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VLT/FLAMES survey of massive stars in 30 Doradus

VLT/FLAMES survey of massive stars in 30 Doradus. Alex de Koter

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VLT/FLAMES survey of massive stars in 30 Doradus

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  1. VLT/FLAMES survey of massive stars in 30 Doradus Alex de Koter Chris Evans, Hugues Sana, William Taylor, V. Henault-Brunet, J/ Bestenlehner, S. Simon-Diaz, P.A. Crowther, S.E. De Mink, P.L. Dufton, M. Gieles, A. Herrero, N. Langer, D.J. Lennon, J. Maiz-Apellaniz, N. Markova, F. Najarro, J. Puls, O.H. Ramirez, J.Th. Van Loon, J.S. Vink, N.R. Walborn, et al.
  2. Massive stars as cosmic engines Re-ionization of the universe Nuleosynthesis Chemical processing in ISM Star formation Standard candles First Stars Galaxyformation & evolution Supernovae & gamma-raybursts Double compacts Neutron Stars & Black Holes Star cluster dynamics & evolution Galacticoutflows MOS meeting A'dam, October 2012
  3. ? BIG THE To understand…… Questions … massive stars as a population, in context withtheir environment … (outcome of) formationof single sources, binariesandentirepopulations … evolutionof single sources andbinaries … distributionsof finalproducts, SNe (GRBs) types andNSs & BHs … evolution of young star clusters in terms of dynamics, feedback, integrated light, multiplicityproperties … all these thingsthroughoutcosmological time, back to the First Stars and First Binaries. MOS meeting A'dam, October 2012
  4. ? BIG THE To understand…… Questions … the role of massive star in/towards the formation of life… through nucleosynthesis, chemical processing of complex molecules, imposingchiralpreference on organicmoleculesthrough UV illumination MOS meeting A'dam, October 2012
  5. How to address these questions: Homogeneous analysis of large populations of massive stars in different environments, usingmulti-object spectrographs ..in combinationwithtailoredtheoretical research Fibre Large Array Multi Element Spectrograph (FLAMES) MOS meeting A'dam, October 2012
  6. How to address these questions: Homogeneous analysis of large populations of massive stars in different environments, using multi-object spectrogaphs Galaxy Cyg OB2 NGC 6611 NGC 3293 NGC 4755 FLAMES Survey of Massive Stars Evans et al. 2005 LMC N11 (LH9 & LH10) NGC 2004 SMC NGC 346 NGC 330 MOS meeting A'dam, October 2012
  7. How to address these questions: Homogeneous analysis of large populations of massive stars in different environments, using multi-object spectrogaphs NGC 6611 NGC 3293 NGC 4755 VLT-FLAMES Tarantula Survey Evans et al. 2011, Sana et al. 2013 N11 (LH9 & LH10) NGC 346 MOS meeting A'dam, October 2012
  8. How to address these questions: Homogeneous analysis of small numbers of massive stars in sub-SMC metallicity environments, using X-shooter NGC 6611 NGC 3293 NGC 4755 Dutch X-Shooter GTO program Kaper & Groot et al. N11 (LH9 & LH10) X-Shooter NGC 346 MOS meeting A'dam, October 2012
  9. ? BIG THE To understand…… Questions …massive stars as a population, in context withtheir environment … (outcome of) formationof single sources, binariesandentirepopulations … evolutionof single sources andbinaries … distributionsof finalproducts, SNe (GRBs) types andNSs & BHs … evolution of young star clusters in terms of dynamics, feedback, integrated light, multiplicityproperties … all these thingsthroughoutcosmological time, back to the First Stars and First Binaries. MOS meeting A'dam, October 2012
  10. 22nd Anniversary of Hubble Space TelescopeMay 2012 HST-GO 12499 (PI: D.A. Lennon) MOS meeting A'dam, October 2012
  11. MOS meeting A'dam, October 2012
  12. MOS meeting A'dam, October 2012
  13. ? BIG THE To understand…… Questions … massive stars as a population, in context withtheir environment … (outcome of) formationof single sources, binariesandentirepopulations … evolutionof single sources andbinaries … distributionsof finalproducts, SNe (GRBs) types andNSs & BHs … evolution of young star clusters in terms of dynamics, feedback, integrated light, multiplicityproperties … all these thingsthroughoutcosmological time, back to the First Stars and First Binaries. MOS meeting A'dam, October 2012
  14. In ourgalaxythe outcome of massive star formation is suchthat Intrinsicbinaryfrequencyis 69% forP < 1500d, 71% of O stars experiencebinaryinteraction, of which 24% merge, being in systems with P < 6d Mass ratio distributionMprimary/Msecundary is flat MOS meeting A'dam, October 2012
  15. MOS meeting A'dam, October 2012
  16. 33% of O stars are stripped of theirenvelopebeforetheyexplode as hydrogen-deficientcorecollapseSNe (Ib, Ic, IIb), close toobservedfraction of 37% of allcorecollapseSNe. 1/3th of binaries end in merger, whichmaybe a channeltoproduceverymassive stars (WNh stars, Minit ~ 150-300 M) MOS meeting A'dam, October 2012
