Hunt for Molecules in Local Universe Galaxies

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Hunt for Molecules in Local Universe Galaxies

Hunt for Molecules, November 19-20, 2005, Paris,
France
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• ISM properties in SBs and AGN
• Spectacular energies injected in gas reservoirs
  of SB and AGN through radiation fields(UV,
  X-rays) shocks and cosmic rays modify
• -Physical properties of molecular gas
• -Chemistry of molecular gas

Science driver of an ongoing IRAM survey of SBs
and AGN to go beyond CO maps
team(Garcia-Burillo, Usero, Fuente, Gracia,
Planesas, Boone, Tacconi, Schinnerer,
Aalto) High sensitivityresolution required 30m
(see also pioneering work of Mauersberger,
Henkel, Huttemeister et al) and PdBure
interferometer (the main focus here!).
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Evolutionary trends in SB can be tracked down by
observation of different chemical tracers
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Large-Scale Shocks in Galaxies

Need of higher resolution---gtInterferometer maps
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Large-Scale Shocks in Galaxies
NGC253
García-Burillo et al. 2000

• First high-resolution SiO image of a galaxy,
  made with PdB interferometer.
• NGC253 barred spiral with nuclear SBregion I.
• Widespread SiO emission (v0,J2-1) over
  600pc-disk (regions I II X(SiO)?10-10 -10-9
  )---gtbeyond the nuclear starburst (region I).

I
II

• Region II coincides with bar resonance
  (ILR)-----gtlarge-scale shocks induced by density
  waves in the disk

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Large-Scale Shocks in Galaxies
IC342
Usero, García-Burillo et al. 2005, AA, submitted

• Molecular gas distribution shaped by the bar
  SiO emission along northern spiral arm nuclear
  ring.
• SiO extends beyond the radiocontinuum thermal
  emission -gt shocks are not powered by on-going
  star formation!

• ?X(SiO)? (2-7)?10-10 (nuclear ring) to
  (1-4)?10-9 (northern spiral arm).

Left SiO integrated intensity (contours) on
3.5mm RC (color) PdBI maps. Right H13CO
(contours) on SiO (color) PdBI maps.
SiO-to- H13CO integrated intensity ratio.
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IC342
Large-Scale Shocks in Galaxies
Usero, García-Burillo et al. 2005, AA, submitted

• Turbulence of shocked gas is enhanced compared to
  the quiescent gas.

--gtlarge-scale shocks in IC342 are driven by
density waves X(SiO) largest at x1/x2 orbit
crossing--gtcloud cloud collisions enhanced.

• A fraction of kinetic energy cascades down to
  smaller scales.
• Shocks arise in a turbulent clumpy medium.

Left H13CO (contours) on SiO (color) PdBI maps.
Right SiO and H13CO position-velocity
diagrams.
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Large-Scale Shocks in Galaxies
M82
García-Burillo et al. 2001
chimney

• PdBI maps show SiO emission extends out of
  galaxy plane!
• Two features with X(SiO) ?(2-4)x 10-10
• -a/ SiO chimney.
• -b/ SiO supershell.

• SiO chimney
• Filament of 500pc size
• X(SiO)?(2-4)x10-10
• M(H2)?6x106 M?

supershell

• SiO supershell
• Created by supercluster of young stars.
• M(H2)?1.6x107 M?

SiO map (contours) on 4.8GHz continuum image
(grey) from Wills et al 1999
-gtlarge-scale shocks in the disk-halo interface
building up the gaseous halo
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PDR Chemistry in Galaxies
M82
García-Burillo et al. 2002
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PDR Chemistry in Galaxies
M82
Fuente, García-Burillo, Gerin et al. 2005a, 2005b

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XDR Chemistry in Galaxies
NGC1068
Usero, García-Burillo, Fuente et al. 2004
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XDR Chemistry in Galaxies
NGC1068
Usero, García-Burillo, Fuente et al. 2004

• X(HCO)/X(HOC)300-6000--gtX(e-)10-7-10-6
  (typically measured in molecular clouds).
• X(HCO)/X(HOC) measured in the CND of NGC1068
  (30-80) can be reached in XDR if
  ?X(e-)?10-5--gtmolecular gas is highly ionized

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Molecular Gas Chemistry in ULIRGs
ULIRGs
Gracia, García-Burillo, Planesas et al. 2005, in
prep

• Ultraluminous Infrared Galaxies (ULIRGs, i.e.,
  LIR (gt1012Lo ) extreme starbursts and/or
  embedded AGNs? Puzzle LCO not correlated with
  LIR (Solomon et al. 1997).
• Gao Solomon (2004ab) show fraction of dense gas
  (LHCN/LCO) is correlated with LIR--gt starburst
  origin for ULIRGs!?.

