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 in S18A.
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 exposure sequence in the time domain. Please check the PI document for requirements and remarks regarding this program.
Note on Filler Program¶
- In S16B, we spent about 40% of total on-source exposure time of HSC queue nights for Grade F programs due to bad weather, and we realize the need of more filler programs in the queue in the case that the trend continues. PIs are encouraged to submit filler programs, given that the chance of executing filler OBs seems higher than it has to be (so far).
- 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. 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.
- 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]
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.
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.