Update on April 12, 2018:

Replaced all *.out.d files with *.newout.d versions, including M67 files.
These have only stars and not stars+galaxies.
Stars were selected based on using the dr= MAG_AUTO-MAG_PSF 'concentration parameter' being in a restricted range around 0.
Also added to these *.newout.d files is a column E(B-V), 2nd last column which can be used to undo the reddening correction if we wish to.
g0 = g -3.184*E(B-V)
r0 = r -2.130*E(B-V)
i0 = i -1.568*E(B-V)


Please let me know if you have questions of concerns
------------------------

The union of the *.newout.d files contains PANSTARRS star magnitudes positions,
colors and estimated distances for stars with

140 < l < 220 and 20  < |b| < 65 and r < 21.25 (that's a non-dereddened cut)

also 1.2 < g-i < 3: but one should further restrict this cut based on g-i_0

There is a bright end limit that we need to figure out.


There are lots of stars here, you can cat all the *.d files together
into one big file if you like.

The columns are:

0 RA J2000
1 DEC J2000
2 l Galactic l
3 b Galactic b
4 r_0 Dereddened r magnitude
5 g-r_0 dereddened g-r color
6 g-i_0 dereddened g-i color
7 r-i_0 dereddened r-i color
8 M_r  absolute r band magnitude, based on r-i_0 formula (Juric 2008)
9 zoffset -- adjust z for z_sun = 15 pc above plane
10 rdered -- this is another in the plane distance estimate (consistency check)
11 rgc -- galactocentric R of the star (in the plane distance)
12 d0 -- distance to the star from the sun (kpc)
13 X -- Galactocentric X kpc
14 Y -- Galactocentric Y kpc
15 Z -- Galactocentric Z kpc
16 E(B-V) Use to undo reddening
17 dr This quantity is a star-galaxy separator only those that are consistent with stars are kept

The m67 files have these four extra columns (but not E(B-V), dr).

18 pmra (mas/year,only in m67.csv.newout.d.pm and m67.csv.newout.d.pm.cut)
19 pmdec (mas/year,only in m67.csv.newout.d.pm and m67.csv.newout.d.pm.cut)
20 pmraerr (mas/year,only in m67.csv.newout.d.pm and m67.csv.newout.d.pm.cut)
21 pmdecerr(mas/year,only in m67.csv.out.d.pm and m67.csv.out.d.pm.cut)


============

We've now (as of Sep 19,2017,updated Apr 12, 2018) added a M67 set of PAN star magnitudes and colors.


This file contains mainly M67 members (with a few outliers),
if you want to see 'the whole m67 field', look at the file
m67.csv.out.d (same column indicies) and you can overplot m67c
and see how the M67 members were selected.

If you plot d(kpc) vs. g-i_0 color in m67c you will see a locus of points
at about 0.68 kpc.  The actual distance to M67 is 0.89 kpc, so our distances
are all 'low' by 0.89/0.68- 1 = 31%.  We can correct that at some point,
by multiplying our distances by 1.3088 or adjusting the M_r0 column in
the formula.  We can do this later or now if we like.

The color range to cut, I think should still be something like 
1.8 < (g-i)_0 < 2.4 .  We could go a bit redder, say to (g-i)_0 < 2.6
and a bit bluer, say to (g-i)_0 < 1.2 if we wish, but let's start with
the same color cut as from Deborah's paper:

1.8 < (g-i)_0 < 2.4 and see what that subsample looks like.

We can go brighter that Deborah's paper, where we restricted to 15 < r0 < 21.5

I think, because PANSTarrs is taken with a smaller telescope (1m mirror
vs 2.5m for SDSS), that they saturate brighter, at about 13,
so let's make the magnitude cut 13 < r0 < 20.

That let's us probe closer to the Galactic plane for our reddest stars,
by a factor of 2?? or so in distance.

So I would suggest combining all the out.d files at the link above (not the m67 one) into one file and excluding objects with r0 < 13 or r0 > 20? and
g-i_0 < 1.8 or g-i_0 > 2.4 and then making your N/S or star density plots again.

If you like you can multiple all the d0 distances by a factor of 1.31 to get
a more accurate distance in kpc.


----------------

proper motions of M67 stars:

Are now the last four columns of m67.csv.newout.d.pm

If one does a cut -18 < pmra < -8 and -7 < pmdec < 3 then one
obtains the file:
m67.csv.newout.d.pm.cut

If you plot r0 vs. g-r_0 in this file you nearly all only members
of the cluster, so one can do the distance vs. color plot here to
derive a correction.