• Our HCO survey of LIGs and ULIGs (Gracia et al.
  2005) show that HCO/CO is fairly constant as a
  function of LIR!! --gtat odds with the picture
  drawn from HCN .

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Molecular Gas Chemistry in ULIRGs
ULIRGs
Gracia, García-Burillo, Planesas et al. 2005, in
prep

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High spatial resolution is key to probe
chemical differentation in galaxies!
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Summary

• Highly sensitive mm-interferometers can study
  molecular inventory in active galaxies beyond
  CO.
• Information provided by tracers of PDR, XDR and
  Shock Chemistry key to understand evolution of
  ISM content in SB and AGN.

?First SiO interferometer maps in SB/AGN
show emission on scales of 200-700pc (NGC253,
M82, IC342, NGC1068). ?Variable enhancement of
SiO (X(SiO)10-8-10-10 ) reveal uneven shock
processing evolution along SB sequence.
SHOCK Chemistry at work...
?HCO interferometer map in M82 shows propagation
of PDR Chemistry in 600 pc disk. ?HCO detected
in NGC1068 starburst ring.
PDR Chemistry at work...
?30mPdBure maps (HCN, SiO, CN,
HCO,HOC..) reveal XDR Chemistry in the 200pc
CND of NGC1068.
XDR Chemistry at work...
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Summary

• Highly sensitive mm-interferometers can study
  molecular inventory in active galaxies beyond
  CO.
• Information provided by tracers of PDR, XDR and
  Shock Chemistry key to understand evolution of
  ISM content in SB and AGN.

?First SiO interferometer maps in SB/AGN
show emission on scales of 200-700pc (NGC253,
M82, IC342, NGC1068). ?Variable enhancement of
SiO (X(SiO)10-8-10-10 ) reveal uneven shock
processing evolution along SB sequence.
SHOCK Chemistry at work...
?HCO interferometer map in M82 shows propagation
of PDR Chemistry in 600 pc disk. ?HCO detected
in NGC1068 starburst ring.
PDR Chemistry at work...
?30mPdBure maps (HCN, SiO, CN,
HCO,HOC..) reveal XDR Chemistry in the 200pc
CND of NGC1068.
XDR Chemistry at work...
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PDR Chemistry in Galaxies
M82
Fuente, García-Burillo, Gerin et al. 2005a, 2005b

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• ISM properties in SBs and AGN vs quiescent star
  forming galaxy disks
• Models from mm/IR point out to significant
  differences. Spectacular energies injected in
  gas reservoirs of SB and AGN (radiation fields,
  winds, shocks...).
• Physical properties of molecular gas in SB/AGN
• Need of multilines/multispecies studies.
• Chemistry of molecular gas in SB/AGN
• Influence of radiation fields(UV, X-rays) vs
  shock processing on the chemical status of
  molecular gas.

Science driver of IRAM survey of SB and AGN
beyond CO maps High sensitivityresolution
required 30m and PdBure interferometer
?Interferometer maps using tracers of star
formation (CS,HCN, CN, HCO,SiO...)
?Interferometer maps using chemical tracers of
Photon-Dominated-Regions (PDR) ,
X-ray-Dominated-Regions (XDR), and Shock Chemistry
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Molecular gas drawn out of galaxy disks
starbursts
SiO chimney
The tip of the iceberg!
SiO supershell
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Shock Chemistry in NGC253

• Strong non-circular motions modelled as gas
  response to bar
• Parallelogram signature ring II outer Inner
  Lindblad Resonance (oILR) where orbit crowding
  and large-scale shocks are expected.

• The average value of X(SiO) is high gt10-10 ,
  i.e. an order of magnitude above PDR standards.
• X(SiO) increases in outer region II, reaching
  ?10-9.
• Large-scale shocks driven by DW resonances
  efficiently enhance SiO abundances.

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Shock Chemistry IC342 and NGC253
NGC253 Usero et al. 2005, in prep.
IC342 Usero et al. 2005, AA, submitted
3.5mm radiocontinuum PdBI map (contours) on H?
continuum HST image (color).
SO(32-21) PdBI map of NGC253.
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