GSC2 Science Projects @ ESOGSC2 Science Projects @ ESO

7th GSC2 Meeting7th GSC2 Meeting

20012001

R.MignaniR.Mignani

ESOESO

On Going ProjectsOn 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)

GSC2 ID of ROSAT sourcesR.Mignani (ESO),W.Voges, F.Guglielmetti (MPE),

S. Covino (OAB) et al.

GSC2 ID of ROSAT sourcesR.Mignani (ESO),W.Voges, F.Guglielmetti (MPE),

S. Covino (OAB) et al.

RASS and Pointed ObservationsRASS and Pointed Observations GSC2, 2MASS, NVSS GSC2, 2MASS, NVSS X-correlations with X-ray Cats fromX-correlations with X-ray Cats from PSPC & HRI observationsPSPC & HRI observations

RXH (11,000-19,000) RXH (11,000-19,000) R=5” R=5” RXP (95,000) RXP (95,000) R=10” R=10” RASS/BSC (18,800 sources) RASS/BSC (18,800 sources) R=30” R=30” RASS/FSC (106,000 sources)RASS/FSC (106,000 sources) R=30” R=30”

Better understanding of the G/EG X-ray source populationBetter understanding of the G/EG X-ray source population

Statistical studies Statistical studies Selection of objects with NO opt ctp (e.g. radio silent INSs)Selection of objects with NO opt ctp (e.g. radio silent INSs)

StrategyStrategy

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 Fx/Fopt vs HR A “decision tree like” algorithm must be implemented to A “decision tree like” algorithm must be implemented to

automatize the ID automatize the ID

StatusStatus

X-correlations with X-ray Cats are in progress ...X-correlations with X-ray Cats are in progress ... Tests done with the GSC2.1 ...Tests done with the GSC2.1 ... Definition of algorythms for the decision tree ...Definition of algorythms for the decision tree ... Definition of algorythms for the MC Phot Obj Class ... Definition of algorythms for the MC Phot Obj Class ... Whole, MC, sky coverage down to the plate Whole, MC, sky coverage down to the plate

limiting magnitude is required asap to:limiting magnitude is required asap to: better explore the X/Opt parameter spacebetter explore the X/Opt parameter space avoid continuous repetitions and updatesavoid continuous repetitions and updates

RXH Ids --> paper in preparation (Mignani, Covino et al.)RXH Ids --> paper in preparation (Mignani, Covino et al.)

The Local QSO Lum FS.Cristiani, A.Grazian, R.Mignani, A.Wicenec (ESO)

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

Tidal Tails in GCsS.Zaggia (ESO,OATs), R.Mignani (ESO), R.Smart (OATo)

Tidal Tails in GCsS.Zaggia (ESO,OATs), R.Mignani (ESO), R.Smart (OATo)

Evidence for tidal disruption Evidence for tidal disruption

in GCsin GCs Identify GC objects among Identify GC objects among

fields starsfields stars Photometry approachPhotometry approach CM diagram to characterize the CM diagram to characterize the

GC sequenceGC sequence Comparison with CM of field Comparison with CM of field

stars to isolate GC starsstars to isolate GC stars Astrometric approachAstrometric approach

StatusStatus A sample of 60 Southen GCs selectedA sample of 60 Southen GCs selected with d< 20 kpc and |b|>20 deg GCs identified in GSC2 plates and Bj, F doublets selected GCs identified in GSC2 plates and Bj, F doublets selected Obj in a 2x2 deg regions around GCs extracted from the GSC2 plates Obj in a 2x2 deg regions around GCs extracted from the GSC2 plates GC core stars are not detectable by the GSC2 pipelineGC core stars are not detectable by the GSC2 pipeline Off-line alghoritms (e.g. DAOPHOT) run on the images Off-line alghoritms (e.g. DAOPHOT) run on the images GSC2 astrometry used to match GC stars in doubletsGSC2 astrometry used to match GC stars in doublets GC sequence is not well definedGC sequence is not well defined D-I calibration required to DAOPHOTD-I calibration required to DAOPHOT Project idle .....Project idle .....

