode, where PIs are assigned specific nights, and in queue mode, where observations are carried out by the WIYN Queue Program staff. Program assignment to classical or queue modes will be made after proposals are reviewed by the TAC and the KPNO Director. The availability of the queue observing mode and the opportunity to obtain data for small programs permits broader access by the community to KPNO facilities. Operating in a queue mode also allows NOAO to develop new observing strategies for application to the Gemini 8m telescopes. Further information about the WIYN Observing Program can be found on-line at http://www.noao.edu/wiyn/obsprog. We are now soliciting WIYN proposals for the second semester of 1998 (1998B; 1 August 1998 - 31 January 1999). Proposers should use the standard NOAO observing proposal form, including the Target Tables to provide a detailed summary of their observational program. All proposers must complete the Target Tables for WIYN programs. The new proposal forms are available via ftp to ftp.noao.edu, cd noaoprop, or you can use the new Web-based submission process at http://www.noao.edu/noaoprop/. Please follow the application instructions carefully. After proposals are accepted and placed in the NOAO WIYN queue, investigators are encouraged to submit a WIYNQ form to provide information not included in the original proposal or any revisions of the observing program that will help the queue observers more efficiently execute the science program. 1.1. Supported Instrumentation NOAO supports the two major WIYN facility instruments: the WIYN CCD Imager and the Hydra Multi-Object Spectrograph (MOS/Hydra). The telescope is able to to switch quickly (10-20 min) between these two instruments. NOAO also supports the DensePak fiber array for bright time programs only. Use of DensePak requires the removal of the CCD Imager and switching between these two instruments will not be allowed during the night. 1.2. Supported Observing Program Types Observing programs of all lengths will be accepted for review. Long Programs (which require more than 2 hours of telescope time) will be reviewed by the normal external KPNO TACs and ranked by scientific merit. When estimating how much telescope time to request, please take into account observing overheads as well as integration time. Approved Long Program proposals will be scheduled either classically or in queue mode, subject to review by the KPNO Director. Short Programs (i.e., 2hr queue; those requiring less than 2 hours of observing time) will be reviewed by an internal KPNO TAC. The goal of a typical Short Program could be to obtain a small dataset to complete a larger project, assess the feasibility of a particular type of observation before the submission of a Long Program proposal, or it could be a short, self-contained program. Individual Short Program investigators will be allocated a maximum of three separate Short Program proposals per semester (i.e., a maximum of 6 hours of WIYN time). The 2hr queue programs submitted by a particular investigator must be scientifically distinct from each other (i.e., 2hr queue proposers will not be allowed to submit more than one proposal per area of inquiry per proposal cycle). All approved Short Program proposals will be scheduled in queue mode. A maximum of two hours of WIYN time can be requested per Short Program proposal. If your program is simple, we will absorb the standard observing overhead (e.g., CCD read-down times, target acquisition times, etc.) However, if your program is more complicated, you must include observing overhead into your time request. In short, your program must fit within two hours, including observing overhead. 1.2.1. Target of Opportunity Programs In addition to preplanned observations, we will consider making Imager observations of targets of opportunity. These might include such objects as supernovae, gamma ray bursters, comets, variable stars or other objects that are exhibiting unusual behavior. Because queue observations are scheduled dynamically, targets of opportunity can be inserted into the queue program with minimum impact. However, because projects that have been judged scientifically important will be delayed, we will also require a short scientific justification for observations of targets of opportunity. MOS/Hydra and DensePak Target-of-Opportunity observations will not be allowed at this time. We can accommodate target-of-opportunity proposals which adhere to the following procedure: 1. Proposals for targets of opportunity must be submitted on the standard NOAO LaTeX template form but with the scientific justification limited to 250 words. The LaTeX Target Table addendum form must also be submitted. The justification should mention why immediate observations are required and over what time scale the observations would be interesting. 2. Any proposal approved before 2 PM MST on a day during which observations will be made may be scheduled for that night. Proposals will be reviewed by the KPNO Director for priority and the WIYN queue observing team for feasibility before they are scheduled. 