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 instruction in ProMS.
- Total observing time does not include any overhead time. PI does not need to consider any overhead- readout time, telescope slewing, standard field (SDSS field), etc - when he/she requests total observing time for HSC queue mode.
- The requested observing time must be set in the unit of hours with the conversion relation (0.14 night = 1 hour).
- There is no lower limit in the request hours of Normal Program, i.e., it must be between 0 and equal to or less than 35 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), Moon distance (lower limit), and airmass (upper limit). For example, if one target requires seeing ≤ 0.5" while the others can be made with seeing ∼ 1.0", PI needs to set the seeing constraint as ≤ 0.5 in item 13 of the ProMS. 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.
- The default airmass constraint is 2.0. The PI can specify the upper limit between 2.0 and 3.0 if he/she wishes to allow observation in low elevation. The PI cannot specify the airmass constraint smaller than 2.0.
- Weather may change during observations, so a tolerance of 0.1" for seeing and 20% margin for transparency (T) will be applied. For example, if the PI set observational constraints as seeing ≤ 0.8" and T ≥ 0.90, then the OB will be executed only when seeing ≤ 0.8" and T ≥ 0.90. As a result of observation, however, if the observed frame has seeing ≤ 0.9" and T ≥ 0.72, it will be considered as acceptable.
- 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 need the regularly repeated series of the observations with a time interval, 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 blocks in the time domain. We only accepts monitoring proposals of 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 HSC queue working group 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 have the similar scientific objectives as a Normal/Intensive programs by them, if a part of their scientific goals can be reached even with poor observing conditions. Note that due to the specification of ProMS, the titles must not be identical.
- Requested on-source exposure must be equal to or less than 35 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 compare to other filler programs which have not yet reached 4 hour completion.
- Filler programs may be recycled to the further semesters if a shortage of filler programs is detected.
- 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 (≥ 1.2") or bad transparency (≤ 50%) with cirrus clouds. Higher priority should be given to normal and intensive open-use programs (i.e., Grade A, B, C) and Subaru Strategic Program (SSP). Only when there is no any other programs to be executed in the time slot, filler programs may be selected and observed. [see Filler Program Form]
- PIs can submit filler programs which have the similar scientific objectives as the Normal/Intensive programs by them. Note that in this case the maximum on-source exposure time to be requested is 4 hours per proposal. Note that in this case PIs must use a different title than those of Normal/Intensive programs since ProMS cannot accept the proposals with the identical title.
Statistical Information for Observing Condition Constraints¶
Please set the observing condition constraints to achieve your scientific goal. In the ProMS, 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 the recent observations of HSC.
Seeing statistics to 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 i filter for which SSP-Wide specifically require good seeing condition, two data are provided, including and excluding SSP-Wide data, respectively. Here is a table summarizing median values in the unit 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. Current (Jan 2017) transparency seems degraded due to lower mirror reflectivity by 5-15% depending on wavelength (bluer wavelength is affected more).
- 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¶
Please use HSC Exposure Time Calculator (ETC) to estimate the S/N and total exposure time for your targets.
Target Field Check¶
Please check your important target is not 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 region in the maps below.