Musings about 30 Dor

download Musings about 30 Dor

of 49

  • date post

    02-Jan-2016
  • Category

    Documents

  • view

    24
  • download

    0

Embed Size (px)

description

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). - PowerPoint PPT Presentation

Transcript of 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] imageof the 30 Dor giant HII regiontaken by Walborn at CTIO-4m)

  • LMCGMCs (CO 1-0)

    Fukui et al. 2008NANTEN 4m tel.

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

  • F160W (H-band)NICMOS imagecentred on R136(1 x 1 = 15pc x 15pc)

    Andersen/HZ et al. 2009, Ap.J.

  • 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

  • R136NGC 3603Orion Nebula(to scale)

    Zinnecker & Yorke(Annual Reviews 45)

  • 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 stars9,10) stellar + dynamical evolution (future) 10 question on 30 Dor

  • 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 31.5 Myr

    origin: near LMC stellar bar, gas infall from SMC

    evolution: proto-globular cluster? staying bound?

  • 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

  • kinematic study(slit positions)HII velocity dispersion~ 60km/s over 270pc

    Chu & Kennicutt 1994Violent star formationHII-region (v_rms>c_s)

    Terlevich & Melnick 1981

  • Br (grey)

    CO (contours)Poglitsch et al. 1995

  • NIR images (JHK)

    Rubio et al. 1998

  • NIR images (JHK)red sources:protostars?

    Rubio et al. 1998

  • from Zinnecker & Yorke 2007(Annual Reviews, Vol. 45)

    SPH simulation of a turbulent100 pc 106 MO molecular cloud (Bonnell, Clark, & HZ, in prep.)

  • from Zinnecker & Yorke 2007(Annual Reviews, Vol. 45, 481)

    SPH simulation of hierarchicalcluster formation (sub-clustersin the process of wet merging)(Bonnell, Bate, & Vine 2003)Maybe the N2070/R136 clusterformed by merging of subclusters(cf. WFC3 obs. Sabbi et al. 2012)

  • Massey & Hunter 1998Weigelt & Baier 1985

  • Massey & Hunter 1998Pehlemann et al. 1992

  • R136 SE quadrant (K-band adaptive optics at ESO/3.6m)

    Brandl et al. 1996

  • 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

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

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

  • HST/WFPC2 F814Wimage of R136(A, B, C, D IMF)

    Sirianni et al. 2000

  • IMF in 2-3 pc annulus in R136

    Sirianni et al. 2000

  • Andersen et al.2007, Ap.J. subm.slope x = 1.35 (assumed)

    IMF simulationwith variable reddening

  • ESO 2.2m NIR image(NICMOS finding chart)

    Andersen et al. 2007,Ap.J. subm.

  • F160W (H-band)NICMOS imagecentred on R136(1 x 1 = 15pc x 15pc)

    Andersen/HZ et al. 2009, Ap.J.

  • Andersen et al.2009, ApJ.

  • annular IMFs(vertical arrow =completeness limit)

    Andersen et al.2009, ApJ.

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

  • 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? QUESTIONS for discussion:

  • 24m green 8m red2 MASS K-band blue

    Brandl, Chu, & Townsley(priv. comm.)

  • H green8m redChandra 0.5-2 keV blue

    Brandl, Chu, & Townsley(priv. comm.)

  • Fukui et al. 1999 Kim et al. 2003

  • Maz-Apellniz et al. 2004

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

  • Poglitsch et al. 1995 (KAO)Br (grey)

    FIR (contours)

  • The far-infraredspectral energy distributionof the 30 Dor nebula;the curve is a 75 K blackbody fit.

    Werner et al. 1978 ( based on KAO observations)

  • 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 NASAs Kuiper Airborne Observatory (KAO) C-141 with a 36-inch telescope onboard, based at NASA-Ames near San Francisco, flew from 1975 - 1996,

  • http://www.sofia.usra.edu

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

  • 30 Dor expanding shellsand kinematic features

    Chu & Kennicutt 1994

  • 30 Doradus, NGC 2070, and R136:

    a brief overview of a resolved starburst

    Hans Zinnecker (Astrophysikalisches Institut Potsdam)

    *

    *****