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Jesús Martín-Pintado CENTRO DE ASTROBIOLOGIA (CSIC-INTA) (Spain) ‏ Sergio Martin (ESO-Chile) ‏

MOLECULAR COMPLEXITY IN NEARBY GALAXIES. Jesús Martín-Pintado CENTRO DE ASTROBIOLOGIA (CSIC-INTA) (Spain) ‏ Sergio Martin (ESO-Chile) ‏ Miguel Angel Requena (MPifR) ‏ Arancha Amo Balandron (CAB) ‏ Jairo Armijos (CAB) ‏ Rebeca Aladro (IRAM-G) ‏ Denise Riquelme (IRAM-G) ‏. Outline.

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Jesús Martín-Pintado CENTRO DE ASTROBIOLOGIA (CSIC-INTA) (Spain) ‏ Sergio Martin (ESO-Chile) ‏

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  1. Cumberland Lodge, 5-7 July 2010 MOLECULAR COMPLEXITY IN NEARBY GALAXIES Jesús Martín-Pintado CENTRO DE ASTROBIOLOGIA (CSIC-INTA) (Spain)‏ Sergio Martin (ESO-Chile)‏ Miguel Angel Requena (MPifR)‏ Arancha Amo Balandron (CAB)‏ Jairo Armijos (CAB)‏ Rebeca Aladro (IRAM-G)‏ Denise Riquelme (IRAM-G)‏

  2. Cumberland Lodge, 5-7 July 2010 Outline Introduction • Molecular emission: a powerful tool to study obscured regions • Why molecular studies in galactic nuclei? Chemical complexity and the heating in the Galactic center • Shocks: complex organic molecules & grain chemistry • PDRs: HNCO/CS changes by nearly 2 orders of magnitude • Chemical complexity & density structure of clouds in SB galaxies • Shock heating versus PDRs heating. Starburst evolution • Structure of molecular clouds (chemical and physical)‏ • Feedback: Superwinds in M82 & accretion • AGN activity in NGC1068 • Cosmic Rays Chemistry Chemical complexity in the ULIRG Arp 220 • Very recent starburst versus AGN: Proto starclusters ALMA and Herschel and e-VLA: Astrochemistry at high z 2

  3. Cumberland Lodge, 5-7 July 2010 Extragalactic nuclei are heavily obscured regions ULIRGS (Arp 220 Av >10000) , Sub-mm Galaxies , .. Star formation, nuclear activity, .. 3

  4. Extragalactic Molecular Emission Cumberland Lodge, 5-7 July 2010 Molecular emission trace: • The total mass content of galaxies (CO emission)‏ • The high density component in galaxies (HCN) Gao et al. (2004)‏ Molecular emission diagnostic tool of : • Properties of the ISM: density, temperature, kinematics.. • The deeply obscured nuclear power sources: AGN or starburst – Shocks, XDR, PDR, shock or CRs chemistry • The feeding of the nucleus • The conditions and processes leading to the starbursts • Starburst evolution 4

  5. Cumberland Lodge, 5-7 July 2010 The Galactic Center Radio + IR (MSX)‏ Sgr A Sgr C Sgr B2 • The closest center of a galaxy we can study in detail • In NGC253: 0.040” (ALMA) corresponds to 17” in the GC • The GC contains all ingredients to test molecular tracers (benchmarking): • Star formation seen throughout the region • Hot cores like Sgr B2N, Sgr B2M .. (proto super starclusters)‏ • Large PDRs illuminated by clusters of massive stars • Strong emission of X-rays (Fe 6.4 keV), gamma-rays (XDRs), CRs 5

  6. Cumberland Lodge, 5-7 July 2010 Complex organic molecules H Abundance Atom addition Requena-Torres et al .(2005;2008) Typical Clouds GBT, 30-m Constant abundance < factor 3 Larger abundance than in Hot Cores Similar ice mantles 6

  7. Cumberland Lodge, 5-7 July 2010 Complex organic molecules Requena-Torres et al .(2008) Dust properties: Core: Silicate (SiO- ) and graphite (C)‏ Ices: H2O, CO, CO2, CH4, CH3OH, H2CO, OCS, NH3, C2H6, HCOOH,.. Similar ice mantles • Grain chemistry • Hydrogenation • Cosmic Rays FREQUENT SHOCKS Origin?: Turbulence, .. Ice Mantle 0.05 microns Core Molecules and Radicals Consisting of C, N, O and H 7

  8. Cumberland Lodge, 5-7 July 2010 Complex organic molecules Grain chemistry radical reactions: Bennett & Kaiser (2007)‏ CH3OH + CR CH3O + H CH2OH + H 5 10-8 7 10-9 <10 -9 CH3O CH2OH HCOOCH310 CH2OHCHO 1 CH3COOH << CO + H HCO+ Methanol ~water on grain mantles 8