1.3. Miscellaneous Queue Program Information Proposers should remember that not all observing time will be photometric with 0.5" seeing and should consider submitting proposals that take this into account. It is important to us that we deliver the highest possible quality data. If we are not confident that we have achieved your figure-of-merit or if testing your data requires substantial processing, we will contact you as quickly as possible to determine the best course of action. In particular, we will probably request a location where we can deposit a data sample via anonymous FTP so you can assist us in assessing your data. In the event this becomes necessary, we will send you more complete instructions. Successful observations will be made available to the program principal investigator as quickly as possible. Typically, data will be sent to the principal investigator in FITS format on Exabyte tapes within seven (7) working days of completing their program. Smaller data subsets may be transmitted earlier to the principal investigator as appropriate. To protect proposers' access, data will not be available from NOAO via anonymous FTP. Instead, such transfers will be from NOAO to a site designated by the principal investigator. 1.4. Final Comments The WIYN observing program is still evolving and we know that we haven't thought of everything. We are very interested in comments and suggestions concerning any aspect of the WIYN Queue process. In addition, we realize that not all observing projects lend themselves to the queue approach and this is why some programs are scheduled classically. The main goal of the WIYN queue observing experiment, however, is to empirically test the hypothesis that in the face of a high over-subscription rate, the science throughput of WIYN can be maximized by executing the most highly ranked science programs first, completing programs in a timely manner, allowing a larger range of program lengths, and matching the observing program to the observing conditions on an observation-by-observation basis. For a progress report on this experiment, please see recent NOAO Newsletters. This report is also available on the WIYN Observing Program WWW homepage. If you have specific questions or comments about the WIYN observing program, please send them to the NOAO SCience OPErations Director's office (noao@noao.edu). 1.5. Further Information General information is available from the WIYN Observing Program homepage. Questions about expected instrument performance of MOS/Hydra and DensePak should be directed to Paul Smith (psmith@noao.edu) or Sam Barden (sbarden@noao.edu); questions about the WIYN Imager should be directed to Abhijit Saha (asaha@noao.edu) or Paul Smith; questions about WIYN operations status and queue observing should be directed to the WIYN Queue Program address (wiynq@noao.edu). 2. WIYN Observing Program Application Instructions Applying for WIYN observing time requires submitting a regular NOAO observing proposal form with completed Target Tables giving the observing details of your program. These forms can be acquired in the following ways: Application Forms Locations Type Location Instructions WWW http://www.noao.edu/noaoprop/ . Anonymous FTPftp.noao.edu cd noaoprop E-mail noaoprop-request@noao.edu send e-mail to this address Paper NOAO SCience OPErations Division Call (520) 318-8397 The proposal forms are designed to be processed by LaTeX macros. Briefly, the proposal form consists of a series of keywords followed by fields in which you fill in the information. After editing this information into the form, you may produce a hardcopy by running it through LaTeX and sending it to your laser printer. Proposers will be told how to submit MOS/Hydra fiber configuration data after the proposal review process is completed. Further instructions about submitting NOAO observing proposals are available via anonymous FTP (ftp.noao.edu (cd noaoprop; get README)) or on-line (http://www.noao.edu/noaoprop/). Questions about the application process should be directed to the NOAO SCience OPErations Director's office (noao@noao.edu). 2.1. Important Notes for the NOAO Proposal Form 1. If you are applying for Long Program observations, specify "WIYN" as the telescope. 2. If you are applying for Short Program observations, specify "WIYN---2hr" as the telescope. 3. Short Program scientific justifications should be a half page or less in length. 2.2. Important Notes for the WIYN Target Tables Please remember that we need enough information to evaluate your program fairly during the TAC process. But also keep in mind that if you are allocated queue time, you will get the chance to submit a WIYNQ observing form, giving more information if necessary. So be as brief as possible without selling your program short. Explicit and detailed instructions on how to execute your program are not needed initially. Programs which adhere to the published Imager, MOS/Hydra, and DensePak default operation and calibration procedures do not have to provide additional commentary in the Experimental Design section of the proposal. However, if your proposed program requires significantly different observing procedures, please explain why in the Experimental Design