Title: GSC2 Science Projects @ ESO
1GSC2 Science Projects _at_ ESO
- 7th GSC2 Meeting
- 2001
- R.Mignani
- ESO
2On Going Projects
- 4 Major Projects to be carried out _at_ 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 (PIS.Zaggia,R.Mignani)
- Planetary Nebulae Central Stars
(PIF.Kerber,R.Mignani,A.Wicenec)
3GSC2 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 from PSPC HRI
observations - RXH (11,000-19,000) R5
- RXP (95,000) R10
- RASS/BSC (18,800 sources) R30
- RASS/FSC (106,000 sources) R30
- Better understanding of the G/EG X-ray source
population - Statistical studies
- Selection of objects with NO opt ctp (e.g. radio
silent INSs)
4Strategy
- For RXH, source coo are precise --gt likely
position-wise ID - For RXP and RASS, source coo are more uncertain
--gt - positional coincidence is NOT sufficient to
claim the ID - Additional information is essential ...
- X-rays spectrum - timing - variability --gt X-ray
source Class - Opt MC wrt Template Spectra --gt 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
5Status
- 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 --gt paper in preparation (Mignani, Covino
et al.)
6The 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
7Tidal 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
8Status
- A sample of 60 Southen GCs selected with dlt 20
kpc and bgt20 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 .....
9Planetary Nebulae Central StarsF.Kerber
(ST-ECF), R.Mignani (ESO), F.Guglielmetti
(STScI,MPE), A.Wicenec (ESO)
- Assess coordinates of the PNe SEC Suppl (gt2000
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 -
(GSC2.1GSC2.2) - (Kerber, Mignani, Guglielmetti and Wicenec,
to be submitted to AA.) - To be presented at IAU Symp. 209
11CSs 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 ...
12CS 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 .....
13CS in Pne Sh 2-68
- XE630 LCO
- RA,DEC obtained from the OOPs of 7 plates plus
the GSC2-based astrometry of 3 CCD frames (CAHA,
LCO) - Time Span 47 yrs
14Results
- 53.2 /- 5.5 mas/yr SW
- Largest PN PM ever measured from the ground
(Kerber,Guglielmetti,Mignani,Roth-submitted to
AA) - One of the more precise, comparable to the ones
obtained with Hipparcos - _at_ v30 km/s --gt d100 pc
- PARALLAX measurement to grasp the CS distance
- Not possible with the GSC2 also because of the
random epoch distribution
15Follow up
- Proposal submitted to HST (FGS) in Cycle 11
(PI Kerber) - 5 visits
- Optimal periods March/September
- RA DEC
16PM of the BHC XTEJ114848I.F. Mirabel (CeA),
V.Dhawan (IAFE),R.Mignani (ESO),I.Rodriguez
(IAFE), F.Guglielmetti (STScI)
- XTEJ111848 is a galactic XRB one of the very
few BHCs - Mass Function --gt Mx gt 7 Ms
- Transient in X-ray/radio/optical
- Radio Jets (Microquasar)
- Location outside Gal Plane (d 1.8 Kpc _at_ b62
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
17Optical (GSC2)
- V18 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
- PA240/- 15
18Radio (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
- PA246/- 6
19Optical vs Radio
20BH OrbitU-97/-23 V-191/-23 W-38/-12 km/s
wrt LSR