CFHT Observation Proposals
|The 2017B call for proposals will open Tuesday Feb 21 at 23:59:00 UTC and
close Tuesday March 21 2017 23:59:00 UTC.
CFHT adapted the Northstar Phase 1 tool written initially for the
Radionet community. Northstar has been ported to CFHT and modified in
house to handle our specific requirements. You can access the CFHT Phase
1 tool here during the
call for proposals period or if you are interested in submitting a
Director Discretionary time proposal.
|If you are interested in applying for Gemini time through the CFHT-Gemini time exchange program, please follow this link.
|Information on 2017B [1 Aug 2017 - 31 Jan 2018]
Estimated time allocations
The 2017B share of observing time is not firmly established yet. This
allocation assumes that the associate partners, China and Taiwan, use all
their available nights. This semester's allocation also takes into
account the shutdown of the telescope that is scheduled from Aug 1 to 10
Canada: A minimum of 31 nights (outside the 2017-2019 Large Programs)
France and Opticon: A minimum of 31 nights (outside the 2017-2019 Large Programs).
Of these 31 nights, 2 are offered to Opticon H2020 program through the OPTICON proposal system.
University of Hawaii: A minimum of 15 nights (5 nights are allocated to the 2017-2019 Large Programs).
Taiwan: Up to 10 nights.
China: Up to 15 nights.
Approximate RA pressure from Large Programs.
During the semester 2017B, Large Programs
will be using the RA ranges in the table below. During the semester 2017B, there are 95 dark nights available with the Moon illumination less or equal to 50%, and 89 bright nights when the Moon illumination greater than 50%. The dark time is split between MegaCam and SITELLE and the bright time between ESPaDOnS and WIRCam.
New ESPaDOnS overheads.
Starting in February 2017, ESPaDOnS's detector Olapa has been switched
to its 2amp mode. The readout times and overheads have been cut in
half. When calculating your overheads, please use 33s in Slow readout
mode, and 20s for the Normal and Fast readout modes. The higher gain in
Fast mode (1.5 e/ADU compared to 1.2 e/ADU in Normal mode) allows
integrating longer on a bright target before the detector saturates,
but the readout noise is higher (between 3.1 ADU and
4 ADU for each amp in Fast mode, compared to 3.2 to 3.0 ADU in
SNR-QSO is now the default mode for MegaCam and ESPaDOnS and PIs who want to opt-out of this mode must justify it in their proposal. SAC recommendation #6
of the May 2016 report states: SNR-QSO should become the default mode for MegaCam and ESPaDOnS starting 2017A. Program requesting classical mode should justify their request
For more information about the SNR-QSO mode, please see the SNR-QSO web page
Other references to the SNR-QSO mode:
- SPIE 2016 paper, Devost et al.
- SF2A paper on Espadons by Moutou et al., section 2 covers SNR-QSO
- ADASS 2013 paper, Cuillandre et al.
MegaCam filters availability.
Only the new MegaCam filters will be available for 2017B. Programs cannot request the use of old filters. Recommendation #5 of the may 2015 SAC report states: SAC recommends that the filter selection offered to MegaCam users be rationalized. Programs should use the new filter set, unless a strong scientific case is made in the proposal for the need of the old filters. SAC also recommends that the old filters be decommissioned in the medium-term and not available in semester 17A and beyond. The CFHT user community should be informed of this policy before the 16A proposal call.
New WIRCam overheads.
Starting in 2017A, new overheads will be charged to the science programs
for WIRCam observations. The Wide Dither Pattern (WDP) will now charge
30s of overheads per exposure. Please note that the overheads for the
small Dither Pattern (DP) remain at 10s per exposure.
New PH1 rule.
The PH1 system has been changed to have users include the values of the exposure time calculators into their proposals. Proposals cannot be submitted if this field is not filled. This is not counted toward the page charge.
Exposure time calculators.
A feature has been added to the MegaCam and WIRCam ETC: there is now a galaxy profile mode, in addition to the previous point-source and extended source modes. This new mode corresponds to galaxies more extended than a point-source, but where the seeing still matters. The galaxy profile itself is based on Sersic profiles with indices varying from 1 (exponential disks) to 5 (4 corresponds to de Vaucouleurs’ profiles, typical of elliptical galaxies). The width of this profile is settled by the half-light radius, given in arcsec. The galaxy profile is then convolved with the seeing profile to make the exposure time or signal-to-noise ratio computations. This new feature is intended to replace the “galaxy" choice in the previous ETC. For larger galaxies where the seeing does not matter, you can either use the galaxy mode with a large half-light radius, or the extended source mode if you plan to reach a given surface brightness in the outskirts of the galaxy. Should a replacement for the previous “nearby galaxy” mode be needed, we can easily add it in the future. See the ETC web pages of each instrument for details.
All agencies are invited to encourage their community to submit snapshot programs. These programs must be able to accept an Image Quality worse than 1.2" or significant levels of extinction. Snapshot programs are used not only during bad weather conditions but also to fill gaps in the queues when no A, B or C program are available or suitable. Snapshot programs are not counted toward an agency's allocation.
WIRCam staring mode.
For investigators interested in using the staring mode with WIRCam, please be advised that systematics may be present that limit the achievable accuracy using differential photometry. RMS values <= 0.1% are possible but reaching 0.01% is challenging. See Croll et al (2015) for details. Also, experiments switching back and forth between two filters should be considered risky.
More details on Large Programs.
A new set of Large Programs has been accepted starting 2017A. See recommendation #8 of the May 2016 SAC meeting.
CFHT will flag any proposal which has conflicts in RA and observing conditions with an existing LP. For information about the relative priority of PI programs and Large programs, please see the
recommendation from the SAC (Nov. 2009).
If you wonder about the pressure on telescope time, the relative requests on the main instruments, you can have a look at some graphs for past rounds of proposals here.
|Information on previous semesters
Good luck and clear skies!