section. Please review the observing overheads page for further information. If your program requires a specific set of objects, you must clearly justify this in the Science Justification section of the main proposal form. For example, you may need to observe M15 to test your hypothesis, and no other globular cluster will do. However, if you are awarded time in the queue but with relatively low grade, your objects may set before we make enough progress on higher ranked programs to schedule your program. On the other hand, many programs do not require specific objects but want to observe a representative set. For example, you would like to observe four Abell clusters but it doesn't matter which four clusters are observed. An example fictional sample (e.g. "Cluster A, Cluster B, Cluster C, etc.") complete with typical instrument configuration information (filters, gratings, required exposure times, number of exposures, etc.) must be specified in the Target Tables. You should state clearly in the Scientific Justification and/or the Experimental Design sections of the main NOAO proposal form why your sample needs to be the size you propose. If you are allocated queue observing time, you will be asked to submit your real sample when (and if) your program is scheduled. However, if your mid-semester object selection conflicts with objects and instrument configurations in a different program specifically reviewed by the TAC, you will be asked to select a different target or justify why we should repeat the observation. Also, your revised program will have to fit within the amount of time you are allocated. Note that some sample flexibility will increase the probability that programs with lower TAC grades will be executed since they must be scheduled around programs with higher grades. All WIYNQ forms and revised WIYN Target Tables submitted after WIYN observing time is allocated are subject to review and approval of the KPNO Director. A note to Hydra proposers: you do not have to specify the celestial coordinates of every object in every configuration in your Target Tables. You merely have to tell us the approximate celestial coordinates of the field center for each proposed configuration. It is important that you specify a PER EXPOSURE data quality figure-of-merit in the Experimental Design section of the proposal and in any subsequent WIYNQ form submitted (i.e., a quantitative measure of whether an individual exposure has met your technical goal). Example figures-of-merit include: * S/N per pixel at a specified wavelength * how well two lines were split at a given wavelength * number of detections above sky per configuration Your figure-of-merit could be some combination of these examples or something else entirely. Please be specific. MOS/Hydra and DensePak twilight sky observations are important for radial velocity calibration and potentially for other programs. If your MOS/Hydra or DensePak program requires that twilight sky observations through all fibers be obtained at dusk and/or dawn for calibration purposes, you should request and justify these observations in the Experimental Design section of the proposal. We will NOT automatically observe spectrophotometric and radial velocity standards for MOS/Hydra and DensePak programs. You should note that you will require standards in the Experimental Design section of the proposal and include an overhead estimate for each such observation in your time request. Full information on standards (or choice of standards) you wish to have observed needs to be included on the WIYNQ form if this information is not explicitly included in your proposal. 3. MOS/Hydra Information 3.1. General Information A general description of the instrument may be found in the Hydra/WIYN Users Manual, available on-line as an HTML document, via anonymous FTP, or from the KPNO Observing Support Office. Hydra/Bench Characteristics at WIYN |--------------------------------------------------------------------| | Full unvignetted field | 60 arcmin | | diameters | | |-------------------------------|------------------------------------| | Fiber diameters | 3 arcsec (blue fibers) | | | 2 arcsec (red fibers) | |-------------------------------|------------------------------------| | Fibers available | 96 blue fibers | | | 96 red fibers | | | 12 field orientation probes | | | 84 locations for future fibers| |-------------------------------|------------------------------------| | Minimum fiber separation | 37 arcsec | |-------------------------------|------------------------------------| | Configuration time | 20-25 minutes | |-------------------------------|------------------------------------| | Measured positioning | 0.33 arcsec (30 um) | | accuracy | | |--------------------------------------------------------------------| |--------------------------------------------------------------------| | Grating | 316 line/mm, blaze angle 7 d | | | 400 line/mm, blaze angle 4.2 d | | | 600 line/mm, blaze angle 13.9 d | | | 860 line/mm, blaze angle 30.9 d | | | 1200 line/mm, blaze angle 21.1 d | | | 316 line/mm echelle, blaze angle 63.4 d | |--------------|-----------------------------------------------------| | Cameras | Red: (all-refractive 285mm focal length bench cam.)