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Hunt for Molecules in Local Universe Galaxies

Santiago GARCIA-BURILLO Observatorio Astronómico Nacional (OAN)-Spain. Hunt for Molecules in Local Universe Galaxies. Hunt for Molecules, November 19-20, 2005, Paris, France. Molecular Gas Chemistry in Starbursts (SBs) and Active Galactic Nuclei (AGNs). ISM properties in SBs and AGN

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Hunt for Molecules in Local Universe Galaxies

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  1. Santiago GARCIA-BURILLO Observatorio Astronómico Nacional (OAN)-Spain Hunt for Molecules in Local Universe Galaxies Hunt for Molecules, November 19-20, 2005, Paris, France

  2. Molecular Gas Chemistry in Starbursts (SBs) and Active Galactic Nuclei (AGNs) • ISM properties in SBs and AGN • Spectacular energies injectedin 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 sensitivity+resolution required: 30m (see also pioneering work of Mauersberger, Henkel, Huttemeister et al) and PdBure interferometer (the main focus here!).

  3. Tracking down Galaxy Evolution through Chemistry Energetic Processes in SB & AGN (intense UV/X Radiation, Shocks,Cosmic Rays...) PHASES PROCESSES I/ ONSET OF THE NUCLEAR STARBURST: gas infall driven by density waves and/or tidal forces. • Gas compression, HI H2, cloud-cloud collisions driving large-scaleSHOCKS. • UV field from massive stars create HII regions and PDR locally in disk. • SHOCKS in YSO in disk • XDR when AGN in disk. II/ MASSIVE STAR FORMATION BURSTS: Young Stellar Objects and first SN explosions • Strong UV fields create giant PDR in disk • Expansion of gas heated by SN entrains neutral gas into halo driving SHOCKS • PDR /SHOCKS in halo? III/ BIPOLAR GIANT OUTFLOW: gas plane breaks out due to blast waves of SN remnants. Evolutionary trends in SB can be tracked down by observation of different chemical tracers

  4. Large-Scale Shocks in Galaxies Need of higher resolution--->Interferometer maps

  5. NGC253 3mm-cont SiO H13CO+ Large-Scale Shocks in Galaxies García-Burillo et al. 2000 • First high-resolution SiO image of a galaxy, made with PdB interferometer. • NGC253: barred spiral with nuclear SB=region I. • Widespread SiO emission (v=0,J=2-1) over 600pc-disk (regions I + II :X(SiO)10-10 -10-9 )--->beyond the nuclear starburst (region I). I II • Region II: coincides with bar resonance (ILR):----->large-scale shocks induced by density waves in the disk

  6. IC342 Large-Scale Shocks in Galaxies Usero, García-Burillo et al. 2005, A&A, submitted • Molecular gas distribution shaped by the bar: SiO emission along northern spiral arm + nuclear ring. • SiO extends beyond the radiocontinuum thermal emission -> 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.

  7. IC342 Large-Scale Shocks in Galaxies SiO kinematics Usero, García-Burillo et al. 2005, A&A, submitted • Turbulence of shocked gas is enhanced compared to the quiescent gas. -->large-scale shocks in IC342 are driven by density waves: X(SiO) largest at x1/x2 orbit crossing-->cloud 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.

  8. M82 Large-Scale Shocks in Galaxies SiO 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 ->large-scale shocks in the disk-halo interface: building up the gaseous halo

  9. M82 PDR Chemistry in Galaxies -->M82 disk is a giant PDR of 600 pc size(Mao et al 2000, García-Burillo et al 2002; Fuente et al 2005) NeII contours(Achtermann & Lacy 1995) on HCO map (grey) HCO contours(García-Burillo et al 2002) on CO map (grey; Weiss et al 2001) --->Widespread HCO emission detected in PdBI map of the nucleus of M82 (García-Burillo et al 2002) --->Global HCO abundances comparable to PDR: X(HCO)~4x10-10(Hollis & Churchwell, 1983; Snyder et al 1985; Schilke et al 2001) --->Interferometer map shows strong variations of X(HCO) within disk: --->PDR Chemistry propagates. García-Burillo et al. 2002

  10. M82 PDR Chemistry in Galaxies ->High [CN]/[HCN] ratio ~ 5 Results of multispecies 30m survey of M82 ->Complex carbon chemistry: C3H2, CH3C2H, C2H ->Low [HCO+]/[HOC+] ratio ~ 40 Le Bourlot et al´s model M82----> small (r<0.2pc) and dense (nH2~ 10 4-5) molecular clouds immersed in intense UV-field (G0=104) …and detection of CO+! Fuente, García-Burillo, Gerin et al. 2005a, 2005b

  11. NGC1068 XDR Chemistry in Galaxies -->X-rays suspected to heavily influence molecular gas chemistry in the nuclear disks of AGN(Tacconi et al 1994, Maloney et al 1996) Multispecies 30m survey of NGC1068 CO(1-0) (PdBI;Schinnerer et al. 00) -->X-ray driven chemistry models explain abundance ratios measured in the CND of NGC1068 (Usero et al 2004) Molecular Gas Inventory of the CND of NGC1068 Usero, García-Burillo, Fuente et al. 2004

  12. NGC1068 XDR Chemistry in Galaxies ->The HCO+ / HOC+ equilibrium The 400pc-size CND of NGC1068 has become a giant XDR--->embedded AGNs can alter significantly the chemistry of molecular gas-->relevant for high-z galaxies Usero, García-Burillo, Fuente et al. 2004 • X(HCO+)/X(HOC+)~300-6000-->X(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-->molecular gas is highly ionized

  13. ULIRGs Molecular Gas Chemistry in ULIRGs Probing dense gas in ULIRGs The HCN view The HCO+ view Which one is ‘‘wrong’’? L HCO+(1-0) / L CO(1-0) L HCN(1-0) / L CO(1-0) Gracia, García-Burillo, Planesas et al. 2005, in prep • Ultraluminous Infrared Galaxies (ULIRGs, i.e., LIR (>1012Lo ): extreme starburstsand/orembedded 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--> 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!! -->at odds with the picture drawn from HCN .

