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Musings about 30 Dor

Musings about 30 Dor. Hans Zinnecker DSI @ SOFIA Science Center NASA-Ames Research Center Moffett Field, CA (Univ. Stuttgart, Germany). Tarantula Nebula ([SII] image of the 30 Dor giant HII region taken by Walborn at CTIO-4m).

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Musings about 30 Dor

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  1. Musings about 30 Dor Hans Zinnecker DSI @ SOFIA Science Center NASA-Ames Research Center Moffett Field, CA (Univ. Stuttgart, Germany)

  2. Tarantula Nebula ([SII] image of the 30 Dor giant HII region taken by Walborn at CTIO-4m)

  3. LMC GMCs (CO 1-0) Fukui et al. 2008 NANTEN 4m tel.

  4. 30 Doradus as seen by HST/WFC3/UVIS (courtesy Erick Young)

  5. F160W (H-band) NICMOS image centred on R136 (1‘ x 1‘ = 15pc x 15pc) Andersen/HZ et al. 2009, Ap.J.

  6. 30 Dor, NGC 2070, R136 nomenclature (to avoid confusion) 30 Dor = giant HII region (200 pc) N2070 = starburst cluster (20 pc) R136 = central cluster (2 pc) R136 core radius = 0.2 pc cf. big Galactic cluster NGC 3603

  7. R136 NGC 3603 Orion Nebula (to scale) Zinnecker & Yorke (Annual Reviews 45)

  8. 10 question on 30 Dor 1,2) initial conditions, initial location (past) 3,4) cluster IMF, SF history (num. simul.) 5, 6) feedback trigger on adjacent cloud, two-stage starburst (2nd gen, present) 7, 8) close (“hard”) binaries, runaway stars 9,10) stellar + dynamical evolution (future)

  9. Introductory summary (1) • largest star forming HII region in the Local Group • closest resolved starburst cluster ("Rosetta Stone“) • nearby (LMC at 50 kpc)  details (e.g. IMF, SFH) • high-masses: ~ 100 O-stars • stellar population: • low-masses: < 3MO pre-MS • metallicity and age: Z ~ ZO/2.5 and 3±1.5 Myr • origin: near LMC stellar bar, gas infall from SMC • evolution: proto-globular cluster? staying bound?

  10. Introductory summary (2) • stellar cluster ~ 105 MO • mass total ionised gas 4.105 MO • mol. cloud (CO) ~ 105 MO • central mass density ~ 105 MO/pc3 • total luminosity ~ 108 LO • rate of ionising Lyc photons ~ 1052 s-1 • equivalent number O3-stars ~ 100  Ltot • Ekin (HII gas,tot) ~ 1052 ergs • energetics Ekin (R136 shell) ~ 1051 ergs • Ekin provided by O-star winds, SNRs

  11. kinematic study (slit positions) HII velocity dispersion ~ 60km/s over 270pc Chu & Kennicutt 1994 Violent star formation HII-region (v_rms>c_s) Terlevich & Melnick 1981

  12. Br (grey) CO (contours) Poglitsch et al. 1995

  13. NIR images (JHK) Rubio et al. 1998

  14. NIR images (JHK) red sources: protostars? Rubio et al. 1998

  15. from Zinnecker & Yorke 2007 (Annual Reviews, Vol. 45) SPH simulation of a turbulent 100 pc 106 MO molecular cloud (Bonnell, Clark, & HZ, in prep.)

  16. from Zinnecker & Yorke 2007 (Annual Reviews, Vol. 45, 481) SPH simulation of hierarchical cluster formation (sub-clusters in the process of „wet“ merging) (Bonnell, Bate, & Vine 2003) Maybe the N2070/R136 cluster formed by merging of subclusters (cf. WFC3 obs. Sabbi et al. 2012)

  17. Massey & Hunter 1998 Weigelt & Baier 1985

  18. Massey & Hunter 1998 Pehlemann et al. 1992

  19. R136 – SE quadrant (K-band adaptive optics at ESO/3.6m) Brandl et al. 1996

  20. Reddening map of 30 Doradus calculated with an adaptive algorithm. The circles are centered in R136 with radii of 5", 15", 25", and 40". The reddening scale goes from AV=0 to AV=3.0, calculated assuming RV=3.05. North is up and east to the left; size is 133" or ~30 pc. Selman et al. 1999

  21. Selman et al. 1999 SFH of the cluster (3 bursts) Spatial distribution of stars with M> 20 MO as a function of age: green for youngest, yellow for middle-aged, and red for oldest stars (approx. 1.5, 2.5, 5 Myr). WR stars are plotted using an asterisk.

