Subaru Service Program

1. Definition

Service Program is for observing proposals which require less than or equal to 4 hours including all the "open-dome" calibrations and overheads. All Service Program observations will be executed by the Support Astronomers, so the observing method and technical details must be well described in the proposal.

2. Eligibility

Both Japanese researchers (i.e., either researchers of Japanese nationality or those belonging to Japanese institutes) and non-Japanese researchers can apply to Service Program. Maximum 5% of total nights will be allocated to non-Japanese PIs. Please note Service Program is newly opened to Gemini community as a part of time-exchange framework (see note below), it isn't opened to Keck community, though. Regarding institutes which entered an MoU with Subaru/NAOJ, however, the agreement in the MoU will be exceptionally applied.

[note]Applicants from Gemini Community should submit their proposals to Gemini, not to Subaru ProMS.

3. Available Instruments for Service Program

  • FOCAS (imaging/long-slit spectroscopy/MOS/IFU)
  • HDS
  • IRCS (imaging/spectroscopy with/without AO188)
  • MOIRCS (Imaging and MOS)

4. Notice for Service Program Applicants

Multiple Observations and/or Instruments
A service program proposal requesting observations divided into several different periods or using different instruments is not necessarily excluded as long as the total observing time is within 4 hours. It should be remarked, however, that the possibility of such a complicated observing proposal being completely executed as a service program is considerably low.
Indefinite Targets
Proposals intending to observe indefinite (i.e., unspecific) targets should not be applied for Service Program. Such proposals need to be applied for Normal Program.
Application Requirement
Describe the requirements for observation as a plain text. Each instrument has a different format for specifying the requested observations. Please see the relevant part of Section 7 for FOCAS, HDS, IRCS, or MOIRCS. In addition to specifying the instrument configuration(s) for observations, applicants need to indicate the site conditions (seeing, photometric, etc.) required for observations to achieve the intended scientific goal. Applicants can request the best conditions for observations if really needed, but in general programs requesting strict conditions would have lower chance of being executed.
Scientific Justification
Please follow Section 3 of How to Submit?
Calibration Data
Calibration data taken for one service program may be shared with other service programs (if possible) in order to improve the overall observing efficiency during the nights scheduled for service observations, though applicants do not need to be aware of it.

5. Execution Process

The observations of accepted service programs will be carried out by Support Astronomers (SA). No visiting observers will be accepted. Service Programs will be scheduled in advance, and executed according to the priorities (given by the TAC) and the site conditions. The observing method and technical details must be described well in the proposal, so that SA can execute observations without any need of contacting the PI. SA will send information to PI once his/her program has been completed. In other words, SA will not send any announcements to PI until his/her program has been completed. All the proposed programs will be off (i.e., cleaned from) the active service queue at the end of the semester.

6. Notes on publishing data obtained from a service program

Applicants are required to follow the Subaru Telescope acknowledgment policy. Though SAs who perform service observations are not expected to be involved as co-authors in any publications which may arise, they are always ready to be inquired about possible collaborations.

7. Required Documents for Each Instrument

This section lists the appropriate formats for specifying your requested observations. Each instrument has a different format. Please read carefully the information relevant to the instrument needed for your intended observation.

7-1. FOCAS

(I) General Notice on Service Observation with FOCAS

The available observing modes are:
imaging
long-slit spectroscopy (only sidereal tracking)
multi-object spectroscopy (MOS, no preimaging)
Integral Field Unit (IFU)
Multiple observing modes can be used in a single program. Please note that nonsidereal tracking and polarimetric observing modes are not available, and that preimaging observation for MOS mask will not be made for service programs.
The grisms available for the service program are limited to the followings:
300B
300R
VPH450
VPH520
VPH650
VPH850
VPH900
Please check here for the details of the grisms and here about the combination with order-sorting filters and long-slits.

Those who plan to submit the service program proposal should make a detailed observing plan including overheads, and confirm that the plan can be fit in the 4-hr limit of service program. The overheads that should be considered are target acquisition (2-3min. for imaging, ~10min. for long-slit, ~15min. for MOS, and ~5 minutes for IFU), readout time (see FOCAS web page) and additional time for CAL sources (if required, ~5min. for long-slit, ~10min. for MOS, and ~4 minutes per 1 hour for IFU). Please describe the plan at the beginning of the observation file.

