Richard MASSEY
PhD student at IoA

• Sunset (end of twilight) at LST 19:27. Sunrise (start of twilight) at LST 05:42.

• There are two equatorial DEEP fields; one at RA: 23 30 Dec: +00 (J2000.0), and another at RA: 02 30 Dec: +00 (J2000.0).
  Both are visible, although you will have to hurry to get the first one in during the very first hour of the night (last chance of the year). The second one is a better target at this time of night and can be images for a few hours more (although the sooner the better as far as elevation is concerned).
  A third option is the Groth strip region, which is also a DEEP field and can be targeted towards the end of the night.
  

• Airmass tables are below.

• R band filter.

• I have arranged the PA in the finding charts such that at PA=0^o, the long (34') dimension runs E-W. This enables us to cover the entire DEEP field with contiguous images, with a few arcminutes' overlap between fields. PA=36^o means a clockwise rotation, so that the long axis runs 36^o North from East (see this picture).

• 4x450s dithers on each field
  (differences are from base posⁿ and in real arcseconds, not RA&Dec)

  [+0"    , +0"  ]

  [+4.3", +2.5"]

  [-2.5", +4.3"]

  [+1.8", +6.8"] ...just an square with 5" sides, rotated by 30^o so no (bad) CCD columns line up.

  
  Note that this doesn't quite cover the 16" gaps between CCDs, but I don't like using the edges of images for weak lensing anyway. In my opinion, spreading the dithers wide enough to cover these gaps would cause greater harm in other ways.

• Need photometric standards, bias frames and sky flats.

• Dome flats would be a bonus if you have chance, please. On ESI on Keck in the past they have proved much better than the sky flats.

A target list formatted to Keck specifications is available here.

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