README web version of /home/usg/OPS/MTS/readme_xml/readme_77019800

Principal Investigator Email Address

• ibata@newb6.u-strasbg.fr

Estimated Total Execution Time (hours, including overheads)

• 11.0

General Description

• Observations of Dwarf Galaxies near the Local Group Boundary.
  Refining the distance estimates using the TRGB.  
  All the fields of the same object have been offset already and are intended to avoid
   any interchip gap. I have selected the acquisition mode "MovetoGap" to do this assuming
   that is correct.  Rather than "MovetoPixel" because I could not find documentation
   on either option, so have selected the former.
  If you find this is not the case (ie the object falls on the gap), please feel free
   to adjust the pointing to ensure that the dwarf galaxy is in a clear part of the
   array and away from chip edges. Each dither within the OB is designed to move the
   galaxy around the array ensuring that any part that may have been in a gap in one
   exposure is not in the next. If the galaxy moves off the array we have accidently
   done so and it should be moved back on. Each offset maintains an overlap with the
   previous set of exposures and in most cases consists of a only a shift in DEC.

Waiver Requests

• No Waiver Request was submitted

Critical Observing Condition Constraints

• Due to the density of the fields observed and the low surface brightness
   it is essential that the moon is neither very full or in close proximity to these
   fields. We estimate that the moon should be less than 3 days from new and at worst
   not closer than 50 degrees. Poor image quality and or an increased sky background
   will make this science very difficult.

Time-Critical Aspects

• These OBs can be executed in any order.

Special Execution Requirements

• ---(Empty)---

Special Calibration Information

• We will use the Landolt standards fields you observe as part of a normal
   WFI run.
  The OBs which have short exposures on each field are intended to be observed on
   the same night as the Landolt standards and will allow us to propagate the zero
   point to the full-depth of the data.

ToO Information

• ---(Empty)---

ToO Activators List

• ---(Empty)---

Is this a Pre-imaging run ?

• false

Pre-imaging Requirements

• ---(Empty)---

Source(s) of Pre-imaging

• ---(Empty)---

Pre-imaging sources not listed above

• ---(Empty)---

Do all your OBs comply with the instrument-specific requirements listed
 on the instrument-specific Phase 2 web page ?

• YES

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 ?

• YES

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 ?

• N/A

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 ?

• N/A

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 set 'New Preset' flag in all acquisition templates to 'True'?

• N/A

Have all your submitted OBs the same filter for the acquisition template
 and for the first science template?

• N/A

Did you combine calibration templates with science templates for any
 OB?

• NO

Did you combine imaging and spectroscopic templates for any OB?

• NO

Did you submit any Focus template?

• NO