ALMA DOES GALAXIES!A User’s Perspective on Early Science

Jean TurnerUCLA

gas & star formation in 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...

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the negative K correction & dust emission

fluxes are nearly distance-independent in the submm

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the negative K correction & dust emission

fluxes are nearly distance-independent in the submm

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Z < 2Ken Lanzetta CSNY SBZ > 2

Hubble Deep Field

simulatedALMA Deep Field

CO in galaxies across the universe

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LJ Tacconi et al. Nature 463, 781-784 (2010) doi:10.1038/nature08773

CO maps in EGS 1305123, z = 1.12

channel maps:

9 km/s

109 Msun

clumps of gas,

1-2 kpc across

total Mdyn =

2 x 1011 Msun

CO in galaxies across the universe

SDSS J114816.64+525150.3 QSOtotal extent: 2.5 kpcMdyn 5-6 x 1010 Msun Mgas ~ 1 x 1010 Msun

from CII, SFR ~3000 Msun/yr

Walter et al. 2004, CO(3-2) VLA

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z= 6.42; t = 870 Myr

AGN up close

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NGC 1068 Seyfert 2 CO(1-0) CO(2-1)

Plateau de Bure Interferometer Schinnerer et al. (2000)

extragalactic chemistry

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IC 342 central 300 pc

N2H+ HNC HC3N C2H C34S HNCO CH3OH

Owens Valley Interferometer (now CARMA) Meier & Turner (2005)

ALMA Early Science: sensitivityoh say can you see...

object sourceALMA 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= 9

ALMA Early Science: imaging issuesSurprisingly M51 & other large nearby galaxies are not a

prime Early Science Targets. Why??

Herschel PACS 70+160 microns combined (ESA & PAC team, + JT Photoshop)

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ALMA Early Science: mosaicking limited

M51

with ALMA primary beam

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ALMA Early Science: no OTF mapping

M51: better done with ACA, available in FULL ALMA

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ALMA Early Science: extended structures difficultsimulated largest fringes of Early ALMA on M51

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M51in CO or dust continuum (or any galaxy bigger than ~1’) is a tricky imaging problem requiringfull ALMA (OTF &ACA)

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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