1. Globalization of stellar data: all-sky catalogues and open clusters A.E. Piskunov 1 and N.V. Kharchenko 2 1 Institute of astronomy RAS, Moscow, Russia 2 Main astronomical observatory, Kiev, Ukraine

2. Contents 1.Astronomical data globalization principles practice achievements 2.Open clusters and data globalization Pre-Hipparcos status and current activity Our project ASCC OC as example 3.Prospects

3. 1.1. Globalization of stellar data: principles All-sky coverage Completeness and high resolution at some depth Uniformity of data structure over the sky High precision Homogeneity of stellar data systems over all sky Accessibility

4. 1.2. Realization of the celestial system as a major aspect of the globalization Realization of all-sky coordinate & photometric systems: Hipparcos/Tycho missions Extension of the systems to fainter stars: High precision measuring machines automated telescopes Hipparcos family Hipparcos Tycho-2 ASCC-2.5 Schmidt surveys: GSC USNO SSS Array detector surveys: 2MASS UCAC

5. 1.3. Examples of practical data globalization. Example 1: present-day all-sky catalogues

6. USNO-B1.0 USNO-B1.0 (with PM) USNO-A2.0 UCAC2 2MASS UCAC2 1.4. Practical globalization. Example2: brightness distribution

7. ASCC- 2.5 UCAC 2 2MASS and UCAC2 (black points) SSS USNO-B1.0 and USNO-A2.0 (black points) 1.5. Practical globalization. Example 3: CMD diagrams

8. 1.5. Practical globalization. Example 4: proper motions UCAC2 ASCC-2.5 USNO-B1.0 and SSS (black)

9. 2.0 Open clusters and data globalization in the pre-Hipparcos era in the post-Hipparcos era Dias et al. (on-line): compilation of about 1700 open cluster data; Platais et al. 1998: 15 new clusters/stellar groups, Hipparcos; Alessi et al. 2003, 2004: 11+~50 new clusters, Tycho-2; Bica et al. 2003: ~350 new IR candidates of clusters/stellar groups, 2MASS; Drake (2005): 7 candidates of clusters, USNO-A2; Kharchenko, Piskunov et al. 2005: parameters of 520 known and 130 new clusters, ASCC-2.5 (the sample is complete up to 850 pc); Kumar et al.(2006): over 60 candidates of embedded clusters in 2MASS; Kronberger et al. (2006): 24 candidates from DSS images analysis. A total of 1200 clusters known by 1988 (Lynga, Lund Catalogue rel.5); For about 1200 clusters apparent diameters (eye-estimated from POSS charts or defined by the size of detector FOV) were given; About 400 clusters had accurate, but heterogeneous UBV photometry, distance, reddening, age; Kinematics: heterogeneous proper motions and RVs. Less than 100 clusters with PM in FK4 and RV. The 3-d velocities are available for a few tens of clusters only; No idea on the degree of completeness in cluster statistics; No way to study the population of stellar associations, extended clusters and loose groups (except nearby OB associations).

10. 2.1.Open cluster specifics and all-sky catalogues Successful search/study of various issues of open clusters requires: Object list completeness in dense sky areas Multi dimensionality of data (variety of data types) Kinematics Photometry Supplementary data Data sufficiency for all clusters: Coordinates, PM, 2color photometry  100 % VR, Sp.Classes/3 color photometry ( reddening )  10 % High data accuracy over full magnitude range

11. 2.2. Open clusters: practice of globalization (ASCC OC project) The Sample: 513 known clusters 7 known associations 130 newly detected clusters 2 large nearby clusters Cluster parameters: combined (PM,XY,CMD)membership coordinates core & corona radii PM,VR distances, reddening ages The sources: All-sky compiled catalogue ASCC-2.5 (v.3) 2.5 mln. Johnson B,V and PM 0.5 mln. Spectral Classes 46,0000 RVs and Literature data The results: The methods: Identification of known clusters Detection of new clusters Membership pipeline Cluster parameter determination The input:

12. . 2.3. Open clusters: summary of the ASCC OC project

13. . 2.4. ASSC OC data incompleteness: Radial Velocity

14. Completeness limit 850 pc Density enhancement 552 clusters ~800 missing clusters Background level 552 clusters 2.5. ASCC OC sample: spatial completeness

15. 2.6. Open clusters: 2D distribution in the disk D 0 1015 kpc -3 114 kpc -2 (5 times larger!) Predicted number of OC for R G =15 kpc  100,000 Spiral pattern : Grand design with pitch angle=-6°

16. 2.7. Cluster complexes: tangential velocity VPDs the general environment OCC-1 OCC-2 Perseus-Auriga Hyades log t < 7.9log t = 8.3...8.6 log t = 7.9...8.3 log t > 8.6 Extinction map a V = A V / d Blue triangles - OCC-1 Red circles – OCC-2 Magenta diamonds - Perseus-Auriga group Black crosses - Hyades moving group Small circles - “field” clusters

17. P=1/ – decay probability  a – cluster age, a = t 1 – t, t 1 ⇒ present, t ⇒ at birth – rate of cluster formation N(a) = (t 1 -a) e -a/ t 1/2 0.7 = 364±32 Myr = 0.24± 0.02 1/Myr Literature: = 140-240 Myr = 0.1-0.25 1/Myr All clusters Complete sample Wielen 1971 2.8 Open clusters: ages and lifetime

18. 3.1. Further steps Developing the success on available data basis Further exploration of current resources: ASCC: new cluster parameters: segregation, tidal radii, masses UCAC: new clusters & new cluster parameters, 2MASS: new clusters & new cluster parameters, Extending photometry basis: ASCC+2MASS: ASCC cluster sample increase by 15% Extending accurate Proper Motion space dimension: AC+2MASS: ASCC cluster sample increase by >50% Extending Radial Velocity space dimension: ASCC+RAVE: 25% increase of the RV sample

19. 3.2. Quality leap: waiting for GAIA Current resources unable to provide completeness in: data (RVs, extinction/distances/ages) for more than 2/3 of known OCs space beyond 1 kpc-neighbourhood (effectively beyond Sagittarius and Perseus spiral arms) DIVA: good, but lost opportunity GAIA: the only but far-away opportunity