If it is MOS observation, up to 2 masks are accepted. Because preimages are not available, only the following case is acceptable as a service program.
1. The mask is already available from your past FOCAS observation.
or
2. If you have not done the mask design before, please read carefully the FOCAS MOS time application page at first. We strongly recommend to start the MOS design well in advance, i.e. 2 weeks before the proposal deadline.

Please check the FOCAS web page for the details of the mask design.
Note that if we find anything wrong with the mask (e.g., large rms in the alignment), the observation will not be carried out.

(II) Required Information in ASCII format

Please submit a plain ASCII text file.
The following information should be provided for each target and observing mode, including calibration standards.

1. Target/field name
2. Magnitude/range of magnitudes in a specified band
3. Are photometric conditions necessary? (Yes/No)
4. What is the maximum acceptable seeing size in arcseconds?
5. Right ascension of the target in format HHMMSS.SSS
6. Declination of the target in format (+/-)DDMMSS.SS
7. Equinox of position in format YYYY.Y
8. Position angle in degrees (-180 to +180)
9. Observing mode (imaging/long-slit/mos/IFU)
10. Filter/grism/slit settings for observation.
For spectroscopy, up to 2 spectroscopic settings (the combination of the filter, grism, and long-slit) are accepted.
Note that, for long-slit spectroscopy, you have to specify both slit-width and position (center or offset).
For spectrophotometric standard stars, using 2-wide slit is recommended.
11. CCD binning (X-axis x Y-axis)
With the new CCDs, only 1x1, 2x1, and 2x2 binning are currently available. Only 2x1 binnings are used for the scientific exposures of IFU mode. See the web page for more information.
12. Exposure parameters for each setting
12-1. Filter/grism/slit setting
12-2. Individual exposure time
12-3. Single/dithering
12-4. Number of exposures and dither pattern
  For imaging mode, specify the coordinates (dRA,dDec) in arcsec relative to the original position.
  For spectroscopy, specify the relative position along the slit in arcsec. A positive value moves the target toward +x. See the example files below.
13. Requests for calibration
As a standard set of calibration data, following frames will be taken in the evening or morning of the observing night while the dome is closed.
  dome flat (5 frames with the maximum count below 20000 ADU)
  arc (1 frame, or 2 if the wavelength coverage is wide)
  bias (5 frames)
  For IFU mode, an additional halogen lamp frame and arc frames will be necessary after every ~1 hour integration of scientifc targets. It takes 4 minutes.
If you need any other calibration data, please describe here (note that twilight flat is not available for the service observation).
Then add the following information.
14. Special requests for observation (if any)
15. MOS design files
In case of MOS observation, please attach the mask design files (.sbr) here.
Please use '#' to comment out a line and specify the mask names in the comments.
The snapshots of the design software should be attached as the finding charts (see III-3).

(III) Finding charts

Finding charts should be attached for each targets (For the calibration standards, you don't have to attach finding charts if they are from the FOCAS web page).

Please show the target name, the orientation (north and east), and the scale in the chart. In addition, the following information should be added depending on the observing mode.

