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Star Clusters in the Galactic Center

Star Clusters in the Galactic Center. Donald F. Figer STScI. Sgr A* at 30 Workshop Green Bank W.Va March 25, 26, 2004. Collaborators. Cluster Dynamics Sungsoo Kim, KHU Star Formation History in GC Mike Rich, UCLA Gene Serabyn, JPL. Massive Stars Paco Najarro, CSIC

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Star Clusters in the Galactic Center

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  1. Star Clusters in the Galactic Center Donald F. Figer STScI Sgr A* at 30 Workshop Green Bank W.Va March 25, 26, 2004

  2. Collaborators Cluster Dynamics Sungsoo Kim, KHU Star Formation History in GC Mike Rich, UCLA Gene Serabyn, JPL Massive Stars Paco Najarro, CSIC Tom Geballe, Gemini Rolf Kudritzki, UH IMF Andrea Stolte, UF Pavel Kroupa, U. Kiel Carsten Weidner, U. Kiel Stellar Velocities Mark Morris, UCLA Eric Becklin, UCLA Ian McLean, UCLA

  3. Science Questions • What is the most massive star that can form? • Is the IMF universal? • What is the evolutionary sequence for massive stars? • What causes massive stars to "erupt"? • What is the star formation history of the Galactic Center? • How do super-star clusters form? • How do super-star clusters affect their environments? • What is the dynamical evolution of massive clusters? • What is the connection between nuclear star formation and massive central black holes?

  4. 60 pc N E GC Young Star Geography 20 cm Yusef-Zadeh, Morris, Chance 1984; Lang, Morris, Echevarria 1999

  5. K band V band 60 pc N E Digitized Sky Survey Figer 1995 Galactic Center: Extinction

  6. 1 pc N Pistol Star Arches Cluster Central Cluster E Quintuplet Cluster Galactic Center Clusters

  7. The Central Cluster Schoedel et al. 2002; Genzel et al. 2003

  8. Central cluster: Massive Stars Genzel et al. 2000; Krabbe et al. 1991, 1995

  9. Central cluster: High Resolution Spectra Figer et al. 2004, in prep.

  10. Central cluster: Radial Velocities Figer et al. 2003

  11. Radial Velocity Project

  12. Radial Velocity Project

  13. Arches Cluster Lick 3-m Figer 1995, PhD Thesis

  14. Arches Cluster Keck I 10-m Serabyn, Shupe, & FigerNature 1998, 394, 448

  15. Arches Cluster HST/NICMOS Figer et al. 1999, ApJ. 525, 750

  16. Arches Cluster VLT NAOS/CONICAStolte, A. 2003, PhD Thesis, University of Heidelberg

  17. 19” = 0.75 pc Arches Cluster: P-alpha see also: Nagata et al.1995 Cotera et al.1996 Blum et al. 2001 Figer et al. 2002, ApJ, 581, 258

  18. Arches stars: WN9 stars HeI HeI NIII NIII NIII HeII HeI/HI Figer et al. 2002, ApJ, 581, 258

  19. Arches stars: O stars 68 HI HeI 27 Figer et al. 2002, ApJ, 581, 258

  20. Arches Cluster Mass Function HST/NICMOS VLT/NAOS/CONICA Stolte et al. 2002

  21. Arches Cluster: Mass Segregation Figer et al. 1999, ApJ, 525, 750

  22. Evidence for an upper mass cutoff to the IMF 1000 M! >20 stars Arches Cluster: Upper Mass Cutoff Figer 2003, IAU 212

  23. Quintuplet cluster

  24. Quintuplet cluster: Massive Stars Figer, Najarro, & Kudritzki 2004, in prep.

  25. Quintuplet-proper Members: DWCLs? L~104.6 L T~700 K R~250 AU WR Movie from Monnier, Tuthill, & Danchi 2002, ApJ, 567, L137

  26. WC stars Figer et al. 1999, ApJ, 525, 759

  27. Pistol Star: Estimating the Luminosity • Observing on the Rayleigh-Jeans tail: • Can we guess the animal by observing its tail? +l 1 um

  28. Pistol Star: Estimating the Luminosity +l 1 um Beware!

  29. Pistol Star: Spectrum Figer et al. 1999, ApJ, 525, 759

  30. 2 Myr Lum. + model Mass tracks by Langer Figer et al. 1998, ApJ, 506, 384 Pistol Star: Mass JHKLMN + D.M. + temperature Lum.

  31. LBVs in the Quintuplet • Both the Pistol Star and FMM362 are Luminous, Blue, and Variable Pistol Star FMM362 Figer et al. 1999, ApJ, 525, 759 Geballe et al. 2000, ApJ, 530, 97

  32. LBV 1806-20 • Claim • 1-7 LPistol • 150-1000 Msun • Primary uncertainties • distance • temperature • singularity • Figer, Najarro, Kudritzki • in prep • R=22000 1.5-4.2 um • NIRSPEC/Keck

  33. LBV 1806-20 is a binary? Figer, Najarro, Kudritzki 2004, in prep.

  34. Massive Stars in GC red is estimate

  35. Star Formation History in the GC Figer et al. 2004, ApJ, 601, 319

  36. Conclusions • Massive GC clusters continuously likely form, disperse, and populate the region. • Most massive/compact young clusters in the Galaxy are in the GC • IMF is flat (at least in one cluster), and upper mass cutoff might be observed • The Pistol Star and FMM362 are amongst the most massive stars in the Galaxy

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