  14. ULIRGs Molecular Gas Chemistry in ULIRGs Is HCN an unbiased tracer of dense gas in ULIRGs? ‘Chemistry’ is key to understand what lurks inside ULIRGs! Infrared pumping of HCN lines-->higher I(HCN) XDR-driven chemistry in embedded AGNs-->enhancement of X(HCN) hot-core driven chemistry in starbursts-->higher X(HCN) Potential bias of HCN L HCN(1-0) / L HCO+(1-0) Unexpected correlation with LIR! Gracia, García-Burillo, Planesas et al. 2005, in prep

  15. Conclusions and Perspectives • Evolution in extreme+embedded starbursts will be probed by molecular lines with ALMA-->need of local (low z) templates!!. • Large-scale molecular shocks in the: • pre-starburst phase (e.g., NGC253, IC342, Maffei2) • post-starburst phase (e.g., M82) • High-z Universe is the playground for extreme+embedded starbursts and AGNs. • Giant PDRs in starburst disks (e.g., M82) • XDRsin AGNs (e.g., NGC1068) Extragalactic Chemistry in low-z Universe: tracking down the evolution in local starbursts/AGNs Extragalactic Chemistry in high-z Universe?:

  16. Extragalactic Chemistry: Using Interferometers High spatial resolution needed to trace evolution in starbursts • SiO traces shocks in the disk of NGC253 (SF, density waves...): less evolved starburst. • SiO traces shocks in the disk-halo interface inM82:giant outflow, evolved starburst. SiO IRAM-PdBI map (contours) from García-Burillo et al. 2001 on CO (2-1) map from Weiss et al 2001 (colour ) in M82. SiO IRAM PdBI map in NGC253 from García-Burillo et al 2000. NGC253 M82 10´´

  17. Extragalactic Chemistry: Using Interferometers OVRO maps of IC342 (Meier and Turner 2005) High spatial resolution is key to probe chemical differentation in galaxies!

  18. Conclusions and Perspectives • Evolution in extreme+embedded starbursts will be probed by molecular lines with ALMA-->but we need to study local (low z) templates first!!. • Large-scale molecular shocks in the: • pre-starburst phase (e.g., NGC253, IC342, Maffei2) • post-starburst phase (e.g., M82) • High-z Universe is the playground for extreme+embedded starbursts and AGNs. • Giant PDRs in starburst disks (e.g., M82) • XDRsin AGNs (e.g., NGC1068) Extragalactic Chemistry in low-z Universe: tracking down the evolution in local starbursts/AGNs Extragalactic Chemistry in high-z Universe?:

  19. Summary • Highly sensitive mm-interferometerscan 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... 30m+PdBure maps (HCN, SiO, CN, HCO+,HOC+..) reveal XDR Chemistry in the 200pc CND of NGC1068. XDR Chemistry at work...

  20. Summary • Highly sensitive mm-interferometerscan 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... 30m+PdBure maps (HCN, SiO, CN, HCO+,HOC+..) reveal XDR Chemistry in the 200pc CND of NGC1068. XDR Chemistry at work...

  21. M82 PDR Chemistry in Galaxies ->High [CN]/[HCN] ratio ~ 5 Results of multispecies 30m survey of M82 ->Complex carbon chemistry: C3H2, CH3C2H, C2H ->Low [HCO+]/[HOC+] ratio ~ 40 M82----> small (r<0.2pc) and dense (nH2~ 10 4-5) molecular clouds immersed in intense UV-field (G0=104) Detection of CO+! Fuente, García-Burillo, Gerin et al. 2005a, 2005b

  22. Molecular Gas Chemistry in SB and AGN • ISM properties in SBs and AGN vs quiescent star forming galaxy disks • Models from mm/IR point out to significant differences. Spectacular energies injectedin 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 sensitivity+resolution 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

  23. Dynamics of Disks (IV): The Disk-Halo Interface M82: a huge molecular gas halo! (Seaquist and Clark 2001, García-Burillo et al 2001, Walter et al 2002) PdBI SiO(2-1) map: García-Burillo et al 2001 • IRAM PdBI one-field map shows SiO emission extends out of galaxy plane!:chimney+supershell. OVRO CO(1-0) map :Walter et al 2002 • ALMA will make possible high-resolution mapping of extreme starbursts as M82: key to understand high-z galaxies ! Molecular gas drawn out of galaxy disks: starbursts SiOchimney The tip of the iceberg! SiOsupershell

  24. 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: >10-10, 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.

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

  26. Extragalactic Chemistry:Expanding the Frequency Range ->Pioneering work of R. Mauersberger+C. Henkel (80-90’s) done with 30m telescope (12’’-27’’ resolution) in some galaxies for a limited number of molecular species. LINE SURVEYS 2mm Survey (~40GHz broad) of the NGC253 with IRAM 30m (Martín et al. 2003, 2004) NGC253 M82 and NGC253 spectra (~4GHz broad) by S. Martín (private communication) • Different molecules provide • diagnostic tools to explore starburst evolution: M82 and NGC253 show different chemistries M82 NGC253

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