1. Imaging
Show the FOCAS FOV (6' diameter circle) on the chart. If the target is single or small field (<6') and it is necessary to avoid the CCD gap and bad-columns, please specify how the two FOCAS CCDs are placed in the finding chart.
2. Long-slit spectroscopy
Please attach both wide (~6') and small (~20") FOV charts for each target. The small field chart with a detailed view around the target is essential for accurate acquisition. Show the positions of the target and the long-slit on the charts. If there's no neighboring objects around the target in the 20" chart, please use a wider FOV so that there are a few objects in the FOV and the target can be easily identified in the acquisition image.
If you're going to observe two or more targets in a single exposure, the distance of the targets should be less than 30 arcseconds and provide accurate slit position-angle (~0.1 degree). Fine tuning of the position angle will not be performed.
If the target is spatially extended, please take multiple exposures with dithering to avoid data loss by dead columns.
If the target is faint and cannot be seen in a 30 seconds exposure with FOCAS (use ETC for checking), please specify a bright star (15-22mag.) to acquire first and give either
  i. the coordinate offset (dRA, dDec) to the target from the star in arcsec. Note that the star has to be within 5" from the target for accurate telescope offset using a guide star.
  ii. the position angle of the star from the target with high accuracy (0.1 degree) which is used as the slit PA. The star should be within ~30" from the target due to the error of the slit PA of FOCAS, 0.1 to 0.2 degree.
3. Multi-object spectroscopy
The snapshot of the mask design software must be attached.
4. Integral Field Unit (IFU) observation
Please attach ~20" FOV finding charts. Show the positions of the target and the IFU field of view (13.5" x 10.0") on the charts. Please give us the position angle (PA) which is explained in the webpage, and check whether a bright source is not at the sky slit position.

If you intend to submit more than 2 finding charts, please compile them into one PDF file.

A-1. Number of finding charts contained (number of pages of the PDF file).
A-2. Give information 1 to 5 below for each of the finding chart.
(1. Page number 2. Object name 3. Size of the chart 4. Orientation of the chart (north and east) 5. Other comments (if any))

Here are examples for imaging, long-slit spectroscopy, MOS, and IFU modes to help you prepare your observation file.

7-2. HDS

Required Information in in ASCII format

Please submit a plain ASCII text file. Basically, the following information should be provided for each object. However, in case you use a common instrument setting (#6-12) for all targets, you can combine all targets information (#1-5) into one table.

  1. Target Name (including standard stars, if necessary)
  2. Target coordinate, including the equinox (e.g. J2000).
  3. Target magnitude in an optical band.
  4. Integration time and the desired S/N ratio at a representative wavelength (Please use HDS Exposure Time Calculator).
  5. If you use Image Rotator, please indicate slit PA in degrees.
  6. Requirement for ADC (Yes/No).
  7. Image Rotator Mode (Blue/Red/None).
  8. Wavelength Setup (StdUa/StdUb/StdBc ...etc). If you want to use non-standard setup, describe the desired wavelength range specifically.
    Note that you should use only one wavelength setting for each proposal in order to minimize overheads (10-15minutes).
  9. Wavelength Resolution (slit width).
    If you employ an image slicer, please describe here with the unit number (IS#1 or IS#2 or IS#3).
    Due to operation reasons, there is a possibility that the proposal requesting to use image slicer may be switched to normal-slit observations (and vice versa), if the observatory judges the requested observation can be accomplished in either mode.
  10. CCD binning (spatial × dispersion).
  11. Requested seeing size (if you want to resolve spatially). Select one from the following four cases: <0".5, <0".7, <1".0, >1".0 .
  12. Are photometric conditions necessary? (Yes/No)
Then add the following information:
  1. Priority, if you have more than one target.
  2. Please indicate any other special requests on your proposal, if any (e.g.,requirement for I2-Cell etc.).

A. Finding Charts

(about 10 × 10 arcmin2; as PDF attachment files)

If your targets meet at least one of these conditions,

  • V (or B, R, I...) magnitude, m(V) > 10
  • extended objects (nebula, galaxy etc.)
  • double star or target in crowded region
you should attach additional finding charts for each targets,
which have about 1×1 arcmin2 FOV.

Please describe the following points regarding your finding charts.

  1. Object Name
  2. Do you attach a PDF file of finding charts of this target? (Yes/No)
  3. Page Number of finding charts in your PDF file.
  4. Size of the chart
  5. Orientation of the chart
  6. Other comments (if any)

Here is an example to help you prepare your observation file.

7-3. IRCS

(I) General Notice on Service Observation with IRCS

Available observation modes for IRCS service observations are below.