  9. Cumberland Lodge, 5-7 July 2010 Chemical complexity: Templates S. Martin et al. (2004), (2005)‏ IRAM 30m 13 surveys 2 mm window 3 mm window Martin et al, 2007 Aladro et al. 2009 GC typical GC PDR Nanjing, 26 October 2009 9

  10. Cumberland Lodge, 5-7 July 2010 Diagnostic diagram for PDRs Martin et al. (2008)‏ PDRs: Large abundance changes HNCO & CH3OH ↓↓ Not included in models CS ↑↑ Hot cores 10

  11. Cumberland Lodge, 5-7 July 2010 Picture for typical clouds in the CMZ Large complexity: CH3OH, C2H5OH, (CH3)2O, HCOOCH3, HCOOH, CH3COOH CH3OH HNCO C2H5OH CS , CH3OH HNCO C2H5O CS , CH3OH HNCO C2H5OH CS CH3OH HNCO C2H5OH CS CH3OH HNCO C2H5O CS , CH3OH HNCO C2H5O CS , CH3OH HNCO C2H5OH CS 11

  12. Cumberland Lodge, 5-7 July 2010 Picture for typical clouds in the CMZ Large complexity: CH3OH, C2H5OH, (CH3)2O, HCOOCH3, HCOOH, CH3COOH PDRs: destroy HNCO and CH3OH and produce CO+, HOC+, HCO XDRs: produce SiO, (CO+, HOC+, HCO??)‏ CH3OH HNCO C2H5OH CS , CH3OH HNCO C2H5O CS , CH3OH HNCO C2H5OH CS CS HCO HOC+ CO+ CH3OH HNCO C2H5O CS , Effects of the clusters: HNCO/CS gradient CS HCO HOC+ CO+ , CH3OH HNCO C2H5OH CS 12

  13. Chemical complexity in SBs Cumberland Lodge, 5-7 July 2010 º Martin et al. (2006)‏ M82 2mm Aladro et al. (2010)‏ Nanjing, 26 October 2009 13

  14. Cumberland Lodge, 5-7 July 2010 DETECTED EXTRAGALACTIC MOLECULES the Galactic center H3O+ 37 38 NH OH+ NH2 H2O+ 14

  15. Cumberland Lodge, 5-7 July 2010 Chemical complexity Templates HNCO CS CH3CCH HC3N CH3OH Wang et al. (2004) covered most relevant molecules in NGC 495 15

  16. Cumberland Lodge, 5-7 July 2010 Key molecules (Abundances)‏ NGC 253M82 NG4945 N(CS) / N(H2) 4x10-9 5x10-9 6x10-9 N(CH3OH) / N(CS) 2.41.1 1.5 N(HNCO) / N(CS) 0.3<0.05 0.6 N(HC3N) / N(CS) 0.10.2 0.2 N(CH3CCH) / N(CS) 1.4 14 0.6 16

  17. Cumberland Lodge, 5-7 July 2010 Chemical complexity in SBs • The properties of the ISM in NGC253 and NGC4945 are similar to those found in the typical GC molecular cloud indicating SHOCK dominated ISM • The ISM in M82 is completely different with low Tk from Ammonia and low HNCO and very high CH3CCH abundances. The heating and the chemistry of the ISM are dominated by UV radiation from the stellar superclusters. PDR dominated ISM 17

  18. Cumberland Lodge, 5-7 July 2010 HNCO diagnostic diagram Martin et al. (2009)‏ Maffei2 is heated by shocks HCN/HCO+ ~2.6 NGC253 shocks +(UV?)‏ HCN/HCO+ ~1 NGC4945 shocks+ (UV)‏ HCN/HCO+ ? HCO detected by Wang et al (2004)‏ M82 is dominated by UV HCN/HCO+ ~0.5 HCO Garcia-Burillo et al. (2001)‏ HOC+, CO+ Fuente et al. (2005, 6) Effect of starburst evolution 18

  19. Cumberland Lodge, 5-7 July 2010 PDRs in Shocked ISM: NGC253 Martin et al. (2009) detected HCO, HOC+, CO+ in NGC 253 • For NGC253 and M82: • Similar PDR components: Av~ 3-4 mag • HNCO survive Av> 7 mag 19

  20. Cumberland Lodge, 5-7 July 2010 Structure of clouds in Starburst Chemistry M82 NGC253 /NGC4945 Atomic gas Atomic gas CO+, HCO, HOC+, CS CO+, HCO, HOC+, CS HNCO CS NO shielded core 20

  21. Cumberland Lodge, 5-7 July 2010 IC342: PDR+shocks SiO Usero et al 2006 OVRO & PdBI PDRs Shocks C2H(1-0) C34S(2-1) CH3OH(2-1) HNCO(4-3)‏