  22. slope x = 1.37 (obs. fit) Selman et al. 1999

  23. HST/WFPC2 F814W image of R136 (A, B, C, D  IMF) Sirianni et al. 2000

  24. IMF in 2-3 pc annulus in R136 Sirianni et al. 2000

  25. slope x = 1.35 (assumed) IMF simulation with variable reddening Andersen et al. 2007, Ap.J. subm.

  26. ESO 2.2m NIR image (NICMOS finding chart) Andersen et al. 2007, Ap.J. subm.

  27. F160W (H-band) NICMOS image centred on R136 (1‘ x 1‘ = 15pc x 15pc) Andersen/HZ et al. 2009, Ap.J.

  28. Andersen et al. 2009, ApJ.

  29. annular IMFs (vertical arrow = completeness limit) Andersen et al. 2009, ApJ.

  30. massive eclipsing binaries in R136 Massey et al. 2002 SB2E: 57 MO + 23 MO SB2E: 40 MO + 32 MO

  31. QUESTIONS for discussion: • definition "starburst" (SFR density or lum. density) • 30 Dor: initial conditions? (irrecognisable after MSF) • how to form 100 massive stars in such a small volume? • R136: truncated IMF? one-shot or multi-episode burst? • 5) R136: initial mass segregation and stellar collisions? • (likely conditions for progenitor of GRB or even IMBH?) • 6) 30 Dor: a model for the origin of globular clusters?

  32. 24μm green 8μm red 2 MASS K-band blue Brandl, Chu, & Townsley (priv. comm.)

  33. H green 8μm red Chandra 0.5-2 keV blue Brandl, Chu, & Townsley (priv. comm.)

  34. Fukui et al. 1999 Kim et al. 2003

  35. Maíz-Apellániz et al. 2004

  36. The structure of NGC 604 WFPC2 (Hunter et al. 1996) IRAC #4 (6.5-9.4m) (Brandl et al. 2004)

  37. Br (grey) FIR (contours) Poglitsch et al. 1995 (KAO)

  38. The far-infrared spectral energy distribution of the 30 Dor nebula; the curve is a 75 K blackbody fit. Werner et al. 1978 ( based on KAO observations)

  39. High-flying aircraft --above 40,000 ft -- can observe most of the infrared universe • Airborne infrared telescopes can be more versatile -- and much less expensive -- than space infrared telescopes NASA’s Kuiper Airborne Observatory (KAO) C-141 with a 36-inch telescope onboard, based at NASA-Ames near San Francisco, flew from 1975 - 1996 ,

  40. http://www.sofia.usra.edu

  41. References Werner et al. 1978 Kennicutt 1984 Melnick 1985 Weigelt and Baier 1985 Walborn and Blades 1987 Kennicutt and Chu 1988 Hyland et al. 1992 Pehlemann et al. 1992 de Marchi et al. 1993 Parker 1993 Parker and Germany 1993 Chu and Kennicutt 1994 Malumuth and Heap 1994 Moffat et al. 1994 Hunter et al. 1995 Poglitsch et al. 1995 Brandl etal. 1996 Hunter et al. 1996 Massey and Hunter 1998 Rubio et al. 1998 Bosch et al. 1999 Fukui et al. 1999 Portegies Zwart et al. 1999 Selman et al. 1999 Zinnecker et al. 1999 Grebel and Chu 2000 Sirianni et al. 2000 Bosch et al. 2001 Massey et al. 2002 P. Zwart & McMillan 2002 Zinnecker et al. 2002 Kim et al. 2003 Maíz-Apellániz et al. 2004 Maercker and Burton 2005 Selman and Melnick 2005 Koen 2006 Townsley et al. 2006 Zinnecker 2006 Andersen et al. 2007 Zinnecker and Yorke 2007

  42. 30 Dor expanding shells and kinematic features Chu & Kennicutt 1994

  43. 30 Doradus, NGC 2070, and R136: a brief overview of a resolved starburst Hans Zinnecker (Astrophysikalisches Institut Potsdam)

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