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Imaging star-forming gas in nearby galaxies with ALMA

Imaging star-forming gas in nearby galaxies with ALMA. Jean Turner (UCLA). ALMA studies of star formation on galactic scales complement Galactic and high z studies. ALMA studies of star formation on galactic scales complement Galactic and high z studies.

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Imaging star-forming gas in nearby galaxies with ALMA

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  1. Imaging star-forming gas in nearby galaxieswithALMA Jean Turner (UCLA)

  2. ALMA studies of star formation on galactic scales complement Galactic and high z studies Imaging Star Formation in the Cosmos with ALMA

  3. ALMA studies of star formation on galactic scales complement Galactic and high z studies Observed: Stellar populations, Hubble sequence, “beads on a string”, & Toomre Q Imaging Star Formation in the Cosmos with ALMA

  4. ALMA studies of star formation on galactic scales complement Galactic and high z studies Observed: Stellar populations, Hubble sequence, “beads on a string”, & Toomre Q • What is the relation of spiral structure to star formation? Imaging Star Formation in the Cosmos with ALMA

  5. ALMA studies of star formation on galactic scales complement Galactic and high z studies Observed: Stellar populations, Hubble sequence, “beads on a string”, & Toomre Q • What is the relation of spiral structure to star formation? Observed: LIR/MH2 well-correlated, Schmidt law, excellent correlation of HCN and LIR (Gao & Solomon 2005): Imaging Star Formation in the Cosmos with ALMA

  6. ALMA studies of star formation on galactic scales complement Galactic and high z studies Observed: Stellar populations, Hubble sequence, “beads on a string”, & Toomre Q • What is the relation of spiral structure to star formation? Observed: LIR/MH2 well-correlated, Schmidt law, excellent correlation of HCN and LIR (Gao & Solomon 2005) • How do properties of the gas — atomic vs molecular, dense vs diffuse gas — determine star formation? Imaging Star Formation in the Cosmos with ALMA

  7. ALMA resolution: 10 mas<1 pc at Virgoresolve individual SF regions, structure around AGN in the local universe50 pc out to 900+ MpcGMCs, spiral features, galactic structure for a large sample of neaby galaxies Imaging Star Formation in the Cosmos with ALMA

  8. Direct imaging of extragalactic star-forming regions: ALMA continuum Continuum sensitivities ~10 Jy in an hour Massive HII regions via their free-free emission Super star clusters: imaging to 50 Mpc Orions: image to ~10Mpc, detect to Virgo Dust emission from low and high mass stars More sensitive than free-free Local Group, 10 mas = .04 pc = 10,000 AU Imaging Star Formation in the Cosmos with ALMA

  9. Direct imaging of molecular gas: ALMA line emission Imaging of molecular clouds in CO and other molecules Line brightnesses ~ 0.01K in 10 hours Imaging Star Formation in the Cosmos with ALMA

  10. Care and feeding of AGN NGC 1068 Seyfert 2 CO(1-0) CO(2-1) Plateau de Bure Interf. Schinnerer et al. 2000 Imaging Star Formation in the Cosmos with ALMA

  11. Nurturing of star formation in galaxies N. Sharp, NOAO Imaging Star Formation in the Cosmos with ALMA

  12. Nurturing of star formation in galaxies CO BIMA-SONG N. Sharp, NOAO Helfer et al. 2003 Imaging Star Formation in the Cosmos with ALMA

  13. Nurturing of star formation in galaxies CO BIMA-SONG F. Calvert, A. Block, NOAO/AURA/NSF Helfer et al. 2003 Imaging Star Formation in the Cosmos with ALMA

  14. ALMA is designed to detect extended structure M83 Imaging Star Formation in the Cosmos with ALMA

  15. ALMA is designed to detect extended structure CO (green): NRAO 12 meter telescope HI (red): VLA (NRAO/AUI/NSF) M83 AAT D. Malin Crosthwaite et al. 2003 Imaging Star Formation in the Cosmos with ALMA

  16. ALMA can study gas and interactions VLA NRAO/AUI/NSF Yun, Ho, Lo 1994 Imaging Star Formation in the Cosmos with ALMA

  17. The world of molecules Imaging Star Formation in the Cosmos with ALMA

  18. Detecting molecular gas Imaging Star Formation in the Cosmos with ALMA

  19. Detecting molecular gas H2 is “silent” unless it is hot (100 K) Imaging Star Formation in the Cosmos with ALMA

  20. Detecting molecular gas H2 is “silent” unless it is hot (100 K) CO is a pretty good tracer, easily excited (5.5 K, low densities), abundant, bright. Imaging Star Formation in the Cosmos with ALMA

