MOIRCS Information for Imaging Mode



How To Make an OPE File for Imaging Observation

Please read the following documents before your observation.




Optical Distortion and Mosaicking

The optical distortion pattern for the MOIRCS is expressed well by the third-order polynomial as a function of the distance from the optical center (xc=881, yc=1008 for chip 1, xc=1124, yc=1024 for chip 2). The distortion coefficients could change by the thermal cycle of the main dewar, as we would move the internal focus adjustment system. The mosaicking rule (position/magnification of channel-2 image relative to channel-1 image) may also be changed by the process. The users should be aware of these effect during the observation and data reduction. The SA can give you the geotran database file (for IRAF) for correcting distortion and mosaicking two channels. However, the file is created based on the single observation, and so it might be changed by any reasons (e.g. the affection of the gravitational flexure, main dewar thermal cycle, shock during the instrument exchange, unexpected power outage).

Dates below indicate the thermal cycle of the main dewar after the upgraded MOIRCS. Note that we moved the detector box everytime before June 2016.

    Jan to March, 2016 (3 times)
    Late May, 2016

FYI: Dates below are for the old MOIRCS before 2016.

The default mosaic rule might also change with the elevation or the rotator angle. The measured shift of the relative ch1-ch2 position from the canonical value (e.g., the one provided by MCSRED) is typically ~2 pixels at 30 degree elevation. It will also be affected by the differential atomospheric dispersion when the image are taken at low elevation (<30 deg).




Stray Light from Nearby Bright Stars (updated in Feb 2012)

If your observing field is close to very bright (JHK < 2 mag) stars, the data may suffer from a significant contamination by that stars, like the examples below. It is caused by the reflection of the light from the star by the center cone of the secondary mirror. After the replacement of the center cone in 2010, the behavior of the stray light has been changed. The characteristics described below is for the stray light since 2010. For more detail, some reports are available from the dedicated website (Japanese only).

The light tends to contaminate the field when the bright star is located between 2.5 to 0.5 degrees from the target. Even though the stray light is not always happen in that range, it will always affect the data significantly if the target lies the 75 arcmin +- 4 arcmin area from a bright star (K < 2 mag vega). The area 120 - 140 arcmin away from a bright star could also be affected with fairly high probability (~50%).


We strongly recommend to check whether there are such bright stars or not before the observation. If there is such a star within 2.5-0.5 degree from your target, please prepare the backup targets beforehand.

The Website below (VizieR) is very useful for check. All (potential) observers should check whether your targets have such bright nearby stars beforehand.

Objects listed below are known to have the problem with high probability.

  • SXDS field
  • Rho Oph
  • Abell 1689
  • 4C 23.56
It has been known that the use of the optical secondary mirror can effecively eliminate the stray light, with only the minimal affection being obseved as the rise of thermal background in K-band window (, while Y~H windows have no problem). In 2018 we installed the new cold head with the stray-light blocker, and confirmed that it eliminates the stray light very effectively. Thus the observations with the broadband filter and some narrowband filters (H2, CO, BrG, Fe2, and NB119) now do not need to worry about the stray light coming from the center cone. However, for some NB filters (NB1550, NB1657, NB2071, NB2095, NB2315, OC_ZJ, and OC_HK) the problem unfortunately still remain until we can find the chance to install the new stray light blocker for them.

Those who want to request the use of the optical secondary mirror by the reason should explicitly put comments on the "Instrument Requirement" section of the proposal. Note that we cannot guarantee the use of the optical secondary if the scheduling constraints are tough. For more detail, contact SA.




Affection of Moon for Imaging Mode

The affection of th Moon to the background level in near infrared is generally smaller than in optical wavelength. But the sky tend to be brighter than dark night a bit, especially in bluer band. The affection is large when there is a cirrus in the sky.

On bright night we checked how the background level go up with the distance from the Moon. The figure below is the result of our experiment. In the figure, plus marks at >30deg is the reference sky magnitude that are measured far away from the moon. The rise of sky level is almost negligible at >15 degrees, while at 10 degree a clear affection is observed in all bands measured. We also saw some pattern by the scattered light in background at <10 degree.

