alma does galaxies!
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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 - PowerPoint PPT PresentationTRANSCRIPT
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ALMA DOES GALAXIES!A User’s Perspective on Early Science
Jean TurnerUCLA
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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
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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
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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
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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)
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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)
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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
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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)
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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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