Principal Investigator Email Address
yyang@mpia.de
Estimated Total Execution Time (hours, including overheads)
15.0
General Description
This observation aims for the detection of Halpha emission lines (2.175micron) from z=2.3 galaxies. Since targets are extremely faint (K_AB > 22), we use blind offset to acquire science targets (reference stars have a range of magnitudes: K_Vega = 15.5 - 12.0). Note: we do not attach high-magnification finding chart because our targets are not resolved and not visible in short exposure time. Our finding charts have FOV = 4.5 arcmin against the SINFONI-specific recommendation because our reference stars are often ~2 arcmin away from the science targets. Please let us know if we need to resubmit the finding charts with 1 arcmin FOV. Thanks!
Waiver Requests
Our waiver request is approved: we were granted OBs with execution time up to 1hr 30min.
Critical Observing Condition Constraints
None
Time-Critical Aspects
None
Special Execution Requirements
Because our targets are very faint, we include a PSF standard at the end of science exposure to check the pointings and to make a proper coaddtion from different OBs. This cal_PSF template has the offset opposite to the blind offset. But we are not sure whether or not (1) the telescope is moving back to the reference star or (2) stay on the science target at the end of science exposures (obs_Generic). Here we assume SEQ.RETURN=T (default). If (2) is ture, then the provided offset should work. However, (1) is the case, then the offset in the psf standard cal should be (0,0). We wish that support scientist could verify this before the run.
Special Calibration Information
For the telluric standard star observation, we like to have "B-type" stars with KNOWN K-band magnitudes in order to use those telluric standards as the spectro-photometric standards. The telluric standards should be taken at the same airmass as the science targets. Furthermore, if possible, we wish to have the images (or spectra) from the acquisition templates because this reference star will be observed again with the PSF standard templates at the end. Having two images of reference star at the beginning and the end will allow us to obtain better astrometry.
ToO Information
N/A
ToO Activators List
N/A
Is this a Pre-imaging run ?
false
Pre-imaging Requirements
N/A
Source(s) of Pre-imaging
Pre-imaging sources not listed above
Do all your OBs comply with the instrument-specific requirements listed on the instrument-specific Phase 2 web page ?
If this is a pre-imaging run, did you select PRE-IMAGING for the Observing Category for each Observing Template ?
N/A
Do all your finding charts comply with both the general and instrument-specific Phase 2 Web Pages ?
If you submitted OBs for standard stars, did you specify the magnitude and spectral type of all standard stars in the OBs ?
N/A
Have you included OBs for any calibrations that you need but which are not part of the Calibration Plan ?
If you are observing Moving Targets, have you attached suitable ephemeris files to your OBs?
N/A
If you have preferences which OBs should be executed first, did you make use of the User Priority field in the OBs ?
If this is a run that requires coordinated observations with other facilities, did you give proper instructions in the Time-Critical Aspects Section ?
N/A
Did you indicate the magnitude of the brightest object in the field in each SINFONI OB?
N/A
If you are using the AO: Did you indicate for every OB the magnitude of the guide star, and its distance to the target (if any)?
N/A
If you submitted OBs for standard stars, did you use the provided StandardStar templates?
N/A
If you are using a specific offset pattern or position angle: did you check carefully the definition in the manual?
Did you make really sure that none of your OBs ever saturates the detector?
If you are using the AO: did you enter the correct Strehl Ratio (on-axis, K-band) AND the seeing value in the constraint set?
N/A