Proposal submission is made through the Proposal Management System (ProMS). ProMS has been updated to accommodate HSC queue mode. Please select 'HSC Queue' for Normal and Intensive program or 'HSC Filler' for Filler program, then follow the instructions in ProMS.
- The requested observing time must be set in multiples of 1 hour, with the conversion relation 0.1 night = 1 hour. The observing time must include overheads. Total requested time for observing plan can be calculated using the HSC overhead and required time calculator.
- There is no lower limit in the request hours for Normal Program, i.e., it must be between 0 and equal to or less than 50 hours.
- Observation constraints in the proposal (item 13 in the application form) should be the strictest value for each constraint : seeing (upper limit), transparency (T; lower limit), Moon phase (brightest allowable phase), and Moon distance (lower limit). For example, if one target requires seeing ≤ 0.8" while the others can be observed with seeing ∼ 1.6", the PI needs to set the seeing constraint as ≤ 0.8 in item 13 of the ProMS. The Moon distance from the target should be larger than 30 degrees. Note that the moon-target separation is automatically relaxed to 30 degrees in dark time.
- Time critical observations are supported since S17B for Normal program only. Please put "Time critical" in Comments in the Box 12, and provide sufficient information on the time constraint (i.e., acceptable time windows) in Box 13 of Application Form. If different constraints apply to different targets/fields, please define the constraints in the list of targets, by adding comments in the "Magnitude" field. Multiple time windows are allowable. The time constraints of the windows should be clearly described, preferably in UT time. Note that the chance for the OBs to be observed becomes higher by specifying the time windows as relaxed as possible. The time windows are limited by the number of queue nights in the semester.
- Cadence observations, which require regularly repeated series of the observations, are not supported. Therefore, all observing blocks have to be independent, i.e., order of execution of OBs cannot be specified.
- Starting from S19B, a proposal using narrow-band filters with their central wavelength shorter than 400 nm should only be submitted to classical mode, and will not be accepted in queue mode. Currently, this only applies to filter NB387.
Note on Monitoring Program¶
- Starting in S18B, Subaru Telescope offers HSC queue-mode observations of monitoring programs (shared-risk mode). A monitoring proposal is defined as a proposal whose scientific goal requires more than one observing block in the time domain. We only accept monitoring proposals for which all time windows can be defined at Phase 2. Please check the PI document for further requirements and restrictions regarding this program, and contact the HSC queue working group to ensure whether your program can fit our scheme.
Note on Filler Program¶
- PIs are not allowed to submit multiple filler proposals which have similar scientific/educational objectives. This is identical to the "One Proposal for One Project" policy in the call for proposals.
- PIs can submit a filler program which has similar scientific objectives to a Normal/Intensive program, if a part of their scientific goals can be reached with poor observing conditions. Note that in this case the maximum on-source exposure time to be requested is 4 hours per proposal. Note that due to the specification of ProMS, the titles must not be identical.
- Requested total time must be equal to or less than 50 hours (equivalent to 5 nights).
- Once the on-source exposure time of completed OBs of a filler program reaches 4 hours, the priority of the program will be lowered compared to other filler programs which have not yet reached 4 hour completion.
- Filler programs may be recycled to further semesters if there is shortage of filler programs.
- Proposals for educational and public outreach purposes are also invited for submission.
- In principle, filler programs will only be executed under poor conditions with either bad seeing (≥ 1.3") or bad transparency (≤ 40%) with cirrus clouds. Higher priority should be given to normal and intensive open-use programs (i.e., Grade A, B, C) and the Subaru Strategic Program (SSP). Filler programs will be selected and observed only when there is no other program to be executed in the time slot. [see Filler Program Form]
Statistical Information for Observing Condition Constraints¶
Please set the observing condition constraints to achieve your scientific goal. In the ProMS, the PI needs to set the strictest value for each observation constraint. The following information is provided as references to find the typical frequency of seeing and transparency conditions, based on recent observations with HSC.
Seeing statistics in S16B¶
The above document shows the seeing distribution for each filter. We used data with (1) exposure time longer than or equal to 60 seconds; (2) elevation of 40-75 degrees; and (3) transparency higher than or equal to 0.5. For the i filter, for which SSP-Wide specifically requires good seeing condition, two data are provided, including and excluding SSP-Wide data, respectively. Here is a table summarizing median values in units of arcsecond.
|i (w/o SSP-Wide)||0.70||0.82|
Cumulative probabilities of seeing and transparency¶
|Seeing (arcsecond)||< 0.616||< 0.736||< 0.924||0.809|
|Transparency (0 - 1; 0=worst, 1=best)||< 0.811||< 0.928||< 0.953||0.856|
Seeing was measured from Mar. 2014 to Jul. 2015 and transparency was measured for Jan. - Jul. 2015 based on HSC data.
- Image quality statistics for May 2000 - Sep. 2006 at the Subaru Telescope's foci
- Seeing statistics from Auto Guider for May 2000 - Nov. 2010
Estimation of Total Exposure Time¶
Note that the HSC Exposure Time Calculator is updated on June 2021. Please check the evaluation report.
Target Field Check¶
Please ensure that your important target does not fall on bad CCDs or columns or gaps between CCDs.
- Current HSC detector status
- HSC instrument field of view (FoV) [VOTABLE file] [PNG file]: Note that the HSC FoV map does not include eight Focusing CCDs and four Auto Guider CCDs located at the edge of the CCD cluster.
- How to check target field with Aladin
SDSS Field Check¶
Please check whether your target field is covered by SDSS or not. If not, please find an SDSS field close to your target for the calibration of your science target. We recommand to avoid narrow strip pattern regions in the maps below.