This directory contains the plPlugMapT files for the "Kinematics of the Thick
and Thin Disks" southern survey project (sdss-southern#156).  There are 15
tiles in three fields, 5 tiles each centered on the main survey tiles #179,
181, and 183.  The new tiles are numbered 9253-9267 (9253-9257
centered on main survey tile #179, 9258-9262 centered on main survey
tile #181, and 9263-9267 centered on main survey tile #183).

The three fields are as close to each other as can be without overlapping
(tiles 180 and 182 overlap in the obvious way).  Thus we have essentially one
elongated line of sight.  The following considerations drove the choice of
fields:

1) We wanted to maximize absolute galactic latitude, so as to maximize
   distance above the galactic plane.  All three fields are at galactic
   latitude ~ -62 deg.
2) It was decided to concentrate on one line of sight so as to get the
   best possible statistics, rather than get poorer statistics on 2 or 3
   lines of sights.  This is particularly important at distances high above
   the galactic plane; at 1.7 kpc (where we hope to have tangential velocities
   of order 30 km/s), our sample will include about 100 stars per 100 pc
   slice in z.
3) Overlapping fields were avoided, since creating 5 tiles per field in three
   overlapping fields with a single evenly distributed population of targets
   would necessarily lead to an uneven distribution of targets across some of
   the tiles.

The sample of stars was selected in two steps.  First, the stage
database was queried for all unsaturated primary stars with fiber g, r, and i
magnitudes > 15, unreddened PSF i magnitudes < 18.26, and unreddened i-z
colors > 0.2.  (The i magnitude limit in the proposal was 18;  we had to go
fainter to fill all fibers in 5 tiles per field because we failed to account
for the 2.5 degree stripe widths when calculating the expected density of
targets per tile for the proposal --- that is, there are no targets available
beyond abs(dec) = 1.25 deg, but the tiles of course are 3 deg in diameter).
The specific query used was:
  
SELECT RUN(), RERUN(), CAMCOL(), FIELDID(), OBJID(),
       psfMag[0]-reddening[0], psfMag[1]-reddening[1], psfMag[2]-reddening[2],
       psfMag[3]-reddening[3], psfMag[4]-reddening[4],
       fiberMag,
       RA(), DEC(), reddening, star_L_r, exp_L_r, deV_L_r
FROM Star
WHERE status & AR_OBJECT_STATUS_OK_SCANLINE > 0 &&
      objFlags & OBJECT_SATUR == 0 &&
      fiberMag[1] > 15 &&
      fiberMag[2] > 15 &&
      fiberMag[3] > 15 &&
      (RUN() == 1755 || RUN() == 2662) &&
      RA() BETWEEN 0 AND 15 &&
      psfMag[3]-reddening[3] < 18.26 &&
      (psfMag[3]-reddening[3])-(psfMag[4]-reddening[4]) > 0.2

From this sample, the final sample was chosen as any object which lies
between 100 arcsec and 1.49 degrees from the center of main survey tiles
179 (ra = 5.2229 deg, dec = -0.0332 deg), 181 (ra = 8.8956 deg,
dec = -0.0021 deg), and 183 (ra = 12.7276 deg, dec = -0.0332 deg).
This final sample includes 9040 stars.  48 of those have good redshift
determinations (zStatus=3, 4, 6, 7, 9, or 11) from previous spectroscopic
observations; those 48 objects were not assigned to new tiles.  Of the 8992
remaining targets, 8880 were assigned to tiles, leaving 112 unassigned targets.

All targets have the STAR_RED_DWARF primTarget bit set (along with the
SOUTHERN_SURVEY bit).  Thus, primTarget = 0x80040000, secTarget = 0x80000000.

The file "sample.par" defines the sample of objects from which the targets were
drawn, with an entry for the tile to which they were assigned (0 if not
assigned, to any tile, >9000 for the new tile it was assigned to, else plate
number for old plate on which it already appears).
