Service Observations with ESPaDOnS
Phase 1 Proposal Submission for Semester 2010A
|Table of Contents|
A - Introduction
A - Introduction [Back to Table of Content]
(1) The QSO Project
The main concept behind the queue observation scheme with ESPaDOnS is to perform observation 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).
During 1999, CFHT has started a project to implement the necessary software and to review all the issues for achieving a queue/service observing mode with its CFH12K mosaic camera. This Queued Service Observations (QSO) Project has been developed in parallel to other projects necessary for the data acquisition (NEO), processing and analysis (Elixir), and archiving and distribution (DADS). The necessary software tools for proposal submission (Phase 2), selection of programs, management of the observations and execution of the observations have all been developed within the QSO Project. Most of these software components are for internal use only except for two obvious exceptions: Poopsy, proposals submission tool developed and maintained at CADC, and PH2, a Web based tool developed and maintained by CFHT for the second tier of proposal submission (see below).
The QSO mode has been used for CFH12K for over 200 nights between January 2001 and January 2003. Since the semester 2003A, MegaCam has been operated in the queue mode and starting in 2005B, observations with WIRCam have been entirely conducted under QSO as well. The spectropolarimeter ESPaDOnS has been used for several years at CFHT and has produced spectacular science. Since its first semester in QSO mode in 2008A, ESPaDOnS has benefited from QSO since a good ensemble of programs need specific time constraints to be successful. The success of highly ranked programs also remains at the mercy of the weather under the classical mode. For those reasons, ESPaDOnS is now only operated under QSO, with an automated pipeline also available to produce fully processed data. This tutorial explains how the phase 1 proposal submission should be prepared for this new mode of operations with ESPaDOnS.
For technical information, please see the ESPaDOnS page.
(2) Document Outline
This document presents the information for submitting a QSO proposal with ESPaDOnS. A complete description of the submission process with Poopsy and an outline of what will have to be done following the TAC evaluation for the second phase, planned for Nov or Dec 2009, are included. A few QSO Rules used for the selection of the programs are presented and some other issues related to the QSO programs are also discussed.
(3) An Important Note on non-sidereal tracking and guiding
IMPORTANT NOTE : The non sidereal tracking option (i.e., following a target with non-sidereal rates, but without guiding on stars) is ready, but the telescope shows drifts on exposures of 2-3min or longer. . If you have questions or concerns related to this option for your 2010A proposal, please do not hesitate to contact the QSO Team (qsoteam -=at=- cfht.hawaii.edu).
For more information about the submission of your ESPaDOnS QSO proposal(s), contact the QSO Team qsoteam -=at=- cfht.hawaii.edu.
B - Applying for ESPaDOnS Time [Back to Table of Content]
(1) Programs: Q or not Q?
Starting at the semester 2008A, the QSO mode is the ONLY mode of operation for the ESPaDOnS. The classical mode is NOT offered for ESPaDOnS.
Observation of Solar System targets through the QSO system is possible through ephemeris entries in the Phase 2 Tool, and we offer non-sidereal tracking (not guiding) for 2010A.
(2) Types of QSO Programs
Many types of programs can benefit from the queue observing mode. Programs requesting excellent or exceptional sky conditions, surveys, short- or long-term monitoring, target-of-opportunity programs, are all well suited for the QSO mode. Also, contrary to the classical mode, it is now possible to submit very short programs necessitating only a few hours of observations. Programs scientifically valuable during bad sky conditions are also possible. During the submission phase with Poopsy (Phase 1), you are asked to specify what type of programs you are submitting for the QSO mode. These types of programs are defined below:
(3) Proposal Submission Phases
For ESPaDOnS programs in the queued service observing mode, two submission phases are necessary. The first phase (Phase 1) is done through CADC Poopsy and consists in a general description of the program used for the evaluation by the Time Allocation Committee (TAC). This is the submission procedure for all proposals requesting time at CFHT. The second phase (Phase 2) is requested for ALL the ESPaDOnS queue programs for which telescope time has been allocated by the TAC. As described below, it is done prior to an observing semester (with a few exceptions) through an entirely new Web based tool developed at CFHT. During this phase, all the information necessary for the local staff to perform the observations is entered by the investigators and stored in a database at CFHT.