| | | Blue: Simmons camera (381 mm focal length) | |--------------|-----------------------------------------------------| | Collimators | 6 inch f/6.7 paraboloid | |--------------|-----------------------------------------------------| | Detector | 2048 x 2048 thinned Tektronix CCD (24 um pixels) | |--------------------------------------------------------------------| More detailed information, including grating efficiency curves, can be found in the Hydra/WIYN User's Guide. Information about the red camera is available on-line. Queries about this camera should be directed to Taft Armandroff (tarmandroff@noao.edu). A setup program is also available for defining the spectrograph configuration and planning observations. The setup program is available via anonymous FTP. 3.2. Default MOS/Hydra Operation and Calibration Procedures MOS/Hydra proposers should keep the following queue observing default operation and calibration procedures in mind when filling out their proposals. 3.2.1. Default Operation Procedures (1) The default mode of operation for the Bench Spectrograph CCD will be to read out the entire CCD with no on-chip binning at the default gain of 1.7 electrons/ADU. (2) The number of spectrograph grating and camera configurations per night will be constrained as follows: (a) we will not change cameras at night; (b) we may change gratings but not between the echelle and some other grating; and (c) we may change the grating tilt. (3) We will observe objects at airmasses of 1.5 or less unless: (a) advised that observations at higher airmass are acceptable; and (b) the objects never get above 1.5 airmasses. (4) All target fields within your program will be assumed to have equal priority UNLESS you specify otherwise in the "Comments". 3.2.2. Default Calibration Procedures (1) We will take 9 full bias frames at the start of each night. (2) Comparison lamp exposures will be taken before and after a series of program exposures on a given night with a specific fiber Hydra configuration. (3) Dome flat exposures will be taken at least once per fiber Hydra configuration. A minimum of three flats will be obtained. (4) In addition, we will observe spectrophotometric, radial velocity, and other user-specified standards as requested. However, these will be considered part of the approved program and must fit within the allocated time. See observing overheads discussion. 4. WIYN Imager Information 4.1. General Information The current Imager detector is S2KB, a thinned Tek/STIS 2048x2048 CCD with 21 micron pixels. The default gain is 2.8 electrons/ADU. The read noise is roughly 8 electrons RMS. The plate scale is 0.195 arcsecs/pixel yielding a field-of-view of 6.8 x 6.8 arcmins. The median R-band WIYN Delivered Image Quality (DIQ) for the period June 94 to present is 0.8" FWHM. The median R-band DIQ was 0.7" FWHM or less 25% of the time and 0.6" FWHM or less 10% of the time. We are confident that for nights with DIQ of 0.6" or larger, closed-loop guiding does NOT degrade the DIQ. We do NOT have enough data yet to understand the impact of our current closed-loop guiding system for nights when the DIQ is 0.6" or less. Standard Harris UBVRI (w001 - w005) and Gunn uvgri filters (w006 - w011), as well as three narrow-band H-alpha filters (w012 - w014), are available. Further information about these filters including filter characteristics and transmission curves are available via anonymous FTP (ftp ftp.noao.edu). Other filters may be available from the KPNO collection by specifying the needed filters in the Target Table of the observing proposal. Investigators may provide special filters as well. We can support square 2 x 2 inches and 4 x 4 inches filters without special notification. If your filters are not square or not one of these sizes, please note that in your proposal. Based on extensive testing, we have concluded that for the UBVRI filter set, domeflats work better than twilight flats when tested against the nightsky. We will acquire only dome flats as part of the default calibration process (see below). Queue program investigators may request twilight flats if they desire them. We do not have enough data to draw conclusions about flat-fielding through the Gunn filters, but expect this to be similarly true. S2KB has significant (1%) fringing in Harris I. Observers desiring Harris I or Gunn i data should indicate if fringe correction frames are needed. The telescope pointing accuracy is about 10 - 15 arcsecs RMS all-sky but less than 1 arcsec RMS for offsets. 4.2. Default Imager Operation and Calibration Procedures Imager proposers should keep the following queue observing default operation and calibration procedures in mind when filling out their proposals. 