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Scientific results from RTT150 obtained at IKI

Mikhail Pavlinsky (IKI, Moscow). Scientific results from RTT150 obtained at IKI. The main scientific programs. X-ray selected distant galaxy clusters - 400d survey Optical identifications of INTEGRAL hard X-ray sources Gamma-ray bursts afterglows

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Scientific results from RTT150 obtained at IKI

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  1. Mikhail Pavlinsky (IKI, Moscow) Scientific results from RTT150 obtained at IKI

  2. The main scientific programs • X-ray selected distant galaxy clusters - 400d survey • Optical identifications of INTEGRAL hard X-ray sources • Gamma-ray bursts afterglows • Fast photometry of BH, NS and WD in X-ray binaries • More . . .

  3. 400d galaxy cluster survey Clusters are detected in X-rays and then identified in optical with RTT150 ROSAT 0.5-2 keV image point sources clusters RTT150, R band, cluster at z=0.7

  4. 400d galaxy cluster survey The largest catalog of distant massive clusters The volume of 400d survey at 0.35<z<1 is comparable with that of Abell catalog in the local Universe. Most distant and massive clusters are the legacy project (~1Msec) of CHANDRA (PI Vikhlinin) RTT150 is the main telescope used for direct imaging of 400d clusters in Northern hemisphere Burenin et al. 2007, Astrophysical Journal Supplement. http://hea.iki.rssi.ru/400d/

  5. Power of dark energy constrains from 400d survey Accuracy of dark energy constraints from 400d is comparable to those from WMAP, SNIa and BAO Vikhlinin et al. 2008a, Astrophysical Journal, submitted Vikhlinin et al. 2008B, Astrophysical Journal, submitted

  6. Gamma ray bursts afterglows GRB030329 Currently the most cited paper based on RTT150 data: Burenin et al. 2003, Astronomy Letters

  7. INTEGRAL All Sky Survey Optical identifications of newly discovered INTEGRAL sources: 26 new INTEGRAL sources are identified with RTT150 Among them 20 out of ~100 AGNs in INTEGRAL All Sky Survey Future plans: Galactic bulge LMXBs - grav. waves emitters. (CHANDRA localizations are granted: PI Revnivtsev)

  8. A major part of new INTEGRAL sources are strongly absorbed HMXB AGN/SY2

  9. Identification of puzzling INTEGRAL sources NII Ha NGC973 -- edge-on nearby Sy2 active nucleus, z=0.0162. Previously unknown as AGN due to very weak emission lines, absorbed in the disk of the galaxy. Ha Sy1 AGN at z=0.037, strongly absorbed in Galactic plane the magnitude is =~ 20.5 (!)

  10. LMXB The burst profile, bin size 10 sec GS 1826-264 clock burster, ~18m Reprocessing of X-ray bursts = > size of the accretion disk Optical spectrum – no lines! Very compact optical companion! Accretion from white dwarf? Source of gravitational waves?

  11. SS433 Fast photometry, power spectra of accreting sources Accretion disk variability. Crosscorrelation with X-rays Revnivtsev et al. 2004, A&A Revnivtsev et al. 2006. A&A

  12. Dark dusty clouds Deep optical photometric coverage of ultradeep galactic CHANDRA field (1Msec, PI Revnivtsev) CHANDRA FOV Fields of low interstellar extinction

  13. RTT150 bibliography 2003 - 2008 Publications with co-authors from IKI: - 25 refereed papers - 79 GCN circulars - 14 Astronomy telegrams about 300 references in ADS

  14. Plans for new instrumentation for RTT150 New fast EMCCD, time resolution ~ down to 2-3 msec

  15. Magneto-rotational instability – main ingredient of the accretion! Still no comparison with observations For its study we need to go up to Keplerian time scales in the inner disk. Currently impossible in X-rays > 1кHz for NS!

  16. Accreting white dwarfs: Keplerian time scale at the inner edge of the disk ~0.1-1 Hz. Unique possibilities in optical band! Accreting white dwarfs are bright in optics. But! We need to have time resolution ~10-100-500 Hz!

  17. Magnetic accretion Instabilities in accretion column: time scale~size/speed of sound ~ 10000km/1-2x000 km/sec ~ 10-100 Hz! Start of the eclipse (=>position of poles) SALT

  18. Imaging camera: VLT/ULTRACAM 50 Hz KECK 30 Hz WHT/ULTRACAM 50 Hz SALT/SALTICAM 20 Hz Very fast timing: OPTIMA (MPE) MPPP(SAO, BTA 6m) BUT! No imaging. No correction for atmospheric influence. => No power spectra + Very low photon telemetric throughput!

  19. Planned for RTT150 ANDOR iXon+ EMCCD chip, effectively zero readout noise: Full frame readout rate ~30Hz Strip readout rate ~up to 500-600Hz! Planned primary targets: bright CVs (m~13-8) Up to tens of millions photons per second!

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