Only investigators with approved QSO programs with ESPaDOnS will be given access to PH2. The user ID and password used for Poopsy will still be valid for PH2. Try to remember them
C - Phase 1: Instructions for Proposal Submission with Poopsy [Back to Table of Content]
The current version of Poopsy allows investigators to send proposals for the queue mode. A section has been created which includes some information necessary for TAC evaluation, and for the QSO Team in the preparation of the queue database. Below, we review the questions related to QSO proposals as introduced in this version of Poopsy.
1 - Are you applying for a queue program with ESPaDOnS? (Run Info Section)
As explained above, the queue mode is the only mode of observation for ESPaDOnS. Answer "Yes" and complete the Queue Section.
2 - Indicate the type of queue observing program: Regular, Target-of-Opportunity, Snapshot (Run Info section)
These three types of programs have been reviewed earlier.
3 - Indicate a global image quality (IQ) constraint describing your program ? (Run Info section)
The main concern of the queue mode is to observe targets under sky conditions required to meet the science goals defined for each program. During Phase 2, the investigators will have to define precisely observational constraints for their project. However, it is important that a global image quality for each program is defined during Phase 1 as well. An efficient queue can only be achieved if the database contains programs requesting a wide range in constraints, especially on the image quality, and the TAC will strongly consider the choice of image quality indicated here for the overall selection of the queue programs.
For ESPaDOnS, obviously 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 simulator gives a clear idea on the effect of the seeing on the S/N obtained on a given target. The probability for a specific program to be observed in queue mode depends strongly on the image quality requested versus the statistics of the site. The chance that your program is performed is less if you request a seeing of < 1" than if 1.5" is required. So, do not request a better image quality than what is really needed for your program. For guidance, the table below describe approximately 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 (%)|
|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 reach level of 50% and even more.
|Lost to Weather||~20-30%|
|Usable Photometric Nights||~50%|
4 - How many hours are required for this queue program for this semester ? (Run Info section)
In queue mode, the time requested is in HOURS, and might or might not include overheads. You can follow these directives:
5 - Scheduling Constraints: (Run Info section)
Several program with ESPaDOnS need specific dates and times for the observations to be carried out. This information can be precisely defined during the phase 2 period but it is important to include such constraints here because it can significantly influence the scheduling of the instrument on the sky.
6 - How many additional HOURS would be requested to complete this project ? (General Info section)
If you are planning to submit an additional proposal for the same program for the subsequent semester (and the following, if necessary), please indicate the number of hours that might be required.
Note: For the Phase 1, the Moon options are used to help us evaluate the best periods for a scheduling a queue observing period covering as many programs as possible. The influence of the Moon on the spectra acquired through the narrow optical fiber is very small.
7 - Other Instrument Description: (Instrument section)
ESPaDOnS is an instrument that has 3 Observing
Modes, all offered in QSO mode:
There are also 3 CCD readout modes offered in QSO mode, with different gains, readout noises, and readout times. The "XSlow" mode is not be offered in QSO mode.
Please indicate which observing mode(s) and readout mode(s) are expected to be used for the proposed program.
D - Calibrations [Back to Table of Content]
One of the main advantages of the queue mode scheme is the possibility to share calibrations between a set of programs. To achieve this, a calibration plan has been defined and will be carried out regularly by the queue/service observers. This plan includes the necessary "detrend" frames for removal of the instrument signatures (bias, flat-fields) and wavelength and Fabry-Perot calibrations. More details can be found on the Upena pipeline page.