4.2.1. Default Operation Procedures (1) The default mode of operation for the Imager CCD will be to read out the entire CCD with no on-chip binning at the default gain of 2.8 electrons/ADU. If you require a different mode of operation, please specify the desired mode and justify it in the Experimental Design section of the observing proposal. (2) If multiple exposures of the same field with the same filter are specified, we will: * take all these exposures consecutively * dither the telescope 10" North, South, East, or West between each exposure unless otherwise specified. * if MANY exposures are requested, we will dither in a grid pattern with a grid point spacing of 10" (3) All target objects within your program will be assumed to have equal priority UNLESS you specify otherwise in the "Comments". 4.2.2. Default Calibration Procedures (1) We will take 9 full bias frames at the start of each night. (2) We will take five (5) domeflats through each active filter during the preceding afternoon or following morning. (3) We will take twilight flats for any program which requires large scale flat fielding although we cannot guarantee that they will be taken the night of the program exposure. Note that domeflats appear to work better than twilight flats at WIYN (see comments above). (4) We will only use 3 - 5 filters per night. (5) Photometric programs will be calibrated using a minimum of 12 Landolt (approximate color range: -0.2 <= B-V <= 1.5), Gunn, or KPNO Spectrophotometric standards, depending on the active filters. (6) We will observe objects at airmasses of 1.5 or less unless: (a) advised that observations at higher airmass are acceptable; or (2) the objects never rise above 1.5 airmasses. (7) In addition, we will observe user specified standards as requested. However, these will be considered part of the approved program and must fit within the allocated time. These standards MUST be listed as targets in the Target Tables and should be cross-referenced to their program fields they are calibrating. Please indicate the frequency and timing relative to program objects of special standard star observations. 5. DensePak Information 5.1. General Information Please Note: DensePak is currently limited to bright time use only. In addition, 3 fibers have been damaged during the past 6 months and there are now a total of 5 unusable fibers in the array. DensePak is a fiber optic bundle that forms an array of 91 fibers in a 7x13 rectangle. Each fiber is 300 microns in diameter which corresponds to 3 arcseconds on the sky at the Nasmyth focus of the WIYN telescope. Fiber-to-fiber spacing is 400 microns and the overall dimensions of the array are 30 arcsec x 45 arcsec. The array's orientation on the sky can be selected by setting the instrument rotator to the proper offset angle. Additional fibers are offset from the array corners and serve as sky fibers. The four sky fibers are located roughly 60 arcsec from the array center. The proximity of the sky fibers to the array may necessitate moving the telescope off target to properly sample the sky depending on the angular size of the target. Sky fibers have the same diameter as those in the array. DensePak's fibers have transmission characteristics similar to the Hydra "red" fiber cable. At present, four fibers in the array are unusable. In addition, the throughput of several fibers at wavelengths < 4500-5000 Angstroms has been found to be substantially lower than that found for the majority of fibers in the array. DensePak's fiber bundle feeds the WIYN Bench Spectrograph. Therefore, users have the same spectroscopic options for DensePak as offered for Hydra (see the Hydra Users Manual which can be found at http://www.noao.edu/kpno/manuals/hydraman/hydrawiynmanual.html). Summary of DensePak/Bench Characteristics at WIYN |-------------------------------|------------------------------------| | Fiber array dimensions | 7 fibers x 13 fibers | | | 30 arcsec x 45 arcsec | |-------------------------------|------------------------------------| | Fiber diameter | 3 arcsec | |-------------------------------|------------------------------------| | Fibers available | 89 "red" fibers - transmission| | | characteristics similar to the| | | red fiber cable used for Hydra| | | 2 unusable fibers in the array| | | 4 sky fibers | |-------------------------------|------------------------------------| | Fiber separation | 4 arcsec | |-------------------------------|------------------------------------| | Sky fiber location | 60 arcsec from array center | |-------------------------------|------------------------------------| |--------------------------------------------------------------------| | Grating | 316 line/mm, blaze angle 7 d | | | 400 line/mm, blaze angle 4.2 d | | | 600 line/mm, blaze angle 13.9 d | | | 860 line/mm, blaze angle 30.9 d | | | 1200 line/mm, blaze angle 21.1 d | | | 316 line/mm echelle, blaze angle 63.4 d | |--------------|-----------------------------------------------------| | Cameras | Red: (all-refractive 285mm focal length bench cam.)| | | Blue: Simmons camera (381 mm focal length) | |--------------|-----------------------------------------------------| | Collimators | 6 inch f/6.7 paraboloid | |--------------|-----------------------------------------------------| | Detector | 2048 x 2048 thinned Tektronix CCD (24 um pixels) | |--------------------------------------------------------------------| Information about the red camera is available on-line. Queries about this camera should be directed to Taft Armandroff (tarmandroff@noao.edu). A setup program is also available for defining the spectrograph configuration and planning observations. This program is available via anonymous FTP. When running the spectrograph setup program, investigators should choose the blue cable to match the fiber diameter with that used in DensePak. 