  1. imaging with, or without AO188
  2. Grism spectroscopy with AO188
  3. Echelle spectroscopy with AO188

Please note that IRCS is always operated with AO188 optics for guiding. No-AO observations are limited to imaging observations that does not require guiding (i.e., bright targets).
Spectroscopic programs MUST have suitable NGS, or TTGS* candidates, since spectroscopy without AO188 is NOT available under any circumstance. Any spectroscopic programs without guide stars for AO188 will NOT be considered to be feasible.

* A target with no suitable NGS can be observed if it has a suitable TTGS. The TTGS has to be R≦18.0 mag, and should be located at the separation of ≦ 60 arcsec. Note that there are almost no correction in seeing size.

If you request an observation with NGS or TTGS, the finding chart should provide relative locations of the targets and their guide stars clearly.

For non-sidereal targets, only imaging (1)without AO188, or (2)with NGS mode, is available. Non-sidereal targets should be bright enough (R < 16.5) for the latter case.

The NIR WFS observation is NOT available for service observations.

(II) Required Observation Information

Please submit a plain ASCII text file and finding charts for targets including standard stars and/or, guide stars. The following information should be provided for EACH object, including calibration standard stars. Please note that you MUST provide calibration standard stars (photometric standard stars, and telluric standard stars) and information on their observation. On-sky observation time for these calibration standard stars MUST be considered for the total observation time for any Service programs, while other calibration data (flat, comparison, or dark) should not be charged. If you request to observe more than one target, please provide the priority information.

If multiple modes are desired for a target, please provide the required information for each desired mode separately.

  1. Object/field name.
  2. Right ascension of the target field in format HHMMSS.SSS
  3. Declination of the target field in format (+/-)DDMMSS.SS
  4. Equinox of position in format YYYY.Y
  5. Are photometric conditions necessary? (Yes/No)
  6. Observation mode (Imaging/Grism/Echelle)
    1. For imaging, do you need AO188? (Yes/No)
    2. NGS, or LGS?
  7. Magnitude/range of magnitudes in a specified NIR band. For Grism/Echelle spectroscopy, targets must be brighter than 21.5 AB mag in K-, or K'-bands.
  8. What is the maximum acceptable seeing size (in arcseconds) in the specified NIR band? In case of using AO188, please provide the maximum acceptable FWHM of the point-spread function after the AO correction.
  9. Please describe the AO guide stars as follows.
    1. R (or, V if not available) magnitude of your AO guide star.
    2. Separation between the target and the AO guide star
    3. Whether the AO guide star is a point source or not. If you use an extended object or a star associated with nebulosity, you must describe a FWHM of its spatial distribution or contrast between the star and nebulosity.
  10. Filter(s)/Band configuration for observation. If more than one filter is to be used, separate them with commas.
    Filter names for imaging are: Y, J, H, KP, K, LP, MP, CH4S (CH4 short), CH4L (CH4 long), FE ([FeII] 1.644), HC (H cont NB1550), H2 (1-0), BRG (Br Gamma), KC (K cont NB2315), NB2090, NB2071, H3+, H2OICE, PAH, and BRA (Br Alpha).
    Band configuration names for Grism spectroscopy are: zJH, HK, Iz, zJ, J, H, K, and L.
    Band configuration names for Echelle spectroscopy are: Iz, zJ, H-, H+, K-, K+, K*, LA-, LA0, LA+, LB-, LB0, LB+, M--, M-, M+, and M++.
  11. Pixel scale of camera detector array for imaging, or Grism spectroscopy (20MAS/52MAS).
  12. Slit width for Grism/Echelle spectroscopy. A value must be given for each band configuration specified in item 10, separated by commas.
    Slit widths available for Grism spectroscopy are : 0.1, 0.15, 0.23, and 0.45 @ 20 mas and 0.1, 0.15, 0.23, 0.45, and 0.6 @ 52 mas
    Slit widths available for Echelle spectroscopy are : 0.14 (3.47), 0.27 (3.47), and 0.54 (3.47) for Iz, zJ, and J/ 0.14 (5.17), 0.27 (5.17), and 0.54 (5.17) for all bands within H and K bands/ 0.14 (6.69), 0.27 (9.37), and 0.54 (5.17) for all bands within L and M bands.
    Please note that units for slit widths are arcseconds. The values within parentheses are slit lengths in arcsecond.
  13. Field position angle (PA) for imaging, or slit PA for Grism/Echelle spectroscopy. The PA is defined as the angular offset in degrees relative to the north celestial pole. The PA is measured from North to East, counterclockwise direction.
  14. 
                                                                         N
                                                                         |
         Field or Slit: PA=0deg                 PA=90deg                 |
                                                                         |
                                N<---| SLIT |---          E<---| SLIT |--- 
                                               |
                                               |
                                               |
                                               E
    
