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* Eisenhauer et al. 2005, ApJ, in press M BH = 3.61±0.32 mill. M SOL, R 0 = 7.62±0.32 kpc Schödel et al. 2002, 2003, Eisenhauer et al. 2003, Ghez et al. 2003, 2005

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

6. two coeval disks of young stars clockwisecounter- clockwise OB (I,III) >63 (12)>55 (17) WNL+LB V 20 (7) 22 (11) WNE 2.4 (2.4) 2.5 (3.5) WC 15 (6) 20 (10) t=4±1 Myrs for both disks (Meynet 1995) percentages of different early type stars Levin & Beloborodov 2003, Genzel et al. 2003, Paumard et al. 2005, Nayakshin & Cuadra 2005

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

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

9. More flares

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

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

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

13. Summary More accurate values for mass and distance of SgrA*: M BH = 3.61±0.32 mill. M SOL, R 0 = 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