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ALMA Band 11: t he extragalactic science case

ALMA Band 11: t he extragalactic science case. Roberto Maiolino. Why is Band 11 is important for extragalactic studies?. Band 11: Far-IR Fine structure lines: the strongest lines in galaxy spectra. Band 11: close to the peak of galaxies SED. C +. N +. N +. O 0. 12-11. 10-9. PAH.

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ALMA Band 11: t he extragalactic science case

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  1. ALMA Band 11: the extragalactic science case Roberto Maiolino

  2. Why is Band 11 is important for extragalactic studies?

  3. Band 11: Far-IR Fine structure lines: the strongest lines in galaxy spectra Band 11: close to the peak of galaxies SED C+ N+ N+ O0 12-11 10-9 PAH Molecular lines Warm dust (SFR) Hot dust (AGN) Band 11: high excitation molecular transitions free-free Band 11 @ z=0.5 Band 11 @ z=0

  4. Low metallicity (young) galaxies: enhanced far-IR fine structure line emission [CII]/FIR ~ 0.01 ! [CII]/CO ~ 50000 !!!!! [CII] CO [CII] traces “CO-dark” molecular gas [CII] Herschel-PACS image of NGC 4214 (Z~0.3Z) PDR ([CII]) molecular (CO)

  5. [CII]158mm flux map (Herschel) Herschel PACS M82 3.6 Mpc 15” 260pc optical Contursi+10 [CII]158mm flux map (ALMA band 7 ext. conf.) [CII] velocity field LESS01 z=4.7 SFR = 500 M/yr 0.5” 4 kpc De Breuck+ in prep.

  6. Revealing invisible galaxies with [CII] mapping z=4.4 CO(5-4) IRAM-PdBI [CII] map Lensed quasar LAGN>1046 erg/s quasar host (compact) 10 kpc continuum merging companion Gallerani+12 Gallerani+ in prep The companion is undetected in NICMOS Near-IR images undetected in submm continuum, undetected in CO

  7. [OIII]52mm [NIII]57mm [OI]63mm [OIII]88mm Frequency [GHz] ALMA band [NII]121mm [OI]145mm [CII]158mm [NII]205mm CO redshift

  8. Detectability of [CII] 158mm [CII] in metal-rich galaxy (i.e. conservative) 1 • can detect and map MW-like galaxies • in the nearby Universe Band 11

  9. Detectability of [NII] 205mm 1 • can detect and map MW-like galaxies • in the local Universe Band 11

  10. Constraining the metallicity in heavily obscured galaxies [NII]205mm @ z=4.7 Nagao+12

  11. Quasar+companion at z=4.4 [NII]205mm map: metal-enriched outflows [CII]158mm map: elusive merging companion Gallerani+12 Gallerani+ in prep

  12. Far-IR fine structure lines diagnostic diagrams: physics (UV radiation field, density, etc…) and chemistry of the ISM in galaxies [CII]/FIR Sturm+10 Kauffman+99 Hailey-Dunsheath+10 Nagao+11 CO(1-0)/FIR

  13. High excitation CO transitions: tracing X-ray dominated regions (XDR) Band 11 Powerful tool to identify totally obscured and embeddedAGNs Herschel-SPIRE Van der Werf+10 XDR ~1-0.5” resolution needed to minimize dilution by the host galaxy

  14. Nuclear kinematics and dynamics in AGNs: Black Hole masses MBH (M) JWST 109 108 107 106 105 band 11  ALMA log (Radius Influence) [arcsec] NGC1068 CO(2-1) 2” = 140pc VLTI x log Distance [Mpc] ULIRGs Need to access high CO transition (band 11) to trace nuclear molecular gas (merging Black Holes)

  15. Clumpy versus continuous obscuring “torus” 5 pc Expected mid-IR (~12mm) thermal emission From Meisenheimer 2008

  16. Testing clumpy model for nuclear dust thermal emission Nuclear small dusty clouds should emit both MIR and FIR NGC1068 CO(2-1) 2” = 140pc MIR and FIR morphologies should be on similar scales ionization cone VLTI mid-IR band 11 ALMA bands 3-10 VLTI Raban et al. 2009 Band 11 beam (5 km baseline) In the continuous model far-IR should be much more extended

  17. Quasar feedback Quasar-driven massive outflows cleaning massive galaxies of their gas content Invoked by any model of galaxy formation to quench star formation in massive galaxies

  18. Massive quasar-driven molecular outflows revealed by Herschel through the detection of OH P-Cygni profiles Mrk231 1000 km/s Fischer+10 Sturm+11 lrest (mm) Cosmic Star formation rate density Band 11 will detect and MAP QUENCHING MASSIVE OUTFLOWS in quasars and star forming galaxies throughoutthe QUENCHING EPOCH band 11 Redshift

  19. Summary • A few key extragalactic science cases for Band 11: • Trace the physics, dynamics and chemistry of galaxies at z<1 through the • most luminous lines (and extinction free) in galaxy spectra • Reveal and map “dark gas” and “dark galaxies” (possibly the bulk of • galaxy population) out to z~1 • Map peak of galaxy SED • Test AGN torus models • Identify heavily obscured AGN through highly excited CO transitions • Measure dual Black Holes masses in merging systems • Trace galaxy quenching mechanisms throughout • the galaxy quenching epoch • More science cases…

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