GSC2 Science Projects ESO

1
GSC2 Science Projects _at_ ESO

• 7th GSC2 Meeting
• 2001
• R.Mignani
• ESO

2
On 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)

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 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)

4
Strategy

• 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

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 --gt 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 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 .....

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 (gt2000
  entries)
• MC Identification of CSs in PNe
• (only 30 known)
• PM measurements and Distance
• Estimates for (un)identfied CSs
• (only 5 known)

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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

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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 ...

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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 .....

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CS 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

14
Results

• 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

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Follow up

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

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PM 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

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Optical (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

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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
• PA246/- 6

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Optical vs Radio
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BH OrbitU-97/-23 V-191/-23 W-38/-12 km/s
wrt LSR