QSO Phase1 ESPDOnS

ESPaDOnS is a high-resolution échelle spectrograph/spectropolarimeter fiber-fed from a Cassegrain module including calibration and guiding facilities, as well as an optional polarization analyzer. This instrument offers a complete optical spectrum (from 370 to 1,050 nm) in a single exposure with a resolving power of about 68,000 (by using a slicer in a 3-slice configuration, in spectropolarimetric and 'object+sky' spectroscopic mode) and up to 80,000 (by using the slicer in a 6-slice configuration, in 'object only' spectroscopic mode).

Observers can use the following modes:

a spectropolarimetric mode in which the two orthogonal states of a given polarization - either circular (Stokes V) or linear (Stokes Q or U) - are recorded simultaneously (side by side) throughout the whole spectral range at an average spectral resolution of about 68,000
an object+sky spectroscopic mode in which the spectra of the star and of the background sky are recorded simultaneously (side by side) on the CCD detector with an average spectral resolution of about 68,000
a object only spectroscopic mode in which only the spectrum from the (bright) star is recorded, at a spectral resolution of 81,000

For details about that instrument, please see its webpage. For additional questions, please contact Nadine Manset (manset -=at=- cfht.hawaii.edu).

ESPaDOnS is offered under the Queued Service Observing (QSO) mode only. The main concept behind the QSO scheme is to perform observing programs only during sky conditions or time constraints required to meet their science goals, as defined by the investigators. This can only be achieved if the programs are all grouped together in a database and are selected appropriately according to a set of constraints, rules and sky conditions. Programs are then carried out by a well trained, local team of observers in a service mode (i.e. investigators are not present at the observatory).

Before submitting a CFHT proposal, please read the short tutorial How QSO works at CFHT. [Keywords: QSO, Regular/TOO/Snapshot programs, Deadlines, NorthStar, Exposure Time Calculators, Technical Evaluations, TAC, Ranking, QSO grade, C programs, Snapshot programs, PH2, Observations, Sky conditions, Calibrations, Night Reports, Data reduction and distribution, Proprietary period, QSO rules, Contact information.]

Starting with 2010B, CFHT is using the NorthStar Phase 1 tool. NorthStar is used by Principal Investigators (PIs) to submit their proposal(s). All PIs must register as new NorthStar users; the registration page offers a Help file if assistance is needed. To make things easier, you may use your current PH2 login information as your NorthStar login information. The login information from NorthStar is NOT transferred to PH2. After login in, Help on how to use NorthStar is available on each page.

For technical information regarding ESPaDOnS, please see the ESPaDOnS page.

B - 2013B-specific information and news [Back to Table of Content]

Starting with semester 2011A, ESPaDOnS is used with a new e2v deep-depletion detector called Olapa. Olapa gives about twice as much flux in the red than the previous detector EEV1, so make sure you use the correct Exposure Time Calculator to estimate your integration times!

Please note that during the semester 2013B, Large Programs are using the following RA ranges:

OSSOS on MegaCam : 70hrs for RA=0-4h
Matlas on MegaCam: 4hrs for RA=20-24h, 8hrs for RA=0-4h, 1hr for RA=4-8h, and 18hrs for RA=8-12h
Matysse on ESPaDOnS: 94hrs for RA=4-8h
Binamics on ESPaDOnS: 12.5hrs for RA=0-4h, 1h for RA=8-12h, 27h for RA=16-20h, 40h for RA=20-24h

For information about the relative priority of PI programs and Large programs, please see the recommendation from the SAC (Nov. 2009).

During 2009B, ESPaDOnS has been upgraded with a new triplet lens and a new Atmospheric Disperson Corrector, which brought the overall crosstalk below 1%. During that semester, CFHT has also replaced the Liquid Nitrogen cooling system by a closed-cycle system (CryoTiger).

IMPORTANT NOTE : The non sidereal tracking option (i.e., following a target with non-sidereal rates, but without guiding on stars) is offered, but the telescope shows drifts on exposures of 2-3min or longer. If you have questions or concerns related to this option for your proposal, please do not hesitate to contact the QSO Team (qsoteam -=at=- cfht.hawaii.edu).

For Canadian proposals: the Science justification is now limited to 2 pages, and the Technical justification to 1 page. For all other agencies, the page limits are 3 pages and 2 pages respectively.

For more information about the submission of your ESPaDOnS QSO proposal(s), contact the QSO Team qsoteam -=at=- cfht.hawaii.edu.

C - NorthStar [Back to Table of Content]

NorthStar is the new Phase 1 tool to submit proposals. This tool does not use Latex. The scientific and technical justifications, along with references and figures, are uploaded as PDF files, which may be prepared by the PIs on any software they may wish to use. Figures and references may be included with the Scientific and/or the Technical justifications.

Also note the following regarding the list of targets:

the list cannot be reordered by the user
the list is automatically reordered after each Save, based on a criteria other than name, RA, or DEC; moreover, CFHT does not have control over the final order of the targets
targets in excess of 15 are presented at the end of the proposal

D - Applicants [Back to Table of Content]

For each proposal, there can only be one submitter. However, co-I may be invited to view and edit the proposal too. The PI may also be different than the proposer (contact author). Note that if a proposal is accepted, it will get registered in PH2 under the PI's name, not the name of the contact author or the submitter! Each program belongs to its PI and requires the PI's login information in PH2.

