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A Search for new Active Stars in the Galaxy via VOs CATS & USNO N. Kardashev Astro Space Centre, Moscow, Russia O. B. Slee ATNF, Sydney, Australia M. Rupen National Radio Oservatory, Soccoro, USA R. Stathakis Anglo-Australian Observatory, Sydney, Australia E. Barsukova Special Astrophysical Observatory, N. Arkhyz, Russia V. Goransky Sternberg Astronomical Institute, Moscow, Russia J. Pacheco Observatory d’Cote Azur, Nice, France D. Gabuzda Cork University College, Ireland R. Ojha ATNF, Sydney, Australia I. Chandra GMRT, Bangalor, India E. Budding Carter Observatory, New Zealand G. Tsarevsky ATNF, Sydney, Australia & Astro Space Centre, Moscow, Russia

Aus-VO WORKSHOP2003

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NB: in the presentation, those slides describing virtual

observations in the project have a light blue background like

this one -

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NB: Those slides dedicated to real observations are just white

like this one.

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Microquasar - by definition, - it is an X-ray binary (XRB) which exhibits radio jets, sometimes with relativistic speed.

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Project Description :

= astro-ph/0110511

In: The Physics of Cataclysmic Variables and Related Objects, ASP Conf. Ser., v. 261, eds. B. Gänsicke et al., p. 301, 2002and In: New Directions for Close Binary Studies: “The Royal Road to the Stars”, Publ. of Canakkale University Astrophysics Research Center, vol. 3, p. 246, 2003

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Project’s flow chart: Stage I – selection of the ROSAT

hard spectrum sources [VO].

Stage II – tentative radio IDs [VO]. Stage III – high resolution radio

observations.

Stage IV – optical IDs [VO]; . galaxies to be discarded.

Stage V – optical spectroscopy.

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Stage I – selection in X-ray from the Bright ROSAT Sources Catalogue

(1RXS)

[ W. Voges et al., A&A 349, 389, 1999 ] The main selection criterium = = Motch’s Strip : 0.90 ≤ HR1 ≤ 1.00 0.25 ≤ HR2 ≤ 1.00 [ C. Motch et al., A&A 132, 341, 1998 ] AND Sources in the Galactic Plane:

|b| < 200

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Stage II – tentative identifications in Radio Surveys:

• NVSS (VLA, D-configuration) 1.4 GHz

• 87GB/GB6/PMN (single dish) 4.8 GHz -----&---- radio variability checking

[GB6] = { [1987GB]2 + [1989GB]2 } -2

(J. J. Condon, Private comm.)

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Stage II:

The X-ray-Radio cross-identifications have been made using CATS : a major collection of databases gathered and maintained by S. Trushkin et al. of the Special Astrophysical Observatory

http://cats.sao.ru

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SIMBAD :- no GB6

- no NVSS - no 2MASS

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N E D : no multi-source query on the web;

no 2MASS (only 2MASX)

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C A T S : ► A complete collection of

radio catalogs (191).► Multi-source query.

► 2MASS & USNO Catalogs

(not Charts/Images). ► VOTable format – to be

implemented soon. http://cats.sao.ru

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C A T S :

SUMSS is already there(with a multiple position query,

of course).

http://cats.sao.ru

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Stage III: Targeted radio observations

(with a sub-arcsec coordinate precision):

• VLA

A-configuration, 1.4 & 4.8 GHz • ATCA

6-km configuration, 4.8 & 8.6 GHz

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Stage IV:

Radio-Optical Identifications by the Digital Sky Surveys (DSS)

[obvious galaxies were discarded]

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The best DSS access among many others is …

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A Virtual Observatory of the US Naval Observatory,

Flagstaff Station, Arizona:

USNO PMMhttp://www.nofs.navy.mil/projects/pmm/

Observables: coordinates; charts; images; B, R, I magnitudes at two epochs,

(hence variability) ; image analysis (star/galaxy);

proper motions (!)

of ~1,000,000,000 objects,

release B1.0, 2003.

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USNO PMM: ►flexible multiparameter

interface;► multidata output.

The best, but not perfect: no multisource query.

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Stage V:

A moderate resolution optical spectroscopy of 60 candidates

byAAT (4 m) AustraliaBTA (6 m) RussiaVLT (8 m) Chile

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Have been observed:• ААТ : spectroscopy of 12 objects• BТА : spectroscopy of 34• VLT : spectroscopy of 6======================================================== Total: 52 + 8 objects to be observed

Preliminary results:=============================================================== Stars 12 Featureless spectra 28 Sy1/Sy2/AGN 9 QSO 3=============================================================== .

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.

========================================================

Preliminary results:=============================================================== Stars 12 Active stars =New Featureless spectra 28 if BL Lacs =New Sy1/Sy2/AGN 9 =New QSO 3 =New=============================================================== .

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========================================================

Preliminary results:=============================================================== Stars 12 Featureless spectra 28 BL Lacs ? Sy1/Sy2/AGN 9 QSO 3 =============================================================== .

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‘Featureless’ objects 28

?

They all arestar-like (i.e., not extended in optics),

bright & hard X-ray emittersand radio sources [due to selection criteria].

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‘Featureless’ objects 28↓

Galactic ? Extragalactic ?

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‘Featureless’ objects 28 ↓

If extragalactic – BL Lacs behind the GP.

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‘Featureless’ objects 28

If Galactic –– they could be a NEW type of objects.

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‘Featureless’ objects 28

↓ EGRET sources

in the Galactic plane?

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No

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‘Featureless’ objects 27

↓ PROPER MOTION ?

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Yes !

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From USNO-PMM, six of 28 ‘featureless’ objects have p.m.

≥ 3-σ, e.g. :

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PROPER MOTION : ↓

MCQC J1910+28

μRA = – 0.016 ± 0.002 arcsec/y

μDEC = – 0.010 ± 0.000 arcsec/y

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But we have to get a close look now