All proposals from Canada and France for Semester 2001B must use the electronic proposal system operated by the Canadian Astronomy Data Centre. The Phase One Observing Proposal SYstem (POOPSY) is an electronic submission system which uses a standard Web browser but is based on LaTeX, a familiar formatting language. Consult the Users Guide for more information.
 
 
 

Some important notes:

• CFH12K will again be operated in QUEUED SERVICE OBSERVING (QSO) mode in Semester 2001B. Please consult the Queue Scheduling pages for information regarding this program. QSO is the default mode for CFH12K observations...

• OSIS IR in its new configuration (using CFHTIR as a detector) will be offered to the community for the second half of 2001B on a shared risk basis. OSIS IR won't have been commissioned before the end of the 2000B proposal period, though it is likely to be available for the second half of 2001B.

• OASIS is scheduled to leave CFHT at the end of April 2002. If you have, or plan to start, an observing program with OASIS at CFHT, please take this element in consideration while preparing your proposal.

• The F/35 upper end is no longer available. Neither FTS in its present configuration nor visitor instruments using the F/35 upper end can be scheduled at CFHT anymore.

• The STIS2 detector is no longer available. Though replacement solutions are under study, none is clearly identified yet. Please read carefully the on-line information on MOS and OSIS before selecting the detector you want to use (EEV1 or Loral3).

Instrument Availability

CFH12K   (Contact Jean-Charles Cuillandre (jcc@cfht.hawaii.edu) for information)

Consult the updated CFH12K Web pages for detailed information on the characteristics and performances of the camera.

CFHTIR    (Contact Thierry Forveille (forveille@cfht.hawaii.edu) for more information)

GECKO/CAFE   (Contact Nadine Manset (manset@cfht.hawaii.edu) for more information)

There is no shortage of potential CCDs available for Gecko in 2001B. Beside Loral3 which is a thick 2K x 2K device with 15 micron pixels, EEV1 is available. EEV1 is a 2k x 4.5k device with 13.5 micron pixels. A short summary of device characteristics is:

Loral3: Low Q.E. in blue but the only device which will not have fringing in the red. Read noise around 9 electrons

EEV1: Reasonably high Q.E. from 3000A onward with fringing beyond 7000A or so. Read noise of 3 electrons and 15 seconds of readout time.

MOS   and OSIS-V    (Contact Eugene Magnier (magnier@cfht.hawaii.edu)for information)

OSIS-V is a visible spectrograph covering a 3.6x 3.6 arcmin field.
OSIS fast guiding is working reliably. Images with  0.39" FWHM using the fast guiding have been obtained with OSIS-V.

With the fatal failure of STIS2, EEV1 is the detector of choice for both MOS and OSIS. If the fringing in the red is a problem for the observations, the old Loral3 could still be used. The latest news on MOS and OSIS can be found here.

A summary of the grisms and filters available for MOS and OSIS is available.

The ARGUS mode of MOS is no longer offered (see OASIS).

OASIS   (Contact Pierre Martin (martin@cfht.hawaii.edu) for more information)

EEV1and Loral3 are the two detectors available for OASIS. Check the  latest news on OASIS...

Note that most of the programs which could have been performed with MOS-ARGUS can use OASIS instead.

OSIS-IR (Contact Eugene Magnier (magnier@cfht.hawaii.edu) for information)

OSIS-IR is proposed for the second half of 2001B on a shared risk basis. CFHTIR will be the detector used in this mode. As OSIS-IR won't be tested on the sky before May 2001 (if not later), no on-sky test data are available for this instrument yet... You can look at the OSIS information for a reminder on the previous OSIS-IR configuration (with the redeye detector).

PUEO  (Contact Olivier Lai (lai@cfht.hawaii.edu) for information)

For observations in the visible, FOCAM and a standard CCD are available. There are two modes available for FOCAM with AOB with and without a focal enlarger. Pixel scales are 0.022 or 0.044 arcsec in the visible for Loral 3, with and without the focal enlarger respectively.

NOTE: The GRiF K-band integral field spectrograph will be available on a shared risk basis. What modes will be available will depend on the integration schedule. Currently, KIR can be operated with the Fabry-Perot (R=1800).
The next steps will be the integration of the grism in the filter wheel and the focal plane wheel, which will allow long slit specroscopy with a resolution of R~500. If these two modes are integrated together, the integral field spectrograph will be operationnal. Please check the PUEO web page for the latest news on these developments.

Detectors

Available detectors

CCDs

• Loral3, 2k x 2k thick CCD, 15 micron pixels - no fringing in the red
• EEV1, 2k x 4.5k thin CCD, 13.5 micron pixels (Gecko, OASIS, MOS, MOS/FP and OSIS)

IR Detectors

• The KIR camera which incorporates a 1024 x 1024 Rockwell NICMOS chip with 18.5 micron pixels is available for use with AOB
• CFHTIR is the new IR camera, used for science since the beginning of 2001.