E - Justifications [Back to Table of Content]

The Scientific and Technical justifications must be uploaded as PDF files, and have a limit of 2 and 1 page respectively for Canadian proposals, and 3 and 2 pages respectively for all other agencies.

Please use the CFHT ESPaDOnS + Olapa exposure time calculator to calculate the exposure time for each of your target and justify the total integration time requested. Do not use the original ETC from the Toulouse website, because it has not been updated for the new detector Olapa.

F - Observing Requests [Back to Table of Content]

For ESPaDOnS, you may select QSO Regular programs or QSO Snapshot program. QSO Regular programs include all of the normal QSO programs, with fixed or Solar System objects. Target-of-opportunity (TOO) programs submitted at the same time as all other CFHT proposals may simply be submitted as a QSO regular program. Snapshot Programs must request bad sky conditions and accept a low completion level.

The definition of a snapshot program for ESPaDOnS is the following:

A snapshot program describes valuable science to be obtained on targets observed only in the worse sky conditions (seeing larger than 1.5", and/or high extinction above 2mag)
A snapshot program will be scientifically useful even if the completion is low
A snapshot program preferably requests simple observations (i.e. sidereal tracking, no monitoring)
A snapshot program should preferably include short blocks of observations
The time allocated for such programs is not accounted for in the statistics of time spent for the different Agencies
The proprietary time for the data is 3 months following the end of the semester.

Note that the chance of such programs to be executed, even partially, during a semester can be quite high.

For ESPaDOnS, the seeing is not a fundamental constraint, although it plays an important role in the amount of light that can get into the entrance fiber. The exposure time calculator gives a clear idea on the effect of the seeing on the S/N obtained on a given target. The table below describes the seeing statistics on Mauna Kea. These data are for the R-band and were taken with FOCAM at CFHT between 1993-1995 (more recent statistics confirm these values).

Image Quality (IQ)	Frequency
IQ 1.0"	80%
1.0" < IQ 1.5"	15%
IQ > 1.5"	5%

For your information, the table below gives the average weather statistics for Mauna Kea. Note that the "A" semester is usually more affected by bad weather; time lost during the first few months of the winter can be as high as 50% and even more.

Sky Conditions	Frequency
Usable Nights	~70%
Lost to Weather	~20-30%
Usable Photometric Nights	~50%

In queue mode, the time requested is in HOURS.

If the total time of your program is fractional (e.g. 32.4 hr.), please indicate so (.4 hr in a queue mode is possible).
In your calculation of integration time, only the exposure time and overheads should be included. The overheads depend on the readout speed selected (no binning is offered) for each exposure and additional operational overheads: fast (40 sec), normal (60 sec), slow (85 sec). Of course, to acquire one Stokes parameter in polarimetry mode, 4 exposures are needed; calculation should be done accordingly.
Slewing and acquisition SHOULD NOT be accounted for in your calculations.
CFHT provides instrumental calibrations (biases, flats, comparison exposures) but does not provide any on-sky calibration, such as spectrophotometric standard stars, twilight spectra, or radial velocity standard stars. Those MUST be included in the proposal and in the time requested. The "Calibration Requirements" box may be used to present those calibrations.

Bright stars can saturate the detector. Please use the exposure time calculator and make sure you do not get any Saturation warning!

For various reasons (QSO internal constraints, cosmic rays, overall strategy, scheduling flexibility), single polarimetric exposures + their overheads cannot exceed 1800s, and single spectroscopic exposures should not exceed 1h.

Any time constraint or scheduling constraint must be indicated in the proposal: the need for a certain number of consecutive nights, the need for long blocks of time (for example, 8 hours) per night, the need to coordinate CFHT observations with observations taken by another telescope, etc.

By default, the proprietary period of QSO data extends to 1 year + 1 month starting at the end of the QSO semester. If an extension is requested and approved by TAC, a new date will be set for this program through the QSO system. The release date for the data is indicated in the fits headers by the keyword REL_DATE. For snapshot programs, the proprietary time is 3 months following the end of the semester.

G - Target list [Back to Table of Content]

Besides a list of targets with coordinates, ESPaDOnS proposals must include the Magnitude of each target. This information will be used to evaluate the technical feasibility of each proposal.

H - Additional issues [Back to Table of Content]

The Additional issues tab is used to link various proposals together, if need be.

Z - Check list [Back to Table of Content]

Before submitting your proposal, please make sure that:

You have requested time in HOURS.
Your requested time includes the appropriate OVERHEADS.
You have used the appropriate EXPOSURE TIME CALCULATOR.
If your program is a Snapshot program, it requests bad sky conditions (bad Image Quality or high extinction), is simple, and is made of short OGs.
You have included on-sky calibrations if needed and if not already taken care of by the QSO Team.
You have indicated the magnitude of your targets.
You have contacted the QSO Team for any question or concern.

Need More Information?
Contact the QSO Team at qsoteam -=at=- cfht.hawaii.edu