1. OAG COMMON PROPER MOTIONS WIDE PAIRS SURVEY II MEETING DOUBLE STAR OBSERVERS (Pro-Am) Sabadell 23-24 October 2010 Xavier Miret / Tòfol Tobal Observatori Astronòmic del Garraf (OAG) www.oagarraf.net

2. OAG CPM WPS Project: Search and detection of star pairs with CPM not catalogued yet. FEATURES: VISUAL SURVEY. Visual inspection of digitized plates. SYSTEMATIC SURVEY. Scanning selected areas.

3. HISTORICAL BACKGROUND W.J. Luyten Main contribution to double stars with CPM Year 1979 NLTT > 58.000 stars LDS > 6.000 pairs μ > 0.2 arcsec yr -1

4. HISTORICAL BACKGROUND Lépine & Shara SUPERBLINK software. 2003-2008 LSPM > 122.000 > 1000 doubles μ > 0,15 arcseg yr -1

5. HISTORICAL BACKGROUND GARRAF SURVEY (2008). Search for companions of near 2.000 NLTT between 0,5 and 1 arcseg yr -1 J. A. Caballero & D. Montes

6. GARRAF SURVEY LUYTEN STARS

7. STARS TO STUDY Stellar population with CPM < 0,15 arcsec yr -1 not studied up to now. Some pairs with CPM > 0,15 arcsec yr -1 not catalogued before.

8. COORDINATION & TEAMS Coordination OAG. Collaboration AAS. C. Schnabel. Open information: www.oagarraf.netwww.oagarraf.net

9. OAG CPMWP SURVEY Workshop I & II February and July 2010, Sabadell (Barcelona) Tutorials. Method Techniques Practical examples Resolution of questions. Adjudication sectors. Timetable. Preparation of publications. Organization: OAG / AAS

10. CURRENT STATUS > 500 pairs catalogued up to now. 10 amateur teams on work. Forecast: 12 h RA at the end 2010.

11. METHOD Loading images POSS I and POSS II (15 x 15 arcmin). Δt +/- 40 years. Blinking RGB. Identification of pairs. Crossing catalogues. USNOB1 and NOMAD1. Collecting data. Polar coordinates. Theta/Rho. Aladin vector tool.

12. LOADING IMAGES

13. BLINKING RGB

16. CROSSING CATALOGUES

17. POLAR COORDINATES Theta/Rho measures on digitized plates. Optimization centroid (Image convolution). Aladin vector tool (Manual path). Reference. I Novalbos communication.

18. TARGETS Pairs with sep > 5”. No superior limit. No magnitude limit. PM > 50 marcsec y -1 in at least one coordinate. Maximum difference in PM between components < 10 marcsec y -1 in two coordinates. ◄

19. TARGETS ¿What is the proper motions difference between components? Always < 15% the absolute value of PM Always < 3 X mean error (catalogue value)

20. DATA COLLECTION 1 IDENTIFICATION. USNOB1 / NOMAD1 / 2MASS / TYCHO2 / HIPPARCOS RA / DEC J2000 MAGNITUDE V or R PM RA PM DEC PM CATALOGUE SOURCE

21. DATA COLLECTION 2 THETA RHO EPOCH In case of lack of PM in pairs with suggestive image blinking we make multiepoch astrometry to support the CPM character.

22. MULTIEPOCH ASTROMETRY

23. RESULTS. MAGNITUDE. MAG R MAG (nº Stars)V MAG (nº Stars) 8 - 1017 10 -121527 12 -142943 14 -164666 16 -184291 18 - 20200

24. RESULTS PROPER MOTIONS SAMPLE 187 PAIRS CPM marcsec y -1 Number Stars 50 - 7590 (48.1 %) 76 - 10062 (33,1 %) 101 - 12526 (13.9%) 126 - 1507 (3.7%) 151 - 2002 (1%)

25. PUBLICATION Revision and cataloguing USNO / WDS: B.D.Mason (USNO). Electronic publication: USNO/WDS Website Publication: Webb Society DSSC: B.Argyle Professional studies and publications. J. A.Caballero, D. Montes.

26. FUTURE Encourage professional and amateur teams interested so that the project can be improved. Searching and development a software capable to find the same pairs automatically. Stellar characterization in at least some subgroups of stars.

27. Observatori Astronòmic del Garraf Parc del Garraf (Barcelona)