  21. Detecting molecular gas H2 is “silent” unless it is hot (100 K) CO is a pretty good tracer, easily excited (5.5 K, low densities), abundant, bright. How good is “pretty good”? To factor of two within Galaxy (gamma rays); Overpredicts gas mass in metal-rich galactic centers. Situation in low metallicity galaxies unclear Freeze-out in densest clouds Imaging Star Formation in the Cosmos with ALMA

  22. Detected interstellar molecules H2 HD H3+ H2D+ CH CH+ C2 CH2 C2H *C3 CH3 C2H2 C3H(lin) c-C3H *CH4 C4 c-C3H2 H2CCC(lin) C4H *C5 *C2H4 C5H H2C4(lin) *HC4H CH3C2H C6H *HC6H H2C6 *C7H CH3C4H C8H *C6H6 OH CO CO+ H2O HCO HCO+ HOC+ C2O CO2 H3O+ HOCO+ H2CO C3O CH2CO HCOOH H2COH+ CH3OH CH2CHO CH2CHOH CH2CHCHO HC2CHO C5O CH3CHO c-C2H4O CH3OCHO CH2OHCHO CH3COOH CH3OCH3 CH3CH2OH CH3CH2CHO (CH3)2CO HOCH2CH2OH C2H5OCH3 (CH2OH)2CO NH CN N2 NH2 HCN HNC N2H+ NH3 HCNH+ H2CN HCCN C3N CH2CN CH2NH HC2CN HC2NC NH2CN C3NH CH3CN CH3NC HC3NH+ *HC4N C5N CH3NH2 CH2CHCN HC5N CH3C3N CH3CH2CN HC7N CH3C5N? HC9N HC11N NO HNO N2O HNCO NH2CHO SH CS SO SO+ NS SiH *SiC SiN SiO SiS HCl *NaCl *AlCl *KCl HF *AlF *CP PN H2S C2S SO2 OCS HCS+ c-SiC2 *SiCN *SiNC *NaCN *MgCN *MgNC *AlNC H2CS HNCS C3S c-SiC3 *SiH4 *SiC4 CH3SH C5S FeO DEMIRM Imaging Star Formation in the Cosmos with ALMA

  23. Chemistry in Galaxies Pioneering single dish work on the IRAM 30m Henkel, Mauersberger et al., resolutions ~ 30” (300-500 pc in even the closest galaxies) Galaxies can have distinctive chemistries Imaging Star Formation in the Cosmos with ALMA

  24. Imaging Chemistry in Galaxies IC 342 — Owens Valley Millimeter Array N2H+ HNC HC3N C2H C34S HNCO CH3OH Meier & Turner 2005 Imaging Star Formation in the Cosmos with ALMA

  25. Imaging Chemistry in Galaxies IC 342 — Owens Valley Millimeter Array Meier & Turner 2005 PC Axis 1: Density-weighted mean column density Gas density: CO, N2H+, HCN Imaging Star Formation in the Cosmos with ALMA

  26. Imaging Chemistry in Galaxies IC 342 — Owens Valley Millimeter Array Meier & Turner 2005 PC Axis 1: Density-weighted mean column density PC Axis 2: Shock tracers vs PDR molecules C2H: PDR Methanol, HCNO: shocks Gas density: CO, N2H+, HCN Imaging Star Formation in the Cosmos with ALMA

  27. Imaging Chemistry in Galaxies IC 342 — Owens Valley Millimeter Array M82 — BIMA Array Not detected in M82 maps: shock tracers SiO, HNCO, CH3OH Meier & Turner 2005, 2006 – X X Imaging Star Formation in the Cosmos with ALMA

  28. ALMA: Imaging star-forming gas in nearby galaxiessummaryALMA will be a powerful imaging device HII regions (free-free)dust emission (low and high mass SF)molecular clouds on sizescales of 1pc (SF regions, AGN)to galaxy-wide, out to hundreds of MpcIT WILL BE GREAT! Imaging Star Formation in the Cosmos with ALMA

  29. LMC ALMA Imaging Star Formation in the Cosmos with ALMA

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