  22. Cumberland Lodge, 5-7 July 2010 CS(7-6)‏ CS(5-4)‏ CS(2-1)‏ HC3N (18-17)‏ HC3N (26-25)‏ HC3N (16-15)‏ Structure of clouds in Starburst density NGC253 Physical properties of the clouds: Tk, N, n(H2)‏ Relationship chemistry-physical conditions Multiline analisys of CS, HC3N and CH3CCH M82 Ballet et al (2009) & Aladro et al. (2010) 22 22

  23. Cumberland Lodge, 5-7 July 2010 LTE Analysis NGC253 M82 TkinNH3 = 120 K TkinNH3 = 29 K 60 K < TkinCO < 130 K CS Trot = 6 K CS Trot = 4 K Trot = 12 K Trot = 15 K Trot = 33 K Trot = 24 K HC3N HC3N Trot = 12 K Trot = 26 K Trot = 73 K Trot = 36 K CH3CCH CH3CCH Trot = 45 K Trot = 24 K 23

  24. Cumberland Lodge, 5-7 July 2010 Structure of clouds in Starburst Chemistry M82 NGC253 /NGC4945 Atomic gas Atomic gas CO+, HCO, HOC+, CS n(H2) ~104 n(H2) ~104-5 CO+, HCO, HOC+, CS n(H2) ~105 HNCO n(H2) ~106 CS NO shielded core 24

  25. Cumberland Lodge, 5-7 July 2010 Chemical complexity in M82 • SiO emission (shock tracer) is out of the plane • Traces the walls of the supershells not the star forming regions • Vertical filament: SiO chimney • Gas ejected by the starburst: Superwinds Burrillo et al. (2001)‏ SiO PdBI

  26. Cumberland Lodge, 5-7 July 2010 Metalicity: Isotopic ratios 12C is primary and 13C is secondary Usually 12CO & 13CO are used to derive 12C/13C 12C/13C ratios: Solar: 90 GC: 22 M82 and NGC253 : 40-50 New values (C2H) for M82 and NGC253: > 140-80 -Isotopic fractionation for C2H -Gas has been accreted or undergoing “first” SB Martin et al(2010) 26

  27. Cumberland Lodge, 5-7 July 2010 XDRs in AGNs NGC1068: SiO and HOC+ and strong Fe 6.4 keV ( Usero et al. 2004) Nanjing, 26 October 2009 27

  28. Cumberland Lodge, 5-7 July 2010 XDR and CR CHEMISTRY 28 van der Werf et al. 2010 HIFI A&A special issue

  29. Cumberland Lodge, 5-7 July 2010 XDR CHEMISTRY High J CO lines 29 van der Werf et al. 2010 HIFI A&A special issue

  30. Cumberland Lodge, 5-7 July 2010 CR + XDR CHEMISTRY OH+ and H2O+ in MK231 30 van der Werf et al. 2010 HIFI A&A special issue

  31. Cumberland Lodge, 5-7 July 2010 CR CHEMISTRY H2O+ in M82 H2O Weiss et al. 2010 HIFI A&A special issue 31

  32. Cumberland Lodge, 5-7 July 2010 Chemical Complexity in Arp220 ULIRGs are believe to be nearby counterparts for high-z starburst galaxies Arp220 is in the final stage of galaxy merger Two nuclei at the center (~1” / 370 pc separation)‏ CO 1-0 H Sakamoto et al. (1999)‏ Nanjing, 26 October 2009 24/10/09

  33. Cumberland Lodge, 5-7 July 2010 Chemical Complexity in Arp220 SMA spectral line survey Line emission contributes 30 % of the total H2O abundance of ~2 10-5 Martin et al. (2010) 24/10/09

  34. Cumberland Lodge, 5-7 July 2010 Proto super starclusters in Arp220 Downes et al. 2007 : Compton thick AGN OPTICALLY THICK AT 1.1 MM NH2 ~ 1025 cm-3 Molecular astrophysics: the solution? 34

  35. Cumberland Lodge, 5-7 July 2010 Proto super starclusters in Arp220 Compton thick AGN? DETECTION OF HC3N* = Hot cores =protostars V7 IS TRACING HOT GAS & DUST VIBRATIONALLY EXCITED BY MID-IR RADIATION DUST IS OPTICALLY THICK AT 1.1 MM RADIATES LIKE A BLACK BODY 35

  36. Cumberland Lodge, 5-7 July 2010 Chemistry as a tracer of activity Molecular obervations provides unique information on: • The large of Complex Organic Molecules in the nuclei of galaxies • The powering source (shocks, UV, AGN and CRs?)‏ • The structure of the molecular clouds and their evolution • The evolutionary state of the nuclear starburst • The starburst, AGN and CRs effects on the surrounding ISM • The formation of starbursts (superclusters) at early stages 36

  37. Cumberland Lodge, 5-7 July 2010 THANK YOU A L M A 37

  38. Cumberland Lodge, 5-7 July 2010

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