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SgrA* and the central cluster in NIR

SgrA* and the central cluster in NIR. S. Trippe, T. Ott, F. Eisenhauer, T. Paumard, F. Martins, S. Gillessen, R. Genzel, R. Schödel, A. Eckart, T. Alexander, S. Nayakshin. Observations. Imaging: NAOS/CONICA. Spectroscopy: SINFONI. Tracking SgrA*.

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SgrA* and the central cluster in NIR

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  1. SgrA* and the central cluster in NIR S. Trippe, T. Ott, F. Eisenhauer, T. Paumard, F. Martins, S. Gillessen, R. Genzel, R. Schödel, A. Eckart, T. Alexander, S. Nayakshin

  2. Observations Imaging: NAOS/CONICA Spectroscopy: SINFONI

  3. Tracking SgrA* Schödel et al. 2002, 2003, Eisenhauer et al. 2003, Ghez et al. 2003, 2005 MBH = 3.61±0.32 mill. MSOL , R0 = 7.62±0.32 kpc Eisenhauer et al. 2005, ApJ, in press

  4. 0.5” Deepening the “paradox of youth”: Nearly all S-stars are B main sequence stars Ghez et al. 2003, Eisenhauer et al. 2005

  5. t=4±1 Myrs for both disks (Meynet 1995) two coeval disks of young stars percentages of different early type stars Levin & Beloborodov 2003, Genzel et al. 2003, Paumard et al. 2005, Nayakshin & Cuadra 2005

  6. IRS34W: LBV, not LBV or in between? IRS34W S. Trippe, F. Martins, T. Ott, T. Paumard, et al. 2005 (A&A submitted)

  7. New flares: April 29, 2004 UT 09:14:25 UT 08:30:04

  8. More flares

  9. short-time variability in infrared flares Genzel et al. 2003, Nature 425, Ghez et al. 2004 ApJL, Eckart et al. 2005

  10. a’=0.52 (±0.1,±0.07,±0.14) SgrA* flare variability and evidence for significant BH spin 2003 FFT Scargle / Vaughan Genzel et al. 2004, Aschenbach et al. 2004,Benlloch et al. 2001, Scargle 1982, Vaughan 2004, Trippe, Gillessen et al. 2005

  11. t=0 t=60 t=116 IR SED of weak flares SINFONI 2004: Eisenhauer et al. 2005

  12. Summary • More accurate values for mass and distance of SgrA*: MBH = 3.61±0.32 mill. MSOL , R0 = 7.62±0.32 kpc • More information on stellar populations and dynamics: star disks, the “paradox of youth”, LBV candidates • More NIR SgrA* activity: first NIR spectra of flares, (quasi-)periodicities

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