Planetary Nebulae & Central StarsF.Kerber (ST-ECF), R.Mignani (ESO), F.Guglielmetti (STScI,MPE),

A.Wicenec (ESO)

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 PNeMC Identification of CSs in PNe

(only 30% known)(only 30% known) PM measurements and Distance PM measurements and Distance

Estimates for (un)identfied CSs Estimates for (un)identfied CSs

(only 5% known) (only 5% known)

PNe Positioning PNe Positioning

A SkyCat based Procedure set up to automatize DSS2/GSC2 - FCs comparisons & identifications has been implemented

PNe/CS coordinates classified:PNe/CS coordinates classified:

CS: PN extended, CS resolvedCS: PN extended, CS resolved STELLAR: PN is stellar-likeSTELLAR: PN is stellar-like PHOTO: PN extended, CS not resolvedPHOTO: PN extended, CS not resolved GEO: PN extended, CS ambiguousGEO: PN extended, CS ambiguous

Position confidence graded Position confidence graded Identification Process COMPLETED - (GSC2.1+GSC2.2)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

CSs IdentificationCSs Identification

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

CS Proper MotionsCS Proper Motions

Wait until GSC2.3 for a complete PM survey Wait until GSC2.3 for a complete PM survey A list of candidate PM CSs already producedA list of candidate PM CSs already produced However, off-the-catalogue PMs can be pursued for most However, off-the-catalogue PMs can be pursued for most

interesting cases interesting cases e.g. CS in PN Sh 2-68 .....e.g. CS in PN 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

CS in Pne Sh 2-68CS in Pne Sh 2-68

ResultsResults

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

Follow upFollow up

Proposal submitted to HST (FGS) in Cycle 11 (PI: Kerber)Proposal submitted to HST (FGS) in Cycle 11 (PI: Kerber) 5 visits5 visits Optimal periods March/September Optimal periods March/September

RA RA

DECDEC

PM of the BHC XTEJ1148+48I.F. Mirabel (CeA), V.Dhawan (IAFE),R.Mignani (ESO),I.Rodriguez

(IAFE), F.Guglielmetti (STScI)

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: XTEJ1118+48 is a galactic XRB: one of the very few BHCsone of the very few BHCs Mass Function --> MMass Function --> Mxx > 7 Ms > 7 Ms

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

Optical (GSC2)Optical (GSC2)

V=18 Opt Ctp (quiescence), K7V=18 Opt Ctp (quiescence), K7 4 Epochs selected spanning 43 yrs (1954-1996)4 Epochs selected spanning 43 yrs (1954-1996) Rel PM - correction for galactic rotation wrt EG reference frameRel PM - correction for galactic rotation wrt EG reference frame Correction for Sun PMCorrection for Sun PM Ra=-10.5+/-3.2 mas/yrRa=-10.5+/-3.2 mas/yr Dec=-5.9+/-3.2 mas/yrDec=-5.9+/-3.2 mas/yr 12.0+/- 3.2 mas/yr12.0+/- 3.2 mas/yr PA=240+/- 15PA=240+/- 15

Radio (VLBA)Radio (VLBA)

Timespan 3 months (May-July 2000)Timespan 3 months (May-July 2000) Two independent measurements (1.5 GHz and 8.4 GHz)Two independent measurements (1.5 GHz and 8.4 GHz) PM wrt EG calibratorsPM wrt EG calibrators Correction for Parallax and PM of the SunCorrection for Parallax and PM of the Sun Ra=-16.8+/-1.6 mas/yrRa=-16.8+/-1.6 mas/yr Dec=-7.4+/-1.6 mas/yrDec=-7.4+/-1.6 mas/yr 18.3+/- 1.6 mas/yr18.3+/- 1.6 mas/yr PA=246+/- 6PA=246+/- 6

Optical vs RadioOptical vs Radio

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

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