CTIO  >  YALO (1-m Telescope)

The YALO 1-m Telescope


PLEASE NOTE! THE YALO 1.0-M PROJECT FINISHES OPERATIONS ON SEPTEMBER 2 2002. FOR 2003A, ANDICAM IS MOVING TO THE 1.3-M.

Time Allocation Instrument Details Proposal Preparation Data Product Info

The YALO 1-m telescope at CTIO is operated by a consortium consisting of Yale, AURA, (U. of) Lisbon, (Portugal), and Ohio (State University). The YALO telescope is run in queue mode, with observers provided by CTIO. The instrument is a permanently-mounted, dual-channel, optical-IR imager called ANDICAM, built at Ohio State by a group led by Darren DePoy.


For a brief summary of the observing parameters with ANDICAM (including filter transmission curves), click here.

YALO queue observations with the optical detector have been carried out successfully since the 1998B semester. The IR array was installed in July 1999, enabling simultaneous optical and infrared imaging, including dithering in the IR channel while the optical channel integrates. Please check the Ohio State YALO Telescope & Instrument News wepage and the following links for the most recent instrument news.

Latest IR channel news Latest optical channel news

Nick Suntzeff's data reduction webpage contains useful hints on YALO data reduction as well as measured color terms.

Proposals for observing time should be submitted using the standard NOAO observing form, and will be evaluated in the same way as all other proposals submitted to NOAO. Since the YALO telescope provides a queue/service/ target-of-opportunity observing capability not available on most other CTIO telescopes, preference will be given to (a) proposals for synoptic programs where a few frames per night will yield significant scientific benefits, or (b) proposals which require < 10 hours observing time total. Programs which require a large fraction of a given night are strongly discouraged and should be carried out at the 0.9m telescope in the "classical" observing mode. Successful proposals have to avoid duplicity with programs being pursued by the other YALO partners. Click here for a list of the YALO partner observing programs.

The requested amount of observing time should be given in minutes per night and has to include an estimate for the overheads (readout: ~80 sec for a single 2048x2048 CCD image; slew to target and acquisition: ~3 minutes per target).

Once a project has been approved for observing with YALO, the PI needs to submit a detailed "Phase II" observing plan to the queue manager. This plan consists of a set of observations to be carried out, each "unit" observation of which is described by one or more data-acquisition template files. The observing plan has to be created by following the instructions for the "Phase II" Preparation & Electronic Submission forms.

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Data will be distributed via ftp (data can be distributed via tape upon request, however, the cost of the tapes will have to be paid by the PI). PIs will be notified by email when data are available and where to retrieve them. PIs should expect a 2-3 week delay from the time when the data are taken to when they become available. Data sets have to be retrieved from the ftp site within 5 days of notification. Please direct any inquiries regarding the data retrieval to Dr. Bailyn bailyn@astro.yale.edu with a copy to Suzanne Tourtellotte swt@astro.yale.edu. IR data will consist of combined flat fields (both lights-on and lights-off) and all on-target images. Optical data can consist of EITHER combined flat and bias files and raw data OR data processed using standard IRAF routines. The default is to process the data, the PIs have to notify Dr. Bailyn bailyn@astro.yale.edu if they prefer the unprocessed data.

The following calibration frames are obtained every night. Special processing or calibration requests will be carried out only when there is demonstrated scientific need. (note: double-binned calibrations are no longer supported !):

These individual calibration frames are subsequently combined into one bias and one flat (per filter) per night with the "imcombine" (combine = average, reject=crreject) task in IRAF. Only these combined calibration frames are passed on to the PI.

Details about the observing conditions and/or any problems encountered during the nights the data were taken can be found on the Observing and Trouble Report Archives.


YALO Webpages by other consortium members:

Some technical details about the TCS and motor systems are given for engineering purposes here

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This page was last modified on January 30 2002

swachter@noao.edu
 

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