    
  15. Single frame exposure time in seconds. One exposure time must be provided for each filter/band configuration specified in item 10, separated by commas. Exposure time for slit viewer for Echelle spectroscopy in seconds. One exposure time must be provided for each filter/band configuration specified in item 10, separated by commas.
  16. Number of coadds at each dithering position. A specific value must be given for each filter/band configuration specified in item 10, separated by commas.
  17. Dither patterns. A pattern must be given for each filter/band configuration in item 10, separated by commas.
     Valid pattern names for imaging are S5, S9, D5 and D9. If you wish to repeat the pattern, write "S5*2", for example.
     The dither patterns are:
            (S5)   5       4     |        (S9)   8   7   6    |  
                                DITH                         DITH
                       1         |               9   1   5    |  
                                                                
                   2       3                     2   3   4       
    
                ----------------------------------------------
    
                                           (D9)       7
    
            (D5)       4          |               8       6       |  
                                DITH                             DITH
                   5   1   3      |            9      1      5    |  
                                                                
                       2                          2       4       
                                                      
                                                      3 
     The valid pattern names for spectroscopy are one frame, ABBA, OSO(object-sky-object), and OSSO(object-sky-sky-object).
     The ABBA dither pattern is:
            A                C                B
            |<----DITH/2---->|<----DITH/2---->| 
     where C is the target acquisition position on the slit.
  18. Dithering size in arcseconds ("DITH" in the above figures). Please provide RA and DEC offsets toward the sky position in case of using OSO, or OSSO patterns.
  19. Type of target. Use "OBJ" for objects, "STD" for standards.
  20. Name of the target, to be written in the OBJECT field of the image FITS header.

Here is an example to help you prepare your observation file.

7-4. MOIRCS

[A] Imaging Mode

(A-I) General Notice on Imaging Service Observation

All the standard broadband filters as well as the narrowband filters are available for Imaging Service Mode. Note that, due to very dark background level, the observation by the NB119 filter will need the multi-sampling readout with autoguider, which will take more overheads. Please consult to the SA if you plan to use NB119.

The use of the standard n-point dithering mode (0<n<10) is recommended for the usual observation. However, the experienced observers can make any change on it, including the use the SKYNOD option (see below).

The use of the autoguider is highly recommended for observation by the NB119 or Y band filters, due to very dark sky by the filters. Note that the use of the autoguider will add some more overhead (15-30 sec per dither).

Applicants for service proposals should describe your observing plan in detail at the header part of the generated OPE file, which would help us understanding your intention. Make sure that the whole operation (observation + overhead) does not exceed the 4 hour slot. A crude estimate of the observing time with overhead is shown on the top part of the MOIRCS Service Observation Form Generator. Applicants should also refer to the MOIRCS Imaging Observation Guide as well as the relevant information therein.

(A-II) Submission of the Imaging Service Form

Please use MOIRCS Service Observation Form Generator for your preparation. This tool will generate operation file data in response to the input data given by the user. First, read the description on the website about the details of data input. Run the web program for each target as well as each filter. Copy all the generated lines to a new text file, and repeat this procedure for each target and each filter/exposure setting one by one (insert space between each set: appending short headers is also welcomed). The resulting operation file should be submitted in the text format.

All applicants are highly recommended to use the Web Observation Form Generator. But the experienced observers of MOIRCS may want to revise the generated commands, such as the addition of SKYNOD option to the GETOBJECT. Please add short comments on the file to clarify your purpose when you revise the commands from Web Generator. Please note that there is in principle no chance to correct any mistakes by applicants once it is submitted.