  17. ? BIG THE To understand…… Questions … massive stars as a population, in context withtheir environment … (outcome of) formationof single sources, binariesandentirepopulations … evolutionof single sources andbinaries … distributionsof finalproducts, SNe (GRBs) types andNSs & BHs … evolution of young star clusters in terms of dynamics, feedback, integrated light, multiplicityproperties … all these thingsthroughoutcosmological time, back to the First Stars and First Binaries. MOS meeting A'dam, October 2012
  18. FLAMES Survey of Massive Stars What are we after? where does the mainsequence end? rotationandrotationalmixing massloss in stellarwinds magneticfields? binaries MOS meeting A'dam, October 2012
  19. FLAMES Survey of Massive Stars Big samples allowyouto “see” the stellarinterior Where does mainsequence end? (= overshootingcalibration) Hunter et al. 2009, Brott et al. 2011 MOS meeting A'dam, October 2012
  20. ? BIG THE To understand…… Questions … massive stars as a population, in context withtheir environment … (outcome of) formationof single sources, binariesandentirepopulations … evolutionof single sources andbinaries … distributionsof finalproducts, SNe (GRBs) types andNSs & BHs … evolution of young star clusters in terms of dynamics, feedback, integrated light, multiplicityproperties … all these thingsthroughoutcosmological time, back to the First Stars and First Binaries. MOS meeting A'dam, October 2012
  21. Mass-loss at sub-SMC metallicity Z ~ 0.14 Zdwarfgalaxies in Local Group Low line-of-sightextinction Young stellarpopulationsrich in massive stars IC 1613, WLM & NGC 3109 Six brightest O stars observedwith X-Shooter NGC 3109 @ 1.3 Mpc WLM @ 995 kpc IC 1613 @ 720 kpc
  22. Mass-loss at sub-SMC metallicity Tramper et al. 2011
  23. Identification of massive stars in IC 1613 Tramper et al. 2011 New Garcia et al. 2009 MOS meeting A'dam, October 2012
  24. ? BIG THE To understand…… Questions … massive stars as a population, in context withtheir environment … (outcome of) formationof single sources, binariesandentirepopulations … evolutionof single sources andbinaries … distributionsof finalproducts, SNe (GRBs) types andNSs & BHs … evolution of young star clusters in terms of dynamics, feedback, integrated light, multiplicityproperties … all these thingsthroughoutcosmological time, back to the First Stars and First Binaries. MOS meeting A'dam, October 2012
  25. WNh stars Exceptionally massive (a1, a2, a3) = (Minit ~ 320, 240, 165 M) Also stars in core of NGC 3603 found to be very massive, up to Minit ~ 170 M de Koter et al. 1997, Crowther et al. 2010 VLT MAD K image Campbell et al. 2010 MOS meeting A'dam, October 2012
  26. Example of a serendipitousdiscovery WNhstars Exceptionally massive (a1, a2, a3) = (log L/L ~ 6.94, 6.78, 6.58) Also stars in core of NGC 3603 found to be very massive, up to Minit ~ 170 M de Koter et al. 1997, Crowther et al. 2010 VLT MAD K image Campbell et al. 2010 MOS meeting A'dam, October 2012
  27. The monster maybehiding! WN5h star VFTS 682 Exceptionally massive WN5h star (Minit ~ 200 M); the first one of this type to be found outside of a massive young cluster Spectroscopic “twin” of R136a3 (Minit ~ 240 M) Bestenlehner et al. 2011 MOS meeting A'dam, October 2012
  28. The monster maybehiding! WN5h star VFTS 682 The star is in (the line-of-sight toward) an active star forming region Did it form in situ or is it a slow runaway object (~40 km/sec) from R136? In either case, this poses an interesting challenge for massive star formation theory or dynamical ejection scenarios Bestenlehner et al. 2011 MOS meeting A'dam, October 2012
  29. Spectroscopic requirements E-ELT/MOS High throughput, high sensitivity Large spectral coverage at once (> 100 A), even at high spectral resolution, so more detector "real estate" than applied in FLAMES Spectroscopy down to 3800 (Ca H&K) at least. "We could live with a non-cryogenic instrument (i.e. only in J and H), like X-shooter” R ~ 3000-5000 at lambda > 8000 A for dust embedded populations R ~ 8,000-20,000 in optical and near-IR for detailed abundance studies Ability to take advantage of the AO provided by the telescope "Tricky trade between multiplicity, wavelength coverage and spectral resolution, however, the more (multiplicity) the better". MOS meeting A'dam, October 2012
  30. Conclusions VLT/FLAMES has lead togreat break-throughs in ourunderstanding of massive stars (and has raisedmany new questions) Though X-Shooterallowsustoexplore the brightest stars in (metal poor) dwarfgalaxies in and even beyond the Local Group; it does notallowfor studies of large populations of massive stars To do so, E-ELT/MOS is key. Only way toperform studies of populations of massive stars in environments representative of the earlyuniverse And, E-ELT/MOS will have greatpotentialforserendipitousdiscoveries MOS meeting A'dam, October 2012
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