Use capital letters, numbers, and underscore ("_") only. Dash ("-") is not acceptable.
e.g. MOIRCS_1, MESSIER_3, COSMOS_F23_2, RXJ1234P5678
OBJECT keyword in FITS file
Use capital letters, numbers, and some symbols ("+","-","_", " ") only.
e.g. MOIRCS_1, MESSIER_3, COSMOS_F23-2, RXJ1234+5678
Right Ascension of Pointing Position (RA), Declination of Pointing Position (DEC)
In hhmmss.sss and ddmmss.ss format. Note that the
pointing position lies between channel-1 and 2, because MOIRCS is the
mosaic imager. If your target is single compact object and if you set
the target coordinate as the pointing position, the target will jump
between chip 1 and chip 2 by the dither, thus it may introduce any additional uncertainty.
Shifting the pointing position so that the target can come on the center of chip-2 may make the better result. For detail,
see Figure 1 of the MOIRCS homepage.
e.g. For pointing position at RA=12h34m56.78s Dec=12d34m56.7s, we use RA=123456.780 DEC=123456.70.
Position Angle (PA)
Should be -270 ≤ PA ≤ 270. For definition of the PA, please see Figure 2a of the MOIRCS homepage.
Filter (FILTER01)
All open-use filters are available for Service observation.
Each single-expousre time (EXPTIME)
The unit exposure time for each exposure set should appropriately be set. It should be larger than 2 seconds, and smaller than the maximum exposure time listed in the last column of Table 1 in the page. The maximum single exposure time above largely depends on the condition, as the sky level in near infrared changes drastically by hour-to-hour basis. If you do not have any special requirement and want to leave the summit observer for the suitable exposure setting, just set the "typical" values as written in the generator (180 for Y, 60 for J, 25 for H, 45 for Ks, 60 sec for MB, and 180 for NB filters) and explicitly write the request. Then they will set the appropriate exposure so that the sky level to 10000-20000 ADU (within ≤ 3% linearity range).
If your target is so bright that it could saturate under typical exposures, you can explicitly ask in the memo to keep the peak count of the object to be less than (for example) 25000 ADU etc. In such cases, it is highly recommended to submit the finding chart with a clear description so that the observer can easily recognize your target.
NEXPOSURE
You can consider the NEXPOSURE option to increase the observing efficiency (see the relevant page and/or "MOIRCS Observing Guide" for detail). The NEXPOSURE operation will take a set of exposure at each dither position in order to reduce overhead time by the dither. If you take 5-point dither exposure with NEXPOSURE=3 setting, you will get 3 frames at each dither position, and you will get 15 frames in total after the sequence. Keep in mind that telescope tracking is reasonably accurate for 2 to 3 minutes. The longer you stay at a dither position by NEXPOSURE, you will have higher chance to see the guiding error among the nexposure set. Typically, we use EXPTIME=180 with NEXPOSURE=1 for Y and NBs, EXPTIME=60 with NEXPOSURE=2 for J, EXPTIME=25 with NEXPOSURE=4 for H, and EXPTIME=45 with NEXPOSURE=3 for Ks and MBs. If you do not have any special requirement for the exposure setting, please just set the EXPTIME and NEXPOSURE as the values above.
We then flexibly change the exposure time and NEXPOSURE option appropriately according to the condition of the observing night for maximum effeciency.
Dithering number (DITHNUM), DITHCENTER, Dithering length (DITHLENGTH)
The number of dither and the optional exposure at the center of the dither circle before the start of the sequence. For dither pattern please refer the MOIRCS website. As a default we use "DITHCENTER=YES". Note that the exposure by DITHCENTER=YES is NOT counted as a number of dither; i.e., you will get 10 frames if you set "DITHNUM=9 DITHCENER=YES". The maximum number allowed for DITHNUM is 9. Please copy the generated GETOBJECT command until your required total exposure time is achieved.
Note that the DITHANGLE in OPE file will be set 5 degrees for the first dither set. If you repeat GETOBJECT in the same setting several times, please change the DITHANGLE (and DITHLENGTH too if necessary) randomly in order not to trace the same dither pattern among each dither set.
DITHLENGTH should be (at least) larger than the diameter of the largest object in your field of view. At least larger than 15 arcsec is recommended for making good median
sky. And also, it is important to take at least 7 frames per filter by the same reason.