Applicants may want to attach finding charts for the targets (indicate the exact MOIRCS FOV with channel 1/2 sign, as well as the direction of North). Please avoid using deep optical images: 2MASS or similar NIR images are preferable. Although the observatory staff usually checks the FOV before the science exposure of the fields, it is the PI's responsibility to set the correct values in the submitted service OPE form.

Here is an example to help you prepare an observation file.

[B] Multi-Object Spectroscopy (MOS) Mode

A conditional access to the Multi-Object Spectroscopy (MOS) Mode for Service Program has been available since S24A. The same as before, the applicants of the MOS mode have to have the MOS masks that were previously-cut (namely, this program is a promotion for the publication of old data by offering the supplement). Maximum number of the masks for service mode are 2. The use of the common-use longslit masks are not allowed.

Who Can Apply?

If your old data can be published by adding small amount (<4hr) of supplementary data, you can consider applying this program. We consider the situation below.

  • Loss of critical data by weather loss or technical trouble.
  • Failure taking good calibration star.
  • The S/N could not reach to the level for publication.
  • MOS masks were cut but never used due to bad weather or technical trouble.

Those who wants to apply this promotion program must carefully read below.

In order to avoid any conflict with the Dual- Anonymous Review System introduced for Subaru's proposal reviewing, you must avoid mentioning any information of previously-awarded program (PI name, proposal ID, etc) related to the MOS you want to re-use. You have to make sure that any information related to the previous observation is through "Private Communication". Please make sure to keep it.

Applicants must follow the steps below.

  1. Contact the primary SA first!! We will check 1) the availability of the MOS Masks, 2) validity of justification for Service within observatory. It should be at least 1 week before deadline.
  2. The SA will give you an Approval ID to you.
  3. Clearly state the ID on the Technical Justification part.
  4. Submit your proposal.

The applicants for the MOS mode for service program should first contact the SA at least 1 week before the deadline with the following information.

1. The ID, Title, and the PI information of the previously-accepted program for the current MOS program.

2. The name of the MOS masks previously used.

3. Filter, Grism settings, and the total integration time for each MOS mask. There should be no change from your last observation. If you need any minor change, please put the short justification on why. If the change is big and significant, observatory may reject this. You should first consider submitting it to the regular open-use program.

4. The Target Definition part for each MOS from previously used OPE. The part is something like below. M83=OBJECT=MESSIER83 RA=133700.900 DEC=-295156.00 EQUINOX=2000.0 PA=0.0

5. The Exposure Definition part for each MOS from previously used OPE. The part is something like below. You can modify the DITHLENGTH and EXPTIME(*), and put a note on the values as necessary.

GETOBJECT $DEF_MOS EXPTIME=180 NDR=10 DITHNUM=2 DITHLENGTH=2.5 AUTOGUIDE =YES

(*) Note that the exposure parameter changed since 2015 (nuMOIRCS upgrade). The applicants who were awarded the time before 2015 have different GETOBJECT parameters. In such case, you may use EXPTIME=180 and NDR=10 for R500, and EXPTIME=600 and NDR=16 for VPH, as a default. We may change the parameters on site considering the night condition. If you want to avoid changing the parameters by us, explicitly state as so.

6. The information for a telluric standard star. We suppose you already have the star information from previous observations. Please provide the OBJECT information from the used OPE. You may change the star to be used for the current program. As a default, we take the standard star data on one channel only, with one A-B dither sequence. But if you have any additional requests, you can put the note here. Any additional information about the star (r-band and Ks-band magnitude, finding chart, etc) would be useful.

Note for overhead calculation: Total observing time should be within a 4-hr slot, including MOS alignment (20 min for each), and standard star obs (20 min including single A-B dither for each grism each MOS). And also, please consider the overhead for individual exposure (readout etc) as 85%.

We will review your request in the observatory. If we consider it is okay to go ahead, we will send an "Acceptance ID" back to you. Please explicitly state the ID number at the Technical Justification part of your proposal. Without the ID, your proposal will automatically rejected.



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updated on February 5, 2024