As the autoguider (AG) is operated in R-band wavelength, the affection of the moon is serious. The AG software will fail the automatic sky estimation roughly at <15 degrees (in some cases, the affection occurs even at 25 degrees away). If the observation uses the autoguider, <30 degree from the moon may be with high risk of AG failure. Of course the affection of the scattered moonlight will be much stronger if the condition of the sky is not clear. Especially the halo from the moon (at ~22deg) will affect the AG background level much.

In conclusion, the affection of the moon on the MOIRCS data may be negligible if your targets are away from the moon by >20 degrees (on clear condition). If you plan to use the AG (for Y, NB, and the spectroscopic observation), the separation must be at least >30 degrees. You should check the separation between the moon and your targets when submitting the proposals, and should explisitly state the dates you want to avoid the assignment on the "Scheduling Requirement" section of the proposal.




Notes on the Autoguider Users

You may require the use of the Autoguider (AG) for more accurate tracking if the single exposure is longer than 3 minutes. The users of some NB filters or Y-band filters might have to consider this. We strongly recommend the AG users to check the availability of the suitable stars for Autoguider before you finalize the observing coordinates. You can find the more detailed description about the Autoguider Issue below.




Flat Fielding

(!! This is for OLD MOIRCS before 2016 !! We will update the informations for new MOIRCS situation soon.)

The dome flat in J band shows a tilt along x direction with a level of ~6%. In H-band a slimilar level of tilt is also suspected. These tilt pattern should be removed from the raw dome data using the sky flat. On the other hand, the sky flat generally contain some level (< a few %) of affection by the fringe pattern caused by filter substrate.

The sky under the narrowband imaging observation is usually not "flat". This is because the central wavelength is the function of the angle of incidence to the filter, or approximately, the distance from the pointing center. The use of dome flats for NB data is recommended, especially the observation is aimed the high-accuracy photometry.

If the sky during an exposure varies rapidly due to cloulds etc, you will see a tilt pattern at each detector quadrant on the image. It is the artificial pattern caused by the CDS readout method. If such pattern appears frequently and strongly on your data, the accuracy of the sky flat by these dataset will become poor, though it depends on the level of tilt patterns on your dataset (low-level pattern is usually seen). We recommend to use the domeflat as well as the sky flat if the sky changes significantly during your observation.




Fringe Patterns

The data taken by some filters (NB119, Fe2, H2, NB1550, K_CONT, STD_K, OC_HK, OC_ZJ) may occasionally show a fringe pattern. Due to the move of the pattern during the exposure (possibly by the instrument flexure), sometimes it is difficult to subtract the pattern by the simple scaled median-sky subtraction, as shown below.

In the above figures, the top two images show the data taken by the H2 NB filter flatfielded by the dome flats (left is channel 1, right is channel 2). A clear fine fringe pattern is seen. This is caused by the parallel-plane interference of the night emission lines inside the filter substrate.

The bottom two frames are after the scaled median-sky subtraction. The fringe pattern is stronger for the upper left area of channel 1 as well as the lower-left area of the channel 2. Thus, more complex pattern subtraction is necessary.

In order to remove these patterns, a novel method was developed by Dr. Wei-hao Wang for his reduction program (see the Data Reduction below). A similar method was also introduced by Kajisawa et al. (2011, PASJ, S63, 379). If you have the problem by this, you may contact to these authors for some help.

Note that the large ring-like pattern is caused by the two strong OH night lines at 2.118um and 2.125um. This is due to the position-dependent shift of the transmission curve. For more, see the NB filter information.




Information about Troubled Data

Some of the fits header information after the detector and control system updrade in 2016 are known to be incorrect. As of July 2016, it has been known that all the time-related keywords are inaccurate. The exposure start time is the same for ch1 and ch2. However, it is not in all the data taken.

(for old MOIRCS before 2016) The periods with any kind of troubled data are summarized in the Spectroscopy Information page.




Data Reduction Packages


Questions/comments are welcomed. Please contact to each author.


If you are developing your own software and want to put the link to your software website here, please contact to the SA. We greatly appreciate your contribution.



Please note that all data on these pages are subject to change. Any questions/comments should be directed to the SA (Ichi Tanaka: ichi [at] subaru.naoj.org ; change " [at] " to @).

Updated 2018-08-05


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