1. GSC2 Science Projects @ ESO 7th GSC2 Meeting 2001R.MignaniESO

2. On Going Projects ä ä 4 Major Projects to be carried out @ ESO Approved in 1999 ä ä GSC2 ID of ROSAT sources (PI: R.Mignani) ä ä The Local QSO Luminosity Function (PI: S.Cristiani,R.Mignani,A.Wicenec) ä ä Tidal Tails in GCs (PI:S.Zaggia,R.Mignani) ä ä Planetary Nebulae & Central Stars (PI:F.Kerber,R.Mignani,A.Wicenec)

3. GSC2 ID of ROSAT sources R.Mignani (ESO),W.Voges, F.Guglielmetti (MPE), S. Covino (OAB) et al. ä RASS and Pointed Observations ä GSC2, 2MASS, NVSS ä X-correlations with X-ray Cats from PSPC & HRI observations ä RXH (11,000-19,000) R=5” ä RXP (95,000) R=10” ä RASS/BSC (18,800 sources) R=30” ä RASS/FSC (106,000 sources) R=30” ä Better understanding of the G/EG X-ray source population ä Statistical studies ä Selection of objects with NO opt ctp (e.g. radio silent INSs)

4. Strategy ä ä For RXH, source coo are precise --> likely position-wise ID ä ä For RXP and RASS, source coo are more uncertain --> positional coincidence is NOT sufficient to claim the ID ä ä Additional information is essential... ä ä X-rays: spectrum - timing - variability --> X-ray source Class ä ä Opt: MC wrt Template Spectra --> Opt Ctp Class   Fx/Fopt ä ä ID in the X-ray/Opt parameter space e.g. ä Fx/Fopt vs HR ä A “decision tree like” algorithm must be implemented to automatize the ID

5. Status ä X-correlations with X-ray Cats are in progress... ä Tests done with the GSC2.1... ä Definition of algorythms for the decision tree... ä Definition of algorythms for the MC Phot Obj Class... ä Whole, MC, sky coverage down to the plate limiting magnitude is required asap to: ä better explore the X/Opt parameter space ä avoid continuous repetitions and updates ä RXH Ids --> paper in preparation (Mignani, Covino et al.)

6. The Local QSO Lum F S.Cristiani, A.Grazian, R.Mignani, A.Wicenec (ESO) ä ä Selection of QSO candidates from the RASS/BSC based on HRs (done) ä ä X-correlation with GSC2... in progress ä ä ID of QSO counterparts from the expected Fx/Fopt + colors + class (... as before) ä ä Spectroscopic follow-ups ä ä Compute Luminosity function of QSOs ä ä Tests computed on pilot fields ä ä Complete sky coverage required

7. Tidal Tails in GCs S.Zaggia (ESO,OATs), R.Mignani (ESO), R.Smart (OATo) ä Evidence for tidal disruption in GCs in GCs ä Identify GC objects among fields stars fields stars ä Photometry approach ä CM diagram to characterize the GC sequence GC sequence ä Comparison with CM of field stars to isolate GC stars stars to isolate GC stars ä Astrometric approach

8. Status ä A sample of 60 Southen GCs selected ä A sample of 60 Southen GCs selected with d 20 deg ä GCs identified in GSC2 plates and Bj, F doublets selected ä Obj in a 2x2 deg regions around GCs extracted from the GSC2 plates  GC core stars are not detectable by the GSC2 pipeline ä Off-line alghoritms (e.g. DAOPHOT) run on the images ä GSC2 astrometry used to match GC stars in doublets ä GC sequence is not well defined ä D-I calibration required to DAOPHOT ä Project idle.....

9. Planetary Nebulae & Central Stars F.Kerber (ST-ECF), R.Mignani (ESO), F.Guglielmetti (STScI,MPE), A.Wicenec (ESO) ä ä Assess coordinates of the PNe SEC + Suppl (>2000 entries) ä MC Identification of CSs in PNe (only 30% known) (only 30% known) ä PM measurements and Distance Estimates for (un)identfied CSs Estimates for (un)identfied CSs (only 5% known) (only 5% known)

10. PNe Positioning ä ä A SkyCat based Procedure set up to automatize DSS2/GSC2 - FCs comparisons & identifications has been implemented ä PNe/CS coordinates classified: ä CS: PN extended, CS resolved ä STELLAR: PN is stellar-like ä PHOTO: PN extended, CS not resolved ä GEO: PN extended, CS ambiguous ä Position confidence graded ä Identification Process COMPLETED - (GSC2.1+GSC2.2) (Kerber, Mignani, Guglielmetti and Wicenec, to be submitted to A&A.) To be presented at IAU Symp. 209

11. CSs Identification ä Selection of PNe with candidate CSs from the revised Cat ä CSs identification through J-F vs J ä Automatic procedure to produce CM diagrams around PNe ä J-F vs J of known CSs used as calibrators ä in progress...

12. CS Proper Motions ä Wait until GSC2.3 for a complete PM survey ä A list of candidate PM CSs already produced ä However, off-the-catalogue PMs can be pursued for most interesting cases ä e.g. CS in PN Sh 2-68.....

13. XE630 LCO ä ä RA,DEC obtained from the OOPs of 7 plates plus the GSC2-based astrometry of 3 CCD frames (CAHA, LCO) ä ä Time Span: 47 yrs CS in Pne Sh 2-68

14. Results ä ä 53.2 +/- 5.5 mas/yr SW ä ä Largest PN PM ever measured from the ground ( Kerber,Guglielmetti,Mignani,Roth-submitted to A&A) ä ä One of the more precise, comparable to the ones obtained with Hipparcos ä ä @ v=30 km/s --> d=100 pc ä ä PARALLAX measurement to grasp the CS distance ä ä Not possible with the GSC2 also because of the random epoch distribution

15. Follow up ä Proposal submitted to HST (FGS) in Cycle 11 (PI: Kerber) ä 5 visits ä Optimal periods March/September RA DEC

16. PM of the BHC XTEJ1148+48 I.F. Mirabel (CeA), V.Dhawan (IAFE),R.Mignani (ESO),I.Rodriguez (IAFE), F.Guglielmetti (STScI)  XTEJ1118+48 is a galactic XRB: one of the very few BHCs ä Mass Function --> M x > 7 Ms ä Transient in X-ray/radio/optical ä Radio Jets (Microquasar) ä Location outside Gal Plane (d =1.8 Kpc; @ b=62 deg) ä Local BH population? Evaporation from Gal plane? ä PM studies to Constrain the birthplace ä Critical for BH formation models (SN) ä PM Done in both optical (GSC2) and radio (VLBA) ä ä Mirabel et al. (2001) Nature 413, 139 + STScI PR

17. Optical (GSC2) ä V=18 Opt Ctp (quiescence), K7 ä 4 Epochs selected spanning 43 yrs (1954-1996) ä Rel PM - correction for galactic rotation wrt EG reference frame ä Correction for Sun PM ä Ra=-10.5+/-3.2 mas/yr ä Dec=-5.9+/-3.2 mas/yr ä 12.0+/- 3.2 mas/yr ä PA=240+/- 15

18. Radio (VLBA) ä Timespan 3 months (May-July 2000) ä Two independent measurements (1.5 GHz and 8.4 GHz) ä PM wrt EG calibrators ä Correction for Parallax and PM of the Sun ä Ra=-16.8+/-1.6 mas/yr ä Dec=-7.4+/-1.6 mas/yr ä 18.3+/- 1.6 mas/yr ä PA=246+/- 6

19. Optical vs Radio

20. BH Orbit U=-97+/-23 V=-191+/-23 W=-38+/-12 km/s wrt LSR