1 / 20

GSC2 Science Projects @ ESO

GSC2 Science Projects @ ESO. 7th GSC2 Meeting 2001 R.Mignani ESO. On Going Projects. 4 Major Projects to be carried out @ ESO Approved in 1999 GSC2 ID of ROSAT sources (PI: R.Mignani) The Local QSO Luminosity Function (PI: S.Cristiani,R.Mignani,A.Wicenec)

winchell-vance
Download Presentation

GSC2 Science Projects @ ESO

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

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

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

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

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

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

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

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

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

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

  10. PNe Positioning • A SkyCat based Procedure set up to automatize DSS2/GSC2 - FCs comparisons & identifications has been implemented • PNe/CS coordinates classified: • CS: PN extended, CS resolved • STELLAR: PN is stellar-like • PHOTO: PN extended, CS not resolved • GEO: PN extended, CS ambiguous • Position confidence graded • 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 • Selection of PNe with candidate CSs from the revised Cat • CSs identification through J-F vs J • Automatic procedure to produce CM diagrams around PNe • J-F vs J of known CSs used as calibrators • in progress ...

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

  13. CS in Pne Sh 2-68 XE630LCO • RA,DEC obtained from the OOPs of 7 plates plus the GSC2-based astrometry of 3 CCD frames (CAHA, LCO) • Time Span: 47 yrs

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

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

  16. PM of the BHC XTEJ1148+48I.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 • Mass Function --> Mx > 7 Ms • Transient in X-ray/radio/optical • Radio Jets (Microquasar) • Location outside Gal Plane (d =1.8 Kpc; @ b=62 deg) • Local BH population? Evaporation from Gal plane? • PM studies to Constrain the birthplace • Critical for BH formation models (SN) • PM Done in both optical (GSC2) and radio (VLBA) • Mirabel et al. (2001) Nature 413, 139 + STScI PR

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

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

  19. Optical vs Radio

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

More Related