Explanation of the Proper motion differences between catalogs matrix.

PM / PM error

For each catalog, this lists:

1. N) The number of stars found in that catalog.
2. μ PMe) The (mean proper motion) / (mean proper motion error) of those stars in mas/yr.
3. σ PMe) The standard deviation of this ratio in mas/yr.

Catalog to catalog variation

This matrix lists the differences in proper motion measurements between the astrometric catalogs PPMXL¹ URAT1², UCAC4³, Tycho2⁴, and Gaia⁵.

Each catalog pair's differences are given in a 7 element data group at the intersection of the row and column of the catalog pair. The 7 elements are defined as:

1. N) The number of stars found that were common to each catalog.
2. μ RA) The mean difference in mas/yr between the right ascension of proper motions for the stars in common for both catalogs.
3. σ RA) The standard deviation of μ RA, again in mas/yr.
4. μ Dec) The mean difference in milliarcseconds/year (mas/yr) between the declination of proper motions for the stars in common for both catalogs.
5. σ Dec) The standard deviation of μ Dec, again in mas/yr.
6. μ Err) The mean difference in mas/yr between the proper motion error for the stars in common for both catalogs.
7. σ Err) The standard deviation of μ Err, again in mas/yr.

Method

The catalogs were downloaded, and C programs were written to put the data from each catalog into a common structure:

typedef struct StarData {
  double ra;    // J 2000 Right ascension in radians.
  double dec;   // J 2000 Declination in radians.
  int mv;       // Visual magnitude. * 100. 3000 == no data.
  int mb;       // blue magnitude. * 100. 3000 == no data.
  int mk;       // K band magnitude. * 100. 3000 == no data.
  int pmRa;     // Proper motion in RA in mas/yr. * 100.
  int pmDec;    // Proper motion in dec in mas/yr. * 100.
  int pme;      // Proper motion error in mas/yr. * 100.
  char cat;     // Catalog the data is from.
  char id[23];  // Catalog ID.
} sData;

This data was then sorted into a master file that contained all entries from the catalogs in ascending order of right ascension.
The master file was then sorted into a separate file that eliminated all non stellar objects, all stars with no proper motion error, and finally all stars fainter that 17.0mv.

The file was parsed by a C program that located stars from different catalogs that were within an arc second of each other. These stars were considered to be the same star, and their proper motions were compared. This data was incorporated into an algorithm that calculated a running mean and standard deviation⁶.

References

1) The PPMXL catalog web site.

2) The URAT web site

3) The UCAC4 web site.

4) The Tycho catalog web site.

5) The Gaia Data Release 1 web site.

6) Knuth's preferred method for calculating a running standard deviation.