5.2. Default DensePak Operation and Calibration Procedures DensePak proposers should keep the following queue observing default operation and calibration procedures in mind when filling out their proposals. 5.2.1. Default Operation Procedures DensePak will have a significant impact on the planning and operation of the WIYN Queue program because DensePak and the WIYN Imager use the same instrument port. Given the delicacy of the two instruments and the amount of time necessary for an instrument change, DensePak and the imager will not be swapped during nightly operations. To minimize conflict with the imager, DensePak is only offered for use during bright time. The default mode of operation for the DensePak is the same as that described for MOS/Hydra (section 3.2.1). 5.2.2. Default Calibration Procedures The default calibration for DensePak is the same as for MOS/Hydra (section 3.2.2). 6. Estimating WIYN Observing Overheads When requesting WIYN observing time, please use the following rules to account for the observing overhead required to execute your program. That is, your total requested program time should include your estimated total integration time and your estimated total overhead time. Important 2hr Queue Note: You must fit your entire program into two (2) hours maximum. However, we will absorb some of the overhead for your program. Where appropriate, this is noted in italics. Current overhead estimates are as follows: You must add 2.5 minutes for every requested exposure. This overhead charge compensates for the CCD read-down time. For example, if you are requesting six program exposures, please increase the total requested time by 15 mins. Two-Hour Queue proposers: you get three (3) "free" readouts. You must add five (5) minutes for every requested target. This overhead charge compensates for the target acquisition time. For example, if you request four target fields, add 20 mins to your total requested time. Two-Hour Queue proposers: you get two (2) "free" targets acquisitions. You must add 45 minutes per Hydra fiber configuration (except when using the echelle grating, as discussed below). This overhead compensates for fiber positioning time (roughly 25 - 30 mins) and calibration time (roughly 15 mins for most gratings). Two-Hour Queue proposers: you get one (1) "free" fiber configuration. When using the echelle grating, please add 60 minutes per Hydra fiber configuration. Programs that require photometric calibration should add two (2) hours for every eight (8) hours of program (integration+overhead) time. Note that this is an underestimate of the actual time required but we always try to spread this overhead over several projects whenever possible. Two-Hour Queue Imager proposers: we will absorb your photometric calibration overhead. Hydra and DensePak programs which require night-time radial velocity standards must add 15 mins per standard. If using the echelle grating, please add 30 mins per standard. We will continue to absorb all focusing overhead for now. Questions about these overhead estimates should be directed to Abhijit Saha (asaha@noao.edu). 7. Submitting a WIYN Queue Form Beginning with the 1998A (Spring 1998) semester, proposers have not been required to submit a WIYN Queue (WIYNQ) form along with their observing proposal. Instead, proposers have been required to complete "target tables" as part of their proposals which outline their observing programs. However, the WIYNQ form is still availible to provide the WIYN queue team with more detailed information about an observing program and any necessary, nonstandard calibrations, or alert the team of any revisions to the observing program that you request. In fact, we highly recommend that you submit a WIYNQ form if you need to revise any technical information that was included in your original accepted proposal. If you feel that your proposal lacks any information that would improve our ability to obtain the science data and calibrations that you require, please submit a WIYNQ form. The LaTeX template file (wiyn_qform.tex), .sty file (wiynq15.sty), and a sample WIYNQ form (wiyn_qsample.tex) can be found at http://www.noao.edu/wiynq/obsprog/proginfo/WIYNQ. WIYNQ forms should be submitted to wiynq-submit@noao.edu. Questions about the WIYNQ form should be directed to wiynq@noao.edu. 8. EMAIL ADDRESSES Requests to receive the electronic NOAO proposal form should be sent to noaoprop-request@noao.edu. Completed proposals should be sent to noaoprop-submit@noao.edu. General questions about KPNO observing proposals should be sent to noaoprop-help@noao.edu. Specific questions about the WIYN queue observing experiment should be sent to wiynq@noao.edu. MOS/Hydra and DensePak contacts: Paul Smith (psmith@noao.edu) and Sam Barden (sbarden@noao.edu). WIYN Imager contact: Abhijit Saha (asaha@noao.edu). Paul Smith February 23, 1998