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ALMA DOES GALAXIES!

ALMA DOES GALAXIES!. A User’s Perspective on Early Science. Jean Turner. UCLA. gas & star formation in galaxies across cosmic time. free-free continuum & radio recombination lines: extinction free tracers of star formation gas distribution & mass: CO

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ALMA DOES GALAXIES!

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  1. ALMA DOES GALAXIES! A User’s Perspective on Early Science • Jean Turner • UCLA

  2. gas & star formationin galaxies across cosmic time free-free continuum & radio recombination lines: extinction free tracers of star formation gas distribution & mass: CO kinematics & dynamical masses of galaxies and galaxy systems molecules, chemistry, & gas diagnostics: density, temperature, pressure, radiation fields, abundances (PDRs, XDRs) observed consequences of feedback & regulation of star formation, HCN, CN...

  3. the negative K correction & dust emission fluxes are nearly distance-independent in the submm

  4. the negative K correction & dust emission fluxes are nearly distance-independent in the submm Hubble Deep Field Ken Lanzetta CSNY SB Z < 2 Z > 2 simulated ALMA Deep Field

  5. CO in galaxies across the universe CO maps in EGS 1305123, z = 1.12 109Msun clumps of gas, 1-2 kpc across total Mdyn = 2 x 1011Msun channel maps: 9 km/s LJ Tacconi et al.Nature463, 781-784 (2010) doi:10.1038/nature08773

  6. CO in galaxies across the universe SDSS J114816.64+525150.3 QSO total extent: 2.5 kpc Mdyn 5-6 x 1010MsunMgas ~ 1 x 1010Msun from CII, SFR ~3000 Msun/yr Walter et al. 2004, CO(3-2) VLA z= 6.42; t = 870 Myr

  7. AGN up close NGC 1068 Seyfert 2 CO(1-0) CO(2-1) Plateau de Bure Interferometer Schinnerer et al. (2000)

  8. extragalactic chemistry IC 342 central 300 pc N2H+ HNC HC3N C2H C34S HNCO CH3OH Owens Valley Interferometer (now CARMA) Meier & Turner (2005)

  9. ALMA Early Science: sensitivityoh say can you see... objectsourceALMA ES ALMA W49 free-free continuum 20 Mpc Milky Way submm dust continuum Milky Way CO(4-3) z=3 z=3 Arp 220 CO(4-3) z=7 z= Arp 220 HCN(4-3) z=3 z=

  10. ALMA Early Science: imaging issues Surprisingly M51 & other large nearby galaxies are not a prime Early Science Targets. Why?? Herschel PACS 70+160 microns combined(ESA & PAC team, + JT Photoshop)

  11. ALMA Early Science:mosaicking limited M51 with ALMA primary beam

  12. ALMA Early Science: no OTF mapping M51: better done with ACA, available in FULL ALMA

  13. ALMA Early Science:extended structures difficult simulated largest fringes of Early ALMA on M51 M51in CO or dust continuum (or any galaxy bigger than ~1’) is a tricky imaging problem requiring full ALMA (OTF & ACA)

  14. early science & galaxies early science ALMA will be a significant improvement in sensitivity over existing instruments expect breakthrough science in understanding the structure & star formation history of high z, intermediate z galaxies; what are submillimeter galaxies close up views of gas near AGN extragalactic chemistry & radiative feedback from star formation the best imaging will come with full ALMA, including the capability of mapping large nearby galaxies

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