For this semester, you can can consider the following situations:
E - Program Evaluation [Back to Table of Content]
Following the submission of your queue proposal, the TAC will review it and evaluate it. Your proposal, if accepted, will receive the following grades, ranks and allocated time. This information will be entered by us in the queue database and will be available through PH2 for the second submission phase.
|Grade||Grade Name||Global Priority||% of Telescope Time|
F - The ESPaDOnS Exposure Time Simulator [Back to Table of Content]
An important component in the preparation of the proposals during Phase 1 and 2 of all the queue mode programs instituted around the world is the availability of a exposure time simulator. Since the investigators are not present during the observations, it is crucial for the QSO observers to know that if the observations are undertaken during sky conditions requested, the science goals should be reached because the proposers have verified that using a robust exposure time simulator. It is not always easy to judge the science merit of an exposure frame and this is better accessed by quantitative evaluation.
An exposure time simulator for ESPaDOnS has been developed by Jean-Francois Donati. A Web based interface for the simulator is available here. Note that the space of parameters available in the simulator is much larger than the options offered by QSO. It is strongly recommended to use the simulator during Phase 1 and Phase 2 of the queue programs with ESPaDOnS!
Approximate exposure times for which the detector becomes non-linear and/or saturates (i.e., over ~66,000 ADUs) are given in the following table:
|A star of
|Will saturate |
with individual exposure times
|4.0||180 sec (3 min)|
|5.0||480 sec (8 min)|
|6.0||1200 sec (20 min)|
|7.0||3000 sec (50 min)|
|8.0||7500 sec (125 min = 2h 05 min) - MAX possible|
G - A Few QSO Rules [Back to Table of Content]
Maybe the most difficult task facing the queue observing model is found in the selection process leading to the execution of a science program. This selection algorithm can be based on simple criteria (e.g. mounted filters) but it becomes immensely complicated when other parameters like actual sky conditions, completeness level, science merit, monitoring constraints, or targets visibility are taken into account.
The process, resulting in the choice of a specific program to be undertaken for the queue observations with ESPaDOnS, will be done in three steps:
(1) Communication and Night reports
The QSO Team is always available by email at qsoteam -=at=- cfht.hawaii.edu . To ensure prompt replies, emails have to be sent to the whole QSO Team and not to individuals! Emailing the whole team also allows all members to be aware of current issues, and to be up to date with all available information.
After each observing night, a Night Report detailing what observations were performed is available on the CFHT Web site. These reports include the observations groups executed and the sky conditions at the time of the observations. This does not mean that your data will be immediately available (see below). The goal of these reports is to inform the community of the progress of the queue and, in particular, the current status of your program.
Current global statistics for a semester are also available on the QSO Web page.
(2) Data Evaluation
As part of the data quality control assessment, all data taken will be automatically processed and calibrated by the Elixir Team. Data evaluation will be done in two steps: during the observation by the Service Observer ("on-line" evaluation) and, during and after the data processing. This last step is very involving and represents one of the reasons why data cannot be distributed immediately after a QSO run, unless specifically justified during the Phase 2 period. If the observations are judged satisfactory, the queue database is then updated by the Queue coordinator.
(3) Data Distribution
Data distribution (raw and processed data) will be ensured by the Upena Team. Our goal is to be able to distribute the data to the PI of each project (or another member if specified during the Phase 2) and the relevant calibrations by noon the day following observations.
(4) Proprietary Period
By default, the proprietary period of QSO data extends to 1 year + 1 month starting at the end of the QSO semester. For instance, data taken for the 2010A semester (Feb 1 to Jul 31 2010) will have a default release date set to 08/31/2011. If an extension is requested in Poopsy 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.
The QSO Team members are: Nadine Manset (QSO
Manager), Billy Mahoney (Database/System Programmer), Tom Vermeulen
(System Programmer), and Mary Beth Laychak, Peter Forshay, Adam
draginda, and Todd Burdullis as Service
Observers. During a QSO run, supervision is ensured by the QSO
Coordinator who, among other things, is responsible for managing the
queue database, planning of the observations, and maintaining the
contact with the investigators, if necessary. Observations will be
conducted by the Service Observer and the Resident Astronomers, with a
strong involvement by the Observing Assistants. Software support will
also be provided during the observing nights. For TOO programs and
decisions related to the viability of some programs, the CFHT Executive
Director acts as the final authority.
|Need More Information? Contact the QSO Team at qsoteam -=at=- cfht.hawaii.edu|