See "Guide to Observing with MOIRCS" for more detail.
Use Autoguider?
The telescope can track target enough accurately without the Autoguider for about 3 minutes. Usually the AG is not necessary. However, the use of the autoguider is highly recommended for observation by the NB119, due to very dark sky by the filters. Note that the use of the autoguider will add some more overhead (~30 sec per dither). The applicants who want to use AG tracking for NB119 filter must check the availability of the AG star (and put the info in the finding charts). Make sure that the AG probe does not vignette your field of view. You can find the AG-related information from here.
If your target goes up to high elevation (>75 deg), the open tracking sometimes become quite poor, and the AG tracking greatly helps better guiding. We might have to start the AG tracking for the fields at very high elevation, without regard to your request.
Do you accept non-photometric condition?
Choose "No" only if any of your scientific aims can only be achieved
under photometric condition. If "No" we will go to other low-priority
programs instead under poor condition. Instead, we may go back to your
program again if there are next chances in better condition and if your
target is still available at that time.
Do you need photometric standards?
Usually we take several standard star data considering various
condition (target visibility, the position on the sky, weather
condition etc.) during one service night. We choose one standard star
under similar airmass value to target data. We take 3 shots in each
chip with the filters used, and take the data on both channel.
Typically two independent standard star data will be taken during one
program, if condition is allowed. If you choose this option to "YES",
please add 10 minutes per filter for the estimate of the observing time
(< 4hr).
If "No" we do not take standard data. But if we take standards for
other programs during the same night, we will also send the data.
Please copy and paste the generated form (in OPE file
format) for each setting to one new text file. Put space between each
output of the setting. Submit the text file.
Notes:
NB119: The NB119 narrow-band filter is open from S16A. Due to very dark background level by the filter,
we may consider the use of the multi-sampling readout method to reduce the readnoise.
The use of the filter is under the shared-risk policy.
Stray Light: We strongly recommend to check if there is no very bright star (K < 2 mag) within 1 to 2.5 degrees from your target. Especially if there is such a bright star at the separation of 75+-5 arcmin, or around 150 +- 5 arcmin, the target field could suffer from the significan stray light with high possibility. In this case, the use of the Optical Secondary Mirror (CsOpt) is a solution to avoid it. You can put the request in Section 5 "Observing Run". Note that there will be less chance of execution, if CsOpt is requested as "essential". For more detail, please visit the relevant webpage.
Finding Chart: Putting the correct RA & DEC info to the submitted service form is the observer's responsibility. However you can put the finding charts for check. If you have any special request (such as target saturation check etc) on the summit operation, it is mandatory. Write the FOV of MOIRCS as well as the direction of North and channel 1/2. Please use the images taken by the similar filter to the one we will use (by 2MASS image etc). Note that the use of the deep optical image (such as Suprime-cam image or the HST ACS image) often confuses the summit observer, thus definitely not recommended.
Dome Flats: We will try to take dome flats for your filter sets. However, due to the limitation of the calibration time, they may not always available. Instead you can creat the "sky flats" by median-combining the data (you should have plenty of frames for it: ask the SA for more detail). For dome flats, NB filter and Ks-band filter dome flats have higher priority. If you want to request YJH dome flats with higher priority, you must explicitly request it. For NB filter data, dome flat is taken as a default.
Darks: Dark data is usually not taken for imaging observation.
Flexibility: If necessary, you can edit the generated OPE file as you like (experienced
observer only!!). This includes the addition of SKYNOD option to GETOBJECT command
if you are familiar about the option. You must attach the memo and describe your intention in detail.
Be VERY careful about the change, as any mistakes or any wrong setting may not be corrected even if
we recognize it during the observation (except the exposure setting according to the sky condition).
Contribution to Observation: We may need to contact you to revise the program in short notice, considering the expected condition of the night
assigned for Service Program. Please be aware of it once your program is assigned as Rank-A. Note, however, that attending Service Observation remotely
via network communication tool is currently not permitted (though in future it may be changed). We are sorry for this.
OPE Manual: An introductory manual for the imaging OPE file ("Guide to Observing with MOIRCS") is available. Check if necessary.
Any questions should be directed to Ichi Tanaka (ichi[]naoj.org: change [] to @).
Acknowledgement
IT would like to express special thanks to Dr. K.Aoki for initiating this web ope file generator.