1. Proper motion accuracy of WFPDB stars
VII BSAC  "ASTROINFORMATICS" – Chepelare, 1-4 June 2010
Proper motion accuracy of WFPDB stars
Yavor Chapanov1, Jan Vondrák2, Cyril Ron3, Vojtéch Štefka2
1 – Central Laboratory for Geodesy, Bulgarian Academy of Sciences
2 – Astronomical Institute, Academy of Sciences of Czech Republic

2. VII BSAC "ASTROINFORMATICS" – Chepelare, 1-4 June 2010
DATA SELECTION
PLATE SCALE <100"/mm
SCAN RESOLUTION 2400dpi
PLATE CENTER AND ORIENTATION
IMPROVED DISTORTION MODEL
ACCURACY: 0”.5 – the best case,
1” – raw plate center,
5” – scan resolution 300dpi

3. VII BSAC "ASTROINFORMATICS" – Chepelare, 1-4 June 2010
DATA SOURCE
Catalogues of Wide-Field Plates
RA: , DEC: , radius: 5 deg – 2000 plates
2. RA: , DEC: , box size: 5 deg – 700 plates
3. RA: , DEC: , box size: 3 deg – 150 plates

4. VII BSAC "ASTROINFORMATICS" – Chepelare, 1-4 June 2010
ERROR MODEL – NORMAL DISTRIBUTION
Normally distributed pseudo random numbers

5. VII BSAC "ASTROINFORMATICS" – Chepelare, 1-4 June 2010
TIPICAL ASTROMETRIC ERRORS
According daily residuals of latritude observations
at observatory Plana for the period

6. VII BSAC "ASTROINFORMATICS" – Chepelare, 1-4 June 2010
A MODEL OF TIPICAL ASTROMETRIC ERRORS
10000 Normally distributed numbers N (0, 0.1)
Replaced by:
1% evenly distributed numbers from intervals (0.8, 0.4], [0.4, 0.8);
6% evenly distributed numbers from intervals (0.4, 0.1], [0.1, 0.4);
6% evenly distributed numbers from intervals (0.06, 0.06).
Resulting s=0.14

7. VII BSAC "ASTROINFORMATICS" – Chepelare, 1-4 June 2010
ERROR MODEL – I (the best case)
Standard 0.5 arcsec

8. VII BSAC "ASTROINFORMATICS" – Chepelare, 1-4 June 2010
ERROR MODEL – II
Standard 1.0 arcsec

9. VII BSAC "ASTROINFORMATICS" – Chepelare, 1-4 June 2010
ERROR MODEL – III (the worst case)
Standard 5 arcsec

10. VII BSAC "ASTROINFORMATICS" – Chepelare, 1-4 June 2010
RESULTS FROM 0.5” SERIES
PM: 0.001”/a ”/a ,05”/a
Estimates:

11. VII BSAC "ASTROINFORMATICS" – Chepelare, 1-4 June 2010
RESULTS FROM 1” SERIES
PM: 0.001”/a ”/a ,05”/a
Estimates:
RESULTS FROM 5” SERIES
PM: 0.001”/a ”/a ,05”/a
Estimates:

12. VII BSAC "ASTROINFORMATICS" – Chepelare, 1-4 June 2010
CONCLUSIONS
The WFPDB provide significant number of plates, containing a given star. The plates numbers vary from hundreds to several thousands and they cover century time span. It is possible to estimate the star proper motion with enough accuracy by means of the corrected plates for image center and distortion with 100”/mm scale and scan resolution 2400dpi.
It is possible to use the raw star images for estimation of the great proper motions, if the number of plates is more than 1000.

13. VII BSAC "ASTROINFORMATICS" – Chepelare, 1-4 June 2010
THANK YOU
FOR ATTENTION