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Star Formation in the Milky Way and its Neighbors in the Mid-IR

Star Formation in the Milky Way and its Neighbors in the Mid-IR. Chris Wilson McMaster University. Outline. Catching massive star formation “in the act” Forming massive star clusters in nearby galaxies Theme: synergies between JWST and FIR/submm telescopes (Herschel, ALMA).

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Star Formation in the Milky Way and its Neighbors in the Mid-IR

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  1. Star Formation in the Milky Way and its Neighbors in the Mid-IR Chris Wilson McMaster University

  2. Outline • Catching massive star formation “in the act” • Forming massive star clusters in nearby galaxies Theme: synergies between JWST and FIR/submm telescopes (Herschel, ALMA)

  3. SED of a massive young stellar object ALMA Herschel JWST Figure from Beuther et al. 2010, A&A

  4. Integrated SEDs of galaxies ALMA JWST Herschel Figure from Galliano 2004, PhD thesis

  5. The advantage of angular resolution:M81 near the dust emission peak Spitzer MIPS 160 um Herschel PACS 160 um (Gordon et al. 2004) (Bendo et al. submitted)

  6. Searching for buried protostars:Not all “Starless cores” are starless • Spitzer 24 um observations of L1521f from c2d survey reveal a protostar in an evolved “starless” core Bourke et al. 2006, ApJ

  7. Catching the start of high-mass star formation • Infrared dark cloud with an IRAS protostar • 24-500 um reveals new protostar plus apparently starless cores Beuther et al., 2010, A&A

  8. Many candidates from Herschel surveys • HOBYS project mapping massive GMCs within 2 kpc (Motte et al. 2010, A&A) • Example: NGC 7538 imaging reveals cores and filaments (Reid et al., in prep.) 20’

  9. Sites of Massive Star Formation in the LMC Spitzer: R/G/B= 24, 8, 4.5 um Indebetouw et al. 2008, AJ

  10. SEDs and luminosity function • Lots of molecular gas but little evidence of star formation before Spitzer observations • Sensitive to protostars > 3 Mo N Indebetouw et al. 2008 Lo

  11. Massive Young Stellar Objects in the LMC • Spitzer SAGE discovered 1800 massive YSO candidates (Whitney et al. 2008, Gruendl & Chu 2009) • First Herschel strip reveals 207 embedded candidate YSOs (40% previously unknown) Sewio et al. 2010 A&A

  12. The youngest massive protostars in the LMC • SAGE survey missed youngest embedded sources since only went to 24 um • Spectroscopic confirmation of YSOs through ice absorption (or maybe Silicate or PAH emission) • 300 YSOs confirmed with Spitzer (i.e. van Loon et al. 2010, AJ) Sewio et al. 2010

  13. Mid-IR Imaging and Spectroscopy with JWST • Spectroscopic confirmation of lower luminosity YSOs • 24 microns: 1” = 0.25 pc • Can isolate individual stars/binaries • May be able to identify dense compact young clusters • Imaging should detect protostars below 1 Mo • What are the effects of metallicity on the formation of individual stars?

  14. Physical conditions in the ionized gas Indebetouw et al. 2009, ApJ R/G/B = 8 um, B band, X-ray

  15. Spectrum of entire 30 Doradus nebula Indebetouw et al. 2009, ApJ ~4’x4’ region Note rising MIR continuum

  16. Mid-IR spectroscopy inside an HII region • Brightest source • low excitation region • CO emission peak • Prominent MIR source outside main bubble • R136 cluster • Diffuse region, harder radiation field • Known WN6 star R145 Indebetouw et al. 2009

  17. Star cluster formation in M51 Calzetti et al. 2007, Spitzer SINGS image Mentuch et al., in prep., Herschel VNGS image

  18. Individual regions in M51 24 um 70 um Spitzer SINGS image, Calzetti et al. 2007 Herschel VNGS image, Mentuch et al., in prep.

  19. Individual regions in M51 24 um 70 um Spitzer SINGS image, Calzetti et al. 2007 Herschel VNGS image, Mentuch et al., in prep.

  20. Antennae: the closest major merger CO overlaid on HST optical image • Wilson et al. 2000, ApJ • Whitmore et al. 1999, AJ

  21. The Antennae in cool dust emission • Two infrared bright regions in overlap region with different 6cm/FIR indicating different ISM properties • Herschel PACS data: Klaas et al. 2010, A&A

  22. The Antennae in cool dust emission • Two infrared bright regions in overlap region with different 6cm/FIR indicating different ISM properties • Herschel PACS data: Klaas et al. 2010, A&A

  23. Complex mid-IR spectra in the Antennae NeIII NeII rising continuum PAH ISO 15 um image • Wilson et al. 2000, ApJ ISO CVF spectra

  24. Complex mid-IR spectra in the Antennae • Wilson et al. 2000, ApJ NeII NeIII PAH

  25. Complex mid-IR spectra in the Antennae • Wilson et al. 2000, ApJ PAH NeII

  26. Mid-IR Spectroscopy with JWST • Is the hot continuum source in the Antennae co-located with the strong NeIII emission? • 12 microns: 0.5” = 50 pc • Can resolve an individual molecular cloud (100 pc), but not a cluster-forming core (1 pc) • Extended sources may need small spectroscopic mosaics • Can we locate other targets with rising continuum in Antennae? M51? Etc?

  27. Comparing the Antennae peak with the R136 star cluster in the LMC Indebetouw et al 2009, ApJ Brandl et al. 2009, ApJ 10 um 30 um 10 um 30 um

  28. Summary • MIRI on JWST has great promise for studying individual star and star cluster formation, both in our own Galaxy and in other galaxies • Great synergies between JWST and ALMA for high resolution imaging and spectroscopy!

  29. End

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